acta polytechnica ctu proceedings doi:10.14311/app.2017.12.0079 acta polytechnica ctu proceedings 12:79–82, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app automatic generation of road infrastructure in 3d for vehicle simulators adam orlický faculty of transportation sciences, czech technical university in prague, konviktská 20, prague 1, czech republic correspondence: orlicada@fd.cvut.cz abstract. one of the modern methods of testing new systems and interfaces in vehicles is testing in a vehicle simulator. providing quality models of virtual scenes is one of tasks for driver-car interaction interface simulation. nowadays, there exist many programs for creating 3d models of road infrastructures, but most of these programs are very expensive or canâťt export models for the following use. therefore, a plug-in has been developed at the faculty of transportation sciences in prague. it can generate road infrastructure by czech standard for designing roads (čsn 73 6101). the uniqueness of this plug-in is that it is the first tool for generating road infrastructure in nurbs representation. this type of representation brings more exact models and allows to optimize transfer for creating quality models for vehicle simulators. the scenes created by this plug-in were tested on vehicle simulators. the results have shown that with newly created scenes drivers had a much better feeling in comparison to previous scenes. keywords: vehicle simulator, road design, 3d modeling. 1. introduction with emerging technologies, many branches of the technical sciences have appeared during the last few decades. one of such branches is computer graphics, whose one of the sections is the 3d modeling. it deals with displaying the real world in virtual threedimensional space. for this the 3-d modeling is used. in road transportation 3d modeling is used for the planning and design of newly projected or reconstructed roads and highways. generation of 3d models in special software is usually restricted by local laws, besides, the price of the software is rather high. most of these applications allow to create project documentation for the designed roadways, display the developed models in 3d and, in the case of highly sophisticated software, create visualization and animation. typically, exporting is not really possible, that is why this software can’t be used for other purposes[1]. in transportation, virtual reality is widely used in creation of interactive vehicle simulators. the real world can be displayed in virtual scenes with the help of projectors, or on monitors. one of the advantages of exploitation of driving simulators is a possibility to evaluate driver behavior in the conditions and situations that are precisely set up in driving scenarios. it is important that while driving the simulator a driver would get a feeling maximally approaching the experience of real driving. quality 3d models can contribute to the improvement of the visual perception. in most modern driver simulators, the road infrastructure isn’t generated according to these standards. all of this provides a motivation for the creation of a tool (as a plug-in for 3d modeling program) which is able to generate 3d road infrastructures according to czech standard[2], developed for a minimal price and for wide-ranging applications. for this purpose, we were looking for a software, where both design drawing and 3d modeling are possible. besides the generation of road infrastructure models, a tool (plug-in) should be able to complete a scene around roads in such a way, that the resulting virtual scenery would be as close to reality as possible. 1.1. driving simulator scene requirements there are rather specific requirements for 3d models of virtual scenes. driving simulator scenarios are most commonly created using the tin (triangulated irregular network) model[3]. with such a representation, the models are being created within an irregular network of triangles. these models should be as maximally close to reality as well as being simple (composed of the minimum possible number of triangles). another important requirement are the models, which are not visible to a driver (proband), needn’t be created. the last requirement would be the complexity of a model inversely proportional to the object’s distance from the road axis. application of these approaches makes it possible to use the less powerful hardware for creating virtual sceneries for driving simulator. optimized 3d scene models allow higher frame rates for the projected scenes, which provides a better illusion of a real world. 79 http://dx.doi.org/10.14311/app.2017.12.0079 http://ojs.cvut.cz/ojs/index.php/app adam orlický acta polytechnica ctu proceedings figure 1. tin models. 2. plug-in road creator for rhino plug-in road creator for rhino was created for 3d modeling and visualization program rhinoceros. the program is focused on creating models in nurbs (non-uniform rational basis spline) representation, where objects are mathematically described with the help of control points and their importance[4]. thus, the objects are more precise and don’t contain sharp edges. this kind of representation is also valuable for the possibility of further transformation of 3d model into tin model, for which it is possible to optimize the count of triangles of the model itself and thus optimize models for a driving simulator scene. figure 2. nurbs models. in the created plug-in it is possible to generate 3d models of road infrastructure (according to czech standard čsn 73 6101) into the rhinoceros software[2]. the standard is about the creation of designing roads and highways in the czech republic. other important elements in the infrastructure are generated per the corresponding standards and technical specifications. the plug-in was designed in a way that allows fast generating of the driver simulator scenes. that’s why databases with modelled objects was created for plugin. overall two databases have been formed. the first one is the database named "trees" that contains models of trees, bushes and grass and it is necessary for the completion of vegetation in the scene. the second database named "buildings" contains building and specific elements present around the roads. plug-in contains 54 new functions, due to which the scene creation is not as difficult as it used to be before. for user convenience, all the functions have been placed on a specially created control panel. for possible viewing of the scene model, the plug-in structures have newly created objects as layers. 2.1. plug-in functions the plug-in was created for the creation of driving scenarios. the creation of road infrastructure deploys five groups of functions of the plug-in. those include: • 2d road, • 3d road, • extras, • nature, • city. the functions can be accessed from the interface toolbar (see figure 3 for reference). figure 3. plug-in functions (interface toolbar). the process itself consists of four sequential stages. schematic and logical representation is shown in figure 11. stage 1 (model pre-processing) serves for the creation of a terrain model which is the basis of a road network. for transferring the 3d terrain model into the contour lines the function "contour lines" from the first group is applied (see figure 4). figure 4. terrain transfer to contour lines. at stage 2 basic curves for the future road communication are created using the functions from 2d group. with the help of horizontal (successive use of functions "tangential polygon", "arch with transition curve", and "vertical alignment" + "tangential polygon" from road 2d group) and vertical (functions "vertical alignment" and "parabolic arch") alignment combination a road track is created (see figure 5). 80 vol. 12/2017 automatic generation of road infrastructure in 3d by adding the cross-section type from the defined database of the cross-sections one defines the character of the road being created, i.e. number of lanes, their width etc. the database contains the crosssections corresponding to classes of the road defined in czech standard čsn 73 6101. figure 5. creation of road track. the plug-in provides automatic modification of the cross-sections according the curvatures and with respect to the location coordinates (e.g., at intersections) on the created road track (see figure 6). figure 6. basic road curves. now, when the basic curves are created, the 3d model of the road track can be created by using the function "3d road" from the "road 3d" menu section – the 3rd stage of the process. for the integration of the model into the terrain the function "slopes" is applied. see the result in figure 7. figure 7. road with slopes, 3d model. the 4th stage is the final one, it results in a complete road track model that includes such attributes as barriers, traffic signs, pillars etc. see example on figure 8. figure 8. complete road track model. with the help of the plug-in described, it is also possible to create other scenario attributes, such as nature, buildings etc. see the final model example in figure 9. figure 9. final 3d model. for the creation of the basic city infrastructure, a group of functions "city" shall be applied. these functions allow creation of different intersection types (see example in figure 10), sidewalks, pedestrian crossings etc. figure 10. city infrastructure – roundabout model. 3. conclusions the developed plug-in is nowadays unique regarding its possibility to create nurbs models of road infrastructure according to standard čsn 73 6101. unlike the tin models, the nurbs models are more precise, while there is a possibility of transformation of nurbs models into tin models with setting the quality of created tin models in rhinoceros software. the advantage is quality of tin models can be optimized for driving simulators. during the transferring 81 adam orlický acta polytechnica ctu proceedings figure 11. road infrastructure creation process. it has been accomplished that the models in simulator are not containing visible sharp transitions and are being formed with minimal possible number of triangles. the created 3d road infrastructure models can be also used for visualization, the plug-in can also be applied for schematic drawings of track situation and longitudinal profile, which can be used for the project documentation. besides, the major advantage of this plug-in is that it significantly reduces the time spent at modeling. creation of 3d scenery models with road infrastructure in this plug-in is the matter of several minutes. after processing of the created infrastructure in the 3d modeling engine the scenario for simulation is ready (see figure 12). figure 12. final simulation scenario. the plug-in is presently being used at transportation faculty at czech technical university in prague as a main tool for generation of scenes for driving simulators. the functions of these plug-ins were also used for the creation of animations and visualizations in the final theses of students studying at the faculty of the author. references [1] road design by autocad civil 3d and 3d max design. youtube [online]. 2014 [cit. 2016-04-29]. dostupné z: https://www.youtube.com/watch?v=eeo0wabu7ow. [2] čsn 73 6101 projektování silnic a dálnic. praha: český normalizační institut, 2004. [3] počítačová grafika: základy počítačové grafiky. ict kompetence [online]. olomouc: katedry technické a informační výchovy pdf up. [cit. 2016-04-29]. dostupné z: http://www.kteiv.upol.cz/frvs/ictkubricky/?page=pocitacova-grafika/pocitacova-grafika. [4] rhino developer docs [online]. robert mcneel & associate, ©1997-2016 [cit. 2016-04-30]. dostupné z: http://developer.rhino3d.com/. 82 acta polytechnica ctu proceedings 12:79–82, 2017 1 introduction 1.1 driving simulator scene requirements 2 plug-in road creator for rhino 2.1 plug-in functions 3 conclusions references acta polytechnica ctu proceedings doi:10.14311/app.2016.3.0071 acta polytechnica ctu proceedings 3:71–74, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app deformation characteristics of chopped fibre composites subjected to quasi-static tensile loading jan šleichrta,∗, marcel adornaa, michaela neühauserováa, nela fenclováa, veronika petráňováb a czech technical university in prague, faculty of transportation sciences, konviktská 20, 120 00 prague 1, czech republic b czech academy of sciences, institute of theoretical and applied mechanics, prosecká 76, 190 00, prague 9, czech republic ∗ corresponding author: sleicjan@fd.cvut.cz abstract. this work presents deformation behaviour of cost effective chopped fiber composites. use of chopped fibre is advantageous for manufacturing however complex shape parts production technology could be challenging. batches of samples with different fibres composition were subjected to uni-axial tensile loading to obtain overall materials properties and inspection of proper manufacturing based on local deformation inhomogeneities. both crossbeam displacement and optical strain measurement were used for elastic characteristics evaluation. deformation response was derived from full-field optical strain measurements based on digital image correlation method. relatively large variation of mechanical properties testing of samples was found. keywords: chopped fibre composites, full-field measurement, digital image correlation. 1. introduction carbon fiber reinforced thermoplastic composite become a standard construction material in last decades mainly for its good strength to weight ratio, chemical resistivity and recyclable [1]. moreover operating of light weight structures is economically beneficial. because of damage-tolerance approach used for the composite material a comprehensive knowledge of the material deformation response is required [2]. the high strength composites are in the large majority manufactured as long fibres composited. this material was intensively investigated on macromezzoand micro-level to obtain the detailed information about its deformation response to the various type of the loading [3, 4] and description of the internal damage propagation [5, 6]. however there have excellent mechanical properties its production cost is relatively high and manufacturing of complex shaped parts is challenging. for less loaded complex shaped parts are an appropriate solution usage of chopped fibre composite [7]. this cost effective material allows due to the stochastic orientation of the carbon fibre pellets manufacturing of the parts with variable thickness, holes and branchings [8]. presented article is focused on deformation behaviour of newly developed chopped fibre composite subjected to quasi-static loading. prototyped material prepared by custom designed molding system have to be inspected to discover detect defects in materials and to describe its deformation behaviour. full-field optical strain field measurement method [9] was employed for assessed of reliability of the manufacturing techfigure 1. detail of damage structure after tensile test obtained by scanning electron microscope. nology based on overall material properties and local deformation inhomogeneities. the collapsed structure of the composite specimen can be seen in fig. 1. 2. experimental procedure 2.1. specimen description dog bone shaped samples (fig. 2) with width of 20 ± 0.4 mm and thickness of 2.5 ± 0.1 mm were manufactured using custom designed mould. two sets of samples were prepared from carbon pellets with dimensions 25 × 6 mm and 13 × 3.25 mm respectively bounded with a thermoplastic matrix. thickness of the pellets was 0.14 mm in both cases. density of the final material was around 1.35 g · cm−3. the orientation of the pellets was completely random because the process of filling pellets into the shape was uncontrolled. the temperature of glass transition was 90 ◦. 71 http://dx.doi.org/10.14311/app.2016.3.0071 http://ojs.cvut.cz/ojs/index.php/app j. šleichrt, m. adorna, m. neühauserová et al. acta polytechnica ctu proceedings figure 2. visualization of sample shape. figure 3. experimental devices: 1-led light source, 2-specimen, 3-camera, 4-loading device. final samples were cut from the plate using water-jet cutter. finally, the surface of sample was equipped by random pattern point for image processing. 2.2. experimental setup experimental setup consists of instron 3382 (instron, inc.) loading device for tensile measurements and digital single-lens reflex camera with accessories. displacement controlled tests were performed with 10µm · s−1 loading rate. force was measured by high-durability load cell with loading capacity 50 kn. strain was measured optically using eos 550d (canon, japan) camera equipped with macro-objective ef100mm/1:2.8l macro (canon, japan). complete equipment is depicted in fig. 3. artificial pattern on the sample surface was illuminated by laboratory led light source kl 2500 (shott, germany). images were captured in equidistant time intervals and were labeled by unique time stamp for a precise synchronization of dic and force log. 2.3. digital image correlation strain was evaluated from the acquired image sequence using custom dic software [10] based on lucas-kanade tracking algorithm [11]. evaluating script was written in matlab environment. in the first image (prior the loading) an array of tracking features (10 × 15 points) was defined. as shown in fig. 4, the displacement of each point was identified. paths of each point were used to calculation local deformation in measured object. figure 4. detail of the displacement of a point during measurement. based on shifts of points the map of displacement was formed to verification dic method. obtained data were further processed to establish full-field strain maps. 3. results 3.1. full-field strain map for representation inhomogeneities and local deformation in object full field maps were created. calculation and evaluation those processes were completed using matlab script as well. displacements and strains calculated in each correlation point using set of matlab scripts are represented by strain maps depicted in fig. 5 to 9. from the results of the displacement mapping of the sample no. 22 (see fig. 5) expected linear behaviour without significant local inhomogeneities was observed. strains maps of selected samples of both types of pellets represented by sample no. 22 consisted of 13.0 × 3.25 mm depicted in fig. 8 and by sample no. 45 consisted of 25.0 × 6.0 mm depicted in fig. 9 discovered local strain concentrations (represented by red colour) indicating material imperfections. in case of 13.0 × 3.25 mm pellets the absolute values are lower but spread on larger area compared to 25.0 × 6.0 mm pellets specimen where deformation are higher in discontinuous area. 3.2. young’s modulus calculation of young’s modulus was done by three different approaches. firstly, results were computed from crossbeam displacement and force log. another results were calculated using displacements of points acquired from dic. average displacement of first and last line of points was used to comparison with results calculated from 5th and 11th line of points. similarly, results of two ways of calculation from dic method were found. 72 vol. 3/2016 deformation characteristics of chopped fibre composites figure 5. map of the total displacements of points. figure 6. full-field strain map of the sample 22 (smaller pellets). figure 7. full-field strain map of the sample 45 (bigger pellets). • green curve optical strain measurement, calculated between first and last row of grid. • yellow curve optical strain measurement, calculated between 5th and 11th row of grid. • red curve calculated from crossbeam displacement. figure 8. stress-strain diagram of 13 × 3.25 mm pellets; sample 22. figure 9. stress-strain diagram of 25 × 6 mm pellets; sample 45. 4. conclusions deformation behaviour of chopped fibre composites represented by stress-strain curves and strain maps was described based on optical measurement of standard tensile test. similar elastic properties in comparison with long fibre samples [3] and small differences in young’s modulus values in each set were observed. in contrary significant differences in ultimate stress (80 − 150 mpa) were observed. differences caused by fabrication technology mainly given by imperfections in the material structure was measured. as expected, the values of strains was significantly lower using optical evaluation method. strains derived from cross-head displacement were affected by backlash of the grips of the loading device. with respect to the measured data, the reliability of the optical method for investigation of local strain concentrations was proven. delivered sets of tested material were considered still unsuitable for small structural parts for the mass production. the investigated composite material and requires further improvements of fabrication process. acknowledgements the research was supported by grant agency of czech technical university in prague (project no. sgs15/225/ohk2/3t/16), by technology agency from 73 j. šleichrt, m. adorna, m. neühauserová et al. acta polytechnica ctu proceedings the czech republic (grant no. ta03010209) and by institutional support rvo: 68378297. references [1] d. steenkamer, j. sullivan. on the recyclability of a cyclic thermoplastic composite material. composites part b: engineering 29(6):745–752, 1998. [2] j. gallagher, u. s. a. force. usaf damage tolerant design handbook: guidelines for the analysis and design of damage tolerant aircraft structures : final report for period september 1980 to march 1984. no. v. 1 in usaf damage tolerant design handbook: guidelines for the analysis and design of damage tolerant aircraft structures : final report for period september 1980 to march 1984. flight dynamics laboratory, air force wright aeronautical labortories, 1984. [3] j. valach, d. kytyr, t. doktor, et al. comparison of mechanical properties of cfrp laminate obtained from full-scale test and extrapolated from local measurement. chemicke listy . [4] d. kytyr, t. fila, j. sleichrt, et al. assessment of the post-impact damage propagation in a carbon-fibre composite under cyclic loading. materials and technology 48(5):25–28, 2014. [5] p. koudelka, t. fila, t. doktor, et al. inspection of post impact fatigue damage in carbon fibre composite using modulus mapping technique. key engineering materials 606(4):245–248, 2014. [6] t. doktor, j. valach, d. kytyr, et al. analysis of cross-section surface roughness evolution of carbon fibre reinforced polymer under fatigue loading. chemicke listy 106(3):399–400, 2012. [7] composites becoming the standard in aircraft seats. jec composite magazine 43(23):34, 2006. [8] r. bockstedt, j. sajna. low cost composites based on long carbon fiber thermoplastics. proceedings of sampe 2010 conference, anaheim, usa pp. 2011–2020, 1993. [9] j. dourmaxa, s. bouvier, a. aouafi, p. vacher. fullfield measurement technique and its application to the analysis of material behaviour under plane strain mode. materials science and engineering a(500):47–62, 2009. [10] i. jandejsek, j. valach, d. vavrik. optimalization and calibration of digital image correlation method. proccedings ean 2010 pp. 121–126, 2010. [11] b. lucas, t. kanade. an iterative image registration technique with application to stereo vision. proceedings of image understanding workshop pp. 121–130, 1981. 74 acta polytechnica ctu proceedings 3:71–74, 2016 1 introduction 2 experimental procedure 2.1 specimen description 2.2 experimental setup 2.3 digital image correlation 3 results 3.1 full-field strain map 3.2 young's modulus 4 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.12.0094 acta polytechnica ctu proceedings 12:94–98, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app simulation of electric and hybrid vehicles in a vehicle simulator based on a detailed physical model, for the purpose of hmi evaluation d. rozhdestvenskiya,b,∗, j. fulemb a czech technical university in prague, faculty of transportation science, horská 3, prague, 120 00, czech republic b their ricardo prague s.r.o., palác karlín, thámova 11-13, 186 00, praha 8, czech republic ∗ corresponding author: rozhddmi@fd.cvut.cz abstract. in this article, we propose a software solution to study hmi of electric and hybrid electric vehicles in vehicle simulators. we will start with the description of a development process of a physical model for hev simulation in ignite software and equation-based language modelica. a short introduction to the language, its possibilities, and explanation, why it is more suitable for the development of such models (vehicle powertrain), are presented in the first part of the article. a fusion mechanism of the physical engine with the model by means of fmu (functional mock-up interface)[1] is also described in this part the second part is dedicated to the description of the model constructed in third party software ignite. this model has a detailed calculation of energy consumption and energy flow based on the selected control strategy. the last part of the article describes a possible experiment methodology. keywords: electric vehicle, hybrid vehicle, powertrain simulation, hmi simulation. 1. introduction electric and hybrids vehicles are slowly gaining popularity not only because it can help to reduce co2 emissions and improve the environmental situation in big cities [2], but because of the rapid development in the area of electric motors batteries and fuel cells technologies. during the latest paris motor show (2016), both vw and mercedes benz claimed to have overcome so far minimal acceptable limit of their pure ev (300 km is a minimal range acceptable by the user when considering to switch from conventional cars to ev or hev [3]) almost twice. this can be achieved because of the new ev and charging architecture developed by companies[4]. additionally, the ambitions of the automotive industry to introduce semi-autonomous and, later, fully autonomous vehicles on public roads before 2020, puts an extra urgency into design and evaluation of hmi technics for such vehicles. user vehicle interaction is shifting to a new, so far, unstudied area with familiar knobs and gauges are being substituted with touchscreens, menus, and voice interactions[5]. the notion of "familiar" car is slowly vanishing, putting a new driver (user) in a position where he has to learn how to drive a vehicle all over again if he switches the brand. this become even more crucial if we take into account that car sharing is slowly substituting car ownership[6]. the processes of development, design, and evaluation of hmi is to adapt to this rapidly changing environment. an efficient way of assessment of vehicle interfaces at different stages of their development can be achieved by testing it in a simulated environment. a model of an interactive ev and hev driving simulator with a possibility of rapid adaptation to vehicle type or architecture, with an accurate simulation of the powertrain components developed in modelica language, is hereby suggested. 2. modelica programming language modelica is an open source object-oriented language for modeling of massive, complex systems. it is suited for multi-domain modeling (including electrical, physical, thermal, mechanical and other domains), additionally, it can be used for hardware-in-the-loop simulations and for embedded control systems [7] models in modelica are mathematically described by differential, algebraic and discrete equations. from a user perspective, models are described by schematic object diagrams). the internal part of a component is defined by another schematic or on a lower level, by an equation-based description of the model in modelica syntax. an example of such a model is shown in figure 1. components can be combined in a complex model by drawing connection lines between "connectors". connectors describe the interaction possibilities (electrical pin, mechanical flange, or an input signal. regarding development time for complex models, modelica language is on average, twice as fast as any other technics in proprietary code or in any other 94 http://dx.doi.org/10.14311/app.2017.12.0094 http://ojs.cvut.cz/ojs/index.php/app vol. 12/2017 simulation of electric and hybrid vehicles in a vehicle simulator figure 1. modelica model architecture (example of schematic diagram and corresponding programming code). figure 2. development time chart. block modeling languages. this is explained by several factors: • a developer does not have to manually derive relationships between inputs and outputs between subsystems models in modelica are mathematically described by differential, algebraic and discrete equations. no particular variable needs to be solved for manually • modelica code has been developed since 1996 so a lot of subsystem components have been already developed and available for public • implementation time and complexity is the same as for any block modeling language all these points are summarized in figure 2. as mentioned above this puts modelica language ahead of others, especially when dealing with simulation of such a complex and multidisciplinary system as hybrid and electric vehicle powertrain. integration of the model in the virtual world creates a new engineering task which can be solved with an application of the fmi (functional mock-up interface standard). 3. function mockup interface functional mock-up interface (fmi) is a standard to support both model exchange and co-simulation of dynamic models developed in different independent tools, its primary goal is to support the exchange of simulation models between suppliers and oems, providing a possibility to protect product knowledge, which could be recovered from these models. this standard is going to be used to perform a simulation of the ev or hev powertrain inside a physical world simulated in ode or bullet physical engine. figure 3. fmi integration concept[1]. 4. model creation and validation a lot of commercial software available on the market are using modelica as a simulation language, and either already have, or are planning to implement fmu import/export routine. one such software is ignite, developed by ricardo software. ignite is 95 d. rozhdestvenskiy, j. fulem acta polytechnica ctu proceedings a physics-based system simulation package focused at complete vehicle system modeling and simulation. it consists of set of libraries containing vehicle and thermal system components such as engine, transmission, controllers, motors and e.t.c. these components allow faster and easier modeling and parameterization of a powertrain system for any type of vehicle, and a simulation of temperature dependent systems, which will allow further possibilities to simulate hvac and battery management of hev and ev. figure 4. model hybridization. creation of a model of hev in ignite is a straightforward process that consists of several steps [8]: (1.) collect all necessary vehicle information (tires, aerodynamics, mass etc.). vehicle manufacturer usually provides this data in technical documentation. (2.) collect powertrain information (gear efficiencies, shifting maps, engine and electric machine maps and battery characteristics). this data can either be obtained from the automaker directly on request or derived from an experimental data mathematically. (3.) build a conventional vehicle model using ignite libraries: • parametrize the model with collected data. • run test cases to validate the model. • turn the conventional model into a hybrid – add hybrid components (electric motor, battery, controller). validation of the model cacan be performed using standard driver cycles, for instance, ndc or ftp72, results obtained from the simulation on the drive cycle should be compared with an experimental data or figure 5. engine map, torque and soc results. analyzed analytically. results of the simulation contain comprehensive data for every model component and provide the possibility to perform this analysis. an example of the validation for a p2 hybrid with 1.4l tsi motor and 25 kw electrical motor is shown in figure 5. the simulation showed an average fuel consumption of 4.3 l/100km, which is equivalent to 100 g/km co2 emissions on nedc drive cycle for this model. these results closely corelate with the experimental date for similar vehicles. this validation was performed during the development stage of the hybridmodelt at ricardo p.l.c.and described in details in [8]. figure 6. engine map results. 5. integration of fmi into the simulator once the model was created and validated, it has to be modified, to perform a simulation with a physical engine. as we are interested in the interactive simulation for the purpose of hmi evaluation, we need to provide the means of control for a driver to interact with the model. at least 3 inputs have to be 96 vol. 12/2017 simulation of electric and hybrid vehicles in a vehicle simulator introduced to provide a longitudinal control of the simulated vehicle to the user. these inputs are: • acceleration demand (acceleration pedal position <0,1>). • break demand (brake pedal position <0,1>). • current vehicle velocity. velocity input provides a feedback of an actual speed of the vehicle simulated in the ode (open dynamic engine) simulation environment, which is calculated there with respect to elevation grade, tire/road contact friction, collisions, bumps etc. as a direct output, an applied wheel torque should be obtained from the model, this torque is applied to the physical model of the vehicle in the ode or bullet physical engine which is simultaneously handling latitudinal behavior. all other losses (aerodynamic, acceleration, internal and rolling losses) are calculated in ignite model directly. for the purpose of hmi simulation, we have to obtain additional outputs from the model to simulate gauges and control element of hev. these inputs are: • state of battery charge soc. • engine speed. • electric machine engine speed. • battery temperature. • ice state. these outputs can then be further processed to be displayed on a virtual gauge or in any other graphical form. the architecture of this simulation environment is shown in figure 7. figure 7. simulation architecture. 6. possible experiments with detailed consumption model after the vehicle model and simulation environment has been created, an experiment itself should be designed. we can look at four possible types of experiments with evs and hevs: • experiments aimed at determination of general user acceptance of hmi and its efficiency. • experiments aimed at study of acceptance and effect of particular hmi element. • experiments aimed at comparing different hmi. • experiments aimed to determine preferred system types of notifications per different kinds of events. even though any of these types of experiments should be adapted to a specific requirement, one may distinguish ten high-level steps essential for any type of experiment. (janssen at al. 2004): (1.) to determine the goals of evaluation in terms of usability, safety, workload, acceptability, time frame. (2.) to describe a system (systems) which will be tested during the experiment. (3.) to define a high-level scenario (scenarios) in terms of road type, and conditions, visibility, traffic type and actors, tasks, and goals. (4.) define the subject testing cohort in terms of amount, age and experience group. (5.) define subjective and objective evaluation parameters and instruments for data acquisition. (6.) develop experimental instruction for both participants and experimenters. (7.) perform a pilot experiment test and data evaluation. (8.) carry out the experiment. (9.) analyze data. (10.) produce summary report and draw a conclusion. 7. conclusion in this article, we presented a methodology for development and integration of high fidelity powertrain model of ev or hev into three-dimensional virtual simulation environment. this model provides a comprehensive and precise data results to simulate next generation hmi for ev or hev including gauges and functions (such as power-in-out gauges, predictive navigation and others). these models are written in modelica programming language and coupled with ode or bullet physical world with the help of fmi. this approach allows a rapid development and validation of models, and a quick way of switching between them. references [1] t. b. at all. the functional mockup interface for tool independent exchange of simulation models. in proceedings of the 8th international modelica conference. [2] d. rozhdestvenskiy, p. bouchner, a. mashko, et al. dynamic human-machine interface for electrical vehicle design guidelines. smart cities symposium prague 2015, isbn 978-1-4673-6727-1. 97 d. rozhdestvenskiy, j. fulem acta polytechnica ctu proceedings [3] t. smith, h. vardhan, b. malet, d. mingay. are we there yet. thoughts on in-car hmi. 2014. [4] g. e. outlook2016. beyond one million electric cars. international energy agency, electric vehicle initiative. [5] s. heath, p. sant, b. allen. do you feel lucky? why current range estimation methods are holding back. ev adoption hybrid and electric vehicles conference 2013 (hevc 2013), iet year: 2013. [6] p. b. et al. professional vehicle drivers training and performance measurements with use of advanced driving simulator laboratory. 1.ed., prague: ctu in prague, faculty of transportation sciences, department of vehicles, 2013, 1st, electronic edition. isbn 978-80-01-05421-5. [7] j. tobolar, m. otter, t. bunte. modelling of vehicle powertrains with the modelica powertrain library. in: dynamisches gesamtsystemverhalten von fahrzeugantrieben. [8] j. fulem. ignite & wave-rt powertrain model connected to ipg virtual test driving platform. in: ricardo software usercon europe. 98 acta polytechnica ctu proceedings 12:94–98, 2017 1 introduction 2 modelica programming language 3 function mockup interface 4 model creation and validation 5 integration of fmi into the simulator 6 possible experiments with detailed consumption model 7 conclusion references acta polytechnica ctu proceedings doi:10.14311/app.2016.5.0022 acta polytechnica ctu proceedings 5:22–25, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app infrastructure parameters affecting capacity of railways in ten-t vít janoš∗, milan kříž department of logistics and management of transport, faculty of transportation sciences, ctu in prague, czech republic ∗ corresponding author: janos@fd.cvut.cz abstract. the article presents possible solutions of the issue of the lost capacity on a double-track line. it is shown a solution where an inserted train on the double-track line use the lost capacity of the opposite line track using active overtaking. the feasibility of such a solution is discussed and the length of sections suitable for active overtaking is calculated. keywords: capacity, uic 406, speed ratio . 1. introduction the capacity of the railway infrastructure can be considered as a usable time space for the train paths. capacity is thus influenced not only by the parameters of the infrastructure, but also by the character of the traffic – by the designed train paths and their heterogeneity. with increasing degree of heterogeneity the capacity consumption increases too and the number of possible train paths in a defined time windows declines. this phenomenon is also called "capacity balance" [1]. in the capacity balance there are four factors on whose interdependencies the capacity is based: number of trains, average speed, stability and heterogeneity. relationships among the individual factors are shown in figure 2 [1]. principle of figure 2 is explained as follows: "in this qualitative model, an axis for each parameter is drawn from a unique origin. a chord links the points on the axes, corresponding to the value of each parameter. the length of the chord represents the capacity. capacity utilisation is defined by the positions of the chord on the four axes. increasing capacity means increasing the length of the chord". general effect associated with the modernization of the trans-european conventional rail network (typically the modernization of the transit railway corridors in the czech republic in the original routes to a maximum speed of 160 km/h) is the rising heterogeneity of the traffic on some routes in the network. it is caused by increasing the line speeds. on the one hand regional passenger train paths remains after increasing the line speed about as fast as before the modernization (journey speed of the regional trains usually does not exceed 60 km/h due to the higher number of stops). on the other hand long-distance passenger trains should logically utilize all characteristics of infrastructure for the maximum journey speed (at the fastest trains the journey speed of 120-140 km/h can be reached in some line sections). these both cases are thus usually marginal and between these limits figure 1. possible situation of active overtaking on a double-track line. the freight trains paths occur (with journey speeds in the range of 70-100 km/h). 2. heterogeneity and its measuring heterogeneity can be measured in different ways. one way is to compare running speeds of individual train (or train paths). for this purpose krueger [2] proposed and used so called speed ratio (sr). the speed ratio is the ratio of the fastest train speed to the slowest train speed: sr = max(v1, v2, ..., vn) min(v1, v2, ..., vn) so the sr on the typical line section on some transit railway corridor in the czech republic can reached value of 3 (the speed of the fastest train about 140 km/h and the speed of the slowest train about 45-50 km/h). 22 http://dx.doi.org/10.14311/app.2016.5.0022 http://ojs.cvut.cz/ojs/index.php/app vol. 5/2016 infrastructure parameters affecting capacity of railways in ten-t figure 2. capacity balance [1]. the very high sr is problematic only when it comes to the line or line section with a high number of train paths. but the lines of the trans-european conventional rail network usually show a high number of train paths. line sections with high demand for train paths and a high sr can usually be solved by segregating the various types of traffic. this entails increasing the number of line tracks (e.g. quadruple-track line sections in urban agglomerations with two tracks for long-distance passenger trains and fast freight trains and two tracks for slower regional passenger trains and slower freight trains) or construction of lines dedicated exclusively for a certain type of traffic (typically on the one hand high-speed railway lines and, on the other hand, lines dedicated only for freight train as e.g. betuwelijn). this approach, however, is not yet common in the czech republic. 3. active overtaking on double-track lines, where high degree of heterogeneity is because of the mixed traffic and high requirements for the number of the train paths, so called lost capacity arises. lost capacity is unusable time space between train paths with different train speeds, where any additional train path cannot be inserted (e.g. because there is no other station). lost capacity can be limited by reducing heterogeneity of train paths. either the slowest trains can be accelerated (e.g. these trains can pass some stops), or vice versa the fastest trains can be slowed. lost capacity may be also used for active overtaking1. an example of this solution is shown in the figure 1. active overtaking is a very interesting possibility of using a part of the lost capacity. this idea can be very helpful in cases, when the number of stations on a line section is reducing within modernization of infrastructure. in the former stations there are only crossovers for crossing between the line tracks for cases of interruptions. in such cases there is no possibility to insert one more train path into a sequence of differently 1active overtaking can be defined as an overtaking of slower train by faster train, when the slower train does not have to stop [3]. fast train paths, but they can also be used for crossing between line tracks and in regular operation. the actual possibility of using these crossovers for regular traffic, however, depends on the diverging speed that affects the train speed (and thus journey time) of the overtaking or the overtaken train and thus affects the length of the section required for overtaking. furthermore, it is obvious that the greater the heterogeneity of the train paths in the reference section is (i.e. the larger the difference of the journey speeds between the overtaken and the overtaking train), the shorter the section required for overtaking is. with regard to the above mentioned borderline cases it is evident that the overtaken slower train is always a regional passenger train. there are generally two cases possible: (1.) the slower train crosses over to the other line track and runs against the right direction, the faster train runs in the right direction. (2.) the faster train crosses over to the other line track and runs against the right direction, the slower train runs in the right direction. the cases from the first group are suitable for situations, in which the platforms of stations and stops in the line section are situated between the line tracks, or in which only stations equipped with a good visual and audible information system are. this system should provide clear information about platforms and tracks of arriving and departing trains. the cases from the second group are suitable, if the speed limit over the crossovers between the line tracks corresponds or is close to the line speed or the maximum train speed. 4. case study: the first transit railway corridor between prague and děčín the part of the first transit railway corridor between prague and děčín links the prague metropolitan area [4] with the ústí metropolitan area and with the north part of germany. the most typical situation for the active overtaking is an interaction of a fast freight train (maximum train speed about 100 km/h) and a regional passenger train (journey speed about 50 km/h). the active overtaking of the first type can be used in the line sections: • hněvice – hněvice seř.n. • roudnice nad labem – hrobce • lovosice jih – lovosice • prackovice nad labem – ústí nad labem jih – ústí nad labem hl.n. now we have to analyse these line section, whether the active overtaking leads to time saving in comparison with overtaking of the regional passenger train 23 vít janoš, milan kříž acta polytechnica ctu proceedings figure 3. relationship between speed ration and length of section for overtaking. by the fast freight train, when the regional passenger train is dwelling in some station. sections hněvice – hněvice seř.n. and lovosice jih – lovosice can be excluded immediately, because the result time savings will be negative. in both cases the regional passenger train is stopping only once in the line section and in both cases the speed limit over crossovers in the stations which bounds the line section is lower than the speed limit on passing sidings in these stations. sections roudnice nad labem – hrobce and prackovice nad labem – ústí nad labem jih – ústí nad labem hl.n. show always positive time savings. in both cases the regional passenger train is stopping twice in the line section2. in these cases, the parallel run is generally about 2 minutes more effective then overtaking of the slower train in the station. it is very important that the overtaking train is guided precisely to the desired time position. the accuracy of this guidance may have a significant effect on the resulting time savings. by the active overtaking of the second type the journey time of the overtaking train is extended because of the diverging speed of the crossovers in the bounding stations. in table 1 values for typical situation on the first transit railway corridor are shown. the values were calculated with linear margin 9%. value are graphically illustrated in figure 3. from table 1 it is possible to determine the length of the line section which is needed for active overtaking. if the actual line section is shorter, then the dwell times of the slower train have to be extended. 5. conclusions the verification of heterogeneity in relation to the partial use of the lost capacity by active overtaking of differently fast trains showed clearly that in the case of the interaction of regional passenger trains and freight trains there are solutions which can be divided into 2also the stops in bounding stations of the line section are counted, if the regional passenger is being already overtaken during the stay in the station. sum of operating intervals and time reserves [min] 5 journey speed of slower train [km/h] 50 speed ratio [1] speed of faster train [km/h] length of section for overtaking [km] 1,1 55 45,83 1,2 60 25,00 1,3 65 18,06 1,4 70 14,58 1,5 75 12,50 1,6 80 11,11 1,7 85 10,12 1,8 90 9,38 1,9 95 8,80 2 100 8,33 2,1 105 7,95 2,2 110 7,64 2,3 115 7,37 2,4 120 7,14 2,5 125 6,94 2,6 130 6,77 2,7 135 6,62 2,8 140 6,48 2,9 145 6,36 3 150 6,25 table 1. length of section for overtaking. two situations. either if the diverging speed over the crossovers in the bounding station of the line section is clearly lower than the running speed of the fast freight train, then the regional passenger train should run against the right direction on the other line track. or if the diverging speed over the crossovers in the bounding station of the line section is high enough (minimum is 80 km/h), then then the fast freight train should run against the right direction on the other line track. it is important to mention that by modernizing the infrastructure, which should also allow such use of the lost capacity, platforms should be mostly located between the main line tracks. with regard to the actual length of the line sections for active overtaking and with regard to demand for the train paths it is necessary to mention that on 24 vol. 5/2016 infrastructure parameters affecting capacity of railways in ten-t trans-european conventional rail network this solution will be usually marginal. furthermore, it is likely that the heterogeneity of demanded train paths will not decline. authorities ordering the long distance passenger trains and open access operators do not want to, on the one hand, slow down artificially their trains. on the other hand, local authorities ordering the regional passenger trains do not want to reduce the number of operated railway stops, which is a very problematical political topic. in the czech republic the construction of quadrupletrack line sections remains as a permanent challenge in cases where a high degree of heterogeneity connected with high demand for train paths occurs. only such a solution leading to the segregation of various types of traffic allows homogenization of the train paths and effective elimination of the lost capacity. references [1] uic leaflet 406 capacity. paris: international union of railways (uic). [2] h. krueger. parametric modeling in rail capacity planning. simulation conference proceedings. az, phoenix, 1999. [3] m. drábek. periodic freight train path in network. čvut, praha, 2014. [4] t. kostelecký, d. čermák. metropolitan areas in the czech republic definitions, basic characteristic, patterns of suburbanisation and their impact on political behaviour. sociologický ústav av čr, 2004. 25 acta polytechnica ctu proceedings 5:22–25, 2016 1 introduction 2 heterogeneity and its measuring 3 active overtaking 4 case study: the first transit railway corridor between prague and decín 5 conclusions references 235 acta polytechnica ctu proceedings 1(1): 235–239, 2014 235 doi: 10.14311/app.2014.01.0235 data analysis of globular cluster harris catalogue in view of the king models and their dynamical evolution. ii. observational evidences marco merafina1, daniele vitantoni1 1department of physics, university of rome la sapienza, piazzale aldo moro 2, i-00185 rome, italy corresponding author: marco.merafina@roma1.infn.it abstract we summarize some observational comparison concerning the features of globular clusters (gcs) population in connection to the evolution of king models. we also make a comparison with some extragalactic gcs systems, in order to underline the effects of the main body on the dynamical evolution. keywords: globular clusters gravothermal catastrophe king models thermodynamical stability. 1 introduction globular clusters (gcs), for their proprieties of symmetry and their high relaxation times, are important to test theories about thermodynamical stability of spherical self gravitating systems. the actual sample of is a mixture of various and not homogeneus gcs types. therefore, it is difficult to analyze properties of milky way (mw) gcs population in connection to core-collapse and gravotermal instability. the last version (2010) of harris gcs catalogue (see also harris, 1996) includes 157 objects. it was pointed out by van der bergh (2011) that harris catalogue could includes three not typical gcs, probably remnant cores of dsph galaxies: omega centauri, terzan 5 and ngc 6715 (m54). the harris catalogue also includes pcc gcs, namely gcs with collapsed cores that cannot be described by classical single mass king models profiles. zinn (1985) identifies two classes of gcs, respectively known as disk population (metal rich) and halo population (metal poor), distinct by the threshold value [fe/h] ' −0.8 (or, according to some authors, −0.75). recently bica et al. (2006) showed that the actual gcs population seems to have been contaminated by capture of smaller galaxies (and their possible gcs populations) during the milky way formation. possible evidences of extragalactic origin of some gcs are retrograde motion (compared to galactic disk motion) and unusual young absolute age. it seems that the original gcs population suffered deep and incisive processes of disruption (see aguilar et al., 1988; hut & djorgovski, 1992; gnedin & ostriker, 1997; mackey & gilmore, 2004), until almost 50% of original gcs are destroyed in the last hubble time. 2 discussion we start to consider the problem introduced by katz in the paper about thermodynamic stability in 1980. the study of the distribution of galactic gcs in terms of w0 (central gravitational potential) shows a peak value of 6.9. we should expect that the peak value coincides with the known stability critical value w0 = 7.4, due to the old age of mw gcs and the onset of the instability in the high w0 region. this problem had remained unsolved (fig.1). figure 1: distribution of galactic gcs at different k (katz, 1980). the quantity k is related to w0 (see merafina & vitantoni, part i). with the introduction of the effective potential (see merafina & vitantoni, part i) and including the additional term in the expression of the total energy, we can revise the katz study. the result is a very satisfactory coincidence of the observative peak value with the stability limit. we can also repeat the analysis on a more detailed and updated sample (using data of the harris gcs catalogue). the peak value, in the non-symmetric 235 http://dx.doi.org/10.14311/app.2014.01.0235 marco merafina, daniele vitantoni gaussian hypothesis, is exactly at w0 = 6.9 (fig.2). 0 2 4 6 8 10 12 14 0 2 4 6 8 10 12 14 figure 2: w0 distribution of pre-core-collapse mw gcs. for a better understanding of the evolution of a gcs population, we briefly analyze the role of environmental features. the effect of the distance from the galactic center (fig.3) is not clear at all. generally speaking, the more a gc lives near the galactic center, the more quickly it evolves towards the gravothermal catastrophe, being more affected by tidal forces of the galaxy. 2 4 6 8 10 12 14 1 10 100 r gc figure 3: galactocentric distance rgc in function of w0. the dashed lines represent the values at 3kpc and 30kpc. if we look at the gcs distribution in the [fe/h]-w0 plane (fig.4), we find no correlations between these two quantities. this means that the difference between halo and disk population, first introduced by zinn (1985) does not influence the dynamical features and the evolution. nevertheless, if we analyze the disk population (fig.5), this seems to be more dynamically evolved than the halo one. the w0 peak value is slightly larger for the disk population, mainly due to a lower rgc (in average) for this class of objects. on the other hand, it is well known that the tidal shocks played a more incisive role in the evolution of the disk gcs. 2 4 6 8 10 12 14 -2.5 -2.0 -1.5 -1.0 -0.5 0.0 figure 4: total metallicity [fe/h] in function of w0. 2 4 6 8 10 12 14 0 2 4 6 8 10 12 n w0 external halo internal halo figure 5: w0 distribution of astronomical populations. the contamination of the halo gcs with the extragalactic origin ones is suggested by the bimodality in the absolute age distribution, by the rotation in the plane of galactic disk, and by the age-metallicity dependence. the situation is shown in figs.6, 7 and 8. regarding the age-metallicity dependence, we can say that few objects are located out of the main well defined sequence of clusters (and probably have a different origin with respect to all the others). 236 data analysis of globular cluster harris catalogue... part ii figure 6: absolute age distribution for mw gcs. older gcs, presumably all native in the milky way, are evidenced in dark grey. figure 7: motion over the galactic plane for mw gcs (from dinescu et al., 1999). figure 8: age-metallicity behavior, using the absolute age values extimated by dotter et al. (2010). pcc clusters are indicated by grey squares, suspected pcc ones by white triangles. if we analyze the behavior of the central relaxation time trc in function of w0 (fig.9), we can note a linear decreasing, that indicates an increasing of evolutional speed towards the collapse. below the treshold value log trc = 8.0 there is a region of coexistence of pre-core collapse gcs with post-core collapse (pcc) ones. the behavior of core collapse time tcc (that is the remaining time before the collapse of the model), changes over the stability limit w0 = 6.9 (fig.10). 2 4 6 8 10 12 14 4 5 6 7 8 9 10 11 rgc< 3 kpc 3 kpc < rgc< 30 kpc rgc> 30 kpc lo g (t rc /1 yr ) w0 ngc6717 figure 9: behavior of trc in function of w0; three classes of cluster distances are represented. vertical dashed line represent the stability limit, whereas the horizontal one represent the trc critical value (cohn & hut, 1984) distinguishing pre-core-collapsed and postcore-collapsed objects. suspected pcc clusters are indicated by filled symbols. in the harris catalogue ngc6723 has been erroneously included among the suspected pcc clusters in place of ngc6717. 2 4 6 8 10 12 14 7 8 9 10 11 12 lo g (t cc /1 yr ) figure 10: core-collapse time in function to w0. the tcc values are estimated as in quinlan (1996). we also consider a comparison among four gcs populations, shown in fig.11: the lmc is the less evolved, as well as the smc and fornax systems (mackey & gilmore, 2003b, 2003c); it presents a peak value close to w0 = 4.3. for this kind of gcs population, the presence of a low massive main body allowed to preserve 237 marco merafina, daniele vitantoni more informations about primeval distribution features. on the contrary, ngc5128, whose main body is a giant elliptical galaxy, seems to be an evolved population with a maximum value up to the threshold value w0 = 6.9. finally, the m31 system is the most similar to our gcs population, with a main peak value around the stability limit and an extended tail in low-w0 region, that is produced by the presence of low evolutionary speed objects or extragalactic origin clusters. also the effects of disk and bulge shocking, realistically, concurred to the formation of the tail. 3 conclusions in order to analyze the dynamical evolution of king single mass gcs, we have analyzed the mw gcs population. the mw clusters w0 distribution presents a peak very close to the new stability limit w0 = 6.9 and a pronounced tail in the low-w0 region. 3 6 9 12 0 5 10 0 5 10 0 3 6 3 6 9 12 0 3 6 w0 mw n m31 lmc figure 11: comparison among w0 distributions of different gcs systems. in addition to mw system, m31, ngc5128 and lmc systems are reported. m31 data come (or are deduced) from barmby et al. (2007), ngc5128 ones from gòmez et al. (2005), lmc data from mackey & gilmore (2003a). mw histogram differences from fig.2 are given by a different binning choice. we can instead exclude a direct relation between astronomical gcs populations and dynamical evolution, except for a very weak increasing of w0 peak value for disk clusters. from the time-scales we can deduce that clusters with high w0 value have an higher collapsing speed. the gravothermal catastrophe produce an alteration of the natural evolutionary sequence for clusters with w0 ≥ 6.9. from the comparison with extragalactic gcs systems we have deduced that, in the case of lmc, smc and fornax system, these clusters have a gaussian like distribution around a peak value w0 ∼ 5. mw and m31 system are very similar in their features and w0 distribution, with low-w0 tail and a peak value in corrispondence of the stability limit. we can assume this as the main product of disk shocking, as well as extragalactic capture and low speed evolution objects mentioned above. for ngc5128 there is no low w0 region tail, but only a narrow peaked distribution around the stability limit. references [1] aguilar, l., hut, p., ostriker, j.p.: 1988, apj, 335, 720 doi:10.1086/166961 [2] barmby, p., mclaughlin, d.e., harris, w.e., gretchen, l.h., forbes, d.a.: 2007, aj, 133, 2764 [3] bica, e., bonatto, c., barbuy, b., ortolani, s.: 2006, aap, 450, 105 doi:10.1051/0004-6361:20054351 [4] cohn, h., hut, p.: 1984, apj, 277, l45 doi:10.1086/184199 [5] dinescu, d.i., terrence, m.g., van altena, w.f.: 1999, aj, 117, 1792 [6] dotter, a. et al.: 2010, aj, 708, 698 [7] gnedin, o.y., ostriker, j.p.: 1997, aj, 474, 223 [8] gòmez, m., geisler, d., harris, w.e., richtler, t., harris, g.l.h., woodley, k.a.: 2006, aap, 447, 877 doi:10.1051/0004-6361:20053393 [9] harris, w.e.: 1996, aj, 112, 1487 [10] hut, p., djorgovski, s.: 1992, nat, 359, 806 doi:10.1038/359806a0 [11] katz, j.: 1980, mnras, 190, 497 doi:10.1093/mnras/190.3.497 [12] king, i.: 1966, aj, 71, 64 [13] mackey, a.d., gilmore, g.f.: 2003a, mnras, 338, 85 doi:10.1046/j.1365-8711.2003.06021.x 238 http://dx.doi.org/10.1086/166961 http://dx.doi.org/10.1051/0004-6361:20054351 http://dx.doi.org/10.1086/184199 http://dx.doi.org/10.1051/0004-6361:20053393 http://dx.doi.org/10.1038/359806a0 http://dx.doi.org/10.1093/mnras/190.3.497 http://dx.doi.org/10.1046/j.1365-8711.2003.06021.x data analysis of globular cluster harris catalogue... part ii [14] mackey, a.d., gilmore, g.f.: 2003b, mnras, 338, 120 doi:10.1046/j.1365-8711.2003.06022.x [15] mackey, a.d., gilmore, g.f.: 2003c, mnras, 340, 175 doi:10.1046/j.1365-8711.2003.06275.x [16] mackey, a.d., gilmore, g.f.: 2004, mnras, 355, 504 doi:10.1111/j.1365-2966.2004.08343.x [17] quinlan, g.d.: 1996, newa, 1, 255 [18] van den bergh, s.: 2011, pasp, 123, 1044 doi:10.1086/662132 [19] zinn, r.: 1985, apj, 293, 424 239 http://dx.doi.org/10.1046/j.1365-8711.2003.06022.x http://dx.doi.org/10.1046/j.1365-8711.2003.06275.x http://dx.doi.org/10.1111/j.1365-2966.2004.08343.x http://dx.doi.org/10.1086/662132 introduction discussion conclusions acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0022 acta polytechnica ctu proceedings 4:22–26, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app thermal-hydraulic analysis of irt-4m in reactivity insertion accident at vr-1 reactor filip fejt faculty of nuclear sciences and physical engineering, czech technical university in prague, czech republic correspondence: filip.fejt@fjfi.cvut.cz abstract. the paper deals with thermal-hydraulic analysis during reactivity insertion accident, i.e. a step increase of nuclear system reactivity by 0.7βeff , at vr-1 reactor. the reactor utilizes irt-4m type of fuel assemblies, and even though these fuel assemblies are designed for an operation at the high-power research reactors, they might be also used for zero-power reactors. the thermal-hydraulic analyses must take into account several specific assumptions that are derived from vr-1 reactor specifications. the reactor does not require a forced water flow for a fuel cooling, the core is placed in an open vessel with atmospheric pressure, and amount of coolant water in the vessel is sufficient for providing the inlet water at room temperature for the whole event. coolant circulation is expected to be formed only by natural convection. keywords: irt-4m, ria, relap5, trace5, natural convection. 1. introduction thermal-hydraulic analysis is a necessary part of every safety analyses report. the adequate cooling of the fuel assemblies must be ensured to maintain the core integrity during normal and abnormal operational transients, and accidents. in general, the research reactors may be designed for both natural convection and forced convection. the pool type research reactor vr-1 uses a natural convection of coolant to remove a core heat. the upward flow in natural convection is caused by different fluid densities of heated and unheated volumes. important point of safety analyses is an onset of nucleate boiling (onb) [1] that is defined as a difference between the fuel surface temperature at the starting point of a nucleate boiling and the fuel surface temperature at a local cooling condition. reaching a nucleate boiling significantly limits the heat transfer leading to a dramatic increase of the fuel surface temperatures in order to maintain the total heat flux. the main purpose of thermal-hydraulic analysis is to inspect all of possible events that may lead to an accident, and verify that normal and abnormal operation has safety margins before the critical level is reached. 2. thermal-hydraulic codes due to the various research reactor designs, i.e. operational mode, fuel type and applications, each reactor has a unique thermal-hydraulic characteristic. computational codes must be capable of dealing with a broad range of different designs. since the current codes are still based on dimensionless quantities that are used to calculate flow patterns in different fluid situation, the equations are mostly derived from simplified benchmarks and loops that must be considered similar to a problem of interest. although many well-known codes, e.g. relap, trace, paret, have been designed for power reactors at first, they have been developed into general calculation tools that may be used even for research reactors. the main phenomena of vr-1 reactor analysis is natural convection, and therefore the chapter is followed by a brief description of natural convection part of the codes. 2.1. relap5 the relap5/mod3.3 code has been developed for best-estimate transient simulation of light water reactor coolant systems during postulated accidents [2]. the code includes several behaviors effecting a reactor coolant, e.g. loss-of-coolant accident, anticipated transient without scram, loss of feedwater, loss of flow etc. unlike its predecessors, relap5 series uses a two-fluid, nonequilibrium, nonhomogeneous, hydrodynamic model for transient simulation of the two-phase system behavior. convection calculations rely on evaluating forced convection, laminar convection, and natural convection and selecting the maximum of these values. the correlations are by dittus-boelter [3], kays [4], and churchill-chu [5] respectively. 2.2. trace trace has been designed to calculate best-estimate analyses of loss-of-coolant accidents, operational transients, accidents in pressurized light-water reactors and boiling light-water reactors [6]. the code includes multidimensional two-phase flow, nonequilibrium thermo-dynamics, generalized heat transfer, level tracking, and reactor kinetics. the partial differential equations that describe twophase flow model are solved using finite volume numerical methods. components are solved in one-dimension 22 http://dx.doi.org/10.14311/ap.2016.4.0022 http://ojs.cvut.cz/ojs/index.php/app vol. 4/2016 thermal-hydraulic analysis of irt-4m in ria at vr-1 or three-dimensions when necessary. timesteps are limited by courant-limit factor to ensure the computational stability of an examined system. the courantlimit depends on a phenomena and current conditions in a system. description of this factor can be found in [2]. similar to relap5, the trace follows a component-based approach to modeling a reactor system. each part of the system is inserted as a unique component. list of components in the code is designed to cover all power plant models. after that all the components are connected as the user requires. expected mode of calculation in examined ria is pre-critical heat flux region. the correlations are provided for the laminar and turbulent forced convection regimes and for natural convection. the wall heat transfer coefficient for single-phase liquid [6] convection is taken as the maximum of the values for laminar and turbulent forced convection and natural convection (1) hwl = max{hlam, hturb, hnc}, (1) where hnc is the wall heat transfer coefficient for natural convection, hlam is the wall heat transfer coefficient for laminar forced convection, and hturb is the wall heat transfer coefficient for turbulent forced convection. heat transfer coefficient for natural convection uses correlations for both the laminar and turbulent regimes and a maximum of the two values is used to ensure continuity. the heat transfer coefficient is computed from (2) hnc = kl dh ·nunc, (2) where k is thermal conductivity evaluated at the bulk fluid temperature and dh is the hydraulic diameter. the nusselt numbers are given by (3) and (4) nunc,turb = 0.1 · (gr l · pr l)1/3, (3) nunc,lam = 0.59 · (gr l · pr l)1/4. (4) both grashof and prandtl numbers are evaluated at bulk fluid temperature. 3. vr-1 reactor model the vr-1 core is placed in a vessel with large water reserve. during the transient the water reserve ensures the room temperature at the core inlet. even though the transient may last several hundred seconds, the average water temperature in the vessel will not increase because the flow rate caused by natural convection is very small. in order to maximize the first power peak, the coolant is expected to be stationary at the beginning of the simulation. this condition can be achieved when the main pump in the vessel is turned off and the reactor is operated at the very low power causing minimal flow velocity. the irt-4m fuel assemblies used the vr-1 reactor consist of 4, 6, or 8 fuel layers arranged in rounded rectangular tubes [7]. each fuel layer is surrounded by cladding layer from both inner and outer side. cladding layers are made of aluminium similar to fuel layers where the uo2 is dispersed also in aluminium. a thin layer thickness, both the fuel and the cladding, in addition to a high thermal conductivity of the aluminium leads to a very flat radial temperature profile in fuel assemblies. the core is represented by an averaged 8-tube fuel assembly (fig. 1) to comply with point kinetic equations that are integrated into the computational codes [8]. figure 1. top view of 8-tube irt-4m fuel assembly (yellow – water coolant, blue – cladding layer, green – fuel layer). 3.1. relap5 specification using the component-based structure of input files, a list of utilized components can be found in tab. 1. the bottom plenum serves as a coolant distributing element at the bottom part of fuel assembly. distributed coolant flows through the fuel assembly (each pipe represents one coolant flow area between heatstructures), and at the top of the fuel assembly the top plenum mixes the heated coolant that flows directly to the vessel water reserves. the model can be seen in fig. 2. component number pipe (fa coolant) 8x pipe (vessel) 1x heatstructure (fuel tubes) 8x plenum 2x table 1. list of relap5 components utilized in the single assembly vr-1 model. 23 filip fejt acta polytechnica ctu proceedings figure 2. relap5 model with green pipes connected to heatstructures, bottom and top plenum, and a large pipe serving as a reactor vessel. 3.2. trace specification unlike relap5 model, the trace model is not using the plenum component for distributing and mixing the coolant because it is assumed to be obsolete in current development. its role has been taken by advanced pipe settings; unfortunately, the low dimensions of fuel assembly flow surfaces and complex flow distribution made it inapplicable in this model. therefore the bottom and top plenum were replaced by independent pipes denying any interaction between coolant coming to/from flow surfaces. similar idea had to be applied also to the pipe representing the vessel; the vessel is divided into 8 pipes. the model can be seen in fig. 3. this pipe separation requires an extended usage of components (tab. 2). component number pipe (fa coolant) 8x pipe (vessel) 8x heatstructure (fuel tubes) 8x pipe (bottom plenum) 4x pipe (top plenum) 4x table 2. list of trace components utilized in the single assembly vr-1 model. 4. results for the sake of clarity, the graphical interpretation of results follows two main rules – relap results are plotted with connected points and -r is added in the legend; trace results are plotted with separate points and -t is added in the legend. each figure 3. trace model with green pipes connected to heatstructures, set of pipes serving as bottom and top plenum, and set of pipes serving as a reactor vessel. spatial value is considered to be averaged over flow surface, therefore such a value has a two digit number representing a number of outer and inner fuel layer (fuel layer number starts from the outside of the fuel assembly: 1, 2, 3, . . . , 8, v denotes central area). 4.1. reactor power output the reactor power and the reactivity of the system can be seen in fig. 4. the reactivity is increased to the value of 0.7βeff at t = 0.5 s, after that the value is decreased by feedback effects created from both the fuel and the moderator. the reactivity increase starting at t = 20 s is caused by the slowly increasing coolant velocity effecting its heat removal capabilities. after 200 seconds the reactivity reaches the zero value. 4.2. coolant velocity fig. 5 shows a fast velocity increase of coolant that causes the reactivity peak shown in fig. 4. this analysis is valid as long as the initial coolant velocity is zero, i.e. vessel pump is turned off, and the reactor power is very low. 4.3. coolant temperatures the temperatures of flow surfaces are shown in fig. 6. no coolant reaches the boiling point during the occurring ria event. it can be clearly seen that both relap5 and trace have a very good agreement in coolant temperatures between outside fuel layers. the difference between the codes is approx. 10 ◦c in the middle of the fuel assembly. 5. conclusions despite the equation differences that can be found in both codes, relap5 and trace code shows a very good agreement in both point kinetics and thermalhydraulic. even though a difference can be observed 24 vol. 4/2016 thermal-hydraulic analysis of irt-4m in ria at vr-1 figure 4. reactor power and reactivity of system during step increase of reactivity accident by 0.7βeff . figure 5. outlet coolant velocity during step increase of reactivity accident by 0.7βeff . figure 6. outlet coolant temperature during step increase of reactivity accident by 0.7 βeff . 25 filip fejt acta polytechnica ctu proceedings in the final power, it has no effect on maximal outlet coolant temperature. higher power, i.e. higher heating, is always compensated by an increase of velocity of a coolant that leads to a temperature decrease. the coolant velocity can be compared to negative reactivity feedback effects. the separate pipes can be considered as the most significant difference between both models. this effect can be seen in inner flow cross sections where the temperature difference can reach up to 10 ◦c. since the maximal temperatures are reached in outer flow cross sections and both codes compute the same coolant temperature, it can be safely assumed that the separate pipe model does not effect the maximal temperatures. references [1] j. daeseong, p. suki, p. jonghark, et al. cooling capacity of plate type reserach reactors during the natural convective cooling mode. progress in nuclear energy 56:37–42, 2012. [2] u.s. nuclear regulatory commission. relap5/mod3.3 code manual volume i: code structure, system models, and solution methods, 2010. division of systems research, office of nuclear regulatory research. [3] f. dittus, l. boelter. heat transfer in automobile radiators of the tubular type. publications in engineering 2:443–461, 1930. [4] w. kays. numerical solution for laminar flow heat transfer in circular tubes. american society of mechanical engineers 77:1265–1274, 1955. [5] s. churcill, h. chu. correlating equations for laminar and turbulent free convection from a vertical plate. international journal of heat and mass transfer 18:1323–1329, 1975. [6] u.s. nuclear regulatory commission. trace v5.840 theory manuals: field equations, solution methods, and physical models, 2013. division of systems research, office of nuclear regulatory research. [7] j. rataj, l. sklenka. calculations and measurement at the training reactor vr-2. international atomic energy agency, publications 2007. [8] j. daeseong, p. jonghark, c. heetaek. development of thermal hydraulic and margin anlysis code for steady state forced and natural convective cooling of plate type fuel research reactor. progress in nuclear energy 71:39–51, 2014. 26 acta polytechnica ctu proceedings 4:22–26, 2016 1 introduction 2 thermal-hydraulic codes 2.1 relap5 2.2 trace 3 vr-1 reactor model 3.1 relap5 specification 3.2 trace specification 4 results 4.1 reactor power output 4.2 coolant velocity 4.3 coolant temperatures 5 conclusions references acta polytechnica ctu proceedings doi:10.14311/app.2017.11.0039 acta polytechnica ctu proceedings 11:39–42, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app its on railway martin leso czech technical university in prague, faculty of transportation sciences, praha, czech republic correspondence: leso@fd.cvut.cz abstract. development of technology management and security, transmission and information systems allows the concept of process management and security of railways and organizing the operation of a new, as yet non-phase in a non-traditional way. requirements for higher efficiency, accuracy and flexibility of the attractiveness of rail transport connection in the integrated transport systems are a challenge for the railways. these requirements can be solved just by changing the concept and technology of the presented here as an its-r. keywords: ertms/etcs, gsm-r, inteligent traffic systems on railway (its-r), traffic management systems (tms), railway control and command systems (ccs). 1. state of the art modern technologies are applied for control, command and signaling and in the area of information systems (for both control and passengers check-in) on the czech railway. electronic systems are installed (station electronic interlocking systems, crossing interlocking system and etc.) including remote control systems (central dispatching center). information systems allow to enter process and provide data to be able to control direct and on strategic level control and plan of railway transport. systems also provide information to passengers via panels and monitors. today’s approach is focused towards to install interlocking technologies on the infrastructure and the problems related to the movement of vehicles are missed out. vehicles are equipped by systems checking the driver’s watchfullness and by the lvz system transmiting signals to the driver’s cabine. but, the responsibility of reading signals and satisfy all rule remains on the driver himself. about 1500 km of the czech corridors is equipped by the system lvz. remaining parts of the infrastructure have no lzv and the driver is monitored only by periodical vigilance button pushing. this state of the art is analogical in easterneuropean countries (poland, slovakia, hungary). some vehicles (čd 471 series) are equipped by intelligent technology ato (automatic train operation), denoted avv in czech language, that makes possible to automate vehicle and driver’s work control. these systems lead to decrease operating costs but their wide application is not optimal now due to missing pieces of information from the infrastructure and absence of safety level of vehicle driving. despite the avv system developed in the czech republic reached excellent operating parameters on the world level. ertms implementation plan was ratified and published in 2014. this plan is a crucial document to define the ertms implementation strategy in the czech republic. the fundamental change (in comparison with existing plans) is a new strategy to equip vehicles by "etcs onboard part". on the continuous track sections equipped with etcs of hundreds of km length immediately after entry into service will be prohibited trains without functional compatible vehicle on-board etcs. it is planned to equip about 1000 vehicles by etcs onboard system up to 2020 and about 1500 vehicles up to 2024. it may be stated the most vehicles will be equipped by etcs. but ertms implementation plan is concerned only to ten-t track net, other track net is not supported yet. the czech rail net included core ten-t track with length of 1329 km (3670 km of rails), others tracks ten-t 1265 km (3022 km), other main tracks of the length 2430 km (3633 km kolejí) and 4409 km (5079 km kolejí) of regional tracks. european legislative tsi (technical specifications of interoperability) defines requests to adapt main and regional rails outside of ten-t including all vehicles and industrial vehicles to be interoperable, i.e. etcs compatible. the issue of dealing with these types of lines forming around 2 / 3 of railway network in czech republic, therefore remains a major challenge for the future. the ertms implementation plan prepare the implementation of its-r systems well. with regard to the locomotives complete on board etcs fulfilment, both national main line and regional lines shall be calculated to be vehicles to be equipped with ertms / etcs on-board units. the assumption of full ertms/etcs onboard fulfillment is the big opportunity for change scope and type of interlocking technologies installed on infrastructure. today’s "full" installation with railway interlocking systems (station, track and level crossing systems with signals, track circuits od axel counters and etc.) on this types of tracks aren’t full installed not yet. on focus mainly to the regional tracks, using of conventional interlocking systems is not economical justified. these types of track are therefore suitable for installation of ertms/etcs systems, mainly 39 http://dx.doi.org/10.14311/app.2017.11.0039 http://ojs.cvut.cz/ojs/index.php/app martin leso acta polytechnica ctu proceedings etcs – level 1, or etcs – ls mode. most forward-looking of all functions with regard to its systems may be etcs – l3 (currently validated as ertms / etcs regional). with these systems may also consider the use of new technologies gnss, which are not yet in place in the tsi, but there may be early implemented. on this types of tracks, on the corridors main tracks to, it is possible to minimalize investment and services costs by choosing the strategy and type of control of the railway system based on minimalizing of parts of infrastructure technologies with reduction of signals and vehicle detection systems. it is necessary to consider, having regard to its applicability of technologies, the use of radio communication between vehicle and infrastructure. they must also be addressed, in particular freight train integrity to enable the detection systems in infrastructure. in 2015 was also approved and published other strategic document of ministry of transportation of czech republic (md čr), the "action plan its", which also deals with the implementation of its to rail. action plan for ertms / etcs and its implementation in the czech republic and, in principle, only referred to the downstream transport technologies (remote control, automation driving, etc..). the overall system is the concept of its in rail. in another development, it is therefore advisable to ertms / etcs, gsm – r and its one unit, in order to implement appropriate design and integration of all systems to ensure the function of its – r. 2. european best practices western european countries, the issue of long-term facilities of vehicles already addressed since 1950 mainly due to the provision of safe movement of vehicles. for example, german railway has wholly used vehicle systems controlling train movements (lzb main lines, branch lines pzb). very high level of amenities vehicles ertms / etcs (level ls, level 2) currently have swiss railways. for example, german railways has a wholly owned equipment vehicles systems controlling train movements (main line system lzb, pzb byline). very high level equipment of vehicles ertms / etcs (level ls, step 2) currently has swiss railways. in europe and globally range, can be seen guideline facilities especially vehicle management systems for rail traffic on the principles of ertms / etcs. ertms / etcs is promoted by the european union as one of the subsystems to ensure the interoperability of the whole rail system in europe. ertms / etcs ensures compliance with the requirements of the its-r in particular parameters ensure the safety of vehicle movement. other parameters, such as reliability and operational efficiency, are more dependent on the conditions of application of the system in specific countries. a comprehensive approach to its technology is not yet defined, but it is limited to defining the figure 1. interlinkages partial rail subsystems in its-r. structure of the exchange of data on passenger and freight (taf, tap) – subsystem of telematics applications for freight and passenger transport. in the area of intelligent transport systems can be seen similar trends as in the czech republic, ie. centralizing operations management together with the strong support of information systems for traffic management, but at the european level is already increasingly applied in real operation automatic setting routes, including optimizing traffic management (ie. the swiss system rcs). apply new systems for the management and security of railway traffic. 3. system approach to railways the subject of deployment of the railway is an intelligent transport system whose architecture and elements are interconnected in order to optimize and increase the efficiency of the whole process (fig. 1). its overall concept must be focused on increasing the parameters of the rail system, particularly the safety, reliability, economic efficiency operation. assumption for the goals of its on the rail is availability of all vehicles as a main target in the system, which provides transport (goods and people). these include the installation of ertms / etcs system including automatic train control, wireless data transfer by train (gsm-r). these basic components enable implementation of the concept of intelligent vehicle concept, which ensures the function as safe motion control, as well as optimizing its movement. for proper operation of intelligent vehicles, it is necessary to equip the corresponding intelligent infrastructure that will provide adequate information, intelligent vehicles with the least economic and technical complexity. a necessary condition is also coverage of wireless twoway communication infrastructure, which can provide information not only for the management and operation, but it will also provide an information service for dispatching and public services to passengers. target status should lead to the integration and overall optimal solutions to the infrastructure, and 40 vol. 11/2017 its on railway figure 2. conceptual vision of its-r. especially on vehicles with the aim of using all the components for securing the services of its-r. to ensure sufficient functionality and quality of services must be technology-r its implemented using modern telecommunications and emerging technologies. as a basis for solving the safety features of the system (of trains) must be the movement of all vehicles within the control signaling system ertms / etcs (fig. 2. part draw black). these systems need infrastructure equipment gsm-r system. according to the chosen level of ertms / etcs infrastructure must be equipped with the appropriate infrastructure components. for etcs-l1 (ls) and etcs-l2 infrastructure must be fully equipped with conventional technology infrastructure. etcs level-l3 enables significant savings on the side of infrastructure facilities, conventional systems management and security are not necessary and are fully replaced by technology on the vehicle condition to ensure the integrity (integrity) of the train. to increase efficiency and optimize operations management, increase infrastructure capacity, reduce operating costs (fuel consumption and energy use, vehicle wear and infrastructure) is required all vehicles equipped with automatic train control system. this subsystem most of the information for their activities (information on the line, the vehicle allowed to travel etc ..) can be obtained through a signaling system ertms / etcs. to ensure greater attractiveness of traveling using modern information and check-in systems and logistics services for parent carriers and their customers is also needed to ensure coverage of railway infrastructure, high-speed data services (eg. the technology 4g / 5g; fig. 2. showing green and red). high speed data connectivity is to be ensured in all vehicles, i.e. not only driving the vehicle but also to all connection (in the case of complete sets embedded) vehicles. 4. advantages of the benefits of its deployment at railway the introduction of intelligent transport systems on the railways should provide ways to increase the efficiency of the entire transport system in the czech republic: (1.) state managers of transport infrastructures: (a) increasing the capacity of transport infrastructure (b) increasing transport reliability, minimize delays (c) reducing wear of the transport infrastructure (d) efficient rail transport with possibility of creation the integration transport systems with using railways as the transport backbone (e) optimization of investment in transport infrastructure (f) increasing the level of safety throughout the rail network (thanks to the strategy is to increase the safety of the entire network, after which the vehicle is moving under conditions appropriate infrastructure facilities) (2.) railway carrier and passangers: (a) a. reduction of vehicle operation costs (energy, operating costs) (b) reducing of traffic accidents (c) increasing the attractiveness of rail transport for passengers (d) increasing the attractiveness of rail transport for freight transporters (e) increasing the attractiveness of rail transport for carriers (passenger and freight) (f) increased profits from transport (3.) railway industry: (a) an opportunity for the development and implementation of new products and services (b) exports of modern technology with the potential to assert themselves on foreign markets 5. final conclusion this paper describes the concept of new technology for the management and security of railway traffic solutions enable intelligent transportation systems. at present day, all the key technologies are developed yet. if we want to fulfill the above-mentioned strategic action is needed as soon as possible to start with a pilot project of the its-r. the pilot project should be implemented at the appropriate regional railway track, which will be verified and mastering functionality of the various sub-components and the whole concept of traffic management. the subject of verification should be technology ertms / etcs l3 system including automatic train control, information and communication systems to ensure transmission 41 martin leso acta polytechnica ctu proceedings of data necessary for the management and operation, logistic processes and services for passengers. after this necessary phase of technology adoption may be considered for their further expansion into the real network traffic lanes regional and national railways. the main benefit of technology its-r is not only to increase safety on the regional railways, but also increase the flexibility and the possibility of significant automation and optimization of traffic on main line of railways. consequences should be in greater competitiveness and attractiveness of rail transport. 42 118 acta polytechnica ctu proceedings 1(1): 118–122, 2014 118 doi: 10.14311/app.2014.01.0118 v2282 sgr revisited roberto nesci1, corinne rossi2, antonio frasca3, ettore marilli3, paolo persi1, nicola cornero4 1inaf-iasf, via fosso del cavaliere 100, 00133 roma, italy 2university la sapienza, p.le a. moro 2, 00186 roma, italy 3inaf/oact, catania, italy 4cdso, aosta, italy corresponding author: roberto.nesci@iaps.inaf.it abstract the nature of v2282 sgr is examined on the basis of several multiband observations: a 20 years long i-band light curve of v2282 sgr obtained from archive photographic plates of the asiago and catania observatories; a ccd r-band light curve obtained at cornero observatory; jhk photometry from 2mass and ukdiss; spitzer irac and mips images; optical spectra from loiano observatory; x-ray flux from chandra. the star has a k-type spectrum with strong emission lines and is irregularly variable at all wavebands. the overall evidences suggest that v2282 sgr is a pre main sequence star with an accretion disk. keywords: variable stars pre-main-sequence stellar evolution. 1 introduction the m20 (trifid) nebula is a spectacular star forming region of the milky way: it is projected in the sky over the open star cluster ngc 6514, and its distance has been estimated by several authors, ranging from 1.4 kpc [6] up to 2.7 kpc [1]. the variable v2282 sgr was mainly studied by [5] who reported an amplitude of about 0.5 mag in the i band and classified it as a possible orion type variable. the star is positionally consistent with the soft x-ray source cxom20 180216.8-230347 detected by chandra in m20 [9]; it appeared not to be variable in x-rays, with a flux level of 0.167 c/s, and therefore was not further discussed in that paper. it is also consistent with a spitzer infrared source of the mid-infrared survey of the m20 by [10], classified as a proto-stellar source (class i/0 n.16) without comments about a possible optical counterpart. a nebular variable (either of the t tau, rw aur or t ori type) is believed to be a pre main sequence (pms) star already partially clear of its originating circumstellar envelope [2]: this seems at odds with classification as a class i/0 object, which is a still deeply embedded source. for this reason we decided to explore in more detail its nature. 2 photographic light curve we measured the magnitude of v2282 sgr on 25 plates with i-n emulsion and rg650 filter taken with the 65/90/235 schmidt telescope of the asiago observatory, and on 109 (i-n + rg650) plates of the 40/40/120 schmidt of the catania observatory. plates were digitized with an epson 1680 pro scanner in transparency mode at 1600 dpi. a sequence of comparison stars was defined selected from the gsc2.3.2 catalog, using the n band magnitudes (see fig. 1 and table 1). aperture photometry was made with iraf/apphot. the photometric accuracy of our magnitudes ranges from 0.08 mag at i = 13 to 0.18 mag at i = 14.5: fainter stars have larger dispersion, as expected. the rms deviation of the values of n magnitude for v2282 sgr was 0.25 mag in the asiago and 0.34 mag in the catania datasets, substantially larger than the faintest comparison star. the resulting overall light curve of the asiago and catania observations is shown in fig. 2. v2282 sgr shows substantial variations up to 1 magnitude, with an average level n = 14.0. 118 http://dx.doi.org/10.14311/app.2014.01.0118 v2282 sgr revisited figure 1: finding chart of v2282 sgr from a poss ii plate with iv-n emulsion. the variable is marked with l. comparison stars are labelled. the field is 12 arcmin wide in dec, north is up and east to the left. 0 2000 4000 6000 8000 10000 15.0 14.5 14.0 13.5 13.0 12.5 jd-2,440,000 v2282 sgr asiago-catania figure 2: light curve in the i photographic band of v2282 sgr from the asiago (open squares) and catania (filled squares) archives. due to its southern sky position the coverage shows a marked seasonal bias. 119 roberto nesci et al. 3 ccd observations ccd images of m20 were taken at the cornero observatory1 with a 30cm f/6.5 schmidt-cassegrain telescope and an rc filter in 19 different nights, from june to october 2009. the star showed an oscillating behaviour, with an amplitude of about one magnitude (see fig. 3.) the time interval between a minimum and a maximum may be as short as 10 days, so that the loose time sampling of historic plates may underestimate the actual variability range. furthermore, we obtained with the bfosc instrument at the loiano 1.52 m telescope a b, v and r photometric point on 2011 and an r one in 2012. the star was at b = 17.60, v = 16.31, r = 14.70 on 2011 and r = 14.40 on 2012; both r values are within the variability range of the light curve of 2009. 4 optical spectroscopy with the bfosc instrument we also secured two spectra of the star (on 2011-08-02 and 2012-07-18) at 4 å/pixel dispersion (resolution ∼12 å). the spectra were reduced using the iraf reduction package, following the standard procedures. due to the large airmass no reliable flux calibration could be obtained. the one dimensional spectrum of v2282 sgr shows a number of emission lines which are most probably formed in a region physically close to the star. the two spectra taken at a distance of one year from each other look rather similar. the only remarkable difference is that the [n ii] 6584å line is not apparent in july 2012. figure 3: the light curve of v22822 sgr from ccd images of the cornero observatory. crosses are a comparison star, filled squares are the variable. table 1: adopted comparison stars sequence ra dec id n b v f 270.591 -23.040 a 12.69 13.99 13.37 270.560 -23.068 b 13.52 15.47 14.73 270.522 -23.091 c 12.26 13.15 12.96 12.66 270.503 -23.103 d 13.02 13.72 270.497 -23.096 e 13.49 13.82 270.503 -23.070 f 13.29 14.81 14.44 13.57 270.494 -23.061 g 13.27 13.93 270.486 -23.001 h 12.63 13.15 12.96 12.82 270.633 -23.059 m 12.49 14.40 13.73 270.647 -23.114 n 12.82 13.37 270.637 -23.108 o 12.22 12.44 12.29 12.36 270.612 -23.095 p 12.52 13.71 13.15 12.87 270.692 -22.955 q 13.11 270.696 -22.980 r 13.68 15.36 14.55 270.703 -22.992 s 14.13 270.716 -22.993 t 14.21 14.38 270.685 -23.025 u 14.40 14.52 270.722 -23.067 v 13.89 15.35 14.53 270.689 -23.086 x 13.80 270.685 -23.095 y 12.85 14.42 13.72 13.24 270.696 -23.108 z 13.82 15.40 14.71 table 2: emission lines in v2282 sgr wavelength ion ew (å) 6584 [n ii] -5 6563 hα -20 6548 [n ii] -0.6:: 5007 [o iii] -10 4959 [o iii] -5 4861 hβ -16 4363 [o ii] -6:: 4340 hγ -15 the emission lines in the stellar spectrum are listed in table 2, together with their equivalent width (ew ). we remark that doing the sky subtraction from the raw spectrum of the star all the night-sky emission lines disappeared, while the [o iii] and balmer emission lines remained, so we are strongly convinced that they are real. 1http://www.cdso.it 120 v2282 sgr revisited among the absorption lines, the most prominent are the nai d doublet (6.5 å), the mgi b triplet (3.3 å), the blends of several atomic lines centered at 5269 and 6497 å, the cai 4227 å and the g band, indicating an intermediate g-k spectral type. the nai d doublet is very strong, compared to the typical value (2.5 å) of the main sequence or giants g-k stars, suggesting the presence of substantial interstellar/circumstellar matter, as expected in a pms star. figure 4: sed of v2282 sgr from photometric de-reddened (av = 1.3 mag) data. the best-fitting nextgen synthetic spectrum with t=4200 k and log g = 3.5, is over-plotted with a continuous line. to gain information about the stellar photosphere, we fitted the observed sed with low-resolution synthetic spectra calculated from the nextgen model atmospheres [3]. we fixed the star distance and extinction to the values d = 1.7 kpc and av = 1.3 mag reported by [4] and we let teff and log g free to vary, adopting a standard extinction law av = 3.1e(b − v ). this interstellar absorption is consistent with the typical value of av = 0.8 mag/kpc and a distance of 1.7 kpc. the fit was limited to the photometric bands from b to j , because afterwards the photospheric flux could be significantly contaminated by an ir excess. the result of the sed fit is shown in fig. 4 where the optical and near-ir fluxes have been corrected for the extinction and the error bars include the average variation of ± 0.5 mag observed both in r and i bands. the best-fit model is that with log g = 3.5 and teff = 4200 k. with these parameters, a radius of about 4.8rsun would be derived for the star at the adopted distance. the observed flux appears to be dominated by the stellar photosphere up to the k band, while an ir excess, likely related to a circumstellar disk, is quite evident longward of 3µm. to quantify how much the derived temperature is sensitive to the adopted av we performed several tests: two extreme cases are reported below. adopting av =0.5 gives teff = 3800 k, log g = 2.5 and a radius 5.1 rsun: such a low temperature is not compatible with the observed spectrum, which shows no molecular bands. adopting a substantially higher value (av =3.0) gives teff = 5600 k, log g = 3.5 and a radius 4.3 rsun: this is still compatible with the observed spectral features but produces somewhat larger residuals than the av = 1.3 case. the derived stellar temperature is clearly an increasing function of the assumed absorption. we remark that the actual absorption is the sum of the interstellar absorption, the circumstellar absorption and the possible contribution from the m20 nebula whose outskirts include the star. a measure of the actual absorption is not easy because the star spectrum is peculiar: in particular the ew of the mgi triplet is low for a g5 star (5600 k), and even more so for a k0 (4400 k) one: it would be typical of a main sequence f5 star, which is too hot for the observed spectral features. this suggests that a strong 121 roberto nesci et al. veiling is present in the spectrum, as indicated also by the presence of strong balmer emission lines. therefore we cannot reliably derive the amount of absorption by comparing the intrinsic b-v with the observed one. the ew of the nai d doublet is 6.5 å, so it is well in the saturated part of the relation between e.w. and e(b-v) by [8] and cannot give an accurate estimate of the color excess, save indicating that it must be substantially larger than the simple interstellar one. 5 infrared observations to better understand the nature of v2282 sgr we considered the j , h and k magnitudes taken at different epochs from 2mass, denis, ukidss catalogues and from [10] (see table 3). from this table it appears evident the near ir variability of the star. table 3: near infrared photometry date j h k note 1998/06/14 12.74 12.02 11.54 2mass 1996/04/01 12.90 ... 11.51 denis 2004/08/23 12.99 12.26 11.93 200inch 2006/07/23 15.71 14.21 12.78 ukidss spitzer/irac images between 3.6 and 8 µm were taken in three different epochs. we performed the photometry of the star using iraf/apphot with the same aperture size of [10]. the star was significantly variable, mainly at shorter wavelengths, enforcing the evidence of its pms nature. a bolometric luminosity, with an uncertainty of about one magnitude, may be computed from the infrared spitzer, jhk, and our optical data. we derived a value of 4.1 lsun in the range from b to k and 24.3 lsun in the range from b up to 24 µm, quite reasonable values for a pms star. 6 conclusions v2282 sgr can be classified as a probable class i premain sequence star associated with an accreting circumstellar disk. its observed optical spectrum is consistent with a late g type star. its long-term irregular optical variability, typical of accreting t tauri stars, can be due to a combination of stellar rotation and circumstellar dust occultation, while the observed transient near-ir excess arises from a combination of variable extinction and changes in the inner accretion disk. its x-ray luminosity (7.6 × 1032erg cm−2 s−1) is compatible with the value for pms with mass ∼ 2 msun [7]. one may wonder if v2282 sgr is actually a foreground object unrelated to the trifid nebula: we think that the strong high-excitation [o iii] and n[ii] lines in its spectrum prove the presence of hot gas in front of the star, which cannot be heated by the low temperature of the stellar photosphere and is therefore related to the m20 nebula. acknowledgement r. nesci thanks the direction of the asiago observatory for hospitality during the scanning of the archive plates. references [1] cambresy, l., rho, j., marshall, d.j., reach, w.t., 2011 a&a 527, 141 [2] glasby j.s., the nebular variables, pergamon press, 1974 [3] hauschildt, p. h., allard, f., ferguson, j., baron, e., & alexander, d. r. 1999, apj, 525, 871 doi:10.1086/307954 [4] lynds, b. t., canzian, b. j., & o’neil, e. j., jr. 1985, apj 288, 164 doi:10.1086/162775 [5] maffei, p., 1963, memsait 34, 441 [8] munari, u., zwitter, t., 1997, a&a 318, 269 [6] ogura, k., & ishida, k. pasj 1975, 27, 119 [7] preibisch t. 2007, memsait 78, 1 [9] rho, j., ramirez, s.v., corcoran, m.f., hamaguchi, k., lefloch, b., 2004, apj 607, 904 doi:10.1086/383081 [10] rho, j., reach, w.t, lefloch, b., fazio, g.g, 2006, apj 643, 965 doi:10.1086/503245 122 http://dx.doi.org/10.1086/307954 http://dx.doi.org/10.1086/162775 http://dx.doi.org/10.1086/383081 http://dx.doi.org/10.1086/503245 introduction photographic light curve ccd observations optical spectroscopy infrared observations conclusions 41 acta polytechnica ctu proceedings 2(1): 41–45, 2015 41 doi: 10.14311/app.2015.02.0041 cvs around the minimum orbital period s. zharikov1, g. tovmassian1 1observatorio astronomico nacional, instituto de astronomia, universidad nacional autonoma de mexico, ensenada, bc, mexico, 22860 corresponding author: zhar@astrosen.unam.mx abstract we discussed features of cataclysmic variables at the period minimum. in general, most of them must be wz sge-type objects. main characteristics of the prototype star (wz sge) are discussed. a part of wz sge-type objects has evolved past the period limit and formed the bounce back systems. we also explore conditions and structure of accretion disks in such systems. we show that the accretion disk in a system with extreme mass ratio grows in size reaching a 2:1 resonance radius and are relatively cool. they also become largely optically thin in the continuum, contributing to the total flux less than the stellar components of the system. in contrast, the viscosity and the temperature in spiral arms formed at the outer edge of the disk are higher and their contribution in continuum plays an increasingly important role. we model such disks and generate light curves which successfully simulate the observed double-humped light curves in the quiescence. keywords: cataclysmic variables dwarf novae period minimum. 1 introduction a widely accepted evolutionary theory of cataclysmic variables (cvs), as presented in kolb & baraffe (1999, and references therein), predicts a significant accumulation of cv systems around the orbital period minimum (paczynski 1981). it also envisions that ∼70% of the current cv’s population has evolved past the orbital period minimum and formed so-called bounce-back systems. figure 1 illustrates the current concept of cv evolution at the orbital period turn-around point on the mass-transfer rate and mass-ratio to orbital period diagrams. cataclysmic variables with orbital periods close to the 80 min orbital period minimum that undergo infrequent (years to decades) super-outbursts are called wz sge-type stars. objects with short periods that have not been observed in outburst or super-outburst but have spectral characteristics similar to wz sge are listed also as wz sge-type candidates. those systems are dominated at the period minimum. the bounce-back systems are cataclysmic variables evolved beyond the minimum period limit, which is reached when the secondary star becomes of a substellar mass (brown dwarf) and partially degenerate. bounce-back systems are expected to float within the 80 100 min orbital period range. bounceback systems are spectroscopically similar to these, but not every wz sge-type object has necessarily passed through the turning point. figure 1 also displays the expected position of the bounce-back systems. in this paper we discuss observational characteristics of cataclysmic variables at the period minimum and explore conditions and structure of its accretion disk. figure 1: schematic distribution of cv-types on the plot of the mass ratio and mass transfer rate vs. the orbital period. 2 wz sge-type stars wz sge is the prototype star of the class of short-period cataclysmic variables (named wz sge-type stars). it is a high inclination (∼77o; steeghs et al. 2007) cataclysmic variable with a late m-type dwarf secondary star (0.078m� < m2 < 0.13m�) orbiting at 81.6 min the fastest-spinning (∼ 28 sec, robinson et al 1978) 41 http://dx.doi.org/10.14311/app.2015.02.0041 s. zharikov, g. tovmassian white dwarf (0.88m� < m1 < 1.53m�). the distance to wz sge is only 43.5 pc. for most of its life it is in quiescence with a v ∼ 15, corresponding to mv ∼ 12. below the main characteristics of wz sge are summarised: • a short orbital period of 81.6 min, close to the predicted period minimum of cvs ∼ 77min with a main sequence secondary. • a spectrum in quiescence shows strong double-peaked balmer emission lines from the accretion disk surrounded by broad absorptions, formed by the primary white dwarf (see for an example howell et al. (2008)). • an infrequent ∼20-30yr and largeamplitude (∼ 8mag; 1913, 1946, 1978, 2001 yy.) super-outbursts succeeded by echo outbursts, absence of normal (as in su umatype stars) outbursts. in order to avoid an earlier occurrence of normal outburst in wz sge-type systems, it can be accepted as an extreme low viscosity parameter a ∼0.010.001 in accretion disks (smak (1993), osaki (1994)). • the light curve during a super-outburst shows long-lasting super-humps (patterson, et al. 2002). • the optical light curve are double-humped sometimes during super-outburst and in quiescence (patterson, et al. 1998; patterson, et al. 2002). • there is evidence of forming spiral arms in the disk during super-outburst (baba et al. 2002, howell et al. 2003). • in quiescence the accretion disk is asymmetric, and the bright spot region is shown to be extended along the mass transfer stream (skidmore et al. 2000, mason et al. 2000). • the outer layers of the accretion disk must be of low density and low temperature ∼3000k (howell et al. 2004). • a cavity most likely formed in the inner part of the disk during quiescence implying an annulus-shaped accretion disk (kuulkers et al. 2011). • the outer radius of the disk is about a 3:1 resonance radius (rdisk ≤ r3:1) in quiescence and it can reach to 2:1 resonance radius (rdisk ≤ r2:1) during a super-outburst. there are about ∼100 objects proposed or confirmed as wz sge-type systems. most of them were suggested based on features of spectra or the amplitude of the super-outbursts. figure 2 summarise current conception about wz sge-type systems which do not yet pass the period minimum. figure 2: the current conception about wz sgetype systems which do not yet pass yet the period minimum. 3 bounce-back systems after reaching the period minimum the cvs should evolve back toward longer periods and form a so-called bounce-back or post-period minimum systems. the increasing of orbital periods of bounce-back systems is accompanied by a decline in mass transfer rate about an order of magnitude according to the existing models of cvs evolution (kolb & barrafe 1999, sirotkin & kim 2010). the list of the bounce back candidates are given in table 2 and figure 3 (zharikov et al. 2013). the optical spectra in quiescence of proposed candidates are similar to wz sge. all those systems include a massive and relatively cool (∼ 12000k) white dwarf primary and a m2/m1 mass ratio less than 0.075. such low mass ratio implies a jupitersize secondary (a late type m-dwarf or a brown dwarf) and with a 2:1 resonance radius is within of the roche lobe of the primary. also, similar to wz sge, the bounce back candidates do not show normal outbursts which implies an extremely low α ∼ 0.01 − 0.001 viscosity parameter (smak (1993), osaki (1994)). this together with the low ∼ 10−11m�/year mass transfer rate, allows the accretion disk to expand in bounce back systems up to a 2:1 resonance radius and form a two spiral wave structure in those systems (lin & papaloizou, 1979). the large size of the disk and domination of white dwarf radiation in the optical range and the secondarys radiation in the jhk bands in sdss0804 and sdss1238 bounce back candidates (zharikov et al 2013, aviles et al 2010) lead to the conclusion that the ”standard accretion disk model” (frank et al. 2002) does not apply to bounce-back systems. 42 cvs around the minimum orbital period table 1: parameters of wz sge and of bounce-back candidates. nn/object porb v q m1 m2 twd eff i lc1 (days) (mag) (m�) (m�) (k) (o) wz sge 0.0567 ∼ 15 0.092 0.85 0.078 13500 77 +sq 1. gw lib∗ 0.0533 19.1 0.060 0.84 0.05 11 2. v455 and∗ 0.0563 16.5 0.060s >m9 11500 83 +q 3. al com∗ 0.0567 19.1 0.060 16300 +q 4. sdss1035 0.057 18.7 0.055e 0.94 0.05 10100 83 5. sdss1238 0.056 17.8 0.05 ∼ 1.0 0.05 12000 ∼70 +q 6. sdss0804∗ 0.059 17.8 0.05s ∼ 0.9 0.045 13000 ∼ 70 +q 7. eg cnc∗ 0.060 18.8 0.035s 12300 +s 8. rx1050-14 0.062 17.6 <0.055v 13000 <65 9. gd552 0.0713 16.6 <0.052v <0.08 10900 <60 10. re1255 0.083 19.0 <0.064v >0.9 <0.08 12000 < 5 1 light curve (lc) features: ”+” lc shows a double-hump during the orbital period; ”s” during super-outburst; ”q” during quiescence; ”-” absent of double-humps in lc. ∗ objects which demonstrated wz sge-type superoutburst. figure 3: the systems with known mass ratio vs. orbital period are plotted. the left axes is the mass ratio and estimated mass transfer rates are given on the right axes. the bounce-back candidates are enclosed in a dash-dotted box. cannizzo & wheeler (1984) studied the vertical structure of a steady-state, α-model thin-accretion disk for an accreting object of 1 m�. they found that, for low accretion rates, the disk structure is optically thin and can be doublevalued with high(∼5000 k) and low(∼2000 k) temperature branches. for α > 0.1 a warm solution is possible in the inner region of the accretion disk, but disk annuli at larger radii will be in a cold state with t < 2000 k. only the low-temperature solution exists for α ≈ 0.1. as α decreases with temperature, the tendency to develop cold solutions in quiescence is enhanced. therefore, accretion disks in bounce back systems are most probably cool (∼2500 k). the optical light curve of the high inclination bounce back candidates shows permanently a doublehumped light curve (marked by ”+q” in table 2). the spiral arm structures were found from doppler tomography mapping in quiescence in two well studied example of bounce back candidates sdss1238 (aviles et al. 2010) and sdss0804 (zharikov et al. 2013). also important, that, because the mass transfer rate significantly decrease after the period minimum the size of the magnetosphere of the primary with faint magnetic field will increase with the decreasing of ṁ and a relatively faint (≤ 1mgauss) magnetic field is enough to form a cavity in the inner part of the accretion disk (zharikov et al 2013). taking into account all these features a geometrical model of bounce back system was constructed to explain the observed double-humped light curve in quiescence. the model takes into account the positions of the bright structures in the doppler maps, the large size of the accretion disk, and the description of the spiral density waves in hachisu et al. (2004). figure 4 presents the geometry used in the model (central panel) and grayscale images present the height of the disk (left) and the temperature distribution (right) of the accretion disk. 43 s. zharikov, g. tovmassian figure 4: from left to right: vertical thickness of the accretion disk, model configuration used to calculate the light curves of bounce-back systems and the temperature distribution of the model. figure 5: left: examples of double-humped light curve; right: examples of the light curve generated by the model. we calculated a variety of models using the typical average parameters of bounce-back systems presented in table 1 and the double-hump-shape light curve (fig. 5, (left panels) is easily reproduced by such models, two examples of which are shown in fig. 5, (right panels). 4 conclusions the galactic age is high enough that ∼ 70% of cvs will have reached the cvs orbital period minimum. in general, most of them must be wz sge-type objects. a part of wz sge-type objects have already passed the period limit and formed the bounce back systems. the structure of the disk must be changed when the system pass through the minimum. before the minimum, mass transfer rate is higher and the accretion disk is hotter and smaller. after the period limit it is larger and reaches a 2:1 resonance radius. the disk is cool (∼ 2500k) and has a cavity in the inner part and presents permanently existing spiral arms. the spirals should be denser and hotter that the rest of the disk. based on these features we propose the double-humped light curve in quiescence state of a system together with orbital period longer than the period limits and the mass ratio of q < 0.08 as the main manifestation of a wz-sge system which already passed through the minimum orbital period. when accretion has ended the cvs can form very close short period wd+bd systems, two examples of which are found recently (wd0137-349, burleigh et al. (2006) and nltt5306, steele et al. (2013)). acknowledgement we acknowledge papiit grants in-109209/in-103912 and conacyt grants 34521-e; 151858. references [1] aviles, a., et al. 2010, apj, 711, 389 [2] baba, h. et al. 2002, pasj, 54, l7 44 cvs around the minimum orbital period [3] burleigh, m. r., et al. 2006, mnras, 373, l55 doi:10.1111/j.1745-3933.2006.00242.x [4] cannizzo, j. k., & wheeler, j. c. 1984, apjs, 55, 367 [5] frank, j., et al. 2002, accretion power in astrophysics, cambridge university press doi:10.1017/cbo9781139164245 [6] hachisu, i. et al. 2004, apjl, 606, l139 doi:10.1086/421295 [7] howell, s. b., et al. 2003, a&a, 399, 219 [8] howell, s. b., et al. 2004, apjl, 602, l49 doi:10.1086/382481 [9] howell, s. b., et al. 2008, apj, 685, 418 doi:10.1086/590491 [10] kolb, u., & baraffe, i. 1999, mnras, 309, 1034 [11] kuulkers, e., et al. 2011, a&a, 528, a152 [12] lin, d. & papaloizou, j., 1979, mnras, 186, 799 doi:10.1093/mnras/186.4.799 [13] osaki, y. 1995, pasj, 47, 47 [14] mason, e., et al. 2000, mnras, 318, 440 [15] paczynski, b. 1981, acta astron., 31, 1 [16] patterson, j., et al 1998, pasp, 110, 403 [17] patterson, j., et al. 2002, pasp, 114, 721 [18] robinson, e. l., et al. 1978, apj, 219, 168 [19] sirotkin, f. & kim, w. 2010, apj, 721, 1356 doi:10.1088/0004-637x/721/2/1356 [20] skidmore, w., et al. 2000, mnras, 318, 429 [21] smak, j. 1993, acta astronomica, 43, 101 [22] steeghs, d., et al. 2007, apj, 667, 442 doi:10.1086/520702 [23] steele, p. r., et al. 2013, mnras, 429, 3492 doi:10.1093/mnras/sts620 [24] zharikov, s., et al. 2013, a&a, 549, a77 discussion raimondo baptista: the opening angle of the spiral structure in an accretion disk depends on the ratio of the local sound speed to a keplerian speed. the disk region containing the spirals must be quite hot in order for the spiral will be wide open as in your model. is it physically consistent to get wide spiral in the disk with such low temperature such as ∼ 2000 k. sergey zharikov: our model is a geometrical model only. based on proposed geometrical shape and size of the disk in bounce back systems we can explain observed double-humped light curves in quiescence. formation such spiral arm structure and physical conditions in such cool disk is not clear yet. the first approach to describe such disks was presented in paper of cannizzo, & wheeler, (1984). 45 http://dx.doi.org/10.1111/j.1745-3933.2006.00242.x http://dx.doi.org/10.1017/cbo9781139164245 http://dx.doi.org/10.1086/421295 http://dx.doi.org/10.1086/382481 http://dx.doi.org/10.1086/590491 http://dx.doi.org/10.1093/mnras/186.4.799 http://dx.doi.org/10.1088/0004-637x/721/2/1356 http://dx.doi.org/10.1086/520702 http://dx.doi.org/10.1093/mnras/sts620 introduction wz sge-type stars bounce-back systems conclusions 288 acta polytechnica ctu proceedings 1(1): 288–292, 2014 288 doi: 10.14311/app.2014.01.0288 soft x-ray polarimeter: potential instrumentation and observations herman l. marshall1, norbert s. schulz1 1mit kavli institute, cambridge, ma, usa corresponding author: hermanm@space.mit.edu abstract we present an instrument design capable of measuring linear x-ray polarization over a broad-band using conventional spectroscopic optics. a set of multilayer-coated flats reflects the dispersed x-rays to the instrument detectors. the intensity variation with position angle is measured to determine three stokes parameters: i, q, and u – all as a function of energy. by laterally grading the multilayer optics and matching the dispersion of the gratings, one may take advantage of high multilayer reflectivities and achieve modulation factors >90% over the entire 0.2 to 0.8 kev band. this instrument could be used in a small suborbital mission or adapted for use in an orbiting satellite to complement measurements at high energies. we present progress on laboratory work to demonstrate the capabilities of key components. keywords: polarimetry x-rays. 1 introduction polarimetry is an inherently multiwavelength phenomenon. in the radio band, the detectors provide linear polarization information but for other bandpasses, special steps are required, so an observer has to choose whether to obtain the additional stokes parameters. polarization studies in the optical and radio bands have been very successful. radio polarization observations of pulsars provided “probably the most important observational inspiration for the polar-cap emission model” (taylor & stinebring1986) developed by radhakrishnan (1969), critical to modeling pulsars and still widely accepted (taylor & stinebring). tinbergen (1996) gives many examples in optical astronomy such as: revealing the geometry and dynamics of stellar winds, jets, and disks; determining binary orbit inclinations to measure stellar masses; discovering strong magnetic fields in white dwarfs and measuring the fields of normal stars; and constraining the composition and structure of interstellar grains. perhaps the most important contribution of optical polarimetry led antonucci & miller (1985) to develop the seminal “unified model” of seyfert galaxies, a subset of active galactic nuclei (agn). their paper has been cited in over 1000 papers in 30 years, over 5% of all papers ever written about agn. thus, the extra information from polarimetric observations has provided a fundamental contribution to the understanding of agn. although tens of thousands of x-ray sources are known from the rosat all-sky survey, polarization studies were carried out only in the 1970s and were limited to the brightest sources. in over 40 years, the polarization of only one source has been measured to better than 3σ: the crab nebula (novick et al. 1972; weisskopf et al. 1987). even for bright galactic sources, the polarizations were undetectable or were marginal 2 − 3σ results (silver, et al. 1979; long et al. 1980). furthermore, over the entire history of x-ray astronomy, there has never been a mission or instrument flown that was designed to measure the polarization of soft xrays. because of the lack of observations, there has been very little theoretical work to predict polarization fractions or position angles but there has been some recent progress in support of the now-cancelled mission, gems (the gravitation and extreme magnetism smex; see swank et al. 2010). the x-ray extreme universe satellite (xeus) and the international x-ray observatory (ixo) both had been planned to include a polarimeter but their probable successor, athena+, does not, so there is now no mission that is planned to include a polarimeter. here we describe a few potential scientific studies to be performed with an x-ray polarimetry mission with sensitivity in the 0.1-1.0 kev band that would complement observations with an instrument such as gems. 2 the scientific value of soft x-ray polarimetry there is significant scientific potential of an x-ray polarimeter operating below 1 kev. here, we discuss a few types of potential targets; for details see marshall et al. (2010), schnittman et al. (2013), ghosh et al. (2013). 288 http://dx.doi.org/10.14311/app.2014.01.0288 soft x-ray polarimeter: potential instrumentation and observations figure 1: a prediction of the variation of the polarization percentage (left) and its position angle (right) as a function of energy for agn with varying spin, a/m , and eddington ratio, l/ledd (schnittman & krolik, 2009). such studies were initiated with the prospect of obtaining polarization data in the 2-8 kev band using gems. the figures show that predictions depend strongly on energy. observations with a multilayer-based polarimeter would complement those by an instrument such as gems. 2.1 active galactic nuclei blazars are believed to contain parsec-scale jets with β ≡ v/c approaching 0.995. the x-ray spectra are much steeper than the optical spectra, indicating that the x-rays are produced by the highest energy electrons, accelerated closest to the base of the jet or to shock regions in the jet. brindle (1986) showed that the polarization of blazars increases from the ir to the optical band and can be as high as 25%, indicating that the x-ray polarization should be greater than 30%. the jet and shock models make different predictions regarding the directionality of the magnetic field at x-ray energies: for knots in a laminar jet flow it should lie nearly parallel to the jet axis (marscher 1980), while for shocks it should lie perpendicular (marscher 1985). see also poutanen (1994). mcnamara et al. (2009) recently suggested that x-ray polarization data could be used to deduce the primary emission mechanism at the base, discriminating between synchrotron, self-compton (ssc), and external compton models. their ssc models predict polarizations between 20% and 80%, depending on the uniformity of seed photons and the inclination angle. their spectra are very soft, brightest below 1 kev. theoretical work indicates that agn accretion disks and jets should be 10-20% polarized (mcnamara et al. 2009; schnittmann & krolik 2009, dovčiak, et al. 2011) and that the polarization angle and magnitude should change with energy in a way that depends on the system inclination. schnittmann & krolik (2009) particularly show that the variation of polarization with energy could be used as a probe of the black hole spin and that the polarization position angle would rotate through 90 deg between 1 and 2 kev in some cases, arguing that x-ray polarization measurements are needed both below and above 2 kev (fig. 1). 2.2 isolated neutron stars isolated neutron stars (pavlov & zavlin 1997) and magnetars (heyl, shaviv, & lloyd 2003, lai; & ho 2003) should be bright enough for soft x-ray polarimeters. with temperatures below 0.5 kev, they can only be detected below 1-2 kev. magnetars are thought to be powered by the decay of enormous magnetic fields (1014– 1015 g). these fields are well above the quantum critical magnetic field, where a particle’s cyclotron energy equals its rest mass; i.e. b = m2c3/eh̄ (=4.4×1013 g for electrons). measuring the polarization of the radiation from magnetars in the x-ray band will not only verify the strength of their magnetic fields, but also can provide an estimate of their radii and distances and provide the first demonstration of vacuum birefringence, a predicted but hitherto unobserved qed effect (heyl, shaviv, & lloyd 2003) . the extent of polarization increases with the strength of magnetic field and decreases as the radius increases so compact neutron stars are predicted to be highly polarized, > 80% (heyl et al. 2003) . detailed models of less strongly magnetized neutron star atmospheres show that the polarization fraction would be 10-20% at 0.25 kev averaged over the visible surface of the star (pavlov & zavlin 2000). we can constrain not only the orientation of axes, but also the 289 herman l. marshall, norbert s. schulz m/r ratio for the thermally emitting neutron stars due to gravitational light bending. constraining m/r, impossible from the radio polarization data, is extremely important for elucidating the still poorly known equation of state of the superdense matter in the neutron star interiors. we note that these isolated neutron stars do not produce significant flux above 2 kev, so polarimeters with significant effective area in the 0.1 to 1.0 kev band will be needed to test polarization predictions from neutron star atmospheres. figure 2: bottom: overview of a small telescope designed for soft x-ray spectropolarimetry, based on a design suggested by marshall (2008). a small set of nested mirror shells focusses x-rays through gratings that disperse to an array of detectors about 2 m from the entrance aperture. top left: view from the front aperture. gratings are placed behind the mirror with the grating bars oriented along the average radius to the mirror axis. the gratings are blazed in the directions shown. top right: the view from above the detectors and polarizers. spectra from the gratings are incident on multilayer-coated flats that are tilted along the dispersion axis which contains the zeroth order (dot in center). the angle of the tilt is the same for all mirrors and always redirects the x-rays to the adjacent detector in a clockwise direction. the multilayer coating spacing, d, increases linearly outward from zeroth order, just as the wavelength increases, in order to match the first order wavelength to the peak of the multilayer reflectivity. the detectors face the corresponding mirror. measuring the intensity at a given wavelength as a function of clocking angle then provides i(λ), q(λ), and u(λ). 3 a soft x-ray polarimeter we have been working on soft x-ray polarimetry concepts using multilayer-coated optics for almost 20 years, starting with a very simple design (marshall 1994). briefly, multilayer coatings consist of thin layers of contrasting materials usually one with a high index of refraction and the other with a low value. the input wave is divided at each layer into transmitted and reflected components. when many layers are placed on a surface, then the reflected components may constructively interfere, enhancing the overall reflectivity of the optic. the bragg condition must be satisfied: λ = 2d sin θ, where d = da + db is the thickness of the bilayer consisting of one layer of material a with thickness da, and one layer of material b with thickness db; λ is the wavelength of the incident radiation; and θ is the graze angle. when used at brewster’s angle, θ = 45 deg, the reflectivity of p-polarization is reduced by orders of magnitude, so that nearly 100% of the exiting beam is polarized with the e−vector perpendicular to the plane defined by the incoming and outgoing beams. designs for flight instruments based on multilayer coated optics generallly have limited bandpasses. we now have a new design that overcomes this weakness that we are prototyping in the lab. marshall (2007) 290 soft x-ray polarimeter: potential instrumentation and observations showed that it is possible to develop a laterally graded multilayer-coated mirror that combines with a dispersive optic to obtain a broad bandpass. we have studied how to develop a multilayer polarimeter as a small mission (marshall 2008; marshall et al. 2010). fig. 2 shows the results from a design suitable for a mission of opportunity or a small explorer, using one mirror assembly of a size planned for gems but with a 2 m focal length. this telescope would take 5 min to detect a polarization fraction of 8% for a source like mk 421 at its current intensity. 4 conclusions soft x-ray polarimetry has excellent prospects for scientific study of agn, blazars, and isolated neutron stars. we have designed an instrument capable of detecting a polarization fraction as low as 8% in a suborbital mission. we are prototyping components for such a mission in the lab and will have a flight-like configuration within a few months. acknowledgement this work was funded in part by nasa grant nnx12ah12g. references [1] antonucci, r. r. j., miller, j. s.: 1985, apj, 297, 621. [2] brindle, c., et al.:1986, mnras, 221, 739 doi:10.1093/mnras/221.3.739 [3] dovčiak, m., et al.:2011, apj, 731, 75. doi:10.1088/0004-637x/731/1/75 [4] ghosh, p., et al. 2013, arxiv:1301.5514 [5] heyl, j. s., shaviv, n. j., lloyd, d.: 2003, mnras, 342, 134. doi:10.1046/j.1365-8711.2003.06521.x [6] lai, d., & ho, w. c.: 2003, prl, 91, 071101. doi:10.1103/physrevlett.91.071101 [7] long, k.s., chanan, g.a., and r. novick: 1980, apj 238, 710 doi:10.1086/158027 [8] marscher, a.p.: 1980, apj, 235, 386. [9] marscher, a.p., gear, w.k.: 1985, apj, 298, 114. doi:10.1086/163592 [10] marshall, h.l.: 1994, in proceedings of the spie, s. fineschi (ed.), 2283, p. 75-84. [11] marshall, h.l.: 2007, in proceedings of the spie, s.l. o’dell, g. pareschi (eds.), 6688, p. 66880z. [12] marshall, h.l.: 2008, in proceedings of the spie, s.l. o’dell, g. pareschi (eds.), 7011 [13] marshall, h.l., et al.: 2010, in proceedings of the spie, s.l. o’dell, g. pareschi (eds.), 7732. [14] mcnamara, a.l., kuncic, z., and wu, k.: 2009, mnras, 395, 1507. doi:10.1111/j.1365-2966.2009.14608.x [15] novick, r., et al.: 1972, apjl, 174, l1. [16] pavlov, g.g., zavlin, v.e.: apjl, 490, l91. [17] pavlov, g.g., zavlin, v.e.: 2000, apj, 529, 1011. doi:10.1086/308313 [18] poutanen, j.: 1994, apjs, 92, 607. [19] radhakrishnan, v., et al. 1969, nature, 221, 443. doi:10.1038/221443a0 [20] schnittman, j.d., krolik, j.h.: 2009, apj, 701, 1175. doi:10.1088/0004-637x/701/2/1175 [21] schnittman, j.d., et al. 2013, arxiv:1301.1957. [22] silver,e.h., et al.: 1979, apj, 232, 248. [23] swank, j., et al. 2010, x-ray polarimetry: a new window in astrophysics by ronaldo bellazzini, enrico costa, giorgio matt and gianpiero tagliaferri. cambridge university press, p. 251 doi:10.1017/cbo9780511750809.038 [24] taylor, j.h., stinebring, d.r.: 1986, annreva&a, 24, 285. [25] tinbergen, j.: 1996, astronomical polarimetry, cambridge, uk: cambridge university press, pp. 174. doi:10.1017/cbo9780511525100 [26] weisskopf, m.c., et al.: 1978, apjl, 220, l117. discussion jim beall: this arrangement sounds like it’s pretty delicate. how much of a challenge dos this pose for rocket flight? herman marshall: all but one of the components have been flown on satellite missions. the remaining component, the laterally graded multilayer coated mirrors, are likely to survive based on experience with other ml coated optics, used primarily for solar astronomy. the remaining challenge is to maintain alignment and pointing, needed to match the dispersed x-rays to the ml coated mirrors. the sensitivity 291 http://dx.doi.org/10.1093/mnras/221.3.739 http://dx.doi.org/10.1088/0004-637x/731/1/75 http://dx.doi.org/10.1046/j.1365-8711.2003.06521.x http://dx.doi.org/10.1103/physrevlett.91.071101 http://dx.doi.org/10.1086/158027 http://dx.doi.org/10.1086/163592 http://dx.doi.org/10.1111/j.1365-2966.2009.14608.x http://dx.doi.org/10.1086/308313 http://dx.doi.org/10.1038/221443a0 http://dx.doi.org/10.1088/0004-637x/701/2/1175 http://dx.doi.org/10.1017/cbo9780511750809.038 http://dx.doi.org/10.1017/cbo9780511525100 herman l. marshall, norbert s. schulz to misalignments will require stiff structures while variations due to pointing jitter will require that the ml coatings have a sufficiently broad response at a target wavelength, which ultimately depends on the dispersion of the gratings used. so, mitigating jitter will depend on a tradeoff between improving pointing stability and the availability of high dispersion gratings. 292 introduction the scientific value of soft x-ray polarimetry active galactic nuclei isolated neutron stars a soft x-ray polarimeter conclusions acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0038 acta polytechnica ctu proceedings 4:38–42, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app hydrogen charging of fuel cladding methodology jakub krejčía,∗, jitka kabátováb, jan kočíb, zuzana weishauptovác, věra vrtílkováb a department of nuclear reactors, faculty of nuclear sciences and physical engineering, czech technical university in prague, czech republic b ujp praha, a.s., prague, czech republic c department of geochemistry, institute of rock structure and mechanics, czech academy of sciences, v.v.i., prague, czech republic ∗ corresponding author: krejci.jakub@seznam.cz abstract. hydrogen content is a very important parameter for mechanical properties of fuel cladding, especially after loca transients. therefore, it is necessary to take into account the amount of hydrogen absorbed in the fuel cladding during normal operation (before a hypothetical loca). the required value of hydrogen content is possible to reach by a long-term pre-oxidation test or a much shorter hydrogen charging experiment. the methodology of hydrogen charging developed in ujp is described in this contribution. results of experiments aiming to prepare samples with uniform hydrides and samples with a rim-layer and other hydrides are shown. keywords: fuel cladding, hydridation. 1. introduction thanks to a low absorption of neutrons and corrosion resistance zirconium alloys are an indispensable material for nuclear fuel cladding tubes. however, their mechanical properties deteriorate during operation in the reactor conditions, where corrosion reactions take place leading to the formation of oxide layers and also to dissolution and precipitation of hydrogen, and the formation of hydrides [1]. zirconium hydrides are brittle, and can initiate crack and fissure formation in the alloy. hydrogen also has a considerable effect on the ductility of the cladding, after a hypothetical loca (loss of coolant accident). much attention has been focused on this topic worldwide [2, 3]. the requirement of sufficient fuel rod strength upon quench taking into account an additional mechanical load is used regarding to the brittle mode, which is associated with cladding oxidation in the presence of steam at high temperature. this requirement led to a new equivalent cladding reacted (ecr) design limit based on loca semi-integral tests developed by jaea (japan atomic energy agency). this criterion is expressed as a function of in-reactor hydrogen pickup [3, 4]. alternative k-criterion and o-beta criterion for e110 alloys were developed in ujp [5, 6] also. both are applicable for specimens with hydrogen content. the presented study shows the methodology of hydrogen charging developed in ujp. samples with uniform hydrides and specimens with rim-layer and other hydrides are shown. double-sided and singlesided hydrogen charging is presented. 2. experimental and methodology 2.1. speciment preparation all samples examined in this study were fabricated of the e110 alloy. the chemical composition is presented in table 1. wt. nb h o hf zr [%/ppm] [%] [ppm] [ppm] [ppm] zr1nb 1.0 3 <400 400 balanced table 1. the chemical composition of studied alloy. the tested tubular specimens had the following dimensions: outside diameter ∼9.1 mm and wall thickness ∼686 µm. for double-sided hydrogen charging 30 mm or 90 mm long non-irradiated segments were used, which were cleaned, degreased, and then weighted, and measured (length, diameter). for single-sided hydrogen charging 90 mm long nonirradiated segments and end-plugs made of a rod from the same material were used. the tube-part and endplugs were welded together using the electron beam welding method. these specimens were cleaned, degreased, and then weighted and measured (length, diameter). after that, the samples were filled with inert gas (argon) at required inner pressure (0–12.5 mpa), and welded in a pressure chamber. the procedure of welding was developed in ujp, and the device can be seen in fig. 1. the samples were weighted after welding, and based on the mass gain of inner gas the inner pressure was recalculated. 38 http://dx.doi.org/10.14311/ap.2016.4.0038 http://ojs.cvut.cz/ojs/index.php/app vol. 4/2016 hydrogen charging of fuel cladding methodology figure 1. device used for-welding samples. 2.2. hydrogen charging using gravimetric sorption analyzer double-sided hydrogen charging was performed in cooperation with the institute of rock structure and mechanics of the czech academy of sciences, and it was published in 2015 [2]. the hydrogen charging was carried out using a microscale of an iga 002 gravimetric sorption analyzer (hiden). a sample was placed into the reactor chamber of the instrument by hanging it vertically on the microscale beam, and the entire system was evacuated at a temperature of 200 ◦c. hydrogen charging was carried out by hydrogen of 99.9999 vol.% purity at a temperature of 405 ◦c and pressure of 0.1 mpa. the mass changes of the sample and the thermodynamic conditions of the process were observed during hydrogen charging. an example of the course of the hydrogen charging process is presented in fig. 2. after the required mass gain was reached, a hydride layer was observed on the surface of the samples with the higher hydride concentration. figure 2. sample packed in aluminum foil. 2.3. autoclave charging an alternative method for hydrogen charging was developed in ujp. the autoclave method provides the possibility to charging bigger amount of samples together. target amount of hydrogen content is up to 600 ppm for pwr conditions (zirlo ∼70 gwd/t [3]), and up to 120 ppm for e110 in vver environment (∼5 years in reactor conditions). specimens were packed in an aluminum foil, which was used as a protection against oxidation, see in fig. 2. the prepared samples were placed in the autoclave with an inner volume of about 4.5 dm3. the hydrogen charging was carried out by hydrogen of 99.9999 vol.% purity at a temperature of 350 ◦c, and pressure of about 0.1 mpa. the temperature and the pressure in the autoclave during the hydrogen charging process are shown in fig. 3. figure 3. temperature and pressure during hydridation process. after the hydrogen charging process as the aluminum foil was removed, a hydride layer and oxide layer was observed on the surface of the samples, see in fig. 4. figure 4. the typical outlook of specimen after hydrogen charging process. samples were weighted after, and based on the mass gain the hydrogen pick-up was calculated. the following form is used for calculation. it presumes, that the whole mass gain corresponds to hydrogen pick-up h = ∆m v0 ∆m v0 + m0 v0 × 106 = 1 1 + m0 ∆m × 106, (1) where h is hydrogen content in ppm, ∆m is mass gain during hydridation, m0 is initial weight and v0 is sample volume. 39 j. krejčí, j. kabátová, j. kočí et al. acta polytechnica ctu proceedings 2.4. vacuum annealing the dissolving of hydride-layer was processed in a vacuum furnace (clasic). at a pressure about 10−6 bar, and temperatures of about 575 ◦c were used for annealing. the length of the exposure time was chosen up to 6 hours of duration. an influence of the temperature and the exposure time on the hydride-layer dissolution was observed. the surface of the samples after annealing was the same as before the charging process, as can be seen in fig. 5. figure 5. the typical outlook of specimen before and after vacuum annealing process. the samples were weighted after the vacuum annealing, and based on the mass loss the hydrogen pick-up was recalculated. for calculation of hydrogen content is used the equation (1), where ∆m is mass gain after annealing. 2.5. metallographic observations parts of the samples intended for a metallographic evaluation of the hydrides were fixed in epoxy resin, were prepared using a standard polishing procedure, and were etched after. on the prepared metallographic sections, the hydrides were observed and evaluated using a nikon ephiphot 300 light microscope and a lucie image analyzer. 2.6. hydrogen content measurements parts of the samples intended for hydrogen content measurements were analyzed using the analyzer g8 galileo (bruker), which works on the inert gas fusion (igf) principle. 3. results 3.1. uniform distribution of hydrides preparation of specimens with uniform distribution of hydrides was one of the objectives of the presented work. the methodology consisting of autoclave charging and vacuum annealing was applied on the sample ch21. a predicted hydrogen content value – based on weight gain and calculation – was evaluated at 123 wppm. it was in a good agreement with the experimental value gained using the g8 galileo, which was 135 wppm. a satisfactory dissolution of the hydride-layer was observed after 90 minutes of annealing in the vacuum furnace at a temperature of 575 ◦c. figure 6. sample ch21 was prepared using methodology for uniform distribution of hydrides. 3.2. influence of vacuum annealing the gravimetric sorption method was used for doublesided hydrogen of the sample 1h001. this sample was cut into 7 segments which were used for hydrogen content measurements and for experiments focused on the influence of the annealing parameters. the predicted hydrogen content value – based on the weight gain during the hydrogen charging – was evaluated at 540 wppm. it was in a very good agreement with the experimental value gained using the g8 galileo, which was 544 wppm. vacuum annealing conditions for several segments of the sample were described in table 2. segment temperature exposure time figure [◦c] [min] 1h001-6 no annealing no annealing 7 1h001-4 350 20 8 1h001-3 575 20 9 1h001-1 575 60 10 and 11 table 2. the sample 1h001, annealing conditions. the sample 1h001-6 was processed for hydrides evaluation after the hydrogen charging process. hydride layers and a uniform distribution of hydrides in the sample were found (fig. 7). the detail of sample numbered 1h001-4 did not show any observable hydridelayer dissolution (fig. 8). an observable beginning of the hydride-layer dissolution was seen for detail the sample numbered 1h001-3 (fig. 9). the metallographic evaluation of sample numbered 1h001-1 40 vol. 4/2016 hydrogen charging of fuel cladding methodology showed the hydride-layer in an advanced state of dissolution (fig. 10), or the whole hydride-layer dissolved (fig. 11). figure 7. sample 1h001, section 6. prepared after hydrogen charging (without annealing). figure 8. sample 1h001, section 4. after hydrogen charging was used annealing at temperature 350 ◦c and 20 minutes of time duration. figure 9. sample 1h001, section 3. after hydrogen charging was used annealing at temperature 575 ◦c and 20 minutes of time duration. figure 10. sample 1h001, section 1, detail b. after hydrogen charging was used annealing at temperature 575 ◦c and 60 minutes of time duration. figure 11. sample 1h001, section 1, detail a. after hydrogen charging was used annealing at temperature 575 ◦c and 60 minutes of time duration. 3.3. influence of inner pressure the mechanical properties of the fuel cladding depend not only on the hydrogen content, but as well on the orientation of the hydrides. radial hydrides can appear in some specific cases of operation, which can initiate a crack and failure of the fuel cladding. precipitation of radial hydrides was observed during slow cooling of heated samples with inner gas pressure under the temperature of hydrogen dissolution. after hydrogen charging were samples cut into segments. two were used for hydrogen content evaluation and one for metallography. the experimental values of hydrogen content gained using g8 galileo, were 328 wppm (829 447), and 393 wppm (829 463). the number of radial hydrides is directly connected with the value of applied stress, which is caused by the inner gas pressure. figures 12 and 13 show hydrides distributions for several values of inner pressure. an outer hydride-layer was observed in all cases and 41 j. krejčí, j. kabátová, j. kočí et al. acta polytechnica ctu proceedings for samples with inner pressure, especially sample numbered 829 463, radial hydrides were observed. radial hydrides for inner pressure of 0.05 mpa were not observed. the number of radial hydrides was evaluated as 34 % for 829 447 (inner pressure at 20 ◦c – 3 mpa), and 70 % for 829 463 (inner pressure at 20 ◦c – 9 mpa). figure 12. sample 829 447. after hydrogen charging with inner pressure 3 mpa. figure 13. sample 829 463. after hydrogen charging with inner pressure 9 mpa. 4. conclusions the experiments have shown that a requested hydrogen content and a uniform distribution of hydrides can be reached using hydrogen charging, and a further vacuum annealing procedure. influence of temperature and time exposure of vacuum annealing was observed. the experiments have shown the level of hydride-layer dissolution under several conditions. radial hydrides were observed during experiments with inner pressure. a large amount of radial hydrides, about 70 %, were observed for an inner pressure value which can be possibly reached in reactor conditions also. this contribution presented the methodology used for hydrogen charging in ujp. prepared samples is possible to use for loca experiments focused on testing material deteriorated during operation in the reactor conditions. future works will be focused on a more detailed elaboration of several topics. a quantitative evaluation of hydride-layer dissolution and radial hydrides precipitation will be provided. acknowledgements the authors would like to thank to j. šustr, j. sýkora, v. rozkošný, f. manoch, and m. štukbauer for the samples, and metallographic sections preparation, and for the hydrogen content evaluation. financial support for this research through grants no. cz.2.16/3.1.00/21563 and “ta02011025, program alfa – tačr” is gratefully acknowledged. references [1] h.-h. hsu. an evaluation of hydrided zircaloy-4 cladding fracture behavior by x-specimen test. journal of alloys and compounds 426(1–2):256–262, 2006. doi:10.1016/j.jallcom.2005.12.113. [2] z. weishauptová, j. navrátilová, v. vrtílková. the influence of hydrogen on high temperature oxidation of zr1nb cladding tubes. in conference topfuel 2015, proceedings – poster, pp. 319–326. 2015. https://www.euronuclear.org/events/topfuel/ topfuel2015/transactions/ topfuel2015-transactions-poster.pdf. [3] y. yan, t. burtseva, m. billone. recent results at argonne on post-quench ductility of high-burnup cladding. in fuel safety research meeting. japan atomic energy agency, 2009. [4] s. boutin, s. graff. a new loca safety demonstration in france. in conference topfuel 2015, proceedings – part ii, pp. 440–449. 2015. https://www.euronuclear. org/events/topfuel/topfuel2015/transactions/ topfuel2015-transactions-oral-2.pdf. [5] v. vrtílková, l. novotný, r. doucha, j. veselý. an approach to the alternative loca embrittlement criterion. in proceedings of segfsm topical meeting on loca fuel issues. 2004. https://www.oecd-nea. org/nsd/docs/2004/csni-r2004-19.pdf. [6] m. négyesi, v. klouček, j. lorinčík, et al. proposal of new oβ oxidation criterion for new types of the zr1nb alloy of fuel claddings. nuclear engineering and design 261:260–268, 2013. doi:10.1016/j.nucengdes.2012.09.033. 42 http://dx.doi.org/10.1016/j.jallcom.2005.12.113 https://www.euronuclear.org/events/topfuel/topfuel2015/transactions/topfuel2015-transactions-poster.pdf https://www.euronuclear.org/events/topfuel/topfuel2015/transactions/topfuel2015-transactions-poster.pdf https://www.euronuclear.org/events/topfuel/topfuel2015/transactions/topfuel2015-transactions-poster.pdf https://www.euronuclear.org/events/topfuel/topfuel2015/transactions/topfuel2015-transactions-oral-2.pdf https://www.euronuclear.org/events/topfuel/topfuel2015/transactions/topfuel2015-transactions-oral-2.pdf https://www.euronuclear.org/events/topfuel/topfuel2015/transactions/topfuel2015-transactions-oral-2.pdf https://www.oecd-nea.org/nsd/docs/2004/csni-r2004-19.pdf https://www.oecd-nea.org/nsd/docs/2004/csni-r2004-19.pdf http://dx.doi.org/10.1016/j.nucengdes.2012.09.033 acta polytechnica ctu proceedings 4:38–42, 2016 1 introduction 2 experimental and methodology 2.1 speciment preparation 2.2 hydrogen charging using gravimetric sorption analyzer 2.3 autoclave charging 2.4 vacuum annealing 2.5 metallographic observations 2.6 hydrogen content measurements 3 results 3.1 uniform distribution of hydrides 3.2 influence of vacuum annealing 3.3 influence of inner pressure 4 conclusions acknowledgements references 298 acta polytechnica ctu proceedings 1(1): 298–302, 2014 298 doi: 10.14311/app.2014.01.0298 the world space observatory -ultraviolet (wso-uv) space telescope; status update in 2013 ana i. gómez de castro1, boris shustov2, mikhail sachkov2 1aegora research group, universidad complutense de madrid, spain 2institute of astronomy of the russian academy of sciences, russia corresponding author: aig@ucm.es abstract this is a short primer and a brief update on the status of the world space observatory-ultraviolet (wso-uv) project dated in may 2013. wso-uv is a 170m primary space telescope equipped for ultraviolet imaging and spectroscopy that will be operational in 2017 hosting an open science program for the world-wide scientific community. keywords: astronomical instrumentation space astronomy ultraviolet astronomy. 1 introduction the ultraviolet (uv) range is fundamental for astrophysical investigations, since the resonance transitions of the most abundant species in the universe occur at these wavelengths/energies. the radiation cut-off at wavelengths shorter than 2800 å by the earth’s atmosphere makes uv astronomy only accessible from space. thus uv astronomy began with space exploration. after the copernicus mission, the international ultraviolet explorer (iue) was launched in 1978, becoming the first uv space observatory operated in real time; the iue allowed to carry out spectroscopic observations from 1150å to 3200å. later on, the far ultraviolet spectroscopic explorer (fuse) mission (19992007) opened the 900å -1000å spectral range for spectroscopic studies. the galaxy evolution explorer (galex, 2003-2011) has mapped, for the first time, the uv sky. as today, the hubble space telescope (hst) is the only operational mission in the uv range. hst is expected to last for a few more years. all these missions have amply demonstrated the feasibility and relevance of uv studies (see gómez de castro et al. 2006, gómez de castro & brosch 2009, for detailed compilations). the world space observatory-ultraviolet (wsouv) is an international space mission born as a response to the growing demand for uv facilities by the astronomical community. in the horizon of the next decade, the wso-uv will be the only two-meters class mission in the post-hst epoch which will guarantee access to uv wavelenghts. the project is managed by an international consortium led by the federal space agency roscosmos (russia). in this article, we briefly describe the wso-uv project, its general objectives and its main features. special emphasis is made on the ground segment and the instrument issis, the contributions of spain to the project. figure 1: the wso-uv space observatory. 2 the wso-uv scientific objectives the wso-uv is a multipurpose observatory on a geosynchronous orbit, which will provide data of large importance to investigate several open problems in astrophysics. the science drivers of the project are: • the study of the diffuse baryonic content in the universe and its chemical evolution – the main topics will be the investigation of baryonic content in warm and hot igm, of damped lyman-α 298 http://dx.doi.org/10.14311/app.2014.01.0298 the world space observatory -ultraviolet (wso-uv) space telescope; status update in 2013 systems, the role of starburts and the formation of galaxies. • the study of the formation and evolution of the milky way – the uv plays a particularly important role in the determination of energy inputs of the gas interacting with stars, and in the investigation of magnetic fields on star formation. the milky way history could be tracked through observations complementary to those obtained by the gaia mission. • the physics of accretion and outflows: the astronomical engines – this cathegory includes stars, black holes, interacting binaries, pre-main sequence stars an, in general, all those objects where accretion plays an important role in the evolution of the system. the efficiency and time scales of the phenomena will be studied, together with the role of the radiation pressure and the disk instabilities. • the investigation of the (extra)solar planetary atmospheres and astrochemistry in presence of strong uv radiation fields – the properties of the atmospheres of t tauri stars to study the environment where protoplanets grow. (see also gómez de castro et al. 2009) 3 the wso-uv mission and instrumentation the wso-uv telescope has an f/10 ritchey-chretien mounting with a primary diameter of 170 cm. wsouv has been thought as an observatory-type mission henceforth carrying instrumentation for uv imaging and spectroscopy (shustov et al. 2009, 2011). the wso-uv imaging and slitless spectroscopy instrument (issis) is a multipurpose instrument with a mode selector wheel that permits to carry out imaging and slitless spectroscopy in the 1150-3200 å spectral range. the instrument is equipped with two mcp detectors, with csi and cste photocathods for fuv and nuv observations, respectively. the wso-uv spectrographs (wuvs) consists of a set of three instruments: • the far uv high resolution spectrograph (vuves) that will permit to carry out echelle spectroscopy with resolution r∼50,000 in the 1150-1760 å range. it will be equipped with a photon-counting, micro channel plate (mcp) detector • the near uv high resolution spectrograph (uves) to carry out echelle spectroscopy with resolution r∼55,000 in the 1740-3050 å range. it will be equipped with a ccd detector to observe in the near uv. • the long slit spectrograph (lss) that will provide low resolution (r∼ 1000), long slit spectroscopy in the 11500-3050 å range. the spatial resolution will be 1 arcsec also, the width of the slit is 0.5 arcsec. the detector is a ccd cooled to −100o c to be sensitive to the far uv. figure 2: the instruments compartment in wsouv.the numbered sections correspond to: [1] optical bench with issis and wuvs mounted, [2] spectrographs, [3] cylinder inset of the instruments compartment, [4] protective cover of the instruments compartment and [5] heat pipes. (see also, sachkov 2010) prior to final tests, after the end of the construction phase, wso-uv instrumentation is expected to provide sensitivities similar to those of the hst instrumentation. the factor of 2 difference in the collecting surface between hst and wso-uv is compensated by the, much more efficient, high earth orbit of the wsouv, a geosynchronous orbit with inclination 51o. this will also allow to carry out efficiently monitoring programs. moreover, modern ”state of the art” ccd detectors will be used in the spectrographs. wso-uv expected launch date is 2016 and will be operational for five years with a possible extension to five years more. the space telescope is planned to be operated from two sites at madrid (ucm) and moscow (inasan) that will also host also the science and mission archives. the ground segment is being designed under a shared operations scheme. 299 ana i. gómez de castro, boris shustov, mikhail sachkov 3.1 issis design and expected performance the imaging and slitless spectroscopy instrument (issis) will be a key part of the wso-uv instrumentation. issis is the first uv imager to be flown to high earth orbit, above the earth geocorona. hence the uv background will be dominated by the zodiacal contribution and the diffuse galactic background due to dust-scattered starlight (murthy et al. 2010). the instrument has been designed to make full benefit of the heritage left by the galactic evolution explorer (galex) mission. galex has surveyed about 80% of the sky at uv wavelengths, providing for the first time a nearly complete view of the uv universe (martin et al. 2003, bianchi et al. 2011). however, galex spatial resolution was ∼ 4.2 arcsec and had very moderate spectroscopic capabilities. issis resolution will be ≤ 0.1 arcsec. the fine guiding system of the wsouv telescope will guarantee a high pointing stability (better than 0.1 arcsec at 3σ). moreover, issis will be equipped with gratings for slitless spectroscopy with resolution 500, in the full 1150-3200 spectral range. in imaging mode, issis effective area is about 10 times that of the galex imagers. figure 3: the layout of the imaging and slitless spectroscopy instrument (issis). the acronyms mark the location of: detectors (mcp), filter wheels (fw), pickup mirror mechanism (rm), calibration lamp (cl), mode selector mechanism (msm) and the mirrors m1 and m2. issis is designed to be an instrument for analysis of weak uv point sources or clumpy extended sources, especially those with well defined geometry. uv imaging instruments have been often equipped with prisms or very low dispersion grisms. the rapid decay of the resolution of prisms such as the available in the solar blind channel (sbc) of the advanced camera system (acs) makes very difficult its use to map extended line emission at wavelengths above some 1350 å. as the transmittance of narrow band filters in the far uv is ≤ 3% , integral-field low resolution spectroscopy is the main mean to map nebular emission. issis gratings will make feasible to use the powerful uv diagnostic tools to determine the location of dusty blobs and measure electron densities and temperatures. the instrument is located below the primary mirror and above the optical bench. this location imposes additional constraints to the design, in terms of weight and size: the maximum weight on the optical bench is 61.5 kg, and the full instrument has to be fit within a flat cylinder of height 17 cm. issis is fed by the central part of the beam but a pick-up mirror is required to fold the beam from the telescope adding one reflection. the final design is a compromise between the scientific requirements and the telescope/platform requirements. figure 3 shows the layout of the instrument. 4 wso-uv science programs the wso-uv will run three major science programs (see malkov et al. 2011 for details): • the core program includes the key scientific programs that will carry over the scientific objectives of the mission. the core program will be run for the first two years of the mission by the consortium building and operating wso-uv. • national programs: each country or funding body contributing to the project is entitled to receive a fraction of the observing time proportional to its contribution. after the third year of the project, 60% of the observing time will be awarded to these programs. national calls are expected to be issued for the national programs though they will be synchronized with the general project calls. guaranteed time for the instruments teams should be included in the national contributions. • open program to the world wide scientific community. this program will handle a 40% of the observing time after the 3rd year of the mission. targets of opportunity observations will be managed within these programs. 5 wso-uv ground segment (gs) the wso-uv gs is comprised of all the infrastructure and facilities involved in the preparation and execution of the wso-uv mission operations, which typically encompass real-time monitoring and control of the spacecraft, telescope and instruments as well as reception, processing and storage of the scientific data. in principle, there will be two complete gs systems: the russian 300 the world space observatory -ultraviolet (wso-uv) space telescope; status update in 2013 one will be located in moscow (lavochkin association and institute of astronomy of the ras), and the spanish one will be sited at madrid. the satellite operations will be shared between both ground control centers, transferring the mission control from one center to the other on a regular basis (lozano et al 2011). figure 4: basic layout of wso-uv ground segment. the science operations system and a fraction of the mission operations system are part of the spanish contribution to the wso-uv. the remote proposal system (rps), the science data processing system (sdps), the science archive (sa) and the scheduling systems are defined by the international science team composed by spanish and russian science support teams based at the universidad complutense de madrid (ucm) and russian science institute of astronomy of the russian academy of science (inasan). the science support team (st) is part of the man power of the gs, and is responsible of laying the foundation of and supervising all the operations related to the mission primary users: the scientists. at mission level, the st constitutes the core of the future wso-uv international observatory. a sumary of the high level definition documents, approved at mission level, for the development of the main science systems for wso-uv gs can be found in gómez de castro et al. 2011. 6 conclusions wso-uv is an international observatory that will grant access to the uv range in the post-hst era. at the time these proceedings are being written, the project is evolving into the construction phase. acknowledgement the spanish participation in the wso-uv project is being funded by the ministry of industry, energy and tourism (minetur). the scientific contribution to wso-uv is being funded by the ministry of economy and competitivity through the grant aya2011-29754c03. the authors wish to thank the large industrial and scientific team in russia and spain who are involved in the project for their dedication and expertise. references [1] bianchi, l., efremova, b., herald, j. et al. 2011, ap&ss, 335, 161 doi:10.1007/s10509-010-0581-x [2] gómez de castro, a.i., wamsteker, w., barstow, m. et al. 2006 ap&ss, 303, 133 doi:10.1007/s10509-006-9057-4 [3] gómez de castro, a.i., & brosch, n. 2009 ap&ss, 320, 1 doi:10.1007/s10509-009-0005-y [4] gomez de castro a.i. et al. 2009, in: chavez et al., new quests in stellar astrophysics. ii. ultraviolet properties of evolved stellar populations. p.319 springer, berlin [5] gómez de castro, a.i., sestito, p., sanchez doreste, n., et al. 2012, space ops 2012, on-line proceedings (http://www.spaceops2012.org/proceedings/ proceedings.html) [6] gómez de castro et al. 2012, space telescopes and instrumentation 2012: ultraviolet to gamma ray. proceedings of the spie, volume 8443, article id. 84432w. [7] lozano, j.m. et al. 2010, space ops 2010, aiaa 2010-2212 [8] malkov, o. et al., 2011 ap&ss, 335, 323 doi:10.1007/s10509-010-0589-2 [9] martin, c. et al. 2003, future euv/uv and visible space astrophysics missions and instrumentation. edited by j. chris blades, oswald h. w. siegmund. proceedings of the spie, volume 4854, pp. 336-350. [10] murthy, j., henry, r. c., & sujatha, n. v. 2010, apj, 724, 1389 doi:10.1088/0004-637x/724/2/1389 [11] reutlinger a. et al. 2011, apss 335, 311 [12] sachkov m. 2010, apss 329, 261 [13] shustov, b. et al. 2009 ap&ss, 320, 187 [14] shustov, b. et al. 2011 ap&ss, 335, 282 301 http://dx.doi.org/10.1007/s10509-010-0581-x http://dx.doi.org/10.1007/s10509-006-9057-4 http://dx.doi.org/10.1007/s10509-009-0005-y http://dx.doi.org/10.1007/s10509-010-0589-2 http://dx.doi.org/10.1088/0004-637x/724/2/1389 ana i. gómez de castro, boris shustov, mikhail sachkov discussion james beall: any idea of a possible launch date?. it’s a beautiful instrument. ana i. gomez de castro: the foreseen launch date is end of 2016. nino panagia: i believe this is a very important project. i’m wondering what is its expected lifetime. ana i. gomez de castro: the mission lifetime is 5 years plus 5 additional years after review. a 302 introduction the wso-uv scientific objectives the wso-uv mission and instrumentation issis design and expected performance wso-uv science programs wso-uv ground segment (gs) conclusions 38 acta polytechnica ctu proceedings 1(1): 38–41, 2014 38 doi: 10.14311/app.2014.01.0038 fullerenes, pahs, amino acids and high energy astrophysics susana iglesias-groth1,2 1istituto de astrofisica de canarias, la laguna, via láctea sn, 38201 la laguna, spain 2departamento de astrof́ısica de universidad de la laguna, la laguna, tenerife, spain corresponding author: sigroth@iac.es abstract we present theoretical, observational and laboratory work on the spectral properties of fullerenes and hydrogenated fullerenes. fullerenes in its various forms (individual, endohedral, hydrogenated, etc.) can contribute to the uv bump in the extinction curves measured in many lines of sight of the galaxy. they can also produce a large number of absorption features in the optical and near infrared which could be associated with diffuse interstellar bands. we summarise recent laboratory work on the spectral characterisation of fullerenes and hydrogenated fullerenes (for a range of temperatures). the recent detection of mid-ir bands of fullerenes in various astrophysical environments (planetary nebulae, reflection nebulae) provide additional evidence for a link between fullerene families and diffuse interstellar bands. we describe recent observational work on near ir bands of c60 + in a protoplanetary nebula which support fullerene formation during the post-agb phase. we also report on the survival of fullerenes to irradiation by high energy particles and gamma photons and laboratory work to explore the chemical reactions that take place when fullerenes are exposed to this radiations in the presence of water, ammonia and other molecules as a potential path to form amino acids. keywords: ism molecules: fullerenes, pahs nebulae. 1 introduction the discovery of fullerenes in 1985 when trying to reproduce the chemistry of the atmospheres of red giant stars (kroto et al., 1985) led to the identification of the third allotropic form of carbon. the most abundant fullerene molecule produced in those experiments was c60, a hollow molecule with 60 carbon atoms distributed in 12 pentagons and 20 hexagons (truncated icosahedron symmetry). comparetively, we recall polycyclic aromatic hydrocarbons (pahs) are planar molecules consisting of carbon rings and hydrogen, these rings are similar to benzene. the naphthalene and anthracene are the most simple pahs with two and three benzene rings, respectively. these molecules have been postulated as potential carriers of the unidentified infrared emission bands and of the diffuse interstellar bands which are ubiquitous in the interstellar medium (see e.g. léger and puget 1984). similarly, fullerenes and their hydrogenated forms, are potential carriers of the interstellar bands. several studies have shown that carbon ring based molecular forms are very stable against uv radiation. this is remarkable because the basic structures of amino acids and in general of the molecular basis of life are essentially conformed by such carbon rings making them rather stable against possible mutations. laboratory work bychen et al. (2008) have aaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaa aaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaa demonstrated that under strong uv radiation a mixture of naphthalene, ice and methane at low temperature, it is possible to form a large variety of amino acids. fullerenes with carbon atom number of 20 (m2 + n2 + nm) where n and m are integers have icosahedral symmetry groups ih and exhibit high stability. these molecules are very stable against uv/gamma radiation and collisions with other particles. fullerenes have been detected in carbonaceou chondrites, a type of meteorite that originated in the early solar system,with abundances of the order of 0.1 ppm (pizzarello et al. 2000). on earth, fullerenes have been detected in sedimentary layers of the cretaceous-tertiary boundary (ktb) in china and bulgaria and in the mineral shunghite of the region of karelia (russia). in the various phases of the interstellar medium it is likely the presence of both, fullerenes and hydrogenated fullerenes, the socalled fulleranes (cnhm). a review of the properties of fullerenes and fulleranes can be found in cataldo & iglesias-groth (2009, 2010). here, recent developments on the astrophysical search for ionised fullerenes and on the properties of fullerenes when exposed to high energy radiation. 38 http://dx.doi.org/10.14311/app.2014.01.0038 fullerenes, pahs, amino acids and high energy astrophysics 2 astrophysical searches for fullerenes theoretical work on the photoabsorption spectrum of icosahedral fullerenes suggests that these molecules can be responsible of the strongest feature in the interstellar extinction curve, the uv bump at 2175 å. for large fullerenes and buckyonions the experimental photoabsorption spectrum is very poorly known and the potential role of these molecules in interstellar absorption has been explored on a theoretical basis (see, for example, iglesias groth et al., 2002, 2003). in these works a theoretical approach to the photoabsorption specturm was based on a hückel and pariser-parr-pople (ppp) model. fits of the computed spectra to measurements of the interstellar extinction in the uv/optical for different lines of sight in our galaxy (fitzpatrick, 1999) were obtained (see details of the model can be found in iglesias-groth, 2004). very good fits to the extinction curves are provided by the photoabsorption cross sections computed for both individual fullerenes and buckyonions. the comparison of these models with the observed uv bump leads to an estimate of the number density of these molecules (in the range 0.2-0.08 ppm) and of the percentage of carbon locked in fullerenes and buckyonions in the ism (iglesias-groth 2004, 2007) which depending the size distribution of these molecules could reach up to 25 % of all carbon in the ism. fullerenes c60 and c70 present active vibrational bands in the near infrared (3-20 µm) which have been key for their identification in planetary nebulae, reflection nebulae and post-agb stars (see e.g. cami et al. 2010, zhang and kwok, 2011). experimental measurement of the molar absorptivity for these infrared transitions is essential for the determination of fullerene abundances in such astrophysical contexts. laboratory work is being conducted to measure the dependence of the molar absorptivity of fullerene infrared bands with temperature from approx. 100 k to 500 k to cover a variety of conditions in the interstellar medium (iglesias-groth et al. 2011). 2.1 new results on ionised fullerenes: c+ 60 recently, it was reported the detection of mid-ir vibrational transitions of the fullerene c60 in a carbon rich protoplanetry nebula, iras 01005+7910 (zhang and kwok 2010). we recorded the spectrum of this object between 5500 and 10000 å with resolving power of 57,000 and detected two bands at 9577 and 9632 å which are consistent with laboratory measurements of the c60 cation (see figure 1. iglesias-groth and esposito, 2013). if these two bands were produced by c+ 60 in the material surrounding the central post-agb star we could infer that ∼ 1 % of carbon is trapped in this ionized form of fullerenes and that the cation abundance is much higher than that of the neutral fullerene species. it appears that ionized fullerene species in this protoplanetary nebula are significantly more abundant than in neutral form, which is consistent with the predictions of ionization models of pahs (bakes and tielens 1995, salama et al. 1996) for irradiated clouds near a hot star. figure 1: the two near ir bands in the spectrum of iras01005+7910, attributed to the cation of c60 (iglesias-groth & esposito 2013) these observations provide additional evidence for the presence of fullerenes in protoplanetary nebulae and suggest that a significant production takes place in this late stage of stellar evolution. mid-ir bands of c+ 60 could be present in the 7-20 µm spectrum of iras 01005+7910 and are also likely to be detected in the spectra of planetary nebulae. accounting for the ionized species of fullerenes appears necessary in nebulae with a nearby source of ionizing photons. a caveat: the derived abundances and excitation temperatures of planetary nebulae with claimed detections of fullerenes may have to be revised if indeed there is a significant contribution of cations to the formation of the bands used in these analyses. high resolution spectroscopy will be required for a reliable determination of the relative abundance of neutral and ionized fullerenes in these objects. 2.2 the stability of c60 and c70 towards copuscular and γ radiation the stability of c60 and c70 fullerenes in the interstellar medium and embedded in meteorites and comets has been investigated with γ irradiation and with he+ ion bombardment. the radiation dose generated by radionuclides decay expected to be delivered to fullerenes buried at a depth of ≥ 20 m in comets and meteorites is about 3 mgy per million years. we have exposed fullerenes to various radiation doses and found that these molecules are by far resistant to this type of radiation. laboratory measurements on the concentra39 susana iglesias-groth tion of samples of fullerenes exposed to strong radiation doses indicate that these molecules can survive millions of years inside comets and meteorites (cataldo et al. 2009). this provides a natural explanation to their presence inside certain carbonaceous chondrites. in this laboratory experiments, fullerenes were also exposed to intense particle bombardment. fullerens adsorbed or deposited on the surface of carbon are exposed to cosmic ray bombardment with estimated doses of radiation comprised between 30 and 65 mgy per 106 years. we carried out experiments to test the survival of both c60 and c70 fullerenes and found that the complete amorphization occurs at about a radiation dose of 250 mgy. thus we infer that after 4-8 millions of years exposure to cosmic rays it is expected to producce a complete amorphization (cataldo et al. 2009). 2.3 gamma radiolysis of c60 fullerene in water and water/ammonia mixtures; relevance of fullerenes fate in ices of interstellar medium in order to explore the potential astrochemical role of fullerenes,iglesias-groth et al. (2013) have explored the radiolysis of fullerene c60 dispersed in h2o, h2o/nh3, h2o/methanol and h2o/nh3/methanol under gamma radiation doses of 250 and 500 kgy. it was found that c60 originally insoluble in the above mentioned hosting matrix became soluble as a consequence of multiple hydroxylation and oxidation reaction produced by the free radicals generated by the radiolysis of the hosting matrix. the changes undergone by c60 were studied by infrared spectroscopy (ft-ir) and by electronic absorption spectroscopy. the astrochemical consequences of the present study are that c60 ejected in the interstellar medium for instance from protoplanetary and planetary nebulae can condense together with water and other ices in dense molecular clouds. under the action of high energy radiation c60 reacts with the free radicals generated from the matrix where it is embedded it is solubilized and consequently its carbon content becomes available for further abiotic processes of synthesis of molecules of astrobiological interest. the behavior of c60 appears comparable to that of common pahs which are also hydroxylated and oxidized under similar conditions. 3 stability toward high energy radiation of non-proteinogenic amino acids: implications for the origins of life in order to investigate the response of amino acids to high energy radiation, cataldo et al. (2013) have taken a series of non-proteinogenic amino acids, most of them found frequently in carbonaceous chondrites, and exposed them to solid state radiolysis in vacuum to a total radiation dose of 3.2 mgy. this corresponds to 23% of the total dose expected to be taken by organic molecules buried in asteroids and meteorites since the beginning of the solar system in 4.6 x 109 years. the radiolyzed amino acids where studied by ft-ir spectroscopy, differential scanning calorimetry (dsc) and by polarimety and optical rotatory dispersion (ord). it is found that an important fraction of each type of amino acid is able to ”survive” to the massive dose of radiation and also the enantiomeric excess is partially preserved. based on these results it is concluded that it is not a surprise to find amino acids even in enantiomeric excess in carbonaceous chondrites. 4 conclusions the astrochemical consequences of the recent discoveries of fullerenes in various astrophysical contexts are not fully understood yet. fullerenes are far resistant to high doses of gamma radiation and bombardment by high energy particles. it is likely that fullerenes ejected in the interstellar medium,for instance from protoplanetary and planetary nebulae can condense together with water and other ices in dense molecular clouds. under the action of high energy radiation fullerenes react with the free radicals generated from the matrix where they are embedded. if c60 is trapped in water ices it is hydroxylated and oxidized by the radiolysis products of water. the oxidation of c60 makes this molecule hydrophilic and hence soluble in water. the same phenomenon occurs in water/ammonia, in water/methanol and in water/ammonia/methanol mixtures. thus, c60 which in the solid state displays a considerable radiation resistance, when embedded in radiolytic sensitive matrices like those just mentioned, it reacts swiftly, it is solubilized and consequently its carbon content becomes available for abiotic processes of synthesis of other molecules of astrobiological interest. this compares well with the behavior of pahs which are also hydroxylated and oxidized by the free radicals produced by the radiolysis of the hosting matrix (gudipati & allamandola 2006, ricca et al. 2007, ashbourn et al. 2007, cuylle et al. 2012, nuevo et al. 2012). it is known that pahs and ices exposed to strong uv radiation can lead to the formation of amino acids. fullerenes exposed to gamma radiation provides a path for a variety of astrochemical reactions which have to be explored in much more detail, which ultimately could lead to the formation of amino acids, which are likely to survive under the intense gamma radiation. further laboratory work is essential to explore the role of high energy radiation in astrophysical sources and carbon molecules as a route to prebiotic molecules. 40 fullerenes, pahs, amino acids and high energy astrophysics references [1] bakes, e. & tielens, a. g. g. m. 1995, aspc, 73, 59 [2] cami, j, bernard-salas, j, peeters, e & malek, s. e. 2010, science [3] cataldo, f., iglesias-groth, s. 2009, mnras, 400, 291 doi:10.1111/j.1365-2966.2009.15457.x [4] cataldo, strazzulla and iglesias-groth et al. 2009, mnras, 394, 615 [5] cataldo, f & iglesias-groth,s 2010, in fullerenes:the hydrogenated fullerenes, springer, berlin [6] chen et al. , 2008, mnras, 384, 60 [7] cuylle, s. h., tenenbaum, e. d., bouwman, j., linnartz, h. & allamandola, l. j. 2012, mnras, 423, 1825 doi:10.1111/j.1365-2966.2012.21006.x [8] fitzpatrick, e. l 1999, pasp, 111, 63 [9] iglesias-groth, s. et al., 2002, jchph, 116,1064810655 [10] iglesias-groth, s. et al., 2003, jchph, 118, 71037111 [11] iglesias-groth, s. 2004, ,apjl 608, l37 doi:10.1086/422216 [12] iglesias-groth, s. 2007, apjl, 661,l167 doi:10.1086/518832 [13] iglesias-groth, s., cataldo, f., ursini, o.& manchado, a. 2011, mnras, 210, 1447-1453. [14] iglesias-groth,s.,cataldo, f. & manchado, a. 2011 , mnras, 413, 213 doi:10.1111/j.1365-2966.2011.18124.x [15] iglesias-groth, s. & esposito, m. 2013,apjl ,776, l2 doi:10.1088/2041-8205/776/1/l2 [16] iglesias-groth, s., hafez, y., angelini, g. & cataldo, f. 2013, in press [17] kroto, h. w. et al. 1985, nature, 318, 162 [18] léger, a. & puget, j. 1984, a&a, 137,5 [19] nuevo, m., milam, s. n.& sandford, s. a. 2012, asbio 12, 295 [20] pizzarello, s. & cronin, j. r. 2000,gecoa,64, 329 doi:10.1016/s0016-7037(99)00280-x [21] ricca, a., bakes, e. l. o. & bauschlicher, c. w., jr. 2007, apj, 659, 858 doi:10.1086/512037 [22] salama, f., bakes, e. l. o., allamandola, l. j.& tielens, a. g. g. m. 1996, apj, 458, 621 [23] zhang, y., kwok, s. 2011,apj , 730, 126 doi:10.1088/0004-637x/730/2/126 41 http://dx.doi.org/10.1111/j.1365-2966.2009.15457.x http://dx.doi.org/10.1111/j.1365-2966.2012.21006.x http://dx.doi.org/10.1086/422216 http://dx.doi.org/10.1086/518832 http://dx.doi.org/10.1111/j.1365-2966.2011.18124.x http://dx.doi.org/10.1088/2041-8205/776/1/l2 http://dx.doi.org/10.1016/s0016-7037(99)00280-x http://dx.doi.org/10.1086/512037 http://dx.doi.org/10.1088/0004-637x/730/2/126 introduction astrophysical searches for fullerenes new results on ionised fullerenes: c60+ the stability of c60 and c70 towards copuscular and radiation gamma radiolysis of c60 fullerene in water and water/ammonia mixtures; relevance of fullerenes fate in ices of interstellar medium stability toward high energy radiation of non-proteinogenic amino acids: implications for the origins of life conclusions 269 acta polytechnica ctu proceedings 2(1): 269–272, 2015 269 doi: 10.14311/app.2015.02.0269 x-ray observations of vy scl-type nova-like binaries in the high and low state p. zemko1,2, m. orio2,3 1sternberg astronomical institute, moscow state university, 13, universitetskij ave., moscow, 119991, russia 2inaf osservatorio di padova, vicolo dell’ osservatorio 5, i-35122 padova, italy 3department of astronomy, university of wisconsin, 475 n. charter str., madison, wi 53704, usa corresponding author: polina.zemko@gmail.com abstract four vy scl-type nova-like systems were observed in x-rays both during the low and the high optical states. they are bz cam, mv lyr, tt ari, and v794 aql. using archival rosat, swift and suzaku observations we found that the x-ray flux for bz cam is higher during the low state, but there is no supersoft x-ray source (sss) that would indicate the thermonuclear burning predicted in a previous article. the x-ray flux is lower by a factor 2–10 in the low than the high state in other systems, and does not reflect the drop in ṁ inferred from optical and uv data. the best fit model for the x-ray spectra is a collisionally ionized plasma model. the x-ray flux may originate in a shocked wind or in accretion onto polar caps in intermediate polar systems that continues even during the low state. keywords: cataclysmic variables dwarf novae x-rays. 1 introduction nova-like (nls) stars are non-eruptive cvs (warner, 1995), classified into several subtypes according to their properties. here we will focus on the vy scl-type nls or “anti-dwarf novae” characterized by the presence of occasional dips on the ilight icurve, iso-called ilow states. the large optical and uv luminosity has suggested that in the high state these objects are undergoing mass transfer onto the wd at a high rate ṁ , > 10−10 m� year−1, sustaining an accretion disk in a stable hot state and preventing dwarf novae (dne) outbursts. the low states have been attributed to a sudden drop of the ṁ from the secondary, or even to a total cessation of a mass transfer (hessman, 2000). greiner et al. (1999) proposed a link between the vy scl-type stars and super soft x-ray sources based on a rosat observations of v751 cyg. these authors found an anti-correlation in the optical and x-ray intensity, and despite the very poor spectral resolution of the rosat hri, the spectrum appeared to be very soft in the low state. these authors suggested that quasi-stable thermonuclear burning occurs on the surface of the wd in the low state. in this framework, vy scl-type stars are key objects in the evolution of interacting wd binaries, in which hydrogen burning occurs periodically without outbursts. thus they may reach the chandrasekhar mass and the conditions for type ia supernovae explosion. using archival x-ray observations, in this paper we compare the high and low state x-ray data of 4 vy scl-type stars attempting to reveal evidence of nuclear burning during the low state, or seeking alternative explanations for the changes that take place during the transition from the high to low state. 2 observation and data analysis we examined the archival x-ray data of vy scl-type stars obtained with swift and rosat and chose the objects that were observed both in the high and low states: bz cam, mv lyr, tt ari and v794 aql. to determine when the low and high optical states occurred, we relied on the data of the variable star network (vsnet) collaboration (kato et al., 2004), aavso1 and asas databases. we used heasoft version 6-13 to analyze the data and xspec version 12.8.0 for spectral modeling. we also estimated the uv magnitudes of the objects using both swift/uvot and additional galex archival observations. 3 results in figure 1 we show the high and low state x-ray spectra of tt ari, bz cam, mv lyr and v794 aql and 1 http://www.aavso.org 269 http://dx.doi.org/10.14311/app.2015.02.0269 p. zemko, m. orio the fits to these spectra. the fit parameters are summarized in table 1 and 2. tt arietis (top panel of fig. 1) is one of the most optically luminous cvs, usually at mag. 10–11. sometimes it abruptly falls into an “intermediate state” around 14 mag. or even into a “low state” at about 16.5 mag. according to belyakov et al. (2010), this binary system consists of a 0.57–1.2 m� tt ari 1 2 3 4 5 6 7 0. 0 0. 1 0. 2 0. 3 bz cam 1 2 3 4 5 6 7 0. 00 0. 02 0. 04 0. 06 mv lyr no rm al iz ed c ou nt s (c nt s/ s/ ke v ) 2 4 6 8 0. 00 0. 02 0. 04 v794 aql 1 2 3 4 5 6 0. 00 0. 04 0. 08 0. 12 energy (kev) figure 1: the low and high states x-ray spectra of bz cam and mv lyr observed with swift. tt ari and v794 aql were observed with swift during the low and intermediate states. the high and intermediate state spectra are plotted in red and the low state spectra in black. the solid lines show the spectral fits, the dots with error bars are the data points. white dwarf and a 0.18–0.38 m� secondary component. the orbital period is porb = 0.13755114 d. (thorstensen, smak & hessman, 1985). the high state x-ray flux appeared to be about ten times larger than in the low state. we fitted the high state spectrum with a two components thermal plasma model (apec model – emission spectrum from collisionally ionized diffuse gas calculated using the atomdb code v2.0.1), and also with one component black body model. the low state spectrum is also well fitted with a 2 components thermal plasma model. bz cam is a nl star at a distance 830 ± 160 pc. (ringwald & naylor, 1998) with an orbital period of porb = 0.153693(7) d. (patterson et al., 1998). most of the time it shows brightness variations around 12– 13 mag., with rare occasional transitions to the 14– 14.5 mag. low states. bz cam is surrounded by a bright emission nebula with a bow-shock structure. hollis (1992) proposed that the bow shock structure must be due to the interactions of wind from bz cam with the interstellar medium. greiner et al. (2001) suggested that this nebula is photoionized by a bright central object that must be a super soft x-ray source, while the bow shock structure is due to the high proper motion of bz cam. from the second plot of fig. 1 it can be seen that the luminosity is higher in the low state, however, in the very soft spectral region, at energy ≤0.5 kev, the x-ray flux is almost twice higher in the high state, which is exactly the opposite of the idea proposed by greiner et al (1999). interestingly, the spectral fits in both states indicate that we may be observing a strong ne x lyα line at 1.02 kev. we fit the low and high state spectra of bz cam, with a two-component apec model with variable abundances. in this fit we found an underabundance (with respect to solar values) of c and n and and an overabundance of o, ne, and intermediate mass elements like s and ca. figure 2: the swift uvot image of bz cam, in which the bow-shock emission nebula is clearly detected. the uv magnitudes of bz cam in the high and low states indicate a smaller variation than observed in the other objects (albeit in different uv filters). this is explained by figure 2 in which we show the uv image of the nebula obtained with swift/uvot observations. obviously the ionized nebula also emits copious uv flux. comparing the image of bz cam in figure 2 and the one, presented in the figure 4 in (greiner et 270 x-ray observations of vy scl-type nova-like binaries in the high and low state al., 2001), one can see an additional prominent feature of the nebula in the former image. mv lyr is at about 12–13 mag. in the high state and 16–18 mag. in the low state. hoard et al. (2004) have shown that the distance to the object is 505 ± 50 pc. with their fuse (far ultraviolet spectroscopic explorer) observations these authors estimated an upper limit to ṁ during the low state ≤ 3×10−13 m� year−1. the orbital period of this system is porb = 0.1329 d. (skillman, patterson & thorstensen, 1995). our data show that the high state x-ray flux of mv lyr is higher by an order of magnitude than in the low state. the spectrum is also harder with additional component prominent above 1.7 kev. we fitted the high state spectrum of mv lyr with a two components thermal plasma model. a good fit is also obtained with a thermal plasma and a power law model (see table 1). v794 aql varies between 14 and 15 mag. in the high optical state, and in the low states it can plunge to 18 – 20 mag. the orbital period is porb = 0.1533 d. (honeycutt & schlegel, 1985). godon et al (2007) derived the following binary system parameters: mwd = 0.9 m�, high state ṁ = 10−8.5 − 10−8.0 m� year−1, inclination i = 60o, and distance to the system d = 690 pc. we fitted the intermediate state spectrum of v794 aql with two vapec components (see table 2). in both components we need high abundance of mg and ni and underabundant s and fe. 4 discussion and conclusions the first conclusion that can be derived from the presented spectra is that in all the objects both in high and low states there is no evidence of the thermonuclear burning on the surface of wd. an important motivation for this research has been the claim by greiner (1998) and greiner et al. (2001) that some of the wd table 1: fitting models and parameters for bz cam and mv lyr bz cam mv lyr high state low state high state low state satellite swift swift swift swift models vapec vapec+vapec vapec+vapec vapec+plow apec+apec apec+apec n(h)(1022) 0.14 ± 0.03 0.29 ± 0.11 0.6 ± 0.3 0.002+1.049 −0.002 0.87 ± 0.23 0.12+0.34 −0.12 photon index 0.8 ± 0.3 t1 (kev) 10.4 ± 2.7 0.57 ± 0.26 0.6 ± 0.4 0.9 ± 0.7 0.09 ± 0.03 0.7 ± 0.4 t2 (kev) 11 ± 3 63.9+0.1 −54.9 12 ± 7 4.8+42.8 −2.6 flux∗ abs 3.78 ± 0.26 3.95 ± 0.27 5.8+6.4 −5.8 5.3 ± 0.8 4.4 ± 0.6 0.9 ± 0.7 flux∗ unabs 4.24 ± 0.26 4.84 ± 0.27 8.6 5.5 ± 0.9 367 ± 50 1.6 ± 1.2 χ2 1.1 1.0 1.0 1.0 1.1 ∗the x-ray flux (×10−12erg cm−2 s−1) was calculated in the following energy range: 0.3 – 10.0 kev for swift xrt table 2: fitting models and parameters for tt ari and v794 aql tt ari v794 aql high state low state intermediate state low state satellite rosat swift swift swift models apec+apec apec+apec apec vapec+vapec apec n(h) (1022) 0.030 ± 0.002 0.056+0.106 −0.056 0.026+0.054 −0.026 0.05 ± 0.04 0.029+0.086 −0.029 t1 (kev) 0.812 ± 0.014 0.7 ± 0.4 3.6 ± 1.2 16.4+39.1 −8.7 8.8+29.1 −3.7 t2 (kev) 14 ± 9 4.4 ± 1.9 0.97 ± 0.35 flux∗ abs 5.52 ± 0.17 0.97 ± 0.17 0.94 ± 0.15 7.5 ± 1.1 2.1 ± 0.7 flux∗ unabs 6.76 ± 0.17 1.08 ± 0.17 1.02 ± 0.15 8.8 ± 1.1 2.7 ± 0.7 χ2 1.0 1.0 1.2 1.0 0.7 ∗the x-ray flux (×10−12erg cm−2 s−1) was calculated in the following energy ranges: 0.2 – 2.5 kev for rosat pspc and 0.3 – 10.0 kev for swift xrt 271 p. zemko, m. orio in vy scl-type stars must be burning hydrogen quietly in the low state, without ever triggering thermonuclear flashes because of the short duration of the burning. we find that the predicted supersoft x-ray source (manifestation of the thermonuclear burning) does not appear in the low states. we also find another unexpected result, namely that the x-ray luminosity does not follow the optical/uv drop. in one case, bz cam, the x-ray luminosity increases in the low state, and in the others, the decrease in x-ray flux in the low state is smaller than that in the optical and uv. the x-ray flux varies much less than the optical flux, by a factor of 2 to 10 during the transition from high to low state. the best-fit model for the 0.3–10.0 kev broad band spectra is two-component absorbed thermal plasma model. we do not find evidence of a boundary layer of the accretion disk emitting in the x-ray range. probably the emission is mainly in the far uv (e.g godon et al., 2007). it appears likely that some, or all the x-ray flux is produced in a wind from the system: an ongoing fast wind may be the cause of the extended bz cam nebula, initially classified as a planetary nebula. however, tt ari shows a quasi periodic oscillations in x-rays, which can be understood in the context of accretion, but is not explained by a wind. the x-ray flux may also be due to a different, and coexistent mode of accretion other than the disk, i.e. a magnetically driven stream to the polar caps of an intermediate polar. the x-rays and optical flux variations anticorrelate only in bz cam, which may be due to a wind causing additional absorption and obscuring the luminous disk. a second explanation for the lack of correlation of uv/optical versus x-ray flux variations, involving magnetic accretion, appears more plausible at least for three of the systems. the scenario we suggest is that the stream to the polar caps still continues, at decreased rate, when the accretion disks ceases to exist. references [1] belyakov k. v., suleimanov v. f., nikolaeva e. a., borisov n. v., 2010, in werner k., rauch t., eds, american institute of physics conference series vol. 1273 of american institute of physics conference series, p. 342–345. [2] greiner j., 1998, a&a, 336, 626 [3] greiner j., tovmassian g., orio m., lehmann h., chavushyan v., rau a., schwarz r., casalegno r., scholz r., 2001, a&a, 376, 1031 [4] greiner j., tovmassian g. h., di stefano r., prestwich a., gonzález-riestra r., szentasko l., chavarŕıa c., 1999, a&a, 343, 183 [5] godon p., sion e. m., barrett p., szkody p., 2007, apj, 656, 1092 doi:10.1086/510775 [6] hessman f. v., 2000, new astronomy reviews, 44, 155 doi:10.1016/s1387-6473(00)00030-0 [7] hoard d. w., linnell a. p., szkody p., fried r. e., sion e. m., hubeny i., wolfe m. a., 2004, apj, 604, 346 doi:10.1086/381777 [8] hollis j. m., oliversen r. j., wagner r. m., feibelman w. a., 1992, apj, 393, 217 doi:10.1086/171499 [9] honeycutt r. k., robertson j. w., 1998, astronomical journal, 116, 1961 doi:10.1086/300539 [10] honeycutt r. k., schlegel e. m., 1985, pasp, 97, 1189 doi:10.1086/131684 [11] kato t., uemura m., ishioka r., nogami d., kunjaya c., baba h., yamaoka h., 2004, pasj, 56, s1 [12] patterson j., raymond j. c., 1985, apj, 292, 535 doi:10.1086/163187 [13] patterson j., patino r., thorstensen j. r., harvey d., skillman d. r., ringwald f. a., 1996, astronomical journal, 111, 2422 doi:10.1086/117976 [14] ringwald f. a., naylor t., 1998, astronomical journal, 115, 286 [15] skillman d. r., patterson j., thorstensen j. r., 1995, pasp, 107, 545 [16] thorstensen j. r., smak j., hessman f. v., 1985, pasp, 97, 437 [17] warner b., 1995, cataclysmic variable stars (cambridge: cambridge university press). discussion dmitry bisikalo: could you estimate the impact of bow shock to observed x-ray flux? polina zemko: the bz cam image in hα (figure 4 of greiner et al., 2001) shows two distinct bright features in the bow shock front, one at ∼12 arcsec, the other at ∼40-45 arcsec from the central source. nevertheless, the psf of the source in x-ray image obtained with swift is quite symmetric and typical of a point source. so even with the modest spatial resolution of swift we can rule out that the bow shock contributes significantly to the x-ray flux. 272 http://dx.doi.org/10.1086/510775 http://dx.doi.org/10.1016/s1387-6473(00)00030-0 http://dx.doi.org/10.1086/381777 http://dx.doi.org/10.1086/171499 http://dx.doi.org/10.1086/300539 http://dx.doi.org/10.1086/131684 http://dx.doi.org/10.1086/163187 http://dx.doi.org/10.1086/117976 introduction observation and data analysis results discussion and conclusions 123 acta polytechnica ctu proceedings 1(1): 123–126, 2014 123 doi: 10.14311/app.2014.01.0123 a multi-wavelength view of the xmm-newton galactic plane ada nebot gómez-morán1, christian motch1, on behalf of the xmm-newton survey science centre 1observatoire astronomique de strasbourg, université de strasbourg, cnrs, umr 7550, 11 rue de l’université, 67000 strasbourg, france. corresponding author: ada.nebot@astro.unistra.fr abstract we present an x-ray survey of the galactic plane conducted by the survey science centre of the xmm-newton satellite. the survey contains more than 1300 x-ray detections at low and intermediate galactic latitudes and covering 4 deg2 well spread in galactic longitude. from a multi-wavelength analysis, using optical spectra and helped by optical and infrared photometry we identify and classify about a fourth of the sources. the observed surface density of soft x-ray (< 2 kev) sources decreases with galactic latitude and although compatible with model predictions at first glance, presents an excess of stars, likely due to giants in binary systems. in the hard band (> 2 kev) the surface density of sources presents an excess with respect to the expected extragalactic contribution. this excess highly concentrates towards the direction of the galactic centre and is compatible with previous results from chandra observations around the galactic centre. the nature of these sources is still unknown. keywords: stars binaries spectroscopy photometry ir optical x-rays. 1 introduction galactic x-ray surveys can help us to learn about the galaxy’s structure, stellar formation and evolution. since long we know that the soft x-ray emission (< 2 kev) of the galaxy is dominated by stars. but the x-ray luminosity function of hard x-ray emitting sources (>2 kev) is still not well constrained, in particular at low to intermediate x-ray luminosities (10 s ) [s o u rc e s /d e g 2 ] |b| = 0o |b| = 15o |b| = 50o |b| = 60o b = 50º b = 60º b = 15º b = 0º 0.5-2.0 kev observed figure 2: logn – logs curves in the soft band (< 2 kev) and as a function of galactic latitude. we included the data from lopez-santiago et al. 2007 and barcons et al. 2007 at high galactic latitudes. using infrared colour-colour diagrams for the stellar content of our survey we could distinguish main sequence stars from evolved giants. on the one hand, due to magnetic braking, stellar rotation decreases with the age of the stars. on the other hand the x-ray luminosity is strongly related to rotation. this implies that normal old giant stars are not expected to be strong x-ray emitters. a possible explanation for the origin of the x-ray emission of these evolved stars could be if they are in synchronised binary systems, where the rotation period is equal to the orbital period, breaking thus the relation between x-ray emission and age. to test this hypothesis we calculated the x-ray colours expected for stars of different age and for binaries, in particular for rs cvn and by draconis. we found that observed xray and infrared colours for dwarfs are compatible with young to intermediate age stars, while giant stars have colours compatible with rs cvn binaries, i.e. binaries where at least one of the stars is a giant star. the giant stars we find in our survey mostly have k spectral type, i.e. they are “yellow stars”. 4 results we computed the logn – logs curves in the soft band, i.e. the surface density of sources as a function of the sensitivity of our survey, for different bins of galactic latitude. we find that the number of stars per square degree decreases with galactic latitude. although this result is not a surprise, it’s the first time that is shown in x-rays. we also see that the x-ray luminosity function has a varying slope with galactic latitude. we compared our results with the expected curves from a modified version of the galactic x-ray model from guillout et al. 1996. at first glance we obtained compatible results, a varying slope of the x-ray luminosity function and a decreasing number of sources towards higher galactic latitudes, reflecting the different scale-height of stars and the relative contribution of different populations. but for a given flux, the number of observed stars is higher than the predicted value. this result is not surprising since binaries have not been taken into account in our model. in other words, the excess of observed sources with respect to model predictions is due to the yellow giant stars that we have found in our survey, and are likely in binary systems. 10-14 10-13 10-12 10-11 s (2-12 kev) [erg cm-2s-1] 10-1 100 101 102 103 n (> s ) [s o u rc e s /d e g 2 ] galactic center motch et al 2010 1032 1033 1034 luminosity (2-12 kev) [erg s-1] 2-12 kev gc region (l,b) ~ (1º,0º) ‣ ‣ ‣ hands+2004, motch+2010 (l,b) =(20º,0º) b ~ 0º figure 3: logn – logs curves of hard sources (> 2 kev) in the direction of the galactic center. the expected extragalactic contribution from mateos et al. 2008 has been subtracted. we carried out the same exercise for hard sources, we constructed logn – logs curves for sources harder than 2 kev. since stars are not expected to contribute at this high energies, we subtracted the expected extragalactic contribution. the logn – logs curves present an excess of sources with respect to the expected extragalactic contribution close to the galactic center region studied in this survey (l ∼ 0.9◦, b ∼ 0◦). we compared this result with that obtained by motch et al. 2010 at l ∼ 20◦, b ∼ 0◦ and obtained that the number of sources per square degree observed at a given flux decreases steeply with galactic longitude in the direction of the galactic center. we obtained consistent results with hong et al. 2009 based on chandra observations of seven fields around the galactic center. this sources contribute to the galactic ridge emission, initially thought to be of diffuse origin. the nature of these sources is unknown, but if this population would be associated to the galactic center itself, the x-ray luminosities obtained are in the range 1033−1034 erg s−1, i.e. values which are comparable with pre-hmxbs and pre-lmxbs. 125 ada nebot gómez-morán, christian motch acknowledgement we would like to thank the organisers of this conference for their work and for giving us the opportunity to show our results. references [1] anderson l. d., bania t. m., jackson j. m., clemens d. p., heyer m., simon r., shah r. y., rathborne j. m., 2009, apjs, 181, 255 doi:10.1088/0067-0049/181/1/255 [2] barcons, x., carrera, f. j., watson, m. g., et al. 2002, a&a, 382, 522 [3] barcons, x., carrera, f. j., ceballos, m. t., et al. 2007, a&a, 476, 1191 [4] della ceca, r., maccacaro, t., caccianiga, a., et al. 2004, a&a, 428, 383 [5] favata, f., sciortino, s., rosner, r., & vaiana, g. s. 1988, apj, 324, 1010 doi:10.1086/165957 [6] guillout, p., haywood, m., motch, c., & robin, a. c. 1996, a&a, 316, 89 [7] guillout, p., sterzik, m. f., schmitt, j. h. m. m., motch, c., & neuhaeuser, r. 1998, a&a, 337, 113 [8] hands, a. d. p., warwick, r. s., watson, m. g., & helfand, d. j. 2004, mnras, 351, 31 doi:10.1111/j.1365-2966.2004.07777.x [9] hong, j. s., van den berg, m., grindlay, j. e., & laycock, s. 2009, apj, 706, 223 doi:10.1088/0004-637x/706/1/223 [10] lópez-santiago, j., micela, g., sciortino, s., et al. 2007, a&a, 463, 165 [11] lutovinov a., revnivtsev m., gilfanov m., shtykovskiy p., molkov s., sunyaev r., 2005, a&a, 444, 821 [12] mauerhan j. c., muno m. p., morris m. r., stolovy s. r., cotera a., 2010, apj, 710, 706 [13] mateos, s., warwick, r. s., carrera, f. j., et al. 2008, a&a, 492, 51 [14] motch, c., lopes de oliveira, r., negueruela, i., haberl, f., & janot-pacheco, e. 2007, in astronomical society of the pacific conference series, vol. 361, active ob-stars: laboratories for stellare and circumstellar physics, ed. a. t. okazaki, s. p. owocki, & s. stefl, 117 [15] motch, c., warwick, r., cropper, m. s., et al. 2010, a&a, 523, a92 [16] nebot gómez-morán a. et al., 2013, a&a, 553, a12 [17] pfahl, e., rappaport, s., & podsiadlowski, p. 2002, apj, 571, l37 doi:10.1086/341197 [18] sazonov, s., revnivtsev, m., gilfanov, m., churazov, e., & sunyaev, r. 2006, a&a, 450, 117 [19] sciortino, s., favata, f., & micela, g. 1995, a&a, 296, 370 [20] willems, b. & kolb, u. 2003, mnras, 343, 949 discussion david buckley: can you give the percentages of the different optical counterpart types of the ∼ 300 sources identified? ada nebot: among the 316 classified sources there are three t tauri stars, one herbig ae star, two cataclysmic variables, and four γ-cas analogues. a few sources are extragalactic (in the highest galactic latitude fields), and the remaining sources are stars, where about 10% are giants. classification of giants was only done for stars with the best 2mass photometry, meaning that the number of giants in our survey could be higher. 126 http://dx.doi.org/10.1088/0067-0049/181/1/255 http://dx.doi.org/10.1086/165957 http://dx.doi.org/10.1111/j.1365-2966.2004.07777.x http://dx.doi.org/10.1088/0004-637x/706/1/223 http://dx.doi.org/10.1086/341197 introduction xmm-newton survey science centre the galactic plane survey multi-wavelength identification source classification results 293 acta polytechnica ctu proceedings 1(1): 293–297, 2014 293 doi: 10.14311/app.2014.01.0293 design and tests of the hard x-ray polarimeter x-calibur m. beilicke1, r. cowsik1, p. dowkontt1, q. guo1, f. kislat1, s. barthelmy2, t. okajima2, j.w. mitchell2, j. schnittman2, b. zeiger2, g. de geronimo3, m.g. baring4, a. bodaghee5, t. miyazawa6, k.d. finkelstein7, h. krawczynski1 1department of physics and mcdonnell center for the space sciences, washington university, st. louis, mo, usa 2goddard space flight center, md, usa 3brookhaven national lab, ny 4rice university, tx, usa 5uc berkeley, ca 6nagoya university, japan 7cornell university, ny corresponding author: beilicke@physics.wustl.edu abstract x-ray polarimetry promises to give qualitatively new information about high-energy astrophysical sources, such as binary black hole systems, micro-quasars, active galactic nuclei, and gamma-ray bursts. we designed, built and tested a hard x-ray polarimeter, x-calibur, to be used in the focal plane of the infocus grazing incidence hard x-ray telescope. x-calibur combines a low-z compton scatterer with a czt detector assembly to measure the polarization of 20− 60 kev x-rays making use of the fact that polarized photons compton scatter preferentially perpendicular to the electric field orientation; in principal, a similar space-borne experiment could be operated in the 5−100 kev regime. x-calibur achieves a high detection efficiency of order unity. keywords: x-rays polarization black hole infocus x-calibur. 1 introduction motivation. spectral and morphological studies in the x-ray energy band have become established tools to study the non-thermal emission processes of various astrophysical sources. however, many of the regions of interest (black hole vicinities, jet formation zones, etc.) are too small to be spatially resolved with current and future instruments. spectro-polarimetric x-ray observations are capable of providing additional information – namely the fraction and orientation of linear polarization – and would help to constrain different emission models [1, 2] of sources with compact emission regions and high x-ray fluxes such as mass-accreting black holes (bhs) and neutron stars. so far, only a few missions have successfully measured polarization in the soft (oso-8 [3]) and hard (integral [4]) x-ray energy regime. the crab nebula is the only source for which the polarization of the x-ray emission has been established with a high level of confidence [3, 4]. the source exhibits a polarization fraction of 20% at energies of 2.6− 5.2 kev (direction angle of 30◦ with respect to the x-ray jet) [3] and 46% ± 10% above 100 kev (direction aligned with the x-ray jet observed in the nebula). integral observations of the x-ray binary cygnus x-1 indicate a high fraction of polarization in the hard x-ray/gamma-ray bands [5]. model predictions of polarization fraction for various source types lie slightly below the sensitivity of the past oso-8 mission, making future, more sensitive polarimeter missions particularly interesting. future missions. as polarimetry was not the main objective of the integral mission, the results are plagued by systematic uncertainties, and there are currently no other missions in orbit that are capable of making sensitive x-ray polarimetric observations. the situation could be changed by a mission like the gravity and extreme magnetism smex (gems) [6] – using two wolter-type x-ray mirrors to focus 2 − 10 kev photons onto photo-effect polarimeters. for higher energies e > 5 kev x-ray polarimeter designs can make use of the compton effect. the soft gamma-ray imager on astro-h [7] (launch scheduled for 2015) will have capabilities of measuring polarization, but the results may suffer from similar systematic uncertainties as the ones 293 http://dx.doi.org/10.14311/app.2014.01.0293 m. beilicke et al. figure 1: left: incoming x-rays are compton-scattered (scintillator rod, optical axis) and subsequently photoabsorbed in one of the surrounding czt detectors. middle left: ’exploded’ view of the polarimeter: four sides of detector columns surround the central scintillator rod. middle right: polarimeter with csi shield, electronic readout and azimuthal rotation bearing. right: the infocus balloon gondola. measured by integral. the czt imager on astrosat (http://astrosat.iucaa.in/) is expected to be used for polarization measurements in the 150− 250 kev band. the hard x-ray polarimeter x-calibur discussed in this paper has the potential to cover the energy range above 10 kev. furthermore, x-calibur combines a high detection efficiency with a low level of background and has well-controlled systematic errors. these features make it a particularly useful instrument for astronomical x-ray polarimetry. scientific potential. polarization measurements are of general interest as tests of non-thermal emission processes in the universe. synchrotron emission, for example, will result in linearly polarized photons with their electric fields oriented perpendicular to the magnetic field lines (projected) and the observed polarization map in the x-rays can therefore be used to trace the magnetic field structure of the source. an observed polarization fraction close to theoretical limits can be interpreted as an indication of a highly ordered magnetic field since non-uniformities in the magnetic field will reduce the fraction of polarization. the polarized synchrotron photons can be inverse-compton (ic) scattered by relativistic electrons – weakening the fraction of polarization (but not erasing it) and imprinting a scattering angle dependence [8] to the observed fraction of polarization. such ic signals usually (but not always) appear in hard gamma-rays, where polarimetry is difficult, due to multiple scattering in pair production detectors. another important mechanism for polarizing photons is thomson scattering which creates a polarization perpendicular to the scattering plane. curvature radiation is polarized, as well. for more details on the scientific prospects see for example [1] and references therein. addressing these science goals requires spectro-polarimetric observations over the broadest possible energy range. 2 x-calibur design the conceptual design of the x-calibur polarimeter is illustrated in figure 1. a low-z scintillator (ρ ≈ 1 g/cm3) is used as compton-scatterer: the cross section for photoelectric absorption and compton scattering are equal around 15 kev (0.26 cm2/g). at 20 kev the cross section of the photoelectric absorption already drops to 0.1 cm2/g and can be neglected as compared to the compton scattering for higher energies. the mean free path for the compton scattering is ≈ 4 cm so that the length of the scintillator (14 cm) covers ' 3.5 path lengths leading to a p ' 90% probability for absorption in the energy regime of 20 − 60 kev. for sufficiently energetic photons, the compton interaction produces a measurable scintillator signal which is read by a pmt. the scattered x-rays are photo-absorbed in surrounding rings of high-z cadmium zinc telluride (czt) detectors. this combination of scatterer/absorber leads to a high fraction of unambiguously detected comp294 design and tests of the hard x-ray polarimeter x-calibur ton events. linearly polarized x-rays will preferably compton-scatter perpendicular to their e field vector – resulting in a modulation of the azimuthal event distribution. the czt detectors were ordered from different companies (endicott interconnect, quikpak/redlen, creative electron). each detector (2× 2 cm2) is contacted with a 64-pixel anode grid (2.5 mm pixel pitch) and a monolithic cathode facing the scintillator rod. two detector thicknesses (2 mm and 5 mm) will be used. each czt detector is permanently bonded (anode side) to a ceramic chip carrier which is plugged into the electronic readout board. each czt detector is read out by two digitizer boards (32 channel asic developed by g. de geronimo (bnl) and e. wulf (nrl) [9] and a 12-bit adc). the readout noise is as low as 2.5 kev fwhm. 16 digitizer boards (8 czt detectors) are read out by one harvester board transmitting the data to a pc-104 computer with a rate of 6.25 mbits/s. xcalibur comprises 2048 data channels. four detector units form a ’ring’ surrounding the scintillator slab. the scintillator ej-200 is read by a hamamatsu r7600u-200 pmt. the (optional) pmt trigger information allows to effectively select scintillator/czt events from the data, which represent likely compton-scattering candidates. the polarimeter and the front-end readout electronics will be located inside an active csi(na) anticoincidence shield with 5 cm thickness and a passive tungsten shield at the top (fig. 1, middle right) to suppress charged and neutral particle backgrounds. the x-calibur polarimeter will be flown in a pressurized vessel located in the focal plane of the infocus1 x-ray telescope [10] (fig. 1, right). the total mass of the gondola and the x-ray telescope will be 1, 400 kg. a wolter grazing incidence mirror focuses the x-rays on the polarimeter. the x-calibur scintillator rod will be aligned parallel to the optical axis of the infocus x-ray telescope. the focal length is ∼ 8 m and the field of view (fwhm) is 10 arcmin. the design of infocus allows for very stable pointing of the telescopes to <1 arcmin as the focus of the x-ray telescope moves across the sky. in order to reduce the systematic uncertainties of the polarization measurements (including biases generated by the active shield, a possible pitch of the polarimeter with respect to the x-ray telescope, etc.), the polarimeter and the active shield will be rotated around the optical axis (∼ 3 rpm) using a ring bearing (see fig. 1, middle right). a counterrotating mass will be used to cancel the net-angular momentum of the polarimeter assembly during the flight. power will be provided to the polarimeter by sliding contacts and communication will be done via a wireless network. the data will be stored to solid state drives and will be down-linked to the ground. the advantages of the x-calibur/infocus design are (i) a high detection efficiency by using more than 80% of photons impinging on the polarimeter, (ii) low background due to the usage of a focusing optics instead of large detector volumes, and (iii) minimization and control of systematic effects and achievement of a corresponding quantitative estimate thereof. detailed simulations were performed using the geant4 package [11]. an x-calibur balloon flight in the focal plane of the infocus mirror assembly was assumed. for a crab-like source the simulations predict an event rate of 1.1(3.2) hz with (without) requiring a triggered scintillator coincidence detected by the pmt. the x-calibur modulation factor is µ = 0.52 for a 100% polarized beam. the mdp in the 20 − 60 kev energy range will be 4% assuming 5.6 hr of on-source observations of a crab-like source combined with a 1.4 hr background observation of an adjacent empty field. more detailed simulations are discussed in guo et al. (2010) [12]. czt energy [kev] 20 40 60 80 /s ] 2 f lu x[ 1/ cm -310 -210 -110 1 ring1 ring2 ring3 figure 2: energy spectra after compton scattering of a 40/80 kev x-ray beam. vertical lines: incoming beam energy (solid), energy after 90◦ scattering (dashed), and energy after 180◦ scattering (dotted). 3 performance measurements using funding from washington university’s mcdonnell center for the space sciences and nasa grant nnx12ad51g, a flight-ready version of the x-calibur polarimeter was assembled and tested. for energy calibration of the czt detectors a eu152 source is placed inside the individual rings. the calibration data also allow to quantify the energy resolution and threshold on a pixel-by-pixel basis. we find an average resolution of 4.2 kev fwhm at 40 kev. in turn, we completed the full assembly and studied the x-calibur respsonse to incoming x-ray beams. in order to measure the response to a polarized xray beam we operated the x-calibur polarimeter at the 1http://infocus.gsfc.nasa.gov/ 295 m. beilicke et al. cornell high energy synchrotron source (chess) [13]. using bragg reflection from a 2-bounce silicon (220) monochrometer a 40 kev beam was generated (2nd harmonic at 80 kev). the event rates were normalized by azimuthal acceptance on a pixel-by-pixel basis. the acceptance was determined from the response to an unpolarized beam (superposition of two perpendicular polarization planes). the energy spectrum of the compton scattered xray beam is shown in fig. 2. figure 3 shows the azimuthal scattering distribution of the polarized beam (analysis ongoing). the expected 180◦ modulation is clearly seen and the reconstructed orientation of the electric field agrees with the expected direction of the chess beam setup – confirming the functionality of the x-calibur polarimeter. detector x [m] #1 #2 #3 #4 #5 #6 #7 #8 x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x x polarized (acpt) 0 100 200 300 0.5 1 1.5 0 100 200 300 0.5 1 1.5 0 100 200 300 0.5 1 1.5 0 100 200 300 0.5 1 1.5 0 100 200 300 0.5 1 1.5 0 100 200 300 0.5 1 1.5 0 100 200 300 0.5 1 1.5 0 100 200 300 0.5 1 1.5 0 100 200 300 0.5 1 1.5 0 100 200 300 0.5 1 1.5 0 100 200 300 0.5 1 1.5 0 100 200 300 0.5 1 1.5 0 100 200 300 0.5 1 1.5 0 100 200 300 0.5 1 1.5 0 100 200 300 0.5 1 1.5 azimuth angle [deg]0 100 200 300 0.5 11.5polarized (acpt) figure 3: x-calibur measurement of a polarized beam (energy cut: 36 − 40 kev). left: 2d map (pixel-bypixel) of counts. the (blue) boxes indicate the outline of the scintillator. right: azimuthal scattering distribution (corrected for azimuthal acceptance) for different rings. the data are fitted by a sine function. the vertical lines indicate the plane of the e field vector of the polarized beam. 4 discussion and conclusions we designed a hard x-ray polarimeter, x-calibur, and studied its performance and sensitivity. x-calibur combines a detection efficiency of close to 100% with a high modulation factor of µ ≈ 0.5, as well as a good control over systematic effects. x-calibur was successfully tested/calibrated in the laboratory and at the chess x-ray facility [13]. a 1-day x-calibur/infocus balloon flight is funded by nasa (nnx12ad51g) for fall 2013. our tentative observation program includes galactic sources (crab, her x-1, cyg x-1, grs 1915, exo 0331) and one extragalactic source (mrk 421) for which sensitive polarization measurements will be carried through. we envision follow-up longer duration balloon flights (from the southern hemisphere). successful balloon flights would motivate a satellite-borne hard x-ray polarimetry mission. acknowledgement we are grateful for nasa founding from grant nnx10aj56g & nnx12ad51g and discretionary funding from the mcdonnell center for the space sciences to build the x-calibur polarimeter. polarization measurements: this work is based upon research conducted at the cornell high energy synchrotron source (chess) which is supported by the national science foundation and the national institutes of health/national institute of general medical sciences under nsf award dmr-0936384. q.guo thanks the chinese scholarship council from china for the financial support (no.2009629064). references [1] krawczynski, h., et al.: 2011, aph. 34, 550. [2] schnittman, j.d., et al.: 2010, apj. 712, 908. doi:10.1088/0004-637x/712/2/908 [3] weisskopf, m. c., et al.: 1978, apj. 220, l117. doi:10.1086/182648 [4] dean, a. j., et al.: 2008, science. 321, 1183. doi:10.1126/science.1149056 [5] laurent, p., et al.: 2011, science. 332, 438. doi:10.1126/science.1200848 [6] http://heasarc.gsfc.nasa.gov/docs/gems. [7] tajima, h., et al.: 2010, spie 7732, 34. [8] krawczynski, h.: 2012, apj 744, 30. doi:10.1088/0004-637x/744/1/30 [9] wulf, e. a., et al.: 2007, nima 579, 371. doi:10.1016/j.nima.2007.04.085 [10] ogasaka, y, et. al.: 2005, spie 5900, 217. [11] http://geant4.cern.ch/ [12] guo, q, et. al.: 2010, arxiv 1101.0595. [13] http://www.chess.cornell.edu/ 296 http://dx.doi.org/10.1088/0004-637x/712/2/908 http://dx.doi.org/10.1086/182648 http://dx.doi.org/10.1126/science.1149056 http://dx.doi.org/10.1126/science.1200848 http://dx.doi.org/10.1088/0004-637x/744/1/30 http://dx.doi.org/10.1016/j.nima.2007.04.085 design and tests of the hard x-ray polarimeter x-calibur discussion roland walter’s comment: according to the current schedule the flight model of the hard x-ray polarimeter polar (http://www.isdc.unige.ch/polar/) should be delivered to china this year. herman marshall: how is the unpolarized flux generated? perhaps by rotating the polarization plane or by a radioactive source? matthias beilicke: we super-imposed data with the orientation of the polarization plane of 90◦ and 0◦ and independently confirmed the findings with a radiactive source (unpolarized). a 297 introduction x-calibur design performance measurements discussion and conclusions acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0062 acta polytechnica ctu proceedings 4:62–67, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app numerical multigroup transient analysis of slab nuclear reactor with thermal feedback filip osuský∗, branislav vrban, peter ballo, štefan čerba, jakub lüley, gabriel farkas institute of nuclear and physical engineering, faculty of electrical engineering and information technology, slovak university of technology in bratislava, bratislava, slovakia ∗ corresponding author: filip.osusky@stuba.sk abstract. the paper describes a new numerical code for multigroup transient analyses with a thermal feedback. the code is developed at institute of nuclear and physical engineering. it is necessary to carefully investigate transient states of fast neutron reactors, due to recriticality issues after accident scenarios. the code solves numerical diffusion equation for 1d problem with possible neutron source incorporation. crank-nicholson numerical method is used for the transient states. the investigated cases are describing behavior of pwr fuel assembly inside the spent fuel pool and with the incorporated neutron source for better illustration of the thermal feedback. keywords: diffusion equation, neutronics, transient state, crank-nicholson method, thermal feedback. 1. introduction nuclear reactors are most reliable source of energy at present time. the advantage of new fast neutron reactor concepts is the possibility of the transmutation of the 238u into the fissionable 239pu, so the worldwide resources of fissionable materials could be enlarged when the fast neutron reactors will be commercialized. however, it is necessary to carefully investigate the transient states of these new concepts, because the recriticality after accident scenario may be achieved [1]. for this purpose, a new numerical code has been developed within the frame of neutronic calculation group at the institute of nuclear and physical engineering (inpe). the code has been used as the basic step in understanding of transient state and fast reactor r&d and we refer to it as transos. the transos code is able to solve a time dependent neutron flux distribution of slab systems with respect to the thermal feedback in multigroup approximation. the power method with infinity norm (manhattan norm) is used for a calculation of stationary state [2]. the transient state is calculated by the crank-nicholson numerical method [3]. it is possible to define the geometry in the form of coarse mesh intervals with material parameters assigned to each of the mesh interval. point and linear neutron sources can be incorporated to the design with different fluency for each investigated energy group of neutrons. the boundary conditions have to be specified in conjunction with design parameters such as temperature of the system and power generation rate. initial state of neutron flux should be given for successful run. the developed code can be used for academic purposes at the faculty and for investigation of simple systems. this paper follows the previous work [4] and next sections describe calculation methodology of time dependent and in-dependent solution, accuracy of the methodology and analysis of two nuclear systems with different 235u enrichment. higher impact of the thermal feedback can be observed on microscopic cross section properties for low energy neutron interaction with matter, so the thermal systems are investigated to show this effect. 2. calculation methodology 2.1. stationary state (time in-dependent solution) the code solves common neutron diffusion equation with internal sources for the stationary state given by [5] dg∆φg − σa,gφg − ∑ h σg→hφg+ + ∑ h σh→gφh + χg ∑ h νσf,hφh = 0. (1) lower index g in all equations represents the neutron energy group and d stands for the associated diffusion coefficient. the first term represents the leakage of neutrons from the system, the second term represents absorptions (radiation capture), the third represents scattering from the group to another group h, the fourth represents contributions of scattering from another group and the last term describes the contribution of fission source to specified energy group (χg is the proportion of neutrons emitted by fission in group g, ν is an average yield of neutrons from the fission). the box scheme was used for the discretization of examined area and therefore (1) can be written in a numerical form (2) for two energy groups 62 http://dx.doi.org/10.14311/ap.2016.4.0062 http://ojs.cvut.cz/ojs/index.php/app vol. 4/2016 numerical analysis of slab nuclear reactor with thermal feedback of neutrons [2, 4], −d̃k−1 g φk−1 g + ( d̃k−1 g +d̃k g +σkrghk ) φk−d̃k gφ k+1 g = = λχkghk ( 2∑ g′=1 νσkfg′φkg′ ) + hk ( 2∑ g′=1 g′ 6=g σks,g′gφ k g′ ) , (2) where σr represents the removal macroscopic cross section (3), k represents spatial node, hk is the length of the spatial interval, λ stands for the fundamental eigenvalue, σf is the fission macroscopic cross section, σs is the scattering macroscopic cross section between energy groups of neutrons, and d̃ arbitrary coupling coefficient (3) [2]. σkrg = σkag + 2∑ g′=1 g′ 6=g σks,gg′ d̃k k = 2 dk g hk dk+1 g hk+1 dk g hk + dk+1 g hk+1 (3) 2.2. transient state (time dependent solution) 2.2.1. crank-nicholson numerical method the crank-nicholson method is often applied to the diffusion problems and achieves good numerical stability for the transient states. the finite difference method is used as for the stationary state. this method is able to solve heat equation and similar partial differential equations [3] m ∂2u(x, t) ∂x2 = ∂u(x, t) ∂t , (4) where m represents material parameters and u is solution of the differential equation. applying the finite difference method, the central node of the common diffusion equation can be rewritten numerically for the transient state as − m̃k−1ht 2hk uk−1,j − m̃kht 2hk uk+1,j + ( 1 + m̃k−1ht 2hk + m̃kht 2hk ) uk,j = m̃k−1ht 2hk uk−1,j+1 + m̃kht 2hk uk+1,j+1 + ( 1− m̃k−1ht 2hk − m̃kht 2hk ) uk,j+1 + f(hk), (5) where the index k represents spatial node, index j represents step time ( u ·,j stands for initial condition of the function at present time step, u ·,j+1 is initial condition of the function at next time step), the hk length of the spatial interval, ht length of the time interval, f(hk) is increment of the function u (particular solution). the variables and unknowns from (5) can be rewritten in the form (6) for the neutron diffusion equation (1) and (2). − d̃k−1 g ht 2hk φk−1,j g − d̃k ght 2hk φk+1,j g + ( 1 + d̃k−1 g ht 2hk + d̃k ght 2hk ) φk,jg = d̃k−1 g ht 2hk φk−1,j+1 g + d̃k ght 2hk φk+1,j+1 g + ( 1− d̃k−1 g ht 2hk − d̃k ght 2hk ) φk,j+1 g + χkght ( 2∑ g′=1 νσkfg′φ k,j g′ ) − σkrghtφk,jg + ht ( 2∑ g′=1 g′ 6=q σks,g′gφ k,j g′ ) + sght, (6) where the last term s represents the external neutron source. the heat diffusion equation k ρc ∂2t (x, t) ∂x2 + q̇ = ∂t (x, t) ∂t (7) can be similarly rewritten to [6] − k̃k−1ht 2hk t k−1,j − k̃kht 2hk t k+1,j + ( 1 + k̃k−1ht 2hk + k̃kht 2hk ) t k,j = k̃k−1ht 2hk t k−1,j+ + k̃kht 2hk t k+1,j+1 + ( 1− k̃k−1ht 2hk − k̃kht 2hk ) t k,j+1 + ( 2∑ g′=1 σkfg′φ k,j g′ ) e ht ρkck e, (8) where k̃k = 2 kk kkρkck kk+1 kk+1ρk+1ck+1 kk kkρkck + kk+1 kk+1ρk+1ck+1 , and where k represents material conductivity, ρ is material density, c stands for material heat capacity, q̇ is power generation, t stands for temperature, e is an average released energy per fission in ev and parameter e is an electron charge. accuracy of the above mentioned method is discussed in the next subsection. 2.2.2. accuracy of the crank-nicholson method the accuracy of the method for the initial and boundary conditions (more in section 3) is presented in fig. 1. the analytical solution of the differential equation for a homogenous slab system is sinus, so the problem can be approximated by function f(x) f(x) = a sin(bx) + c. 63 filip osuský, branislav vrban, peter ballo et al. acta polytechnica ctu proceedings figure 1. accuracy of crank-nicholson method. in this case, the whole system is homogeneous subcritical nuclear system. it is necessary to insert the external neutron source because the neutron flux will never stabilize on non-zero value without it. the external neutron source is linear, located between 217–227mm, with fluency 1.0× 106 s−1 in thermal energy spectrum. deviations between the modeled problem and analytical solution are presented in table 1. parameter mean value dispersion rel. error a 111 935 126.1 0.1127 % b 7.076 99 × 10−3 2.015 × 10−6 0.028 47 % c −785.941 97.17 12.36 % table 1. deviation between numerical and analytical solution. amplitude (a) and shape parameter (b) are in accordance with the analytical solution (table 1). deviance in location parameter (c) is caused by the external neutron source and by zero flux boundary condition. 3. geometry of the nuclear slab system the investigated geometry represents middle cut of one heterogenic vver440 fuel assembly that is placed in the middle. one edge of the investigated geometry is represented by homogenous representation of the heterogeneous fuel assembly. control rod assembly is placed on the opposite edge. this case was introduced due to simulation of the transient state during operational conditions. geometry is also simplified into one dimension and some lengths are changed for faster convergence of numerical calculation (fig. 2). red material represents uo2 (dimension d1 is 7 mm and is the same for every red and orange material). orange material is the representation of uo2 with 3.35 % of 153gd. the two cases of the enrichment are investigated (table 2). green is b4c (dimension d5 is 142 mm), figure 2. graphical representation of investigated nuclear reactor core. enrichment material case 1 case 2 uo2 5 % 22 % uo2 + 153gd 4.4 % 21.4 % table 2. enrichment of uo2. blue stands for h2o (dimension d2 is 5 mm, d3 = 19 mm, d4 = 10 mm). purple is a mixture of the whole area between x–y points (d5 is 142 mm). all cross sections are obtained from endf/b-vii.1 library for the temperatures of 296.3 k, 600 k and 1800 k, for the discrete energies of 0.0253 ev and 2 mev [7]. isotropic scattering is assumed and the diffusion coefficient can be calculated according to (9) [8], where σt stands for the total macroscopic cross section, σtr is the transport macroscopic cross section, and µ̄0 represents unsymmetrical parameter of neutron scattering (if 64 vol. 4/2016 numerical analysis of slab nuclear reactor with thermal feedback isotropic scattering is applied µ̄0 = 0). in this case, a molecular cross section of h2o is not considered, even if the molecular cross section is higher than calculated cross sections of particular nuclides [8]. d ' λtr 1 3 = 1 3σtr = 1 3 ( σt − µ̄0σs ) ≈ 1 3σt . (9) more details about geometry input can be found in [4]. it is necessary to note that this is the only theoretical approximation and that it is mainly because the values of the macroscopic scattering cross section were simplified with certain degree of uncertainty. 4. initial and boundary conditions the zero incoming current boundary condition is used in all cases of the neutron diffusion α = j φ = 0.5, where j is the neutron current and φ is the neutron flux. this can be interpreted as that the environment behind the boundary of the nuclear system is vacuum. according to (2), the stationary state is represented by proportional neutron flux distribution that is normed to maximal value 1. it is necessary to set the initial condition in the form of total power generation p = ∫ v e ( 2∑ g′=1 σfg′φg′ ) edv. (10) the absolute value of the neutron flux distribution is calculated from the proportional neutron flux distribution (2) and from the initial power generation condition (10). the power generation rate is calculated for the case 1 from the typical power generation of vver reactor (1375 mwth) and it is approximately 1.576 kw/m per the assembly p [w/m] = pth assembly nr ·height = = 1375× 106 349 · 2.5 = 1576, where assmebly nr is the total number of fuel assemblies in the reactor and height represents height of the core. the power generation rate is the same for the case 2 with higher enrichment to lower impact of the thermal feedback to ensure the nuclear system’s subcritical state. temperature is kept at constant 296.3 k at the boundaries that correspond to dirichlet boundary condition. temperature of the whole system is also set to 296.3 k before the transient for all cases. no thermo-mechanical physics is applied (the densities of the particular materials are constant). also no fluid mechanics is applied (the heat diffusion equation solves just thermal conduction equation) and this simplification results in total temperature increase of the whole nuclear system. 5. results 5.1. case 1 keff = 0.282 601 is calculated from the stationary state of trnasos code for this scenario. this condition may be achieved in spent fuel pool. the worst case is simulated by the neutron flux corresponding to the operational state before the transient (the power generation is 1.576 kw/m). it is possible to observe (fig. 3) that the thermal energy spectrum of neutrons decreases rapidly due to deep subcritical state of the nuclear system. the same evolution can be seen in case of fast energy spectrum of neutrons in fig. 4. the temperature is set to 296.3 k at the beginning of the transient state. the power is generated by (10) according to the neutron flux and the temperature evolution is shown in fig. 5. the temperature increases up to 460 k and according to the temperature change, the microscopic cross sections are modified. the whole system is below melting point temperature of the fuel. figure 3. neutron flux distribution for energy group 0.0253 ev in case 1 (the neutron flux decreases with time evolution due to deep subcritical state). figure 4. neutron flux distribution for energy group 2 mev in case 1 (the neutron flux decreases with time evolution due to deep subcritical state). 65 filip osuský, branislav vrban, peter ballo et al. acta polytechnica ctu proceedings figure 5. temperature evolution in case 1 with keff = 0.282601 (the temperature decreases with time evolution – the nuclear system is brought into safeconditions). 5.2. case 2 the keff is equal to 0.982 693 in this case, due to higher enrichment of 235u (table 2). the neutron source is incorporated within the core and its total emission of neutrons is 1.1× 106 s−1 in the area between 217–227mm on x-axis. it corresponds to the concept of super-thermal liquid-helium (4he) source (ucn) [9] and portion of 1.0× 106 s−1 is in the thermal energy spectrum. subcritical multiplication can be derived from n∞ = s 1 1− keff = 1.1× 106 1 1− 0.982 693 ≈ 108. the result of subcritical multiplication formula is consistent with the calculated results that are shown in fig. 6 and fig. 7. the whole system starts from zero power level. the transient state of the neutron flux is stabilized approximately after 50 000 s. however, the transient of the temperature evolution is represented by higher inertia and the transient state is stabilized in the region of 140 000 s (fig. 8). the temperature does not exceed 380 k. figure 6. neutron flux distribution for energy group 0.0253 ev in case 2 (nuclear system is stabilized after subcritical multiplication for keff = 0.982 693). figure 7. neutron flux distribution for energy group 2 mev in case 2 (nuclear system is stabilized after subcritical multiplication for keff = 0.982 693). figure 8. temperature evolution in case 2 (temperature is stabilized below melting point of fuel material for keff = 0.982 693). 6. conclusions the successful application of the transos code was demonstrated. it has been found that the maximum value of the neutron flux and its temperature is located in the middle of the system within the heterogeneous region. on the other hand, the diffusion theory is more appropriate for the homogenous problems and calculation error increases with greater heterogeneity. in all cases, the temperature does not exceed melting point of fuel material. the code that was written in c++ can be used for academic purposes at the institute and for solution of simple nuclear systems. it has been confirmed that the diffusion theory is suitable for fast calculations and it is used during development of theoretical reactor design. therefore, development of simple codes increases the knowledge level of neutron physics and it can result in enhancing of nuclear safety. the contribution of 238u thermal feedback with thermo-hydraulic properties of the system has to be investigated in the future. acknowledgements this work was financially supported by grant of science and technology assistance agency no. apvv-0123-12 and stu grant scheme for support of young researchers. 66 vol. 4/2016 numerical analysis of slab nuclear reactor with thermal feedback references [1] h. ninokata, t. sawada, h. tomozoe, et al. a study on recriticality characteristics of fast reactors in pursuit of recriticality-accident-free concepts. progress in nuclear energy 29:387–393, 1995. doi:10.1016/0149-1970(95)00067-t. [2] j. han-gyu. solution of one-dimensional, one-group neutron diffusion equation, lecture note 1. seoul national university, reactor physics laboratory, 2008. [3] p. b. patil, u. p. verma. numerical computational methods. alpha science international, ltd, 2006. [4] f. osuský, b. vrban, š. čerba, et al. two-group numerical analysis of one dimensional table nuclear reactor. in proceedings of the 20th international conference on applied physics of condensed matter (apcom2014), pp. 320–323. 2014. [5] p. reuss. neutron physics. edp sciences, 2008. [6] m. kalousek, b. hučko. prenos tepla. vydavateľstvo stu, bratislava, 1996. [7] nuclear data services. point2015 data. temperature dependent endf/b-vii.1 cross section data, https://www-nds.iaea.org/point/. [8] j. r. lamarsh. introduction to nuclear reactor theory. amer nuclear society, 2002. [9] e. lychagin, v. mityukhlyaev, a. muzychka, et al. ucn sources at external beams of thermal neutrons. an example of pik reactor. nuclear instruments and methods in physics research section a: accelerators, spectrometers, detectors and associated equipment 823:47–55, 2016. doi:10.1016/j.nima.2016.04.008. 67 http://dx.doi.org/10.1016/0149-1970(95)00067-t https://www-nds.iaea.org/point/ http://dx.doi.org/10.1016/j.nima.2016.04.008 acta polytechnica ctu proceedings 4:62–67, 2016 1 introduction 2 calculation methodology 2.1 stationary state (time in-dependent solution) 2.2 transient state (time dependent solution) 2.2.1 crank-nicholson numerical method 2.2.2 accuracy of the crank-nicholson method 3 geometry of the nuclear slab system 4 initial and boundary conditions 5 results 5.1 case 1 5.2 case 2 6 conclusions acknowledgements references 194 acta polytechnica ctu proceedings 1(1): 194–199, 2014 194 doi: 10.14311/app.2014.01.0194 multi-wavelength view of supernova remnants manami sasaki1 1institute for astronomy and astrophysics, eberhard karls university tübingen, sand 1, d-72076 tübingen, germany corresponding author: sasaki@astro.uni-tuebingen.de abstract this contribution gives a very short overview on the emission of supernova remnants and the processes that are responsible for both the thermal and non-thermal origins of the emission, typically observed in radio, x-rays, and up to γ-rays. we discuss in particular the case of the galactic snr ctb 109. as detailed x-ray studies combined with observations in radio have shown, ctb 109 is interacting with a giant molecular cloud complex. the interaction of the snr shock with dense interstellar clouds is responsible for both the unusual semi-circular morphology of the snr and the bright x-ray feature inside the snr, and, as has been shown recently, seems also to play a major role in the production of γ-rays. keywords: supernova remnants radio ir optical x-rays γ-rays. 1 introduction supernova remnants (snrs) are objects that are formed by a supernova (sn) explosion at the end of the life of a star. owing to the shock waves of the sn explosion, the stellar ejecta as well as the ambient medium is heated to temperatures higher than a million kelvin. therefore, snrs are responsible for the heating of the interstellar medium (ism) and the distribution of heavier elements that were processed inside a star. in addition, both electrons and nuclei can be accelerated in the shock waves of the snrs to relativistic energies. therefore, snrs are also considered to be one source of galactic cosmic rays. by now, about 280 snrs are known in our galaxy and about 50 in the magellanic clouds. detailed studies of snrs in the galaxy and the magellanic clouds allow us to understand the nature of their shocks, the various radiation processes that are responsible for the complex emission observed over the full electromagnetic spectrum from radio to γ-rays, the interaction of the shock with the cooler, and often inhomogeneous ism, and the acceleration of particles. 2 snrs at lower energies 2.1 radio emission in the strong shock waves of snrs, electrons are accelerated and interact with the interstellar magnetic fields. these electrons emit synchrotron radiation and thus make the snr bright in radio. the distribution of the surface brightness of the electron synchrotron emission in snrs can be obtained from radio imaging observations. in general, the radio emission consists of narrow shell-like or filamentary emission and additional diffuse emission. the reason for these two kinds of synchrotron emission is that particles with higher energies lose their energy faster through synchrotron emission than those with lower energies. the long-lived lower-energy particles can diffuse further away from the shock and radiate over a much wider area, producing the more extended diffuse emission with a steeper spectrum. figure 1: radio continuum emission from snr da 530 (1420 mhz) in contour representation (left) and gray scale (right). vectors in the left image show the polarized intensity by their length and the direction of the e-field by their orientation (landecker et al., 1999). since synchrotron emission is polarized, radio observations can reveal the magnetic field structure in and around snrs. observations have shown that young remnants in general have a radial field structure. for remnants in the free expansion phase and in the early phases of the adiabatic expansion, radial motions due 194 http://dx.doi.org/10.14311/app.2014.01.0194 multi-wavelength view of supernova remnants to rayleigh-taylor instabilities at the contact discontinuity between the shocked ejecta and the shocked ism can enhance the radial magnetic fields. on the contrary, older remnants have a more tangential field structure with higher polarized fractions (milne, 1987). the polarized fraction in younger remnants are typically p = 10− 15%, while older remnants like snr da 530 can have a polarized fraction of p = 50% (fig. 1, landecker et al., 1999). 3 thermal x-ray emission the outward moving shock wave of an snr heats the interstellar medium, while the reverse shock that propagates inward heats the ejecta of the sn explosion. as a whole the ionized gas inside an snr has temperatures of ∼ 106−7 k typically. in plasmas the excitation and ionization of the atoms are mainly induced by electrons that collide with ions. snrs have very low densities and thus are optically thin. they can be considered to be out of thermal and ionization equilibrium, especially when they are still young. if the time after the plasma has been shocked is short, only a few collisions have occurred that cause ionization. the ionization states of the ions at a given temperature are thus lower than in the case of collisional ionization equilibrium (cie). instead, the plasma in snrs is characterized by non-equilibrium ionization (nei). the shape of the continuum of the thermal plasma is primarily determined by the electron temperature, while the temperature of ions might be different than that of electrons. the line emission in the x-ray band can be used to derive the ionization states of the ions as well as the element abundances. therefore, the x-ray spectrum can, on the one hand, reveal the element distribution in the ejecta, and on the other hand, the typical abundances of the ism in which the snr expands. 3.1 charge exchange newer observations of snrs in x-rays have revealed spectral features indicating charge exchange (cx) between the hot thin plasma of an snr and the cold interstellar gas. x-ray emission from cx can in principle be produced at any astrophysical site where hot plasma interacts with (partially) neutral gas, and was originally discoverd in x-ray data of comets (lisse et al., 1996, cravens, 1997). first observational evidences of cx in snrs had been obtained as a broad component of hα emission (e.g., chevalier et al., 1980). observations of the rim of the cygnus loop using suzaku and xmmnewton have revealed a significant emission feature at 0.7 kev, which was identified to be a complex of he-like o k(γ + δ + ε) and was interpreted as cx emission from interaction between he-like o and neutrals (fig. 2, katsuda et al., 2011). figure 2: non-x-ray background subtracted spectrum of a northeastern region of the cygnus loop snr taken with suzaku along with the best-fit model consisting of a bremsstrahlung plus gaussians (katsuda et al., 2011). line identifications are given on top of the upper panel. the gaussian shown in red represent the cx emission. the x-ray background components are shown in green. 3.2 overionization new suzaku observations of mixed-morphology (mm) snrs in the last few years have shown that in many cases the thermal x-ray emission can be interpreted as that from an overionized, recombining plasma in ionization non-equilibrium (e.g., yamaguchi et al., 2009, see fig. 3). mixed-morphology snrs, also called thermalcomposite remnants, are usually found in dense regions near molecular clouds and show very little or no shell emission. the x-ray emission is bright in the (projected) interior and is of thermal nature. the signature of an overionized plasma is a radiative recombination continuum (rrc) and strong ly emission of, e.g., si, s, or fe. in general, snrs are underionized and the shocked plasma slowly develops to ionization equilibrium. therefore, it is rather surprising to observe overion195 manami sasaki ization in snrs. to reach overionization in a plasma above ∼ 106 k, electrons have to cool rapidly. possible processes for such a cooling are either fast expansion, thermal conduction, or radiative cooling with enhanced abundances, which are all processes that are likely to occur in particular in snrs evolving in significantly inhomogenous ism. figure 3: suzaku xis spectrum in the 1.75 – 6.0 kev band (black: fi, red: bi). the best fit model is shown including the cxb (black) and vapec and gaussians for the source emission. rrc emisison of h-like mg, si, and s are shown in magenta (yamaguchi et al., 2009). 4 snrs as particle accelerators 4.1 non-thermal x-ray emission supernova remnants are non-thermal, extended radio sources with a flux spectrum described by a power-law with sν ∝ να with α ≈ −0.5. the synchrotron radiation is emitted by a non-thermal population of relativistic electrons, which can be described by a powerlaw. synchrotron emission in radio indicates that there are electrons with energies in the gev range in the snr shell. synchrotron emission from an snr in the x-ray band was confirmed for the first time for the remnant of sn 1006 (koyama et al., 1995) based on asca data, which showed that the non-thermal emission is dominating the emission of two outer shell regions. soon after, more snrs were also confirmed to radiate non-thermal x-ray emission: cas a (e.g., the et al., 1996, allen et al., 1997), rx j1713.7-3946 (g347.30.5, pfeffermann & aschenbach, 1996), rx j0852.04622 (g266.2-1.2, vela jr, aschenbach 1998). the xray emission of rx j1713.7-3946 and rx j0852.0-4622 is completely of non-thermal nature with no thermal emission detected so far. x-ray synchrotron emission is only observed in younger snrs and is indicative of electrons with energies of up to 1014 ev. the angular resolution of the newer x-ray telescopes, in particular that of the chandra x-ray observatory, made it possible to reveal narrow filaments of non-thermal x-ray emission close to the outer shock in several young snrs: sn 1006, rx j1713.7-3946, rx j0852.0-4622, cas a, tycho, and kepler. these filaments are very thin (∼ 1 − 2′′) and indicate relatively high magnetic fields (b = 100 − 600µg). recently, a deep chandra observation of tycho’s snr revealed bright non-thermal stripes, clearly seen in the energy band of > 4kev (fig. 4, eriksen et al., 2011). the stripes are likely caused by peaks in magnetic fields. figure 4: chandra image of the tycho’s snr in the energy band of 4.0 – 6.0 kev. the boxes show the regions with stripes or filaments of non-thermal emission (eriksen et al., 2011). 4.2 gamma-ray emission in the last decade some snrs have been detected with γ-ray observatories and are now well established astrophysical γ-sources. there are two major origins of γ-ray emission in snrs: • leptonic: interactions of relativistic electrons with low-energy photons of the cosmic microwave background cause inverse compton up-scattering of the photons. in addition, the non-thermal electrons will also emit bremsstrahlung through interactions with ions in the snr. • hadronic: accelerated nuclei can produce γray emission if they collide with atomic nuclei, thereby creating, among others, neutral π0s, which decay into γ-ray photons. this is believed to be enhanced in snrs near high-density clouds where the probability for the collision of the accelerated protons from the snr with cold protons or nuclei is higher (e.g., ic 443, w44, see fig. 5). the gev and tev emission of snrs can thus give us a direct view of the accelerated particles. 196 multi-wavelength view of supernova remnants figure 5: gamma-ray spectra of the snrs ic 443 and w44 and fitted models (ackermann et al., 2013). 5 the galactic snr ctb 109 the galactic supernova remnant ctb 109 (g109.1– 1.0) is the host of the anomalous x-ray pulsar (axp) 1e 2259+586 (fahlman & gregory, 1981) and has an interesting semi-circular morphology in both the x-ray and the radio. it is believed to be located next to a giant molecular cloud (gmc) complex and is thus one of the most striking examples of an interaction of an snr with a molecular cloud. the snr was discovered in x-rays with einstein by gregory & fahlman (1980). hughes et al. (1981) identified the radio counterpart in the galactic plane survey at 49 cm with the westerbork synthesis radio telescope. its shell is incomplete on the western side both in x-rays and in radio. the semi-circular radio and x-ray morphology of ctb 109 suggests the shock has been stopped by the gmc complex in the west. an elongated feature in co (‘co arm’) extends from the gmc complex to an x-ray minimum inside the snr in the north (tatematsu et al., 1987), indicating that a part of the dense gas of the gmc complex extends in front of the remnant. we performed observations of the entire snr ctb 109 with xmm-newton using the european photon imaging cameras (epics). a mosaic of all observations is shown in fig. 6. as mentioned before, ctb 109 seems to have expanded into a dense medium in the west, while the shock wave is expanding into a lowerdensity medium in the east. the radii of the northern and the southern periphery of ctb 109 are slightly smaller than to the east suggesting that ctb 109 is confined by denser material also in the north and the south. however, the relative difference is only ∼5 – 10%. therefore, the overall shape of the shell can be considered as a semi-sphere. there is an x-ray bright interior region known as the lobe, which is brighter than any part of the snr shell. the x-ray spectrum from the lobe obtained with xmm-newton is completely thermal (sasaki et al., 2004). we found co clouds around the lobe in new high-resolution co data from the five college radio observatory (sasaki et al., 2006). one of the co clouds overlaps with the lobe and has an additional component towards higher negative velocities in the velocity profile. we believe that the bright x-ray emission of the lobe is the result of the interaction of the snr shock with a dense molecular cloud, which was hit by the blast wave on the western side. the main part of the cloud was heated and is now visible as the lobe, while some denser parts might have survived. figure 6: mosaic rgb image of the snr ctb 109 created from the xmm-newton observations: red = 0.3 – 0.9 kev, green = 0.9 – 1.5 kev, blue = 1.5 – 4.0 kev (sasaki et al., 2004). 197 manami sasaki 0 0.5 1 1.5 2 2.5 3 3.5 4 4.5 5 vnei+vnei fe (0.0 5.0 x solar) 0 0.5 1 1.5 2 2.5 3 3.5 4 4.5 5 vnei+vnei abund. (0.0 5.0 x solar) 1 1.2 1.4 1.6 1.8 2 2.2 2.4 2.6 2.8 3 vnei+vnei si significance (1 3 ) 0 0.5 1 1.5 2 2.5 3 3.5 4 4.5 5 vnei+vnei si (0.0 5.0 x solar) 1 1.2 1.4 1.6 1.8 2 2.2 2.4 2.6 2.8 3 vnei+vnei fe significance (1 3 ) (b) (d) (e) (c)(a) figure 7: best fit abundances obtained for the emission of snr ctb 109 from the analysis of the chandra acis spectra by assuming a thermal model that consists of two vnei components for thermal non-equilibrium plasma for the shocked ism and for the shocked ejecta (sasaki et al., 2013). the shown parameters are: abundances for elements other than si, s, and fe fitted for the ejecta emission (a), si abundance fitted for the ejecta emission (b) and its significance calculated as (abundance of the si – abundance of the other elements)/error of the abundance of si (c), fe abundance and its significance (d and e, respectively). through the analysis of a deep, high-resolution data of the region around the lobe taken with chandra advanced ccd imaging spectrometer (acis), we discovered ejecta emission inside the snr west of the lobe (sasaki et al., 2013). the distriubtion of the siabundance and fe-abundance are shown in in fig. 7. these images show the parameter values obtained from the analysis of the spectra extracted in the regions indicated. the abundances measured for the ejecta emission are all comparable to or lower than solar values, except for the lobe. here, the si and fe abundances are in particular significantly higher. the enhanced abundances in the lobe suggest that there is an ejecta clump or a conglomeration of an ejecta clump and a shocked cloud. at the position of ctb 109 a gev source was detected with fermi (castro et al., 2012, see fig. 8). this γ-ray source is located southwest of the lobe where the snr appears dark in x-rays and thus is most likely highly absorbed. castro et al. (2012) performed a comprehensive modeling of the emission of ctb 109, in which they could reproduce the fluxes in radio, x-rays, and γ, as well as the x-ray spectrum taken with the xmm-newton epic in a model including a significant contribution by π0-decay. this is again consistent with the picture that there is significant interaction between the snr shock and a dense interstellar cloud. 6 summary being driven by strong shock waves formed in supernova explosions, supernova remnants are one of the main drivers of the matter cycle and dynamic evolution of galaxies. they are responsible for the chem198 multi-wavelength view of supernova remnants ical enrichment of galaxies. the shock waves create new structures in the ism by forming a cavity filled with hot thin gas and sweep the colder gas around it. particles are accelerated in the shock waves and their emission is observed over the entire range of the observable electromagnetic spectrum. in recent years observations of x-ray synchrotron radiation confirmed the existence of electrons with energies in the tev range in snr shocks. newest gev and tev obervations indicate inverse compton scattering as well as pion-decay processes in and around snr shocks. self-consistent modeling of the spectrum from radio to tev as in the case of the galactic snr ctb 109 helps us to understand both the heating and acceleration processes in snr shocks. figure 8: smoothed fermi-lat count maps in the range 2 – 200 gev (castro et al., 2012). white contours show the x-ray emission (0.5 – 5.0 kev) from xmm-newton data. acknowledgement m.s. acknowledges support by the deutsche forschungsgemeinschaft through the emmy noether research grant sa 2131/1. references [1] ackermann, m., et al. 2013, science, 339, 807 doi:10.1126/science.1231160 [2] allen, g. e., et al. 1997, apjl, 487, 97 [3] aschenbach, b. 1998, nature 396, 141 doi:10.1038/24103 [4] castro, d., slane, p., ellison, d. c., patnaude, d. j. 2012, apj, 756, 88 doi:10.1088/0004-637x/756/1/88 [5] chevalier, r. a., kirshner, r. p., raymond, j. c. 1980, apj, 235, 186 [6] cravens, t. e. 1997, geophys. res. lett., 24, 105 [7] eriksen, k. a., et al. 2011, apjl, 728, 28 doi:10.1088/2041-8205/728/2/l28 [8] fahlman, g. g. & gregory, p. c. 1981, nature, 293, 202 doi:10.1038/293202a0 [9] gregory, p. c. & fahlman, g. g. 1980, nature, 287, 805 doi:10.1038/287805a0 [10] hughes, v. a., harten, r. h., costain, c. h., van den bergh, s. 1981, apj, 246, l127 doi:10.1086/183568 [11] [12] katsuda, s., et al. 2011, apj, 730, 24 doi:10.1088/0004-637x/730/1/24 [13] koyama, k., et al. 1995, nature, 378, 255 doi:10.1038/378255a0 [14] landecker, t. l., et al. 1999, apj, 527, 866 [15] lisse, c. m., et al. 1996, science, 274, 205 doi:10.1126/science.274.5285.205 [16] milne, d. k., 1987, aujph, 40, 771 [17] pfeffermann, e., aschenbach, b. 1996, proc. of ‘röntgenstrahlung from the universe’, 267 [18] sasaki, m., kothes, r., plucinsky, p. p., gaetz, t. j., brunt, c. m. 2006, apj, 642, l149 doi:10.1086/504844 [19] sasaki, m., et al. 2004, apj, 617, 322 [20] sasaki, m., plucinsky, p. p., gaetz, t. j., bocchino, f. 2013, a&a, 552, 45 [21] tatematsu, k., et al. 1987, a&a, 184, 279 [22] the, l.-s., et al. 1996, a&as, 120, 357 [23] yamaguchi, h., et al. 2009, apjl, 705, 6 doi:10.1088/0004-637x/705/1/l6 discussion carlotta pittori’s comment: to distinguish between ic and π0 decay in the gev range, at least in some cases like w44, the new planck data combined with agile and fermi data are very much constraining. the mw picture in the case of middle-aged snrs interacting with molecular clouds seem to largely favour the hadronic scenario (π0 decay). 199 http://dx.doi.org/10.1126/science.1231160 http://dx.doi.org/10.1038/24103 http://dx.doi.org/10.1088/0004-637x/756/1/88 http://dx.doi.org/10.1088/2041-8205/728/2/l28 http://dx.doi.org/10.1038/293202a0 http://dx.doi.org/10.1038/287805a0 http://dx.doi.org/10.1086/183568 http://dx.doi.org/10.1088/0004-637x/730/1/24 http://dx.doi.org/10.1038/378255a0 http://dx.doi.org/10.1126/science.274.5285.205 http://dx.doi.org/10.1086/504844 http://dx.doi.org/10.1088/0004-637x/705/1/l6 introduction snrs at lower energies radio emission thermal x-ray emission charge exchange overionization snrs as particle accelerators non-thermal x-ray emission gamma-ray emission the galactic snr ctb 109 summary 222 acta polytechnica ctu proceedings 1(1): 222–226, 2014 222 doi: 10.14311/app.2014.01.0222 x-ray and near-infrared spectroscopy of dim x-ray point sources constituting the galactic ridge x-ray emission kumiko morihana1, masahiro tsujimoto2, ken ebisawa2 1nishiharima astronomical observatory, center for astronomy, university of hyogo, 407-2 nishigaichi, sayo-cho, sayogun, hyogo, 679-5313, japan 2japan astrospace exporation agency, institute of space and astronautical science, 3-1-1 yoshino-dai, chuo-ku, sagamihara, kanagawa 252-5210, japan corresponding author: morihana@nhao.jp abstract we present the results of x-ray and near-infrared observations of the galactic ridge x-ray emission (grxe). we extracted 2,002 x-ray point sources in the chandra bulge field (l =0◦.113, b = 1◦.424) down to ∼10−14.8 ergs cm−2 s−1 in 2–8 kev band with the longest observation (∼900 ks) of the grxe. based on x-ray brightness and hardness, we classified the x-ray point sources into three groups: a (hard), b (soft and broad spectrum), and c (soft and peaked spectrum). in order to know populations of the x-ray point sources, we carried out nir imaging and spectroscopy observation. we identified ∼11% of x-ray point sources with nir and extracted nir spectra for some of them. based on x-ray and nir properties, we concluded that non-thermal sources in the group a are mostly active galactic nuclei and the thermal sources are mostly white dwarf binaries such as cataclysmic variables (cvs) and pre-cvs. we concluded that the group b and c sources are x-ray active stars in flare and quiescence, respectively. keywords: galaxy: bulge galaxy: disk ir x-rays. 1 introduction since the dawn of the x-ray astronomy, an apparently diffuse emission of low surface brightness has been known to exist along the galactic plane (gp; |l| <45◦, |b| <1◦), which is referred to as the galactic ridge xray emission (grxe; e.g.,worral et al. 1982; warwick et al., 1985). the x-ray spectrum is characterized by hard continuum with a strong 6.7 kev fe k emission line (koyama et al., 1986a). the origin of the grxe had been a mystery for a long time. a long-standing debate had been whether it is a truly diffuse plasma (ebisawa et al., 2001, 2005) or a sum of unresolved xray point sources (revnivtsev et al. 2006). recently, revnivtsev et al (2009) showed that ∼80% of the fe k emission line was resolved into dim point sources using the deepest x-ray observations (∼900ks) made with the chandra at a slightly off-plane region of (l, b)=(0◦.113, –1◦.424) in the galactic bulge (chandra bulge field; hereafter, cbf). if the grxe is composed of the dim x-ray point sources, new questions arise. what are the populations of the dim x-ray point sources? which class of sources contribute to the fe k emission line? we do not know the population of majority of the dim point sources due to a limited number of x-ray photons. thus, we focus on near-infrared (nir), which has almost the same penetrating power as x-rays into deep interstellar extinction toward the gp. we studied the population constituting the grxe combining x-ray data with nir data in this paper. in particular, we focus on the population contribute to the fe k line of the grxe spectrum. 2 analysis and results 2.1 x-ray 2.1.1 observation and source extraction we retrieved 10 archived data of the cbf taken with the advanced ccd imaging spectrometer (acis)-i array on board chandra with a total exposure time of ∼900 ks. we merged 10 data set and extracted 2,002 valid point sources down to ∼10−14.8 ergs cm−2 s−1 in 2–8 kev (figure 1). for all the sources, we extracted source and background events. 2.1.2 spectral fittings for the bright sources (source counts>100), we constructed the background-subtracted spectra and generated instrumental response files. we carried out spectra fittings with thermal (apec; smith et al. 2001) and 222 http://dx.doi.org/10.14311/app.2014.01.0222 x-ray and near-infrared spectroscopy of dim x-ray point sources... non-thermal models (power-law) for the bright sources. as the results, 11 bright sources with more than 1000 counts have hard power-law like hard spectra with the photon index γ∼1.5. figure 1: smoothed and exposure-corrected x-ray image of the cbf (0.5–8 kev). the field of view of the sirius (nir) observations are shown by red squares. the white circle shows the region, the result of which was published in revnivtsev et al (2009). 2.1.3 grouping 0.5 1.0 1.5 2.0 2.5 3.0 -1.4 -1.2 -1.0 -0.8 -0.6 -0.4 -0.2 0.0 0.2 0.4 1 2 3 4 5 q 2 = 3 *q 2 5 /q 7 5 q1=log10 q50/(1-q50) median energy (kev) c a b figure 2: x-ray color-color diagram of all detected xray sources. the converted median energy is shown in the upper x-axis. color difference shows groups defined in § 2.1.3. we constructed an x-ray color-color diagram (hong et al., 2004) using the quantiles (e25, e50, and e75) characterizing the spectral shape of each source (figure 2). here, ex (kev) is the energy below which x% of photons reside in the energy-sorted event list. e50 is equivalent to the median energy (the details are in morihana et al., 2013). here, the q1 value indicates the degree of photon spectrum being biased toward the higher (q1 > 0) or lower (q1 < 0) energy end (hard or soft spectra), and the q2 value indicates the degree of photon spectrum being less (q2 > 1) or more (q2 < 1) concentrated around the peak (broad or narrow spectra). based on the x-ray color-color diagram, we classified all the point sources into three groups, which are the group a (hard), b (soft and brooded spectrum), and the group c (soft and peaked spectrum). 2.1.4 global spectral fittings furthermore, we performed global spectral fittings in 0.5–8 kev for the composite spectrum for each group in a similar manner in § 2.1.2 (figure 4). for the group a spectrum, neither a power-law nor a thin-thermal plasma model reproduced the spectrum well, respectively because of the excess emission at 6.7 kev or a flatness of the continuum. so we fitted the spectrum with a combination of the two models, which was successful. the equivalent width (ew) of the fe k feature becomes larger as the flux decreases (figure3), which suggest that the thermal component becomes strong against the non-thermal component as the flux decreases. for the group b spectrum, several emission lines are seen, including the 6.7 kev emission line from fexxv and 2.5 kev from sxv. this set of emission lines indicates a multiple-temperature plasma, and indeed the spectrum was reproduced well with two thin-thermal plasma components, but not with one component. for the group c spectrum, several emission lines are also seen. unlike the group b sources, the fexxv emission at 6.7 kev is absent. we fitted the spectrum using the same model with group b. 0 200 400 e q u iv a le n t w id th ( e v ) 10-1610-1510-1410-13 fx (ergs cm-2 s-1) figure 3: equivalent width of the fe k line against the decreasing flux in 2-8 kev above which the cumulative combined spectra in the group a were constructed. the 1σ statistical uncertainty is shown for each data. 2.2 nir imaging 2.2.1 observation and source extraction to identify the x-ray point sources with nir, we carried out nir observations using simultaneous infrared for unbiased survey (sirius; nagayama et al., 1999) on the infrared-survey facility (irsf) 1.4 m telescope 223 kumiko morihana, masahiro tsujimoto, ken ebisawa c o u n ts s -1 k e v -1 0 .0 1 1 0 -3 1 0 -4 -2 0 2 χ energy (kev) 0.5 1.0 2.0 3.0 5.0 (a) a c o u n ts s -1 k e v -1 0 .0 1 1 0 -3 1 0 -4 -2 0 2 χ energy (kev) 0.5 1.0 2.0 3.0 5.0 (b) b c o u n ts s -1 k e v -1 0 .0 1 1 0 -3 1 0 -4 -2 0 2 χ energy (kev) 0.5 1.0 2.0 3.0 5.0 (c) c figure 4: composite spectra and the best-fit global model of the group (a) a, (b) b, and (c) c. the lower panel shows the residuals of the data to the fit. the best-fit parameters can be found in table 1. table 1: best-fit parameters for global spectral model in 0.5–8.0 kev group nh (1)1 kbt (1)2 nh (2) kbt (2) z3 γ4 χ2/d.o.f. (1022 cm−2) (kev) (1022 cm−2) (kev) a 1.09+0.39 −0.50 6.65+3.24 −3.03 2.46+2.35 −0.58 ... 0.97+0.36 −0.32 1.29+0.18 −0.40 205.36/504 b 0.75+0.06 −0.05 0.74+0.54 −0.45 0.80+0.22 −0.18 7.87+1.86 −4.84 0.99+0.33 −0.29 ... 98.68/103 c 0.70+0.18 −0.11 0.78+0.04 −0.03 0.04+0.05 −0.04 4.50+0.65 −0.35 0.15+0.16 −0.12 ... 85.86/102 1interstellar extinction column density for the first component (the lower temperature component for the twotemperature model. 2plasma temperature for the second component (the higher temperature component for the two-temperature model). 3metal abundance relative to the solar value for the thermal component. 4photon index for the power-law model as the second component. in south africa astronomical observatory. we covered the cbf as we show in figure 1. we extracted nir source with a 3σ level using sextractor version 2.8.6, which are 52312 (j), 61,188 (h), and 65,051 (ks) sources down to ks∼16 mag. for asymmetry and photometry correction, we rendered the two micron all sky survey (2mass) point source catalog. for asymmetry, the sirius positions are determined at an accuracy of the pixel size of sirius (0.45′′). 2.2.2 cross correlation we search for possible nir counterparts for all the xray point sources using 2mass and the sirius. we searched nir counterpart sources within 1σ error circle (x-ray-2mass source; 1.3′′, x-ray-sirius source; 1.2′′). when there are two or more sources within the 1σ circle, we assumed the closest one to be the counterpart. then, we finally recognized 222 x-ray sources to have nir counterpart within 1σ circle (∼11% of all the x-ray point sources). 2.3 nir spectroscopy we conducted nir spectroscopy observation for some selected objects in the cbf using subaru/multi-object infrared camera and spectrograph (moircs). we selected 51 sources for spectroscopy in ks-band based on x-ray hardness and source variability. figure 5 shows examples of nir spectrum. we finally obtained 33 nir spectra of the x-ray point source in the cbf. combined x-ray results, there are two type of sources in the cbf, which are (1) sources with hi (brγ) and co absorption features in nir spectra and hard x-ray spectra, (2) sources only with co absorption features in nir spectra and soft x-ray spectra. from these properties, type (1) sources are k or m spectral type stars and type (2) sources are m spectral type stars. 21000 22000 23000 24000 wavelength (angstroms) b a b a c c coco co cohi hei cainai n o rm a liz e d i n te n s it y figure 5: examples of ks-band spectra in the cbf. upper label of each spectrum shows groups in § 2.1.3 defined by x-ray properties. 224 x-ray and near-infrared spectroscopy of dim x-ray point sources... 3 discussions & conclusion we now discuss likely populations in each group based on the results presented above. the transition from one class to another is continuous along the color and flux, so the groups are naturally a mixture of sources of different classes. first, we consider that the group a sources are mostly mixture of active galactic nuclei (agns) and white dwarfs (wds) binaries, each responsible for the power-law and thermal plasma components in the composite spectrum (figure 4). in the spectral fitting, the power-law component has a spectral index of 1.29+0.18 −0.40, which is similar to the typical spectral form of agns (table 1 e.g.; rosati et al., 2002). for the thermal component of the composite spectrum of the group a, a strong fe k feature and 6.7 kev plasma temperature are seen. both of these features are observational characteristics of magnetic cvs (ezuka & ishida 1999). other classes of wd binaries, such as dwarf novae, pre-cvsmay also considered for the likely classes. precvs are poorly recognized class of sources, which are detached binaries of a wd and a late-type star, unlike conventional cvs that are semi-detached systems. some of them show strong fe k emission in the hard x-rays (matranga et al. 2012). in fact, showed nearinfrared spectra of selected x-ray sources presented in this paper, in which some thermal a sources do not exhibit the brγ emission that is typical for the conventional cvs (dhillon et al. 1997). we thus consider that pre-cvs, most of which do not show the brγ emission (howell et al. 2010; schmidt& mikoajewska 2003), also account for at least some fraction of the thermal source population in the group a. the group b and c sources are galactic sources with a soft thermal spectrum, and we consider that most of them are likely to be x-ray active stars. the composite spectra of these two groups were fitted with two plasma components. in these groups, the spectra type of the sources are kor m-type spectra, which has no brγ emission line. we speculate that the differences between b and c is that most c sources represent active binary stars in the quiescence, while most b sources represent those during flares. from these things, we consider that the group b and c sources are x-ray active stars in flare and quiescence, respectively. acknowledgement this research has made use of public data obtained from chandrax-ray center which is operated for nasa by the smithsonian astrophysical observatory. this work has also made use of software from high energy as astrophysics science archive research center (heasac) which is provided by nasa goddard space flight center. references [1] dhillon, v. s., marsh, t. r., duck, s. r., & rosen, s. r. 1997, minareas, 285, 95 [2] ebisawa, k., maeda, y., kaneda, h., & yamauchi, s. 2001, science, 293, 1633 doi:10.1126/science.1063529 [3] ebisawa, k., tsujimoto, m., paizis, a., et al. 2005, apj, 635, 214 doi:10.1086/497284 [4] ezuka, h. & ishida, m. 1999, apjs, 120, 277 [5] hong, j., schlegel, e. m., & grindlay, j. e. 2004, apj, 614, 508 doi:10.1086/423445 [6] koyama, k., makishima, k., tanaka, y., & tsunemi, h. 1986, pasj, 38, 121 [7] matranga, m., drake, j. j., kashyap, v., & steeghs, d. 2012, apj, 747, 132 doi:10.1088/0004-637x/747/2/132 [8] morihana, k., tsujimoto, m., 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http://dx.doi.org/10.1086/423445 http://dx.doi.org/10.1088/0004-637x/747/2/132 http://dx.doi.org/10.1088/0004-637x/766/1/14 http://dx.doi.org/10.1038/nature07946 http://dx.doi.org/10.1086/338339 http://dx.doi.org/10.1086/322992 http://dx.doi.org/10.1038/317218a0 kumiko morihana, masahiro tsujimoto, ken ebisawa discussion takeshi go turu’s comment: is the fe line a mixture of fe lines (6.4, 6.7 7.0 kev) or 6.7 kev line? the fe line in our grxe spectrum is a mixture of the fe lines (6.4, 6.7, and 7.0 kev). the line center of the fe line is ∼6.7 kev. guainazzi matteo’s comment: radio-quiet agns normally exhibit iron kα lines. this may suggest that your iron free agns could be orimary radio-loud. do you have radio measurements, that could validate this hypothesis? i consider that fe k line of most background agns are red-shifted, because most background agns constituting the grxe are at far distance. 226 introduction analysis and results x-ray observation and source extraction spectral fittings grouping global spectral fittings nir imaging observation and source extraction cross correlation nir spectroscopy discussions & conclusion 84 acta polytechnica ctu proceedings 1(1): 84–89, 2014 84 doi: 10.14311/app.2014.01.0084 agn/starburst connection eleonora sani1 1inaf osservatorio astrofisico di arcetri corresponding author: sani@arcetri.astro.it abstract two main physical processes characterize the activity in the nuclear region of active galaxies: an intense star formation (starburst, sb) and an active galactic nucleus (agn). while the existence of a starburst-agn connection is undisputed, still it is not clear which process dominates the energetic output in both local and high redshift universe. moreover there is no consensus on whether agn fueling is synchronous with star formation or follows it during a post-starburst phase. here i first review how to disentangle the relative sb-agn contribution, then i focus on the physical and geometrical properties of the circumnuclear environment. keywords: agn starburst merging feedback imaging spectroscopy mid-ir x-rays. 1 introduction the issue of agn – star formation (agn–sf) connection in local and distant galaxies is possibly relevant for understanding several processes: from galaxy formation and evolution, and the star formation and metal enrichment history of the universe, to the the origin of the extragalactic background at low and high energies and the origin of nuclear activity in galaxies. it is well known that sf traces the growth of a galaxy in terms of stellar mass, and that galaxies assemble their mass through sb episodes. for example, local ulirgs (ultraluminous infrared galaxies) and high-z smgs (submillimeter galaxies) harbor the large molecular-gas reservoirs that are necessary to switch on sb episodes (tacconi et al. 2010, 2013). on the other hand, agns trace the growth of supermassive black holes (smbhs, with masses mbh > 106m�) and quiescent smbhs are believed to dwell in almost all galaxy bulges as agn relics, i.e. the result of a past agn activity (soltan 1982, marconi et al. 2004, merloni & heinz 2008). 1.1 evidence of agn–sf connection a direct link between bulge formation and the growth of the central smbhs has been inferred from tight relations between bh mass mbh and the bulge structural parameters, such as velocity dispersion (ferrarese & merrit 2000, gebhardt et al. 2000, gultekin et al. 2009), luminosity (kormendy & richstone 1995, marconi & hunt 2003, sani et al.2011) and mass (magorrian et al. 1998, mh03, häring & rix 2004). since a sb is a natural consequence of dissipative gaseous processes associated with spheroid formation (e.g. barnes & hernquist 1991) and agn–sf connection dating back to the early universe is implied by these results, a mergerdriven scenario is well suited to reproduce such scaling relations. recently, attention has been drawn to the coexistence of pseudobulges and bhs (nowak et al. 2010, sani et al. 2011). indeed pseudobulges seem to follow their own relation with bhs, hosting less massive bhs than classical bulges (greene, ho, & barth 2008, hu 2009), or they are at least displaced from the scaling relations for classical bulges (sani et al. 2011, kormendy et al. 2011). this may indicate a dichotomy in the formation history of galaxies (major merger vs. secular evolution) and/or that activity in galaxy nuclei can be stochastically driven by local processes such as minor mergers, bar/disk instabilities. in the following i concentrate the discussion on the major-merger scenario, its implications and observational evidences. the reader is anyhow advised about the importance of secular evolution processes, especially in low-luminosity, local seyfert galaxies. 1.2 the major-merger scenario (ulirgs-qso path) the merger between galaxies of approximately the same size is relevant for the cosmological evolution of sbs, quasars and early type galaxies (sanders et al. 1988, silk & rees 1998, fabian 1999, granato et al. 2001, di matteo et al. 2005, hopkins et al. 2008, menci et al. 2008). a schematic view of the main steps in the merging process is given in fig. 1. 84 http://dx.doi.org/10.14311/app.2014.01.0084 agn/starburst connection sfr dmbh/dt figure 1: major-merger scenario. starting from the merger of two spiral galaxies (left side), the merger produces a violent sb and the onset of qso activity (middle) and ends with the formation of a dead spheroid (right side). from hopkins et al. 2008. during first encounters, the mergers between gasrich galaxies (i.e. spirals) drag the gas which fuels both sf and agn activity. thus a violent sb occurs (ulirg-phase) as well as heavily embedded smbh growth (observed as obscured agn). then, the peak of accretion happens when the systems coalesce. at this point the quasar is cleaning the circumnuclear environment thanks to strong winds that blow out the gas, the agn becomes x-ray and optically thin. finally, due to feedback processes both bh growth and further sf are quenched leaving a qso relic in a red galaxy (passive evolution). therefore, obscured qso and feedback processes are key ingredients in the bh– host galaxy co–evolution. in the following, after a brief description of the agn and sf emission, i review the agn-sf observations for both single sources (interesting for their physics/structure) and large samples (to infer statistical properties). 2 the agn vs sf emission an issue in agn–sf studies is to correctly identify agns that represent only a small fraction of sources compared to the population detected at optical and ir wavelengths, and their properties can be elusive. obscured agns can be elusive because their optical emission resembles that of normal galaxies and therefore they cannot be identified by the color-selection techniques used for qsos, or because their spectra do not show any agn signature. their ir emission can be dominated by pah features, typical of star-forming galaxies, instead of continuum emission from hot dust. radio observations reveal the radio-loud population of obscured agns (e.g., radio galaxies), but this comprises only a small fraction, 10%, of the total agn population. a hard x-ray selection fails to detect the luminous narrow-line agns in the numbers predicted by some models of the cosmic x-ray background. polletta and collaborators (2007) show the differences in the spectral energy distributions (seds) of agn and star forming galaxies. the average seds of the three classes show some clear differences. they become increasingly blue in the optical–near-ir (λ < 1 µm), warmer in the ir (i.e. red at λ ' 1−10 µm), and brighter in x-rays in the sequence sf→agn2→agn1. 85 eleonora sani more in detail, most of the diagnostics developed till recently fail in identifying an agn when it is intrinsically faint and/or deeply obscured. as an example of a possible case where the agn is hardly detectable, i consider in fig. 2 an intrinsically faint agn, contributing only 20% to the bolometric source luminosity, and moreover its primary emission is absorbed by gas and dust. only two spectral regions are useful for such an agn detection: the hard x-rays (above 2 kev) and the near-mid infrared between 3 and 10 µm. indeed in the near-ir and optical ranges the dust and gas extinction respectively avoid the agn detection, and at radio wavelengths the sb emission peak dilutes agn emission properties. figure 2: top: simulated seds of a sb (blue) and an agn (black) contributing to 80% and 20% respectively of the lbol. bottom: extinction of the agn emission by gas (green) and dust (red), the horizontal black line indicates an absorption factor of 5. the agn is undetectable in the range 3 µm-2 å due to dust and gas extinction, and at λ ≥ 10 µm for the sb dilution. only the hardest x-rays and 3-10 µm observations reveal the agn. it is thus clear that the diagnostic performed in the x-ray and ir bands can highlight the main agn-sf differences and represent the wavelength rages where we do have the most detailed information respectively. 3 x-ray and ir screenings: imaging and spectroscopy here i briefly describe recent results obtained thanks to x-ray – ir imaging and spectroscopy in two puzzling sources. the final goal is to constrain the physics of ongoing processes and the structure of the nuclear region. 3.1 the case of ngc 6240 thanks to imaging techniques we can simultaneously observe the agn and sf activity in the nuclei of local galaxies (e.g. ngc 1068, ngc 6240, mrk 231, arp 299, circinus...). the angular resolution represents the only limit for this analysis. ngc 6240 is a well known double-merging system 107 mpc far away. here the xray imaging and spectroscopy performed with chandra (komossa et al. 2003) revealed a compton thick double agn, that was confirmed at all wavelengths, plus a sb covering a projected ∼ 2 kpc scale (risaliti et al. 2006, medling et al. 2011, feruglio et al. 2013). hst and spitzer images (bush et al. 2008) show how the thermal emission follows the optical dust obscuration very closely. ngc 6240 is thus an active interacting remnant viewed at the point of nuclei merging where two agns are visible. the results are well consistent with a major merger scenario with the transition from disk galaxies to a spheroid. 3.2 iras 12071-0444: a ct type 2 qso mid-ir (data from irs/spitzer) and x-ray spectroscopy (data from bepposax, chandra, suzaku) allow to investigate the nature and peculiar structure of the nearby (z= 0.128) ulirg (lir = 9 × 1045erg/s) iras 12071-0444. it is one of the few ulirgs optically classified as a type 2 agn and its mid-ir spectrum (in fig. 5–right, nardini et al. 2009) shows the typical features of ongoing sb (traced by pah emission) plus a buried agn (traced by a reddened power-law). however, the marginal emission below 10 kev (fig. 5– left) is consistent with the sole sb component, the typical fe kα line is undetected, and the agn is only seen above 20kev where the much narrower suzaku fov eventually confirms an early tentative detection by bepposax. the x-ray data are well fitted by an absorbed power-law with nh = 3.5 × 1024cm−2 and l2−10 ∼ 7×1044erg/s, i.e. about 10% of the bolometric luminosity is given by the agn intrinsic emission. the result proves iras 12071-0444 as the closest comptonthick quasar 2 yet known. finally, a simple visual comparison with the prototypical ct seyfert ngc 4945 reveals that the reflection efficiency is about a factor of ten lower than for a standard geometry. a peculiar geometry of the absorber is thus required to explain the x-ray/ir data. there are basically two possibilities: (i) a geometrically thick torus, with a small opening angle (i.e. large covering factor). in this case both the direct and reflected components are absorbed. 86 agn/starburst connection agn template sb template figure 3: iras12071-0444 data. left: the spitzer/irs ∼ 5− 8µm spectrum (green dots) is reproduced (black line) by means of an agn (blue dashed line) and sb (red dot-dashed line) templates. right: suzaku data (blue) well agrees with the chandra/acis spectrum (red) in the 0.5-5 kev range, and beyond 15 kev with the bepposax/pds points (orange). the shaded blue and orange areas in the upper left corner allow to compare suzaku and bepposax/pds fields of view respectively. i also compare iras 12071-0444 with the ngc 4945 x-ray spectrum observed by xmm-newton (green). the ngc 4945 data are scaled to match iras 12071-0444 at 0.5–10 kev. alternatively, (ii) the reflection component is absent due to a small compact cloud along the line of sight (i.e. with a small covering factor). the last picture implies both photoelectric compton absorption without scattering. the resulting intrinsic luminosity exceedes the bolometric one a factor of 3 thus the compact cloud scheme is unphysical. as a probe of the iras 120710444 represents a key evolutionary step of the galaxybh growth. 4 statistical analysis of composite sources by selecting large samples of composite sb+agn sources, it is possible to link the agn–sf connection processes with the system properties. in the following i show recent results concerning ir and x-ray statistical analysis. i ) the availability of a reliable measure of the relative agn/sb contribution to ulirgs (risaliti et al. 2006, sani et al. 2008, nardini et al. 2008) allows a quantitative investigation of the relation between total luminosity and agn contribution. it is known from optical spectroscopy that the fraction of seyfert-like systems among ir galaxies grows along with luminosity (veilleux et al. 1999; goto 2005). in nardini et al. 2010 we have quantified how sf and nuclear activity are the primary engine at the opposite ends of the ulirg luminosity range. the sb component dominates at log(lir/l�) < 12.5, where the agn is a significant contributor in only ∼ 30% of the composite sources. the power supplied by bh accretion grows stronger along the luminosity scale, and ultimately it represents the trigger of the extreme ir activity. ii ) the same technique has been applied by sani et al. 2010 to a sample of local seyfert galaxies to relate their sb activity with the bh growing parameters. we found that sf activity around narrow line seyfert 1 (nls1s), i.e. the more accreting agns, is larger than around bls1 of the same agn luminosity. this result seems to hold over the entire range of distance and luminosity. moreover, the star formation rate is higher in low black hole mass (log(mbh/m�) < 7) and high eddington ratios (l/ledd > 0.1) systems indicating that black hole growth and star formation are occurring simultaneously. iii ) with ir and x-ray analysis we can also investigate the sf–agn connection as a function of obscuration. on one side we do have evidence (veilleux et al. 2009, nardini et al. 2010) that, as expected, the fraction of sb-dominated objects shows a constant decline as the radiation field grows harder with absorption features anti-correlating with the optical classification (siroki et al. 2008). concerning the individual classes, it is worth noting that a sizable number of very powerful agn actually lies among liners (low ionization narrow emitting regions, see also risaliti, imanishi & sani 2010). interestingly seyfert 2, liners and hii regions harbor a similar agn content, supporting the idea of a connection between the sf activity and nuclear obscuration. moreover, sb dominated galaxies host the most obscured agns (see also georgakakis et al. 2004, sani et al. 2008, nardini & risaliti 2011). on the other hand, no enhancement of sf is observed 87 eleonora sani in obscured agns (rovilos et al. 2012) and the specific sf rate of type 2 agn hosts is consistent with the value for normal galaxies (daddi et al. 2007, sarria et al. 2010, mainieri et al. 2011). this is thus a debated matter, but we can not relate the sf physics to the bh physics in a complete and unbiased way because we can not measure e.g. bh mass and accretion rate in type 2 objects. 5 catching feedback in action as mentioned at the beginning of this review, a key ingredient of the merger scenario is feedback. so far a direct detection of the agn winds able to quench sf in the host galaxy is lacking. indeed according to veilleux et al. 2005, ∼ 30% of qso show fast winds (100 km/s < vout < 1000 km/s) but the outflow affects the circumnuclear environment only on the broad/narrow line region scales and thus can not inhibit the sf in the host (muller-sanchez et al. 2011). only in nearby sources like mrk 231 is possible to detect strong molecular outflows (feruglio et al. 2010, fisher et al. 2010) acting on kpc scales as expected by qso-feedback models. the current challenge is to detect such molecular winds at the epoch of the agn activity peak (i.e. at about redshift 2). 6 what we know and what is missing • while the agn accretion history is well traced, we still do not know how the smbh mass function evolves. • if the sf–agn structure on large scales is well studied, we still lack in constrainig the physical processes on small scales (i.e. with extreme adaptive optics corrections for imaging and ifu observations). • we are confident that smbh growth happens simultaneously to the bulk of sf in unobscured composite sources, but the issue for type 2 objects is open. to solve it, we need to identify the entire population and to measure their mbh , l/ledd, sfr etc. • it is well known that agn powers strong winds in local galaxies. nonetheless most of them affect only the ionized gas on circumnuclear spatial scales and further observational efforts are required to identify kpc–scale molecular outflows at the peak of agn activity (z∼ 2). acknowledgement i would like prof. giovannelli and the soc for organizing this stimulating workshop. references [1] barnes, j. e., & hernquist, l. e.: 1991, apjl 370, l65. 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[51] veilleux, s., kim, d.-c., rupke, d. s. n., et al.: 2009, apj 701, 587. discussion casiana munoz-tunon: more obscured agns have larger sf, and you mention that no correlation is found between sf and obscuration. what sort of connection do you expect? eleonora sani: on the basis of hydrodinamical symulations of major mergers, we do expect the co-presence of a violent sb event and a buried agn at the time of galaxies coalescence. thus a correlation between the sfr and the agn obscuration behaviours (e.g. column density) is expected. analysis based on the cosmos survey don’t find such relation. nonetheless the issue is still a matter of debate since the lack of this correlation could be due to aperture effects. moreover deeply embeded agns are found in local ulirgs and high-redshift smgs. 89 http://dx.doi.org/10.1088/0004-637x/743/1/32 http://dx.doi.org/10.1086/518113 http://dx.doi.org/10.1086/500588 http://dx.doi.org/10.1086/523784 http://dx.doi.org/10.1038/nature08773 http://dx.doi.org/10.1088/0004-637x/768/1/74 introduction evidence of agn–sf connection the major-merger scenario (ulirgs-qso path) the agn vs sf emission x-ray and ir screenings: imaging and spectroscopy the case of ngc 6240 iras 12071-0444: a ct type 2 qso statistical analysis of composite sources catching feedback in action what we know and what is missing acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0050 acta polytechnica ctu proceedings 4:50–55, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app ion source for a single particle accelerator tomáš matlochaa,b a faculty of nuclear sciences and physical engineering, czech technical university in prague, břehová 7, 115 19 praha 1, czech republic b nuclear physics institute of the cas, 250 68 řež u prahy, czech republic correspondence: matlocha@ujf.cas.cz abstract. this paper proposes a method to obtain very low beam current on the injection side of an particle accelerator. by using a combination of a well known ion source type and a short photo-emissive laser pulse, very low amount of ions can be created. the method could be used in the ion source of various types of the accelerators, where very low beam current is essential. the design is adapted to build a compact internal ion source and the dimensions of the device are adjusted to fit central region of the cyclotron u-120m. the functional parameters of the device are discussed and the amount of the produced ions is estimated. keywords: single particle accelerator, cyclotron ion source, low beam current, laser ion source, pulsed ion source, u-120m, proton radiography. 1. introduction this paper presents a principle of delivering a very low beam current to the injection system of a single stage or low energy accelerator. a control of the ion creation process is a complex task with effect of many parameters. one of the control parameter can be the length of the primary ionizing pulse in the ion source. this length is naturally restricted and usualy can not be arbitrary lowered. when the ionizing pulse is driven using a high voltage discharge, the pulse length with duration about tens of nanosecond can hardly be achieved. from this reason, a primary ionizing plasma in presented ion source is not made using ordinary high voltage discharge, but using a laser pulse. with the present-day laser systems, the high intensity laser pulses with the duration of few ps could be generated and used for photo-emission. electrons from photo-emission then controllably ionize gas and produce ions for the low energy proton or heavier particle accelerator. a usage of the low current beams vary accordingly with the technical field where the beam is applied. the low current beams are required in the radio-biological microbeam study of the living cells [1], in the single proton detectors tests or in the proton radiography. a benefit of using proton beams instead of classical gamma-rays in the radiography, is that the scanned sample receive significantly lower dose for similar image result [2]. with a proper magneto-optic lens system, very high-resolution images could be obtained. usual resolution even with the low energy proton beams is several tens of µm. this resolution of the proton radiography method could be apparently further improved and its limits are far beyond present ranges [3]. very good resolution of the proton radiography [4] could lead to a specific high resolution 3d imaging, where a complete 3d image of the sample could be obtained by two or three laser shots in the proposed ion source. for a very small and sensitive scanned samples, the lowest possible irradiation can be important, so precise control of the number of the created ions is essential. schematic principle of the proton radiography is shown in fig. 1. figure 1. the proton beam lens system with the particle trajectories as colored lines [3]. 2. beam current limitation the idea presented in this paper has grown from the response tests of the silicone detectors and electronics for the planed upgrade of the inner tracking system of the alice detector [5]. the tests were performed on the old cyclotron u-120m, shown in fig. 2. these tests however require very low intensity of the delivered beam current [6]. a minimal beam current which can be delivered comfortably by this cyclotron is ca. 2.5 fa/cm2, which corresponds to ca. 15 600 protons per second per cm2. the beam intensity is usually decreased only after its extraction from the ion source. it means that regardless of the output cyclotron beam current, the amount of ions at the 50 http://dx.doi.org/10.14311/ap.2016.4.0050 http://ojs.cvut.cz/ojs/index.php/app vol. 4/2016 ion source for a single particle accelerator figure 2. cyclotron u-120m. beginning of the acceleration process is almost the same. this factor limits stability of the accelerator and reduces utilization of low current beams. the laser induced photo-emission ion source presented in this paper, can significantly reduce the number of ions entering the machine. 2.1. u-120m pig ion source the ion source of the cyclotron is a movable part and its position can be fine-adjusted with respect to the puller. the extraction window of the ion source has area approx. 2 mm2. the puller has an input window with an area of about 20 mm2. an optimal position of the ion source opposite to the puller guarantees a maximal extraction to loss ratio. in normal operation this extraction ratio is kept as high as possible. when the low current beam is required, this ratio is lowered. this is achieved mainly by changing the position of the ion source extraction window. the ion source is moved slightly to one side, so the extraction window of the ion source does not overlap with the puller input window. subsequently, only a minimal number of ions are able to pass the initial extraction. the rest of the ions are lost on the puller body as can be seen in fig. 3 and 4. although the above mentioned current regulation is very easy, it has some disadvantages. the u-120m cyclotron ion source is a penning ion gauge (pig) type ion source with a cold cathode, operating in continuous regime. in fig. 5 is photo of the ion source oriented with its head on the left side, and in fig. 6 is its head detail. the ion source has a cylindrical plasma chamber parallel to the cyclotron magnetic field of approx. 1 t. the chamber is enclosed from both sides by tantalum cathodes. the cylindrical wall of the ion source is an anode and whole body is made from a tungsten-copper composite. electrons emitted from the cathodes are accelerated by the anode potential. due the strong magnetic field the electrons are trapped by the field lines and are not able to directly reach the anode. the electrons repeatedly oscillates between the cathodes and are slowly drifting to the anode figure 3. central region top view – optimal extraxion for proton regime 37 mev simulated with durycnm4 [7]. figure 4. central region top view – minimal extraxion for proton regime 37 mev simulated with durycnm4 [7]. body. the electrons ionize the gas in the cylinder and create the plasma. the amount of the produced ions can be slightly regulated by changing the plasma current and by regulating the ion source gas presure. for stable operation, the penning ion source needs some minimal plasma current to heat up cathodes and some minimal corresponding gas concentration. in the usual working regime the plasma current is about 1 a and the minimal plasma current for stable operation is several miliamperes. basically in the ion source are two concurrently 51 tomáš matlocha acta polytechnica ctu proceedings figure 5. u-120m pig ion source. figure 6. current u-120m pig ion source. processes which lead to creation of ions. the first process is based on stripping orbital electrons of neutral atoms and generates positive ions. the degree of ionization is done by temperature of the plasma electrons and by a time of interaction. our penning ion source has plasma electron temperature up to approx. 70 ev. it is enough to produce ions with low ionization potentials, e.g. h+, d+, he2+, li2+, c4+, etc. in second process, the negative ions are produced. the second process leads to production of negative ions via the surface and the volume production process. the section 5.1 describes the negative hydrogen ions formation process in more detail. after their creation, both negative and positive ions are simultaneously extracted from the ion source by an alternating rf high voltage field. negative polarity extracts positive ions and oppositely. polarity of the cyclotron magnetic field determines the type of ions which will be accelerated. the second type of ions are simply extinguished on the puller body. 2.2. pulsed pig ion source from above mentioned penning ion source operation principle it follows, that the ions are produced permanently. from that reason the lowest current of extracted ions is limited from below. there were several attempts to switch our penning ion source to a pulsed operation mode. these studies were motivated by other reasons than lowering the output current, but a deeper knowledge of the pig pulse regime capabilities were gained. an ignition process of the pig ion source from the full off state is very long and lasts couple of seconds. when the pig plasma is once ignited, the plasma current can be lowered to five miliamperes, and the ion source is in low current state. in this state changing of the plasma current can be done quickly with a reaction time of a few microseconds. then the ion source can be fast and easily modulated between low and high current states. but the ion source even in the low plasma current mode is still producing much more ions than required. there is an option to further lower the low current value by at least an order of magnitude by driving the cathodes temperature. nevertheless, continuous operation of the ion source is not suitable for the low current beams. from this reason, the possibilities of other ion production were studied and the main findings are presented in the next paragraphs. 3. inspiring ion sources 3.1. ebis/ebit ion source a principle of operation of an electron beam ion source (ebis) and an electron beam ion trap (ebit) is very similar. the electrons are extracted from a cathode by thermionic emission and accelerated in a strong solenoidal magnetic field by an anode voltage. the shape of the magnetic field forms the entering electrons to well focused beam with densities up to several ka/cm2. this beam ionizes the gas and forms the ions. because the electron beam temperature can be very high, a high ion charge state is possible. in the ebit the ions are confined in a space charge of a dense electron beam, where attractive force of electrons prevent the ions to move. an electrostatic potential of external electrodes is applied to trap the ions and hold their position. when the trapping potential is switched off, the ions can be extracted. this type of ion source is mainly used for heavy ions for which high charge states or full stripping by other techniques is complicated. temperature of electrons could be from 10 kev to 200 kev. the extracted ion current is low, typically ranging from 105 to 109 ions per second. the ebis/ebit sources exist in many designs from ultra compact devices for low current and low charge states to huge machines capable of delivering fully stripped uranium ions [8, 9]. principial schematic of the ebit is in fig. 7. figure 7. schematic design of ebit ion source [10]. 52 vol. 4/2016 ion source for a single particle accelerator 3.2. rf gun modern light sources such as the energy recovery linac (erl) or free electron lasers (fel) use as an electron beam generator pulse operated rf guns. the rf gun is a laser induced photo emission electron gun, where photo electrons are accelerated by a strong electric field generated during the rf pulse. schematic design is shown in fig. 8. the photosensitive cathode is placed near the center of a 3/2 cell rf cavity (0.5–2ghz), where a high electric field is produced (up to 120 mv/m). a very short laser pulse (10 ps) with a proper phase is applied onto the photo-cathode. a bunch of photoelectrons is emitted, accelerated to proper energy and delivered further into the system. currently exist a number of devices of this type, capable to produce electron beams with energies in the range 0.1–5 mev. figure 8. schematic design of the rf gun. photo-cathodes used in these electron sources can be from metal or semiconductor. in general, metals have lower electron conversion efficiency(qe) and need uv lasers. on the other hand they have fast response and are resistant to impurities. semiconductor cathodes are more efficient and can be operated with visible/ir laser, but have slower time response and are sensitive to contamination and photon radiation. charge emitted per bunch is approx. 1 nc. required peak rf power is up to 10 mw. mean laser power is 1 w and required frequency is few thousands pulses per second [11, 12]. 4. laser induced photo-emission ion source the above mentioned devices could probably be combined. by applying a short laser pulse on a photo sensitive cathode one could produce an electron bunch. this bunch could be then accelerated to a desired energy by an anode potential. during travel from a photo-cathode to an anode, this bunch could ionize gas present in the discharge chamber. because the electron temperature is expected only few tens ev, sufficient to ionize hydrogen and helium, and emitted charge is low, the device could be kept compact. such a compact device could be placed inside the central region of the cyclotron and in demand of very low beam currents replace the present pig ion source. dimensions of the pig ion source must be preserved to fit into the cyclotron central region. these dimensions determine the discharge chamber shape and possible arrangement of the electrodes. unlike in the pig ion source, where the cylindrical chamber is anode enclosed by cathodes from both sides as in fig. 6, here will be photo-cathode on one side and anode on the other side of the cylinder as in fig. 9. in this configuration the electron bunch will pass through the chamber only once per one laser pulse. the laser pulses with energies of few µj are driven to the photo-cathode through ion source arms enclosed by a high vacuum sealed window, from an external laser generator placed out of the cyclotron site. figure 9. proposed laser ion source. 4.1. photo-cathode in general, the photo-cathode should have work function below 3 ev to avoid a necessity of using uv lasers. considering a gamma radiation always present at the cyclotron site, the photo-cathode should be metallic. other reason for this choice is good resistance to adverse conditions such as bad vacuum and impurities in the system, where semi-conductors cathodes are very sensitive. in theory, the metal photo-cathodes should not work when irradiated by photons with energies below the work function hν < φ. in reality, an effect of multiple photon absorption were observed in high density laser pulses, and even photons energies below the threshold energy can be used for photoemission [13]. the quantum efficiency is defined by ratio between incident photons and emitted electrons. the metals have qe low, but in our case it should be helpful for limiting a parasitic emission by photons captured from de-excitation and neutralization of the gas atoms. copper, which has qe 5× 10−5 at wavelength 320 nm, could be suitable for the first try. 53 tomáš matlocha acta polytechnica ctu proceedings 5. ions production 5.1. negative hydrogen ion formation as the principle of proposed pulsed ion source is simple, many practical limitations will probably occur. the main questions are, if this device will be capable to produce any negative ions and how long this ions will live for. a creation of the negative hydrogen ion h– is a multi-step process, where several conditions should be fulfilled. there are many processes involved in h– formation. one of them, the volume negative ion production process which needs at least two different temperature of electrons. faster electron with energies near 20 ev which ro-vibrationally excites the hydrogen h*2 and a cold electron, which can than dissociate the h2 molecule and attach to one of the atoms to form an negative hydrogen ion: h2 + e− −−→ h∗ 2 + e− −−→ h0 + h−. this process is called a dissociative attachment process and the dissociative low temperature electron energy needs to be close to 1 ev. bounding energy of the second electron in the h– ion is 0.75 ev, so the once formed h– ion can be easily destroyed by collisions with other ion or on residual gas. the second important h– formation process is the surface negative ion production. in this process the previously formed h0 atom from h2 dissociated molecule collides with a metallic surface of the plasma chamber. when bouncing back from the wall, an conductive electron from the metal surface can be trapped by the atom and form an h– ion. work function of the chamber metal tungsten surface is near 4.5 ev, far above 0.75 ev electron affinity of h atom. from this reason the cross-section of h– formation from pure metal surfaces is commonly increased by covering surface with caesium layer. this thin cs layer lowers the work function of surface to approx. 1.6 ev. the cs is widely used in h– ion sources and has its significant role also in the volume h– production. in both processes significantly increases h– formation probability. in the u-120m cyclotron penning ion source cs is not used, so the volume process is therefore considered to be more important [14–16]. 5.2. positive ions formation a situation with positive ions should be more simple. ionization of a low atomic number elements is done by stripping their orbital electrons in energetic collisions. as for heavier elements the process is gradual, because the atoms are ionized in a stepwise processes where each electron collision removes one or two orbital electrons. for light atoms such as h and he, this can be done very fast. ionization energy for hydrogen is 13.6 ev and has maximal cross-section σ = 0.6× 10−16 cm2 at 50 ev. full ionization energy for helium is 54.4 ev and its maximal cross-section σ = 0.3× 10−16 cm2 is near 100 ev [17]. 5.3. ions yield estimation for the laser pulses with duration 20 ps the emitted charge 100 pc could be expected. with optimal electron temperature and for h2 concentration in range from 109 cm−3 to 1013 cm−3 [18] in a volume similar to current used pig ion source 2 cm3, from current density 18 a/cm2 there can expected from 102 to 105 positive ions. in normal operation the ratio between protons and h– ions is 10−2. very low probability of formation h– ion in the single pulse can be expected. even if the production ratio is lowered by two orders to 10−4, still up to 10 h– ions per volume could be expected. with considering a fact, than an exact h– formation process understanding is still in progress, an influence of more factors or processes, such as a wall biasing, could play its role. from this reason a formation of an h– ion in the single discharge bunch should not be rejected in advance. 5.4. discharge conditions and ions extraction after formation of the electron bunch by an irradiation of the photo-cathode, a multiple side effects can be expected. one from these effects could be the above mentioned parasitic photo-emission. other important effect will be positive ion bombardment of the cathode. parameter which can highly affect performance of the device will be a lifetime of produced ions which will probably reduce a minimal length of the ion pulse. 6. beam time distribution the low current regime of h– ions with energy 36.9 mev has its cyclotron frequency 25.8 mhz. this main carrier frequency is modulated by a 150 hz signal. particles in the cyclotron are accelerated with each half period and are caught in phase angle of about from −30° to 30° of this half period. the ions are revolving in approx. 6 ns micro-bunches with 32 ns spaces between them. with 10 % carrier modulation these micro-bunches are formed into 0.67 ms long bunches with 6 ms spaces. a simulation of the cyclotron response to a 110 ps short input pulse with 330 ions was made in the code durycnm4 [7, 19]. the ions from one input pulse are accelerated for 503–507 periods and divided into five output micro-bunches. output signal than lasts for 160 ns. energy range of the particles is from 36.75 to 36.9 mev. this cyclotron impulse response is made by a phase instabilities and space distribution of the micro-bunch, which affects energy increment difference particle gains each turn and leads to energy spread of the beam. because the extraction is made on the desired energy, each particle from the input bunch needs a different number of the accelerating turns. as a result on the output, the signal is time dispersed. this dispersion is coming from the machine nature and cannot be avoided by shortening of the input pulse. number of ions in individual micro-bunches are shown in fig. 10. 54 vol. 4/2016 ion source for a single particle accelerator figure 10. simulated u-120m impulse response. 7. conclusions this paper proposes a method which possibly could be used to produce a very small amount of the ions. considering many variable parameters that can be used to tune the ion source, it can be expected that the ions could be produced in countable amounts and delivered to the accelerating process on the request. the benefits of the presented method is mainly in the controlled production of the selected charge state and the number of the generated ions. as the demand of low current ion beams is increasing rapidly, overcoming the difficulties with generation the ions by the laser induced photo-emission 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http://www.lepp.cornell.edu/~hoff/lectures/08s_688/08s_688_080225.pdf http://www.lepp.cornell.edu/~hoff/lectures/08s_688/08s_688_080225.pdf http://dx.doi.org/10.1007/s00339-013-7600-z http://dx.doi.org/10.5170/cern-2013-007.265 http://dx.doi.org/10.1109/tps.2005.860067 http://physics.nist.gov/cgi-bin/ionization/ion_data.php?id=hi&ision=i&initial=&total=y http://physics.nist.gov/cgi-bin/ionization/ion_data.php?id=hi&ision=i&initial=&total=y http://dx.doi.org/10.1109/tps.2005.860069 http://accelconf.web.cern.ch/accelconf/c07/papers/385.pdf http://accelconf.web.cern.ch/accelconf/c07/papers/385.pdf acta polytechnica ctu proceedings 4:50–55, 2016 1 introduction 2 beam current limitation 2.1 u-120m pig ion source 2.2 pulsed pig ion source 3 inspiring ion sources 3.1 ebis/ebit ion source 3.2 rf gun 4 laser induced photo-emission ion source 4.1 photo-cathode 5 ions production 5.1 negative hydrogen ion formation 5.2 positive ions formation 5.3 ions yield estimation 5.4 discharge conditions and ions extraction 6 beam time distribution 7 conclusions references 175 acta polytechnica ctu proceedings 1(1): 175–180, 2014 175 doi: 10.14311/app.2014.01.0175 be/x-ray binaries with black holes in the galaxy and in the magellanic clouds janusz zió lkowski1 1copernicus astronomical center, ul. bartycka 18, 00-716 warsaw, poland corresponding author: jz@camk.edu.pl abstract i will start with the statistics indicating that the objects named in the title of my talk are either non-existing or very elusive to detect (not a single such object is known against 119 known be/neutron star x-ray binaries). after brief reviewing of the properties of be/x-ray binaries i discuss several objects that were proposed as the long sought for candidates for be/black hole x-ray binaries. after three unsuccessful candidates (ls i +610 303, ls 5039 and maxi j1836-194), a successful candidate (agl j2241+4454/mwc 656) was finally, very recently, announced. keywords: stars: binaries – stars: x-ray binaries – stars: be/x-ray binaries – stars: black holes – stars: be. 1 introduction the objects named in the title of my talk seem not to exist neither in our galaxy nor in the magellanic clouds. not a single such object is known today (this statement was still true during our conference). at the same time, we know (today) 184 be/x-ray binaries (74 in the galaxy and 110 in the magellanic clouds). 2 properties of be/x-ray binaries be x-ray binaries (be xrbs) are the most numerous subclass among high mass x-ray binaries. they outnumber all other high mass x-ray binaries by a factor of three (we know about 180 be xrbs vs about 60 other high mass x-ray binaries). these systems consist of a be star and a compact object (a neutron star or a black hole). the be stars are massive, generally main sequence, stars of spectral types a0-o8 with balmer emission lines (negueruela 1998). the be xrbs are rather wide systems (orbital periods in the range of ∼ 10 − 1180 days). the orbits are frequently eccentric. a compact component accretes from the wind of a be star (even massive be stars are well within their roche lobes for these wide orbits, so there is no question of roche lobe overflow). at present, 184 be xrbs are known in the galaxy and in the magellanic clouds, and in 119 of them, the compact object was confirmed to be a neutron star by the detection of the x-ray pulsations (with the pulse periods in the range of 34 ms to ∼ 1400 s). in the remaining cases, whenever we have information concerning the nature of the compact component (such as an x-ray spectrum), it also indicates a neutron star. although one cannot exclude that a few of these systems contain white dwarfs or black holes, it is safe to state that majority of them contain a neutron star as compact component. however, not a single black hole binary containing a be type component has been found so far. this disparity (119 be xrbs with neutron stars versus not a single one with a black hole) seems indeed striking (this was the situation during our conference; today the statistics is 119 to one − see the section 4.2). the x-ray emission from be xrbs (with a few exceptions) is of a distinctly transient nature with rather short (days to weeks) active phases separated by much longer (months to tens of years) quiescent intervals (a typical flaring behavior). there are two types of flares, which are classified as type i outbursts (smaller and roughly regularly repeating) and type ii outbursts (larger and irregular. this classification was defined by negueruela & okazaki 2001 and negueruela et al. 2001. type i bursts are observed in systems with highly eccentric orbits. they occur close to periastron passages of a neutron star. they are repeating at intervals ∼ porb. type ii bursts may occur at any orbital phase. they are correlated with the disruption of the excretion disc around be star (as observed in hα line). they repeat on time scale of the dynamical evolution of the excretion disc (∼ few years to few tens of years). this recurrence time scale is generally much longer than the orbital period (negueruela et al. 2001). be xrbs systems are known to contain two discs: excretion disc around be star and accretion disc around neutron star. both discs are temporary: excretion disc disperses and refills on time scales ∼ few years to few decades (dynamical evolution of the be star disc, formerly described as ”the activity of a be star” (negueru175 http://dx.doi.org/10.14311/app.2014.01.0175 janusz zió lkowski ela et al. 2001)), while the accretion disc disperses and refills on time scales ∼ weeks to months (which is related to the orbital motion of a neutron star on an eccentric orbit and, on some occasions, also to the major instabilities of the other disc). the accretion disc might be absent over a longer period of time (∼ years), if the other disc is very weak or absent. the x-ray emission of be xrbs binaries is controlled by the centrifugal gate mechanism, which, in turn, is operated both by the periastron passages (type i bursts) and by the dynamical evolution of the excretion disc (both types of bursts). this mechanism explains the transient nature of the x-ray emission ( see zió lkowski 2002 and references therein). the more detailed description of the properties of be xrbs is given, e.g. in negueruela et al. 2001, zió lkowski 2002, belczyński & zió lkowski 2009, reig 2011 and references therein. considering the numbers of different (neutron star vs black hole) be xrbs, it is important to note, that if we take all other xrbs (both high and low mass), except be xrbs, then the ratio of neutron star systems to black hole systems is about 2:1 (remillard & mcclintock 2006, zió lkowski 2008). for be xrbs this ratio is 119 to zero. the disparity is indeed striking. this disparity is referred to as a missing be – black hole x-ray binary problem. trying to understand the reasons for which we do not observe be – black hole xrbs, belczyński & zió lkowski (2009) carried out stellar population synthesis calculations aimed at estimating the ratio of neutron star to black hole be xrbs, expected on the basis of the stellar evolution theory. the results of their calculations predict that for our galaxy the expected ratio of be x-ray binaries with neutron stars to the ones with black holes fns/bh should be, most likely, equal ∼ 54. since we know 48 neutron star be systems in the galaxy, then it comes out that the expected number of black hole systems should be just one. the observed number (zero) is consistent with this prediction. zió lkowski & belczyński (2010) carried out also preliminary stellar population synthesis calculations for the magellanic clouds. this time, the result was that the expected ratio fns/bh for magellanic clouds be xrbs should be equal ∼ 9. since we know 71 neutron star systems in the magellanic , then the expected number of black hole systems should be about 8. this time, the observed number (zero) is not consistent with the prediction. the most likely reason for this discrepancy is a different history of the star formation rate in the magellanic clouds, with respect to the galaxy. the calculations mentioned above used the galactic scenario for the star formation history. the new, more realistic calculations for magellanic clouds are necessary. 3 new be/x-ray binaries zió lkowski & belczyński (2011) published a full list of the 170 be/x-ray binaries known in 2011 (72 in the galaxy and 98 in the magellanic clouds). table 1 of this paper contains the list of the 14 new objects belonging to this class which were discovered in meantime (2 of them lie in the galaxy and 12 − in the magellanic clouds). this list contains two interesting systems (added after the end of our conference). one of them is system with the longest orbital period (swift j010745.0-722740 with porb ≈ 1180 days). the second is the first long sought be/black hole x-ray binary (agl j2241+4454). 4 candidates proposed for be/black hole x-ray binaries 4.1 unsuccessful candidates 4.1.1 ls i +610 303 this binary of the orbital period 26.5 d consists of a b0ve star and a compact object the nature of which is not firmly established yet. no pulsations were detected in the x-ray emission. the radio emission also does not show pulses. this might indicate a black hole rather than a neutron star. however, in many respects, the system reminds another x-ray and radio binary − psr b1259-63, the nature of which is already well understood. psr b1259-63 belongs to the category of so called colliding winds binaries. this wide (3.4 y orbital period) binary consists of an o9.5ve star and a neutron star which is observed as a fast (pspin = 47.7 ms) radio pulsar. neutron star moves along a very eccentric (e = 0.97) orbit. the system is also a source of tev emission (in fact, it was the first binary detected in this energy range). in all three energy ranges (radio, x-ray and tev) the emission is modulated with the orbital period. the binary was most recently extensively discussed by dubus (2013). after reviewing both the observations and the numerical simulation modeling, he strongly supports the much earlier idea of tavani et al. (1994) that both x-ray and tev emission are due to collision of two winds: stellar wind from be star and pulsar wind 176 be/x-ray binaries with black holes in the galaxy and in the magellanic clouds table 1: new be x-ray binariesa porb pspin lb x,max spectral name [d] [s] [erg/s] type refc xmmu j004814.0-732204 11.866 4.2 × 1036 b1.5-2.5ve 1 xmmu j005011.2-730026 29.9 214 5.0 × 1034 be 2,3,4 igr j00569-7226 17 5.05 5.5 × 1037 b0.5e 5,6,7,8 cxou j005758.4-721620 40.03 7.918 4 × 1035 be 9,10 2xmm j010247.4-720449 490 ? 521.4 2.8 × 1035 be 11,12 swift j010745.0-722740 1180 be 13 igr j01217-7257 84 ∼ 1 × 1037 be ? 14 cxo j012745.97-733256.5 656 1062 6.3 × 1035 b0-0.5iiie 15,16,17 igr j0154-7253 36.3 11.483 2.5 × 1037 o9.5-b0iv-ve 18 igr j015712-7259 35.1 11.6 4 × 1036 be 19,20,21 swift j04558.9-702001 5.1 × 1035 be 22 swift j053041.9-665426 ∼ 415 9.7 × 1036 be 23,24,25 maxi j1932+091 be 26,27 agl j2241+4454 60.37 3.7 × 1031 b1.5-2iiie 28,29,30,31,32 asince this table is a natural supplement to tables 1 and 2 of zió lkowski & belczyński (2011), i should add following updates to these tables: swift j0513.4-6547 porb ≈ 27 d (coe et al. 2013d) rx j0520.5-6932 pspin = 8.035 s (vasilopoulos et al. 2013b), porb = 23.93 d (kuehnel et al. 2014) smc sxp707 pspin is unknown (707 s is an instrumental effect, maggi et al. 2013) bmaximum x-ray luminosity c (1) sturm et al. 2011a; (2) coe et al. 2011; (3) schmidtke & cowley 2011; (4) schmidtke et al. 2013a; (5) coe et al. 2013a; (6) kennea 2013; (7) schmidtke & cowley 2013a; (8) coe et al. 2013b; (9) israel et al. 2013; (10) schmidtke & cowley 2013b; (11) sturm et al. 2011b; (12) sturm et al. 2013; (13) maggi et al. 2014; (14) coe et al. 2014; (15) henault-brunet et al. 2012; (16) schmidtke et al. 2012a; (17) schmidtke et al. 2012b; (18) townsend et al. 2011; (19) coe et al. 2008; (20) bodaghee et al. 2009; (21) schmidtke et al. 2013b; (22) vasilopoulos et al. 2013a; (23) sturm et al. 2011c; (24) charles et al. 2011; (25) sturm et al. 2011d; (26) negoro et al. 2014; (27) itoh et al. 2014; (28) williams et al. 2010; (29) casares et al. 2012; (30) casares et al. 2014; (31) paredes & ribo 2014; (32) munar-adrover et al. 2014. from rapidly rotating neutron star. the shock formed as a result of the collision gives the rise to a non-thermal emission in a similar way as in the pulsar wind powered nebulae. the characteristic element of such model is elongated radio emission with position angle dependent on orbital phase. elongated emission is pointing from the vicinity of the pulsar in the direction opposite to the direction towards the be star. such ”comet tail” behavior of radio emission is clearly observed for psr b1259-63. at present, there are no significant doubts that the system is powered by the pulsar spindown and that the colliding winds model is, in general, a correct explanation of the properties of this binary. ls i +610 303 is, in many respects, similar to psr b1259-63. in particular, the spectral and timing properties of the emission (through all ranges of electro177 janusz zió lkowski magnetic spectrum) are very similar. also the ”comet tail” behavior of radio emission is clearly seen for ls i +610 303 (dhawan et al. 2006). as i mentioned earlier, no pulsations were detected and, therefore, the case is not so clear cut as for psr b1259-63. this system (ls i +610 303) is also discussed by dubus (2013) and he concludes that indirect evidence strongly supports the colliding winds case. the compact object is, most likely, a rapidly rotating pulsar. the lack of the observed pulsations might be explained as the result of the absorption of the radio emission by the circumstellar material. even in psr b1259-63 the pulsed radio emission disappears for about 40 days around periastron. ls i +610 303 is much more compact binary (orbital period is ∼ 50 times shorter) and the absorption is strong throughout all orbital cycle. since the compact component is, most likely, a neutron star, the system is not a good candidate for a be/black hole binary. 4.1.2 ls 5039 this binary of the orbital period 3.9 d consists of an o6.5((f)) star and a compact object the nature of which is still a subject of controversy. no pulsations were detected neither in the x-ray nor in the radio emission. both x-ray and tev emission are modulated with the orbital period. the radio emission is variable but the flux is not modulated with the orbital phase. the morphology of the radio emission (which has an elongated shape) is variable with the orbital phase but the positional angle, at first look, seems to be roughly constant (moldon et al. 2012). this would not be a typical ”comet tail” behavior observed in psr b1259-63 and in ls i +610 303. however, analyzing more subtle changes in radio morphology and modeling radio emission with colliding winds model, moldon et al. (2012) demonstrate that the observed radio emission is compatible with the presence of a young non-accreting pulsar in the system. the authors obtain the best fit for a relatively high inclination of the orbit (i ≈ 700). as they note, this value has deep implication for the estimate of the mass of the compact component. radial velocities of ls 5039 (the optical component) were measured by casares et al. (2005). assuming pseudo-synchronization at periastron, they got i ≈ 200 for the inclination of the orbit and mx = 4.0 ÷ 7.3 m� for the mass of the compact component. this value clearly indicates a black hole. however, using the same radial velocities with the inclination derived by moldon et al. (2012), one gets only mx = 1.3 ÷ 2.7 m� for the mass of the compact component. this value corresponds to a neutron star and is compatible with the observed variability of radio morphology. it seems, that at present we cannot firmly establish the nature of the compact component. the black hole still cannot be excluded but its presence became somewhat doubtful. even if the presence of a black hole in the system would be confirmed, it is clear that the stellar component is not a be star and therefore the system is not a good candidate for a be/black hole binary. 4.1.3 maxi j1836-194 this system was discovered as an x-ray source by maxi in august 2011 (negoro et al. 2011). further observations strongly suggested that the system contains an accreting black hole (spectral states, timing characteristics, ejection of a radio jet). however, to classify the system as a be/black hole binary, we need a second ingredient − namely a be component. initially, it seemed that it is indeed present in the system. cenko et al. (2011) after spectroscopical observations of the optical counterpart with the 8 m gemini south telescope concluded that it is a be star. this finding was questioned by rau et al. (2011), who noted that the archival search of kennea et al. (2011) indicates that the optical counterpart undergoes outbursts of at least 4-5 magnitudes which is very unlikely for a be star. subsequent spectroscopical observations were made by pakull & motch (2011) who used vlt ut1 telescope. they found that the optical spectrum is not that of a be star. in this way, maxi j1836-194 joined the ranks of unsuccessful candidates. 4.2 the first successful candidate 4.2.1 mwc 656 this system was first discovered by agile as a gammma-ray source agl j2241+4454 (williams et al. 2010). the discovery paper identified the optical counterpart as a be star hd 215227 (known also under the name mwc 656) and determined the orbital period as equal 60.37 d. the nature of the optical component (of spectral type b1.5-2iiie) permits no doubts − it is a be star. the nature of the compact component was not established until very recently. casares et al. (2012) measured the amplitude of the radial velocities of mwc 656 and its rotational broadening obtaining 41.7 ± 6.8 km/s and 346 ± 10 km/s respectively. next, they analyzed fe ii lines reflecting the the keplerian rotation in the excretion disc around be star and under some assumptions estimated the inclination of the orbit as i = 67÷800. finally, they estimated the mass of the compact component to be in the range 2.7 to 5.5 m�. this range suggested rather a black hole but a neutron star could not be excluded. taking into account the overall low precision of this estimate, the nature of the compact component remained undecided. authors made more observations and published their analysis in 178 be/x-ray binaries with black holes in the galaxy and in the magellanic clouds a most recent paper in nature (casares et al. 2014). this time they got two sets of radial velocities: they measured the accretion disc emission line he ii 4686 reflecting the orbital motion of the compact component and they improved the measurements of radial velocities of be star by using sharp fe ii lines of the equatorial excretion disc. as a result they could come to a firm conclusion that the compact component is a black hole of the mass 3.8 to 6.9 m�. in this way the first be/black hole binary was finally found! the authors noted that the system seems to be xray quiescent (lx < 1032 erg/s). this led them to a general comment that due to lack of a solid surface and a very low mass transfer rate (leading to extremely long outburst recurrence periods), be binaries with black hole companions might be difficult to detect by conventional x-ray surveys. after completing their work, the authors requested and obtained observing time with xmm newton. they found that the system emits xrays, after all (munar-adrover et al. 2014), but at a very low level lx ≈ 3.7 × 1031 erg/s, similar to the quiescent luminosity of black hole x-ray novae. this result does not change their conclusions. 5 summary during our conference, the statistics of be x-ray binaries in our galaxy indicated that we know 72 such systems. among them, 48 contain a confirmed neutron star and none, so far, is known to contain a black hole. the stellar population synthesis calculations (belczyński & zió lkowski 2009) indicate that the expected ratio of be x-ray binaries with neutron stars to the ones with black holes, fns/bh is equal ∼ 54. this ratio implies that, if we know 48 neutron star systems, then the expected number of black hole systems should be just one. few months after the conference this one system was just found! it is a binary agl j2241+4454/mwc 656. the problem for magellanic clouds remains unsolved (8 expected black hole be x-ray binaries and none observed). acknowledgement this work was partially supported by the polish ministry of science and higher education grant n203 581240 and by the polish national science center project 2012/04/m/st9/00780. references [1] belczyński, k., zió lkowski, j.: 2009, apj 707, 870. doi:10.1088/0004-637x/707/2/870 [2] bodaghee, a., tomsick, j.a., rodriguez, j.: 2009, atel 2252. 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[41] schmidtke, p. c.; cowley, a. p.; udalski, a.: 2013b, atel 5473. [42] sturm, r., haberl, f., coe, m.j. et al.: 2011a, a&a 527, 131. [43] sturm, r., haberl, f., freyberg, m., coe, m., udalski, a.: 2013, atel 4719. doi:10.1086/187542 [44] sturm, r., haberl, f., pietsch, w.:: 2011c, atel 3747. [45] sturm, r., haberl, f., pietsch, w.:: 2011d, atel 3751. [46] sturm, r., haberl, f., pietsch, w., udalski, a.: 2011b, atel 3761. [47] tavani, m., arons, j., kaspi, v.m.: 1994, apj 433, 37. doi:10.1088/2041-8205/723/1/l93 [48] townsend, l.j., coe, m.j. corbet, r.h.d. et al.: 2011, mnras 410, 1813. [49] vasilopoulos, g., sturm, r., haberl, f. et al.: 2013a, atel 5540. [50] vasilopoulos, g., sturm, r., maggi, p., haberl, f.: 2013b, atel 5673. [51] williams, s.j., gies, d.r., matson, r.a. et al.: 2010, apj 723, 93. [52] zió lkowski, j.: 2002, msait 73, 1038 (arxiv:astro-ph/0208455). [53] zió lkowski, j.: 2008, chin.j. a&a suppl.8, 273. [54] zió lkowski, j., belczyński, k.: 2010, unpublished. [55] zió lkowski, j., belczyński, k.: 2011, in frontier objects in astrophysics and particle physics (procs. of the vulcano workshop 2010), f. giovannelli & g. mannocchi (eds.), conference proceedings, italian physical society, editrice compositori, bologna, italy, 103, 511 (arxiv:1111.2330). 180 http://dx.doi.org/10.1007/s10509-010-0575-8 http://dx.doi.org/10.1086/187542 http://dx.doi.org/10.1088/2041-8205/723/1/l93 introduction properties of be/x-ray binaries new be/x-ray binaries candidates proposed for be/black hole x-ray binaries unsuccessful candidates ls i +610 303 ls 5039 maxi j1836-194 the first successful candidate mwc 656 summary acta polytechnica ctu proceedings doi:10.14311/app.2015.1.0022 acta polytechnica ctu proceedings 2:22–28, 2015 © czech technical university in prague, 2015 available online at http://ojs.cvut.cz/ojs/index.php/app vector maps in mobile robotics ales jelinek central european institute of technology, brno university of technology, technicka 10, brno, czech republic correspondence: alesjelinek@ceitec.vutbr.cz abstract. the aim of this paper is to provide a brief overview of vector map techniques used in mobile robotics and to present current state of the research in this field at the brno university of technology. vector maps are described as a part of the simultaneous localization and mapping (slam) problem in the environment without artificial landmarks or global navigation system. the paper describes algorithms from data acquisition to map building but particular emphasis is put on segmentation, line extraction and scan matching algorithms. all significant algorithms are illustrated with experimental results. keywords: robotics, slam, vector map, point cloud, edge extraction. 1. introduction mapping in robotics is a subject of research for a number of years and large progress was already achieved. paper [1] describes theoretical way, how to build and update a consistent map, which converges to a precise image of the real environment (at certain level of detail). through the years, more improvements and new algorithms were invented for this task, good tutorial papers are for example [2] [3], or the book [4]. formulation and mathematical description of the slam problem is unified and generally accepted today, but a complete solution for 3d dynamic environment is still not known and slam as a whole is still under active research. the most of today’s work in the field is concentrated on two main bottlenecks of known algorithms: (1.) computational optimization. every map contains some data describing the real environment. computational efficiency is usually evaluated in big o notation with respect to n, reflecting the number of cells in an evidence-grid map, the number of landmarks in a geometric map, etc. non-optimized solutions have o(n2) or even exponential complexity, but several algorithms are more efficient, for example fastslam [5] with o(m log(n)) complexity (where n is the number of landmarks and m the number of particles in the rao-blackwellized filter). this algorithm can handle orders of magnitude more landmarks than o(n2) solutions. computational efficiency is a key to large maps with a lot of details. (2.) feature recognition and matching. robust and reliable feature (landmark) extracting and matching is crucial for most of slam algorithms. new data has to be associated with older measurements precisely, or at least with negligible number of mismatches. feature extraction is needed when camera or laser scanner is used to provide information about the robot surroundings. for example corners and t-junctions are usually searched in input data and then the whole pattern is correlated with an already known map. several complications may arise, because the same feature may look different from different points of view and data registration in its straightforward implementation is exponentially complex task. data structure of a map is closely related to both of these problems. operations executed on the map have to be as fast as possible especially updates with the new information and feature search/comparison are crucial. representation of obstacles, free space and unexplored areas effects feature recognition robustness. another attribute of a map is its ability to approximate the real environment. importance of this attribute depends on further usage of the map. if the robot is meant to explore unknown area and provide information about it, requirements will be probably higher than in case of a robot, which just needs to avoid obstacles and memorize a short history of its path. there are more possible ways to represent a robotic map. one of the most common is robot evidence grid, which parcels continuous world into a set of squares (cubes in 3d). size of a square is optional and may be even adaptive to better fit the reality, but this style of approximation of smooth world is still rather crude, because straight edges which are not co-linear with grid lines are jagged regardless of grid resolution. evidence grids are widely used and well established in many applications, where this downside is negligible. visually better results are achieved with vector maps, where edges are represented with line segments. good example of classical vector based mapping system is vecslam described in [6]. the aim of authors work is to create a system for high quality mapping, therefore vector maps were chosen as a good approximation of the real world. map representation is only one part of the problem. robot exploring unknown environment needs 22 http://dx.doi.org/10.14311/app.2015.1.0022 http://ojs.cvut.cz/ojs/index.php/app vol. 2/2015 vector maps in mobile robotics to update its map with new information. data are usually obtained from rangefinder sensors such as laser scanners and sonars in the form of a point cloud and need to be incorporated in the current map. probably the most used technique for point cloud registration is iterative closest point (icp). good description and historical survey of this method is available in [7]. efficient variants of this method were published in [8]. furthermore, it is possible to use icp for registration of more complex formations, such as surfaces of scanned objects. this approach is described in [9] and [10]. there are several alternatives to icp, which are trying to generalize the notion of “closeness” or “similarity” from points to lines, triangles etc. similarity of points is usually measured as their euclidean distance. an edge is often described as a segment of a line. having two such segments, we can define an area they demarcate and use it as a measure of similarity. this definition is not unified and it is possible to find several different approaches, for example sum of squared distances from point in a scan to the nearest edge in the map [11], penalizing function of “non collinearity” and spatial distance [12], or a criterion based on newly introduced matrix scalar product [13]. another interesting approach is critical ray method proposed in [14], which does not use line similarity at all. diversity of these approaches is high and none of them is considered to be remarkably better than the others, therefore the author have decided to develop his own method and test new ideas, because this field of research is definitely not fully explored. reducing point cloud to a set of line segments (in 2d) or triangles (in 3d) has very useful properties. at first, information from hundreds or thousands of points is expressed with (at most) tens of objects. data reduced in count are processed faster and therefore more complex algorithms may be used. on the other hand, mathematics becomes more complicated, because lines and faces have more degrees of freedom and constraints than points and as written above, similarity is not as easy to enumerate. the process of line extraction has generalizing ability. after interpolation by line segments (or triangles), corners become sharper and noise is suppressed, which results in better looking (more corresponding to the real world) map. in addition (depending on line extraction algorithm) edges might be estimated with higher accuracy than single point due to averaging effect. there is no restriction on using n − 1 dimensional objects in n dimensional space. a generalization of icp for lines in 3d space is described in [15]. paper [16] describes whole set of algorithms for matching sets of lines in 3d and many others are possible to find. for even better approximation of the real world, curves and curved planes could be used. these are more complicated for computation and not too much papers are related to this topic. an example of such approach is a method [17] based on graph theory. 2. point cloud processing system the overall diagram of the measurement and mapping process is depicted in fig. 1. every time a measurement is acquired, the whole process is run through. each rectangular box in the diagram means one algorithm performing operation on its input data. the whole process leads to update of the map the robot creates and the pose of the robot itself. slam itself is implemented in a very elementary way and no attempts to build converging map were made yet. the main objective in current state of development is to test data processing, edge extraction and scan registration algorithms. laser scanner used to obtain all data in this chapter is velodyne 32 hdl, which provides approximately two thousand points (per turn) in polar coordinates for each of its thirty two lasers. only horizontal set of measurements was taken into account for 2d map. at the beginning, all data from sensors need to be converted into the data format useful for following algorithms. this step also ensures usability of the system for any instrumentation with suitable properties. a disadvantage of this process is a certain enlargement of data size, because laser scanners and other sensors usually use some sort of data compression to minimize data flow. in case of velodyne 32 hdl this means conversion from 16-bit integer to 32-bit floating point number. to speed up corresponding edge selection, crude pose estimation is useful. it enables to specify part of the map, where the robot most probably is, and therefore, the search space of correspondences is reduced a lot. as is well known in robotics community, techniques such as inertial sensors or odometry cause integration of error of pose estimation. this makes them useless after a certain amount of time. in the presented algorithm, these are only used for measurement of relative pose change between two following scans. this ensures that the estimated pose error is always in a known limit. to get an absolute pose, this estimation is added to the last known pose, determined in the previous iteration of the data processing (dashed arrow leading to “pose estimation” block in fig. 1). 2.1. filtering and clustering treatment of raw point cloud is a more complex task. at first it is necessary to filter out noise and outliers and to find dense clusters of points defining edges of solid objects in the environment. raw data from one set of measurements are shown in fig. 2a. it is clear that scans are full of irrelevant points and odometry was not very accurate. some noise is always present. laser scanner measures distance with certain precision, which is stated in the datasheet. the other sake of noise is too dissected environment, where individual faces of objects 23 ales jelinek acta polytechnica ctu proceedings measured data conversion from scanner data format to cartesian and polar coordinate system point cloud segmentation and filtering edge extraction corresponding edge selection finding the best transformation for incorporation of the scan in a map map update map inertial sensors pose estimation most probable pose pose correction data flow data from previous step scanner data processing operation result conversion form scanner data format to common physical quantities figure 1. overall scheme of point cloud processing system from data acquisition to map and pose update. are so small that rangefinder cannot scan them properly. a good examples are treetops and bushes. noisy parts of point cloud are best to treat as a solid body with defined borders and density. other possibility is to filter them out, which causes loss of information, but on the other hand, with a careful filtering, it is possible to “see” through low density objects (e.g., see wall behind a bush). outliers in point cloud are usually caused by scanning too distant or too close objects, which are out of the range of the particular laser scanner. these are easy to identify and can be removed without serious impact on the quality of a scan. more interesting to deal with are outliers originating from a reflection. in a common environment, there can always be objects, which are able to reflect laser beam and corrupt the measurement. if the reflecting object is small and curved, few beams, which hit it, are scattered wide apart and appear as randomly distributed single points in a point cloud. these are generally easy to remove. another case are large, flat objects such as mirrors and windows, which uniformly reflect a large amount of rangefinder beams. this effect causes phantom objects to appear in the scan and there is probably no way to detect this without additional sensors or a set of scans from different positions. clustering is used to remove all unnecessary points from a scan and to determine dense clusters of points, which could potentially form an edge of a real object. an algorithm used to get result depicted in fig. 2b is as follows: from the laser scanner we get data sorted by an angle. algorithm proceeds from one point to another and checks if k previous points are closer or farther, than a certain distance. three alternatives may occur. a point might be too far away from all of the previous ones. this leads to establishment of a new cluster. if the working point is close enough to some previous points and all these points belong to the same cluster, the working point is added to it. third case arises, when the working point can belong to more than one cluster. in such a situation, all those clusters and the working point are joined together. in the end, clusters with the size under a certain threshold are called outliers and are removed from the scan. from a practical point of view, it is wise to make the distance comparison threshold adaptive, because the farther the detected obstacle is, the sparser the measured points are. scaling the threshold linearly with the distance between the working point and the robots position is a good strategy. the proposed algorithm safely removes noise from too dissected objects as well as random outliers, because these create large number of very small clusters (typically less than ten points), which are removed in the final stage of the process. phantom objects are not recognized. noise caused by laser scanner itself removes the following algorithm for line extraction. this theme is directly related to line simplification algorithms (because points in a scan are sorted) and both of these are discussed in a lot of fields of re24 vol. 2/2015 vector maps in mobile robotics (a) . raw data. (b) . segmentation. (c) . line extraction. (d) . complete map. figure 2. a) depiction of all measured point clouds (yellow) with estimated robot path (green). no scan fitting or other postprocessing is used, image corresponds to raw data from sensors. b) segmentation of one scan is shown on this figure. each color means a cluster, which is believed to be continuous edge in reality and which is separate from the others. noise and outliers are filtered out and not displayed. c) line extraction in segmented point cloud (black). each cluster is approximated by a line or a poly-line (red). d) a map composed using the line similarity criterion. red edges are long enough to participate in scan fitting process, blue edges are shorter and just add details to the map. green trajectory is acquired from odometry and dark blue one is an estimation of true trajectory. search. in addition to robotics, similar approaches can be found in cartography, computer vision and computer graphics. plenty of algorithms were developed during last decades, having different properties, such as speed, memory requirements and quality of approximation. good survey comparing line extraction/simplification algorithms in robotics is [18]. results of this paper clearly show that algorithms such as ransac or hough transform are not fast enough for online processing of point clouds. good performance was observed when using splitmerge, incremental and line regression algorithms. split-merge (also known as douglas-peucker algorithm [19]) was the fastest one and belongs to wide family of o(n) and o(n log(n)) complex algorithms used in cartography [20]. main drawback of these algorithms is that they are based on point elimination, and therefore, a lot of information is discarded. the edge extraction algorithm from the diagram in fig. 1 is based on line regression and works as follows: it passes through the cluster and computes the least square approximation and the variance of selected set of points. if the variance gets over predefined limit, the line is saved, and algorithm proceeds computing new line. the last line terminates at the end of the cluster. this approach is advantageous, because all points contributes to the result and contained information is better utilized. although loss of information was overcome by the least squares approximation, the algorithm is still not optimal in terms of “best fit poly-line”. all but the last line have maximal permitted variance, which means, that for too high threshold lines go over corners and an approximation is worse, than it could be. more technically, the total sum of squared distances from each point to its regression line is higher, than is achievable with given number of lines. fine tuning of the threshold is therefore necessary. complexity of the algorithm is o(n). result of line extraction is depicted in fig. 2c. 2.2. scan fitting when updating a map with a new scan, corresponding edges must be selected at first. it is responsibility of an operator or a path planing algorithm to obtain new scans frequently enough to ensure overlap of a new scan and the map. this means the robot always has to see part of the already known environment (except the first scan of course). acquiring more scans from one location leads to a more precise map (averaging effect). scan fitting is the point, where crude pose estimation comes in useful, because searching through the whole map would be very computationally expensive. knowing approximate pose and its maximal error allows us to considerably reduce search space and keep computational complexity constant, independent on the size of the whole map (assuming the number of visible details is comparable across the map). if the robot is suddenly moved far away from its previous location, it becomes lost and the algorithm is not capable of working correctly anymore. only long enough edges are used for the process, because the shorter ones are not determined with a sufficient precision. the maximal angular error of the pose estimation is directly used as the maximal angle between possibly similar edges. if the angle is inside a tolerance, shortest distances of end points of first edge to the second edge are computed. if at least 25 ales jelinek acta polytechnica ctu proceedings one is shorter than maximal permitted shift between two scans, edges are overlapping each other and can belong to one real edge. there are three possible situations after this step. for some edges from the new scan, there is no similar one in the map. these probably belong to an area which was not explored yet, or where only short edges were determined. new edges do not contribute to scan fitting process. the second group of new edges has one similar match in the map and these are directly used for scan matching. in the last group, there are edges with more than one possible match. at this situation, it is hard to say, which possible pair is the best one, or if more edges should be connected together. current practice is to remove edges already used in the second group and from the rest to select the closest one (in the sense of overlapping). in rare cases, the edges corresponding in real world are not the closest ones. this leads to mismatch and can even corrupt the map, but in most cases, correctly matched edges prevail and the mismatch is unnoticeable. at this point, pairs of corresponding edges from the new scan and the map are known and the actual fitting may take place. as well as in the previous step, the line similarity criterion will be used, but now with slightly different properties. an idea, that lines are more similar as the angle they form is smaller is still true, but overlapping criterion used before is not advantageous. instead, as already mentioned in the introduction, an area defined by both edges is used. the main idea of the criterion is depicted in fig. 3. let two edges be defined by lines p and q with the end points ab and cd. at first, an axis of angle formed by these edges is found. then, for all end points, their perpendicular projections (with respect to the axis o) on an opposite line are found. two end points and their projections form a quadrangle as shown in fig. 3 for points ab (both cases). there are six possible quadrangles and the largest one has to be used for the criterion enumeration. the square of that area is used as a similarity metric. the function for the similarity enumeration is not strictly convex, therefore for one pair of edges, there is not a single minimum defining one pose in which both edges are the most similar. instead, there is an infinite number of possible poses, in which the criterion is zero. this property is clear from the geometrical visualization of collinear edges sliding over each other and corresponds to the problem of localization in a long corridor. if a robot “sees” only collinear walls, it is not able to determine the displacement along an axis of the corridor one degree of freedom cannot be estimated from available data. for an exact solution, at least two skew pairs of edges must be used. fitting itself is an iterative process, because no closed form solution was found so far. a new scan is transformed using the standard homogeneous transformation. the goal is to find such translation and (a) . no intersection. (b) . with intersection. figure 3. line segments similarity criterion. the smaller is the gray area, the more similar are both line segments. rotation, so that the sum of the squared areas of all edge pairs is the smallest possible. nelder-mead simplex method was used to find the global minimum. for longer edges, the area they demarcate is large even if an angle they form is relatively small. this means, that longer edges have greater impact on scan fitting, which is correct, because long edges are determined by more points, and therefore, be more precisely known. 2.3. map building after the fitting process is finished, a new scan is transformed using the found parameters and edge pairs are joined to form a new set of edges in updated map. the same transformation, which was used to update the map, is applied on the path estimate to correct the odometry error. assuming static environment, the information about pose gotten from scan fitting is absolute, and therefore, an error should not have integrative characteristics, however, this is ideal state which requires a precise map corresponding to the environment. the main problem of map building process in current state of development is that the map does not converge. scans are incrementally fitted to the map, but new measurement influences only the part of the map, which is currently visible and new information is not propagated through the whole map to assure convergence. in other words, change in length of one edge should affect all connected edges (including those which are not actually seen), but current implementation is not able to handle this. integrative 26 vol. 2/2015 vector maps in mobile robotics figure 4. a larger map composed using the presented processing system. edges are colored in the same way as in fig. 2d. gray trajectory is acquired from odometry and dark blue one is an estimation of the true trajectory. characteristics of error of pose and map is therefore not suppressed. on the other hand, using edges and line similarity criterion for scan fitting is very accurate and divergence process is much slower. results of this step are maps in fig. 2d and fig. 4. in comparison with a naive scan merging in fig. 2a, new maps are much more usable for navigation as well as environment documentation. further processing for even better results can follow at this point, one example of possible operations is additional merging of shorter edges (blue edges in fig. 2d and fig. 4) to form a cleaner map. 2.4. experimental results practical testing was made in office and laboratory environment. algorithms based on edge detection are well suited for such application, because artificial objects are usually simply shaped with a lot of flat surfaces. on the contrary, a natural environment is much more complicated with lot of details and lack of flat surfaces, therefore effective line extraction would be very complicated or even impossible. the robot used for testing was orpheus x3, which is four-wheeled vehicle with differential steering. laser scanner used was velodyne 32 hdl. during the experiments, the robot was manually operated and all measurements were taken, when the robot was not moving. the first experiment used for demonstration of the processing pipeline is depicted in fig. 2a to fig. 2d. ten measurements 60 centimeters apart were taken. the odometry error was intentionally increased to demonstrate correction ability of scan fitting algorithm. outliers and noise filtration was also proved to be working, for example small cloud of points on top of fig. 2a was correctly removed. the second experiment was made in a larger scale on a corridor and resulting map is shown in fig. 4. robot moved from starting position to the end of the corridor and then returned back. total length of the traveled path was 46.710 meters and 33 measurements were taken along the way. the difference between the real and the estimated position of the last point of trajectory was only 6 mm, which is even less than the precision of used laser scanner (20 mm). the experiment was held only once, therefore repeatability is not yet determined. fairly good results are caused by two main factors. at first, the line extraction algorithm with the least squares approximation is capable of reducing noise through averaging and provide more accurate edge positions than single points in a point cloud. the second reason is that the robot moves in one room and always sees edges from the first scan, therefore an error of map and pose is not integrating. if the robot would move along a path with a lot of turns and after some time would not see its starting location, this problem would start to manifest. however, these experiments were made to proof the concept of scan fitting via edge similarity criterion and slam itself is not yet at the center of the research. 3. conclusion and future work the paper presents the set of algorithms used to process data from laser scanner and build a vector based map. the whole scheme of the process is depicted in fig. 1. most algorithms used are new and still under testing, but findings stated in literature (e.g., [10], [12], [16]) were proved to be true, because scan matching based on edge detection yields quality results and definitely can be used for solving slam problem. at least, considering results in fig. 2d and fig. 4, current state of the research is very promising. the main task for the nearest future is development of good representation of the topological-metric map, to enable a real slam to be implemented. topological information is necessary for visible (or just close) edges finding algorithm and for path planning. metric information is crucial for mapping itself, scan matching, and path planning. term “good representation” means such data structure, that would be efficient for search and computing algorithms. nearest neighbor of polygon search or finding an edge in area with certain coordinates are only a few examples of problems which are necessary to be efficient in a good mapping algorithm. the second requirement expected from a good map is a convergence. as the robot explores surrounding 27 ales jelinek acta polytechnica ctu proceedings environment, the map should adapt to be closer to reality. this is not achieved now and lot of work is focused on this task. with an authentic map and well working fitting algorithm, localization itself should not be too complicated and a solution for the slam problem using vector maps should be completed (at least in its main aspects). acknowledgements this work was supported by the project ceitec central european institute of technology (cz.1.05/1.1.00/02.0068) financed from european regional development fund. references [1] m. dissanayake, p. newman, s. clark, et al. a solution to the simultaneous localization and map building (slam) problem. ieee transactions on robotics and automation 17(3):229–241, 2001. doi:10.1109/70.938381. [2] h. durrant-whyte, t. bailey. simultaneous localization and mapping: part i. ieee robotics & automation magazine 13(2):99–110, 2006. doi:10.1109/mra.2006.1638022. [3] t. bailey, h. durrant-whyte. simultaneous localization and mapping (slam): part ii. ieee robotics & automation magazine 13(3):108–117, 2006. doi:10.1109/mra.2006.1678144. [4] s. thrun, w. burgard, d. fox. probabilistic robotics. the mit press, 2005. [5] m. montemerlo, s. thrun, d. koller, b. wegbreit. fastslam: a factored solution to the simultaneous localization and mapping problem. aaai/iaai 2002. [6] h. j. sohn, b. k. kim. vecslam: an efficient vectorbased slam algorithm for indoor environments. journal of intelligent and robotic systems 56(3):301–318, 2009. doi:10.1007/s10846-009-9313-2. [7] l. oswald. recent development of the iterative closest point algorithm, 2010. [8] s. rusinkiewicz, m. levoy. efficient variants of the icp algorithm. proceedings third international conference on 3-d digital imaging and modeling pp. 145–152. doi:10.1109/im.2001.924423. [9] p. besl, h. mckay. a method for registration of 3-d shapes. ieee transactions on pattern analysis and machine intelligence 14(2):239–256, 1992. doi:10.1109/34.121791. [10] z. zhang. iterative point matching for registration of free-form curves and surfaces. international journal of computer vision 13(2):119–152, 1994. [11] h. pottmann, s. leopoldseder, m. hofer. registration without icp. computer vision and image understanding 95(1):54–71, 2004. doi:10.1016/j.cviu.2004.04.002. [12] j. elseberg, r. t. creed, r. lakaemper. a line segment based system for 2d global mapping. 2010 ieee international conference on robotics and automation pp. 3924–3931, 2010. doi:10.1109/robot.2010.5509138. [13] q. li, j. griffiths. iterative closest geometric objects registration. computers & mathematics with applications 40(10-11):1171–1188, 2000. doi:10.1016/s0898-1221(00)00230-3. [14] e. tsardoulias, l. petrou. critical rays scan match slam. journal of intelligent & robotic systems 72(3-4):441–462, 2013. doi:10.1007/s10846-012-9811-5. [15] m. alshawa. icl : iterative closest line a novel point cloud registration algorithm based on linear features. ekscentar (10):53–59, 2007. [16] b. kamgar-parsi, b. kamgar-parsi. algorithms for matching 3d line sets. ieee transactions on pattern analysis and machine intelligence 26(5):582–93, 2004. doi:10.1109/tpami.2004.1273930. [17] k. demarsin, d. vanderstraeten, t. volodine, d. roose. detection of closed sharp edges in point clouds using normal estimation and graph theory. computer-aided design 39(4):276–283, 2007. doi:10.1016/j.cad.2006.12.005. [18] v. nguyen, s. gächter, a. martinelli, et al. a comparison of line extraction algorithms using 2d range data for indoor mobile robotics. autonomous robots 23(2):97–111, 2007. doi:10.1007/s10514-007-9034-y. [19] d. h. douglas, t. k. peucker. algorithms for the reduction of the number of points required to represent a diditized line or its caricature. cartographica: the international journal for geographic information and geovisualization 10(2):112–122, 1973. doi:10.3138/fm57-6770-u75u-7727. [20] w. shi, c. cheung. performance evaluation of line simplification algorithms for vector generalization. the cartographic journal 43(1):27–44, 2006. doi:10.1179/000870406x93490. 28 http://dx.doi.org/10.1109/70.938381 http://dx.doi.org/10.1109/mra.2006.1638022 http://dx.doi.org/10.1109/mra.2006.1678144 http://dx.doi.org/10.1007/s10846-009-9313-2 http://dx.doi.org/10.1109/im.2001.924423 http://dx.doi.org/10.1109/34.121791 http://dx.doi.org/10.1016/j.cviu.2004.04.002 http://dx.doi.org/10.1109/robot.2010.5509138 http://dx.doi.org/10.1016/s0898-1221(00)00230-3 http://dx.doi.org/10.1007/s10846-012-9811-5 http://dx.doi.org/10.1109/tpami.2004.1273930 http://dx.doi.org/10.1016/j.cad.2006.12.005 http://dx.doi.org/10.1007/s10514-007-9034-y http://dx.doi.org/10.3138/fm57-6770-u75u-7727 http://dx.doi.org/10.1179/000870406x93490 acta polytechnica ctu proceedings 2:22–28, 2015 1 introduction 2 point cloud processing system 2.1 filtering and clustering 2.2 scan fitting 2.3 map building 2.4 experimental results 3 conclusion and future work acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.12.0024 acta polytechnica ctu proceedings 12:24–31, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app development of an electric bicycle for a sharing system in prague william deleenheera,∗, lukáš jánešb, akshaya jayakumarb a kuleuven, faculty of industrial engineering, gebroeders de smetstraat 1, 9000 gent, belgium b czech technical university in prague, faculty of transportation sciences, department of vehicle technology. konviktská 20, 110 00 prague ∗ corresponding author: william.deleenheer@gmail.com abstract. by means of a development of an e-bike sharing system the electromobility project wants to provide an alternative way of comfortable transportation for students and staff of the ctu, primarily to commute between different campuses. the research for this project contains at least three different fields of study, namely electric vehicle and docking station development, intelligent transport systems and management and economics of transportation and telecommunication. after briefly stating general requirements for the sharing system, this paper focuses on the development of the electric bicycle. first an ideal bike design is defined. then necessary motor power and battery capacity are calculated by estimating characteristics of cycling in prague. a prototype was developed by converting a normal bicycle to an electric bicycle. being equipped with devices for e-bike monitoring, controlling and data recording for a post trip analysis, this prototype is also intended to have an educational value for future students in the project. results consist of an electrical bicycle configuration that matches the requirements and a sketch of an ideal e-bike for this project. keywords: e-bike sharing, requirements, e-bike design, motor power, battery capacity. 1. introduction the demand and supply of electric bicycles is a fastgrowing market. a market study on e-bike purchasing has increased for this year, mainly in the netherlands, denmark and germany. it is said that the market first concentrated on the netherlands and germany due to its overall size. figure 1. e-bike unit sales per 1000 inhabitants in 2015, data from ecf advocacy group’s publication[1]. but eventually the per head market demand increase in switzerland, austria, denmark proved to be relatively stronger. customers start to have innumerable options to combine any kind of bicycle with different sorts of batteries and motors at a wide range of prices. nevertheless, to compose a suitable e-bike for a sharing system is less easy. first of all, a responsibility that comes with owning a bicycle lies not with the end user anymore and thus the user has no incentive to care for it or maintain it. and second a sharing system takes into account many bicycles thus the cost of maintenance or theft as well as an initial investment of one e-bike should be as low as possible. furthermore, there are some requirements for a successful and economically viable sharing system, mostly regarding user experience, such as safety and comfort. this paper has tried to list these requirements and develop an electric bicycle accordingly. 2. general requirements for the sharing system determining the requirements for a viable e-bike sharing system for the ctu but also for prague in general has been carried out in three ways. in the first place, there was an existing project vision that originated both in the project goal as in earlier research. then more detailed requirements were defined by a research of existing examples in the academic world and in the market. finally, the requirements as for the station and software for an initial pilot project were summarized. 24 http://dx.doi.org/10.14311/app.2017.12.0024 http://ojs.cvut.cz/ojs/index.php/app vol. 12/2017 development of an electric bicycle in prague 2.1. project vision the primary goal of this project is to provide a more efficient way of transportation for students and staff of the faculty of transportation science as a means to commute among different faculty buildings. the challenge exists in achieving this goal without losing comfort that comes with using a currently available public transport system. the concept of comfort in this context can be specified in four clear requirements: • minimal human physical effort, • protection against bad weather conditions, • possibility to transport certain cargo, • easy access to the system. a priority condition for all other requirements is obviously safety, all the more because cyclists are vulnerable road users and the bicycle infrastructure is still limited in prague. 2.2. market research market examples and previous experience with both conventional bike sharing schemes as well as a few existing e-bike sharing schemes such as go bike[2], bewegen.com[3], bonopark[4] and cycleushare[5] were researched to define components of a successful e-bike sharing system. another useful source was the experience of the institute of transportation and development policy (itdp)[6] with planning and exploitation of bike sharing systems. the following characteristics have been found repeatedly and are here briefly summarized: • integrated and theft protected e-bike components (motor, battery, chain, lights, wires, hid, automated lock); • ergonomic bicycle design (step-thru frame with adjustable saddle); • user friendly bicycle checkout and payment procedures; • high station density (10-16 stations for every square kilometre for conventional bikes); • many bicycles (10-30 bikes for every 1,000 residents for conventional bikes); • large coverage area (10 square kilometres for conventional bikes); • others: auxiliary (digital) lock, gps tracking, modular docks. discussable options are a use of high-end integrated components such as internal gears, belt drives or puncture free tires that reduce maintenance or theft costs but require higher initial investment. the university of brighton in uk conducted a similar e-bike research. the research aimed to understand user needs and to develop a system design necessary to start a fleet of e-bike program. the main outcome was a development of a "smart tracking system" which was implemented in a few e-cycles and proved successful. the system autonomously recorded and transmitted a bikes position, route, level of assistance required in real time and then sent it all in an online interface which was used for both research analysis and participant review. this proved to be an efficient solution for the fleet management and theft control. most of the users were daily commuters to office, the surveys revealed that most of them had found it easy to use and that it was something which had not disturbed or damaged their clothing much. 2.3. station and software requirements this project opted for a system in which the batteries have to be rented and plugged onto a bike by the user. this concept of battery charging and vending machine was first used in the "cycleushare project"[5]. the main advantage is that the station can have more batteries than bicycles and thus always has a fully charged battery for the user. in this concept all the batteries are stored in one charging box which protects the batteries from weather conditions and theft. this way the charging system and the bicycle docks can be made much cheaper compared to a more common way in which every dock needs a charger and the battery is integrated in the bicycle. another advantage is that the batteries, which mostly have a shorter life span than the bicycles themselves, can be maintained or replaced very easily. the biggest disadvantage is a decreased ease of use since the check in and check out procedure involves handling a battery. more experience is needed to determine an exact opportunity cost of this concept. the system is required to be an intelligent system. this includes necessity of mutual communication between the user, server, station, bicycle and battery. the tools to be used for this communication are isic student cards (rfid), gps tracking, rfid controlled locks, hid’s, system managing software and a web application. the main requirements for the software are based on the characteristics of sharing software like the one from "opensourcebikeshare"[7] and general requirements. crucial properties of the software interacting with the users via a web application are a map with real time data about station proximity and bicycle availability, instructions and help for users, feedback from users, reward system for a balanced e-bike distribution. additionally, it could have a routing tool if this is not integrated in the e-bicycle hid. the gui interacting with the administrators needs to provide data about system usage and provide a possibility to manage the fleet in real-time. this is possible via communication with rfid and gps tracking devices or if you like on docks and bicycles as well as user feedback. additionally, it will be connected to the battery charging machines which will provide data about battery state, such as number of cycles and usage patterns. 25 w. deleenheer, l. jáneš, a. jayakumar acta polytechnica ctu proceedings 3. electric bicycle research and design the above stated requirements have been applied on a development of a suitable electric bike. this involved researching an optimal bicycle design as well as a simulating power output and energy consumption during cycling to determine necessary motor and battery specifications. 3.1. bicycle design properties of bicycles in an average bike-sharing scheme are already a good approach to what a comfortable e-bike should look like. they are city-bikes with a step-thru frame, a rear rack for panniers or a basket mounted to the handlebars. with regards to cobblestone streets in prague it is desirable to have some form of suspension. e-bikes with the same purpose should have a similar design except the design also involves a decision about where to place a motor and battery. the requirement of a minimal human effort includes optimal handling and steering behaviour of the bike. the centre of a mass of the rider-bike system affects this behaviour. in fact, the act of cycling is known to be a fairly complex mechanism. in addition to the rider’s skill and gyroscopic forces, there are, acting on the wheel, the centre of gravity lowering torque and castoring forces[8]. in the context of this project we can simplify it by saying that keeping a bicycle from falling comes down to keeping the centre of mass of the rider-bike system over its wheels. at very low speeds or when coming to a halt, the bike is easier to handle with a low centre of mass because thanks to the the leverage, the rider also needs to apply relatively small forces on the handlebars to keep the bike upright. from a certain minimum forward speed, it is easier to steer a bike with a higher centre of mass. f for the same reason it is easier to balance a tall broomstick on the end than a short pencil. the broomstick is a slower inverted pendulum for which one has more time to bring it back to balance[9]. on the other hand, as it is the case for normal bicycles, the mass of the rider still has the most impact on the overall centre of mass of the coupled electric bike – rider system. thus for a placement of a battery and motor it is sufficient to look at handling behaviour at very slow speeds or standstill. furthermore, taking in consideration the idea of transporting certain cargo on the rear rack it is preferable to have the battery weight inside the frame for a better mass distribution, for a minimal inertia high in the rear and thus for a safe and comfortable ride. the decision to choose a mid-drive motor contributes to this logic but is also a consequence of reasons stated in the next paragraph. disadvantages of hub motors are an increased unsprang weight and a more difficult maintenance. apart from an extra mass added to the bicycle, the motor and battery need extra space. one idea on this matter is to use smaller wheels (24 to 18 inch) which are already often used in cargo bikes for this reason. smaller wheels also lower the overall centre of the mass and enable higher acceleration amongst other advantages[10]. one disadvantage is a decreased cushioning. a compromise could be only to have a smaller rear wheel. figure 2. e-bike design: sketch by the writer, scale 1/10. to visualize the previously outlined ideas, the above draft of a possible e-bike design was sketched, keeping in mind low cost, easy fabrication for example with standard aluminum tubes. this draft could be a base for a more advanced (e.g. with integrated components) and attractive design that can be validated with a strength analysis. a last point to look at is a protection against wind, rain and sunlight. there are some solutions on the market to solve this problem, such as detachable shields or poncho’s. in case a full integration of this feature is opted, it is recognizable that the lower the rider sits to the ground the easier it is to design a cover/shield that protects a full body of the rider from the impact of precipitation and wind owing to its forward movement. 3.2. motor the main specification of an electric bike motor is its power. on the market the motors are distinguished by an electrical power they can infinitely continuously handle, for example "a 250 watt motor". this figue is misleading because of two reasons: the input power the motor uses is determined by the voltage of the battery multiplied by the current the controller draws from the battery (e.g. 36v × 15a = 540 watt). the motor will mostly be built for a certain voltage (e.g. a 36v 250 watt motor with a 36v battery) so the maximum power will be proportional to a current limit in the controller. secondly the electrical power is not equal to an output power on the axis of the motor because of internal losses. the latter one is the power assisting the rider in giving a bicycle a forward motion. the average efficiency η of most motors on the market is around 80% at the optimal rpm so 350 watts into the controller will result in 280 watts of a driving power[11]. 26 vol. 12/2017 development of an electric bicycle in prague minimal human effort and a possibility to transport certain cargo are the two initial requirements which come in to play when determining required motor power for this project. in other words, it can be stated that cycling should not be experienced as an exercise and the user can go from a to b in normal clothing without sweating (disregarding the influence of abnormal values for humidity and ambient temperature). the question is which human output power corresponds to this requirement. professional cyclists can sustain 400 watts of leg power for an hour while for a person of an average health and fitness this would be 100 to 200 watts. these values apply for exercise till exhaustion[12]. for a comfortable commuting a continuous human power output of 50 watts is decided to be a reasonable maximum. this amount is comparable to the power needed for a person of 80kg to walk 1 m/s[13]. the last steps in defining a necessary motor power consist first of all of specifying a required driving power for cycling as a function of speed [km/h] and uphill slope [%] and last of simulating required performances for cycling in prague. at a constant speed the driver and motor combined have to overcome three forces: (1.) rolling resistance (frol), frol = mtot × g × cr where: mtot = mass of the rider-bike system, g = gravitational acceleration (9.81 m/s2) and cr = rolling resistance coefficient (±0.006 for normal tire) (2.) aerodynamic resistance (faer), faer = 1 2 × ρ× v2 × cw ×af where: ρ = air density (±1.20 kg/m3 for 20°c and 1 atm), v = bicycle speed [m/s], cw = air resistance coefficient (±1.1 for upright cyclist plus touring bike) and af = frontal surface area (0.6 m2 for upright cyclist) (3.) inclination resistance (fincl), fincl = mtot × g × sinα where: mtot = mass of the rider-bike system, g = gravitational acceleration (9.81 m/s2) and α = is the inclination grade in degrees then ftot = frol + faer + fincl pdriving,tot = ftot × v assumption for mtot = mdriver + mloadedbicycle = 75 + 35 = 110kg. all assumptions were made with a rather inefficient but still realistic set up in mind. the chosen parameter values are the result of a comparison of [12] and [14]. on figure 3: power input during acceleration => from 0 to 25km/h in 3 seconds => f = m×(v2−v1)/t. figure 3. driving power for speeds up to 50km/h and slopes up to 20%. simulating cycling in prague is a rather subjective process but as for a speed it is relevant to take 25km/h which is the maximum speed to which a motor can assist an electric bike by eu legislation. it is known that prague has uphill slopes up to 15% in the form of short streets. it is preferable these can be done with comfort and without the motor failing. with the above two values as a maximum the necessary driving power will be 1300w. eu legislation restricts a rated power to a maximum of 250w. in fact this stands for a 36v motor with a 15a controller which means this motor will be able to handle 540w although not continuously. in the latter case the output power will average around 430w which is far below a defined required driving power. as long as continuous comfort is more important for this project than a continuous speed, it is also useful to define a minimum speed. it was arbitrarily chosen to take 10km/h, which is still a double of an average walking speed, as a minimum speed to go uphill. now the maximum necessary total driving power is 472w. providing the rider takes 50w on his behalf, the required motor input power becomes (472 − 50) × 100/80 = 527.5w. it can be recognised that a motor rated as 250w is still insufficient, especially because at low speeds motor efficiency will be lower than 80% and the total mass might be higher. there is a clear preference of a mid-drive motor to a wheel hub motor or a direct drive for implementation in a hilly city like prague since a mid-drive motor can still work in (or closer to) the optimal rpm range at low speeds such as 10km/h provided a good use of the bicycle gears. present extensive e-bike testing and user experience will tell if this was a good simulation. 3.3. battery the battery is a fuel tank for an electric vehicle(ev). the required amount of energy it must store depends on energy consumed in a trip with a certain minimal range or minimal time. a range of 15 to 20km is 27 w. deleenheer, l. jáneš, a. jayakumar acta polytechnica ctu proceedings v [km/h] avgup hill [%] distance [km] #accel etot,el [wh] +human etot,el [wh] throttle mode 15 0 20 1 9.6 93.0 20 0 20 1 67.8 130.3 25 0 20 1 128.3 178.3 25 0 40 1 255.9 355.9 25 0 50 1 319.7 444.7 25 2 5 1 70.1 82.6 25 2 5 10 76.7 89.2 25 2 5 20 84.1 96.6 25 2 10 1 139.5 164.5 25 2 15 1 208.8 246.3 25 2 20 1 278.2 328.2 25 2 30 1 416.9 491.9 20 2 20 1 217.7 280.2 10 5 5 1 79.0 110.2 15 5 5 1 96.2 117.0 20 5 5 1 110.9 126.5 25 5 5 1 126.2 138.7 10 10 1 1 34.5 40.7 10 10 5 1 171.8 203.1 15 10 1 1 38.0 42.2 20 10 1 1 41.1 44.2 20 10 5 1 203.7 219.3 25 10 1 1 44.4 46.9 table 1. estimated energy consumption within 23 different trips. more than enough to cover an area that includes the center of prague and the majority of ctu buildings. the electrical energy e consumed is equal to the time integral of electrical power p(t). if p = constant for certain time interval ∆t, following expression applies: eelectric = pelect × t = η × pdriv,mot × t assuming the same values for the rider-bike system as in the previous section the energy consumption in over 230 trips was simulated by setting discrete values for the following variables: velocity [km/h] (10,15,20,25), average uphill slope [%] (0, 2, 5), distance [km] (1,3,5,10,15,20) and amount of accelerations at 1.388m/s2 (1,5,10). the table below (table ??) shows some of the more relevant possible trips including scenarios that did not fall into the scope of the simulation. the values in yellow show an effect on power and energy of changing this particular variable. the values in orange show trips with an energy consumption of more than 200w in the throttle mode. the values in green show trips which are more typical for a bike sharing system ( <5km & <0.5h). the values in red show trips that require more than 650w of an input power. taking into account that a deep discharge is to be avoided when trying to maximize a battery life span, it can be stated that 150 to 200wh of a stored energy will be more than enough in the context of this project. practically this could be a 36v × 6.6ah or a 25v × 8ah. the main specifications of a battery pack are voltage [v] and amp-hours [ah]. the electrical energy storable in the battery pack can be estimated with this theorem: eelectric = v (t) × i(t) × t where v (t) = rated voltage of the battery pack [v] and i(t) × t = current discharge over time [ah]. for the 36v motor from the previous section and 300wh, equation (7) gives a 36v × 8.3ah (theoretical) battery. in practice, a battery pack is configured by a spot welding a number of cells in series and parallel e.g. 3.6v × 2200mah cells in a 4parallel10serie configuration makes a 36v × 8.8ah battery pack. the number one chemistry for these cells is lithium-ion e.g. lifepo4 (ifr), licoo2 (icr), limn2o4(imr), linicoalo2 (inr), each with its own benefits and downsides. when optimizing this project, it will be highly relevant to compare these chemistries. for the latter examples it can be simplified by stating li-manganese are especially safe, li-iron-phosphate are the most economical (expensive but a high life span) and li-cobalt have the highest specific energy but they need a good bms to be safe[15]. another important property of a cell is its maximum continuous discharge rate. this rate is defined by its c-rate which expresses the time in which a battery can be discharged compared to its capacity in amp-hours, e.g. a 2c battery cell with 2200mah can be discharged at 4400ma in 30 minutes[16, 17]. if the motor controller draws equal or more amps from the battery pack than its configuration can handle, this will result in a decreased capacity and probably also a decreased life span. in other words: if the e-bike is equipped with a 15amp controller, a 2c rated battery will need to have at least 7.5ah but preferably 10ah. thus, it can be stated that for this e-bike sharing project it is preferable to have a cell chemistry with a high c-rate since enough power is more important than a high capacity depending on what is an average distance between the stations and the characteristics of an average trip. a standard size for these cells is 18650 (18mm diameter, 65mm long, round shape) and their weight is a little less than 50g. a charging rate is mostly between 0.5c and 1c e.g. a 8.8ah battery pack charged at 2a will take about 5-6 hours to be fully charged. note that it will take about as much time to charge a battery from 0 to 80% as from 80% to 100%. it was the case in the "cycleushare" project that the batteries were made available by the system from the moment they were 75% charged which increased efficiency but still a reasonable range[18]. 28 vol. 12/2017 development of an electric bicycle in prague 3.4. electronics just like the system itself is required to be intelligent, so much is the e-bike itself. via a gui on the handlebars the rider can be informed about multiple variables as speed, trip distance, trip time, instantaneous power input and battery capacity, etc. more advanced devices as the cycle analyst will also provide information about wh or ah consumed, estimated wh left (instead of the typical battery icon) and an amount of human power amongst other variables. if a gps tracker is built in and a logging device is installed on the bike it is possible to carry out full post trip analyses which are interesting for further research in this project. using a mid-drive motor, it is preferable to have a gear sensor that cuts off motor power momentarily when the user shifts gears, thereby preventing too much stress on the chain and the gearing system which causes rough gearing and can cause damage as well. a better but more expensive solution would be a continuously variable transmission (cvt). the motor is mostly controlled with hall sensors. there are three main ways the rider can get assistance from the motor: throttle mode (current flow is proportional to angle of (thumb) throttle), cadence based pedal assist (current flow is proportional to crank rotation speed), torque based pedal assist (current flow is proportional to amount of torque exerted on the chain or the pedals). from these three ways the latter feels the most intuitive while the cadence based pas is much cheaper and thus more common. another advantage of torque proportional assistance is an increased battery range[19]. to achieve the proclaimed 50w of human power at all speeds and slopes a torque sensor would be ideal. in practice this can be done with a chain tension sensor or a strain gauge on the cranks or pedal axles. usually the hid offers a chance to set different pas levels so the user can choose how much proportional assistance he or she requires from the motor. most battery packs on the market will have a battery management system (bms) which is a circuitry to keep individual cell voltages balanced during charging and discharging. furthermore, it protects the cells from different circumstances such as high temperatures, deep discharge and overcharging. the quality and intelligence of this bms will have a high impact on the life span of a battery pack and depending on the chosen cell chemistry the bms is essential for safety, more specifically for preventing fires or explosions. 4. e-bike building, testing and results 4.1. choosing a configuration due to a low initial budget it was decided to convert a normal bicycle to an e-bicycle with a commercially available mid-drive kit and a downtube battery. because this battery requires presence of water bottle cage mounting holes it was more convenient to buy a male framed bicycle (see figure 4). figure 4. photo of an assembled e-bike. the configuration of the research bike consisted of a 350w rated mid-drive motor, meaning a 36v motor with 18a controller, i.e. a peak input power of 648w. the battery pack has a capacity of 36v × 8.8ah which is a 4p10s configuration of samsung icr1865022p cells (3.62v × 2150mah). samsung claims these cells have a maximum continuous discharge rate of 3c which means 26.4a. in fact, discharging at 3c the battery will already put quite some stress on the cells and the capacity will be lower due to heat losses as can be seen on discharge curves of this particular cell[7]. 4.2. tests and results firstly, the balancing of the e-bike was found very easy. one indicator for this is that it was very easy to balance the bike without hands on the handlebar. the bike enabled flexible maneuvering. this proves the chosen placement of battery and motor to be correct. secondly acceleration, top speed in the throttle mode was up to 34 km/h on a flat in an upright position. the accelerations perceived a big difference with normal cycling. the ease of getting up to speed was so easy both with the pedal assistance and the throttle mode is similar to riding a scooter or a small motorcycle. the motor did tend to heat up quite quickly after riding the bike several minutes in the highest pas levels (4 and 5). this shows that the set up with 36v and 18a the limit approaches the level a motor with these 62 dimensions can handle. the same motor is rated "250w" with a 15a current limit, in this case the motor will probably not heat up as much, combined with less stresses on the plastic gears inside. it might therefore have a longer lifespan with 15a maximum. riding in prague with this e-bike also revealed possible dangers, mostly concerning the higher speeds achievable. being very vulnerable on an e-bike speeds tended to drop when riding among car traffic. 29 w. deleenheer, l. jáneš, a. jayakumar acta polytechnica ctu proceedings another inconvenience is that not being able to go to a lower gear at low speeds or standstill feels rather unhandy regarding smooth accelerations. this is not any different with normal bikes but with this e-bike there was a tendency to prevent shifting too much and staying in a high gear for higher speeds. because the brakes cut off the motor power there is no need to go down in gears when slowing down and coming to a stop. although the electric motor can handle starting in the highest gear, the acceleration at lower gears is more logical, but shifting to a lower gear at standstill causes much stress on the gearing system and is perceived unsmooth. 5. experiments 5.1. first experiment for last three years two experiments have been carried out with the e-bike for transportation among the three buildings of ctu. these two experiments have been performed by students of the project electromobility. the bikes for the experiments were borrowed with similar or lower configuration as the bicycle, which was constructed. the first experiment covered the connections between the three buildings of ctu. in this project only students of ctu were included. in every buildings there was a spot for borrowing an e-bike, where the students borrowed the e-bike and rode to another building of ctu, where they returned the e-bike. during the trips the students measured parameters of the trip by mobile application and sent data to the folder for processing. in 15 days there were made about 50 rides and every ride proved that transport by e-bike among buildings is faster than other types of transport, such as automobile or public transport[20]. 5.2. second experiment the second experiment was made in 2014, and it examined advantages and parameters of riding the e-bike to the center of prague from an outskirt of the city. for this experiment typical trips for riding to center of prague were chosen, the center was selected as the building of ctu horská. there were 10 trips and every measuring showed that every trip is faster by e-bike opposite to the car or public transport. only one trip, the trip of about 10 kilometers, was faster by metro than e-bike[21]. 5.3. experiments conclusion the e-bike constructed for this thesis and presented in this article, was tested only for the driver’s comfort and for technical parameters, but not for measuring parameters and comparison with another type of transport. the previous two experiments were only for testing e-bikes as a means of transport for students among the buildings of ctu or for transporting students from home to school. it should start as a private public transport for students in "campuses", with private spots for rental and private system of borrowing and security. in the future, it would be beneficial to add new places, such as the central station, where it can be extended to general public which will help to make the system more popular among general population and tourists. 6. conclusion it is clear that e-bike sharing is a useful technology which can be a transportation method made ready to fit to a wide range of possible users. however, the small portion of real world examples show the concept still faces some difficulties, most of which being financial or organizational ones. thus, it is important to plan implementation and exploitation thoroughly with all stakeholders involved in the debate with a strong business plan laid on the table. the research e-bike, equipped with the cycle analyst and logger can be used to acquire accurate data about energy consumption and other trip characteristics when e-cycling in prague meanwhile experimenting with different types of bicycles, installing wind and rain shields or full covers to see their effect on energy consumption and comfort. as a result, the developed e-bike can be optimized further and fabricated. specific recommendations for further successful realization of the e-bike sharing project: • set up a strong business plan by means of a user survey and investment analysis and specific action plans. • further visualize the final result by implementing a (3d) design of both station and e-bike. • cooperate with other institutions and faculties. • set up an organization which will manage this interdisciplinary project and represent it. these 4 recommendations will significantly help with the challenge of an increasing student interest and involvement and increasing interest from sponsors, advertisement companies, university management and city municipalities. according to the market studies prague manages to keep up with the trends and efficient modes of transport. e-bike sharing could be then very soon visualized in prague at ctu. references [1] "european bicycle market analysis 2015", advocacy means sales, european cyclists’ federation. edited by: alexander scholz, published on 25.08.2016. [2] "gobike", gobike. [online], available: http://gobike.com/solution/the-bike/, [geopend 10 may 2016]. [3] "bewegen", bewegen technologies inc. [online], available: http://bewegen.com/our-system/#top, [geopend 10 may 2016]. 30 http://gobike.com/solution/the-bike/ http://bewegen.com/our-system/#top vol. 12/2017 development of an electric bicycle in prague [4] "bonopark", bonopark. [online], available: http://www.bonopark.es/en, [geopend 10 may 2016]. [5] "cycleushare", university of tennessee. [online], available: http://www.cycleushare.com/, [geopend 10 may 2016]. [6] "itdp", the institution of transportation and development policy. [online], available: https://www.itdp.org/wp-content/uploads/2014/ 07/itdp-bike-share-planning-guide-1.pdf, [geopend 10 may 2016]. [7] "open source bike share". [online], available: http://opensourcebikeshare.com/, [geopend 25 may 2016]. [8] d. e. jones. the stability of the bicycle. physics today. pp. 34-40, 1970. [9] j. m. j. p. a. r., a. j. d. g. kooijman. a bicycle can be self-stable without gyroscopic or caster effects. science, no. 332, pp. 339-342, 2011. [10] t. hadland. small wheels for adult bicycles. 25 june 2012. [online], available: https://hadland.wordpress.com/2012/06/25/ small-wheels-for-adult-bicycles/, [geopend 25 may 2016]. [11] j. lemire-elmore. ebiks.ca. grin technologies. [online], available: http://www.ebikes.ca/tools/simulator.html, [geopend 28 april 2016]. [12] m. ikonen. ip-zev. 2 april 2011. [online], available: http://www.ip-zev.gr/files/teaching/t4-2_human_ power.pdf, [geopend 28 april 2016]. [13] d. j. farris, g. s. sawicki. ncbi. pmc, 25 may 2011. [online], available: http://www.ncbi.nlm.nih.gov/ pmc/articles/pmc3223624/table/rsif20110182tb1/, [geopend 28 april 2016]. [14] "coefficient of friction, rolling resistance and aerodynamics", tribology-abc. [online], available: http://www.tribology-abc.com/abc/cof.htm# rolweerstand, [geopend 30 may 2016]. [15] "battery chemistry finally explained", battery bro, 19 february 2015. [online], available: https://batterybro.com/blogs/ 18650-wholesale-battery-reviews/ 18880255-battery-chemistry-finally-explained, [geopend 26 may 2016]. [16] "batteries", grin technologies. [online], available: http://www.ebikes.ca/learn/batteries.html, [geopend 26 may 2016]. [17] "bu-402: what is c-rate?", battery university, 29 february 2016. [online], available: http://batteryuniversity.com/learn/article/ what_is_the_c_rate, [geopend 27 may 2016]. [18] c. r. cherry, s. ji, l. d. han, d. a. jordan. electric bike sharing: simulation of user demand and system. journal of cleaner production. vol. 85, pp. 250-257, 2014. [19] "torque sensors on electric bikes", ectricbike.com, 18 october 2012. [online], available: http://www.electricbike.com/torque-sensors/, [geopend 27 june 2016]. [20] m. lapáčková. bike sharing na fakultě dopravní. praha, 2014, diplomová práce. čvut fd. [21] l. jáneš. využití elektrokol v praze z hlediska bezpečnosti a členitosti terénu. praha, 2015, bakalářská práce. čvut fd. 31 http://www.bonopark.es/en http://www.cycleushare.com/ https://www.itdp.org/wp-content/uploads/2014/07/itdp-bike-share-planning-guide-1.pdf https://www.itdp.org/wp-content/uploads/2014/07/itdp-bike-share-planning-guide-1.pdf http://opensourcebikeshare.com/ https://hadland.wordpress.com/2012/06/25/small-wheels-for-adult-bicycles/ https://hadland.wordpress.com/2012/06/25/small-wheels-for-adult-bicycles/ http://www.ebikes.ca/tools/simulator.html http://www.ip-zev.gr/files/teaching/t4-2_human_power.pdf http://www.ip-zev.gr/files/teaching/t4-2_human_power.pdf http://www.ncbi.nlm.nih.gov/pmc/articles/pmc3223624/table/rsif20110182tb1/ http://www.ncbi.nlm.nih.gov/pmc/articles/pmc3223624/table/rsif20110182tb1/ http://www.tribology-abc.com/abc/cof.htm#rolweerstand http://www.tribology-abc.com/abc/cof.htm#rolweerstand https://batterybro.com/blogs/18650-wholesale-battery-reviews/18880255-battery-chemistry-finally-explained https://batterybro.com/blogs/18650-wholesale-battery-reviews/18880255-battery-chemistry-finally-explained https://batterybro.com/blogs/18650-wholesale-battery-reviews/18880255-battery-chemistry-finally-explained http://www.ebikes.ca/learn/batteries.html http://batteryuniversity.com/learn/article/what_is_the_c_rate http://batteryuniversity.com/learn/article/what_is_the_c_rate http://www.electricbike.com/torque-sensors/ acta polytechnica ctu proceedings 12:24–31, 2017 1 introduction 2 general requirements for the sharing system 2.1 project vision 2.2 market research 2.3 station and software requirements 3 electric bicycle research and design 3.1 bicycle design 3.2 motor 3.3 battery 3.4 electronics 4 e-bike building, testing and results 4.1 choosing a configuration 4.2 tests and results 5 experiments 5.1 first experiment 5.2 second experiment 5.3 experiments conclusion 6 conclusion references acta polytechnica ctu proceedings doi:10.14311/app.2017.8.0008 acta polytechnica ctu proceedings 8:8–10, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app the influence of titanium-niobium alloys on the growth of the oxide layer jan krčil∗, vladimír mára, jana sobotová, stanislav krum department of materials engineering, faculty of mechanical engineering, czech technical university in prague, karlovo náměstí 13, 121 35 prague 2, czech republic ∗ corresponding author: jan.krcil@fs.cvut.cz abstract. this paper discusses issues of growth of a thin oxide layer formed on the surface of titanium alloys. the oxide layer on the surface introduces a corrosion resistance and a bio-compatibility, both of which are required for medical applications. the oxide layer is a result of a spontaneous passivation, but for the practical applications it is necessary to control the growth of oxides. in present work, the oxide layer was formed on the cp ti grade 2, ti39nb alloy and cp ti grade 2 with ti39nb pvd coating of two different thicknesses by a thermal oxidation at 600 ◦c for 8 hours. after the oxidation process the oxide layer was observed by sem. keywords: oxide layer, tinb, coating, biomaterials. 1. introduction nowadays, there is a need for better bio-implants and better bio-materials. it is due to several reasons: prolonging of human life, different lifestyle and activities, formerly incurable diseases and injuries. this may lead to the repairing or replacing parts of human body. the replacement should fit perfectly, act as the integral part of the body, have long lifetime, be bio-compatible, corrosion resistant and should not be expensive [1–3]. there are numerous existing materials used for body replacements. predominantly used are titanium alloys (especially ti-6al-4v and cp titanium) and stainless steel aisi 316l. but as the time progresses, these materials are slowly becoming obsolete. there is need for improved mechanical properties (ideally the same as human bones) and increased bio-compatibility. the new perspective group of materials is the titanium β alloys ti alloys with β structure, usually containing nb, zr, ta and other elements. these show lower modulus of elasticity, higher bio-compatbility but are more expensive on the other hand [2, 4, 5]. titanium alloys are not bio-compatible and corrosion resistant on their own. this effect is brought by oxides on the surface. oxide layer forms on the surface of ti alloys whenever the surface is in contact with air or moisture. resulting layer is very thin (the thickness is in the range of nanometers). the layer of such thickness would not act as the sufficient barrier and it would lead to corrosion and dissolution of the base material into the human body. the easiest way to prepare applicable oxide layer is the controlled oxidation: anodic or thermal. the composition of a layer may differ due to the chemical composition of the oxidized alloy, but the main component of the oxide layers on ti alloys is titanium dioxide (tio2). the tio2 naturally occurs in three different modifications: anatase, rutile and brookite. the rutile structure is stable up to melting temperature (unlike the other two) and in some cases is more suitable for the human body [2, 6]. the rutile structured oxide layer can be obtained by thermal oxidation above 500 ◦c [2, 7, 8]. 2. experiment the experiment was based on the comparison of the oxidation results on cp ti grade 2 and tinb alloy with 39 wt.% of nb (from now on ti39nb). bulk samples and substrates for coating were prepared by grinding and polishing to mirror sheen. afterwards, the two groups of cp ti samples were coated by ti39nb (one with 2 µm, other with 5 µm of ti39nb) using flexicoat 850, hauzer. subsequently, the samples were oxidized. the type of oxidation process and its parameters were based on the literature [7, 9, 10]: oxidation at temperature of 600 °c in the air atmosphere at atmospheric pressure with dwell of 8 hours in the lac lh 30/13 furnace equipped with mt825-a regulator. the course of the oxidation was following: heating from the room temperature with speed of 7.5 °c/min up to required 600 °c. at the end of the oxidation period, the furnace was turned off and the samples were cooled down to ambient temperature. it was expected that this process would result in formation of oxide layers with good adhesion to the substrate material. the measurement of oxide layers was carried out on the cross-section of samples using the jeol jsm 7600f scanning electron microscope. 3. results and discussion the fig. 1 represents the cross-sections of all 4 groups of oxidized samples. the substrate material, the coating and the oxide layer are labeled in every figure. the fig 1a shows oxidized sample of cp ti grade 2. the measured thickness of the oxide layer was app. 500 nm. in the case of oxidized sample of ti39nb 8 http://dx.doi.org/10.14311/app.2017.8.0008 http://ojs.cvut.cz/ojs/index.php/app vol. 8/2017 influence of titanium-niobium alloys on growth of oxide layer (a). (b). (c). (d). figure 1. cross-section of thermally oxidized (600 °c /8 hours) samples: (a) cp ti grade 2, (b) ti39nb, (c) cp ti grade 2 + 2 µm of ti39nb, (d) cp ti grade 2 + 5 µm of ti39nb. (fig. 1b), the oxide layer was considerably thinner than in case of the sample from cp ti. in average, the thickness was app. 140 nm. samples from cp ti with coating of ti39nb are in fig. 1c and 1d. on the sample with 2 µm thick coating the oxide layer with thickness ranging from 300 nm to 400 nm was found. the oxide layer thickness on the sample with 5 µm coating was ranging from 200 nm to 300 nm. from the images it is evident that the oxide layers formed on all samples are compact and with relatively uniform thickness. the adhesion of the oxide layers to the substrate/coating seems to be the same for all samples. the main difference between oxide layers was found in the resulting thickness. the thickest layer was found on cp ti grade 2, the thinnest one on ti39nb. the thickness of oxide layers on ti39nb coatings was in between. these preliminary results indicate that the tinb alloy appears to be less vulnerable to the oxidation process than cp ti grade 2 or that passivation process on tinb alloy is stronger than on cp ti grade 2. it leads to the formation of thinner oxide layer when compared to the samples of cp ti grade 2 which were oxidized in the same conditions and in the very same process. these findings contradict to the information found in the literature [6]. this phenomenon should be further investigated using different oxidizing conditions when compared with other materials and with other methods of the oxidation process. 4. conclusions • the oxide layer was created by the thermal oxidation on all four groups of samples and resulted in oxide layers of different thickness. • however against the assumption, the thickness of the oxide layers showed a different trend. the oxide layer found on the samples with thicker ti39nb coating was thinner than on the samples with thinner ti39nb coating. • the results indicate the dependence between the thickness of ti39nb coating and the thickness of the resulting oxide layer. • it will be further investigated how the results will differ under different oxidation conditions and with use of others method of oxidation. 9 j. krčil, v. mára, j. sobotová, s. krum acta polytechnica ctu proceedings acknowledgements this work was supported by the grant agency of the czech republic (grant no. 15-01558s) and by the ministry of education, youth and sport of the czech republic, program npu1, project no lo1207. references [1] u. kamachimudali, t. m. sridhar, b. raj. corrosion of bio implants. sadhana 28(3):601–637, 2003. doi:10.1007/bf02706450. [2] y. oshida. bioscience and bioengineering of titanium materials. elsevier, oxford, second edition edn., 2013. doi:http://dx.doi.org/10.1016/b978-0-44462625-7.00001-7. [3] biomedical engineering, trends in materials science, chap. novel titanium manganese alloys and their macroporous foams for biomedical applications prepared by field assisted sintering. intech, 2011. doi:10.5772/12874. [4] i. jirka, m. vandrovcová, o. frank, et al. on the role of nb-related sites of an oxidized β-tinb alloy surface in its interaction with osteoblast-like mg-63 cells. materials science and engineering: c 33(3):1636 – 1645, 2013. doi:http://doi.org/10.1016/j.msec.2012.12.073. [5] a. gutiérrez, m. f. lópez, j. a. jiménez, et al. surface characterization of the oxide layer grown on ti-nb-zr and ti-nb-al alloys. surface and interface analysis 36(8):977–980, 2004. doi:10.1002/sia.1816. [6] medical device materials v: proceedings from the 2009 materials & processes for medical devices conference, chap. titanium oxide layer on the surface of anodized dental implants. asm international. [7] g. zorn, a. lesman, i. gotman. oxide formation on low modulus ti45nb alloy by anodic versus thermal oxidation. surface and coatings technology 201(3-4):612 – 618, 2006. doi:http://doi.org/10.1016/j.surfcoat.2005.12.009. [8] z. abdolldhi, a. a. ziaee, a. afshar. investigation of titanium oxide layer in thermal-electrochemical anodizing of ti6al4v alloy. international journal of chemical & biomolecular engineering 2(1):44, 2009. [9] h. jiang, m. hirohasi, y. lu, h. imanari. effect of nb on the high temperature oxidation of ti-(0-50 at.%)al. scripta materialia 46(9):639 – 643, 2002. doi:https://doi.org/10.1016/s1359-6462(02)00042-8. [10] s. sartale, a. ansari, s.-j. rezvani. influence of ti film thickness and oxidation temperature on tio2 thin film formation via thermal oxidation of sputtered ti film. materials science in semiconductor processing 16(6):2005 – 2012, 2013. doi:https://doi.org/10.1016/j.mssp.2013.07.006. 10 http://dx.doi.org/10.1007/bf02706450 http://dx.doi.org/http://dx.doi.org/10.1016/b978-0-444-62625-7.00001-7 http://dx.doi.org/http://dx.doi.org/10.1016/b978-0-444-62625-7.00001-7 http://dx.doi.org/10.5772/12874 http://dx.doi.org/http://doi.org/10.1016/j.msec.2012.12.073 http://dx.doi.org/10.1002/sia.1816 http://dx.doi.org/http://doi.org/10.1016/j.surfcoat.2005.12.009 http://dx.doi.org/https://doi.org/10.1016/s1359-6462(02)00042-8 http://dx.doi.org/https://doi.org/10.1016/j.mssp.2013.07.006 acta polytechnica ctu proceedings 8:8–10, 2017 1 introduction 2 experiment 3 results and discussion 4 conclusions acknowledgements references 123 acta polytechnica ctu proceedings 2(1): 123–127, 2015 123 doi: 10.14311/app.2015.02.0123 photometric and spectroscopic investigation of the dwarf nova hs 0218+3229: a short review n. katysheva1, s. shugarov1,2, n. borisov3, m. gabdeev3, p. golysheva1 1sternberg astronomical institute of the moscow state university, 119991 moscow russia 2astronomical institute of the slovak academy of sciences, 059 60 tatranská lomnica, slovakia 3special astrophysical observatory of the russian academy of sciences, 369 167 nizhnij arkhyz, russia corresponding author: natkat2006@mail.ru abstract this paper is devoted to the study of the cataclysmic variable hs 0218+3229 using the photometric and spectroscopic observations. keywords: cataclysmic variables dwarf novae optical photometry spectroscopy individual: hs 0218+3229. 1 introduction cataclysmic variables (cvs) are highly evolved close binaries consisting of a white dwarf (wd) accreting matter from a red dwarf companion. this matter creates an accretion disc around the white dwarf. dwarf novae (dne) are a subclass of cataclysmic variables, whose members experience outbursts either caused by a thermal-viscous instability in the accretion disc (di) or by a sudden increase in mass transfer rate. outbursts of dne last a few days. in gcvs (samus et al., 2007-2012) dne are described as stars of the type ugss (u gem–ss cyg), with the recurrent time between outbursts lasting from days to several years. hs 0218+3229 (α2000 = 02h21m34s; δ2000 = +32◦ 43’ 24”) was discovered spectroscopically during the large-scale search for cvs in the hamburg quasar survey by gänsicke et al. (2002). rodriguez-gil et al. (2009) carried out photometric and spectroscopic observations of hs 0218+3229 from 2000 to 2005 and determined its orbital period to be 0.d297229661(1). the phase light curve (lc) in the r passband exhibits ellipsoidal modulation. the k5v secondary component gives a contribution of 80-85% to the r light. an analysis of the time-resolved optical spectroscopy and r passband photometry provided some parameters of hs 0218+3229: a mass ratio of 0.52< q <0.65, a white dwarf mass of 0.44< m1/m� <0.65, a secondary component mass of 0.23< m2/m� <0.44, the orbital inclination i = 59o ± 3o. the distance to the system was estimated to be 0.87–1.0 kpc. hs 0218+3229 has been identified as the x-ray source 1rxs j022133.6+324343 and the 2mass source j02213348+3243239. 2 photometric observations of hs 0218+3229 2.1 optical outbursts in 2006 the object was discovered independently by s. antipin using the photo plates of the photographic archive at the sternberg astronomical institute (sai) and identified as a dn. one outburst with an amplitude of about 4.5 mag in the bph passband was detected in september 1980. another outburst was detected in 2002 by wills from neat database (2002). golysheva et al. (2012, 2013) described photometric and spectroscopic observations of hs 0218+3229 from 2006 till 2010. ccd photometry in ubvrcic passbands was carried out at the crimean laboratory of sai (nauchny) and at the stará lesná observatory of the astronomical institute of the slovak academy of sciences. the magnitudes of comparison stars were determined in golysheva et al. (2012). in october 2007 they detected the outburst of hs 0218+3229 with an amplitude of 4 mag and duration of 15–16 days (jd 2454380–395). the shape of the outburst lc was more symmetric than for other dne. its asymmetry coefficient (the ratio of the duration of the ascending branch to the descending branch) was ∼0.22. a new ephemeris was calculated using the initial epoch of the minimum from rodriguezgil et al. (2009). the epoch corresponds to the inferior conjunction (the secondary is in front of the wd): hjdmin = 2453653.0286 + 0.2973559× e (1) the orbital period of the object (7.13 h) largely ex123 http://dx.doi.org/10.14311/app.2015.02.0123 n. katysheva et al. ceeds the average orbital periods of dne, which are in the range 1.5–4 hours. the maximum v magnitude of the 2007 outburst was determined as vmax=12.34±0.05 mag. the maximum magnitudes in other passbands were estimated by extrapolation as u=11.3±0.2 mag, b=12.3±0.2 mag, rj 'ij =12.2±0.2 mag. during 2011–13 we continued observations of the object. as seen from bvrcic light curves (lcs) of the object, obtained in 2006-13 and presented in fig. 1, a new outburst occurred in 2013. its v-maximum magnitude was the same as in 2007 outburst. a sudden 0.5 mag increase of brightness in the b passband was detected on january 31, 2011. the bvrcic plots in fig. 1 show long-term brightness variations during quiescence with a characteristic timescale of a few tens of days and an amplitude of ∼0.2 mag, noted in golysheva et al. (2012). figure 1: the bvrcic lcs of hs 0218+3229 in 2006–2013. the aavso data are marked by grey circles. our observations of the last outburst of hs 0218+3229, detected on september 5, 2013 (vsnet, 2013), were obtained at the stará lesná observatory. taking into account that the object exhibited outbursts also in 2002 and 2007, it is possible to estimate the recurrent time between outburst to be 5–6 years. fig. 2 shows the lcs of the outbursts in 2007 (upper panel) and 2013 (lower panel). the nightly lcs are inserted in separate panels. left lc, obtained directly before the outburst in 2007, shows half of orbital wave with an ellipsoidal effect. this effect is not visible on the other nightly lcs because of the presence of the outbursting disk. in the framework of the di model, the shape of the outburst lc of hs 0218+3229 can be explained by a low mass transfer rate in the system and ”inside-out” outburst in accordance with smak (1984). outburst starts from the inner parts of the disk and extends outward. the 2013 outburst shape is similar to the previous one in 2007. the nightly bv lcs are shown in fig. 2. figure 2: the outburst lcs in 2007 (top) and 2013 (bottom) in v (black points and circles) and b (grey points). the aavso v data are marked by grey circles. the ∆ubv rcic outburst lcs, near the maximum brightness, are presented in fig. 3. all lcs look similar. figure 3: the lcs after removal of the declining trend in brightness during the outburst, on september, 8, 2013. the lcs are displaced by arbitrary magnitudes. 124 photometric and spectroscopic investigation of the dwarf nova hs 0218+3229: a short review the quiescence lcs in the bvrcic passbands, folded with the ephemeris (1), are shown in fig. 4. double wave is clearly seen in the vri passbands, and less clearly in the b passband. it should be noted that the heights of the maxima (in phases 0.25 and 0.75) and depth of the minima (in phases 0 and 0.5) can change from night to night. the displacement of the second minimum around phase 0.5 is clearly seen. this feature was noted also by rodriguez-gil et al. (2009). golysheva et al. (2012, 2013) noted a large uvexcess in quiescence in 2010. during the 2007 outburst the position of the star in the two-colour diagram was close to that of an absolute black body with a temperature of about 15000 k. at the minimum brightness the position of the variable corresponded to a star of spectral class k5v-k6v. more detailed information about two-colour diagrams can be found in the paper of golysheva et al. (2012). figure 4: the average orbital phase bvrcic lcs in 2006–2012, folded with ephemeris (1). individual observations are marked by grey points, mean values by black points. 2.2 the analysis of the aavso data we also present data by the american association of variable star observers (aavso), whose observers were asked to observe the object to support the hubble observations (hst/cos, the aavso ”alert 471” (2012) about monitoring of hst targets). the hst/cos observations were obtained in december 2012. the main bulk of aavso observations were carried out in a clear filter. because of a very good time coverage, the orbital lcs were very well covered by observations in some nights from september 17, 2012 till january 2, 2013. we reduced the data to heliocentric values. the nightly lcs in september and october 2012 are presented in fig. 5 and folded lcs are shown in fig. 6. in spite of the error 0.02–0.03 mag, the shape of the nightly lcs is distinctive. the depth of the primary minimum (marked by 1) is smaller than the depth of the secondary minimum (marked by 2) and the hump after the primary minimum is brighter than the hump after the secondary minimum. this phenomenon is especially evident in the orbital folded phase lcs (fig. 6). figure 5: the aavso lcs obtained in september and october 2012. the primary and secondary minimum are marked by 1 and 2, respectively. figure 6: the average lcs in september–october 2012, folded with ephemeris (1). the notation is the same as in fig. 4. 125 n. katysheva et al. 3 spectroscopic observations our spectroscopic observations of hs 0218+3229 was taken in 2010 and 2012, when the object was in quiescence. golysheva et al. (2013) obtained two spectra of hs 0218+3229 on september 17/18, 2010 in the prime focus of the russian 6-m telescope bta of the special astrophysical observatory of the russian academy of sciences (sao ras) at the spectroscopic mode of the scorpio multi-mode focal reducer (afanasiev, moiseev, 2005) with the long slit and ccd-camera eev ccd 42-40 (2048×2048 pixels) with the exposures of 300 sec. our new spectroscopic observations of the objects were carried out on november 5, 2012 with the same reducer at the 6-m bta telescope. the vphg1200g grating (1200 grooves/mm) were used in both cases. the spectroscopic resolution ∆λ = 5.0 å in the wavelength interval 3950–5700 å was achieved. the spectra were reduced with sky and bias substraction and division by a flat-field frame. the discovery spectrum of the object obtained in 2000 (rodriguez-gil et al., 2009) revealed the absorption-line spectrum of the k5 v secondary, accompanying by the balmer and he i emission lines, arising in the accretion disk of the white dwarf primary. the 2010 spectrum was different. emission line of neutral helium λ5875 å became stronger, emission balmer decrement more flat and the features of the red companion became less pronounced (golysheva et al., 2012, 2013). these changes were probably caused by enhancing of a mass transfer rate and veiling of the spectrum of the secondary component. our spectrum obtained on november 5, 2012 is similar to the spectrum taken in 2000. the red star manifested itself again. 4 discussion and conclusions four outbursts of hs 0218+3229 in 1980, 2002, 2007, 2013 were detected up to now. the 2002 outburst (wills, 2002) was found in the database neat. the duration of 2007 outburst was 15–16 days and its asymmetry coefficient ∼0.22. the maximal amplitudes were 5 mag in the u, b passbands and 4 mag, 3.5 mag, 3 mag in the v, r, i passbands, respectively. it is possible to estimate the recurrence time of the outbursts to 5–6 years. we determined the orbital period to be 0.d2973559(10) and updated the ephemeris of the object. two-colour diagrams, presented in golysheva et al. (2012, 2013), showed that the object was bluer during its outburst than in quiescence. it was caused by cthe additional ontribution of a bright accretion disk to the total luminosity. outburst colour temperature was about 15 000 k. colour indices in quiescence correspond to a star k5 v. as a result, this cataclysmic variable was classified as a very rare subtype of ugsstype dn with a low accretion rate and sparse and more symmetric (”inside-out”) outbursts than it is usual in u gem-type and ss cyg-type of dne. figure 7: the spectrum of hs 0218+3229 on november 5, 2012. acknowledgement we thank to the large telescopes program committee of the sao ras for supporting our program of spectroscopic study of cvs. we would like to express our deep gratitude to dr. d. chochol for his valuable suggestions and critical reading of the manuscript. we are grateful to many amateur astronomers whose observations from the aavso international database were used in this research. nk thank to the soc for possibility to make a report. the work was supported partially by grants: nsh-1675.2014.2, rfbf-11-11-02-00258, 12-0200186, 12-02-97006 and vega grant 2/0002/13. references [1] samus, n., durlevich, o.v., kazarovets, e v. et al.: 2007-2012, general catalogue of variable stars, vizier on-line data catalog: b/gcvs. [2] gänsicke, b. et al.: 2002, asp conf. ser., 261, 190. [3] rodriguez-gil, p., torres, m.a.p., gänsicke, b.t. et al.: 2009, a&a, 496, 805. [4] wills, p.: 2002, near-earth asteroid tracking: http://neat.jpl.nasa.gov. [5] vsnet-alert.: 2013, http://ooruri.kusastro. kyoto-u.ac.jp/mailarchive/vsnet-alert/16355. 126 photometric and spectroscopic investigation of the dwarf nova hs 0218+3229: a short review [6] golysheva, p.yu., antipin, s.v., zharova, a.v. et al.: 2012, astrophysics, 55, 208. doi:10.1007/s10511-012-9229-6 [7] golysheva, p., katysheva, n., shugarov, s. et al.: 2013, ceab, 37, 345. [8] aavso-alert.: 2012, http://www.aavso.org/ aavso-alert-notice-471 [9] afanasiev, v., moiseev, a.: 2005, astron. lett., 31, 194. doi:10.1134/1.1883351 [10] smak, j.: 1984 pasp, 96, 575. doi:10.1086/131295 127 http://dx.doi.org/10.1007/s10511-012-9229-6 http://dx.doi.org/10.1134/1.1883351 http://dx.doi.org/10.1086/131295 introduction photometric observations of hs 0218+3229 optical outbursts the analysis of the aavso data spectroscopic observations discussion and conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.12.0064 acta polytechnica ctu proceedings 12:64–67, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app subjective methods for assessment of driver drowsiness alina mashko czech technical university in prague, faculty of transportation sciences, konviktská 20, prague 1, czech republic correspondence: mashkali@fd.cvut.cz abstract. the paper deals with the issue of fatigue and sleepiness behind the wheel, which for a long time has been of vital importance for the research in the area of driver-car interaction safety. numerous experiments on car simulators with diverse measurements to observe human behavior have been performed at the laboratories of the faculty of the authors. the paper provides analysis and an overview and assessment of the subjective (self-rating and observer rating) methods for observation of driver behavior and the detection of critical behavior in sleep deprived drivers using the developed subjective rating scales. keywords: driver drowsiness, subjective methods, observer rated sleepiness. 1. introduction driving sleepy, drowsy or fatigued at a high extent affects road traffic safety. the research by american centers for disease control and prevention (cdc) reports that 7500 fatal accidents happened in years 2011-2012 due to the drowsy factor [1]. per aaa foundation for traffic safety, 21% of drowsy drivers were involved in fatal traffic accidents in the usa, which is 4,5% higher as compared to the results of the preceding years [2]. similar involvement rates (20% of accidents due to sleepiness at the wheel) have been reported by the australian transport accident commission [3]. two-thirds of the population (71%) are said to be sleeping less than 8 hours per day. the most vulnerable to sleep deprivation are so called risk group that includes shift workers, young drivers and people with children in household. driving drowsy is dangerous, mainly due to the possible consequent impairments caused by this state. according to the national sleep foundation’s poll in 2000, drowsy drivers tend to feel stressed (42%), be impatient (32%) or drive faster (12%) [4] or not use the seat belt during night driving [5]. known reasons of drowsy driving and inattention are driving at the time of day when circadian rhythms are low, or driving for a long time or sleep loss [6]. 2. definition of fatigued and drowsy state due to the individual behaviour of every person in a particular state as well as because of a variety of reasons for drowsy driving, finding common attributes or indicators in this state is especially difficult. drowsiness and fatigue, per self-reported perceptions, influence performance, physiological state, feeling. it has been found that in a state of fatigue individuals have experienced such feelings as being tired, sleepy or exhausted, not feeling inclined to continue performing the task because of a perceived reduction of efficiency, feeling tired, exhausted, lack of energy as related to impaired of both physical and cognitive functioning, need of restoration of resources [7]. individual perception of one’s drowsiness can be determined with the help of questioning objects, conducting self-evaluation tests and is related to subjective observation. according to [8], the physiological state of a fatigued individual this corresponds to the organism’s muscular, visceral and central nervous system a decrease of capacity or energy to maintain initial activity due to insufficient rest is observed. detection of physiological signs of drowsiness and fatigue is carried out via measurements of the heartbeat rate, brain activity, eye blinking and closure. eye behavior can be observed with the help of electrooculogram (eog) [9, 10], with eye tracker, such as in researches presented in [11–13], based on eye image video analysis [14], etc. a lot of research has been done for exploration of brain activity of sleepy and drowsy drivers, some of the latest are [15–19]. the measurement itself is performed with the help of special electrodes of an eeg device that are placed on the human scalp to read brain wave activity. evaluation of the quality of the task performance is another possible measure of drowsiness and fatigue. fatigue caused by sleep deprivation affects driving performance which can reflect in delayed reaction, inability to maintain constant speed, loose of lateral control [20, 21] etc. measurements can be conducted in real traffic as well as in simulated environment, which is safer. usually, the performance indicators are measured for each object under two conditions: in a state of sleep deprivation and in fresh (control or reference) state. 64 http://dx.doi.org/10.14311/app.2017.12.0064 http://ojs.cvut.cz/ojs/index.php/app vol. 12/2017 subjective methods for assessment of driver drowsiness 3. subjective drowsiness and fatigue subjective indicators of sleepiness level include sleepiness scales, such as epworth sleepiness scale (ess), karolinska sleepiness scale (kss) and stanford sleepiness scale. during these tests short questionnaires are given to subjects who are asked to rate their state according to the suggested scale. the self-rating is usually conducted repeatedly during the testing time with either a time interval, or situations (conditions). this kind of rating allows evaluation of the participants’ awareness of their alertness level. when compared to other driver drowsiness measures, it has been demonstrated that kss defined level of sleepiness in most cases has a curve-linear relation to lateral position and blink duration [22]. another method used in experimental investigation of driver fatigue is observer rated sleepiness (ors). the method quantifies observation of behavior by trained individuals or experts who are rating driver performance based on video recordings of the experiment or in real time monitoring. the method can be used for validation of other measures or as a separate measure of driver fatigue [23]. 4. subjective evaluation during experiments on driver simulator all observations described in this chapter are related to experiments conducted on a full body (skoda superb) fixed driving simulator based on a wide projection angle (210° of driver’s view is provided with 5 screens plus 2 screens for side mirrors. see figure 1 for reference). detailed description of simulator and lab is provided in [24]. figure 1. advanced driver simulator for driver drowsiness research. previously, we have conducted observations of sleep deprived drivers during a 2 hours’ driver simulator measurements [25]. different observers tracked changes in the drivers behavior based on video recordings. the target areas were head, face (facial expression and mimicking, eye behavior) and upper torso (hands, shoulders and body). observers were instructed to document all noticed behavioral patterns out of (but not limited to) the suggested list: frequency of eye blinking, change in duration of eye closures, yawning, face muscles relaxation, lip biting, head tilt, shoulders shaking, hands on the wheel position, body relaxation, change of sitting position. also from the shots of the driving scenery driving behavior (steering, correction of position in a lane, lane departure and accident) were observed. it was possible to notice that blinking frequency was observed after 40th minute of driving. blinking was then gradually substituted by longer eye closures often accompanied by worsening of steering behavior, such as weaving and loose of vehicle control up to accidents. in most drivers head rotations (neck muscles stretching) and head tilt were noticed. this, however, didn’t reflect in the alteration of driving behavior (i.e., steering, speed fluctuation etc.) and was considered as a voluntary type of behavior caused by both sleepiness and fatigue from a long drive taken by subjects with a purpose of finding more comfortable position. all observed subjects have displayed dangerous driver behavior, that in real traffic might lead to accident, mainly starting after 30 minutes of experiment. inability to maintain straight trajectory, weaving and lane departure could be observed. at the laboratory for driver sleepiness research a self-rating sleepiness scale has been developed and is being used to assess driver sleepiness rate by the subject him/herself. the scale is presented in table 1, each of its levels corresponds to change in sleepiness level as perceived by subject. state description as perceived by subject 1 i feel fine/fresh & driving does not make me any problems. 2 i feel drowsy & driving does not make me any problems. 3 i feel drowsy & i notice some problems. 4 i feel very drowsy & i need to excessively concentrate to drive correctly. 5 i experienced ’blackouts’ & losing control over the car. table 1. self-rating sleepiness scale developed at faculty of transportation sciences, ctu in prague. evaluation per this scale will be presented in further research outcomes. the ors method was applied for analysis of video recordings of sleep deprived drivers on simulator. 9 observers (7 male and 2 female) who are students of faculty of transportation sciences, czech technical university conducted evaluation. the observations combined body movements, facial expressions and driving and vehicle behavior. initially developed scale contained three basic levels: (1.) subject is sitting straight behind the wheel with eyes open and both hands on the wheel in 10/2 position, he/she is following the road situation and 65 alina mashko acta polytechnica ctu proceedings figure 2. results for ors evaluation by 9 observers of one sleep deprived subject. figure 3. difference between maximum and minimum rates provided by observers. cluster indicators, vehicle is within the lane and is following straight path, (2.) subject experiences some features of drowsiness, like more frequent blinking and episodes of prolonged blinking, vehicle is experiencing some weaving, correction movements are present in steering, subject sitting position is not straight (head inclinations), subject is performing some self-awakening actions, hands positioned in lower part of the wheel, (3.) episodes of lane departure due to the result of longer eye closures (sleep episodes) steering correction movements are more abrupt, body position is not straight (subject adjusts to be more comfortable for rest position), head inclined to the side, one hand may be off the wheel, or on the bottom of the steering wheel. during the evaluation process, it had been decided to extend it to a 5-scale grade by introducing the half-scores for so called transition states (i.e., giving 1.5 and 2.5 scorers when subjects demonstrated only some features of the state). outcome of such observation is presented in figure 2. there one may track the mean, max and min rates of subject state sampled per 5 minutes of two-hour experiment. every human behavior is individual and people display different behavior under same conditions. besides, the subjective perception of each observer influences the ors data (see the difference chart between rates – figure 3). the same type of behavior may vary per subject in severity and impact that’s why it is not possible to assign same weights to the displays of human behavior. for those reasons, precise definition of a state to correspond the rate score is sometimes compromised. this is confirmed by a study, where results have demonstrated poor correlation of ors to srs (self-reported sleepiness) [26]. it is still possible to track a tendency of an increasing sleepiness rate per suggested scale after the 40th minute of driving, which corresponds to conclusions mentioned in [25]. 5. conclusion the research of driver fatigue covers the applications of many branches of science such as sociology, physiology, neuroscience, engineering. individual human behavior is a challenge in finding a single method for detection of drowsiness. besides, validation of detection methods in real traffic conditions is more complicated because these experiments may cause serious accidents. subjective methods have proved to be reliable for rating of fatigue in laboratory experiments and can be considered as a viable method for further exploration of the problem. self-rating and expert observations have proven to provide an adequate picture of driver fatigue and the tendency of increasing sleepiness during prolonged driving and can be correlated to objective measurements. rigid definition of the states to correspond the scale rate is however crucial for evaluation results. difference in scores given 66 vol. 12/2017 subjective methods for assessment of driver drowsiness by observers to the same behavior is crucial of data validity and could make the results questionable. the current research is aimed at tailoring the suggested evaluation method for its further implementation for analyses of driver sleepiness experiments. acknowledgements this research was supported by grant sgs16/254/ohk2/3t/16 "experimental research of driver fatigue by means of observation visual behavior". references [1] a. wheaton, r. shults, d. chapman, et al. drowsy driving and risk behaviors – 10 states and puerto rico, 2011-2012. morbidity and mortality weekly report, vol. 63, no. 26. july 4, 2014. [2] aaa foundation for traffic safety. acute sleep deprivation and risk of motor vehicle crash involvement, 2016. [3] transport accident commission. fatigue statistics. http://www.tac.vic.gov.au/road-safety/ statistics/summaries/fatigue-statistics. [4] national sleep foundation. 2000 facts and stats. http://drowsydriving.org/about/facts-and-stats. [5] u. d. of transpotation. nhtsa.guidelines to observe and estimate statewide seat belt use at night. 2010. dot hs 811 288. [6] u. d. of transpotation. nhtsa.guidelines to observe and estimate statewide seat belt use at night. 1999. dot hs 808. [7] r. phillips. a review of definitions of fatigue – and a step towards a whole definition. transportation research part f 29 (2015) 48-56. [8] r. soames-job, j. dalziel. defining fatigue as a condition of the organism and distinguishing it from habituation, adaptation and boredom. in p. a. hancock & p. a. desmond (eds.), stress, workload and fatigue. ny: crc press. 2000. [9] m. villamizar, j. suarez, j. villanueva, et al. design and implementation of sleep monitoring system using electrooculographs signals. 9th pan american health care exchanges conference, pahce 2014. [10] n. r.-i. nez, p. meca-calderón, m. garcía-gonzález, et al. drowsiness detection by electrooculogram signal analysis in driving simulator conditions for gold standard signal generation. international conference on biomedical electronics and devices, biodevices 2013. barcelona, spain. [11] r. coetzer, g. hancke. eye detection for a real-time vehicle driver fatigue monitoring system. 2011 ieee intelligent vehicles symposium, iv’11; baden-baden, germany. [12] k. anjali, k. athiramol, v. athira, et al. time nonintrusive monitoring and detection of eye blinking in view of accident prevention due to drowsiness. international conference on circuit, power and computing technologies, 2016. [13] a. rahman, m. sirshar, a. khan. real time drowsiness detection using eye blink monitoring. national software engineering conference (nsec), 2015. [14] j. ahmed, l. jian-ping, k. saeed, a. riaz. eye behavior based drowsiness detection system. 12th international computer conference on wavelet active media technology and information processing (iccwamtip). 2015. [15] g. usha, b. radhika, t. shanmuganathan. eeg-based brain wave sensor to detect drowsiness with eye open. far east journal of electronics and communications. volume 16, march, 2016. [16] r. foong, k. ang, c. quek, et al. an analysis on driver drowsiness based on reaction time and eeg band power. 37th annual international conference of the ieee engineering in medicine and biology society, embc, 2015. [17] t. brown, r. johnson, g. milavetz. identifying periods of drowsy driving using eeg. 57th annual scientific conference of the association for the advancement of automotive medicine, canada, 2013. [18] m. jiřina, p. bouchner, s. novotný. identification of driver’s drowsiness using driving information and eeg. neural network world, 2010. [19] j. faber, j. pěkný, r. pieknik, et al. simultaneous recording of electric and metabolic brain activity. neural network world, 2010. [20] r. v. loon, r. brouwer, m. martens. drowsy drivers’ under-performance in lateral control: how much is too much? using an integrated measure of lateral control to quantify safe lateral driving. accident analysis and prevention. volume 84, 2015. [21] s. james, b. vila. police drowsy driving: predicting fatigue-related performance decay. policing, volume 38, issue 3, 2015. [22] m. ingre, t. akerstedt, b. peters, et al. subjective sleepiness, simulated driving performance and blink duration. journal of sleep research. volume 15, issue 1, 2006. [23] a. anund, c. fors, d. hallvig, et al. observer rated sleepiness and real road driving: an explorative study. plos one, 2013. [24] s. novotný, p. bouchner, j. pěkný, et al. hybrid mirrors for driving simulators – design, construction and experiments. in: computational intelligence, man-machine systems and cybernetics. athens: wseas press, 2007, pp. 310-315. issn 1790-5117. isbn 978-960-6766-21-3. [25] a. mashko, p. bouchner. visual investigation of driver behavior for fatigue detection – driving simulator experiments. recent advances on systems, signals, control, communications and computers. 2015. [26] c. ahlstrom, c. fors, a. anund. eur. transp. res. rev. (2015) 7:38. doi:10.1007/s12544-015-0188-y. 67 http://www.tac.vic.gov.au/road-safety/statistics/summaries/fatigue-statistics http://www.tac.vic.gov.au/road-safety/statistics/summaries/fatigue-statistics http://drowsydriving.org/about/facts-and-stats acta polytechnica ctu proceedings 12:64–67, 2017 1 introduction 2 definition of fatigued and drowsy state 3 subjective drowsiness and fatigue 4 subjective evaluation during experiments on driver simulator 5 conclusion acknowledgements references 273 acta polytechnica ctu proceedings 2(1): 273–276, 2015 273 doi: 10.14311/app.2015.02.0273 the ubv color evolution of classical and symbiotic novae i. hachisu1, m. kato2 1department of earth science and astronomy, college of arts and sciences, the university of tokyo, komaba, meguroku, tokyo 153-8902, japan 2department of astronomy, keio university, hiyoshi, kouhoku-ku, yokohama 223-8521, japan corresponding author: hachisu@ea.c.u-tokyo.ac.jp abstract we identified a general course of classical nova outbursts in the b − v vs. u − b diagram. it has been reported that novae show spectra similar to a–f supergiants near optical light maximum. however, they do not follow the supergiant sequence in the color-color diagram, neither the blackbody nor the main-sequence sequence. instead, we found that novae evolve along a new sequence in the pre-maximum and near-maximum phases, which we call the nova-giant sequence. this sequence is parallel to but ∆(u − b) ≈ −0.2 mag bluer than the supergiant sequence. after optical maximum, its color quickly evolves back blueward along the same nova-giant sequence and reaches the point of free-free emission (b − v = −0.03, u −b = −0.97) and stays there for a while, which is coincident with the intersection of the blackbody sequence and the nova-giant sequence. then the color evolves leftward (blueward in b−v but almost constant in u −b) due mainly to development of strong emission lines. this is the general course of nova outbursts in the color-color diagram, which is deduced from eight well-observed novae including various speed classes. for a nova with unknown extinction, we can determine a reliable value of the color excess by matching the observed track of the target nova with this general course. this is a new and convenient method for obtaining color excesses of classical novae. using this method, we redetermined the color excesses of nineteen well-observed novae. keywords: cataclysmic variables novae individual: fh ser, pu vul, pw vul, v1500 cyg, v723 cas. 1 introduction a classical nova is a thermonuclear runaway event on a mass-accreting white dwarf (wd) in a binary. despite of their overall similarity, optical light curves of novae have a wide variety of timescales and shapes. recently, hachisu & kato (2006) found that, in terms of free-free emission, the optical and infrared (ir) light curves of several novae follow a similar decline law. moreover, the time-normalized light curves were found to be independent of the wd mass, chemical composition of ejecta, and wavelength. they called it the universal decline law. evolution of colors is another challenging subject that attracts many researchers, who attempted to find a general behavior among various types of novae. for example, duerbeck & seitter (1979) discussed that color evolutions of six novae are remarkably similar in the intrinsic (b−v )0 versus (u −b)0 color-color diagram independently of their different nova speed classes. van den bergh & younger (1987) derived general trends of color evolutions in nova light curves, i.e., (b − v )0 = 0.23 ± 0.06 at optical maximum and (b − v )0 = −0.02 ± 0.04 at t2, where tm (m = 2 or 3) is the days during which a nova decays by mth magnitude from its optical maximum and (b − v )0 is the intrinsic b − v color of the nova. these two relations, however, often show large deviations from the values obtained by other methods. miroshnichenko (1988) found a stabilization stage of novae in the b−v and u − b color evolutions soon after optical maximum and that this stage showed a general trend of (b − v )0 = −0.11 ± 0.02. he derived extinctions, e(b−v ), of 23 novae assuming that all novae have the same intrinsic (b−v )0 color at the stabilization stage, i.e., e(b−v ) = (b−v )ss−(b−v )0 = (b−v )ss+0.11, where (b−v )ss is the observed b−v color at the stabilization stage. this method looks powerful but sometimes results in a large difference from the true value. according to hachisu & kato’s (2006) universal decline law, optical fluxes in the ubv bands could be dominated by free-free emission. if it is the case, its color is simply estimated to be (b − v )0 = 0.13 and (u − b)0 = −0.82 for the optically thin free-free emission (fν ∝ ν0), or to be (b − v )0 = −0.03 and (u −b)0 = −0.97 for the optically thick free-free emission (fν ∝ ν2/3, see, e.g., wright & barlow 1975), where fν is the flux at the frequency ν. the latter value of (b−v )0 = −0.03 is close to (b−v )0 = −0.02±0.04 273 http://dx.doi.org/10.14311/app.2015.02.0273 i. hachisu, m. kato at t2 derived by van den bergh & younger (1987). however, many novae do not keep these pivot points but further evolves blueward. these different trends of nova color evolutions may represent different sides of the true color evolution which we do not yet fully understand observationally or theoretically. the aim of this presentation is to find a general path of nova color evolutions as duerbeck & seitter (1979) tried to find about thirty years ago. first we examine the color evolutions of slow and fast novae, fh ser, pw vul, v1500 cyg, v1668 cyg, v1974 cyg, pu vul, hr del, and v723 cas. we found that the tracks of color-color evolutions of these slow/fast novae are common. then we redetermined the reddening of nineteen novae by fitting the color evolution of a target nova with the common path in the color-color diagram. thus, we propose a new method for estimating the color excess. figure 1: light and color curves of fh ser 2 nova-giant sequence in the color-color diagram the first example of our analysis is the moderately fast nova fh ser. the v , (b − v )0, and (u − b)0 light curves of fh ser are plotted in figure 1. fh ser showed a gradual optical decay with t2 = 41 and t3 = 62 days followed by a sudden drop of the brightness due to dust shell formation about 2.8 mag below the optical maximum. the (b−v )0 vs. (u −b)0 color-color evolution is plotted in figure 2 (see hachisu & kato 2014 for more detail). the reddening toward fh ser was obtained by kodaira (1970) to be e(b − v ) = 0.6 from the mmrd relation and interstellar reddening relation. della valle et al. (1997) obtained e(b − v ) = 0.82 from the color at optical maximum, i.e., e(b − v ) = (b − v )max − (b − v )0,max = 1.05 − 0.23 = 0.82, e(b − v ) = 0.61 from the line ratio of hα/hβ = 5.7, and e(b − v ) = 0.5 from the equivalent width of na i λ5890. then, della valle et al. (1997) adopted an averaged value of e(b − v ) = 0.64± 0.16. since kodaira’s e(b−v ) = 0.60 and della valle et al.’s e(b−v ) = 0.61 from the line ratio of hα/hβ are coincident with each other, we use e(b−v ) = 0.60 in the present paper and confirm below that this value is reasonable. figure 2: color-color evolution of fh ser in figure 2 we plot only the data before the dust blackout started about 70 days after the outburst. we also depict three known sequences, the blackbody, supergiant, and main-sequence sequence, the data of which are taken from allen (1976). we also added a point, i.e., optically thick free-free emission spectra (open diamond denoted by f) of fν ∝ ν2/3. we have frequently seen in literature such a statement that nova spectra near maximum are similar to those of a–f type supergiants. however, the track of fh ser in the colorcolor diagram does not follow the supergiant sequence as clearly shown in figure 2. the shape of fh ser track is very similar to that of the supergiant sequence but 274 the ubv color evolution of classical and symbiotic novae it locates about ∆(u − b) ≈ −0.2 mag bluer than the supergiant sequence. therefore, we are forced to define a new sequence based on the data of fh ser, which is designated by points a, b, c, d, and f from redder to bluer. these points correspond to epochs in figure 1. in what follows, we will see that many novae evolve along this sequence when their photospheric spectra are similar to those of a–f type supergiants. therefore, we call this track “the nova-giant sequence” after the supergiant sequence. 3 common paths of novae in the color-color diagram we have also studied color-color evolutions of the fast and slow novae, pw vul, v1500 cyg, v1668 cyg, v1974 cyg, pu vul, hr del, and v723 cas, in the (b−v )0 (u−b)0 diagram and showed that these well observed novae follow very similar evolutionary courses in the intrinsic color-color diagram as shown in figure 3. we finally specified four templates, (1) the moderately fast nova fh ser, a proto-type of the nova-giant sequence, (2) the slow nova pw vul and the very fast nova v1500 cyg, (3) the fast novae v1668 cyg and v1974 cyg, and (4) the symbiotic nova pu vul, the very slow novae v723 cas and hr del. the tracks are characterized with several specified points (a, b, c, d, f, 0, 1, ..., 5, 4’, 5’, 4”, and 5”). figure 4(a) shows templates of these eight well observed novae. figure 3: several typical tracks of novae in the colorcolor diagram since these well observed eight novae follow the templates in figure 4(a), we expect other novae also follow the same paths. in other words, if all novae follow this template, we are able to determine the color excess of a target nova by directly comparing its track in the colorcolor diagram with our general track in figure 4(a). figure 4: color-color evolution of (a) template 8 novae, (b) rs oph, (c) v446 her, and (d) v533 her. figure 5: (a) t pyx, (b) lv vul, (c) iv cep, and (d) nq vul. 275 i. hachisu, m. kato 4 estimates of extinctions toward various novae we are able to determine color excesses of various novae using our general color-evolution tracks found in this work. we collected novae as many as possible from literature that have sufficient data points (usually more than ten). we assume that all novae follow the colorcolor evolution tracks in figure 4(a). in order to obtain e(b − v ), we change e(b − v ) by steps of 0.05 to fit the observed track of a target nova with our general tracks in figure 4(a). figure 6: (a) v1370 aql, (b) gq mus, (c) qu vul, and (d) os and. figure 7: (a) qv vul, (b) v443 sct, (c) v1419 aql, and (d) v705 cas. figure 8: (a) v382 vel, (b) v2274 cyg, (c) v475 sct, and (d) v5114 sgr. figures 4, 5, 6, 7, and 8 show results of our analysis for 19 novae. corresponding e(b−v ) excess is denoted in each panel (see hachisu & kato 2014, in detail). references [1] allen, c. w. 1976, astrophysical quantities (3rd ed.; london: athlone) [2] della valle, m., gilmozzi, r., bianchini, a., & esenoglu, h. 1997, a&ap, 325, 1151 [3] duerbeck, h. w., & seitter, w. c. 1979, a&ap, 75, 297 [4] hachisu, i., & kato, m. 2006, apjs, 167, 59 doi:10.1086/508063 [5] hachisu, i., & kato, m. 2014, apj, 785, 97 doi:10.1088/0004-637x/785/2/97 [6] kodaira, k. 1970, pasj, 22, 447 [7] miroshnichenko, a. s. 1988, soviet astronomy, 32, 298 [8] van den bergh, s., & younger, p. f. 1987, a&ap suppl., 70, 125 [9] wright, a. e., & barlow, m. j. 1975, mnras, 70, 41 doi:10.1093/mnras/170.1.41 276 http://dx.doi.org/10.1086/508063 http://dx.doi.org/10.1088/0004-637x/785/2/97 http://dx.doi.org/10.1093/mnras/170.1.41 introduction nova-giant sequence in the color-color diagram common paths of novae in the color-color diagram estimates of extinctions toward various novae acta polytechnica ctu proceedings doi:10.14311/app.2017.11.0031 acta polytechnica ctu proceedings 11:31–34, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app railway traffic optimization dušan kamenický∗, tomáš brandejský, vít fábera, valerii gopak faculty of transportation sciences, czech technical university in prague, konviktská 20, 110 00 praha 1 ∗ corresponding author: kamendus@fd.cvut.cz abstract. the article focuses on analysis of possibilities of operatic control of railway traffic and its automatization and its support by information systems. conditions, necessary pieces of input information like infrastructure description are discussed. railml format is mentioned as suitable format for description in railway area. optimization criterion and use of evolutionary techniques are suggested. the system is modeled in railway laboratory of the faculty of transportation sciences, ctu in prague. keywords: railway traffic optimization, railml, evolutionary techniques, prediction. 1. railway traffic optimization trends increasing demands to railway capacity require to build new railway lines and to apply new approaches like information technologies supporting railway traffic to use effectively given infrastructure. train running is controlled and checked by interlocking systems (and by operations over the devices) that evaluates the state of the infrastructure (mainly occupancy of track sections is detected using track circuits or axle counters), controls infrastructure elements (switches), transmits instructions how to move through signals or automatic train stopping device. there are several trends of rail operation control. firstly, the way of control is shifted from distributed system spread over stations to centralized one in all europe. the most railway lines in the czech republic should be controlled from two offices in přerov and prague. the centralization of the operation control gives spread view of the situation and more information to the operator. on the other hand, there is a disadvantage of this approach. information quantity to evaluate increases if the area is large. it is clear the information capacity of each human operator is limited and different. moreover, operator is negatively influenced by rotes. secondly, next modern trend (especially in switzerland, belgium and germany) is a separation of strategy control (route planning from daily to annual interval) from operative control (conflicts solution caused by deviations from regular time-table due to infrastructure or vehicle faults) and from direct control (safety device operation, shunting). each level of operation control architecture process specific functions and it needs it support. this article is focused especially on operative control and its it support, strategy control is mentioned only marginally. it is supposed that output of the strategy level support is a scheduled daily time table with valid and conflict-free train routes (really realizable with respect to the route capacity). operative control it support should react to deviation from planed daily time table; it monitors actual trains routes and solves potential conflicts with others trains in advance (from minutes to hours). the output is modified conflictfree time table – specific route plan transmitted to direct control level (realized by human operator or automatic system). the direct control level is freed from searching the sequence of runs if the planned time-table is disturbed and processes of the direct control level are focused on safety device operations and guarantee of rail operation safety. 2. it support of operative control it support of operative control was missed out in the czech republic for a long time. today systems only shows planned timetable which is modified based on information about actual train position entered by operators in stations. they reflect neither train properties (parameters) nor infrastructure properties. it depends only on abilities and experiences of operators (dispatchers) if they are able to predict potential conflict and to suggest appropriate solution. moreover, todays systems are not able to transfer such modified timetable to the direct level operating on the plant-interlocking devices. to increase capacity of railway traffic and effectivity by optimization of operative control, it means to solve several partial problems that are very difficult: prediction of train paths, conflicts detection and optimal solution of these conflicts. the necessary premise to be able to search automatically optimal solution is to predict train path. some problems hamper to solve this problem satisfactory. above all, it is necessary to dispose enough description of the infrastructure. the description must contain the information related to the construction of time table (position and height of platform edges, line parameters affecting train resistance – slope, curves, tunnels, ...) and related to the interlocking system (track sections and their dependencies ensuring safety 31 http://dx.doi.org/10.14311/app.2017.11.0031 http://ojs.cvut.cz/ojs/index.php/app d. kamenický, t. brandejský, v. fábera, v. gopak acta polytechnica ctu proceedings running). the prediction is also affected by actual train parameters and their correctness, especially by type of motive power and its traction characteristic, train weight, braking ability of the train (both parameters can change in dependence of weather), eventually coefficients of train resistances. the strategy of run is important as well – ratio of times of thrust/coasting/braking. if the trains are manually controlled by engine drivers the strategies can be dramatically different. the application of ato (automatic train operation) brings the improvement in this area, when strategies became more stable (but the strategies can be different within several ato systems depending on producers). very stochastic quantity is time of stop in stations (getting on and off, operations on train). one possibility to eliminate partially randomness is to collect long-term statistics. dependencies between trains are necessary to take into account – connections, locomotives, coaches and train crew turnround cycles. completeness and up-to dateness of data stored in is are necessary. train routes conflict detection is highly dependent on the interlocking systems. each infrastructure operator has different equipment and it works with different set of risks and their consequences. due to this reason, each operator defines different functional requirements for interlocking systems and procedures to guarantee safety of traffic. different requirements can affect conditions for compatible routes. conditions depend not only on infrastructure but also on equipment of rolling stocks. it is not sufficient to consider only occupation of track sections but locking of sections which are running – before running and after running during defined interval. route locking can have time and space aspect. the specific case is such running conflict when one train run through the station or it is coming to the platform and the arrival to the second platform is at the same level (there is no subway or upperbridge). if a conflict is detected it must be solved. while previous phases (train path prediction and conflict detection) can be defined, modeled and computer relatively exactly, the definition of the optimization criterion by conflicts solution is complicated and "soft". one criterion can be "accuracy of planned time timetable", i.e. minimum of total sum of train delays. afterwards, weights of several trains and stations must be defined (delay of ic train has greater impact). but, weight assignment trenches offering politics of carriers. energetic criterion can be more objective and better definable. power consumption is possible to be good computed. the final criterion function can be multicriterial and be of the weight sum form. requirement to minimize time of closing level-crossing can be included to the criterion function. the set of situation is large that can happen. modern systems are able to solve only several situations automatically and sophistically. it is always considered a human operator and automatic system cooperation. own intervention can be realized not only by time shift of train path but also/or by change of train route – only within the station (to the different line) or the new whole path. in the case of new path there are new constraints as knowledge of line by driver, ability to pass new line by the train, operation of stations, ... 3. implementation in railway laboratory railway laboratory was founded at the faculty of transportation sciences which serves as a place to simulate train traffic control and interlocking system. the laboratory is equipped by interlocking devices typically used in the czech republic – from the oldest (mechanical) ones up to modern (computer based) ones. so, the level of direct control is modeled realistically. the laboratory is extended by higher levels traffic control architecture, namely on operative level. applications are developed which reflect modern trends of rail traffic control, focusing on train path prediction, conflicts detection and their solution. the topology of model railway in railway laboratory was selected as infrastructure on which applications will be developed and tested. we analyzed current concepts of infrastructure description used in reality. the way used in the czech republic prefers time-table point of view. this way is not compatible with the format representing infrastructure from the interlocking architecture point of view. the railml.org initiative [1] tries to uniform the infrastructure description and defines railml standard. the railml standard is based on xml format which is generally used nowadays to store structured data. it is a text format consisting of elements that can be nested; element is a block bounded by tags enclosed in <>. typically, configuration files, some database files have xml structure (html file are types of xml too). the version railml 2.3 was released, the specification railml 3 is in progress – the version 3.0 is released only for internal use in initiative, the version 3.1 is supposed to be released in autumn 2017. the railml defines several subschemas to describe and store information of various railway subsystems and parts: timetable and rostering, infrastructure, rollingstock, interlocking and common. a fragment of railml code 2.3 describing track is shown bellow (the complete example is available at [2]) – fig. 1. experiences show that extraction of infrastructure and connections from railml 2.x is not so clear especially due to separate description of elements and their connections. the railtopomodel project exists concurrently to the railml and it is a logical object model to standardize the representation of railway infrastructure-related data and it uses railml 3.x; the schema railml 3.x is different from 2.x and much better. nevertheless, version 3, as mentioned above, is still in progress. therefore research team decided to utilize existing own xml format describing 32 vol. 11/2017 railway traffic optimization figure 1. description of connection using railml 2.x (source [2]). figure 2. optimization system and its inputs. infrastructure which is used for interlocking devices configuration in railway laboratory [3]. optimization of the timetable is understood dynamic change of timetable (including time shift and route changes) to solve conflicts in our conception, not creation of the new (for example, daily, annual timetable) one. let’s summarize inputs of the optimization system (fig. 2): infrastructure description, train description, timetable description. infrastructure of railway laboratory is described by own xml format, as mentioned above. the net is composed from several types of elements like: tracks sections, signals, insulated rail joints, switches. the model contains other elements which are omitted in our application due to irrelevancy: power supplies, derailers, track circuits. elements and their bindings are read from the file and an oriented graph is constructed in the computer memory. own library was implemented in c++ programming language due to its speed and effective work with pointers. the base of own xml parser to read infrastructure description is an open-source library. there are many general freeware libraries for xml format analysis. we chose xerces library which is also written in c++ and it holds dom (document object model) in its internal structures. it is supposed that railml will be widely applied in real railway in the future. similar parser of railml format can be created and it is not a big problem to program such software module (library) "railml parser" containing functions for the analysis of the railml files – just due to existence of free general xml parsers like xerces. train description has our proprietary format. parameters of specific trains are stored to compute their traction and another physical characteristics (maximal speed) allowing modeling of train move and change it: increment or decrement train speed as one possible solution of collisions. naturally, the railml format concept calculates to store rolling-stock description in xml. timetable is stored in mysql server in railway laboratory (the future is railml format as well) and software library to read the timetable was created. the database contains only stations passed through and arrival and departure times. amount of information is insufficient. it is not possible to derive uniquely train path (there exist more paths between stations very often) and times of track sections occupancy. the identification of collision is not possible without knowledge of this piece of information. the time-table database has to be extended to contain sequence of track sections passing by trains and intervals of occupancy. each track section is labeled during simulation if it is free, occupied or locked. conflicts are searched like intersections of time intervals. if conflict is detected time intervals can be changed (shifted, shortcut, stretched) by the change of the train speed with using train characteristics. conflict solution can be implemented by some heuristic (evolutionary technique). if the change of travelling time doesn’t lead to the conflict solution an alternative paths can be used (which can generate unfortunately additional conflicts). alternative path searching can be implemented by evolutionary technique too. the technique of travelling time change can be applied to alternative paths. the conflict is solved by the path change of one train in the simplest case. if it is not solved the area of changes is spread (to other trains). it is evident the task is very complicated and it must be solved in reality by parallel computation. 4. conclusion the effective railway traffic optimization and following control is very difficult task. it is necessary to have enough described infrastructure, time table and rolling stock and store the data in information systems. prepared railml format and railtopomodel appears to be very perspective. to optimize railway traffic dynamically, especially when unexpected events happen, it needs to predict train runs, search conflict and solve them, for example to shift runs in timetable or to plan alternative paths. the optimal solution can be searched by evolutionary techniques where optimization criterion can be to minimize total sum of train delays or minimize power consumption. parallel computation is supposed to be applied. references [1] railml.org. initiative [online]. [cit. 2017-03-08] "http://www.railml.org". 33 d. kamenický, t. brandejský, v. fábera, v. gopak acta polytechnica ctu proceedings [2] railtopomodel [online]. [cit. 2017-03-08] "http://www.railtopomodel.org". [3] p. koutecký. electronic signal box for ctu transport lab, diploma thesis. faculty of electrical engineering, 2011. 34 acta polytechnica ctu proceedings 11:31–34, 2017 1 railway traffic optimization trends 2 it support of operative control 3 implementation in railway laboratory 4 conclusion references 111 acta polytechnica ctu proceedings 2(1): 111–115, 2015 111 doi: 10.14311/app.2015.02.0111 flickering in cvs and accretion disc viscosity r. baptista1 1departamento de f́ısica, universidade federal de santa catarina, campus trindade, 88040-900, florianópolis, brazil corresponding author: raybap@gmail.com abstract i review observational constraints on accretion disc viscosity inferred from changes of disc structure with time and from disc flickering distributions. the radial run of the disc viscosity parameter in four cases are presented and discussed. keywords: cataclysmic variables dwarf novae accretion discs optical time-series photometry individual: v2051 ophiuchi, ht cassiopeia, v4140 sagitarii, uu aquarii. 1 context accretion discs are cosmic devices where angular momentum and gravitational energy are extracted from matter by an anomalous, still unknown viscosity mechanism, allowing it to be accreted onto a central star (frank, king & raine 2002). currently, the most promising explanation for the disc viscosity is related to magneto-hydrodynamic (mhd) turbulence in the differentially rotating disc gas (balbus & hawley 1991). from the observational standing point of view, because the properties of steady-state discs are largely independent of viscosity, one must turn to observations of timedependent disc behavior in order to obtain quantitative information about disc viscosity. here we adopt the prescription of shakura & sunyaev (1973) for the accretion disc viscosity, ν = αss csh, where αss is the nondimensional viscosity parameter, cs is the local sound speed and h is the disc scaleheight. non-magnetic1 cataclysmic variables (cvs) are excellent sites for studies of disc viscosity, because of their well constrained binary environment and because their accretion discs are usually the dominant light source at uv and optical wavelengths. in particular, the subclass of dwarf novae (dns) show recurrent outbursts in which their discs brighten by factors 20-100 as a consequence of mass and angular momentum redistribution on timescales of a few days. dn outbursts are explained in terms of either a thermal-viscous disc-instability (dim, lasota 2001) or a mass-transfer instability (mtim, bath 1975). dim predicts matter accumulates in a low viscosity disc (αcool ∼ 10−2) during quiescence, whereas in mtim the disc viscosity is always high (α ∼ 10−1). therefore, measuring α of a quiescent disc is key to infer which model is at work in a given dn. 2 flickering in cvs: a short review flickering are the intrinsic brightness fluctuations on timescales of seconds to dozens of minutes seen in light curves of t tau stars, mass-exchanging binaries and active galactic nuclei (bruch 2000 and references therein). the first step in understanding what causes flickering is to find out where is comes from. clues for the location of the flickering sources in cvs come from the analysis of eclipsing systems. in u gem, flickering is stronger at orbital hump maximum and disappears during the eclipse of the bright spot (bs) – where the mass transfer stream hits the outer edge of its accretion disc. these results led to the conclusion that flickering in this dn arises at the stream-disc impact region, because of either unsteady mass inflow (warner & nather 1971) or post-shock turbulence (shu 1976). on the other hand, the flickering in ht cas disappears during eclipse of the central source and recovers well before the egress of its bs (patterson 1981), indicating that it originates in the inner disc regions or at the wd-disc boundary layer (bl). possible explanations for this disc+bl flickering include mhd turbulence + convection (geertsema & achterberg 1992), unsteady wd accretion (bruch 1992) or events of magnetic reconnection at the disc atmosphere (kawagushi et al. 2000). a series of extensive optical flickering studies along the 90’s (bruch 1992, 1996, 2000) strengthened the idea that there are two different sources of flickering in cvs: in objects with strong anisotropic emission from the bs the bs-stream flickering component dominates, whereas the disc-bl flickering component prevails in objects where emission is mostly from the accretion disc. 1white dwarf (wd) surface magnetic fields bwd < 105 g. 111 http://dx.doi.org/10.14311/app.2015.02.0111 r. baptista the power density spectra (pds) of flickering sources show a characteristic power-law behaviour at higher frequencies (∝ f−n), with indexes ranging n = 1 − 2, and a flat slope below a cut-off frequency, fc (bruch 1992). the values of n and fc vary from one object to the other and for the same object at different brightness levels (fig. 1). figure 1: optical (b-band) power density spectra for v2051 oph (top) and ht cas (bottom) at two different brightness levels in their quiescent states (differences between bright, intermediate, and faint are 1-2 orders of magnitude lower than differences between outburst and quiescence). dashed lines show the best-fit powerlaw in each case; the corresponding power-law index n is depicted in each panel. 3 estimating the αss parameter 3.1 time changes in disc structure by measuring the (viscous) timescale tv = r/vr ' r2/ν ' r2/(αss csh) with which the disc responds to changes in mass input rate (frank et al. 2002), one might infer a spatially-averaged disc viscosity parameter αss, αss ' r cs tv [ h r ]−1 (1) where vr is the viscous radial drift speed. application of this time-lapse mapping technique to accretion discs of dn in outburst lead to αss ' 10−1 (e.g., baptista & catalán 2001). 3.2 flickering relative amplitude geertsema & achterberg (1992) investigated the effects of mhd turbulence in an accretion disc. they found that the convection of turbulent eddies lead to large fluctuations in the energy dissipation rate per unit area at the disc surface d(r), which could be a source of flickering in cvs and x-ray binaries. encouragingly, the pds of these fluctuations resemble those of flickering sources, with a power-law dependency of similar index range and the flat slope at low-frequencies. perhaps more important, their model gives a direct relation between the energy dissipation rate fluctuations and the disc viscosity parameter, providing an interesting observational way to infer the local accretion disc viscosity – by measuring the relative amplitude of the energy dissipation rate/flickering. in this model, the number of turbulent eddies that contribute to the local fluctuation is, n(r) = 4π r h ( h l )2 , (2) where l is the size of the largest turbulent eddies. the local rms value of the fluctuations σd(r) in the average energy dissipation rate per unit area 〈d(r)〉 is given by, σd(r) ' 2.5 〈d(r)〉/ √ n(r) , (3) while the disc viscosity parameter can be written as, αss = 3 νt 2 csh ' 0.9 ( l h )2 , (4) where νt is the local disc viscosity. if the disc-related flickering is caused by mhd turbulence, it is possible to infer αss from the relative flickering amplitude, σd/〈d〉, αss ' 0.23 [ r 50h ] [ σd(r) 0.05 〈d(r)〉 ]2 . (5) in the thin disc limit (h � r), disc regions with flickering amplitudes of a few percent already lead to large local αss values (≥ 10−1). in this scenario, cvs with highly viscous accretion discs are expected to show significant disc flickering component. how can we measure σd/〈d〉? from a large, uniform ensemble of light curves of a given cv it is possible to separate the steady-light component, lowand highfrequency flickering amplitudes as a function of binary phase, to derive corresponding maps of surface brightness distributions from their eclipse shapes and, thereafter, to compute the radial run of the relative amplitude of the disc flickering component (flickering mapping, see baptista & bortoletto 2004). 112 flickering in cvs and accretion disc viscosity figure 2: the radial run of the disc viscosity parameter inferred from disc flickering relative amplitude distributions, for three strong flicker dns and for the nova-like variable uu aqr. dots with solid line show average αss values, while dashed lines indicate their 1-σ limits. horizontal dashed lines depict the typical αcool = 10−2 value expected for quiescent dn discs according to dim. 4 results and discussion baptista et al. (2011) analyzed an extensive data set of optical light curves of ht cas. their observations frame a 2 d transition from a low state (largely reduced mass transfer rate) back to quiescence, allowing the application of both time-lapse and eclipse mapping techniques to estimate αss and to compare the independently derived results. they find that, in the low state, the gas stream hits the disc at the circularization radius rcirc, and the accretion disc has its smallest possible size. the disc fast viscous response to the onset of mass transfer, increasing its brightness and expanding its outer radius at a speed v ' +0.4 kms−1, implies αss ' 0.3 − 0.5. the newly added disc gas reaches the wd at disc centre soon after mass transfer recovery (∼ 1 d), also implying a large disc viscosity parameter, αss ' 0.5. flickering mapping reveal a minor bs-stream flickering component in the outer disc, and a main disc flickering component the amplitude of which rises sharply towards disc centre, leading to a radial dependency αss(r) ∝ r−2, and to large values αss > 10−1 for r < rcirc (fig. 2) – in agreement with the time-lapse results. a similar analysis was performed for the dn v4140 sgr (baptista et al. 2012). standard eclipse mapping in quiescence indicate that the steady-light is dominated by emission from an extended disc with negligible contribution from the wd, suggesting that efficient accretion through a high-viscosity disc is taking place. flickering maps show an asymmetric source at disc rim (bs-stream flickering) and an extended central source (disc flickering) several times larger in radius than the wd at disc centre. unless the thin disc approximation breaks down, the relative amplitude of the disc flickering leads to large αss’s in the inner disc regions (' 0.15 − 0.3), which decrease with increasing radius. flickering mapping of the dn v2051 oph reveals that the low-frequency flickering arises mainly in an overflowing gas stream and is associated with the mass transfer process. the high-frequency flickering originates in the accretion disc and has a relative amplitude of a few percent, independent of disc radius and brightness level, leading to large αss ' 0.1 − 0.2 at all disc radii (baptista & bortoletto 2004). in uu aqr, optical flickering arises mainly in tidallyinduced spiral shocks in its outer disc (baptista & bortoletto 2008). assuming that the turbulent disc model applies, its disc viscosity parameter increases outwards and reaches αss ∼ 0.5 at the position of the shocks, sug113 r. baptista gesting that they might be an effective source of angular momentum removal of disc gas. since αss increases by two order of magnitude with increasing radius, it is not surprizing that dobrotka et al. (2012) were not able to reproduce the observed pds of uu aqr with a turbulent disc model of constant αss. 5 summary and future steps the picture that emerges from flickering mapping experiments of three dns and of the nova-like variable uu aqr underscores earlier results, indicating that there are mainly two sources of flickering in cvs: the stream-disc impact region in the outer disc and a turbulent inner accretion disc, the relative importance of which varies from system to system. in combination with an mhd turbulent disc model, flickering mapping provides a powerful probe of accretion disc viscosity by allowing one to derive the local magnitude and the radial run of αss from the distribution of the disc flickering relative amplitude. the large αss values found for the three quiescent dns are critical for the outburst mechanism dispute. they are at odds with dim and indicate that the outbursts of a group of dn (strong flickers) are powered by mass-transfer instabilities. two questions related to this result seem to demand further theory development. the first one is why (and how) mass transfer from the donor star in cvs is unstable? the second one is what is responsible for the difference between the low-viscosity discs of quiescent dim-driven dwarf nova and the highviscosity discs of their mtim-driven counterparts? a good first step towards solving this problem might be asking the related question of what is the influence of the wd magnetic field on the radial distribution of αss (e.g., see bisikalo 2014)? an important test of the mhd turbulent disc model still to be done is to perform a flickering mapping experiment on a bona-fide dim-driven dn to check whether it has a low-viscosity accretion disc (as predicted by dim) and if αss is independent of radius (as generally assumed by dim). acknowledgement this work is supported by cnpq/brazil grant 302.443/2008-8. references [1] baptista, r., catalán, m.s.: 2001, mnras, 324, 599 doi:10.1046/j.1365-8711.2001.04320.x [2] baptista, r., bortoletto, a.: 2004, aj, 128, 411 [3] baptista, r., bortoletto, a.: 2008, apj, 676, 1240 doi:10.1086/528706 [4] baptista, r. et al.: 2011, in the physics of accreting binaries, universal academic press (arxiv 1105.1382) [5] baptista, r., borges, b., oliveira, a.: 2012, iau symposium 285, r.e.m. griffin, r.j hanish & r. seaman (eds.), cambridge univ. press, 278 [6] balbus, s.a., hawley, j.f.: 1991, apj, 376, 214 doi:10.1086/170270 [7] bath, g.t.: 1975, mnras, 171, 311 doi:10.1093/mnras/171.2.311 [8] bisikalo, d.: 2014, this proceedings [9] bobinger, a. et al.: 1997, a&a, 327, 1023 [10] bruch, a.: 1992. a&a, 266, 217 [11] bruch, a.: 1996. a&a, 312, 97 [12] bruch, a.: 2000. a&a, 359, 998 [13] dobrotka, a., mineshige, s., casares, j.: 2012, mnras, 420, 2467 doi:10.1111/j.1365-2966.2011.20210.x [14] frank, j., king, a., raine, d.: 2002, accretion power in astrophysics, cambridge univ. press doi:10.1017/cbo9781139164245 [15] geertsema, g.t., achterberg, a.: 1992, a&a, 255, 427 [16] kawagushi, t., et al.: 2000, pasj, 52, l1 [17] lasota, j.p.: 2001, new astronomy review, 45, 449 doi:10.1016/s1387-6473(01)00112-9 [18] patterson, j.: 1981, apjs, 45, 517 doi:10.1086/190723 [19] shakura, n.i., sunyaev, r.a.: 1973, a&a, 24, 337 [20] shu, f.h.: 1976, in structure and evolution of close binary systems, p. eggleton, s. mitton & j. whelan (eds.), dordrecht, 253 [21] warner, b., nather, r.e.: 1971, mnras, 152, 219 doi:10.1093/mnras/152.2.219 discussion john cannizzo: what is the theoretical expression used in determining αss from the speed of the cooling front? raymundo baptista: inferences of αss from time-lapse mapping of outbursting dns are generally 114 http://dx.doi.org/10.1046/j.1365-8711.2001.04320.x http://dx.doi.org/10.1086/528706 http://dx.doi.org/10.1086/170270 http://dx.doi.org/10.1093/mnras/171.2.311 http://dx.doi.org/10.1111/j.1365-2966.2011.20210.x http://dx.doi.org/10.1017/cbo9781139164245 http://dx.doi.org/10.1016/s1387-6473(01)00112-9 http://dx.doi.org/10.1086/190723 http://dx.doi.org/10.1093/mnras/152.2.219 flickering in cvs and accretion disc viscosity based on measurements of the speed of the heating wave during rise, instead of the cooling wave. [note added: bobinger et al. (1997) adopted the expression αcool = vcool/cs to estimate the disc viscosity parameter from their measured speed of the cooling wave vcool. this expression lead to α values smaller than derived from eq. (1) by a factor (h/r).] 115 context flickering in cvs: a short review estimating the ss parameter time changes in disc structure flickering relative amplitude results and discussion summary and future steps acta polytechnica ctu proceedings doi:10.14311/app.2017.10.0038 acta polytechnica ctu proceedings 10:38–42, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app temperature of soil monitored at experimental sites in perm region (russia) andrey ponomaryov∗, aleksandr zakharov perm national research polytechnic university, kuibysheva street 109, perm, russia ∗ corresponding author: spstf@pstu.ru abstract. the paper presents the monitoring results for soil temperatures in the geological and climatic conditions of the city of perm (russia). the monitoring results are presented for two experimental sites. site 1 is characterized by dense urban development and related to type i soil conditions in perm (the left-bank area of perm). site 2 is located in a low-urbanised region of the city and is related to type ii soil conditions in perm (the right-bank area of perm). keywords: temperature of soil, monitoring site, energy-efficient foundations. 1. introduction the department of construction technology and geotechnics of perm national research polytechnic university has conducted studies of the temperature fields on ground bases in the city of perm since 2009. research is being carried out to quantify the thermal behavior of soil for the main types of geotechnical condition. quantitative assessment of subgrade temperature is one of the main factors allowing introduction of a process based on the use of the soil thermal energy. in particular, these are the energy-efficient foundations and underground structures of buildings. as a rule, technologies based on the use of soil thermal energy are employed for the heating and cooling of buildings, at the very least to provide electricity and hot water. these technologies have been widely used in european and neighboring countries [1–5]. their introduction in russia at this point is not yet much in evidence. 2. geological section of experimental sites research of temperature fields on ground bases are being carried out for two basic types of geotechnical conditions specific to the left-bank and right-bank areas of perm city. studies are being conducted at two sites: • site 1 the monitoring system is installed at the civil engineering faculty pnrpu in the sverdlovsky district of perm (left bank of the city). monitoring has been carried out continuously from december 2008 to the present time. site 1 is characterized by dense urban development. the development age is more than 50 years. the distance from the observation well to the nearest building is about 3 m. taking the results of a geological engineering survey, experimental site 1 is comprised of quaternary alluvialdealluvial clayey soil of a total thickness of 11.6 m, with up to 60-70 % of pebbles at the bottom. quaternary soils are overlaid by filled-up ground of thickness 6.0 m. filled-up ground is represented by clay soil of semi-solid to plastic consistency at the base with an admixture of 60-70 % of construction waste (rubble, broken bricks, glass, wood). the bedrock is argillites uncovered at a depth of 17.6 m. quaternary alluvial-dealluvial deposits are mainly represented by clay of solid to semi-solid consistency underlying the pebble with loamy sand of solid consistency (the content of gravel and pebbles being 60-70 %). the geological section is shown in fig. 1a. • site 2 the monitoring system is installed on the territory of the university campus in the leninsky district of perm (the right bank of the city). monitoring has been carried out since august 2015. currently monitoring data has been obtained up to january 2016. site 2 is located on the undeveloped area of the city. the distance to the nearest building is more than 30 m. according to the results of archival research of the surrounding area, site 1 is comprised of quaternary alluvial sand and clay of a total thickness of 15 m, with 25 % of gravel at the bottom. quaternary alluvial deposits are represented by fine sand, clay and clay soils of plastic to liquid consistency. the gravel inclusion was marked from a depth of 1.0 m along the full thickness of the alluvial soils with an increase to the base up to 25 %. according to the results of archive research the bedrock was uncovered at a depth of 17.0 m. the geological section is shown in fig. 1b. according to the results of geotechnical studies sites 38 http://dx.doi.org/10.14311/app.2017.10.0038 http://ojs.cvut.cz/ojs/index.php/app vol. 10/2017 temperature of soil monitored at experimental sites figure 1. geological section of experimental sites 1 and 2 are assigned to the i and ii types of geotechnical conditions respectively, specific to perm [6]. 3. monitoring results of the temperature fields studies of the temperature field distribution in the soil were carried out by installing a resistive temperature transducer (temperature sensors). installation of this resistive temperature transducer was made in a predrilled hole with a protective casing. to gather the data rtm 59 loggers were used for measuring, continuous recording and monitoring of temperature and other non-electrical values (frequency, pressure, flow, level, etc.), converted into electrical signals of strength, dc voltage and dc resistance [7]. the thickness of the observed soil mass on the site 1 is 19 m. the temperature sensors were installed at intervals of 1 m. monitoring of temperature fields has been held for more than 5 years on site 1. the summarized monitoring results (average monthly temperatures for the period from january 2009 to january 2016) are shown in fig. 2. as given in the diagram the temperature of the soil mass from a depth of 8-9 m is practically independent of the seasonal outdoor temperature fluctuations. the temperature is about 12 °c, falling to 10 °c to the depth of 19 m. to analyze the temperature fluctuations for several annual cycles the average monthly temperatures in september over the period 2009-2015 is shown in fig. 3. as given in the diagram the temperature of the soil mass from a depth of 8-9 m is constant (the difference is not more than 1 °c) during 6 years of monitoring. soil temperatures in september 2015 are explained by abnormally low outside temperatures in summer 2015. the thickness of the observed soil mass on the site 2 is 37 m. the temperature sensors were installed 39 andrey ponomaryov, aleksandr zakharov acta polytechnica ctu proceedings figure 2. site 1. diagram of average monthly temperatures of soil mass according the monitoring results from 2009 to 2016 figure 3. site 1. diagram of average monthly temperatures of soil mass in september for the 2009-2015 at intervals of 2 m, to a depth of 3 m with intervals equal to 0.5 m. monitoring of the temperature fields on site 2 has been carried out since august 2015. currently monitoring data of temperature distribution in the soil mass has been obtained up to january 2016. monitoring results (average monthly temperatures) are shown in fig. 4. analysis of monitoring results on site 2 displays the temperature of soil mass from a depth of 9 m as constant and equal to 6-7 °c. for further analysis the average monthly temperatures of soil mass for september 2015 are shown in table 1 and fig. 5 for both sites. 4. conclusions based on the monitoring of the temperature regime of soils, conclusions are drawn: (1.) the temperature of the ground for the second site is + 6-7 °c and does not change over a depth of 9 m. (2.) the temperature of the ground of the first site is + 10-12 °c and does not change during the year from a depth of 9 m. with the depth reading, the temperature decreases. (3.) on the temperature regime of soils, the density of development of the territory under study has a significant influence. the higher temperatures of the ground massif of the first site are due to the proximity of the building of the faculty of civil engineering with a heated basement. 40 vol. 10/2017 temperature of soil monitored at experimental sites figure 4. site 2. diagram of average monthly temperatures of soil mass according the monitoring results from august 2015 to january 2016 figure 5. diagram of average monthly temperatures in september for sites 1 and 2 table 1. average monthly temperatures of soil mass in september for sites 1 and 2 41 andrey ponomaryov, aleksandr zakharov acta polytechnica ctu proceedings references [1] h. brandl, d. adam, r. markiewicz. ground-sourced energy wells for heating and cooling of buildings. acta geotechnica slovenica 3(1):5–27, 2006. [2] r. katzenbach, d. adam, t. waberseck. on the geotechnical conditions of construction in the city of perm. problems of soil mechanics and foundation engineering in difficult ground conditions. in proc. of the international scientific conference dedicated to the 50th anniversary of bashniistroy 3-5 october. ufa: bashniistroy, 2006. [3] v. g. shapoval, b. v. morklyanyk. the temperature field in the soil base of heat pumps: monograph. dnepropetrovsk: porohy, 2011. [4] a. b. ponomaryov, a. v. zakharov. use of geothermal energy of soils for heating and air-conditioning of buildings. bulletin of volgograd state university of architecture and civil engineering 17(36):119–122, 2010. [5] a. zakharov. application of geothermal energy of the ground for heating of buildings in the climatic and engineering geological conditions of the perm region. bulletin of civil engineers 2 (23) 2(23):85–89, 2010. [6] r. katzenbach, t. waberseck, d. adam, a. ennigkeit. innovationen bei der nutzung geothermischer energie durch erdberührte bauwerke, wie z.b. pfahlgründungen mittels energiepfählen. geothermie-symposium "erdwärme energieträger der zukunft", 25.11.2002 bremerhaven / bremerhavener energiemanagement-agentur. 2002. [7] a. b. ponomaryov, a. v. zakharov. analysis of the interaction of energy foundations in the geological and climatic conditions of the city of perm. pnrpu bulletin 4:24–33, 2011. 42 acta polytechnica ctu proceedings 10:39–43, 2017 1 introduction 2 geological section of experimental sites 3 monitoring results of the temperature fields 4 conclusions references acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0056 acta polytechnica ctu proceedings 4:56–61, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app proton radiography with the pixel detector timepix václav olšanskýa,b,∗, pavel krista, jiří bílab, carlos granjac, radek maříkd, david chvátila a nuclear physics institute of the czech academy of sciences, husinec-řež, czech republic b faculty of mechanical engineering, czech technical university in prague, czech republic c institute of experimental and applied physics, czech technical university in prague, czech republic d faculty of electrical engineering, czech technical university in prague, czech republic ∗ corresponding author: olsansky@ujf.cas.cz abstract. this article presents the processing of radiographic data acquired using the positionsensitive hybrid semiconductor pixel detector timepix. measurements have been made on thin samples at the medical ion-synchrotron hit [1] in heidelberg (germany) with a 221 mev proton beam. the image contrast is generated by the energy of charged particles imparted after passing through the sample. experimental data from the detector were processed for the establishment of the energy loss of each proton using calibration matrices. the interaction point of the proton on the detector was determined with subpixel resolution by a model fitting of the individual signals in the pixel matrix. three methods have been used for the calculation of these coordinates: hough transformation, 2d gaussian fitting and estimate of the 2d mean. parameters of the calculation accuracy and the calculation time are compared for each method. the final image was created by the method with the best parameters. keywords: radiography, charged particles, timepix, medipix, image processing. 1. introduction radiography is often associated with the x-ray radiography, where the image is formed by an attenuation of the beam after passing through the sample. the image is recorded on a radiologic film, a foil or a memory area detector [2]. the process is similar to conventional photography, where negative is created according to radiation intensity. in contrast to this principle proton radiography can get the imaging information about one pixel with only one particle that has passed through this point [3]. therefore it is necessary to know the energy of the particle. thus the principle of proton radiography is to determine the energy of each particle after passing through the analyzed sample. hence proton radiography is suitable for imaging thin samples. the advantages of proton radiography are high sensitivity, high spatial resolution imaging of thin samples and the imaged objects receiving a lower dose [4]. although the absorbed dose by a single proton is significantly higher than that of a photon, the total radiation dose is reduced due to the need for only a single proton to display a single pixel [5, 6]. the aim is to create a system of automatic image processing of proton radiography. proton radiography, unlike traditional x-ray radiography, offers new possibilities and specific imaging thin samples, which can achieve greater sensitivity and spatial resolution. 2. pixel detector timepix 2.1. hybrid semiconductor detector timepix the timepix detector [7] is a position-sensitive semiconductor pixel detector of the family of medipix detectors developed at cern [8]. timepix, based on the previous device medipix2 [9], timepix provides perpixel energy sensitivity. the detector consists of a radiation sensitive semiconductor sensor bump-bonded to the timepix asic readout chip. the sensor can be of different material (si, cdte, gaas) and thickness (e.g. 300, 700, 1000, 1500 µm). the detector provides an array of 256 × 256 pixels for a total of 65 536 independent channels. size of one pixel is 55 µm and the full sensor size is 14 × 14 mm (1.98 cm2). each pixel is connected with its analog and digital signal chain including amplifier, discriminator, counter and digital integrator [7]. 2.2. timepix principle ionizing particles produce in the sensor a cloud of charge which is collected as in a standard semiconductor diode. the collection of charges undergoes charge sharing (due to diffusion) and results in a signal containing several pixels forming a so-called cluster of pixels [10]. the distribution of charge around the impact point has the character of a gaussian. data are recorded in frames which are saved to individual file frames which are time stamped. all data of events are saved to one frame during the selected time. events 56 http://dx.doi.org/10.14311/ap.2016.4.0056 http://ojs.cvut.cz/ojs/index.php/app vol. 4/2016 proton radiography with the pixel detector timepix figure 1. one frame with cropped selection. the left figure shows one frame of radiographic data. this frame contains 9 suitable events and few unwanted values which are recorded by x-rays. three suitable events and three unwanted values are shown on the right figure, where it is displayed the cropped area from left figure. which have been recorded at next selected time are saved to next frame. the detector pixels can be independently operated in three ways depending on the mode in which the detector works [7]: • medipix mode: each event is counted in this mode. it can be used to count the event rate. • timepix mode: value which is recorded in this mode corresponds to the time of interaction during the frame. • time over threshold (tot) mode: the time registers the amount of charge which is given by the energy deposited. data which are measured by mode tot is necessary to calibrate into energy. calibration matrices are used for this calculation [11]. four calibration matrices are used a, b, c and t. the calibration coefficients are obtained by calibration procedure using discrete-energy x-rays from laboratory x-ray sources on xrf [11–13]. the energy was calculated according to equation x = ta + y − b + √ (b + ta − y )2 + 4ac 2a , where x is the matrix with pixel values in energy in [kev], y is the matrix which contains pixel values recorded in [tot] counts and matrices a, b, c and t contain calibration values. 3. experiment and data processing 3.1. description of experimental setup and radiographic data radiographic data used in this work were measured at the hit ion synchrotron [1] in heidelberg (germany). the sample was irradiated by almost monoenergetic proton beam with energy 221 mev. a sample consisting thin foils which were stacked one over the other and a fly’s wing were used a sample. the sample was irradiated in air. the timepix detector which worked at tot mode was placed behind the sample. protons were registered by the detector after passing through the sample. data from the detector were structured into 34 files. each of these files contained around 1000 frames. the duration of one frame was 0.2 seconds. the value of tot and coordinate of each pixel where the threshold had been exceeded were stored. the average number of protons events per frame was about 10 events per frame. the impact of proton on detector creates a round track with a diameter around 7 pixels as shown in fig. 1. this event has as character so called cluster (see fig. 1 and fig. 2) that can be fitted by a 2dgaussian. the highest tot values are located in the center of the track (fig. 2). the position of impact on the detector can be accurately determined based on analysis and fit of all pixels of the event recorded. sub-pixel resolution can be achieved as well. the total energy deposited to the detector by one proton corresponds to the sum of the energy values of all pixels in the cluster. 3.2. data processing methods and their comparasion because all data that were contained in the files were not suitable for processing, it was necessary to select a suitable event record, to avoid unadvisable events and prepare the data for further processing. 2d filtering was used for eliminating unwanted and false events. nonzero pixels were calibrated using energy calibration matrices. furthermore approximate coordinates of each protons impact have been found. an area of 11 × 11 pixels was cropped around these approximate coordinates. because the diameter of the event record was about 7 pixels, it was probable that each pixel corresponding to this event record was included in this cropped area. then the area was evaluated whether it would be suitable for further processing. if two or 57 v. olšanský, p. krist, j. bíla et al. acta polytechnica ctu proceedings figure 2. registration of a proton event in timepix operated in tot (energy mode). the color and height of bars represents the energy of one pixel of the detector. more event records overlapped at one cropped area, this area was not suitable for further work. it was necessary to accurately determine the location of protons impact for image reconstruction. three methods were used for calculation of the precise location of the impact of the proton: hough transform [14], 2d gaussian fitting [15] and estimation of 2d mean [16]. these methods were mutually compared and the reconstruction of image was performed from the results of the most suitable method. hough transform. the detection of the circle, described by equations (1), was used for assessing the center of the event by hough transformation. the idea was in presumption that each event record had a circular nature. a matrix with data of the one frame was converted into a binary map. all contour points of event record were found by using the edge detector. coordinates of circles points which had the same radius as a radius of event records were calculated from the coordinates of each edge point. eighty points of circle coordinates were calculated for each edge point. the value of one was added at each point, whose coordinates were calculated in this manner. maximum of added values was subsequently calculated for each event. there is the impact point. equations (1) describes the calculation of the circles coordinates with center at each edge points, x(θ) = x0 + r cos θ, y(θ) = y0 + r sin θ, (1) where x0, y0 are coordinates of edge points, θ is an angle from 0 to 2π. step of angle θ calculation was chosen up to 1/80 of the circle. variables x(θ), y(θ) are coordinates of the new circle for one angle θ, r is the radius of the circle [14]. 2d gaussian fitting. gaussian fitting was used for calculating center coordinates the impact of one proton as another way. it was performed for only cut selection around traces of impacts. data were fitted to 2d gaussian with equation f(x, y) = c1 + c2 exp ( − ( x− c3 c4 )2 − ( y − c5 c6 )2 ) , where c3 a c5 are coordinates of the center of 2d gaussian. it corresponds to the location of a proton impact. coefficient c1 corresponds to dislocation, c2 is amplitude and c4 and c6 corresponds to spread of the blob. estimation of 2d mean. estimate of 2d mean was used as the last method for determination center of events records. the energy values of events records were normalized, so that the total sum of all values was equal to one. first of all the normalized values were added up vertically. then the results of these sums were multiplied by the respective horizontal coordinates. finally these values were added up too. this result was one number only and it was the horizontal center coordinate. the same method was used for the calculation of the vertical center coordinates. 4. results 4.1. comparision of methods methods have been mutually compared. similar accuracy was reached using methods estimating 2d mean and 2d gaussian fitting. calculation of the estimate of 2d mean value was about 30 times faster than the 2d gaussian fitting. calculation using the hough transform amounted to less accuracy, and it was also significantly slower than the calculation of 2d mean. comparing of the average euclidean distance between the locations of particles impacts detected using each method and their standard deviations are shown by using each method in table 1. compared methods avg. eukl. dist. std [px] [px] gaussian fitting vs. estimate of 2d mean 0.107 0.057 hough transform vs. gaussian fitting 0.749 0.302 estimate of 2d mean vs. hough transform 0.729 0.295 table 1. comparison of euclidean distance between the location of protons impacts and its standard deviation. it is evident from table 1 that similarly accurate results were achieved using methods: 2d gaussian fitting and the estimation of 2d mean. mean euclidean distance between of these methods was caused by mutual displacement in one direction. this shift 58 vol. 4/2016 proton radiography with the pixel detector timepix was caused slight displacement of the resulting reconstructed image only. the representation of centers of events records using different methods is shown in fig. 3. histograms which are shown in fig. 4 and 5 were created on the basis of the calculation euclidean distances between the centers coordinates of events records detected using each method. figure 3. centroid fitting for one event recorded. the calculated centroid coordinates are shown in the middle of this figure. data1 shows centered calculated using the 2d gaussian fitting, data2 shows calculated center using the estimation of 2d mean and a data3 shows the detected center using hough transform. figure 4. histogram euclidean distances between centroids computed by gaussian fitting and estimation the mean 2d. 4.2. image reconstruction the final image was created from centers coordinates of each trace of impact whose calculation was described in the previous section. this image was created from the sum of the total energy. the value of the total energy which was given to the detector by a proton was calculated as the sum of all energy values of one event record. this value was assigned figure 5. histogram euclidean distances between centroids computed by gaussian fitting and hough transform. to the point whose coordinates have been detected as the place of protons impact. if one pixel of the final image was located for more events than one, the average value of these energetic records was assigned this point. points without localized event are assigned zero value. these points appeared as holes in final image. values for these points can be improved in the final image by extrapolating values from the surrounding area. just one proton can suffice for displaying a pixel. each proton passed through the sample carries the information about a point of the sample. the final image can be displayed magnified due to the subpixel resolution of located impacts coordinates. the picture created from all the 33 000 frames was refined at double zoom. localized have been around 340 000 events. this corresponds to an average of 1.3 protons per pixel. an example of such image is shown in fig. 6. 5. discussion and conclusion the resulting images, which were reconstructed from data obtained using the methods of 2d gaussian fitting and estimation of 2d median values were essentially identical. to display a single image pixel was sufficient to locate the coordinates of only one proton impact. because here we do not measure the decline of are irradiance detector, but directly the decrease of the energy particles is achieved by lower radiation load samples compared with other radiological imaging methods for example x-ray radiography. experimentally it was found that it was ideal to enlarge final image twice. in this view, it may well calculate the value of the missing pixel, because in the vicinity of missing values there are many pixels designed so as to have one missing value extrapolated. the algorithm was created for a complete data processing. the data were processed automatically starting from 59 v. olšanský, p. krist, j. bíla et al. acta polytechnica ctu proceedings figure 6. final radiogram. proton radiography of a composite sample consisting of an assembled foil array and a fly’s wing. the final image was made from coordinate locations of proton impacts using estimating the 2d mean. one pixel represents 22.5 × 22.5microns. there was located on the average 1.3 protons per pixel. the records of the detector and the resulting final image. another advantage of proton radiography in addition to lower radiation burden is the availability of application accelerators. for the future it is planned to apply radiography using charged particle accelerators van de graaff hv2500 – ieap ctu [17] and cyclotron u-120m – npi ascr [18], which would also examine pokes energy charged particles after passing the samples. also, the plan is to try and apply electron radiography to microtron mt25 – npi ascr [19, 20]. at the electron radiography should be an option to display an image using electron scattering in the sample. here, the dispersion is measured and determined by using the aperture, which should be placed on the fourier plane between magnetic lenses respectively quadrupoles [21]. it is also planned to develop a new automated data processing systems from new applications and other optimization of automated processing system previously available data. references [1] c. schoemers, e. feldmeier, j. naumann, et al. the intensity feedback system at heidelberg ion-beam therapy centre. nuclear instruments and methods in physics research section a: accelerators, spectrometers, detectors and associated equipment 795:92–99, 2015. doi:10.1016/j.nima.2015.05.054. [2] j. jakubek, j. dammer, t. holy, et al. spectrometric properties of timepix pixel detector for x-ray color and phase sensitive radiography. in 2007 ieee nuclear science symposium conference record, vol. 3, pp. 2323–2326. 2007. doi:10.1109/nssmic.2007.4436610. [3] s. braccini, a. ereditato, i. kreslo, et al. first results on proton radiography with nuclear emulsion detectors. journal of instrumentation 5(09):p09001, 2010. [4] v. w. steward. proton (heavy ion) radiography in medical diagnosis. ieee transactions on nuclear science 26(2):2257–2261, 1979. doi:10.1109/tns.1979.4329851. [5] u. schneider, j. besserer, p. pemler, et al. first proton radiography of an animal patient. med phys 31(5):1046–1051, 2004. doi:10.1118/1.1690713. [6] a. k. biegun, j. visser, t. klaver, et al. proton radiography with timepix based time projection chambers. ieee transactions on medical imaging 35(4):1099–1105, 2016. doi:10.1109/tmi.2015.2509175. [7] x. llopart, r. ballabriga, m. campbell, et al. timepix, a 65k programmable pixel readout chip for arrival time, energy and/or photon counting measurements. nuclear instruments and methods in physics research section a: accelerators, spectrometers, detectors and associated equipment 581(1–2):485–494, 2007. doi:http://dx.doi.org/10.1016/j.nima.2007.08.079. [8] j. vallerga, j. mcphate, a. tremsin, o. siegmund. high-resolution uv, alpha and neutron imaging with the timepix cmos readout. nuclear instruments and methods in physics research section a: accelerators, spectrometers, detectors and associated equipment 591(1):151–154, 2008. doi:http://dx.doi.org/10.1016/j.nima.2008.03.046. [9] x. llopart, m. campbell, r. dinapoli, et al. medipix2: a 64-k pixel readout chip with 55-µm square elements working in single photon counting mode. ieee transactions on nuclear science 49(5):2279–2283, 2002. doi:10.1109/tns.2002.803788. [10] j. jakubek, a. cejnarova, t. holy, et al. pixel detectors for imaging with heavy charged particles. nuclear instruments and methods in physics research section a: accelerators, spectrometers, detectors and associated equipment 591(1):155–158, 2008. doi:http://dx.doi.org/10.1016/j.nima.2008.03.091. [11] j. jakubek. precise energy calibration of pixel detector working in time-over-threshold mode. nuclear instruments and methods in physics research section a: accelerators, spectrometers, detectors and associated equipment 633, supplement 1:s262–s266, 2011. doi:http://dx.doi.org/10.1016/j.nima.2010.06.183. [12] j. jakůbek, j. dammer, t. holý, et al. digitální transmisní radiografie s pixelovými detektory medipix. československý časopis pro fyziku 58(1):25–36, 2008. [13] j. jakůbek, a. cejnarová, s. pospíšil, j. uher. polohově citlivá spektrometrie s pixelovými detektory timepix. československý časopis pro fyziku 58(1):37–45, 2008. 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[16] t. wang, i. y. h. gu, p. shi. object tracking using incremental 2d-pca learning and ml estimation. in 2007 ieee international conference on acoustics, speech and signal processing – icassp ’07, vol. 1, pp. i–933–i–936. 2007. doi:10.1109/icassp.2007.366062. 60 http://dx.doi.org/10.1016/j.nima.2015.05.054 http://dx.doi.org/10.1109/nssmic.2007.4436610 http://dx.doi.org/10.1109/tns.1979.4329851 http://dx.doi.org/10.1118/1.1690713 http://dx.doi.org/10.1109/tmi.2015.2509175 http://dx.doi.org/http://dx.doi.org/10.1016/j.nima.2007.08.079 http://dx.doi.org/http://dx.doi.org/10.1016/j.nima.2008.03.046 http://dx.doi.org/10.1109/tns.2002.803788 http://dx.doi.org/http://dx.doi.org/10.1016/j.nima.2008.03.091 http://dx.doi.org/http://dx.doi.org/10.1016/j.nima.2010.06.183 http://dx.doi.org/10.1016/0031-3203(81)90009-1 http://www.mathworks.com/matlabcentral/fileexchange/37087-fit-2d-gaussian-function-to-data http://www.mathworks.com/matlabcentral/fileexchange/37087-fit-2d-gaussian-function-to-data http://www.mathworks.com/matlabcentral/fileexchange/37087-fit-2d-gaussian-function-to-data http://dx.doi.org/10.1109/icassp.2007.366062 vol. 4/2016 proton radiography with the pixel detector timepix [17] c. granja, m. solar, s. pospisil, et al. basic and applied research with tunable mono-energetic neutrons at prague van-de-graaff accelerator. to be published in proc. xii int. topical meeting on nuclear applications of accelerators (accapp 2015). [18] department of accelerators. isochronous cyclotron u-120m. http://accs.ujf.cas.cz/. [19] a. belov, d. chavatil, c. simane, m. vognar. electron and gamma bremsstrahlung beams of jinr and ctu microtrons. czechoslovak journal of physics 50(1):385–386, 2000. doi:10.1007/s10582-000-0079-9. [20] c. granja, p. krist, d. chvatil, et al. energy loss and online directional track visualization of fast electrons with the pixel detector timepix. radiation measurements 59:245–261, 2013. doi:http://dx.doi.org/10.1016/j.radmeas.2013.07.006. [21] f. merrill, f. harmon, a. hunt, et al. electron radiography. nuclear instruments and methods in physics research section b: beam interactions with materials and atoms 261(1–2):382–386, 2007. doi:http://dx.doi.org/10.1016/j.nimb.2007.04.127. 61 http://accs.ujf.cas.cz/ http://dx.doi.org/10.1007/s10582-000-0079-9 http://dx.doi.org/http://dx.doi.org/10.1016/j.radmeas.2013.07.006 http://dx.doi.org/http://dx.doi.org/10.1016/j.nimb.2007.04.127 acta polytechnica ctu proceedings 4:56–61, 2016 1 introduction 2 pixel detector timepix 2.1 hybrid semiconductor detector timepix 2.2 timepix principle 3 experiment and data processing 3.1 description of experimental setup and radiographic data 3.2 data processing methods and their comparasion 4 results 4.1 comparision of methods 4.2 image reconstruction 5 discussion and conclusion references acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0107 acta polytechnica ctu proceedings 4:107–112, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app comparison of s-co2 power cycles for nuclear energy ladislav veselya,∗, vaclav dostala, slavomir entlerb a faculty of mechanical engineering, czech technical university in prague, technická 4, 166 07 prague 6, czech republic b institute of plasma physics of the cas, za slovankou 3, 182 00 prague 8, czech republic ∗ corresponding author: ladislav.vesely@fs.cvut.cz abstract. the supercritical carbon dioxide (s-co2) is a possible cooling system for the new generations of nuclear reactors and fusion reactors. the s-co2 power cycles have several advantages over other possible coolants such as water and helium. the advantages are the compression work, which is lower than in the case of helium, near the critical point and the s-co2 is more compact than water and helium. the disadvantage is so called pinch point which occurs in the regenerative heat exchanger. the pinch point can be eliminated by an arrangement of the cycle or using a mixture of co2. this paper describes the s-co2 power cycles for nuclear fission and fusion reactors. keywords: s-co2, power cycle, fusion. 1. introduction the supercritical carbon dioxide (s-co) cycles are recently very prospective power cycles for different applications. these applications are ranging from nuclear through geothermal, solar energy and waste heat recovery systems. these cycles are researched all around the world. the research of the power cycles with co2 as working medium has a long history. the first reference is dated back to 1948, when sulzer bros. patented a brayton cycle with the partial condensation of co2. the worldwide research of s-co2 power cycles is dating to the second half of the 20th century [1]. researchers began to realize benefits of co2 as working medium in power cycles at that time. among the first researchers who studied benefits of co2 power cycles belongs angelino, feher, verhivker and gokhstein [2]. the research on czech technical university in prague (ctu) is oriented on the analysis of the s-co2 power cycles with a potential for the nuclear reactors, as well as for the fusion power reactors. the design of the s-co2 power cycle is very important and it has effect on the cycle efficiency and net power. the s-co2 cycle is also suitable for utilization of heat from multiple heat sources with different temperature and heat power. this is important in a case of multiple heat sources providing high and low potential heat like fusion power reactors. this paper is focused on comparison of the s-co2 cycles for nuclear energy. benefits of the s-co2 cycle will be described for the nuclear fission and fusion reactors. the design of the s-co2 cycle will be applied for multiple heat source in fusion reactor. 2. advantages and disadvantages of s-co2 cycles the main advantage of the s-co2 cycles is the compression work which is lower than in case of helium [2]. a compressor work reduction is caused due to operation in near the critical point. the critical point of co2 occurs at the temperature 30.98 ◦c and pressure 7.32 mpa. the s-co2 cycle is more compact than water and helium because this cycle operating at high pressure and allows small size of components. another advantage is that the s-co2 cycle achieves high efficiency with low operates temperature. the s-co2 cycles also have several disadvantages. the existence of so called “pinch point” in heat exchangers significantly affecting their design is the most important and well-known disadvantage. the pinch point may be present for any type of medium, but its influence on components is especially high when co2 is employed as a working medium. the pinch point primarily occurs in recuperative heat exchangers with identical working media and mass flow on both the hot and the cold side. the pinch point is caused by the variations of heat capacity of co2 and occurs when the heat capacity of the hot and cold streams (each at a different pressure level) intersect. due to the pinch point, the heat exchangers may have a large size and low efficiency. however, this problem can be removed in several ways. one of them is an addition of the small amount of other substance into the pure co2. the substances for shift of pinch point could be ar, he, co, o2 or n2 [3]. the other ways is a change of the design of cycles and usage of different mass flows in hot and cold side of heat exchangers. 107 http://dx.doi.org/10.14311/ap.2016.4.0107 http://ojs.cvut.cz/ojs/index.php/app l. vesely, v. dostal, s. entler acta polytechnica ctu proceedings 3. description of gas cycles the s-co2 cycle is a gas cycle derived from the ericsson-brayton cycle, which offers many different layouts for solar, geothermal or nuclear power plants and waste heat recovery. each layout tries to approach the carnot cycle and its efficiency. the basic layouts considering the use of s-co2 are [2]: • simple brayton cycle, • re-compression cycle, • pre-compression cycle, • split expansion cycle, • partial cooling cycle, • partial cooling with improved regeneration. figure 1. simple brayton cycle. the simple brayton cycle is shown in figure 1. this cycle has a turbine (t), compressors (c1), recuperative heat exchanger (rh), a cooler (c) and a heater (h). figure 2. re-compression cycle. the re-compresion cycle is shown in figure 2. the difference between the simple brayton cycle and recompression cycle is twice a number of the compressors and recuperative heat exchanger. the re-compression cycle has a turbine (t), two compressors (c1 and c2), two recuperative heat exchangers (ltr and htr), cooler (c) and heater (h). in figure 3, the pre-compression cycle is shown, and figure 4 presents the split expansion cycle. the pre-compression cycle and the split expansion cycle have same components as the re-compression cycle. only two turbines has the split expansion cycle. figure 3. pre-compression cycle. figure 4. split expansion cycle. the partial cooling cycle is shown in figure 5. the partial cooling cycle contains the two coolers (ca and cb) and three compressors. figure 5. partial cooling cycle. 108 vol. 4/2016 comparison of s-co2 power cycles for nuclear energy 4. the gfr re-compressing cycle the s-co2 cycles for nuclear energy are based on the presented cycles of co2. the re-compression cycle applied to the gas-cooled fast reactors (gfr) is analyzed in this study. the re-compression cycle is used as basic concept for gfr. other type of s-co2 cycle has similar results as the re-compression cycle [4]. the cycle layout is arranged according to the figure 2. the ltr exchanger is sensitive to the pinch point due to operation near the critical point. the recompression cycle eliminates the pinch point using different mass flows of the ltr exchanger. the parameters for calculation are shown in table 1. the compressor inlet temperature is 34 ◦c. the turbine inlet temperature is 550 ◦c. the heat source is considered with the minimum inlet temperature into the heater about 600 ◦c. the thermal power is 600 mw [5]. the cycle was optimized for the best parameters with thermal power 600 mw. thermal power 600 mw compressor efficiency 68 % turbine efficiency 79 % recuperator effectiveness 90 % compressor inlet temperature 34 ◦c turbine inlet temperature 550 ◦c table 1. parameter of the gfr s-co2. 5. the s-co2 cycle for demo2 fusion reactor in the case of the fusion reactor, the re-compression cycle is used as the first. the heat sources are arranged behind [6]. however, the layout of the re-compression cycle can be designed differently. the heat sources can be situated to other streams [7]. the different layout of the s-co2 power cycle can be a benefit for the heat transfer and net power of cycles. a demonstration fusion power plant (demo) represents the first fusion power station capable of producing electricity and operating with a closed fuel-cycle. two demo design options are currently investigated, in an attempt to identify a realistic range of possibilities: a near-term demo1 and an advanced design concept demo2. demo1 is the concept based on reliable technology deliverable in the term of 20 years from now, and it is planned to work in the pulse operation mode. demo2 based on advances in the physics basis deliverable on a longer term is expected in the steady-state operation mode [8]. the demo2 power plant based on the steady-state fusion power reactor is analysed in this study. the demo2 fusion reactor has several different heat sources. the main heat sources are the blanket, first wall, and divertor. each of them operates on different temperatures and powers. the preheating s-co2 cycles may be more suitable for demo2. a layout of the preheating cycle is shown in figure 6. the preheating cycle has benefit for the pinch point mitigation as well as the layout of re-compression cycle. figure 6. preheating cycle. the table 2 brings parameters of the analyzed fusion reactor demo2 model [9]. thermal power of the fusion reactor demo2 is 4109 mw. the blanket has the thermal power of 3887 mw. the thermal power of the divertor and the first wall is 222 mw. the blanket and first wall are cooled by helium, the divertor is cooled by water. the high-grade reactor outlet temperature is projected to 500 ◦c. the low-grade reactor outlet temperature is projected to 160 ◦c. the turbine inlet temperature is 475 ◦c. consequently, the analyzed fusion reactor demo2 has two different heat source. the preheating cycle uses the heater h1 for high-grade primary heat (first wall and blanket). second heater h2 is used for lowgrade secondary heat (divertor). thermal power 4109 mw primary (high-grade) heat 3887 mw secondary (low-grade) heat 222 mw compressor efficiency 68 % turbine efficiency 79 % recuperator effectiveness 90 % compressor inlet temperature 34 ◦c turbine inlet temperature 475 ◦c table 2. parameter of s-co2 for fusion reactor demo2. 6. result of gfr reactor and demo2 fusion reactor the thermodynamic calculation was done for precompression cycle and preheating cycle. the calculation was performed using programming language python. the codes of cycles have been written in python. properties of pure co2 and mixtures are embedded into the python. source of gases and mixtures properties is nist reference fluid thermodynamic and transport properties database, version 9.1. [10]. the calculation of the gfr s-co2 cycle was performed according to the parameters included in table 2. the cycle was optimized for the best results. the results of the gfr re-compression cycle are 109 l. vesely, v. dostal, s. entler acta polytechnica ctu proceedings figure 7. t-s diagram of the gfr re-compression cycle. shown in table 3. the figure 7 shows a t-s diagram of the cycle. according to the table 3, the total net power of re-compression cycle is 201 mw. the cycle efficiency is 33.56 % and the mass flow is 2730 kg/s. cycle efficiency 33.56 % turbine power output 324.98 mw compressor no.1 in. power 89.44 mw compressor no.2 in. power 33.84 mw compressor input power 123.28 mw added heat 600.98 mw removed heat 399.28 mw regenerative heat 1249.15 mw mass flow in ltr (cold s.) 2299.89 kg/s mass flow in com. no.2 430.1 kg/s mass flow ratio 0.842 net power 201.69 mw mass flow 2730.0 kg/s pressure ratio 2.8 pressure no.2 34.0 mpa table 3. result of gfr re-compression cycle. the calculation of s-co2 cycle for demo2 was performed for two cycle. the first cycle is the recompression cycle and the second cycle is preheating cycle. the calculations were performed with the parameters from the table 2. the cycles were optimized for the best results. the result of the demo2 recompression cycle is shown in the table 4. the layout of heat sources corresponds to the figure 2. the heat source h is split into two heat sources arranged serially. according to the table 4, the total net power of the re-compression cycle is 1251 mw. the cycle efficiency is 30.45 %. however, the mass flow for this case is very high and achieves of 20 250 kg/s. cycle efficiency 30.45 % turbine power output 2013.02 mw compressor no.1 in. power 719.62 mw compressor no.2 in. power 42.41 mw compressor input power 762.03 mw added heat 4108.83 mw removed heat 2857.84 mw regenerative heat 8340.95 mw mass flow in ltr (cold s.) 19 589.33 kg/s mass flow in com. no.2 660.66 kg/s mass flow ratio 0.967 net power 1250.98 mw mass flow 20 250.0 kg/s pressure ratio 2.6 pressure no.2 34.0 mpa table 4. result of demo2 re-compression cycle. the figure 8 shows the t-s diagram of the demo2 re-compression cycle. the result of the demo2 pre110 vol. 4/2016 comparison of s-co2 power cycles for nuclear energy figure 8. t-s diagram of the demo2 re-compression cycle. figure 9. t-s diagram of the demo2 preheating cycle. heating cycle is shown in the table 5 and the t-s diagram of the cycle is shown in the figure 9. the layout of heat sources corresponds to the figure 6. the heater h1 was used for high-grade primary heat, the heater h2 was used for low-grade secondary heat. according to the table 5, the total net power of preheating cycle cycle is 1145 mw. the cycle efficiency is 27.87 %, and the mass flow for the preheating cycle is 14 040 kg/s. 111 l. vesely, v. dostal, s. entler acta polytechnica ctu proceedings cycle efficiency 27.87 % turbine power output 1727.14 mw compressor input power 582.005 mw added heat 4108.54 mw removed heat 2963.41 mw regenerative heat 4125.79 mw mass flow in hex 13 338.0 kg/s mass flow in h2 702.0 kg/s mass flow ratio 0.95 net power 1145.13 mw mass flow 14 040 kg/s pressure ratio 3.4 pressure no.2 28 mpa table 5. result of the demo2 preheating cycle. 7. conclusion the results from the table 3 represent the suitable results for the gfr designing with re-compression cycle. improvement of the parameters is possible by future research. the results of the s-co2 cycle for the fusion reactor show the effect of the use of multiple heat sources. the re-compression cycle is better than the preheating cycle according to the table 4 and table 5. however, it is obvious that this advantage is valid only for the net power. the critical disadvantage of the recompression cycle is the mass flow of about 20 000 kg/s. the mass flow of the preheating cycle is lower in comparison with the re-compression cycle. designing and optimization of the s-co2 cycles are of great importance for fusion energy. the preheating cycle is a convenient cycle for utilization of low potential heat, and such cycles are suitable for exploitation of the multiple heat sources of the fusion power reactor like analyzed demo2. further research of the s-co2 power cycles for the fusion power reactors will be focused on the detailed comparison of the s-co2 power cycle and on the development of the new modifications of the s-co2 power cycle, which will take into account the fusion reactor multiple heat source design. references [1] g. angelino. carbon dioxide condensation cycles for power production. j eng power 90(3):287–295, 1968. doi:10.1115/1.3609190. [2] v. dostal, m. driscoll, p. hejzlar. a super critical carbon dioxide cycle for next generation nuclear reactors, vol. mit-anp-tr-100 of advanced nuclear power program. mit center for advanced nuclear energy systems, 2004. [3] v. ladislav, d. vaclav, b. ondrej, n. vaclav. pinch point analysis of heat exchangers for supercritical carbon dioxide with gaseous admixtures in ccs systems. energy procedia 86:489–499, 2016. doi:http://dx.doi.org/10.1016/j.egypro.2016.01.050. [4] e. j. parma, s. a. wright, m. e. vernon, et al. supercritical co2 direct cycle gas fast reactor (sc-gfr) concept. tech. rep. sand2011-2525, sandia national laboratories, 2011. [5] e. a. harvego, m. g. mckellar. optimization and comparison of direct and indirect supercritical carbon dioxide power plant cycles for nuclear applications. in asme 2011 international mechanical engineering congress and exposition, pp. 75–81. 2011. doi:10.1115/imece2011-63073. [6] b. halimi, k. y. suh. computational analysis of supercritical {co2} brayton cycle power conversion system for fusion reactor. energy conversion and management 63:38–43, 2012. doi:http://dx.doi.org/10.1016/j.enconman.2012.01.028. [7] j. i. linares, l. e. herranz, i. fernández, et al. supercritical co2 brayton power cycles for demo fusion reactor based on helium cooled lithium lead blanket. applied thermal engineering 76:123–133, 2015. [8] g. federici, r. kemp, d. ward, et al. overview of eu demo design and r&d activities. fusion engineering and design 89(7–8):882–889, 2014. doi:http://dx.doi.org/10.1016/j.fusengdes.2014.01.070. [9] r. kemp. demo2 reference design, 2015. eurofusion idm eu_d_2lcbvu. [10] e. w. lemmon, m. l. huber, m. o. mclinden. nist reference fluid thermodynamic and transport properties – refprop. national institute of standards and technology, 2013. version 9.1. 112 http://dx.doi.org/10.1115/1.3609190 http://dx.doi.org/http://dx.doi.org/10.1016/j.egypro.2016.01.050 http://dx.doi.org/10.1115/imece2011-63073 http://dx.doi.org/http://dx.doi.org/10.1016/j.enconman.2012.01.028 http://dx.doi.org/http://dx.doi.org/10.1016/j.fusengdes.2014.01.070 acta polytechnica ctu proceedings 4:107–112, 2016 1 introduction 2 advantages and disadvantages of s-co2 cycles 3 description of gas cycles 4 the gfr re-compressing cycle 5 the s-co2 cycle for demo2 fusion reactor 6 result of gfr reactor and demo2 fusion reactor 7 conclusion references acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0013 acta polytechnica ctu proceedings 4:13–18, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app modelling of nuclear fuel cladding tubes corrosion miroslav cecha,∗, martin seveceka,b a department of nuclear reactors, faculty of nuclear sciences and physical engineering, czech technical university in prague, v holesovickach 2, praha 8, czech republic b alvel a.s., opletalova 37, praha 1, czech republic ∗ corresponding author: miroslav.cech@post.cz abstract. this paper describes materials made of zirconium-based alloys used for nuclear fuel cladding fabrication. it is focused on corrosion problems their theoretical description and modeling in nuclear engineering. keywords: corrosion, zirconium alloys, nuclear fuel, cladding, modelling. 1. introduction tubes covering nuclear fuel in current light water reactors (lwr) are made of zirconium-based alloys since the very origin of nuclear power utilization. zirconiumbased alloys were first used in nuclear reactors of u.s. nuclear submarines. later, zr was adopted by fuel vendors as a suitable material for fuel cladding for commercial reactors around the world. zirconium has been chosen for its low cross section for neutron absorption, good corrosion resistance, and other outstanding thermomechanical characteristics. various degradation processes jeopardizing nuclear cladding integrity take place during reactor normal operation such as grid-to-rod fretting, debris-induced failures, crud-induced localized corrosion, waterside corrosion, and hydriding. this article is focused on water corrosion, its quantification, and theoretical description. corrosion reaction caused mainly by an interaction of nuclear fuel cladding and coolant takes place on an external surface of cladding tubes, less frequently reacts internal cladding surface with oxygen released from pelets. in case of lwrs, metal reacts with water and zirconium oxide arises: zr + 2 h2o −−→ zro2 + 2 h2. (1) hydrogen released from the reaction described above partly dissolve in coolant water and partly penetrates tubes causing hydriding of zirconium. the fraction of hydrogen released from the reaction that is locally absorbed by the cladding tube is called pickup fraction and in pwr conditions is found to be constant for particular zr-based alloys [1]. oxygen diffuses through the zirconium oxide layer and in an interface of metal and oxide causes additional oxidation. the density of the zro2 is smaller than zirconium alloy density. the difference in density and different thermal expansion of materilas is the primary cause of tension, internal stresses, and strains in cladding tubes. moreover, thermal conductivity λ of zro2 is much smaller than that of zirconium based alloys causing the zirconium dioxide layer to decrease the heat transfer from the fuel pellet over the cladding to the coolant and consequently increase maximal temperature in the fuel pellet. the exact physical parameters depend on temperature and models of thermal conductivity of zirconium dioxide. they are in details described in [2] and [3]. for example, the thermal conductivity of e110 alloy is about 18 w/mk at the temperature of 300 ◦c. the thermal conductivity of the zro2 for the same temperature is only about 2 w/mk. the bulk density of the zircaloy-4 alloy and zirconium dioxide at the same temperature is 6.5 and 5.6 kg/m3 respectively. when the zirconium dioxide layer thickness exceeds about 100 µm (zircaloy-4), it might crack and it is washed away by the streaming coolant which can lead to cold spots, additional oxidation, hydridation and later cladding breach [4]. oxidation takes place also on the internal surface of fuel cladding, where metal reacts with oxygen released from the fuel pellets where fission takes place. when a high burn-up is reached, a bonding layer consisting of zro2, uo2, and fission products appears. this layer might be the cause of a firm connection between the fuel cladding and pellets. 2. zirconium based alloys zirconium-based alloys has been used as the nuclear fuel cladding since 1950s [6]. there were originally two main groups of zr-based alloys developed: (1.) zirconium-tin and iron-based alloys (originally developed in the u.s.) (2.) zirconium-niobium based alloys (originally developed in former ussr) during the evolution of the nuclear fuel, fuel vendors and research organizations developed dozens of concepts of fuel cladding alloys. however, the two main groups remained as can be seen in figure 1. different cladding concepts can be based on the figure 13 http://dx.doi.org/10.14311/ap.2016.4.0013 http://ojs.cvut.cz/ojs/index.php/app miroslav cech, martin sevecek acta polytechnica ctu proceedings figure 1. nuclear fuel cladding alloys developed for usage in pwr reactors [5]. there were two main groups of cladding alloys developed: zr-sn (right branch) and zr-nb (left branch) based alloys with dozens other concepts depending on the alloying elements introduced around the world. divided into four development directions depending on their composition and development history. each alloy has a different corrosion characteristics depending on the alloying elements but also on manufacturing process and reactor type. 2.1. zirconium-tin alloys a well-known family of alloys called zircaloy was developed under a westinghouse-led program. an alloy first developed is called zircaloy-1. this alloy was replaced by the innovative zircaloy-2, which is still in use in the bwr reactors. after abandoning of the zircaloy-3 alloy development and utilization due to metallurgical processing issues, concerns with the high hydrogen pickup fraction exhibited by the zircaloy-2 alloy led to the development of the zircaloy4 alloy. nickel was substituted by iron in this alloy and it was used from the 1950s to 1990s. 2.2. zirconium-niobium alloys an alloy called e110 has been used by the russian nuclear industry for nuclear fuel cladding fabrication for vver reactors fuels. similar alloys made of zirconium-doped by niobium were used from the origin of the nuclear power utilization in the ussr. recently, westinghouse replaced zircaloy-4 alloy in most of their nuclear fuel for pwrs by the zirlo alloy. in bwr reactors, zircaloy-2 is still in use. zirlo is doped with niobium and is similar to the russian alloy called e635. french alloy called m5 is a zirconium-based alloy containing 1 % of niobium with oxygen. the m5 alloy is produced by the french company areva since 1990s. generally, alloys doped with niobium such as e110, m5, and zirlo have a higher corrosion resistance than alloys from the zircaloy family. summary of composition of currently widely employed alloys is presented in table 1 [7]. 3. corrosion models the growth and development of the cladding corrosion layer for each zirconium-based alloy is usually expressed by corrosion models. 3.1. garzarolli models models developed by garzarolli et al. [8] are adopted for describing the thickness of the corrosion layer of cladding tubes made of zircaloy-4 , m5, and zirlo alloys under pwr conditions. these models generally based on arrhenius law divide a growth of corrosion layer into two phases: (1.) the first phase continues until a transition thickness of oxide layer str is reached. the rate of corrosion layer growth is expressed by the cubic rate law – equation (2) (original units and the temperature of oxide-metal interface is used) [2, 3]. (2.) after reaching an alloy-specific transition thickness of oxide layer str, second phase quantified by a linear differential equation (3) taking into account also fast neutron flux φ is adopted. there are other transition points observed during the corrosion process. however, only the first transition is significant for the general progress of the corrosion kinetics. for modelling purposes the use of only one transition is satisfactory. model is defined for temperature range of 250–400 ◦c. ds3 dt = a s2 exp ( − q1 rt ) , (2) ds dt = (c0 + u(mφ)p ) exp ( − q2 rt ) , (3) where s . . . oxide layer thickness [µm], t . . . temperature [◦c], φ . . . neutron flux [neutrons/m2s], a = 6.3× 109 m3/day, r = 1.98 cal/molk, c0 = 8.04× 107 µm/day, m = 7.46× 10−15 cm2s/n, p = 0.24, u = 2.59× 108 µm/day. values of constants q1, q2 and transition thickness of oxide layer str are alloy-dependent and are summarized in table 2 for four widely used alloys which were subject to many studies. in literature, there were modifications of correlation models (2) and (3) defined. modified models differ by values of constants and consider other physical phenomena neglected in the presented models. these models are implemented for example in femaxi and frapcon fuel performance codes. 14 vol. 4/2016 modelling of cladding tubes corrosion alloying element zircaloy-4 zirlo m5 e-110 e-635 sn 1.2–1.7% 0.96–0.98% 1.25–1.30% fe 0.18–0.24% 0.094–0.105% < 500 ppm 0.30–0.35% cr 0.07–0.13% 79–83 ppm < 200 ppm nb 1.02–1.04% 0.8–1.2% 0.9–1.1% 1.0% ni 0.01% n < 65 ppm 22–30 ppm < 60 ppm 30–40 ppm c 150–400 ppm 60–80 ppm < 200 ppm <200 ppm o 900–1400 ppm 900–1200 ppm 0.11–0.17% < 1000 ppm 0.07% table 1. composition of zirconium-based alloys widely used around the world in pwrs as materials for cladding tubes fabrication [7]. q1[cal/mol] q2[cal/mol] str zircaloy-4 32289 27354 2µm m5 27446 29816 7 µm zirlo 32289 27080 2µm opt.zirlo 32289 27354 2 µm table 2. values of corrosion model’s constants used in corrosion models (2) and (3) as defined by [3]. figure 2. zirconium dioxide layer development from the point of reaching first transition thickness str corresponding to the transition time ttr. axis x represents time in days after the moment, when transition thickness was reached. the temperature of 320 ◦c and neutron flux of 1 × 1015 neutrons/m2s were chosen in this model situation. 3.2. three-phase model another model for describing of zircaloy-4 corrosion layer thickness in pwr conditions divides its evolution into three phases instead of two. the purpose is a faster oxide thickness growth after the second transition thickness is reached [7]. the model was developed by experimental data fitting and is more precise for higher values of oxide thickness than model developed by garzarolli et al. [8]. oxide layer growth during the first phase can be calculated by the following expression [6] ds3 dt = 2.187× 10−13 exp ( −135188 rt ) . (4) the first transition thickness is the same as in the previous model – 2 µm for zircaloy-4. afterward, different formula is used instead of equation (3) ds dt = ( 9.31× 10−4 + 2.75× 10−3 ( φ 5.24× 1018 )0.24 ) · exp ( − 114526 rt ) . (5) after reaching the second transition thickness – 35µm, following equation is used ds dt = ( 9.31× 10−4 + 2.75× 10−3 ( φ 5.24 · 1018 )0.24 ) · 1.8 exp ( − 114526 rt ) . (6) 3.3. e110 corrosion model a model describing the corrosion layer growth of e110 alloy in vver conditions was developed by fitting experimental data at the russian a.a. bochvar hightechnology scientific research institute for inorganic materials. for the e110 alloy following relation was derived [9] ds dt = 40 exp ( −5147 t ) . (7) model was derived byl data base on experiments, which took place in temperature range of 320–360 ◦c. this model considers only one phase of corrosion layer development, transition thickness is disregarded. comparison between corrosion layer growth of zircaloy-4 and e110 is plotted in figure 3. figure 3. comparison of the zirconium oxide layer thickness of zircaloy-4 and e110 alloys in conditions of 320 ◦c and neutron flux of 1e15 neutrons/m2s. the corrosion growth of e110 is considerably lower in comparison with the zircaloy-4 alloy. accelerating 15 miroslav cech, martin sevecek acta polytechnica ctu proceedings growth can be seen for the zircaloy-4 three-phase model which is not the case for the e110 alloy. for that reason, the neglecting of transitions in case of e110 is justified. if the behavior of nuclear fuel during loca, ria or other design basis accidents is calculated by fuel performance codes like fraptran or transuranus, the thickness of oxide layer is an initial condition which strongly influences a progress of the accident and its consequences. 4. corrosion in loca conditions large break loss of coolant accident (lbloca) is the maximal design basis accident of pwrs of second and third generation. during this accident, a temperature of the whole fuel rod including pellets quickly rises due to limited cooling conditions. the high temperature of fuel pellets leads to high-temperature gradients, stresses, and cracking of pellets. rapid release of fission gases from the fuel can be observed and the internal pressure of filling gas rises. the high temperature of cladding together with the high internal pressure can be a cause of a deformation, ballooning, or bursting of the cladding. this geometry changes can limit the coolant flow and further reduce the heat transfer from the fuel rods to the coolant. construction of reactor, design of the nuclear fuel and its properties must ensure that acceptance limits for loca accidents will not be violated: (1.) a peak cladding temperature can nowhere exceed 1204 ◦c (2.) sufficient fuel rod strength upon quench taking into account an additional mechanical load (maintain post-quench ductility) (3.) fraction of zirconium reacted into oxide cannot exceed 1 % (due to hydrogen production) (4.) melting temperature of fuel can not be reached in any place of the reactor core 4.1. corrosion models in loca conditions to develop corrosion models in loca conditions, it is necessary to measure experimental data in similar conditions. experiments are done at high-temperature steam (800–1200 ◦c). experiments with as-received cladding tubes and as well as with cladding tubes with corrosion layer has been performed. preoxidation of experimental samples ensures that simulation will be performed in conditions which are similar to the real loca accident conditions with operating fuel. a model of high-temperature corrosion of sponge based e110 alloy was developed at the ujp in the czech republic and is based on its experimental data [10]. experiments cover a wide range of conditions (temperature 600–1300 ◦c and 0–480 minute long exposition). these wide conditions enable to use the model in various conditions and for various scenario for e110 alloy. no. t [◦c] process 1 600–750 phases α + β transformation 2 750–950 formation of β phase 3 950–1100 delated transformation, tetragonal oxide 4 1100–1300 tetragonal oxide table 3. physical processes taking place in zirconium e110 alloy in different temperature intervals during loca accident conditions. this model describes a mass growth of oxide as defined in [10] ∆g = a exp ( e t ) tn = ktn, (8) where ∆g . . . mass growth [mg/dm2], a,e, k . . . fitting parameters, t . . . time [s], n . . . kinetic constant. figure 4. development of the parameter n with temperature as defined by [10]. figure 5. development of the parameter k with temperature as defined by [10]. for n and k parameters were derived following formulas n = 0.4 for t < 768.4 ◦c (9) n = 2.609− 4.898× 10−3(t − 273.15) + 2.633× 10−6(t − 273.15)2 for t < 960.3 ◦c (10) n = 1.202× 10−3(t − 273.15)− 0.8208 for t < 1098.9 ◦c (11) n = 0.5 for t > 1098.9 ◦c (12) 16 vol. 4/2016 modelling of cladding tubes corrosion figure 6. power history of rods bsm-25 and bk365. figure 7. oxide layer thickness of bsm-25 and bk365 rods. k = 85265.6 exp ( −9875.59 t ) for t < 934.1 ◦c (13) k = 1072.21 exp ( −4592.6 t ) for t < 1054.5 ◦c (14) k = 33.33 for t < 1098.0 ◦c (15) k = 96482.3 exp ( −10913.1 t ) for t > 1098.0 ◦c (16) temperature intervals of equations (9)–(16) approximately correspond to physical processes, which take place in the cladding material during loca accident. these processes are described in table 3. this model well describes a corrosion kinetic for all ranges of temperature covered by experiment. the value of parameter n is 1/2 for high-temperature corrosion and 1/3 for middle-temperature corrosion [7]. these values are the same as in other used models. another model for n also very well describes the n temperature reliance. constant k equals approximately equals to 0 and increase with temperature to about 90 at 1300 ◦c. dividing model into four ranges where different formulas are used brings a good agreement of the model with experimental data. a comparison between this model and data can be found in [10]. 5. model of corrosion in femaxi a calculation of oxide layer development in the femaxi-6 code has been performed for two fuel rods: bsm-25, and bk365. these rods were irradiated in the br-3 reactor and reached burn-up of 66 and 52mwd/kghm. rods were irradiated within the high burnup effect program in the br-3 reactor, cladding was made of zircaloy-4 alloy, coolant inlet temperature was 255 ◦c. a model originally developed by garzarolli et al. [8] (equations (2) and (3)) was used for the zircaloy-4 alloy corrosion modeling. the two power histories used as a model input are plotted in figure 6. corresponding oxide layer thickness growth is shown in figure 7. for both tested fuel rods, an average thickness and the maximal oxide layer thickness are shown. maximal thickness of the corrosion layer is about two times higher than the average value. maximal thickness was reached in the middle of the fuel rod which does 17 miroslav cech, martin sevecek acta polytechnica ctu proceedings not correspond to the case in commercial power reactors. the oxide layer growth is strongly dependent on the temperature, the higher the temperature is the faster the growth. therefore, the maximal thickness of the zirconium oxide layer in commercial power reactors is at the top of the fuel rod where the coolant temperature is highest. figure 7 shows, that higher linear heat rate causes faster oxide layer creation. the graph also shows that the first phase of oxide layer growth is independent of fast neutron flux. small differences are caused by higher temperature. in the later phase of fuel rod’s irradiation, there is a clear dependance of corrosion layer thickness on fast neutron flux and linear heat rate. when bsm-25 rod was operating in high heat rate condition, layer growth was much faster than in the case of smaller heat rate of the second fuel rod. higher heat rate (and corresponding temperature) causes the bigger corrosion layer, even when the burnup of the bsm-25 rod is lower. 6. conclusion this article describes models quantifying corrosion of nuclear fuel cladding tubes made of zirconium-based alloys widely used in nuclear industry in nominal conditions and loca accident conditions. models used for calculating of an oxide layer thickness in normal operation conditions for the widely used alloys zircaloy-4, zirlo, m5 and e110 are presented and compared. a model for corrosion and high-temperature oxidation in loca conditions is described and reliance of particular parameters used in models are shown in graphs. a corrosion model for nominal conditions was applied in the femaxi-6 code to calculate corrosion of fuel rods bk363 and bsm-25 tested in the br-3 reactor. the relations of burnup, linear heat rate, and corrosion layer thickness growth is illustrated in the example. results show faster oxide growth in case of bsm-25 rod after reaching the transition thickness for zircaloy-4 alloy, because this rod was operated at higher linear heat rate. acknowledgements this work was supported by the grant agency of the czech technical university in prague, grant no. sgs ohk4-008/16. references [1] k. geelhood, w. luscher. frapcon-3.5: integral assessment. progress in nuclear energy 2014. [2] m. suzuki, h. saitou, n. g. k. k. kikō. light water reactor fuel analysis code: femaxi-6 (ver. 1): detailed structure and user’s manual. japan atomic energy research institute, 1997. [3] w. g. luscher, k. j. geelhood, et al. material property correlations: comparisons between frapcon-3.4, fraptran 1.4, and matpro. us nuclear regulatory commission, office of nuclear regulatory research, 2011. [4] p. billot, b. cox, k. ishigure, et al. corrosion of zirconium alloys in nuclear power plants. in tecdoc684. international atomic energy agency (iaea), 1993. [5] l. hallstadius, s. johnson, e. lahoda. cladding for high performance fuel. progress in nuclear energy 57:71–76, 2012. [6] a. t. motta, a. couet, r. j. comstock. corrosion of zirconium alloys used for nuclear fuel cladding. annual review of materials research 45:311–343, 2015. [7] d. kobylka. termofyzikální vlastnosti pokrytí nových typů paliva, jejich implementace v kódu femaxi-6 a testování. tech. rep. 14117/2012/02kob, újv řež, a.s., 2012. [8] f. garzarolli, d. jorde, r. manzel, et al. review of pwr fuel rod waterside corrosion behavior. tech. rep., kraftwerk union ag, erlangen (germany, fr); combustion engineering, inc., windsor, ct (usa), 1980. [9] v. konkov, m. sablin, t. khokhunova, et al. assessment of e110 and e635 alloy corrosion behavior in vver-1200 reactors. jsc vniinm 2009. [10] j. krejčí. oxidace palivového pokrytí během havárie loca. bezpečnost jaderné energie 45:311–343, 2015. 18 acta polytechnica ctu proceedings 4:13–18, 2016 1 introduction 2 zirconium based alloys 2.1 zirconium-tin alloys 2.2 zirconium-niobium alloys 3 corrosion models 3.1 garzarolli models 3.2 three-phase model 3.3 e110 corrosion model 4 corrosion in loca conditions 4.1 corrosion models in loca conditions 5 model of corrosion in femaxi 6 conclusion acknowledgements references 96 acta polytechnica ctu proceedings 1(1): 96–102, 2014 96 doi: 10.14311/app.2014.01.0096 star formation in tadpole galaxies casiana muñoz-tuñón1,2, jorge sánchez almeida1,2, debra m. elmegreen3, bruce g. elmegreen4 1instituto de astrof́ısica de canarias, e-38205 la laguna, tenerife, spain 2departamento de astrof́ısica, universidad de la laguna, tenerife, spain 3department of physics and astronomy, vassar college, poughkeepsie, ny 12604, usa 4ibm research division, t.j. watson research center, yorktown heights, ny 10598, usa corresponding author: cmt@iac.es abstract tadpole galaxies look like a star forming head with a tail structure to the side. they are also named cometaries. in a series of recent works we have discovered a number of issues that lead us to consider them extremely interesting targets. first, from images, they are disks with a lopsided starburst. this result is firmly established with long slit spectroscopy in a nearby representative sample. they rotate with the head following the rotation pattern but displaced from the rotation center. moreover, in a search for extremely metal poor (xmp) galaxies, we identified tadpoles as the dominant shapes in the sample – nearly 80% of the local xmp galaxies have a tadpole morphology. in addition, the spatially resolved analysis of the metallicity shows the remarkable result that there is a metallicity drop right at the position of the head. this is contrary to what intuition would say and difficult to explain if star formation has happened from gas processed in the disk. the result could however be understood if the star formation is driven by pristine gas falling into the galaxy disk. if confirmed, we could be unveiling, for the first time, cool flows in action in our nearby world. the tadpole class is relatively frequent at high redshift – 10% of resolvable galaxies in the hubble udf but less than 1% in the local universe. they are systems that could track cool flows and test models of galaxy formation. keywords: starburst galaxies tadpoles cool flows rotation curves galaxy disks. 1 introduction elongated galaxies with bright clumps at one end are visible in deep field images taken with hst or from the ground; van der bergh et al., 1996 called them “tadpole” galaxies”. figure 1 in elmegreen et al. (2005) shows different morphologies of galaxies observed with the hubble ultra deep field (udf). the fourth row presents images of tadpoles. this asymmetric morphology is rather common at high redshift but rare in the local universe. for example, tadpoles constitute 10% of all galaxies larger than 10 pixels in the udf (elmegreen et al. 2007; elmegreen & elmegreen, 2010), and they represent 6% of the udf galaxies identified by straughn et al. (2006) and windshorst et al. (2006) using automated search algorithms. in contrast, elmegreen et al. (2012; hereafter paper i), find only 0.2% tadpoles among the uv-bright local galaxies of the kiso survey by miyauchi-isobe et al. (2010). this decrease suggests that the tadpole morphology represents a common but transition phase during the assembly of some galaxies. since local tadpole galaxies are very low mass objects compared to their high redshift analogues, this phase must be already over for the local descendants of high redshift tadpoles. the tadpole structure has inspired several explanations, such as ram pressure stripping that triggers star formation at the leading edge, to mergers (see sánchez almeida et al. 2013 for an extensive review). the explanation that we propose, based on observational evidence summarized here, is that the starburst head may result from the accretion of an external flow of pristine gas that penetrates the dark matter halo and hits and heats a pre-existing disk, which is viewed to the side as the tail. we will briefly present a summary of recent results showing, first that the local tadpoles share the properties of their higher redshift and higher mass counterparts (section 2), that they belong to the extremely metal poor (xmp) sample of the blue compact dwarfs family (section 3), they are rotating discs (section 4) and, finally, that the starbursts (heads) show a drop in the already low metallicity that can only be understood if fresh metal-poor gas is falling onto the galaxy (section 96 http://dx.doi.org/10.14311/app.2014.01.0096 star formation in tadpole galaxies 5). we finish with a brief summary and future actions. 2 local and hight z tpg share properties we used sloan digital sky survey data to determine the ages, masses, and surface densities of the heads and tails in 14 local tadpoles (shown in figure 1) selected from the kiso and michigan surveys of uv-bright galaxies, and we compared them to tadpoles previously studied in the hubble ultra deep field. the result, published in paper i is that the young stellar mass in the head scales linearly with the rest-frame galaxy luminosity, ranging from ≈ 105 m� at galaxy absolute magnitude u = −13 mag to 109 m� at u = −20 mag. the tails in the local sample look like bulge-free galaxy disks. their photometric ages decrease from several gyr to several hundred myr with increasing redshift. the far-outer intensity profiles in the local sample are symmetric and exponential. we suggest that most local tadpoles are bulge-free galaxy disks with lopsided star formation, perhaps from environmental effects such as ram pressure or disk impacts, or from in-situ gas collapse to a giant star-forming clump with a jeans-length that is comparable to half the disk size. the existence of a disk, proposed from the analysis of the luminosity profiles, has been further confirmed spectroscopically (see section 4). figure 1: tadpole galaxies from the kiso and um samples. figure from elmegreen et al., 2012. 3 belong to the bcdsxmp class blue compact galaxies are important targets for a number of reasons. they are small systems, thought to remain as fossils or debris from the formation of larger galaxies in the early epochs of the universe. their low metallicities, high ssfrs and low doubling time (less than 1gy) and active stabursts make them ideal targets to study the old universe at low redshift. their complete census, as well as the likelihood that they have a long quiescent phase between starbursts, took us to study the whole sample by making use of sdss. the properties of the quiescent and burst phases were determined from detailed studies of the bursts and host galaxies of a nearby sample (amorin et. al., 2007, 2008). these properties allowed us to identify such objects in the database. the sdss dr6 database provides ≈ 21.500 quiescent bcd candidates, a number 30 times larger to those bursting (bcds). this result implies that one out of every three dwarf galaxies in the local universe may be a quiescent bcd. the properties of the two samples are consistent with a single sequence in galactic evolution with the quiescent phase lasting 30 times longer than the burst phase (sánchez almeida et. al., 2008). in sánchez almeida et al. (their figure 9) there is a clear subsample of objects with the lowest luminosity which turn out to be also those that are most metal poor. we carried out a systematic search for extremely metal-poor (xmp) galaxies in the spectroscopic sample of sloan digital sky survey (sdss) data release 7 (dr7) (morales-luis et al., 2011). the xmp candidates are found by classifying all of the galaxies according to the form of their spectra in a region 80 å wide around hα using an automatic classification algorithm, k-means (sánchez almeida et al.,2009). our systematic search renders 32 galaxies having negligible [n ii] lines, as expected in xmp galaxy spectra. twenty-one of them were previously identified as xmp galaxies in the literature, and 11 were new. this was established after a thorough bibliographic search that yielded only some 130 galaxies known to have an oxygen metallicity 10 times smaller than the sun (explicitly, with 12 + log [o/h] ≤ 7.65). xmp galaxies are rare; they represent 0.01% of the emission lines galaxies in sdss/dr7. the xmp galaxies constitute 0.1% of the galaxies in the local volume, or ≈ 0.2% of the emission-line galaxies. all but four of our candidates are bcd galaxies, and 24 of them have either cometary shape or are formed by chained knots. note that this result, the morphology, is absolutely independent of our search criterium (spectra). 4 tadpoles are rotating disks the work in paper i was followed up by mean of high spectral resolution long slit observations at the int (2.5m) at observatorio del roque de los muchachos (orm) with ids spectrograph. in order to determine the dynamical properties and metallicities of lo97 casiana muñoz-tuñón et al. figure 2: sdss mugshots of all xmp candidates (from spectroscopy). the figure is taken from morales-luis et al., 2011. note the prevalence of tadpole shapes. cal tadpoles, we measured hα spectra along the headtail direction in a representative fraction of the original sample. further details are in sánchez almeida et al. (2013). in figure 3, we show spectral flux (the solid lines) and hα flux (the dashed lines) along the slit. note the obvious lopsidedness of the light distributions, as expected from the tadpole shape. the origin of distance on the abscissa has been set as the position of the maximum of the spectral flux distribution. the dotted line represents a gaussian fitted to the hα flux around the head. the horizontal bar in each panel gives a common length scale corresponding to 1 kpc. the thin vertical solid lines indicate the center of rotation obtained from the rotation curve fit shown in fig. 4. velocities, masses, abundances and other physical parameters were determined from the spectra. bulk velocities were measured from the displacement of hα. we computed the displacement both as the barycenter of the emission line, and as the center of a gaussian function fitted to the profile. errors were estimated from the s/n measured in the continuum and then propagated to the centroids. the fwhm of the profiles were also measured directly from the profiles and from the gaussian fits. their errors were also inferred from the noise measured in the continuum by error propagation. figure 4 shows the velocity curves of the tadpole galaxies included in the study. the abscissae represent distances along the major axes of the galaxies from the position of the tadpole head; i.e., the brightest point on the galaxy. the range of distances differs for the different targets, but the horizontal bar in each panel gives a common length scale corresponding to 1 kpc. the points with error bars show the observations whereas the thick solid line represents the best fit of the observed points to the analytic rotation curve. the part of the rotation curve shown in red indicates the portion of the velocity curve used for fitting. the thin horizon98 star formation in tadpole galaxies tal and vertical lines indicate the systemic velocity and the center of rotation obtained from the fit, respectively. the little arrows on top of each panel also indicate the centers of rotation. the zero of the velocity scale is set by velocity of the spatially integrated spectrum of the galaxy; positive velocities are redshifts. figure 3: spectral flux (the solid lines) and hα flux (the dashed lines). formal error bars for photometry are not included since they are negligibly small. the main result shown in figure 4 is that five out of seven targets show velocity gradients interpreted as rotation. another important result is that the tadpole head is not at the rotation center. figure 4: velocity curves of the seven tadpole galaxies obtained from long slit spectroscopy. figure from sánchez almeida et al. 2013 sometimes the interpretation of the velocity curve as rotation is obvious (e.g., kiso8466), but other times the curve looks more like a perturbed rotation (e.g., kiso5639). kiso3193 and kiso3867 have a rather flat velocity curve, and therefore no obvious rotation. however, one of them, kiso3867, shows a systematic line shift of the order 10–20 km s−1 between the two extremes of the galaxy (figure 4). the amplitude is of the order of the error bars, but the displacement is in the raw data as judged by inspection of the individual hα profiles. 5 drops in metallicity at the head location the metallicity along the slit was estimated using the ratio [nii]λ6583 to hα. figure 5 taken from sánchez almeida et al (2013) shows the variation across the galaxies of the oxygen abundance, including their error bars. all galaxies have sub-solar metallicity the thick horizontal line marks the solar oxygen abundance given by 12 + log(o/h)� = 8.69± 0.05 (asplund et al., 2009). the galaxies also present significant abundance gradients, with the lowest abundances tending to coincide with the largest hα emissions (e.g., kiso6669 and kiso6877) in fig. 5. remember that the vertical dotted lines mark the position of the peak hα fluxes. two targets, kiso5639 and kiso6877, have metallicities well below one-tenth the solar value, therefore, they belong to the xmp galaxies class (kunth & östlin, 2000). xmp galaxies are really rare objects: one out of a thousand galaxies in the local universe according to morales-luis et al. (2011). therefore the fact that we observe two in a sample of seven cannot be a coincidence. it is known that a significant fraction of xmp galaxies turn out to be cometary or tadpole (papaderos et al., 2008). we have found that the reverse holds too, i.e., that tadpole galaxies have a significant probability of being xmp. this fact supports the idea that the tadpole morphology is a sign of dynamical youth, as the low metallicity is a sign of being chemically young (see discussion in sánchez almeida et al., 2013). 6 summary and future tadpole galaxies have an easily identified shape, belong to the blue compact dwarf class, and are rare in the nearby universe. their appearance suggests then to be the consequence of some interaction or star formation triggered by ram pressure processes. these local tadpoles seem though to form a continuous sequence with the udf tadpoles, seen in relatively larger number at high redshift (elmegreen & elmegreen 2010). regarding their photometric properties, local tadpoles occupy the low mass end in sequences such as star formation, surface density and mass-to-light ratio. in addition, the radial intensity profiles of both samples (local and high redshift tadpoles) show an exponential decrease at large galactocentric distances, which we interpreted as an evidence for the existence of an underlying disk. from the point of view of their chemical content, extremely metal poor (xmp) galaxies are the least evolved objects in the local universe (pagel et al., 1992; 99 casiana muñoz-tuñón et al. figure 5: oxygen abundance variation across the galaxies. the vertical solid line represents the center of rotation, whereas the vertical dotted line indicates the location of the maximum in the hα flux profile. the thick horizontal solid line indicates the solar metallicity. note the existence of abundance variations, with the minima coinciding with the largest hα signals. note also that kiso5639 and kiso6877 reach very low abundances, below one-tenth of the solar value; therefore, they are members of the set of rare xmp galaxies. kunth & östlin, 2000). they represent only 0.1 % of the galaxies in an arbitrary nearby volume (moralesluis et al., 2011) and a significant fraction of these chemically primitive objects turn out to have tadpole or cometary shape (brinchmann et al. 2008). this association between low metallicity and tadpole shape suggests that both are attributes of very young systems. detailed studies of a significative sample of the local tadpole class by means of high-resolution long-slit spectroscopy put into evidence two important facts: they do rotate and they show oxygen abundances that vary along the disk. a high percentage of them are xmp galaxies and the metallicity is minimum were starformation is maximum. moreover, the rotation center does not coincide with the current starburst location (the head). the oxygen metallicity estimated from [nii]6583/hα often shows significant spatial gradients across the galaxies (∼0.5 dex), being lowest at the head and increasing in the rest of the galaxy, tail included. a similar result with the highest sfr been the lowest metallicity region has also been found in low metallicity grb host galaxies (levesque et al., 2011). the sense of the resulting metallicity gradient differs from the observation of local disk galaxies, where the gas-phase metallicity increases toward the galaxy centers (vilchez et al., 1988) or is just constant (genel et al., 2008). however, the type of variation we measure, with a minimum metallicity at the most intense star-forming region, has been observed in galaxies at redshift around 3 by cresci et al. (2010), where it is interpreted as evidence for infall of pristine gas triggering star formation. as a result of all the evidence found, we propose that local tadpole galaxies are disks still in the process of being formed in our present-day universe. moreover 100 star formation in tadpole galaxies their otherwise very low star formation is enhanced and triggered by cool-flow accretion of pristine metal-poor gas. this triggering causes an extremely metal-poor head to shows up on the side of an immature (still forming) rotating disk. there are a number of parallel actions now being undertaken to go further. we have just finished a study of the hi content of a complete sample of xmp galaxies (fihlo et al., 2013) and compared the properties of the clumps of different galaxy types at different redshifts (elmegreen et al., 2013). the recent analysis of a new sample corroborates the metallicity drop in the xmp galaxies using the so call direct method (sánchez almeida et al. 2014). cosmological simulations predict cold-flow buildup to be the main mode of galaxy formation (dekel et al., 2009). the incoming gas is expected to form giant clumps that spiral in and merge into a central spheroid. to confirm such a scenario at high redshift is neither easy nor feasible and we think we have discovered nearby cases that may allow for comparisons. we are making a comprehensive study of the disks and bursts of other bcds with xmp properties to search for extremely metal poor clumps in 2d spectroscopy. the final aim is to characterize the local xmp galaxy sample within the cool flow paradigm. acknowledgement this work has been partly funded by the spanish ministry for science, project aya 2010-21887-c04-04. results based on observations at the observatorio del roque de los muchachos (orm), operated by the iac at la palma. thanks to franco giovannelli and lola sabau-graziatti, organizers of this workshop for their kindness and dedication. thanks to the referee for useful comments. references [1] van den bergh, s., abraham, r.g., ellis, r.s., tanvir, n.r., santiago, b.x., & glazebrook, k.g. 1996, aj 112, 359 [2] emegreen, d.m., elmegreen, b.g., rubin, d.s. & schaffer, m.a. 2005, apj, 631, 85 doi:10.1086/432502 [3] elmegreen, d. m., elmegreen, b. g., ravindranath, s., & coe, d. a. 2007: apj, 658, 763 doi:10.1086/511667 [4] elmegreen, b. g. & elmegreen, d. m. 2010: apj, 722, 1895 doi:10.1088/0004-637x/722/2/1895 [5] straughn, a. n., cohen, s. h., ryan, r. e., et al. 2006, apj, 639, 724 doi:10.1086/499576 [6] windhorst, r. a., cohen, s. h., straughn, a. n., et al. 2000, newar, 50, 821. 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[26] sánchez almeida, j., morales-luis, a.b, muñoztuñón, c., et al., 2014: apj in press. 102 http://dx.doi.org/10.1038/nature07648 introduction local and hight z tpg share properties belong to the bcdsxmp class tadpoles are rotating disks drops in metallicity at the head location summary and future acta polytechnica ctu proceedings doi:10.14311/app.2017.8.0011 acta polytechnica ctu proceedings 8:11–13, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app dlc/ti thin films properties prepared by hybrid laser technologies jan mikšovskýa,b,∗, miroslav jelíneka,b, petr písaříka,b, tomáš kocoureka,b, jan remsaa,c, karel jurekb a czech technical university in prague, faculty of biomedical engineering, nam. sitna 3105, kladno, czech republic b institute of physics ascr, na slovance 2, prague, czech republic c czech technical university in prague, faculty of nuclear sciences and physical engineering, břehová 7, prague, czech republic ∗ corresponding author: jan.miksovsky@fbmi.cvut.cz abstract. layers of diamond-like carbon are usable in many fields of industry as well as in medicine. many scientific groups have worked with different types of deposition techniques to prepare dlc layers with improved or unique properties. the dlc properties could be improved by various dopations. in this study, we focused on dlc layers doped by titanium, prepared by hybrid laser depositions. two techniques were used: dual pulse laser deposition (dualpld) and pulse laser deposition in combination with magnetron sputtering (pld/ms). preliminary tests for morphology, wettability, adhesion, hardness, corrosion, friction and wearability were examined. dlc samples were prepared on si(100) wafer and on ti6al4v alloy substrates with titanium concentration from pure up to 25 at.%. friction of the prepared layers ranged from 0.09 to 0.18. the films exhibited very low wear for loads 1 n and 2 n. the tested pin wear grew with decreasing titanium dopation. the measurements of the contact angle and determination of surface free energy were done for water, diiodomethane and ethylene glycol. hardness and young's modulus decreased with higher titanium dopation, on the other hand adhesion improved with increasing amount of titanium in film. keywords: pld, dlc, titanium, surface properties, laser deposition, magnetron sputtering. 1. introduction in this study, we focused on the changes in the mechanical and corrosion behavior with various amount of titanium in dlc/ti thin films. two techniques for dopation of titanium were used [1–3]. the first technique was based on pulsed laser deposition (excimer laser, krf, λ = 248 nm) combined with dc magnetron sputtering. the second technique was dualpld. laser fluency was 8 j/cm2 for dlc deposition and 5 j/cm2 for metal dopant. power of magnetron was from 40 w to 300 w for metal dopant. we studied behavior of layers for ti concentration from 1 at.% to 25 at.%. si(100) and ti6al4v alloy were used as substrates. prepared films were characterized with focus on their basic physical properties, such as crystallinity by xrd, morphology by afm and mechanical profilometry, chemical bonding nature by wdx, surface free energy by contact angle. hardness and young’s modulus were studied by nanoindentation. macro adhesion was studied up to 30 n. wearability and tribological properties were studied as well. the content of sp3 bonding was studied by xps. special focus was given on tribological properties. corrosion rates were measured as function of ti concentration. 2. experimental wearability test was performed by tribometer (anton paar) with linear movement. chromium steel testing ball with 6 mm diameter was used. speed of the testing ball was 5 cm/s, total testing length 10 m, used loads during tests were 1 n and 2 n. the tests were performed as dry. the friction was determined from the test records. nanoindentation tests were performed on all samples for determination of hardness and elastic modulus. all measurements were implemented on layers with thickness 500 nm and the indentation depth was less than 10 % of the layers thickness. for more details, see [4]. adhesion of the films was tested for samples on ti6al4v substrates. we tested samples by progressive load from 1 n to 30 n. three types of critical forces were evaluated. at least two scratches for each layer were tested. for more details, see [4]. wettability was measured by three liquids: distilled water, diiodomethane and ethylene glycol, by contact angle measurement system (dsa100, krüss company). surface free energy was determined by drop shape analysis software with fowkes method. the volume of droplets was (0.4 ± 0.1) ml. the measurement technique was sessile droplet and static contact angle. each sample was tested at least on three 11 http://dx.doi.org/10.14311/app.2017.8.0011 http://ojs.cvut.cz/ojs/index.php/app j. mikšovský, m. jelínek, p. písařík et al. acta polytechnica ctu proceedings figure 1. from left wearability of the ti6al4v substrate and samples ti:dlc7(pure dlc), ti:dlc10 (5 at.% ti) and ti:dlc12(25 at.% ti). the figures are captured at magnification 200x. figure 2. wearability of the testing ball after tests for ti6al4v substrate and for samples ti:dlc7(pure dlc), ti:dlc10 (5 at.% ti) and ti:dlc12(25 at.% ti). the figures are captured at magnification 200x. dual pld 0 at.% ti 1 at.% ti 3 at.% ti 5 at.% ti 10 at.% ti 25 at.% ti 0.12 0.14 0.13 0.12 0.11 0.09 pld/ms 0 at.% ti 1 at.% ti 3 at.% ti 5 at.% ti 10 at.% ti 25 at.% ti 0.13 0.15 0.14 0.18 0.15 0.16 table 1. friction on the layers of ti:dlc prepared by dualpld and pld/ms methods. different places. for each liquid, a new sample was used. from each droplet, series of 15 pictures were evaluated. laplace profile fitting was used. tested samples were on si (100) and thickness of the films was around 100 nm. we finished preliminary tests of the corrosion behavior as function of the amount of the titanium dopant in the dlc layers. we used potentiodynamic measurement and tafel plots for icorr determination and then for corrosion rate determination. 3. results contents of the titanium dopant in the dlc layers were determined by wdx and confirmed by xps. prepared samples concentrations were 0, 1, 3, 5, 10 and 25 at.% of titanium. dualpld technique was better to reach the desired dopants concentration. the xrd tests confirmed that all the samples were amorphous with detection of ti and tic phases for the highest ti concentration (10 and 25 at.% ti). thickness of the prepared layers were approximately 500 nm, for layers on ti6al4v substrates and 100 nm for layers on si (100). afm was used for morphology determination. both methods produced smooth layers around 1 nm, just for dualpld method roughness increased for 10 and 25 at.% ti up to 5 resp. 15 nm. wearability tests have been done for loads 1 n and 2 n. for these loads, there were no damage observed on samples. the wearability of the ball decreased with increased amount of titanium in layers. examples are on the figures 1 and 2. from comparison of the coated and uncoated materials, the uncoated materials were seriously damaged. the friction for pure dlc layers was 0.125 ± 0.05. for dual pld method we observed slight increase in friction for lower concentration up to 0.14 and then decrease to 0.09. for pld/ms method we observed slight increase for dopated layers but without clear trend, for more detail see table 1. the hardness for pure dlc layers starts at (31 ± 1) gpa and was decreasing with increasing of the titanium content to 12 ± 2 gpa for 25 at.% of titanium. the decrease was slightly quicker for pld/ms technique. the same behavior we observed for elastic modulus with the highest values around 250 gpa for pure dlc and decrease to 150 gpa for 25 at.% ti content of titanium practically same for both methods. the adhesion values seemed to increase with content of the titanium with exception for highest concentration of titanium for pld/ms method. critical force fc3 started at 5.6 n for pure dlc and increased to 18.4 n for dualpld technique for 25 at.% ti. for pld/ms technique critical force was increasing up to 20.2 n for 10 at.% ti but for 25 at.% ti it reduced to 9.2 n. this could be connected with lower hardness of titanium. the contact angle for water was in range from 57.7° to 71.5° for dual pld method and from 53.8° to 70.0° for pld/ms method. ca for ethylene glycol was in range from 34.5° to 42.8° resp. from 30.1° to 44.0° and for diiodomethane the range was from 12 vol. 8/2017 dlc/ti thin films properties prepared by hybrid laser technologies 34.9° to 38.3° resp. 32.0° to 36.4° for dual pld resp. pld/ms method. the results showed no trends in ca in correlation with titanium content in layers. from the free surface energy calculation we can conclude that all the tested layers are dominantly disperse. from the corrosion tests, the high concentration of the titanium dopants seemed to improve corrosion resistivity against the pure dlc. for various concentrations there were no clear trends observed and further tests should be performed before any conclusions could be made. 4. conclusion we prepared diamond-like carbon samples doped by titanium in concentration up to 25 at.% by two deposition techniques dual pld and pld/ms. we made standard testing as xrd, wdx, xps, afm, profilometry measurements etc. the main focus was put on mechanical and tribology testing. for both techniques, the hardness and elastic modulus were decreasing with higher content of the titanium, as we expected. there were no significant changes based on used methods. we observed better adhesion related to increasing titanium concentration in films. this is connected with lower compression stress due dopation. on the other hand, for the highest concentration for pld/ms there was lower adhesion observed, which could be connected with lower hardness. wearability test showed no damage to the coatings at load 1 n or 2 n (no matter on ti concentration) but wear of the testing ball was significantly higher for lower ti concentration in films. this is probably connected to higher layer hardness. tests will be continued with higher loads. for corrosion behavior, only preliminary tests are available. corrosion resistance was better for higher titanium amounts, when the highest concentration had up to three times better icorr parameter. for wettability, there are no clear trends based on titanium content. all layers are dominantly disperse. acknowledgements this work was supported by the grant agency of the czech technical university in prague, sgs16/110/ohk4/1t/17, sgs16/190/ohk4/2t/17, by meys cr grant lo1409 and by czech grant agency ga15-05864s. references [1] j. bulíř, m. novotný, m. jelínek, et al. plasma study and deposition of dlc/tic/ti multilayer structures using technique combining pulsed laser deposition and magnetron sputtering. surface and coatings technology 200(1 4):708 – 711, 2005. 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[2] q. wei, r. narayan, j. narayan, et al. improvement of wear resistance of pulsed laser deposited diamond-like carbon films through incorporation of metals. materials science and engineering: b 53(3):262 – 266, 1998. doi:http://dx.doi.org/10.1016/s0921-5107(98)00150-0. [3] a. voevodin, m. capano, s. laube, et al. design of a ti/tic/dlc functionally gradient coating based on studies of structural transitions in ti-c thin films. thin solid films 298(1 2):107 – 115, 1997. doi:http://dx.doi.org/10.1016/s0040-6090(96)09145-6. [4] m. jelínek, j. zemek, t. kocourek, et al. dual laser deposition of ti:dlc composite for implants. laser physics 26(10):105605, 2016. 13 http://dx.doi.org/http://dx.doi.org/10.1016/j.surfcoat.2005.01.087 http://dx.doi.org/http://dx.doi.org/10.1016/s0921-5107(98)00150-0 http://dx.doi.org/http://dx.doi.org/10.1016/s0040-6090(96)09145-6 acta polytechnica ctu proceedings 8:11–13, 2017 1 introduction 2 experimental 3 results 4 conclusion acknowledgements references 157 acta polytechnica ctu proceedings 1(1): 157–162, 2014 157 doi: 10.14311/app.2014.01.0157 agile highlights after six years in orbit carlotta pittori1,2 on behalf of the agile collaboration 1asi science data center (asdc), via del politecnico snc, 00133 roma, italy. 2inaf-oar, via frascati 33, i00040 monte porzio catone (rm), italy. corresponding author: carlotta.pittori@asdc.asi.it abstract agile is an asi space mission in collaboration with inaf, infn and cifs, dedicated to the observation of the gammaray universe in the 30 mev – 50 gev energy range, with simultaneous x-ray imaging capability in the 18–60 kev band. the agile satellite was launched on april 23rd, 2007, and produced several important scientific results, among which the unexpected discovery of strong flares from the crab nebula. this discovery won to the agile pi and the agile team the bruno rossi prize for 2012 by the high energy astrophysics division of the american astronomical society. thanks to its sky monitoring capability and fast ground segment alert system, agile detected many galactic and extragalactic sources: among other results agile discovered gamma-ray emission from the microquasar cygnus x-3, detected many bright blazars, discovered several new gamma-ray pulsars, and discovered emission up to 100 mev from terrestrial gamma-ray flashes. we present an overview of the main agile data center activities and the agile scientific highlights after 6 years of operations. keywords: gamma-rays: observations catalogs. 1 introduction agile (astro-rivelatore gamma a immagini leggero) (tavani et al., 2009a) is a gamma-ray astrophysics mission of the italian space agency (asi), with inaf, infn and cifs participation which has been in orbit since 23 april 2007. the agile payload is composed of a pairproduction gamma ray imager (grid) sensitive in the energy range 30 mev-50 gev (barbiellini et al., 2001; prest et al., 2003), an x-ray imager (superagile) sensitive in the energy range 18-60 kev (feroci et al., 2007), and a mini-calorimeter (mcal) sensitive to gamma-rays and charged particles with energies between 300 kev and 100 mev (labanti et al., 2009). the instrument, weighting only ∼ 100 kg, is the most compact ever operational for high-energy astrophysics (approximately a cube of about 60 cm size) with excellent detection and imaging capability. agile is characterized by a very large field of view (∼ 3 sr), a good angular resolution, 0.1 0.2 degrees in gamma rays and 1-2 arcminutes in x rays, and a small dead time (100 µs), which make it a very good instrument to study persistent and transient gamma-ray sources even on very short timescales. recent calibration results of the agile-grid using in-flight data and monte carlo simulations producing instrument response functions have been presented in chen et al. (2013). 2 the ground segment and the agile data center the agile data center (adc) is part of the asi science data center (asdc), previously located in the esa establishment of esrin in frascati, and recently moved within the asi headquarters, rome (italy). satellite data are routinely collected every ∼ 96 minutes by the asi ground station in malindi (kenya), then quickly sent to the satellite operations centre in telespazio, fucino, and then transferred, preprocessed, analyzed, and stored at the adc. adc is in charge of all the scientific oriented activities related to the analysis, archiving and distribution of agile data. from july 2007 july to october 2009 (∼ 2.5 years) agile was operated in “pointing observing mode”, characterized by long observations called observation blocks (obs), typically of 2-4 weeks duration, following a predefined baseline pointing plan, mostly concentrated along the galactic plane. on november 4, 2009, agile scientific operations were reconfigured following a malfunction of the rotation wheel occurred in mid october, 2009. the satellite is currently operating regularly in “spinning observing mode”, surveying a large fraction (about 70%) of the sky each day. since december 21, 2012 due to asi’s malindi ground station technical problems, the acquisition of telemetry data from the agile satellite has been reduced. 157 http://dx.doi.org/10.14311/app.2014.01.0157 carlotta pittori figure 1: whole sky agile intensity map (ph cm−2 s−1 sr−1) in galactic coordinates and aitoff projection, for energies e > 100 mev, accumulated during the first ∼ 6 years of observations up to december, 2012 (pointing + spinning observing modes). malindi downlink efficiency for agile-grid data is currently at a daily level of about 80%. all agile payload functions are nominal, and the daily grid skymonitoring activities are fully operational, despite the telemetry gaps in the archive due to intermittent data acquisition at the ground station. the agile quicklook (ql) alert system is composed of two independent automated analysis parts: the ql scientific pipeline running at adc (pittori et al., 2013) and the agile-grid science alert system (sas) pipeline running at the inaf-iasf bologna (bulgarelli et al., 2013). data are automatically analyzed at every downlink and accumulated on different timescales. lightcurves of potential gamma-ray sources are produced using blind search techniques and crosscorrelation with a reference list of known gamma-ray emitters. as proper flux thresholds are exceeded, alerts for transient gamma-ray sources are automatically generated and notified through e-mails, sms messages, and also through a dedicated application for smartphones and tablets. these alerts are crosschecked, and a manual analysis is performed for the most interesting candidate gamma-ray sources. the daily monitoring activity of the agile ql alerts resulted in the publication of 104 atel and 40 gcn up to may, 2013, among which we mention the first detection of gamma-ray emission from microquasars above 100 mev, from cygnus x-3 and cygnus x-1 in the cygnus region, the prompt alert of many gamma-ray flares from blazars and galactic transients, and the surprising discovery of gamma-ray flares from the crab nebula. the 2012 bruno rossi international prize has been awarded to the pi, marco tavani, and the agile team for this important and unexpected discovery. 3 new agile catalogs and asdc interactive web tools the agile first catalog of high-confidence γ-ray sources detected by agile during its first year of operations (pittori et al., 2009) was recently updated using data covering the whole period of pointed observations, ∼ 2.3 years, in verrecchia et al. (2103) (“an updated list of agile bright gamma-ray sources and their variability in pointing mode”). refined analysis of complex regions of the galactic plane with improved event filter and calibrations yielded a new reference list, and a multi-source maximum likelihood analysis was performed over the timescale of the agile pointed observation blocks (ob) resulting in an updated list of 54 sources. eight 1agl sources, with significance above 4σ from the analysis over the entire observing period, were not detectable on the ob timescale either due to low ob exposures and/or to their positions within complex galactic regions. the new agile-grid variability catalog (verrecchia et al., 2103) is also available from the adc webpages as an interactive web table1. in the on-line version, light curves from fluxes in each ob are accessible within the asdc data explorer, 1http://www.asdc.asi.it/agile1rcat/ 158 agile highlights after six years in orbit in the agile-grid data products tab. the asdc data explorer is a multimission web tool which allows the user to browse both internal multimission archive catalogs (grouped by energy band) and external catalogs from other services (vizier, ned, simbad etc.), providing an easy way to explore and cross-correlate large data sets from radio to tev. moreover by using the asdc sed builder tool (v3.0) it is possible to build and handle spectral energy distributions (seds), time resolved seds, and multi-frequency lightcurves. virtual observatory (vo) tools like topcat can also be used to handle sed data in the time domain. the agile reference list of bright gamma-ray sources above 100 mev over the first 2.3 years of observations thus includes at the moment 62 sources, as compared to the 47 1agl in the first catalog. work is in progress to build new complete catalogs of agilegrid sources over the whole observing period (pointing+spinning). the mcal instrument of the agile satellite can observe the high-energy part of gamma-ray bursts (grb) from 350 kev to 100 mev with good timing capability, and the agile-mcal grb catalog, including 85 grb observed from april 2007 to october 2009, was recently published in galli et al. (2013). an online version of the new agile-mcal grb catalog is available from the adc web pages2. we adapted the asdc data explorer to provide the user with additional services dedicated to gamma-ray bursts through a grb explorer tool. the interactive web table in this case contains all the data for the published grbs, including spectral data for 21 bursts, plus some supplementary information on other 7 events. light curves and energy spectra (when available) can be accessed from the grb explorer tool, in the agile mcal data products tab. it is also possible to browse external services to look for grb-related data products from other missions, such as swift-xrt light curve from leicester repository, swift-bat product analysis, fermigbm quicklook lightcurve, gcns and blog for the chosen grb. 4 agile science highlights fig. 1 shows the total gamma-ray intensity above 100 mev as observed by agile up to december, 2012, during the first ∼ 6 years of observations. we present here a selection of the main agile science highlights and some recent updates. agile has provided the first detection of a colliding wind binary (cwb) system above 100 mev in the η-carinae region (tavani et al., 2009b). agile detected a gamma-ray source (1agl j1043-5931, now 1aglr j1044-5944) consistent with the position of the cwb massive system η-car during the time period 2007 july 2009 january. a 2-day gamma-ray flaring episode was also reported on 2008 oct. 11-13, possibly related to a transient acceleration and radiation episode of the strongly variable shock in the system. a revised gamma-ray source list in the complex carina region shown in fig. 2 has been published in verrecchia et al. (2013). figure 2: agile intensity map of the carina region above 100 mev over ∼ 2.3-year pointing mode observation period. new sources and revised (r) positions for 1agl sources are indicated in magenta, the 1agl error circles are indicated in black. the agile detection of gamma-ray emission from the pwn vela-x, described in a science paper (pellizzoni et al., 2010), has been the first experimental confirmation of gamma-ray emission (e> 100 mev) from a pulsar wind nebula. this result constrains the particle population responsible for the gev emission and establishes a class of gamma-ray emitters that could account for a fraction of the unidentified galactic gamma-ray sources. subsequently the nasa fermi satellite has confirmed the vela-x gamma-ray detection, and has also firmly identified other 4 pulsar wind nebulae plus a large number of candidates. gamma-ray flaring activity for a source positionally consistent with cygnus x-1 microquasar was reported twice by agile (bulgarelli et al., 2010; sabatini et al., 2010a and 2010b). agile extensive monitoring of cygnus x-1 in the energy range 100 mev 3 gev during the period 2007 july 2009 october confirmed the existence of a spectral cutoff between 1-100 mev during the typical hard x-ray spectral state of the source. however, even in this state, cygnus x-1 is capable of producing episodes of extreme particle acceleration on 1-day timescales, and even shorter lived flares in the tev range as detected by magic in 2006 (albert et al., 2007). gamma-ray flares of cygnus x-1 detected 2http://www.asdc.asi.it/mcalgrbcat/ 159 carlotta pittori by agile have been recently confirmed for the first time by a reanalisis of fermi-lat data (bodaghee et al., 2012). agile detected for the first time several gammaray flares from cygnus x-3 microquasar and also a weak persistent emission above 100 mev from the source (tavani et al., 2009c). gamma-ray flares occur either in coincidence with low hard-x-ray fluxes or during transitions from low to high hard-x-ray fluxes, and usually appear before major radio flares, following a clear repetitive pattern. this important agile finding has been confirmed by fermi-lat, which also detected the orbital period (4.8 hours) of the binary system in gammarays, securing unambigously the temporal signature of the microquasar (abdo et al., 2009). in the 9 days from december 2 to december 11, 2009 agile and fermi were able to answer a long-lasting question: cygnus x3 system is able to accelerate particles up to relativistic energies and to emit gamma-rays above 100 mev. figure 3: the cygnus region in gamma-rays: agile intensity map from 100 mev to 10 gev. data taken in ∼ 2-year pointing observing mode, from nov. 2007 to oct. 2009. figure adapted from g. piano presentation, 9th agile workshop, 2012. understanding the origin of cosmic rays is one of the most important issues of high-energy astrophysics, and galactic supernova remnants (snr) are considered to be an ideal laboratory to study cosmic-ray acceleration. experimental data analysis below e = 200 mev is crucial to discriminate between theoretical models, since in this energy range hadronic and leptonic emission spectra have a well distinct behavior due to a steepening of the hadronic spectrum due to the neutral pion emission, which is missing in the leptonic case. the agile gamma-ray imager reaches its optimal sensitivity just at the energies in the 50 mev a few gev range at which neutral pions produced by proton-proton interactions radiate, and it was the first to discover a pattern of gamma-ray emission from the supernova remnant w44 that, combined with the observed multifrequency properties of the source, can be unambiguously attributed to accelerated protons interacting with nearby dense gas. this important agile result was reported in (giuliani et al., 2011), and recently confirmed by new fermi-lat data (ackermann et al., 2013) before agile and fermi observations a direct identification of sites in our galaxy where proton acceleration takes place was elusive. figure 4: the w44 supernova remnant spectral energy distribution in gamma-rays. upper panel: the first direct evidence of the pion bump from agile data below 200 mev (giuliani et al., 2011). lower panel: new fermi-lat data below 200 mev confirm the observed steepening due to the neutral pion emission (ackermann et al., 2013). preliminary results from a new detailed study of the snr gamma-cygni with agile have been presented by g. piano during the 11th agile workshop3 (piano et al., paper in progress). from agile data analysis there are hints of non-thermal emission possibly related to shock-cloud interactions in the north-western part of the shell. the agile minicalorimeter is also detecting terrestrial gamma-ray flashes (tgfs), intense and brief pulses of gamma-rays originating in the earth atmosphere, and associated with thunderstorm activity. tgfs last a few thousandths of a second, and produce gamma-ray flashes up to 100 mev, on timescales as low as < 5 ms (marisaldi et al., 2010a). agile joins other satellites in detecting tgfs, but its unique capa3http://www.asdc.asi.it/11thagilemeeting/program.php 160 agile highlights after six years in orbit bility of detecting photons of the highest energies within the shortest timescales makes it an ideal instrument to study these impulsive phenomena. agile data have shown for the first time that tgf cumulative spectrum at high energy deviates from a power law with exponential cutoff model and can be better fit with a broken power law with significant counts above background up to 100 mev. the crucial agile contribution to tgf science is thus the discovery that the tgf spectrum extends well above 40 mev, and that the high energy tail of the tgf spectrum is harder than expected. combined observations of high-energy photons detected by the agile-grid detector have also provided the first direct localization of tgfs in gamma-rays, within a region clustered around the sub-satellite point (fuschino et al., 2011). thanks to its very low inclination orbit in the ±2.5 latitude band, agile provides the largest tgf surface density across the equator available up to now. as statistics grows, agile data show that the tgf sample is possibly composed by two distinct populations: a low-energy population, consistent with typical tgf characteristics, and a high-energy population, with quite distinct features (tavani et al., 2011; marisaldi et al., 2012). crab nebula variability: the surprising discovery by agile of variable gamma-ray emission above 100 mev from the crab nebula in sept. 2010 (tavani et al., 2010; tavani et al., 2011b), and the fermilat confirmation (buehler et al., 2010; abdo et al., 2011) started a new era of investigation of the crab system. the 2012 bruno rossi international prize has been awarded to the pi, marco tavani, and the agile team for this important and unexpected discovery. astronomers have long believed the crab to be an almost ideal standard candle, a nearly constant source (at a level of few percent) from optical to gamma-ray energies (meyer et al., 2010), with possible long-term nebular flux variations over a few-year timescale reported in the hard x-ray range. on september 2010 agile detected a rapid gamma-ray flare over a daily timescale, see fig.4, and thanks to its rapid alert system, made the first public announcement on september 22, 2010. this finding was confirmed the next day by the fermi observatory. agile had also previoulsy detected a giant flare from the crab in october, 2007 during the initial science verification period of the satellite, and in the first agile catalog paper (pittori et al., 2009), it was reported that anomalous episodic flux values observed from the crab in 2007 were under investigation. we know now of five major gamma-ray flares from the crab nebula detected by the agile-grid and fermi-lat, up to may 2013. gamma-ray data provide evidence for particle acceleration mechanisms in nebular shock regions more efficient than previously expected from current theoretical models. we estimate a recurrence rate for strong gamma-ray flares of ∼ (1 − 2)/year. figure 5: the crab nebula flare in september 2010, as observed by agile at energies above 100 mev, (tavani et al., 2011b). a recent study (striani et al., 2013 ) of the flux and spectral variability of the crab nebula above 100 mev on different timescales, ranging from days to weeks, both in agile-grid and in fermi-lat data, also gives evidence for week-long and less intense episodes of enhanced gamma-ray emission that we call “waves” which can occur by themselves or in association with shorter flares. both the flaring and “wave” events can be related to a population of accelerated electrons consistent with a mono-chromatic or relativistic maxwellian distribution. gamma-ray observations challenge standard magneto-hydrodynamics models of nebular emission. 5 conclusions the study of cosmic gamma-rays in the energy range from a few tens of mev to a few tens of gev is only possible from space due to atmospheric absorption. with the successful launch of the new generation gamma-ray space asi telescope agile on april 2007, followed by nasa fermi on june 2008, gamma-ray astrophysics entered a new era. agile is substantially improving our knowledge on various known gamma-rays sources, such as supernova remnants and black hole binaries, pulsars and pulsar wind nebulae, blazars and gamma ray bursts. moreover, agile has contributed to the discovery and study of new galactic gamma-ray source classes, and of galactic gamma-ray transients. the mission is also giving a crucial contribution to the study of the terrestrial gamma-ray flashes seen in the earth atmosphere. gamma-ray observations challenge standard theoretical models of particle acceleration and dynamics under extreme matter conditions. acknowledgement research partially supported through the asi grants i/089/06/2, i/042/10/0 and i/028/12/0. 161 carlotta pittori references [1] abdo, a. a., et al. 2009, science, 326, 1512. doi:10.1126/science.1182174 [2] abdo, a. a., et al. 2011, science, 331, 739. doi:10.1126/science.1199705 [3] ackermann, m. et al., 2013, science 339, 807. 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[32] tavani, m. et al., 2011b, science, 331, 73. doi:10.1126/science.1200083 [33] verrecchia, f., et al., 2013, a&a 558, a137. discussion luigi piro: how can you distinguish between inverse compton and π0 decay in the gev range (question to manami sasaki talk on snrs, tue 28 afternoon). carlotta pittori comment: my comment to luigi piro question is that, as i have shown in my talk, at least in some cases as w44, in which middle aged snr interacts with molecular clouds, the new infrared planck data are very much constraining, and the overall multiwaveleght picture seem to largely favour π0 decay and hadronic models over the leptonic ones. 162 http://dx.doi.org/10.1126/science.1182174 http://dx.doi.org/10.1126/science.1199705 http://dx.doi.org/10.1088/0004-637x/775/2/98 http://dx.doi.org/10.1029/2009ja014502 http://dx.doi.org/10.1126/science.1183844 http://dx.doi.org/10.1088/2041-8205/712/1/l10 http://dx.doi.org/10.1038/nature08578 http://dx.doi.org/10.1126/science.1200083 introduction the ground segment and the agile data center new agile catalogs and asdc interactive web tools agile science highlights conclusions 170 acta polytechnica ctu proceedings 1(1): 170–174, 2014 170 doi: 10.14311/app.2014.01.0170 black hole results from xmm-newton norbert schartel1 1xmm-newton science operations centre, esa, villafranca del castillo, apartado 78, e-28691 villanueva de la cañada madrid, spain corresponding author: norbert.schartel@sciops.esa.int abstract xmm-newton is one of the most successful science missions of the european space agency. since 2003 every year about 300 articles are published in refereed journals making directly use of xmm-newton data. all xmm-newton calls for observing proposals are highly oversubscribed by factors of six and more. in the following some scientific highlights of xmm-newton observations of black holes are summarized. keywords: x-ray agn black hole. 1 introduction xmm-newton ([1]) is the second cornerstone of european space agency’s (esa) horizon 2000 science programme, providing an observatory-class x-ray facility. the spacecraft was launched by an ariane 5 on 10 december 1999. the observatory provides simultaneous non-dispersive spectroscopic imaging and timing (european photon imaging camera; epic, [2] and [3]), medium resolution dispersive spectroscopy (reflection grating spectrometer; rgs, [4]) and optical/uv imaging, spectroscopy and timing from a co-aligned telescope (optical monitor; om, [5]). the three x-ray mirrors ([6]) in combination with the cameras of epic offer a large effective area over the energy range from 300 ev to 12 kev, up to 2500 cm2 at 1.5 kev and ∼1800 cm2 at 5 kev. the scientific potential of the effective area may be illustrated by the first observation of an evolving dust-scattered x-ray halo around a gamma ray burst ([7]). each of the two modules of the rgs cover the energy range from ∼0.4 kev to 2.2 kev with an effective area of 60 cm2 at 15 å. 2 scientific highlights scientific highlights resulting from the first decade of xmm-newton and chandra observations can be found in [8]. in the following i list a number of highlights from xmm-newton observations of black holes. in this paper i have focused on some of the most exciting discoveries in this field, which also received wide publicity in public relations announcements by esa. 2.1 galactic black holes and ultraluminous x-ray sources globular clusters (gc), containing thousands of stars packed within tens of light years, were considered as a possible breeding ground for black holes. a rival hypothesis suggests that black holes are ejected through close star encounters and consequently gcs are devoid of black holes. xmm-newton observations of ngc 4472 allowed the first detection of a black hole in a gc ([9]) excluding the latter hypothesis. ultraluminous x-ray sources (ulx) were proposed to harbour intermediate-mass black holes, which provides the link between stellar mass black holes and supermassive black holes (smbh) in the centres of galaxies. xmm-newton and chandra observations of cxom31 j004253.1+411422 in andromeda allowed to connect this ulx to low mass x-ray binaries ([10], implying accretion onto a stellar-mass black hole in the eddington regime. a second ulx found in andromeda, xmmu j004243.6+412519, allowed to observe the emission of the accretion disk in x-rays together with the emission form its jets in radio ([11]). the experimental key for both observations was the low absorbing column density towards andromeda whereas absorption is a major obstacle of ulx observations in our own galaxy. [12] found an intermediate-mass black hole in ngc 1313. the x-ray spectra of the ulx can be described with a power law plus an accretion disk (kt ∼= 150 ev) implying a mass of ∼= 103m�. a intermediatemass black hole with m > 500 m� could be associated with an ulx in eso 243-49 based on luminosity variations observed by xmm-newton ([13]). 170 http://dx.doi.org/10.14311/app.2014.01.0170 black hole results from xmm-newton 2.2 the strong gravitational field currently, x-ray observations are the only way to observe the strong gravitational field in the direct vicinity of black holes and neutron stars ([14]). special and general relativistic effects distort the spectra of particles orbiting black holes depending on the orbital parameters and the black hole’s spin. theoretical discussion can be found in [15], [16], [17] [18] or more recently in [19] and [20]. experimentally the iron kα line is most studied as there are no lines of abundant elements nearby. early examples are the xmm-newton observations of the galactic black hole xte j1650-500 in outburst ([21]) and the active galactic nuclei (agn) mgc-6-30-15 in low state ([22]). both spectra are explained by a fast spinning black hole and the extraction and dissipation of rotational energy from it. the simultaneous xmm-newton and nustar observation of ngc 1365 revealed that reflection from an ionized disk readily explains the spectra taken by both satellites ([23]). the xmm-newton spectra of the galactic black hole, gx 339-4 in outburst ([24]) is an example of a black holes with almost maximum spin. the observation of 1h 0706-495 is unique as it shows not only the iron kα, but also the iron lα line ([25]). in addition the light cure shows the expected characteristic variability of reflection from an ionized disk (compare also [26], [27], [28], [29]). 2.3 active galactic nuclei (agn) in low states following [30] x-ray spectra of agns are composed of a power-law continuum emitted above a black hole plus reflection from an ionized disk. during the low state the continuum emission region moves nearer to the black hole and gravitational bending affects its light path. observationally, during low states the continuum emission appears suppressed whereas the reflected emission appears constant or even enhanced, compare also [31]. the most intensive studied agn in low state with xmm-newton is pg 2112+059, where an additional layer of ionized material was used to favour the reflection interpretation versus alternative scenarios ([32], [33] and [34]). [35] used variability considerations to discriminate the reflection interpretation versus an absorption scenario for pg 0844+349 in an x-ray weak state. and [36] could demonstrate for the low state observation of 1h0707-495 reflected emission within one gravitational radius of the event horizon of the black hole. 2.4 aspects of variability near supermassive black holes (smbhs) whereas quasi-periodic-oscillations (qpo) are well established in x-ray binaries for almost 30 years, qpos remained elusive in agns. xmm-newton measured a ∼1 hour qpo for re j1034+396 ([37]). [38] found evidence for orbital motion of material close to the central black hole of mrk 766. a xmm-newton observation allowed [39] to observe a co-rotating flare at a distance of only 3.5 to 8 schwarzschild radii to the smbh of ngc 3516. 2.5 energy budget, winds and outflows [40] established for the fist time simultaneous spectral energy distributions for the majority of the [41] reverberation mapped sample of agn based on xmmnewton epic and om measurements. [42] used xmmnewton observations to show that radio-galaxies produce sufficient mechanical energy to unbind a significant fraction of the intra-group medium, an effect which is negligible in massive clusters of galaxies. combining high resolution rgs spectra with sensitive light-curves of epic, [43] demonstrated an accretion-disk origin for the two warm absorber winds in ngc 4051. 1h 0707495 shows a mildly relativistic, highly ionized outflow which changed its velocity from about 0.11c to 0.17c between 2008 january and 2010 september ([44]). ultrafast outflows are present in >35% of radio-quiet agn observed with xmm-newton, providing a significant contribution to the agn cosmological feedback ([45], [46], [47]). 2.6 flares and tidal disruption events [48] observed several peaks in the power density spectrum of the x-ray light curve of the smbh in the galactic centre during which period a bright x-ray flare was detected ([49]). theoretical studies revealed a previously unknown topological structure inherent to black holes with high spin: in a small region near the event horizon of the spinning black hole the orbital velocity decreases for decreasing orbital radius ([50]). this effect is now rightfully known as the aschenbach effect ([51]). [52] could identify a tidal disruption event based on rosat, chandra and xmm-newton observations. suzaku and xmm-newton observations taken shortly after the occurrence of the tidal disruption event swift j164449.3+573451 reveal a 200-second x-ray quasiperiodicity ([53]). this qpo might be explained with the forming of an accretion disc or precession of the jet. 171 norbert schartel 2.7 deep fields and cosmology a total of 1000 agn detections from a variety of rosat, xmm-newton and chandra surveys allowed [54] to obtain for the first time reliable space densities for low-luminosity (seyfert-type) x-ray sources at high cosmological redshifts. their evolutionary behaviour shows strong dependency on the x-ray luminosity and differs from the dependency found for high luminosity agns and quasars. xmm-newton allows the detection of quasars at highest redshift, e.g. sdss j104433012502 at z=5.80 ([55]). the spacecraft could even establish an x-ray spectrum of sdss j1030+0524 at z=6.30 ([56]). an ionized iron kα absorption edge in the x-ray spectrum of apm 08279+5255 allowed to obtain an, at the time of publication, highly interesting constrain on the age of the universe ([57]). 3 discussion and conclusions since 2003 every year about 300 articles are published in refereed journals making directly use of xmm-newton data. all xmm-newton calls for observing proposals are highly oversubscribed by factors of six and more. within esa’s mission extension scheme all missions are evaluated every 2 years and possibly extended by 4 years subjected to midterm confirmation. xmmnewton is funded up to end of 2016 subject to midterm confirmation and further extension discussion in 2014. currently, the xmm-newton mission is implementing four-reaction-wheel operation schemata, which will reduce fuel consumption significantly. the envisaged operation mode will allow technically operating the mission up to 2026. acknowledgement i thank the organizers of the workshop and especially franco giovannelli for giving him the opportunity to show highlights of xmm-newton black hole observations. and i thank the anonymous referee for many fruitful comments and suggestions. references [1] f. jansen et al. xmm-newton observatory. i. the spacecraft and operations. a a, 365:l1–l6, january 2001. 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[57] g. hasinger, n. schartel, and s. komossa. discovery of an ionized fe k edge in the z=3.91 broad absorption line quasar apm 08279+5255 with xmm-newton. apj, 573:l77–l80, july 2002. 174 http://dx.doi.org/10.1103/physrevd.71.024037 http://dx.doi.org/10.1126/science.1223940 introduction scientific highlights galactic black holes and ultraluminous x-ray sources the strong gravitational field active galactic nuclei (agn) in low states aspects of variability near supermassive black holes (smbhs) energy budget, winds and outflows flares and tidal disruption events deep fields and cosmology discussion and conclusions 20 acta polytechnica ctu proceedings 1(1): 20–26, 2014 20 doi: 10.14311/app.2014.01.0020 gravitational waves and dark energy peter l. biermann1,2,3,4,5, benjamin c. harms1 1department of physics and astronomy, the university of alabama, box 870324, tuscaloosa, al 35487-0324, usa 2mpi for radioastronomy, bonn, germany 3karlsruhe institute of technology (kit) institut für kernphysik, germany 4department of physics, university of alabama at huntsville, al, usa 5department of physics & astronomy, university of bonn, germany corresponding author: bharms@bama.ua.edu abstract the idea that dark energy is gravitational waves may explain its strength and its time-evolution. a possible concept is that dark energy is the ensemble of coherent bursts (solitons) of gravitational waves originally produced when the first generation of super-massive black holes was formed. these solitons get their initial energy as well as keep up their energy density throughout the evolution of the universe by stimulating emission from a background, a process which we model by working out this energy transfer in a boltzmann equation approach. new planck data suggest that dark energy has increased in strength over cosmic time, supporting the concept here. the transit of these gravitational wave solitons may be detectable. key tests include pulsar timing, clock jitter and the radio background. keywords: cosmology dark energy black holes gravitational waves. 1 introduction dark energy was originally detected as accelerated expansion seen in the distance scale for supernovae of type ia (schmidt et al., 1998, riess et al. 1999, perlmutter et al. 1999; for a review see frieman et al. 2008). many suggestions have been made about what dark energy is, what its strength is, what its time evolution is, and what possible further observational results are. the idea that dark energy is gravitational waves may explain its strength and its time-evolution. one possible concept is that dark energy is the ensemble of coherent bursts (solitons) of gravitational waves originally produced when the first generation of supermassive back holes was formed (caramete & biermann 2010); the energy density of such solitons would suffice within the uncertainties. these solitons get their initial energy as well as keep up their energy density throughout the evolution of the universe by stimulating emission from a background (biermann & harms 2013). our model of the background metric resembles the randall-sundrum ideas (1999a, b) but is timedependent, and describes the energy flow from the background (strong-gravity) brane to our world (weakgravity) brane. planck data suggest that dark energy has increased in strength over cosmic time (planck 2013 xvi), as predicted by our model. gravitational waves were far below today’s dark energy at the epoch of early nucleosynthesis and of the formation of the microwave background ripples (as summarized in ligo+virgo-coll. 2009), both much earlier than the likely formation epoch of the first generation of super-massive black holes. our model is also consistent with early star formation (biermann et al. 2014), as we argue below. the transit of the gravitational wave solitons postulated here may be detectable. we discuss the predictions briefly below and elsewhere. we focus on the boltzmann equation approach, working out the energy transfer from the strong gravity background in stimulated emission. 1.1 gravitational solitons from black hole mergers inspired by bekenstein’s (1973) considerations we posit: when the first generation of super-massive black holes was formed, each produced a coherent burst of solitonlike gravitational waves which combine to give a total energy of order ∼ 1 2 nbh,0mbh c 2 (1 + z?) 3 . (1) in the following we also call this an ensemble of soliton waves, or shell fronts. nbh,0 is the original comoving density of super-massive black holes. today supermassive black holes have a density of 10−1.7±0.4 mpc−3 20 http://dx.doi.org/10.14311/app.2014.01.0020 gravitational waves and dark energy above mbh = 3·106 m� (caramete & biermann 2010); assuming that they grow by merging, and allowing for statistical and systematic errors, an original comoving density of nbh,0 = 1 mpc−3 seems possible. this comoving density is the density black holes had at the beginning, so transposed to today without change in their numbers per comoving volume. the data suggest that there was a generation of first super-massive black holes with a mass between mbh ∼ 106m� and mbh ∼ 107m�. the original black hole mass may be ∼ 3 · 106m� considering (i) the black hole mass function (greene et al. 2006, caramete & biermann 2010), (ii) the instability of massive stars (appenzeller & fricke 1972a, b) in an agglomeration picture (spitzer 1969, sanders 1970), and (iii) the observed black hole in our galactic center (e.g. eckart et al. 2005). the redshift of creation z? may be large, as formation of massive stars may begin at redshift 80 (biermann & kusenko 2006). redshifts z? from about 30 to 50 allow a quantitative interpretation of the data of dark energy. at the original density of black holes adopted here redshift 50 is consistent with the mass of mbh ∼ 3 · 106m�, and redshift 30 would imply mbh ∼ 107m�, in either case to make the estimate consistent with dark energy today. what is the motivation for considering gravitational waves? bekenstein (1973) wrote about the entropy of the universe: “... we must regard black hole entropy as a genuine contribution to the entropy content of the universe”. however, entropy is also information, and information must have a carrier. a natural suggestion is that this carrier is gravitational waves, with an energy commensurate with the black hole scale. this suggestion is consistent with the fact that cosmological black holes are not in thermodynamic equilibrium, and therefore the entropy associated with such black holes should be described by statistical mechanics as advocated in harms and leblanc (1992, 1993). this speculation immediately gives s kb = ngw,0 = 4π ( mbh mpl )2 , for zero spin , (2) where ngw,0 is the number of gravitons at the formation of the black hole. for mbh = 3 · 106 m� this is ngw,0 ' 1090. mbh is the original mass of the black hole, mpl is the planck mass, c is the speed of light, and gn is newton’s constant of gravity. egw is the average graviton energy given by egw = 1 8π h̄c3 gnmbh = c2 8π m2 pl mbh . (3) this gives a graviton energy of egw ' 10−30 erg for this black hole mass. the entire energy content then is ngw,0egw = 1 2 mbh c 2 . (4) we picture this as a coherent burst of gravitational waves, or a soliton wave, ejected at formation of the black hole. it is clear from the considerations above that we are not using the weak-field approximation. multiplying with the original density of super-massive black holes reproduces our estimate above. 1.2 five-dimensional background model in our model for the background, which has some similarity to the randall-sundrum (1999a, b) ideas, we identify a possible local metric to describe a 5d world with a 4d strong gravity brane and our 4d world weakgravity brane. ds2 = −e(u/l) m t/ψ c2 dt2 + e(ul ) p t/β du2 + e(1−b(ul ) n ) 2 t/αth e−(ul ) k (1− t φ ) dxi dx i , (5) where i = 1, 2, 3, τh is the hubble time, l = lpl is the planck length, τpl = lpl/c is the planck time, u is the coordinate in the fifth dimension, and the remaining, non-coordinate quantities are arbitrary parameters. although the five-dimensional covariant divergence of the energy-momentum tensor does not vanish everywhere, it vanishes on the weak-gravity (weak) brane (u = 0), and it is approximately zero on the strong-gravity (strong) brane (u = l) for very small dimensionless ratios β/τh and ψ/τh with ψ < 0 and β > 0, with the conditions a) τh(ψ+β)/(ψβ) >> 1, b) 2(b−1)/α > τh/φ−1, and c) α2 = 3. g00 in the metric above then defines the confining potential for the strong brane. gravitons from our brane stimulate transitions between bound states on the strong brane, resulting in the emission of gravitons onto our brane. this metric describes a weak brane for our world which is expanding with time, and a strong brane which is contracting with time, albeit very slowly for the latter brane. the 5d-cosmological constant measured on the weak brane is ωweak = − ( τpl τh )2 . figure 1: the stimulated emission of gravitons in a shell in our model the gravitons on the strong-gravity brane obey a planck-like distribution with planck temperature. we adopt the point of view that the planck scales are limits: nothing can go below planck time 21 peter l. biermann, benjamin c. harms and planck length, and no single particle can go beyond planck energy, in any frame. the strong brane is stable against collapse, since given a planck spectrum for any wavelength λ the free-fall time scale τff is always either equal or longer than the pressure wave time scale τs. figure 2: the strong-gravity (planck brane) and weak-gravity (tev brane) branes τff = τpl ( λ lpl )3/2 ≥ τpl ( λ lpl ) = τs. 2 stimulate emission of energy from the strong-gravity brane in the following we use a particle-wave duality for gravitons at high energy, which thus associates a wavenumber ~k/h̄ and a corresponding length-scale λ to each spatial direction, and we assume localization is possible to about a wavelength. 2.1 rate of energy transfer the distribution function n (k, t) is the distribution of occupied allowed states on our brane for gravitons with momenta k = |~k| and p = |~p| at time t on the shell and satisfies the equation( ∂ ∂t − ṙ(t) r(t) k ∂ ∂k ) n (k, t) = 1 k ∫ d3 k′ (2π)3 2 k′ ∫ cd3 p (2π)3 2e(p) ∫ cd3 p′ (2π)3 2e(p′) ∫ d3 k′′ (2π)3 2 k′′ γ2 |m |2 (2π)4δ4(k +q−k ′ −k ′′ −q′) (2π)6 δ3(~k′ − ~k′′) δ3(~k − ~k′) [gb(p ′, t)(1 +n (k, t)) ((n (k′, t) + 1)(n (k′′, t) + 1)− 1) − n (k, t)gb(p, t)(1 +n (k′, t))(1 +n (k′′, t))] . (6) where k = (k,~k), γ = k3ref,1, and q = (e, ~p). kref,1 is a reference momentum to be determined below. the δ-functions, δ3(~k′ − ~k′′) and δ3(~k − ~k′), have been inserted to impose coherence of the outgoing gravitons. |m |2 is the matrix element squared for the quadrupole emission of a graviton of 4-momentum k′′, and has the dimensions of (momentum)−3 (time)−1. we will assume that this matrix element squared is proportional to k5. gb(p, t) is the occupation number distribution of the background particle sea. r(t) = (1 + z?)/(1 + z) is the scale factor for an expanding universe. the following analysis is done in the observer frame. the boltzmann equation for n (k, t) to lowest order in the expansion of the 4-dimensional δ-function is( ∂ ∂t − ṙ(t) r(t) k ∂ ∂k ) n (k, t) ' +κ k n (k, t) (n (k, t) + 1) , (7) where the factor κ is given, after integration over all the δ-functions, by κ = k2ref,2h(z) 24πkbh |m |2 ln{kbh+ k } . (8) in the equation above kbh+ is the maximum momentum at which stimulated emission of gravitons occurs, just above the momentum of the peak of n (k, t). since the log-term in eq.8 varies very slowly over the range of k of interest we approximate this term with a constant and set β = {ln(kbh+/k)}/(24 π). |m |2 is related to |m |2 by extracting the factors (k/kref,1)3/k3ref,1, h(z). a threshold function of 2 gbn/(gb + n ) arises from the normalized interaction between the gravitons on the background brane and our brane; this function connects to the strong brane only if n > gb, which is the condition for stimulated emission. these choices do not introduce new constraints or additional assumptions. next we redefine (k/kref,2)2 κ = κ to extract the k-dependence from |m |2. making the change of variables k = k̃/r(t), eq.7 can be written as ∂n (k̃, t) ∂t ' h(z) k̃ β kbh r(t) n (k̃, t) (n (k̃, t) + 1) . (9) in terms of the frequency of the wave at emission this equation is ∂n (ν0, t) ∂t ' h(z)h ν0 β kbh r(t) c n (ν0, t)(n (ν0, t) + 1) . (10) introducing the dimensionless variables x = h ν0 kb tg0 , and y = ∫ t 0 kbtg0h(z)β kbh cr(t) dt′ , (11) where kbhc = kbtg0 = mplc 2 mpl 8πmbh . eq.(10) becomes ∂n ∂y ' +xn (x, y) (n (x, y) + 1) . (12) the solution of this equation is n (x, y) = 1 ex(a−y)+b − 1 , (13) 22 gravitational waves and dark energy where a and b are constants, to be determined later. this distribution (eq.13) is planck-like with a timedependent normalized temperature 1/a. the rate at which energy is created can be calculated from the expression for n in eq.10. the rate at which energy is created can be calculated from the expression for n in eq.(10). the rate of energy creation per existing graviton (of the total number ngw,0r(t)4) is d < e > dt = βh(z) r(t) × (14)∫ x3 hν0n (ν0, t) (n (ν0, t) + 1) dx . the total rate of energy creation is d < et > dt = ngw,0r(t)3 kbh ch(z)β a , (15) where a = ∫ x4n (x, t) (n (x, t) + 1) dx (16) inserting all these constants into the integral for y demonstrates that y approaches a constant for the redshift z? being large, and integrating down to today or even into the future, when y approaches a constant of β << 1. a is equivalent to an inverse temperature, and should be of order unity. without loss of generality we can set b = 0. this integral strongly depends on the exact value of a − y, and is of order 30 for a − y ' 1, and b approaching zero. the matrix element |m | does not evolve with time, and scales as momentum |m | = εm ( k mplc ) . (17) above we have used εm = 1; we now generalize and allow εm to be different from unity. writing |m | in this way suggests that the interaction between the gravitons on our brane and the gravitons on the background brane comes down to a fundamental coupling constant. this behavior is consistent with the idea [22], that the gravitational coupling strongly increases with energy to approach the other three coupling constants at near planck energies. this allows the expression for d dt to be consistent with the observed energy density under the condition that aβ εm = 3. for the constant a = 1 above, β of order 0.1, and εm = 1, the quantity {aβ εm} is in fact close to 3. however, if we were to require that the k-range be very large, then β would be larger, and εm would be required to be smaller than unity accordingly. inserting this parameter dependence into eq.(15) then leads back, to within the approximation that aβ εm = 3, to the result we were seeking, 3 2 mbh c 2h(z) ( 1 + z? 1 + z )3 . (18) after integrating we obtain with this redshift dependence a constant dark energy density as in eq.( 1) by multiplying by the redshift evolution of black holes nbh,0 (1 + z)3. the factor of 4 multiplying ρde in eq.22 below derives from the sum of dark energy density and pressure, and corresponds to 3 (ρde+pde/c 2). therefore the rate of change of dark energy with time is 3 (ρde + pde/c 2)h(t) and today 3ρdeh(z = 0) = 3 2 mbh c 2h(z = 0) (1 + z?) 3 . (19) this justifies the ρde h(t) term in eqs.22 and 25. this shows that dark energy remains at the level of eq.(1) throughout the evolution of the universe, in the approximation that most early super-massive black holes were formed over a short span of time. 2.2 equation of state we define ρde(t, u) as the dark energy density, ρ(t, u) as the total energy density, p (t, u) as the total pressure, and we use the equation of state pde(t, u) = ρde(t, u) c2/3 . the dark energy density ρ(t, u) is scaled to the value of the dark energy density observed on our brane today ( redshift z = 0 ). the friedmann-robertson-walker form of the einstein equations on the weak-gravity brane must be (h(t)) 2 = ( ˙r(t) r(t) )2 = 8πgn 3 ρ(t, 0) (20) and r̈(t) r(t) = −4πgn 3 ( ρ(t, 0) + 3 p (t, 0) c2 ) + 16πgn 3 ρde(t, 0) + 4πgn sinj 3h(t) , (21) where the rate of change of the energy density used is ρ(t, 0) = − 3 ( ρ(t, 0) + p (t, 0) c2 ) h(t) + 4 ρde(t, 0)h(t) + sinj . (22) we emphasize that in the second equation, eq.21, the term 16πgn ρde(t, 0)/3 corresponds to the continuous energy transfer by stimulated emission on the basis of existing dark energy; the additional term (4πgn sinj)/(3h(t)) describes new formation of dark energy. this allows a different equation of state for exactly the same cosmological observations, as now for pde = ρdec 2/3 the modified equation 21 becomes identical to the canonical version of this equation for 23 peter l. biermann, benjamin c. harms pde = −ρdec2. the corresponding set of equations for the strong-brane are hsb(t)2 = 8πgn 3 (ρde(t, lsb)− λsb) (23) where λsb is the cosmological constant on the strong brane at the beginning of the epoch of black hole formation and r̈sb(t) rsb(t) = −16πgn 3 ρde(t, 0) h(t) hsb(t) (24) + 8πgn 3 ( 3 ρde(t, lsb)− λsb)− 4πgn sinj 3hsb(t) , the rate of change of the energy density on the strongbrane is correspondingly ρ̇de(t, lsb) = 3 ( ρde(t, lsb) + 1 c2pde(t, lsb) ) hsb(t) −4 ρde(t, 0)h(t)− sinj . (25) eq.24 is derived from eq.23 using the conservation of energy-momentum equations; eqs. 22 and 25 insure that energy is conserved between the two branes, the 4-dimensional boundaries of the 5-dimensional universe described by our model. for epochs before the energy transfer started ρde(t, 0) = 0, and sinj = 0, and we can set ρde(t, lsb) = λsb for t < t(z = z?). 3 comparison to experimental limits our model can be tested by several different types of experiment. we discuss two of these below. 3.1 pulsar timing experiments figure 3: gravitational wave background limit from pulsar timing (dashed line) , and our inferred gravitational wave background from stimulated emission of gravitational waves from the background planck sea constituting dark energy (straight line). the ordinate is the fraction of closure density ω per log bin of frequency, and the abscissa is the frequency of the gravitational waves f . the gravitational waves in our model arise from the production of black holes in the early universe at a redshift of z ' 50. the observed constant dark energy density is maintained by the continuous production of gravitational waves by black-hole interactions with the planck sea background. for an idealized model in which all black holes were created at the same time, and with the same mass, the gravitational wave background peaks near fgw,max ' 10−4.5 hz m−1bh,6.5 (1+50)/(1+ z?). a soliton comes past a given point in space-time on the order of every 20 seconds. wave forms are created by uncorrelated solitons passing by a given point. ultra-precise timing experiments which test the steadiness of timing over time scales of order a few seconds to a few minutes would show these variations in the energy density if the precision is high enough. the precision to detect such a signal has to correspond to seconds in the expansion rate of the universe, which requires the precision to be of order 10−17.5, or a few 10−18. this precision is expected to be reached in the next generation of clocks [16]. t ρ 1 figure 4: the sequential passing of solitons (sharp peaks) can be approximated by a sinusoidal wave form. 4 conclusions if the validity of our model is proven by experimental tests such as the pulsar timing experiments (fig.3), the detection of time jitter (fig.4), or the detection by an observatory such as ligo or virgo of the passage of a shell front by a dedicated type of data analysis, the implications for cosmology are great. the basis of our model is that the source of dark energy is the creation of gravitational waves by the interaction of surfaces at critical density, e.g. the planck surfaces surrounding black holes, with a strong-gravity brane located a few planck lengths from our weak-gravity brane. our model is consistent with the big-bang theory after the first planck time. however, in our model the universe starts from a lemaitre-like ‘atom’ or ‘seed’ [5]. our model also has implications for quantum gravity theory. experimental evidence for the validity of 24 gravitational waves and dark energy our model would imply the existence of a strong-gravity brane and extra dimensions as well as a smallest distance and impenetrable planck surfaces rather than horizons. although our model describes several observed cosmological phenomena, it is largely heuristic. we are currently working on an exact solution of the fivedimensional space-time metric and a more formal mathematical description of the stimulated emission amplitude for the creation of the solitons. acknowledgement discussions with lou clavelli greatly contributed to the development of the paper; discussions with laurenţiu caramete (bucharest, romania), roberto casadio (bologna, italy), marco cavaglia (oxford, ms), laszlo gergely (szeged, hungary), shaoqi hou (tuscaloosa, al), pankaj joshi (mumbai, india), gopal-krishna (pune, india), octavian micu (bucharest, romania), piero nicolini (frankfurt, germany), norma sanchez (paris, france), joe silk (oxford, united kingdom), allen stern (tuscaloosa, al), dijan stoikovic (buffalo, ny), and hector de vega (paris, france) are gratefully acknowledged. helpful comments on earlier versions of the manuscript were received from r. casadio, m. cavaglia, l. gergely, a. graham, p. joshi, o. micu, p. nicolini, and d. stoikovic. this research was supported in part by the doe under grant de-fg02-10er41714. references [1] appenzeller, i., & fricke, k., a&a 18, 10 (1972a); appenzeller, i., & fricke, k., a&a 21, 285 (1972b) [2] bekenstein, j.d., phys. rev. d 7, 2333 (1973) doi:10.1103/physrevd.7.2333 [3] biermann, l., schlüter, a., phys. rev. 82, 863 (1951) doi:10.1103/physrev.82.863 [4] biermann, p.l., kusenko, a., phys. rev. lett 96, 091301 (2006) doi:10.1103/physrevlett.96.091301 [5] biermann, p.l., & harms, b.c., eprint arxiv:1205.4016 (2012); biermann, p.l., & harms, b.c., in proc. at the 13th marcel grossmann meeting, july 2012, eprint arxiv:1302.0040 (2013) [6] biermann p.l., et al., mon. not. roy. astron. soc. 441, 1147 (2014) doi:10.1093/mnras/stu541 [7] caramete, l.i., & biermann, p.l., a&a 521, id.a55 (2010) [8] eckart, a., et al., in the evolution of starbursts: the 331st wilhelm and else heraeus seminar. aip conf. proc. 783, 17 (2005) [9] frieman, j.a., turner, m.s., & huterer, d., ara&a 46, 385 (2008) doi:10.1146/annurev.astro.46.060407.145243 [10] greene, j.e., barth, a.j., & ho, l.c., new astro. rev. 50, 739 (2006) doi:10.1016/j.newar.2006.06.080 [11] harms, b.c., & leblanc, y., phys. rev. d 46, 2334 (1992); harms, b.c., & leblanc, y., phys. rev. d47, 2438 (1993) [12] ligo and virgo collaborations, nature 460, 990 (2009) doi:10.1038/nature08278 [13] munyaneza, f., & biermann, p.l.,a&a 436, 805 (2005); munyaneza, f., & biermann, p.l., astron. & astroph. letters 458, l9 (2006) [14] perlmutter, s., et al., apj 517, 565 (1999) [15] planck collaboration; ade, p.a.r., et al., eprint arxiv:1303.5078 (2013) [16] predehl, k., et al., science 336, 441 (2012) [17] randall, l., sundrum, r., phys. rev. lett 83, 3370 (1999a); randall, l., sundrum, r., phys. rev. lett 83, 4690 (1999b) [18] riess, a.g., et al. aj 116, 1009 (1998) [19] sanders, r.h., apj 162, 791 (1970) [20] schmidt, b.p., et al., apj 507, 46 (1998) [21] spitzer, l., jr., apjl 158, l139 (1969) doi:10.1086/180451 [22] dimopoulos, s, raby, s.a., wilczek, f. phys. today oct., p. 25 (1991) discussion moshe elitzur: are there predictions for the effect of your model on the imprint of fluctuations on cmb and baryon acoustic oscillations? benjamin harms : dark energy in our mode is due to the merging of black holes at a ' 50, so well after the formation of the cmb. there may be some effect on the propagation of the cmb photons, but we have not yet worked out the exact nature of this effect. 25 http://dx.doi.org/10.1103/physrevd.7.2333 http://dx.doi.org/10.1103/physrev.82.863 http://dx.doi.org/10.1103/physrevlett.96.091301 http://dx.doi.org/10.1093/mnras/stu541 http://dx.doi.org/10.1146/annurev.astro.46.060407.145243 http://dx.doi.org/10.1016/j.newar.2006.06.080 http://dx.doi.org/10.1038/nature08278 http://dx.doi.org/10.1086/180451 peter l. biermann, benjamin c. harms jim beall: can you comment on the effect these ’seed’ black holes have on galaxy formation? benjamin harms: the main difference between our model and the ’big bang’ theory is that our model allows for large assemblies of stars which have never merged and do not have an agn, which have apparently been observed. 26 introduction gravitational solitons from black hole mergers five-dimensional background model stimulate emission of energy from the strong-gravity brane rate of energy transfer equation of state comparison to experimental limits pulsar timing experiments conclusions 240 acta polytechnica ctu proceedings 1(1): 240–245, 2014 240 doi: 10.14311/app.2014.01.0240 unveiling the nature of integral objects: a review pietro parisi1, on behalf of a large collaboration 1istituto di astrofisica e planetologia spaziali (inaf), via fosso del cavaliere 100, roma i-00133, italy corresponding author: p. parisi abstract since its launch in october 2002, the integral observatory has improved our knowledge of the hard x-ray sky above 20 kev, carrying out more than ten years of observations in the energy range from 5 kev to 8 mev. the most recently published integral/ibis surveys listed more than seven hundred sources in the 20-100 kev band. most of these objects are either active galaxies (agns) or x-ray binaries; a fraction of both classes is made of highly absorbed sources, often associated with dim optical counterparts. despite the big effort in the identification process, a large part of these ibis objects (∼25% of them) still remains unclassified. cross-correlation with archival catalogues and/or multiwaveband follow-up observations are of invaluable help to identify and properly classify this unknown objects, but only optical or ir spectroscopy with ground based telescopes in the northern and southern hemisphere can reveal the real nature of these objects. in this work we report on source types that we find among the unidentified objects in the most recent integral surveys. keywords: galaxies: seyfert x-ray binaries techniques: spectroscopic. 1 introduction one main objective of the integral mission is a regular survey of the entire sky in the hard x-ray band. this makes use of the unique imaging capability of the ibis instrument (ubertini et al. 2003) which allows the detection of sources at the mcrab level with a typical localization accuracy of a few arcmin. during the first 5 years of its life, the observatory concentrated mainly on a deep exposure of the galactic central radian, regular scans of the galactic plane, pointed observations of the vela region, and target of opportunity follow up observations. through the ibis imager, optimized for survey work with excellent imaging and spectroscopy capability, catalogs devoted either to the galactic plane scan (gps) or to the improvement of the extragalactic coverage were published. up to now, ibis detected more than 700 sources in the hard x-rays between 20 and 100 kev (bird et al. 2010, krivonos et al. 2010, 2012), and ∼ 30% had no obvious counterpart at other wavelengths and therefore cannot yet be associated with any known class of high-energy emitting sources. comparisons with catalogues or surveys at other frequencies (especially soft x-rays, optical, infrared and radio) are of invaluable help in reducing the localization uncertainty of these ibis sources from arcminutes down to a few (< 10) arcseconds, thus making the search for their optical or ir counterparts much easier. once this is done, then spectroscopic follow up observations provide a classification of the source, a confirmation of the proposed association and the study of that source individually or at population level. thanks to the above method, many new hard x-ray sources have been studied for the first time, including new classes of galactic objects, such as absorbed high mass x-ray binaries (hmxb see walter 2007), supergiant fast x-ray transients (sfxt, e.g., sguera et al. 2005, 2006; leyder et al. 2007), magnetic cataclysmic variables (cvs; barlow et al. 2006; bonnet-bidaud et al. 2007; landi et al. 2008) and symbiotic x-ray binaries (syxbs); in the extragalactic sky, a higher percentage of absorbed active galactic nuclei (agns) were reported compared to softer (2-10 kev) surveys, including a few new nearby compton thick objects (malizia et al. 2009), systematically pinpointing, for the first time, extragalactic sources in the so-called ‘zone of avoidance’, which hampers observations in soft x-rays and optical along the galactic plane due to the presence of gas and dust. all of these objects were classified by means of intensive optical and ir spectroscopic campaigns at various telescopes located worldwide. 2 surveys through hard x-ray surveys we can obtain all-sky maps of the celestial high-energy emission and study catalogues of sources unbiased in term of absorption and which are capable of producing non thermal emission 240 http://dx.doi.org/10.14311/app.2014.01.0240 unveiling the nature of integral objects: a review processes, or being the site of the most extreme astrophysical phenomena observed in the universe. the most recent integral/ibis surveys are that of bird et al. (2010) and krivonos et al. (2010, 2012): • the 4th ibis survey (bird et al. 2010) collected data from november 2002 to october 2008 for ∼80 ms of exposure in the 20-100 kev energy range and produced a catalogue of 723 sources (29% unidentified) ; • the ibis 7-years all-sky hard x-ray survey (krivonos et al. 2010) collected data from december 2002 to july 2009 for ∼80 ms of exposure in the 17-60 kev energy range and found 521 sources (12% unidentified); • the 9-year galactic hard x-ray survey (krivonos et al. 2012) collected data from december 2002 to january 2011 for 132 ms of exposure in the 17-60 kev energy range and reported 402 sources (9% unidentified). 3 identification method in the second semester of 2004 we started an optical spectroscopy campaign performed at ground based telescopes of the northern and southern hemisphere to identify unknown hard x-ray sources detected by integral (masetti et al. 2004, 2006a,b,c,d, 2007, 2008a,b, 2009, 2010, 2012, 2013), and we selected unidentified or unclassified hard x-ray sources that contain, within the ibis 90% confidence level error box, a single bright x-ray object detected either in the rosat all-sky surveys (voges et al. 1999, 2000), or in the slew survey (saxton et al. 2008) and/or in the serendipitous source catalog (watson et al. 2009) of xmm-netwon, or having pointed observations either from chandra, swift/xrt or xmm-netwon satellites. this approach was proven by stephen et al. (2006) to be very effective in associating, with a high degree of probability, ibis sources with a softer x-ray counterpart, in turn drastically reducing the positional error circles to better than a few arcsec in radius, making the search area smaller by a factor of 104. taking into account the hard x-ray characteristics and the global properties of the sources, such as the position in the sky, the 20-100 kev light curve and the broad band spectrum, we can have some clues about their nature. after this first selection, we chose among these objects those that had, within their refined 90% confidence level soft x-ray error boxes, a single possible optical counterpart with magnitude r < 20 in the dss-ii-red survey, so that optical or ir spectroscopy could be obtained with reasonable signal-tonoise ratio using medium-sized telescopes (i.e. with diameter up to 4 meters; masetti et al. 2004, 2006a,b,c,d, 2007, 2008a,b, 2009, 2010, 2012, 2013). 4 galactic sources many important results from the integral mission have been obtained in the observations of the galactic sources. specifically, they have shown the existence of a new class of heavily absorbed x-ray binaries and of the sfxts, doubling the number of known hmxbs and allowed the detection of a substantial number of new magnetic cvs. 4.1 cvs cvs are close binary systems consisting of a late-type (i.e. red dwarf) star trasferring material onto a white dwarf (wd) via roche lobe overflow. those which have a magnetic field are called magnetic cvs and fall into two categories: • polar cvs have a strong magnetic field (b > 107 g); their accretion does not occur via accretion disc and the accreting material is channeled by the magnetic field along its lines and falls on the magnetic poles of the wd; • intermediate polars (warner 1995), instead, have a weaker magnetic field (b ∼ 106 − 107 g) that truncates the accretion disc in the inner region close to the magnetosphere, resulting in an accretion curtain, where the accreting material follows the magnetic field lines down to the wd poles. if the wd is not magnetic the accreting material flows towards the wd through an accretion disc. up to now the cvs detected by integral are 35 (∼ 80% are magnetic, mostly intermediate polars), and 29 of these have been identified through optical or nir spectroscopy. this is an important result, if we consider that before integral very few cvs have been detected at high energies. fig. 1 shows the cvs distribution in the sky (white filled circles superimposed on an ibis 20-100 kev image). figure 1: distribution of cvs (white filled circles) in the 20-100 kev sky imaged by ibis. 241 pietro parisi 4.2 low mass x-ray binaries low mass x-ray binaries (lmxbs) are systems consisting of an accreting compact object (neutron star or black hole) and a low-mass (< 1 m�) main-sequence or slightly evolved late-type star. the low mass companion fills and overflows its roche lobe, therefore accretion of matter always occurs through the formation of an accretion disc. up to now ∼ 100 lmxbs have been detected by integral, and only 15 have been classified through optical or nir spectroscopy, this means that almost all the lmxbs have been detected and very few are found among unidentified integral sources. in fig. 2 we report the lmxbs distribution (white filled circles superimposed on an ibis 20-100 kev image): it is clear that they lie in the galaxy bulge or in globular clusters, where we the majority of old stellar populations are located. figure 2: distribution of lmxbs (white filled circles) in the 20-100 kev sky imaged by ibis. they are segregated in the galactic bulge and in globular clusters. 4.2.1 symbiotic x-ray binaries three of the lmxbs spectroscopically identified among unidentified objects are symbiotic x-ray stars (syxbs). they are part of a small subclass of lmxbs in which the compact object (generally a neutron star), receives matter from a red giant rather than from a late-type companion star on the main sequence. compared to lmxbs they show an optical continuum typical of a red giant of m spectral type, with balmer series generally in absorption (of the 7 syxbs known only one, gx 1+4, shows hα in emission, because the donor star is a red supergiant star that fills its roche lobe, accreting matter via accretion disc) and with the presence of absorption bands, and matter is accreted via stellar wind from the donor star. 4.3 hmxbs the galactic plane scans performed with integral revealed a wealth of new hmxbs. these binary systems are composed of a compact object (neutron star or black hole) orbiting and accreting matter from a luminous early spectral type ob high mass (> 10 m�) companion star. hmxbs have different ways to accrete matter: • via roche lobe overflow, but we know only very few cases of this type; • star with a circumstellar disc: the compact objects with a wide eccentric orbit crosses the decretion disc produced by a rapidly rotating be iii/iv/v star, producing accretion through stellar wind; • a massive star (supergiant i/ii star) ejects a fast and dense radially outflowing wind, and the compact object directly accretes from it. up to now ∼ 90 hmxbs have been detected by integral; of these, 45 were identified through optical or nir spectroscopy. this class of objects is distributed along the galactic plane (see fig.3). if we also consider the hmxbs distances, we note that they closely trace the underlying distribution of the massive starforming regions that are expected to produce the progenitor stars of hmxbs (bodaghee et al. 2012). figure 3: distribution of hmxbs (white filled circles) in the 20-100 kev sky imaged by ibis. they lie along the galactic plane. 4.3.1 sfxts this is a new class of transient hmxbs discovered by integral. the sfxts host a massive blue supergiant star (ob) and a compact object, mainly a neutron star. they have fast x-ray flares, from few hours to few days duration, with luminosity of ∼1036-1037 erg s−1; they also have short duty cycles (tinflare/ttotal=0.05% 3%) the accretion mechanism is not clear yet. there are different scenarios, such as the clumpy wind (negueruela et al. 2008, ducci et al. 2009) or the centrifugal/magnetic barrier (bozzo et al. 2008). the clumpy wind scenario has two possible configurations: a neutron star orbiting a supergiant star on a circular orbit, or on an eccentric orbit, accreting 242 unveiling the nature of integral objects: a review from the clumpy stellar wind of the supergiant. in the centrifugal/magnetic barrier scenario, a magnetic barrier or a centrifugal barrier can sets in, and according to the spin period and the strength of the magnetic field of the neutron star, it can cause or not the inhibition of accretion. up to now the sfxts optically or nir identified are ∼10 and other ∼10 are candidates. 5 extragalactic objects the integral satellite has been able to obtain also important results in the field of extragalactic objects. observations are giving fundamental insights into the study of agns located in the zone of avoidance along the galactic plane (see fig. 4 for the agns distribution in the sky) but also positioned across the whole sky. figure 4: distribution of agns (white filled circles) in the 20-100 kev sky imaged by ibis. this is an ibis 20-100 kev image. 5.1 seyfert galaxies the most common extragalactic objects detected by integral are seyfert galaxies; their luminosity ranges from 1042 to 1045 erg s−1, they are located in the nearby universe (z < 0.5) and have an optical spectrum characterized by emission lines. all the seyferts show narrow high ionization emission lines, such as [oiii] or [nii] forbidden emission lines. some show broad permitted lines in emission (generally balmer series), suggesting the presence of a dense and fast moving gas: we call these seyfert 1 galaxies. in these objects, according to the unified model, our line of sight intercepts both broad line regions and narrow line regions. those agns with only narrow emission lines are instead named seyfert 2 galaxies. according to the unified model, in these sources our line of sight intercepts only the narrow line region due to the presence of a torus which hides the broad line region. these gas and dusty regions are photoionized by the central engine; blrs are confined to sub-pc scales around an accretion disk, producing kinematically broadened emission lines with typical velocities of 103–104 km s−1, nlrs are characterized by narrow-lines with typical velocities of 102–103 km s−1 and can span over kpc scales, which are comparable to the size of the bulge or even the entire galaxy. up to now 148 agns detected by integral have been identified through optical and nir spectroscopy. in particular, 68 agns are seyfert 1, while 55 are seyfert 2 galaxies. 5.1.1 narrow-line seyfert 1 these galaxies are peculiar seyfert 1 agns (osterbrock & pogge 1985) with a full width at half maximum (fwhm) of the hβ emission line smaller than 2000 km s−1, with permitted lines which are only slightly broader than the forbidden ones, with a [oiii]5007/hβ ratio < 3, and finally with evident feii and other highionization emission-line complexes (e.g. see fig. 5). a few nls1 galaxies have been discovered so far by integral and recognized as such by optical spectroscopy. figure 5: optical spectrum (not corrected for the intervening galactic absorption) of a typical narrow-line seyfert 1. the main spectral features are labeled. 5.2 low ionization nuclear emission-line regions low ionization nuclear emission-line regions (liners; heckman 1980) are peculiar agns with a level of activity much smaller than that in classical agns and in which some low-ionization lines ([oii]3723, [oi]6300, and [nii]6584) are stronger than in typical seyfert 2 galaxies; the permitted emission-line luminosities are weak; and the emission-line widths are comparable with those of type 2 agns (see fig. 6). according to heckman (1980), liners have [oii]3723 > [oiii]5007 and [oi]6300 > 1/3 [oiii]5007, and often [nii]6584/hα > 0.6. 243 pietro parisi figure 6: optical spectrum (not corrected for the intervening galactic absorption) of a typical liner. the main spectral features are labeled. 5.3 x-ray bright optically normal galaxies some integral objects show a continuum typical of a normal galaxy, dominated by absorption lines due to star forming regions, they are x-ray bright, optically normal galaxies (xbongs; comastri et al. 2002), that is, x-ray bright galactic nuclei with no emission lines in their optical spectra (e.g. fig. 7). figure 7: optical spectrum (not corrected for the intervening galactic absorption) of a typical xbong. the main spectral features are labeled. 5.4 blazars using medium-sized telescopes (i.e. tng, eso), we are also able to identify and classify sources at high redshifts (> 0.6) detected by integral. they are blazars, distant and powerful agns which are oriented in such a way that a jet expelled from the central black hole is directed at small angles with respect to the observers line of sight. an example is igr j12319-0749 a powerful blazar at z = 3.12 (masetti et al. 2012), the farthest opticallyidentified object of any integral survey and the second furthest of all objects detected by integral. 6 summary and conclusions up to now 273 integral objects have been identified and classified through optical and nir spectroscopy using ground-based telescopes of the northern and southern hemisphere. of these objects, 62% are agns, 36% are x-ray binaries and the remaining 2% are chromospherically active stars. going into details, of the 62% agns, 27.8% are seyfert 1 galaxies, 22% are seyfert 2 agns, 8.5% qsos, 2.9% xbongs and 1.1% are other sources. among the galactic sources (36%), we found that 18% are hmxbs, 12.5% are cvs and 5.5% are lmxbs. the ibis surveys secured the detection of extragalactic sources in the so-called zone of avoidance, which hampers observations in soft x-rays along the galactic plane due to the presence of gas and dust. moreover, these surveys are expanding our knowledge about galactic x-ray binaries, by showing the existence of a new class of heavily absorbed supergiant massive xray binaries (first suggested by revnivtsev et al. 2003), by allowing the discovery and the study of supergiant fast x-ray transients (e.g., sguera et al. 2005, 2006; leyder et al. 2007), by doubling the number of known hmxbs (see walter 2007), and by detecting a substantial number of new magnetic cvs. indeed, the new ibis catalogue (in progress) will offer new spectral and timing information on newly detected sources and an insight on peculiar ones, giving us the unique opportunity to discover new hmxbs and understand the differences among them. references [1] barlow, e. j., knigge, c., bird, a. j., et al. 2006, mnras, 372, 224 doi:10.1111/j.1365-2966.2006.10836.x [2] bird, a. j., bazzano, a., bassani, l., et al. 2010, apjs, 186, 1 doi:10.1088/0067-0049/186/1/1 [3] bodaghee, a., tomsick, j.a., rodriguez, j., et al. 2012, apj, 744, 108 doi:10.1088/0004-637x/744/2/108 [4] bonnet-bidaud, j. m., de martino, d., falanga, m., mouchet, m., & masetti, n., 2007, a&a, 473, 185 244 http://dx.doi.org/10.1111/j.1365-2966.2006.10836.x http://dx.doi.org/10.1088/0067-0049/186/1/1 http://dx.doi.org/10.1088/0004-637x/744/2/108 unveiling the nature of integral objects: a review [5] bozzo, e., falanga, m. & stella, l., 2008, apj, 683, 1031 doi:10.1086/589990 [6] comastri, a., mignoli, m., ciliegi, p., et al. 2002, apj, 571, 771 doi:10.1086/340016 [7] ducci, l., sidoli, l., mereghetti, s., et al. 2009, mnras, 398, 2152 doi:10.1111/j.1365-2966.2009.15265.x [8] heckman, t. m. 1980, a&a, 87, 152 [9] krivonos, r., tsygankov, s., revnivtsev, m., et al. 2010, a&a, 523, a61 [10] krivonos, r., tsygankov, s., lutovinov, a., et al. 2012, a&a, 545, [11] landi, r., bassani, l., dean, a. j., et al. 2008, mnras, 392, 630 doi:10.1111/j.1365-2966.2008.14086.x [12] malizia, a., stephen, j.b., bassani, l., et al. 2009, mnras, 399, 944 doi:10.1111/j.1365-2966.2009.15330.x [13] masetti, n., palazzi, e., bassani, et al. 2004, a&a, 426, l41 [14] masetti, n., mason, e., bassani, l., et al. 2006a, a&a, 448, 547 [15] masetti, n., pretorius, m.l., palazzi, e., et al. 2006b, a&a, 449, 1139 [16] masetti, n., bassani, l., bazzano, a., et al. 2006c, a&a, 455, 11 [17] masetti, n., morelli, l., palazzi, e., et al. 2006d, a&a, 459, 21 [18] masetti, n., landi, r., pretorius, m.l., et al. 2007, a&a, 470, 331 [19] masetti, n., mason, e., morelli, l., et al. 2008a, a&a, 482, 113 [20] masetti, n., mason, e., landi, r., et al. 2008b, a&a, 480, 715 [21] masetti, n., parisi, p., palazzi, e., et al. 2009, a&a, 495, 121 [22] masetti, n., parisi, p., palazzi, e., et al. 2010, a&a, 519, a96 [23] masetti, n., parisi, p., jiménez-bailón, e., et al. 2012, a&a, 538, a123 [24] masetti, n., parisi, p., palazzi, e., et al. 2013, a&a, in press. [25] negueruela, i., torrejon, j. m., reig, p., ribo, m., & smith, d. m. 2008, in a population explosion: the nature & evolution of x-ray binaries in diverse environments. aip conference proceedings, volume 1010, 252 doi:10.1063/1.2945052 [26] osterbrock, d.e., & pogge, r.w. 1985, apj, 297, 166 doi:10.1086/163513 [27] revnivtsev, m. g., sazonov, s. y., gilfanov, m. r., & sunyaev, r. a. 2003, astron. lett., 29, 587 doi:10.1134/1.1607496 [28] saxton r.d., read, a.m., esquej, p., et al. 2008, a&a, 480, 611 [29] sguera, v., barlow, e. j., bird, a.j., et al. 2005, a&a, 444, 221 [30] sguera, v., bazzano, a., bird, a.j., et al. 2006, apj, 646, 452 doi:10.1086/504827 [31] stephen, j.b., bassani, l., malizia, a., et al. 2006, a&a, 445, 869 [32] ubertini, p., lebrun, f., di cocco, g., et al. 2003, a&a, 411, l131 [33] voges, w., aschenbach, b., boller, t., et al. 1999, a&a, 349, 389 [34] voges, w., aschenbach, b., boller, t., et al. 2000, iau circ. 7432 [35] walter, r. 2007, ap. space sci., 309, 5 doi:10.1007/s10509-007-9477-9 [36] warner, b. 1995, cataclysmic variable stars (cambridge: cambridge university press) doi:10.1017/cbo9780511586491 [37] watson, m.g., schroder, a.c., fyfe, d., et al. 2009, a&a, 493, 339 discussion pieter meintjes: the novalike cataclysmic variable ae aquarii has been detected by suzaku above 10 kev, showing evidence of non-thermal emission. has it been detected by integral as well? pietro parisi: the cataclysmic variable ae aquarii has not been observed by integral. 245 http://dx.doi.org/10.1086/589990 http://dx.doi.org/10.1086/340016 http://dx.doi.org/10.1111/j.1365-2966.2009.15265.x http://dx.doi.org/10.1111/j.1365-2966.2008.14086.x http://dx.doi.org/10.1111/j.1365-2966.2009.15330.x http://dx.doi.org/10.1063/1.2945052 http://dx.doi.org/10.1086/163513 http://dx.doi.org/10.1134/1.1607496 http://dx.doi.org/10.1086/504827 http://dx.doi.org/10.1007/s10509-007-9477-9 http://dx.doi.org/10.1017/cbo9780511586491 introduction surveys identification method galactic sources cvs low mass x-ray binaries symbiotic x-ray binaries hmxbs sfxts extragalactic objects seyfert galaxies narrow-line seyfert 1 low ionization nuclear emission-line regions x-ray bright optically normal galaxies blazars summary and conclusions 116 acta polytechnica ctu proceedings 2(1): 116–122, 2015 116 doi: 10.14311/app.2015.02.0116 inner disk structure of dwarf novae in the light of x-ray observations ş. balman1 1middle east technical university, department of physics, inonu bulvarı, ankara, 06531, turkey corresponding author: solen@astra.physics.metu.edu.tr abstract diversity of the x-ray observations of dwarf nova are still not fully understood. i review the x-ray spectral characteristics of dwarf novae during the quiescence in general explained by cooling flow models and the outburst spectra that show hard x-ray emission dominantly with few sources that reveal soft x-ray/euv blackbody emission. the nature of aperiodic time variability of brightness of dwarf novae shows band limited noise, which can be adequately described in the framework of the model of propagating fluctuations. the frequency of the break (1-6 mhz) indicates inner disk truncation of the optically thick disk with a range of radii (3.0-10.0)×109 cm. the rxte and optical (rtt150) data of ss cyg in outburst and quiescence reveal that the inner disk radius moves towards the white dwarf and receeds as the outburst declines to quiescence. a preliminary analysis of su uma indicates a similar behaviour. in addition, i find that the outburst spectra of wz sge shows two component spectrum of only hard x-ray emission, one of which may be fitted with a power law suggesting thermal comptonization occuring in the system. cross-correlations between the simultaneous uv and x-ray light curves (xmm −newton) of five dne in quiescence show time lags in the x-rays of 96-181 sec consistent with travel time of matter from a truncated inner disk to the white dwarf surface. all this suggests that dwarf novae and other plausible nonmagnetic systems have truncated accretion disks indicating that the disks may be partially evaporated and the accretion may occur through hot (coronal) flows in the disk. keywords: cataclysmic variables white dwarfs accretion, accretion dics stars: binaries x-rays: stars radiation mechanisms: thermal stars: dwarf novae. 1 introduction dwarf novae (dne) are a class of cataclysmic variables (cvs) which are interacting compact binaries in which a white dwarf (wd, the primary star) accretes matter and angular momentum from a main (or post-main) sequence star (the secondary) filling its roche-lobe. the matter is transferred by means of an accretion disk that is assumed to reach all the way to the wd surface. ongoing accretion at a low rate (quiescence) is interrupted every few weeks to months or sometimes with longer durations by intense accretion (outburst) of days to weeks where ṁ increases (see warner 1995 for a review). the material in the inner disk of nonmagnetic cvs initially moving with keplerian velocity dissipates its kinetic energy in order to accrete onto the slowly rotating wd creating a boundary layer (bl) (see mauche 1997, kuulkers et al. 2006 for an overview). standard accretion disk theory predicts half of the accretion luminosity to originate from the disk in the optical and ultraviolet (uv) wavelengths and the other half to emerge from the boundary layer as x-ray and/or extreme uv (euv)/soft x-ray emission which may be summerized as lbl∼ldisk=gmwdṁacc/2rwd=lacc/2 (lyndenbell & pringle 1974, godon et al. 1995). during low-mass accretion rates, ṁacc<10−(9−9.5)m�, the boundary layer is optically thin (narayan & popham 1993, popham 1999) emitting mostly in the hard xrays (kt∼10(7.5−8.5) k). for higher accretion rates , ṁacc≥10−(9−9.5)m�, the boundary layer is expected to be opticallly thick (popham & narayan 1995) emitting in the soft x-rays or euv (kt∼10(5−5.6) k). the transition between an optically thin and an optically thick boundary layer, also depends on the mass of the white dwarf (also rotation) and on the alpha viscosity parameter. 2 x-ray observations of dwarf novae in quiescence and outburst the quiescent x-ray spectra are mainly characterised with a multi-temperature isobaric cooling flow model of plasma emission at tmax=6-55 kev with accretion rates of 10−12-10−10 m� yr−1. the x-ray line spectroscopy indicates narrow emission lines (brightest oviii kα) and near solar abundances, with a 6.4 kev line expected to be due to reflection from the surface of the wd. the detected doppler broadening in lines during quies116 http://dx.doi.org/10.14311/app.2015.02.0116 inner disk structure of dwarf novae in the light of x-ray observations cence is <750 km s−1 at sub-keplerian velocities in the boundary layer with electron densities >1012 cm−3 (see baskill et al. 2005, kuulkers et al. 2006, rana et al. 2006, pandel et al. 2005, balman et al. 2011, balman 2012). the total x-ray luminosity during quiescence is 1029 -1032 erg s−1. lack of bl emission in the xrays have been suggested due to low lx/ldisk ratio (see kuulkers et al. 2006). it has been suggested for dn in quiescence that if the wd emission is removed and some disk truncation is allowed, this ratio is ∼1 (pandel et al. 2005). dn outbursts are brightenings of the accretion disks as a result of thermal-viscous instabilities summerized in the dim model (disc instability model; lasota 2001,2004). during the outburst stage, dn x-ray spectra differ from the quiescence since the accretion rates are higher (about two orders of magnitude), the bl is expected to be optically thick emitting euv/soft xrays (lasota 2001, see the x-ray review in kuulkers et al. 2006). on the other hand, soft x-ray/euv temperatures in a range 5-25 ev are detected from only about five systems (e.g., mauche et al. 1995, mauche & raymond 2000, long et al. 1996, mauche 2004, byckling et al. 2009). as a second and more dominantly detected emission component, dn show hard x-ray emission during the outburst stage however, at a lower flux level and x-ray temperature compared with the quiescence (e.g., ww cet & su uma: collins & wheatley 2010, fertig et al. 2011, ss cyg: wheatley et al. 2003, macgowen et al. 2004, ishida et al. 2009). on the other hand, some dn show increased level of x-ray emission (gw lib & u gem: byckling et al. 2009, guver et al. 2006). the total x-ray luminosity during outburst is 1030 -1034 erg s−1. the grating spectroscopy of the outburst data indicate large widths for lines with velocities in excess of 1000 km s−1 mostly of h and he-like emission lines (c,n,o,ne, mg, si, fe, ect.) (mauche 2004, rana et al. 2006, okada et al. 2008). a characteristic of some dn outburst light curves are the uv and x-ray delays in rise to outburst (w.r.t. optical) indicating possible disk truncation ((meyer & meyer-hofmeister 1994 and references therein) . these delays are a matter of several hours (upto a day) that need dedicated simultaneous multi-wavelength observations. during outburst no eclipses are detected in the eclipsing systems (particularly of soft x-ray emission) or no distinct orbital variations are seen. (e.g., pratt et al. 1999, byckling et al. 2009). note that both in ss cyg (mc gowan et al. 2004) and in su uma (collins & wheatley 2010) the x-ray flux in between outbursts have been found to decrease as opposed to expectations of the dim model. wz sge is a short period su uma type dwarf nova with long interoutburst interval of 20-30 yrs. the system is believed to show no normal outbursts but only superoutbursts. the most recent outburst in julyaugust 2001 (previous outbursts in 1978, 1946 and 1913) was observed from ground and space over several different wavelength bands including the x-ray wavelengths and the euv using the chandra observatory (see wheatley & mauche 2005, kuulkers et al. 2002). there has been three letg (low energy transmission grating) and three acis-s (advanced camera imaging specreometer) observations obtained in the continuousclocking (cc) mode. i report a preliminary analysis on the spectral fitting of the acis-s cc-mode data. figure 1: chandra x-ray outburst spectra of wz sge in 0.3-10.0 kev range obtained with acis-s (ccmode). the observation days after the outburst are labeled on each spectrum. the spectra and response files were prepared in a standard way (task specextract is used) by choosing the source and the background photons using a suitable extraction box (10 arcsec in size) on the data strip using ciao 4.4 and the caldb 4.4.8 (see http://cxc.harvard.edu/ciao/). for further analysis, heasoft version 6.13 is utilized. the spectra were fitted with the multi-temperature plasma emission models (e.g., cevmkl in xspec, see http://heasarc.nasa.gov/xanadu/xspec/) according to the expections from earlier work of dn analysis in quiescence and outburst. cevmkl model is a multitemperature plasma emission model (built from mekal code, mewe et al. 1986) where emission measures follow a power-law in temperature (dem = (t/tmax)α−1 dt/tmax). the reduced χ2 of the fits were above a value of 2 with either a single mekal model or cevmekl alone (the α parameter of the power law distribution of temperatures is set free) for days 6, 15, 30 after outburst. i added a second component of a power law which reduced the χ2 values to desirable levels. in general, the plasma has variable abundance of n,o,ne,fe, and s. the spectral parameters for day 6 after the outburst were ktmax=0.7-1.3 kev with a photon index of γ=0.8-1.4. the x-ray flux of the ther117 ş. balman mal cevmkl component was 1.1×10−11 erg s−1 cm−2 and lcevmkl is 2.7×1030 erg s−1 where the power law component has 5.8×10−12 erg s−1 cm−2 and lpower is 1.3×1030 erg s−1 (43.5 pc is assumed, harrison et al. 2004). the parameters for day 15 were ktmax=0.5-1.5 kev and γ=0.2-1.1. between these two dates the x-ray flux of the cevmkl component decreased by 2 and the power law component inceased by about 1.4 . for day 30 ktmax=1.2-3.0 kev and γ=1.5-2.0. therefore, the x-ray emitting region gets hotter and the photon index decrease. the x-ray fluxes recover to day 6. the final observation on day 58 which is almost quiescence after the outburst shows ktmax=26-46 kev and no power law emission is detected. the x-ray flux is the highest 4.4×10−11 erg s−1 cm−2 and lx is 1.1×1031 erg s−1 (at 43.5 pc). all ranges correspond to 90% confidence level errors. the neutral hydrogen absorption has stayed at the interstellar level in all fits within errors. no optically thick blackbody emission is detected and only x-ray suppression of the quiescent emission is observed just like some other dn. the x-ray temperatures on days 6-30 are in good agreement with the letg results as well. a model of three additive mekals yield acceptable fits on days 6-30, however allowing for very high x-ray tempartures. a partial covering absorber model improves the cevmkl fits, however the high intrinsic absorption when modeled yields inconsistent count rates for the letg observations. 3 inner disk structure using eclipse mapping techniques flickering is a fast intrinsic brightness scintilation occurring on time scales from seconds to minutes (e.g., amplitudes of 0.01 1 mag in the optical). it is observed in all accreting sources. eclipse mapping methods have been used to reproduce the spatial distribution of flickering in cvs in the optical and uv wavelengths. some eclipse mapping studies of flickering in quiescent dwarf novae indicate that mass accretion rate diminishes by a factor of 10-100 and sometimes by 1000 in the inner regions of the accretion disks as revealed by the brightness temperature calculations which do not find the expected r−3/4 radial dependence of brightness temperature in standard steady-state constant mass accretion rate disks (see e.g., z cha and oy car: wood 1990, v2051 oph: baptista & bortoletto 2004, v4140 sgr: borges & baptista 2005). biro (2000) finds that this flattening in the brightness temperature profiles may be lifted by introducing disk truncation in the quiescent state (e.g., r ∼ 0.15rl1 ∼4×109 cm; dw uma, a nova-like). a comprehensive uv modeling of accretion disks at high accretion rates in 33 cvs including many nova-likes and old novae (puebla et al. 2007) indicate an extra component from an extended optically thin region (e.g., wind, corona/chromosphere) evident from the strong emission lines and the p cygni profiles. this study also indicates that the mass accretion rate may be decreasing 1-3 orders of magnitude in the inner disk region (divergence starts r≤ afew ×1010 cm towards the wd). 4 inner disk structure of dwarf novae the truncation of the optically thick accretion disk in dne in quiescence was invoked as a possible explanation for the time lags between the optical and uv fluxes in the rise phase of the outbursts (meyer & meyerhofmeister 1994), and for some implications of the dim (see lasota 2001, 2004) or due to the unusual shape of the optical spectra or light curves of dne (linell et al. 2005, kuulkers et al. 2011). theoretical support for such a two-phase flow was given by a model of the disk evaporation of (meyer & meyer-hofmeister 1994). this model was later elaborated to show that the disk evaporation (coronal “syphon” flow) may create optically thick-optically thin transition regions at various distances from the wd (liu et al. 1997, mineshige et al. 1998). 4.1 propagating fluctuations model another diagnostic tool proposed to study the inner disk structure in accreting objects is the aperiodic variability of brightness of sources in the x-rays. while the long time-scale variability might be created in the outer parts of the accretion disk (warner & nather 1971), the relatively fast time variability (at f >few mhz) originates in the inner parts of the accretion flow (bruch 2000; baptista & borteletto 2004). properties of this noise is similar to that of the x-ray binaries with neutron stars and black holes. now, the widely accepted model of origin for this aperiodic flicker noise is a model of propagating fluctuations (lyubarskii 1997, churazov et al. 2001, uttley & mchardy 2001, revnivtsev et al. 2009,2010, uttlet et al. 2011, scaringi et al. 2012).the modulations of the light are created by variations in the instantaneous value of the mass accretion rate in the region of the energy release. these variations in the mass accretion rate, in turn, are inserted into the flow at all keplerian radii of the accretion disk due to the stochastic nature of its viscosity and then transferred toward the compact object. thus, variations are on dynamical timescales. this model predicts that the truncated accretion disk should lack some part of its variability at high fourier frequencies, i.e. on the time scales shorter than a typical time scale of variability. 118 inner disk structure of dwarf novae in the light of x-ray observations 4.2 broad-band noise of dwarf novae a recent work by balman & revnivtsev (2012) have used the broad-band noise characteristic of selected dn in quiescence (only one in outburst: ss cyg) and studied the inner disk structure and disk truncation via propagating fluctuations model. the power spectral densities (pds) expressed were calculated in terms of the fractional rms amplitude squared following from (miyamoto et al. 1991). the light curves were divided into segments using 1-5 sec binning in time and several pds were averaged to create a final pds of the sources. the white noise levels were subtracted hence leaving us with the rms fractional variability of the time series in units of (rms/mean)2/hz. next, the rms fractional variability per hertz was multiplied with the frequencies to yield νpν versus ν. for the model fitting a simple analytical model is used p (ν) ∝ ν−1 ( 1 + ( ν ν0 )4 )−1/4 , which was proposed to describe the power spectra of sources with truncated accretion disks (see revnivtsev et al. 2010,2011). the broad-band noise structure of the keplerian disks often show ∝ f−1...−1.3 dependence on frequency (churazov et al. 2001, gilfanov et al. 2005), and this noise will show a break if the optically thick disk truncates as the keplerian motion subsides. balman & revnivtsev (2012) show that for five dn systems, ss cyg, vw hyi, ru peg, ww cet and t leo, the uv and x-ray power spectra show breaks in the variability with break frequencies in a range 1-6 mhz, indicating inner disk truncation in these systems. the truncation radii for dn are calculated in a range ∼(310)×109 cm including errors (see table 2 in balman & revnivtsev 2012). the same authors used the archival rxte data of ss cyg in quiescence and outburst listed in table 1 of their paper to derive the broad-band noise of the source in different states (i.e., accretion rates). for the outburst phases, authors investigated times during the x-ray suppression (e.g., the x-ray dips; optical peak phases of the outburst) and the x-ray peak. this, in turn is expected to indicate the motion of the flow in the inner regions of the disk and the geometry of the inner disk. authors show that the disk moves towards the white dwarf during the optical peak to ∼ 1×109 cm and receeds as the outburst declines to quiescence to 5-6×109 cm. this is shown for a cv, observationally, for the first time in the x-rays (see figure 2). this is also supported with the optical data analysis of ss cyg in quiescence and outburst (revnivtsev et al. 2012) 4.3 x-ray and uv light curve cross-correlations balman & revnivtsev (2012) calculated the crosscorrelation between the two simultaneous light curves (x-ray and uv), using the archival xmm -newton epic pn and om data utilizing heasoft task crosscor. to obtain the ccfs (cross-correlation functions), datasets were divided into several pieces using 1-5 sec binning in the light curves and fitted the resulting ccfs with double lorentzians since it was necessary for adequate fitting (see the paper for details). the ccfs for all the dne show clear asymmetry indicating that some part of the uv flux is leading the x-ray flux. in addition, they detect a strong peak near zero time lag for ru peg, ww cet and t leo, suggesting a significant zero-lag correlation between the x-rays and the uv light curves. figure 2: the rxte pds of ss cyg in quiescence and during the optical peak of outburst (top). the solid lines show the fit with the propagating fluctuations model along with two lorentzians. the same authors also calculated the crosscorrelation between the simultaneous uv and x-ray light curves by subtracting the zero time lag components in the five dne pds, yielding more correct time lags consistent with delays in the x-rays of 96-181 sec (see the paper on details of the modeling). the lags occur such that the uv variations lead x-ray variations which shows that as the accreting material travels onto the wd, the variations are carried from the uv into the x-ray emitting region. therefore, the long time lags of the order of minutes can be explained by the travel time of matter (viscous flow) from a truncated inner disk to the white dwarf surface. zero time lags (∼ light travel time) indicate irradiation effects in these systems since we do not have resolution better than 1 sec. 119 ş. balman figure 3: see figure 10 in balman & revnivtsev (2012). the cross-correlation of the epic pn (x-ray) and om (uv) light curves with 1 sec time resolution. the two-component lorenzian fits are shown as solid black lines (except for ss cyg). figure 4: the rxte pds of su uma in quiescence and in optical outburst is displayed (top panel). xmm newton epic pn pds of v426 oph and ht cas in quiescence (middle and bottom panel). the solid lines are the fits with the propagating fluctuations model. an analysis on the rxte data of su uma in quiescence and outburst following six consecutive outburts reveal a similar broad-band noise structure to ss cyg in quiescence showing a break frequency ∼ 5.5-7.5 mhz with a truncated optically thick disk ∼ 3.8×109 cm. the preliminary analysis of the outburst data during the x-ray suppression episodes (optical peak of the outburst) indicates no disk truncation or a truncation around 0.1 hz (see figure 4). therefore, su uma indicates a similar behaviour of the disk during the outburst to ss cyg where the inner disk moves in almost all the way to the wd during the optical peak and moves out in decline to quiescent location further out. the lower level of broadband noise during outburst stage of su uma may be due to the high radiation pressure support of an optically thick disk flow during the peak of the outburst suppressing the variations. a similar pds analysis of the xmm -newton data of the dne, v426 oph and ht cas in quiescence reveals break frequencies 4.6-2.6 mhz and 7.2-2.8 mhz, respectively. the approximate keplerian radii where the optically thick disk truncates is ∼ 6.2×109 cm and ∼ 4.5×109 cm, respectively (see figure 4). 5 conclusions studies of dne broad-band noise characteristics in the x-rays (see also balman & revnivtsev 2012) indicate that dne have truncated accretion disks in quiescence detected in at least 8 systems in a range ∼(3.0-10.0)×109 cm including errors. the magnetic cvs (mcvs) show rather smaller truncation radii (0.9120 inner disk structure of dwarf novae in the light of x-ray observations 2.0)×109 cm (revnivtsev et al. 2010, 2011). this can also explain the uv and x-ray delays in the outburst stage and the accretion may occur through hot (coronal) flows in the disk. note that extended emission and winds are detected from dn in the outburst stage which may be an indication of the coronae/hot flows in these systems (e.g., mauche 2004). time delays detected in a range of 96-181 sec, are also consistent with matter propogation timescales onto the wd in a truncated nonmagnetic cv disk in quiescence. balman & revnivtsev (2012) approximate an α of 0.1-0.3 for the inner regions of the dne accretion disks in quiescence. in addition, the outburst spectra of wz sge shows two component spectrum of only hard x-ray emission, one of which may be fitted with a power law suggesting thermal comptonization of the optically thick disk photons or scattering from an existing wind during the outburst. the spectral evolution and disapearance of the power law component after outburst may support this issue and that the accretion disk goes back to its quiescent truncated structure and comptonization stops. a general picture of the accretion flow around a wd in quiescence thus might be somewhat similar to that of the black hole/neutron star accretors with an optically thick colder outer accretion disk and an optically thin hot flow in the inner regions where the truncation occurs (see esin et al. 1997, done et al. 2007). the appearance of a hot flow (e.g., adaf-like) in the innermost regions of the accretion disk will differ from that of ordinary rotating keplerian disk because it is no longer fully supported by rotation, but might have a significant radial velocity component with sub-keplerian speeds. it is important to monitor dne in the x-rays to measure the variability in the light curves in 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[58] wilms, j., allen, a., & mccray, r. 2000, apj, 542, 914 [59] wood, j. h.: 1990, mnras, 243, 219 122 http://dx.doi.org/10.1086/421438 http://dx.doi.org/10.1086/309489 http://dx.doi.org/10.1086/380758 http://dx.doi.org/10.1038/362820a0 http://dx.doi.org/10.1086/587161 http://dx.doi.org/10.1086/429983 http://dx.doi.org/10.1111/j.1365-2966.2012.20512.x http://dx.doi.org/10.1046/j.1365-8711.2001.04496.x http://dx.doi.org/10.1111/j.1745-3933.2011.01056.x http://dx.doi.org/10.1017/cbo9780511586491 http://dx.doi.org/10.1093/mnras/152.2.219 http://dx.doi.org/10.1111/j.1365-2966.2003.07149.x http://dx.doi.org/10.1086/317016 introduction x-ray observations of dwarf novae in quiescence and outburst inner disk structure using eclipse mapping techniques inner disk structure of dwarf novae propagating fluctuations model broad-band noise of dwarf novae x-ray and uv light curve cross-correlations conclusions 90 acta polytechnica ctu proceedings 1(1): 90–95, 2014 90 doi: 10.14311/app.2014.01.0090 cosmological evolution of the central engine in high-luminosity, high-accretion rate agn matteo guainazzi1 1european space astronomy centre (esac), p.o. box, 78, e-28691 villanueva de la cañada, madrid, spain corresponding author: matteo.guainazzi@sciops.esa.int abstract in this paper i discuss the status of observational studies aiming at probing the cosmological evolution of the central engine in high-luminosity, high-accretion rate active galactic nuclei (agn). x-ray spectroscopic surveys, supported by extensive multi-wavelength coverage, indicate a remarkable invariance of the accretion disk plus corona system, and of their coupling up to redshifts z ' 6. furthermore, hard x-ray (e ∼>10 kev) surveys show that nearby seyfert galaxies share the same central engine notwithstanding their optical classification. these results suggest that the high-luminosity, high accretion rate quasar phase of agn evolution is homogeneous over cosmological times. keywords: active galactic nuclei. 1 outline thanks to its leap in sensitivity by over two orders of magnitude, the medium sensitivity survey carried out by the einstein observatory (emss, maccacaro et al. 1981) collected for the first a statistically sizable sample of extragalactic x-ray sources. studying a sample of 190 extragalactic sources, giovannelli & polcaro (1986) concluded that the observed linear relation between xray luminosity and redshift over several orders of magnitude made evident a physical continuity between the different classes of extragalactic x-ray objects. the sample in giovannelli & polcaro (1986) was a “mixed bag” of different objects: active galactic nuclei (agn), elliptical/s0 galaxies, and spiral/irregular galaxies. while it is now accepted that most of the x-ray emission in inactive galaxies is due to a combination of diffuse inter-stellar medium, halos, and x-ray binaries (see fabbiano 1989 for an early review), there is almost undisputed consensus that the formidable energy output emerging from agn is due to accretion onto super-massive black holes (see, however, the contribution by prof. kundt for a different view). sub-arcsecond resolution imaging with chandra, as well as the unprecedented xmm-newton throughput have made possible a detailed characterisation of the high-energy spectral energy distribution (sed) in large samples of agn, covering a range in luminosity of almost ten orders of magnitudes, and cosmological distances well beyond the peak of the nuclear activity (brandt & hasinger 2005, elvis et al. 2012, pounds 2013). time is ripe to address some fundamental questions on the nature of accretion onto super-massive black holes, that the small size of the emss extragalactic sample left open. in this contribution i will focus on two of them: • do agn share the same engine at all cosmological times? • do agn share the same engine? the answer for all types of agn at all accretion rates would be clearly: “they don’t”. however, similarities in the observational properties of specific subclasses of agn allow us to give these question astrophysically useful positive answers, at least as far as the members of these sub-classes are concerned. in this review i deal with mainstream radio-quiet1, higheddington ratio (ṁ/ ˙medd ∼> 10−2)2 agn. i assume hereby the traditional wisdom separation in bolometric luminosity between seyfert galaxies (l < 1044 erg s−1) and quasars (qso), whenever relevant. the contribution by m.elitzur to these proceedings discusses a central engine unification scheme encompassing also lowluminosity, low-accretion rate systems. 1in this paper, i assume a qualitative definition of radio-quiet (as opposed to radio-loud) agn as those where the contribution of relativistic jets to the optical-to-x-ray spectral energy distribution is negligible. quantitative definitions of agn radio-loudness were introduced by kellermann et al. (1989), miller et al. (1990), and panessa et al. (2007), among others. 2we define the mass accretion rate in units of eddington as: ṁ ≡ ηledd/c 2, where ledd ≡ 4πgmbhmpc, mbh is the black hole mass, mp is the proton mass, c is the speed of light, and η ' 0.1 is the efficiency of gravitational losses into radiation conversion. 90 http://dx.doi.org/10.14311/app.2014.01.0090 cosmological evolution of the central engine in high-luminosity, high-accretion rate agn 2 cosmological evolution of the agn central engine 2.1 direct observables agn are multi-wavelength machines. they emit comparable power per decade frequency from the ir to the γ-ray band (elvis et al. 1994). more importantly for the astrophysical study of accreting super-massive black holes, the bulk of the radiation emitted in each rest-frame energy band carries information on a specific astrophysical process occurring in the nuclear region. uv and x-rays are the most appropriate bands to study spectroscopically the sub-pc scale around accreting massive black holes. in agn accreting at a rate ṁ ∼>10−2 the eddington value the uv emission is dominated by a “blue bump”, believed to be due to thermal emission from the accretion disk (czerny & elvis 1987). the high-energy band is dominated by comptonisation of disk photons by a ∼102 kev temperature corona (zdziarski et al. 1995, perola et al. 2002) with a largely unknown geometry. haardt & maraschi (1991) proposed a “sandwich” geometry embracing the accretion disk. compact coronal geometries have recently experienced a revival following the possible discovery of relativistic light bending (miniutti & fabian 2004) and disk reverberation (fabian et al. 2009) in x-ray observations of nearby seyfert galaxies. uv and x-rays are therefore the natural energy bands where to look for any cosmological evolution of the central engine in luminous agn. in practical terms, metrics accessible to ccd-resolution agn spectra are the intrinsic shape of the x-ray spectrum, parametrised through the photon index γ, which yields information on the corona; and the uv to x-ray flux ratio, parametrised through the αox ∝ log(l2kev /l 2500å ) (tananbaum et al. 1979), which yields information on the disk-corona coupling. for unsaturated comptonisation of non relativistic thermal distributions of electrons, γ ∝ y−1/2, where the comptonisation parameter y ∝ kt × max(τes, τ 2 es), kt is the electron temperature and τes the optical depth for electron scattering (rybicki & lightman 1979). the measurements of the spectral exponential cut-off at energies e ∼ kt would provide a full characterisation of the physical properties of the corona. however, such measurements are accessible only for a handful of x-ray bright nearby agn even in the nustar (harrison et al. 2013) era. other observables probe in principle the innermost regions of the accretion flow, such as the ubiquitous, and black hole mass dependent, x-ray variability (mc hardy et al. 2006, ponti et al. 2012) and the relativistic distortion of x-ray emission lines produced in a x-ray illuminated accretion disk within a few gravitational radii from the innermost circular stable orbit (fabian et al. 1989). these effects are, however, also difficult to measure at high redshift. fig. 1 shows a qualitative scheme of the intrinsic agn uv-to-x-ray sed for reference. figure 1: schematic view of an agn intrinsic uvto-x-ray spectrum. blue: thermal emission from a luminous accretion disk with a temperature at the innermost radius of 30 ev; red: unsaturated comptonisation of soft disk photons with kte=100 kev and τes=1; magenta: reflection from a plane-parallel infinite slab of cold (∼104k) matter (compton continuum plus fe and nickel kα and kβ fluorescent emission lines; after nandra et al. 2007) sizable samples of x-ray selected agn up to redshift '6 have been collected by difference catalogues and surveys: champ (green et al. 2012), chandra deep fields (steffen et al. 2006), 2xmm (watson et al. 2009, young et al. 2009), cosmos (elvis et al. 2012, lanzuisi et al. 2013). they agree in finding no evidence for cosmological evolution of either γ or αox. similar results were obtained by specific observational programs targeting the farthest x-ray selected qso (vignali et al. 2005). the constrains on αox are particularly tight: once its dependency on the luminosity is corrected for, the average of the αox distributions in different redshift bins agree within ±0.1 (steffen et al. 2006). taken as a whole, these results indicate a remarkable invariance of the corona-disk coupling over 90% of the look-back time. 2.2 indirect observables other observables can be used to probe indirectly the nuclear sed: we focus in this section on emission lines in the optical, and in the x-ray band. optical spectroscopy probes the physical condition of gas on a variety of different scales in the nuclear environment: from the broad line regions (blrs) clouds, emitting lines primarily from permitted transitions with widths ∼>2000 km s−1, to the narrow line regions 91 matteo guainazzi (nlrs), emitting lines primarily from forbidden transitions with widths ∼<1000 km s−1. these gaseous systems cover the whole range of distances from the central engine between light-days (peterson et al. 2004) to tens-hundreds of kpc (pogge 1988, 1989a, 1989b). extended nlrs are also copious sources of x-rays (young et al. 2001, bianchi et al. 2006). gas in these regions is photo-ionised by the agn. photo-ionisation models applied to the observed spectra allows one to reconstruct the ionising sed, and even in a few cases the past history of the accreting black hole (dadina et al. 2010). the farthest optically identified agn is ulasj1120+0641 at z = 7.085, a mbh = 2 × 109m� quasar (qso). its optical spectrum is almost indistinguishable from composite spectra of agn at lower redshift (mortock et al. 2011). studies of qso optical spectra at z ≥ 5 indicate no evolution of the metallicity as a function of redshift (juarez et al. 2009). these results suggest that the invariance of the central engine extends to the immediate environs of the accreting black hole up to redshifts '7. due to the combination of high fluorescent yield and abundance, iron kα fluorescent emission line is among the most common spectral features in x-ray spectra of cosmic sources. it is well isolated from transitions due to the closest elements; even at ccd resolution (e/∆e∼40) one can easily resolve fluorescence emission lines from he-like, and h-like recombination lines (statistics permitting). an unresolved component of the neutral iron kα fluorescent line has been detected almost ubiquitously in nearby agn (yaqoob & padmanabhan 2004; nandra 2006). this feature traces reprocessing of the primary nuclear emission by optically thick gas. while this feature is too weak to be detected in x-ray spectra of individual sources at high redshift, spectra stacking techniques allowed the cosmos survey to probe its presence up to redshift z ' 3. fitting these stacked spectra with simple phenomenological continua leaves residuals consistent with neutral iron kα emission (and weaker residuals consistent with recombination lines from heand h-like iron). the equivalent width of such features is independent of redshift (chaudhary et al., 2010; iwasawa et al. 2012), once corrected for the known dependence on the absorption-corrected x-ray luminosity, the so called “iwasawa-taniguchi” effect (iwasawa & taniguchi 1993; bianchi et al. 2007). this result implies a similarity of the primary x-ray sed, as well as of the geometrical configuration and ionisation stage of the reprocessing matter at different cosmological times. 2.3 however, agn do evolve ... these results shall not be interpreted as due to the fact that the agn population as a whole do not evolve! the agn population evolves in density and luminosity over cosmological times (see brandt & hasinger 2005 for a recent review). this may in principle affect the agn population being probed at different redshift by current surveys. hopkins et al. (2008) and hickox et al. (2009) present an evolutionary scenario whereby all agn go through the same evolutionary steps. merging or secular processes (gas instabilities) trigger simultaneously the quasar phase and the growth of the stellar bulge when a galaxy’s dark matter halo reaches a critical mass ∼1012−13 m�. the peak of the quasar phase accreting at high eddington ratio, when massive black holes accrete the bulk of their mass, occurs at different redshifts depending on the mass of the primeval dark mass halo. the whole agn evolutionary sequence would start from a cold gas-rich, rotation dominated galaxy, pass through a dustand optically-thick gas enshrouded phase, evolve into the qso phase, and then to a gradual decline of the agn activity until the galaxy become a “red and dead” elliptical with intermittent radio activity. all these phases would be present in an observed agn sample at any redshift. the qso phase is, however, the best one to probe the conditions of the innermost regions close to the central engine. the discovery of a ∼109m� black hole at z ∼ 7 is puzzling for models of cosmological black hole growth. it is not simple to understand how the required mass could have accreted from seed black holes at z ≥ 10. broadly speaking (see volonteri 2010 for a review) models of seed black hole formation and evolution can be classified as: a) light (mbh ∼102−3 m�) and rapidly accreting seeds forming at very early cosmic time (z '20–50); b) heavy (mbh ∼104−6 m�) and slowly accreting seeds forming at later stages (z '5– 10): c) intermediate seeds between the two cases above. none of these scenarios is free of potential shortcomings (milosavljević et al. 2009; volonteri & begelman 2010). if massive enough (∼>105 m�), electromagnetic signals from these early seeds could be detected by future large observatories. otherwise the detection of gravitational waves produced when compact objects fall onto the seed could provide constraints on a population in the mass range mbh ∼104−7 m�. these topics will be addressed by a future esa’s l-class x-ray mission in the framework of the cosmic vision program, one of whose basic science theme is: “how did the universe originate and what is it made of?” (esa 2005). 3 do really agn share the same engine? so far we have assumed the all agn in the quasar phase at a given time share the same central engine. x-rays provide the ideal wavelength to test this assumption for radio-quiet agn in the local universe. in order to 92 cosmological evolution of the central engine in high-luminosity, high-accretion rate agn understand why, we need to have a closer look at the configuration of gas and dust surrounding the agn central engine, and on how it affects the phenomenological appearance of agn. in sect. 2.2 it was shown that the ubiquitous detection of kα fluorescent emission lines corresponding to neutral or mildly ionised iron (together with the associated continuum compton-reflection “hump”; nandra & pounds 1994) is considered a clear evidence for reprocessing of the primary nuclear emission by optically thick gas in the agn environs. the geometry of this gas structure is controversial. traditional wisdom invoked a compact symmetrical molecular “torus” (antonucci & miller 1985). its azimuthal symmetry would introduce a dependence of the agn observational properties on the line-of-sight to the nucleus. these orientation effects would be primarily (but not exclusively; see nicastro 2000) responsible for the properties of their optical spectra: blrs would be visible only through lines-ofsight not intercepting the torus. for the high reddening expected when radiation passes through the torus clouds (nh > 1022 cm−2) optical broad lines would be suppressed, and only narrow emission lines would be visible (see antonucci 1993 for a review). in this “agn unified scenario” broadand narrow-line agn share the same common engine. hoverer, early simulations (pier & krolik 1992) pointed out that it is difficult to prevent such a structure from gravitationally collapsing on time-scales much shorter than the typical agn duty-cycle (∼>1 gyr). recent models invoke a ”clumpy” model as a solution to this issue (nenkova et al. 2002, 2008). in this framework, the agn classification into broadand narrow-line agn should be reinterpreted in probabilistic terms: even agn seen at very high inclination angles (i.e., for which the traditional unified scenario would predict that they could be only narrow-line agn), would have some probability of being detected as broad-line agn depending on the number, size and dynamics of the torus clouds (eliztur 2012; see also eliztur’s contribution to these proceedings for a discussion of this interpretative scenario). first direct x-ray evidence for the torus clumpiness might have been recently detected in the heavily obscured agn markarian 3 (guainazzi et al. 2012). notwithstanding the detailed structure of the torus, and the consequently corrected interpretation of the unified scenario, there is a tight correlation between optical and x-ray spectroscopic properties in nearby agn: optical “narrow-line” agn exhibit x-ray spectra seen through large column densities of cold photoelectrically absorbing gas (nh ∼> 1022 cm−2; awaki et al. 1991; risaliti 2002); optical “broad-line” agn are x-ray unobscured. exceptions to this rules are '3% in large agn x-ray spectroscopic surveys (mateos et al. 2010), and can be easily explained by variability between non-simultaneous optical and x-ray observations, x-ray obscuration by matter in the host galaxy, or even classification issues in poor-quality optical spectra. one needs to carefully correct for absorption (singh et al. 2011), or observe in energy ranges (as much as possible) unaffected by obscuration to probe the innermost region of agn belonging to different optical classes. the latter avenue have been recently opened by the unprecedented sensitivity achieved by the integral/ibis and the swift/bat instruments above 10 kev. sample of more than 100 nearby agn detected above 10 kev are discussed, among others, by beckmann et al. (2009); ricci et al. (2011), molina et al. (2013) for ibis, and burlon et al. (2012) for bat, respectively. the distributions of γ in samples of x-ray obscured and unobscured agn are consistent within ∆γ ' ±0.1. the distributions of αox remain indistinguishable also when the x-ray luminosity density is calculated in the hard x-ray band (beckman et al. 2009). interestingly enough, ricci et al. (2011) suggested that the reprocessing continuum spectra components are stronger when agn are obscured by a column density 1023 cm−2≤nh≤1024 cm−2. this ingredient does not belong to the 0th order unified scenarios. at this level of obscuration a contribution by blr clouds is likely (elvis et al. 2004; risaliti et al. 2005, 2007; bianchi et al. 2009). while this result is a wise reminder of the intrinsic complexity of gas and dust structures responsible for orientation(and time-)dependent obscuration of the primary continuum, it does not in itself invalidate the basic assumptions of the unified scenario. 4 conclusions in summary: • hard x-ray spectroscopy shows that all (local) high-accretion rate agn share the same central engine notwithstanding the optical classification • uv and x-ray spectroscopy shows that agn in the same phase of their evolution (the high accretion rate, unobscured “quasar phase”) share the same engine up to z ' 6 • optical (blr emission) and x-ray spectroscopy (fe kα fluorescent line) show that the physical properties and geometrical configuration of the circumnuclear gas in highly accreting agn are similar in local and high redshift agn up to z ' 7 the contribution by dr. moshe elitzur to these proceedings discusses aspects of the agn central engine unification encompassing also low-luminosity, lowaccretion rate systems. 93 matteo guainazzi references [1] antonucci r.r.j., miller j.s., 1985, apj 297, 621 [2] antonucci r., 1993, ara&a 31, 473 [3] awaki h., koyama k., inoue h., halpern j.o., 1991, pasj 43, 195 [4] beckmann v., soldi s., ricci c., alfonso-garzón j., et al., 2009, a&a, 505, 417 [5] bianchi s., guainazzi m., chiaberge m., 2006, a&a, 448, 499 [6] bianchi s., guainazzi m., matt g., fonsecabonilla n., 2007, a&a, 467, l19 [7] bianchi s., piconcelli e., chiaberge m., jiménezbailón e., et al., 2009, apj, 695, 781 doi:10.1088/0004-637x/695/1/781 [8] brandt w.n., hasinger g., 2005, ara&a, 43, 827 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done c., smith d., et al., 1995, apj, 438, 63 95 outline cosmological evolution of the agn central engine direct observables indirect observables however, agn do evolve ... do really agn share the same engine? conclusions 94 acta polytechnica ctu proceedings 2(1): 94–98, 2015 94 doi: 10.14311/app.2015.02.0094 supersoft x-ray source cal83: a possible ae aqr-like system a. odendaal1, p. j. meintjes1, p. a. charles2, a. f. rajoelimanana3 1department of physics, university of the free state, p.o. box 339, bloemfontein, 9300, south africa 2school of physics and astronomy, southampton university, southampton so17 1bj 3department of physics, north-west university, private bag x2046, mmabatho 2735, south africa corresponding author: winka@ufs.ac.za abstract cal 83 is a close binary supersoft x-ray source in the large magellanic cloud. a ∼67 s periodicity detected in supersoft x-rays is most probably associated with the spin period of a highly spun-up white dwarf (wd). the variability in the period is ascribed to the obscuration of the wd by the hydrogen burning envelope surrounding it, rotating with a period that is close to, but not quite synchronized with, the wd rotation period. optical spectra obtained with salt exhibit accretion disc emission lines with broad wing structures and p cyg profiles, indicating mass outflows. timing analysis of photometrical observations performed at the south african astronomical observatory (saao) revealed variable signals at ≤1 mhz which are thought to be associated with quasi-periodic oscillations from an accretion disc. the short spin period inferred for cal 83 can be the result of spin-up by accretion disc torques during a long mass transfer history, placing this source on a similar evolutionary track as the cataclysmic variable ae aqr. keywords: stars: individual: cal 83 binaries: close white dwarfs stars: oscillations stars: winds, outflows stars: evolution. 1 introduction supersoft x-ray sources (sss) are highly luminous in the supersoft x-ray band, with >90% of the unabsorbed x-ray flux being below ∼0.5 kev. these sources were first discovered by the einstein x-ray observatory and rosat (see kahabka & van den heuvel (2006) and references therein). van den heuvel et al. (1992) (hereafter vdh92) showed that the low effective temperatures and high luminosities of sss can be explained by the nuclear burning of hydrogen on the surface of a white dwarf (wd) accreting from a binary companion (the close binary sss model). the accretion rate required for steady nuclear burning is ∼ 1− 4× 10−7 m� yr−1. such a high accretion rate can be sustained if the companion mass is comparable to or greater than the wd mass, as this will cause the roche lobe of the donor to shrink and drive mass transfer on the thermal time-scale of the donor. cal 83 is a close binary sss in the large magellanic cloud. however, it is not a persistent x-ray source and several x-ray off-states have been observed, with long-term optical variability anti-correlated with the long-term x-ray variability, as described by e.g. rajoelimanana et al. (2013). these authors also derived a refined orbital period of 1.047529(1) d for cal 83 from ogle-iii photometry. the inclination has been estimated to be in the i = 20 − 30◦ range (see cowley et al. (1998) and references therein, hereafter co98). lanz et al. (2005) used nlte models during a combined analysis of xmm-newton and chandra data, and their results indicate a massive wd (mwd ∼ 1.3± 0.3 m�). schmidtke & cowley (2006) found a periodic signal of 38.4-minutes in the chandra letg data of cal 83, which they ascribed to possible non-radial pulsations in the accreting wd. the optical spectrum of cal 83 is characterized by balmer and he ii accretion disc emission lines (co98 and references therein). the he ii λ4686 emission line has a broad, variable wing structure that has also been observed in some of the balmer lines. in each particular spectrum, these wing structures are either all towards the blue side of the main components of these emission lines, or all towards the red side. according to crampton et al. (1987) (hereafter cr87), this may be associated with the slow precession of an accretion disc with outflows through either wind or a weakly collimated jet. the ∼67 s x-ray periodicity is briefly summarized in §2.1 (a detailed discussion is provided in odendaal et al. 2014). preliminary results of the analysis of optical data are presented in §2.2 and §2.3. after this discussion, the possible evolutionary scenario of cal 83 is brought into context with that of the cv ae aqr in §3, followed by the conclusions in §4. 94 http://dx.doi.org/10.14311/app.2015.02.0094 supersoft x-ray source cal 83: a possible ae aqr-like system 2 cal83: observations and results 2.1 the ∼67 s x-ray pulsation the xmm-newton archive contains 23 observations of cal 83, 4 of which were during an x-ray off-state. a systematic search for short time-scale periodicities that may be associated with the wd spin was performed on the 19 on-state light curves. the starlink period1 package was used to obtain a lomb-scargle (ls) periodogram of each light curve. a power peak at a period of 66.8 ± 0.4 s was discovered at a > 99.9999% significance level in the periodogram of the epic pn light curve of observation 0506531501, and at a lower significance level in 6 of the other pn periodograms. in 3 of these observations, 1 of the mos light curves also exhibited a weak ∼67 s periodicity. the ls periodogram of observation 0506531501, as well as the light curve folded on the 66.8 s period, are shown in fig. 1. 0 10 20 30 40 0 15 30 45 60 75 90 l o m b -s ca rg le p o w er frequency (mhz) 99.73% -0.60 +0.60 7.98 0.0 0.5 1.0 1.5 2.0 c o u n ts s -1 phase figure 1: lomb-scargle periodogram (left) and folded light curve (right) of cal 83 xmm-newton dataset 0506531501 pn. both the periodogram and folded light curve display a significant 66.8 s oscillation. the overall significance of this detection, considering the pn datasets of all 19 the on-state observations, is ≥ 3σ. the detected period exhibits a spread of ±3 s around ∼67 s between different observations, and even within a single observation. this variability cannot be explained by doppler shifts due to wd orbital motion. the long-term presence of the pulsation suggests its association with the wd spin, although the variation in the detected period complicates matters. it is possible, however, that we are observing the wd spin, but through an extended envelope around the accreting wd. according to ibragimov et al. (2003), the photospheric radius in a steady nuclear burning sss may have a radius 2-3 times the radius of the wd itself. the spread in the observed period can possibly be explained by the envelope not being quite synchronized with the wd, resulting in a slippage effect and associated variation in the pulsation period. 2.2 optical spectroscopy with salt a series of optical spectra of cal 83 has been obtained with the robert stobie spectrograph (rss) on the southern african large telescope (salt), using the pg0900 grating to obtain a resolution of r ∼ 1500. these spectra show similar characteristics to those discussed in §1, with strong balmer and he ii emission lines. the velocity widths of these lines indicate emission from regions compatible with an accretion disc around the wd. these lines also exhibit blue wing structures extending to ∼2000 km s−1 from the line centres, supporting the existence of a wind or weakly collimated jet in the system. p cyg profiles are also evident in the hα and hβ lines, serving as further evidence of mass outflow. shown in fig. 2 are the hα and hβ profiles from a spectrum obtained on 2 february 2013. 1000 1250 1500 1750 2000 −5000 −2500 0 2500 c o u n ts velocity (km s −1 ) hβ λ4861 1000 2000 3000 4000 −5000 −2500 0 2500 velocity (km s −1 ) hα λ6563 figure 2: hβ and hα profiles of cal 83, obtained with salt on 2 feb 2013. for mwd ∼ 1.3 m�, the wd radius is rwd ≈ 4 × 108(mwd/1.3 m�)−0.8 cm (see eracleous & horne 1996 and references therein). the mass function can be determined if the semi-amplitude (k1) of a spectral line originating close to the wd is known. although the orbital coverage of the salt spectra was not adequate to calculate a new k1, various values have been reported in the literature. adopting k1 ∼ 35 km s−1, i ∼ 25◦ (see co98) and porb = 1.047529 d, the mass function is 4.7× 10−3 m�, and a secondary mass of m2 ∼ 0.61 m� is obtained, yielding a mass ratio q = m2/mwd ∼ 0.47. however, this value of k1 was derived from the radial velocity modulation of the he ii λ4686 disc emission line, and this line would only represent the wd orbital motion if the he ii emission was distributed symmetrically about the wd. as discussed by e.g. kaitchuck et al. (1994), there are some problems with this assumption, compromising the mass function calculation. 2.3 fast photometry with shoc in april 2013, fast photometrical observations were obtained with one of the sutherland high-speed optical 1www.starlink.rl.ac.uk/star/docs/sun167.htx/sun167.html 95 a. odendaal et al. cameras (shoc2) on the saao 1.9-m telescope at sutherland. these cameras have been commissioned recently, and are optimized for high time resolution photometry. a clear filter was used for the cal 83 observations, and with this sensitive instrument, exposure times in the 0.5-5 s range were adequate, depending on observing conditions. aperture photometry was utilized to obtain light curves, and the cal 83 light curves were corrected by performing differential photometry using 4 comparison stars. the starlink period package was used to perform a ls analysis. the ls periodograms of cal 83 did not reveal any significant pulsation at the inferred spin period of ∼67 s or at higher frequencies. however, some of the cal 83 periodograms exhibited a significant peak in the region just below 1 mhz. these peaks have broadened profiles, and their positions do not stay constant. in fig. 3, the ls periodogram of the shoc observation on 15 april 2013 is presented, showing a peak at 1168± 214 s. the light curve folded on this period is also shown. this observation had a total length of 3245 s, and the light curve was binned to 20 s for this analysis. these peaks are ascribed to quasi-periodic oscillations associated with the accretion disc around the wd. 0 3 6 9 12 15 0 2 4 6 8 10 l o m b -s ca rg le p o w er frequency (mhz) 99.73% -7.650 -7.625 -7.600 -7.575 -7.550 -7.525 0.0 0.5 1.0 1.5 2.0 d if fe re n ti al m ag n it u d e phase figure 3: shoc periodogram and light curve folded on the detected period of 1168± 214 s (obtained on 15 april 2013). these quasi-periods at ≤ 1 mhz may be the keplerian periods of blobs of material orbiting the wd in the accretion disc, or possibly beat periods between the presumed spin period of p∗ ∼ 67 s and blobs orbiting in the inner regions of the disc. assuming that the 1168±214 s periodicity is a keplerian period, the associated keplerian radius is 46rwd. on the other hand, it may be a beat period between p∗ ∼ 67 s and a keplerian period of ∼71 s associated with blobs orbiting at ∼7rwd. adopting the orbital parameters in §2.2 yields a circularization radius of ∼150rwd, supporting the compatibility of both the keplerian radii above with emission from the accretion disc. 3 the evolution of cal83: an ae aqr analogue? ae aqr is a nova-like variable with a short wd spin period (33.08 s), and a long orbital period (9.88 h). a review of the multi-wavelength properties of ae aqr is provided by meintjes, odendaal and van heerden elsewhere in this volume. it has been shown by meintjes (2002) and schenker et al. (2002) that the properties of this source indicate a high mass transfer history, during which ae aqr could have been a supersoft source. during this phase, accretion disc torques would have been able to spin-up the wd to such a short rotation period. the probable association of the ∼67 s period in cal 83 with a short wd spin may place this source on a similar evolutionary path as ae aqr. evidence indicating that cal 83 has already passed through quite a long mass transfer history does indeed exist. the high wd mass, just below the chandrasekhar limit, is one of the factors supporting an extended period of mass accretion. however, with the wd being more massive than the wd in ae aqr, it may be driven over the chandrasekhar limit before entering the cv stage. emission lines of ionized carbon, nitrogen and oxygen are present in the optical and uv spectra of cal 83, and as remarked by cr87, the low ratio of h to he ii and cno lines indicate a donor with an h-poor envelope. therefore the secondary may already have shed most of its envelope during a long period of mass transfer to the wd, with cno cycling resulting in the observed line ratios. assuming that the secondary mass is as low as ∼0.61 m� (see §2.2), the roche lobe of the secondary should be r2 ∼ 1.7 r�. as the secondary has to be in contact with its roche lobe for roche lobe overflow, this implies a donor that is too large for its mass, possibly an evolved star that has lost a large fraction of its envelope, also supporting the long mass transfer history. the thermal time-scale is of the order τth ≤ 5 × 107 (m2/0.61 m�) −2 (r2/1.7 r�) −1 yr (e.g. meintjes 2002 and references therein), while the spin-up timescale corresponding to a ∼1.3 m� wd accreting from a disc extending to its surface is τs−u ≤ 107 yr (e.g. wang 1987). these time-scales are comparable, showing that the wd in cal 83 could have been spun-up to a short spin period if it has been in the supersoft phase with its characteristic high mass transfer rates for a sufficiently long time. to sustain a τ ∼ 107 yr mass transfer, q > 5/6 is required for a conservative process, as described by the vdh92 model. however, evidence indicating significant mass and accompanied angular momentum losses is present in the optical spectra, suggesting a nonconservative mass transfer process. given the possible wd spin period of ∼67 s, the outflow mechanism 96 supersoft x-ray source cal 83: a possible ae aqr-like system may be the ejection of accreting material by a similar magnetospheric propeller mechanism as in ae aqr. for non-conservative mass transfer, the roche lobe will shrink according to the relation ṙl,2 rl,2 = −ṁ2 m2 [ 5 3 − 2 (1− α) q − 2 3 qα 1 + q − 2η m2 (gmwdrcirc) 1/2 jorb ] + 2j̇ j , (1) where α and η represent the fraction of mass and angular momentum transferred through l1 that is lost from the system (e.g. meintjes 2002). therefore, for cal 83, mass transfer that can sustain nuclear burning is perhaps only possible in the phase when the evolved donor is expanding, with significant angular momentum loss contributing substantially in keeping the roche lobe in contact with the donor. this will be explored more quantitatively in the future. 4 conclusion it has been shown that cal 83 exhibits a transient ∼67 s x-ray periodicity. this is expected to be associated with the wd spin period, which would make it one of the shortest known spin periods in the white dwarf binary population. results from optical data support the scenario of accretion through an accretion disc, creating the possibility of the wd being spun-up by disc torques during an extended period of mass accretion, similar to what happened during the evolution of ae aqr. optical spectra also present evidence of mass outflows in cal 83, which can be related to the ejection of accreting blobs from a fast rotating wd magnetosphere or accretion disc winds. however, many questions about this fascinating source still remain unanswered, and detailed follow-up studies are essential. acknowledgement the authors would like to thank the conference organisers for the invitation to present this work. the observations reported here were obtained with xmmnewton, salt (proposal 2012-2-rsa uksc-006), and the saao 1.9-m telescope. the authors would also like to thank the salt team for performing the observations, and marissa kotze for technical support and the use of the shoc pipeline. iraf was also used during the optical data analysis. the financial assistance of the south african ska project towards this research is hereby acknowledged. references [1] cowley a. p., schmidtke p. c., crampton d., hutchings j. b., 1998, apj, 504, 854 [2] crampton d., cowley a. p., hutchings j. b., schmidtke p. c., thompson i. b., liebert j., 1987, apj, 321, 745 [3] eracleous m., horne k., 1996, apj, 471, 427 [4] fender r. p., southwell k., tzioumis a. k., 1998, mnras, 298, 692 doi:10.1134/1.1562213 [5] ibragimov a. a., suleimanov v. f., vikhlinin a., sakhibullin n. a., 2003, astronomy reports, 47, 186 [6] kahabka p., van den heuvel e. p. j., 2006, super soft sources. cambridge university press, new york, pp 461–474 doi:10.1086/192065 [7] kaitchuck r. h., schlegel e. m., honeycutt r. k., horne k., marsh t. r., white ii j. c., mansperger c. s., 1994, apjs, 93, 519 doi:10.1086/426382 [8] lanz t., telis g. a., audard m., paerels f., rasmussen a. p., hubeny i., 2005, apj, 619, 517 doi:10.1046/j.1365-8711.2002.05731.x [9] meintjes p. j., 2002, mnras, 336, 265 doi:10.1093/mnras/stt2111 [10] odendaal a., meintjes p. j., charles p. a., rajoelimanana a. f., 2014, mnras, 437, 2948 doi:10.1093/mnras/stt645 [11] rajoelimanana a. f., charles p. a., meintjes p. j., odendaal a., udalski a., 2013, mnras, 432, 2886 doi:10.1046/j.1365-8711.2002.05999.x [12] schenker k., king a. r., kolb u., wynn g. a., zhang z., 2002, mnras, 337, 1105 [13] schmidtke p. c., cowley a. p., 2006, aj, 131, 600 [14] van den heuvel e. p. j., bhattacharya d., nomoto k., rappaport s. a., 1992, a&a, 262, 97 [15] wang y.-m., 1987, a&a, 183, 257 discussion mariko kato: how do you determine the secondary mass for cal 83? is it really so small? i expect q ≥ 1 to explain anti-correlation with x-ray. alida odendaal: the radial velocity semiamplitude of the he ii λ4686 line was used to calculate 97 http://dx.doi.org/10.1134/1.1562213 http://dx.doi.org/10.1086/192065 http://dx.doi.org/10.1086/426382 http://dx.doi.org/10.1046/j.1365-8711.2002.05731.x http://dx.doi.org/10.1093/mnras/stt2111 http://dx.doi.org/10.1093/mnras/stt645 http://dx.doi.org/10.1046/j.1365-8711.2002.05999.x a. odendaal et al. m2 ∼ 0.61 m�, which is only valid if the he ii emission is uniformly distributed around the wd. this assumption can be highly problematic (e.g. kaitchuck et al. 1994), therefore this approach does not yield a conclusive m2. a more reliable wd radial velocity profile may be obtained by constructing doppler tomograms for the emission lines. margaretha pretorius: is there a radio detection of cal 83? alida odendaal: no, but an upper limit of < 0.12 mjy at 3.5 and 6.3 cm was determined by fender, southwell and tzioumis (1998) from data obtained with the australia telescope compact array. 98 introduction cal83: observations and results the 67 s x-ray pulsation optical spectroscopy with salt fast photometry with shoc the evolution of cal83: an ae aqr analogue? conclusion acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0033 acta polytechnica ctu proceedings 4:33–37, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app impact of the chemical form of in-containment source on fission product release from wwer-1000/v-320 type npp containment during loca adam kecek department of nuclear reactors, faculty of nuclear sciences and physical engineering, czech technical university in prague correspondence: kecekada@fjfi.cvut.cz abstract. nuclear power plant accidents may be followed by a release of fission products into the environment. this release is dependent on several phenomena, such as chemistry, pressure, type of the accident etc. the aim of this paper is to assess the impact of the chemical form of iodine on the fission product release into the environment. keywords: npp, loca, iodine, containment, cocosys, fission products transport, wwer1000/v-320. 1. introduction fission product behaviour and its simulation recently become more important. nuclear power plant accidents in past decades revealed the need of proper definition and calculation of fission product mass entraining the environment. to successfully calculate such phenomena, one has to specify the in-containment source correctly. several different approaches existing up to date vary in the mass, the chemical form or time characteristics. this paper is focused on assessment of the impact of the chemical form of iodine release, which is well known for its extensive range of chemical compounds and reactions within the containment. a fundamental opinion on the complexity of iodine chemistry in the containment during loss-of-coolant accidents can be obtained from fig. 1. used models, codes and brief overview on existing approaches are presented further. 2. description of cocosys the containment code system is a lumped parameter computer code developed and maintained at gesellschaft für reaktorsicherheit (grs mbh). it is used for best-estimate analysis of lightwater reactor containments during severe accidents. the code itself consists of several modules, which calculate all relevant phenomena. the thermal hydraulic (thy) module solves the pressure and temperature build-up history together with mass and energy flow. furthermore it can simulate behaviour of engineering systems like valves, fans, pumps and sprays. a feedback from aerosol and fission products is also considered. the aerosol fission product (afp) module is used to estimate the behaviour and transport of fission products and aerosols within the containment. the core concrete interaction (cci) module provides an investigation of interaction of the molten core with concrete structures during severe accidents. all menfigure 1. scheme of iodine chemistry in npp containment [1]. tioned modules are coupled to provide the desired feedback on relevant phenomena. furthermore, cocosys provides a coupling option with several codes like athlet to simulate primary circuit behaviour or a cfd code for detailed analysis [2]. cocosys has been validated against several validation experiments and is often used in safety analysis of npp concepts and existing power plants including wwer type npps [2]. 3. wwer-1000/v-320 model description the wwer-1000/v-320 type npp containment is a cylindrical shaped building made of pre-stressed 33 http://dx.doi.org/10.14311/ap.2016.4.0033 http://ojs.cvut.cz/ojs/index.php/app adam kecek acta polytechnica ctu proceedings concrete with an inner steel liner. for thermal hydraulic calculations, the inner volume has to be divided into several smaller rooms. the presented model provides an approximation based on 20 volumes, so called nodes, which simulate the real space surrounded by the building. these volumes are connected through junctions providing mass and energy transfer. the walls, floor, ceiling and inner structures are also modeled to provide realistic heat transfer. furthermore the containment spray systems are also modeled. two large nodes (environ and building) simulate the outer volume surrounding the containment. these provide boundary conditions of the problem. the nodalisation of the containment is presented in tab. 1. compartments nodes description e1 environ environment building surrounding buildings iga501 ga501 upper part of the reactor shaft iga301 ga301a lower part of the reactor shaft iga401 ga401a2 spent fuel pools iga701 ga701 reactor hall iasupp cnt-u1 upper section of the building surrounded by the containment wall and steam generator boxes cnt-u2 iasgbox1 sgbox-1 steam generator box 1 iasgbox2 sgbox-2 steam generator box 2 iasmed cnt-m1 middle section of the builcnt-m2 ding at the containment wall iaslow cnt-l1 lower section of the containment building cnt-l2 ga311 ga306-1 ga306-2 ga306-3 iga201 ga201 spray water sump iastl22 tl22p fan system table 1. containment discretization. the simulation of containment leak is maintained by atmospherical junction. this is estimated to follow the limits and conditions of operation of the wwer1000/v-320 type containment. the junction itself is placed in the upper part of the containment connecting the reactor hall and environment. the reason for choosing this position is to simulate shortest and easiest way for ejecting the material from containment into the environment. for calculation of fission product and aerosol behaviour the containment building has to be divided into volumes so-called compartments formed by nodes. thus, compartments provide coarser fragmentation of the containment building. the fragmentation of the containment volume for iodine calculations is presented in tab. 1 and fig. 2. the calculations were done using the afp and thy cocosys computational modules. figure 2. iodine compartment discretization of wwer-1000/v320 npp containment. 4. initial and boindary conditions before the accident, the nuclear power plant is operated at 104 % nominal power. the initiating event is a primary circuit hot leg guillotine rupture at t = 0 s with leak through breaks of equivalent diameter equal to 850 mm (large break loca) into one of the steam generator boxes. moreover, following assumptions are taken into account [3]: • loss of on-site power, • only 1/3 of safety systems in operation (according to conservative approach), • no action expected from operators. the entrainment of fission products into the containment is maintained through the break in the primary hot leg. the ejecting coolant brings the fission products and aerosols released from the core. in accordance with local practice the in-containment source term is based on ref. [4]. following this approach failure of all fuel assembly is expected. in addition, whole fission product mass released into the primary circuit is transferred into the containment. this means that no fission products remain in the primary circuit. the ref. [4] divides the problem of fission product release into two areas, namely normal and core melt. 34 vol. 4/2016 impact of the chemical form of in-containment source the investigated accident does not expect the molten core, so only the pellet-cladding gap inventory is taken into account. the fraction of released fission products is given in tab. 2. fission product pellet-cladding gap fuel melt release release fraction fraction (30–1800 s) (1800–4680 s) i, br 0.05 0.95 xe, kr 0.05 0.35 cs, rb 0.05 0.25 te, sb, se 0.00 0.05 ba, sr 0.00 0.02 ru, rh, pd, mo, 0.00 0.0025tc, co la, zr, nd, eu, 0.00 0.0005nb, pm, pr, sm, y, cm, am ce, pu, np 0.00 0.0002 table 2. fraction of the fission products released during an accident [4]. a research on available in-containment fission product source showed a significant difference between each approach. synchronization efforts on this problem throughout europe pointed out the diversity of the iodine species, the target medium (water, sump or aerosol) and also the fraction of the core inventory released [5]. it has to be mentioned that there is no information on time characteristics of the release. based on this it was decided to test, whether the chemical form and also the target part of the zone has any influence on iodine mass entraining the environment. the time characteristics and fraction released was adopted from ref. [4]. finally, five calculations were done in this sensitivity study, where the distribution of iodine mass varied in chemical form. in addition, the target part of the zone was changed too. overview on all calculations is given in tab. 3. calculation chemical target part iodine mass form of the zone distribution [%] c00 csi atmosphere1 95 i2 4.85 ch3i 0.15 c01 csi atmosphere 0.15 i2 95 ch3i 4.85 c02 csi sump 0.15 i2 95 ch3i 4.85 c03 csi atmosphere 4.85 i2 0.15 ch3i 95 c04 csi sump 4.85 i2 0.15 ch3i 95 table 3. overview on calculated variants. the total mass of fission products in the core is based on values provided in ref. [3]. the total amount of iodine used in this calculation is 22.7 kg. it has to be noted that not all the fission product mass is expected to be radioactive. this study calculates the behavior of the whole mass of iodine entraining the containment. 5. results and comparison the calculations were done for 14 400 s, what equals to 4 hours. this time range was chosen to be representative as the testing calculations showed that the marginal contribution to the mass ejecting the containment during the accident is within first two hours. calculation c04 was neglected due to numerical error. no. description mass [g] deviation from c00 [%] c00 base case (95 % csi, 4.85 % i2, 0.15 % ch3i) a 4.94 × 10−3 0.00 c01 modified iodine mass distribution (95 % i2, 4.85 % ch3i, 0.15 % csi) a 2.33 × 10−2 371.51 c02 modified iodine mass distribution (95 % i2, 4.85 % ch3i, 0.15 % csi) s 4.78 × 10−3 −3.39 c03 modified iodine mass distribution (95 % ch3i, 4.85 % csi, 0.15 % i2) a 1.14 × 10−1 2204.44 c04 modified iodine mass distribution (95 % ch3i, 4.85 % csi, 0.15 % i2) s err err table 4. overview on calculation and results. the trend of the release is in good agreement with all calculations except c03, where almost constant release rate can be observed. the ejected mass in calculations c00 through c02 shows a massive growth of the release within the first hour, then it slows down and in long time view it shows stabilization of the mass entraining the environment. this may be caused by several phenomena, such as sedimentation or wash down of fission products from walls into the sump. the worst case presented in this sensitivity analysis is c03, where the main mass was injected as organic iodine into the atmosphere. it has to be noted that this form is not expected to be a typical contributor to the in-containment source, thus the results seem to be unrealistic. the second worst case is c01, where the iodine in elemental form is injected into the gas part of the zone. this leads to a high release of iodine into the environment. in accordance to ref. [6] the elemental 1the csi aerosol can be injected only into the gas part of the zone. 35 adam kecek acta polytechnica ctu proceedings figure 3. distribution of iodine in the containment (c00–c03, 14 400 s). iodine is one of the main options of iodine mass release into the environment. the base case c00 provided results lower than the two calculations presented before. the mass behaves significantly different as the compound is expected to be in aerosol particle form. the lowest release was calculated for elemental iodine injected into the sump part. this may be caused by high solubility of iodine species. the results are presented in tab. 4 and fig. 4. the distribution within the containment varies for each calculation. in the case of c00 the mass is centralized in the containment sump. this may be induced by the aerosol wash down. the c01 shows significant concentration in the reactor hall. this is probably caused by the chemical form, as the injection was in form of elemental iodine into the atmosphere. furthermore, c02 provides results close to the c00 calculation. the injected iodine might be dissolved in water and then washed down into the containment sump. finally the c03 calculation shows distribution close to the c01. this is again induced by the injection of iodine as a gas. the iodine mass is mainly distributed within the reactor hall. the results of the calculations c00 through c03 at 14 400 s are presented in fig. 3. figure 4. iodine release into the environment (c00–c03, 14 400 s). 36 vol. 4/2016 impact of the chemical form of in-containment source 6. conclusion the presented calculations proved a significant impact of the chemical form of iodine on release into the environment. furthermore the injected phase (water, gas) is also an important factor significantly influencing the ejected mass. future effort should be made on the assessment of the in-containment source, e.g. the time range and the fraction of ruptured fuel assembly. references [1] irsn. the astec software package. http://www.irsn.fr/en/research/ scientific-tools/computer-codes/pages/ the-astec-software-package-2949.aspx. [2] w. klein-heßling, et al. cocosys v2.4 user’s manual. gesellschaft für anlagenund reaktorsicherheit (grs) mbh, 2010. [3] a. kecek. testovací výpočty úniku štěpných produktů z kontejnmentu je temelín v průběhu loca události programem cocosys. tech. rep. z4339, újv, 2016. [4] u.s. nuclear regulatory commission. alternative radiological source terms for evaluating design basis accidents at nuclear power reactors, 2000. regulatory guide 1.183. [5] nuclear fuel behaviour in loss-of-coolant accident (loca) conditions. tech. rep. 6846, nea oecd, 2009. [6] u.s. nuclear regulatory commission. methods and assumptions for evaluating radiological consequences of design basis accidents at light-water nuclear power reactors, 2003. regulatory guide 1.195. 37 http://www.irsn.fr/en/research/scientific-tools/computer-codes/pages/the-astec-software-package-2949.aspx http://www.irsn.fr/en/research/scientific-tools/computer-codes/pages/the-astec-software-package-2949.aspx http://www.irsn.fr/en/research/scientific-tools/computer-codes/pages/the-astec-software-package-2949.aspx acta polytechnica ctu proceedings 4:33–37, 2016 1 introduction 2 description of cocosys 3 wwer-1000/v-320 model description 4 initial and boindary conditions 5 results and comparison 6 conclusion references 113 acta polytechnica ctu proceedings 1(1): 113–117, 2014 113 doi: 10.14311/app.2014.01.0113 star formation as seen by low mass stars nino panagia1,2,3, guido de marchi4 1space telescope science institute, 3700 san martin dr, baltimore md 21218, usa 2inafosservatorio astronomico di capodimonte, salita moiariello 16, i-80131, naples, italy 3supernova ltd, oyv #131, northsound road, virgin gorda, british virgin islands vg1155 4european space agency, keplerlaan 1, 2200 ag noordwijk, netherlands corresponding author: panagia@stsci.edu abstract using the hubble space telescope (hst) we have characterised and compared the physical properties of a large sample of pre-main sequence (pms) stars spanning a wide range of masses (0.5 − 4 m�), metallicities (0.1 − 1 z�) and ages (0.5−30 myr). this is presently the largest and most homogeneous sample of pms objects with known physical properties. the main results of this ongoing study are briefly summarised here. keywords: star formation solar mass stars magellanic clouds milky way photometry. with a group of european colleagues, whose names are listed in the acknowledgments, we have undertaken a systematic study of the star formation process in the milky way and magellanic clouds (mcs), with special emphasis on moderate mass stars, say 0.5 to 4 m�. our motivations are: i) stars in this range account for most of the star formation in a galaxy, e.g. more than 65% for a salpeter initial mass function (imf); ii) low mass stars can form in small parent clouds as well as in big ones; iii) as a consequence, low mass stars are forming near massive stars as well as in isolated groups. on the other hand, when considering distant galaxies we can probe their star formation rates only by considering the phenomena induced by the presence of massive stars, such as bright hii regions, supernova explosions, unresolved, bright stellar clusters. however, using massive star diagnostics to measure the overall star formation rates is valid if and only if we are confident to be able to extrapolate correctly from what we see coming from a bunch of massive stars to the total amount of mass that is forming the bulk of stars, i.e. the low mass stars. in other words, we need to understand how the formation of moderate mass stars works as a function of the environmental conditions and how it relates to the massive star formation. ground-based spectroscopic studies of nearby young star-forming regions (e.g. taurus, auriga, ophiuchus) show that the mass accretion rate appears to decrease steadily with time, from about 10−8 m� yr−1 at ages of ∼ 1 myr to ∼ 10−9 m� yr−1 at ∼ 10 myr. at face value this is in line with the expected evolution of viscous discs, but the scatter of the data exceeds 2 dex at any given age (see also fig. 3). such a scatter may be explained in part by the wide mass range covered by the observations, but the true limitation is the paucity of available measurements. indeed, all the results so far obtained are based on the mass accretion rates of a few hundred stars, located in nearby regions, covering a limited range of ages and no appreciable range of metallicity. using the hst, we have started a study of the pms phase is a number of star forming regions in the local group. among others, these include ngc 3603 in the milky way, 30 doradus and surrounding regions in the large magellanic cloud, and ngc 346 and ngc 602 in the small magellanic cloud. thanks to a novel method that we have developed to combine broad-band (v , i) photometry with narrowband hα imaging (de marchi et al. 2010), we have identified more than 3 000 bona-fide pms stars still undergoing mass accretion (fig. 1). we have determined their physical parameters, i.e. temperature, luminosity, age, mass and mass accretion rate. this is presently the largest and most homogeneous sample of pms objects with known physical properties. 113 http://dx.doi.org/10.14311/app.2014.01.0113 nino panagia, guido de marchi figure 1: the v −hα colour as a function of v − i in fields around sn 1987a in the lmc (left; de marchi et al. 2010), in the cluster ngc 346 in the smc (middle; de marchi et al. 2011a) and in ngc 3603 in the galaxy (right; beccari et al. 2010). all colours are corrected for extinction. stars with small photometric errors (small dots in light gray) define the reference template for normal stars (i.e. with no hα emission), shown here as a dashed line. strong hα emission results in a greater than average value of v −hα. we have identified in this way ∼ 3 400 pms stars in the three galaxies. figure 2: colour–magnitude diagrams for the fields around sn 1987a (left) and around ngc 346 (right). stars with significant hα excess are highlighted. whilst some are still very young, and as such still very distant from the ms, many are older objects already approaching the ms, and as such would not be distinguishable from normal ms stars using standard broad-band photometry alone. by detecting all stars with an hα excess, we can easily identify and study multiple stellar populations in any given region. the virtue of this new method is that it derives the luminosity of the photospheric continuum of a star inside the specific hα band simply by interpolation from the average v −hα colour of stars with the same v −i index (fig. 1), the majority of which have no emission. equipped with the knowledge of the continuum level in the hα band, we can easily determine the hα luminosity, lhα, of each star. the method and its applications are fully explained in a series of papers (de marchi et al. 2010; 2011a, 2011b; spezzi et al. 2012) and the accuracy of the hα continuum and lhα derived in this way is independently confirmed by spectroscopic measurements (barentsen et al. 2011). this method allows us to identify all objects with an excess emission, including relatively “mature” pms stars, already close to the ms (see fig. 2), that broad-band photometry alone could not distinguish from normal ms stars. thus, we can (1) identify different generations of stars within the same region, (2) derive their physical propertiest through comparison to evolutionary tracks for the appropriate metallicity, and (3) study their spatial distribution to establish the relationship to massive stars and nebular gas. 114 star formation as seen by low mass stars figure 3: the left panel shows the mass accretion rate as a function of stellar age for pms stars in ngc 346 (diamonds) compared with that of galactic t tauri stars (see legend) from the work of sicilia–aguilar et al. (2006; the large cross indicates the uncertainties as quoted in that paper). the solid line shows the evolution for current models of viscous disc evolution from hartmann et al. (1998). our measurements are systematically higher than the models, and the effect remains when we consider separately stars of different masses (right panel, see legends for mass values). all four mass groups show the same decline of ṁacc with age (α ' −0.6, thick dashed lines), but ṁacc is higher for more massive stars (see value of intercept q at 1 myr). figure 4: run of ṁacc/m as a function of age for the pms objects in ngc 346 (circles) and for galactic stars in taurus (crosses) and in trumpler 37 (squares). the hatched band show the best fit (±1σ) to the ngc 346 data, the dark-shaded band is the fit to the pms stars in the 30 dor region (de marchi et al. 2011c) and the light-shaded band is the fit to the galactic stars. we note that the value of ṁacc in the galaxy is systematically lower than in the mcs at all masses and ages. all regions that we studied exhibit multiple recent episodes of star formation, indicating that star formation has proceeded over a long time, even though our age resolution cannot discriminate between an extended episode or short and frequent bursts. we also find that there is no correlation between the projected spatial distribution of young and old pms stars and that the younger population is systematically more concentrated. a fundamental parameter that we can derive with this method is the mass accretion rate, ṁacc. since the energy released by the accretion process goes towards ionising and heating the circumstellar gas, the accretion luminosity lacc can be derived from lhα. with the mass and radius of each pms star determined from the evolutionary tracks, the value of ṁacc can be obtained from the free-fall equation. we find that older pms stars have typically lower mass accretion rates (see fig. 3) and this suggests an evolutionary effect (assuming that the initial conditions are the same at all times). however, the effects of temporal evolution are partly masked by the considerable scatter around the best fit due to the wide range of masses that we cover. a multivariate linear regression fit to the distribution of ṁacc as a function of age (t) and mass (m), allowed by the size of our sample, gives log ṁacc ' −0.6 × log t + logm + c, where c is a function of the metallicity z and is approximately proportional to z−1/3 (fig. 5). 115 nino panagia, guido de marchi figure 5: the average mass accretion rates for stars of 1m� and age 2 myrs for clusters in the smc (ngc 346, ngc 602), lmc (30 dor, sn 1987a field) and the mw (ngc 3603) as a function of their average metallicities. it appears that the accretion rates are a monotonically decreasing function of the metallicity, i.e ṁ ∝ z−1/3. in terms of this relationship, the systematic offset of galactic pms stars relative to stars in the magellanic clouds is as large as factor of six (see fig. 4). while our method will inevitably miss some pms stars with weak hα excess emission, it is very unlikely that ground-based searches of nearby star-forming regions have missed pms stars with strong lacc. thus, the difference is real, showing that the accretion process depends not only on age and mass, but also on metallicity (see fig. 5). other important results of our studies are: • in each region we find evidence for several episodes of star formation, with typical time separation of 10 myrs. • younger generations are spatially more concentrated. • there are large mass function variations across star formation regions, in that we see stellar groups that are rich of young low mass stars but lack any massive stars, and, viceversa, there are isolated massive stars with no low mass stars associated to them. • these findings suggest that the processes of star formation be appreciably different for highand low-mass stars. actually it is possible that a large number of lowmass stars are forming in regions where massive stars cannot be produced and, therefore, they remain unnoticed. for certain low surface density galaxies this might be the predominant mode of star formation, which would imply that their total mass based on their luminosity can be severely underestimated and that their evolution not be correctly understood. acknowledgement we are indebted to our collaborators martino romaniello, giacomo beccari, loredana spezzi, elena sabbi, pier prada moroni, scilla degl’innocenti, francesco paresce, and morten andersen for participating in this project. np research was funded in part by stsci-ddrf grant d0001.82435. references [1] barentsen, g., vink, j., drew, j., et al. 2011, mnras, 415, 103 [2] beccari, g., spezzi, l., de marchi, g., et al. 2010, apj, 720, 1108 doi:10.1088/0004-637x/720/2/1108 [3] de marchi, g., panagia, n., romaniello, m. 2010, apj, 715, 1 doi:10.1088/0004-637x/715/1/1 [4] de marchi, g., panagia, n., romaniello, m., et al. 2011a, apj, 740, 11 doi:10.1088/0004-637x/740/1/11 [5] de marchi, g., panagia, n., sabbi, e. 2011b, apj, 740, 10 doi:10.1088/0004-637x/740/1/10 [6] de marchi, g., paresce, f., panagia, n., et al. 2011c, apj, 739, 27 doi:10.1088/0004-637x/739/1/27 [7] hartmann, l., calvet, p., gullbring, e., d’alessio, p. 1998, apj, 495, 385 doi:10.1086/305277 [8] sicilia–aguilar, a., hartmann, l., furesz, g., et al. 2006, aj, 132, 2135 [9] spezzi, l., de marchi, g., panagia, n., et al. 2012, mnras, 421, 67 discussion manami sasaki: in order to increase the statistics for metal abundance dependencies would it be possible to study stellar populations in m 31 od m 33? nino panagia: i wish it was possible but, unfortunately, at present the angular resolution of the available telescopes, even hst, is not good enough to resolve solar mass objects in star forming regions at the distance of m 31 or m 33. in the future the combination of very large telescopes, say >30 m and adaptive optics should eventually do the miracle. jim beall: would you expect the same relationship between accretion rates and abundances in massive stars? 116 http://dx.doi.org/10.1088/0004-637x/720/2/1108 http://dx.doi.org/10.1088/0004-637x/715/1/1 http://dx.doi.org/10.1088/0004-637x/740/1/11 http://dx.doi.org/10.1088/0004-637x/740/1/10 http://dx.doi.org/10.1088/0004-637x/739/1/27 http://dx.doi.org/10.1086/305277 star formation as seen by low mass stars nino panagia: the pre-main-sequence evolution of massive stars is so fast that it is hard to catch one of them while it is still accreting from their parent envelope. therefore, i don’t have an observational answer to your question. from a theoretical point of view, one would need a detailed knowledge of what determines the accretion process under conditions appropriate for massive stars. and, unfortunately, i don’t have that, either. 117 acta polytechnica ctu proceedings doi:10.14311/app.2017.12.0056 acta polytechnica ctu proceedings 12:56–63, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app human-machine interaction in solving tasks of the planning department boris kucherov∗, vladimir artyushenko department of information technology and control systems, information and technology faculty, university of technology, gagarina 42, korolev, moskovskaya oblast, russia ∗ corresponding author: boris.ku4erov@gmail.com abstract. the paper discusses issues of human-machine interaction in solving tasks of the planning department under severe resource restrictions using information technology. the negative factors influencing specialists of the planning department in solving their tasks under the given circumstances are shown. specific features of designing the user interface in this subject area are noted. directions to increase the efficiency of reaction of the planning department’s specialists to change the current situation by visual and sound notification of various events are marked. various ways to develop user interface to generate a conflict-free plan under severe resource restrictions are considered. the variants of informative presentation of operational and statistical information to stakeholders are analyzed. these issues are discussed by the example of the planning department which solves the tasks of allocation of control facilities for spacecraft (a subset of satellite range scheduling problem). keywords: planning department, human-machine interaction, notification, conflict-free plan, spacecraft. 1. introduction the allocation of shared resources (resources of collective usage) is a current problem with a large number of different modifications [1–5]. planning departments solving such tasks are used in many industrial areas, such as transportation industry, rocket and space industry, nuclear power industry, etc. as examples, planning departments of railway traffic, planning departments of road works, department of logistics transportation, traffic control departments, etc. [4–9]. in modern world such departments often work under severe resource restrictions caused not only by scarcity of allocated resources, but also by high requirements on time for solving the tasks. these requirements could be satisfied by using modern information technology. however, interaction of specialists with an automated information system of a planning department has sufficient influence on the efficiency of solving the tasks even when there is a high degree of automation. the main negative factors influencing the specialists of a planning department in solving their tasks under current conditions may include: • a large amount of data to be processed, a significant number of factors to be analyzed; • strict requirements to time of solving tasks under conditions when specialists should be resistant to stress; • a necessity of the current situation continual monitoring for a prompt response to its changes. the usage of successful approach to human-machine interaction can significantly increase the efficiency of solving tasks of a planning department. the issues of human-machine interaction in the already mentioned subject area are considered by the example of planning department solving tasks of allocation of control facilities for spacecraft. in such case, the control facilities are considered as shared resources (resources of collective usage) and the spacecraft are considered as their consumers. the control facilities (ground stations) are used to carry out communication sessions with spacecraft to receive telemetry information, to transfer command and program data, to measure parameters of spacecraft orbit, etc. [10, 11]. herewith, a control facility can carry out only one communication session with only one spacecraft at any given time. the problem of allocation of control facilities for spacecraft can be considered as a subset of satellite range scheduling (srs) problem. most papers related to srs [4, 5, 12, 13] discuss mainly a schedule (plan) optimization. various approaches, based on an integer linear programming [12], genetic algorithms [13–17], graph color theory [14, 18], etc. [2, 6, 19, 20], are proposed. however, not enough attention is paid to issues of human-machine interaction in solving tasks of allocation control facilities for spacecraft under severe resource restrictions using information technology. 2. the increasing efficiency of response of the planning department’s specialists on changing the current situation one of the main factors, influencing the efficiency of solving tasks of a planning department, is a timeli56 http://dx.doi.org/10.14311/app.2017.12.0056 http://ojs.cvut.cz/ojs/index.php/app vol. 12/2017 human-machine interaction in solving tasks of the planning department ness of specialists’ response on changing the situation. this factor could be parried by prompt notification of specialists about changing the situation. such notification has a number of specificities. first of all, a group of persons to be informed is not so large (from few to tens). employees’ workplaces equipped with computers are located on a quite small area (one or few rooms). the data flows of notifications have address direction. generally [21, 22], specialists of a planning department are always at their workplaces during their shift (except time for endorsing originals of documents and submitting them for approval), so they can be notified about changes in the current situation by computers. receiving information into a database can be considered as a completion of one technological operation and a start of another. when receiving new information from subscribers, specialists of a planning department are notified about this fact using both visual and sound messages. its implementation can be based on principles of multimodal alerts used in various services and applications (email, social media, organizers, etc.). after receiving a new message a pop-up window with brief information about it appears and a playback of sound alert or speech comment is played [23–27]. the notification may vary depending on the properties of the received information and of the current situation. it enables the specialist to make a decision promptly about the level of urgency to process the received data even if he/she performs other tasks and does not work on the computer at that time. the specialist can interrupt the current task and switch to performing a more priority one or begin processing the received information after the completion of the current task. the visual component of notification is a pop-up window containing data about the received information. an individual icon can be assigned to each type of event. a specialist can switch to processing the received data directly from the message of visual notification. the sound notifications may vary depending on the properties of the received information. they may be repeated at specified intervals before receiving notification by the specialist. however, notification about large number of events during short time can cause cognitive overload of specialists of a planning department. such overload could be prevented by tasks reallocation [28]. for a small number of specialists on the shift (e.g., 2-3 persons) and a large number of simultaneously occurring events, notifications can be arranged by its priorities and processed consistently according to their priorities in addition to tasks reallocation. during the process of notification of specialists about changes of situation, all information is received into a database, which is a central element of planning department’s automated information system. the generalized diagram of propagation of messages about receiving new information is presented in figure 1 figure 1. the propagation of messages about receiving new data figure 2. schematic representation of the principle of increasing the efficiency of solving tasks of planning department by using the notification system about changes of situation [22]. it was implemented by a mechanism of advanced queues support in database management system oracle oracle advanced queuing. the visual component of notifications (message) was implemented by devexpress vcl (visual component library). it should be noted that the usage of notification about changes of situation usually does not influence the time of making a decision, but it enables the specialists to start making a decision earlier (see figure 2). this causes one of two consequences (or their combination): the decision making process is completed earlier or there is more time to make a decision. thus, the notification about changes of situation can not only increase the efficiency of solving tasks of a planning department by earlier start and, as a consequence, by the earlier end of the decision making process: it can also contribute to improving the decisions due to additional time for its production. when the notification is received by the specialist and all more priority tasks are completed, then the processing of received data starts. for example, after the planning department receives requests on using control facilities, developing plan of allocation of control facilities starts. another example can be receiving data about changing the state of control facilities data preparation for analysis of current situation begins after it. processing various data about changing the situation may require different time. so, the processing of 57 boris kucherov, vladimir artyushenko acta polytechnica ctu proceedings such data as requests on using control facilities that don’t lead to conflict situations (which will be discussed below), request for cancellation of communication sessions, maintenance plans received beforehand, consists of performing a sequences of typical (routine) actions. that is, the processing of such data is carried out at the rule-based level of skill-rule-knowledge framework of rasmussen [29] and does not create a large cognitive load on specialists. processing other data such as requests on using control facilities that lead to conflict situations, troubles when performing communication sessions, malfunctions of control facilities is carried out at the knowledge-based level which creates a significant cognitive load on specialists and require more time to process. 3. developing a conflict-free plan under strict resource restrictions issues of human-machine interaction during solving the task of developing conflict-free plan under strict resource restrictions have significant influence on the efficiency and the quality of solving this task. so, information capacity and ergonomic of user interface of software for developing a plan are very important. it is especially significant when the scarcity of shared resources grows due to increasing the number of consumers of shared resources under resource restrictions. such circumstances cause increasing the number of conflict situations (conflicts). the conflict is a contradiction between request on using shared resources and existing restrictions [21]. it can be caused by the need to use the same resource for different consumers at the same time, the need to use the resource at the time of service operations, etc. resolution of conflicts is rather time-consuming process. moreover, it is hard for specialists of planning department to solve successfully a large number of conflicts under severe resource restrictions without using appropriate software. as a result, growing number of conflicts causes the increase of workload of specialists of planning department. so, developing the user interface of software for planning department should include proactive steps aimed to parry the increase of workload of the specialists. for such purpose it is necessary to predict a situation in the allocation of control facilities for spacecraft. also, the results of situation prediction can be used to make decisions during developing a plan to control facilities allocation. 3.1. prediction workload of specialists of planning department to solve tasks of workload prediction of specialists it is necessary to take into account a number of factors: structure and state of shared resources (control facilities), number and properties of requests on its usage, statistical data about its usage, planned maintenance, etc. as it has been already mentioned, one figure 3. the dependence of a quantity of conflicts per day from the number of spacecrafts and the number of control facilities (calculated in 100 model experiments): 2d-plot (top) and 3d-plot (bottom) of the major factors influencing the workload of specialists is a number of conflicts, arising during the allocation of control facilities for spacecraft. the number of conflicts significantly depends on the number and properties of requests on the use of control facilities as well as structure and state of control facilities. the number and properties of requests depend on structure and state of spacecrafts constellation and their mission profiles (technological control cycles of spacecrafts). the workload of specialists of planning department can be predicted by evaluating the number of conflicts which occur when changing the structure and state of spacecraft constellation and control facilities, using series of model experiments. each series can be used to determine the dependence of each indicator (e.g., number of conflicts) from some factors (e.g., the number of spacecraft). the example of dependence of quantity of conflicts from the number of consumers for the various number of planning objects is presented in figure 3. this dependence was obtained as a result of series of 100 model experiments using the model, developed to solve the tasks of workload prediction of specialists of planning department. the developed model implemented in matlab, which allows getting numerical probability characteristics of the situation in allocation of control facilities 58 vol. 12/2017 human-machine interaction in solving tasks of the planning department for spacecrafts, contains the following units: • a unit of loading initial data; • a unit of calculation windows of radio visibility for spacecrafts by control facilities; • a unit of generation different sets of input data for series of model experiments; • a unit of generation requests on using control facilities for spacecrafts (choosing windows of radio visibility to carry out communication sessions); • a unit of detection and count conflicts; • a unit of statistical data processing. the calculation of windows of radio visibility for spacecrafts was implemented using orekit a low level space dynamics library written in java. precision of orekit was proved during its usage in real missions [30]. windows of radio visibility were calculated using input data in the form of tle (two-line elements), which are provided by norad (north american aerospace defense command) and publicly available for free in its catalog at [31]. sampling 140 spacecraft on low-earth orbits from this catalog was performed. windows of radio visibility between these spacecrafts and 4 ground points were calculated. it was mentioned that there are 3 control facilities on each ground point. time of preparation for communication sessions was set as 15 minutes. a hypothetical constellation of 35 spacecrafts was generated during each experiment by random sampling spacecrafts from the previously sampled ones. for each constellation requests on using control facilities were generated from various number of spacecrafts (from 5 to 35) for various number of control facilities (from 3 to 12 facilities on 4 ground point). the requests were generated using approach of random sampling 3 windows of radio visibility from the most preferred 10 ones (which have the largest duration). conflicts were detected and counted for each subset of requests. the model results show numerical probability values of progressive increase in number of conflicts during increasing the number of spacecrafts and, consequently, progressive increase of workload of specialists of planning department. the largest number of conflicts is observed at the least number of control facilities. note that the number of conflicts can vary significantly for the same number of spacecrafts and control facilities (e.g., figures 4 and 5). however, the trend of progressive growth of the number of conflicts during increasing the number of spacecrafts is still preserved. it should be taken into account in developing the user interface of software for planning department. this is particularly important due to the fact that increasing the number of specialists on the shift will not completely parry the increasing load. it is caused figure 4. the example of range of variation of the conflicts’ number for 5 control facilities figure 5. the example of the probability density of the number of conflicts for 35 spacecrafts and 5 control facilities by the specificities of the task of developing (changing) a plan of allocation of control facilities which do not allow to parallelize its execution between several specialists. for example, parallel solution of several conflicts at the same date by different specialists in the most cases is impractical due to the fact that new conflicts may occur. furthermore, as shown in [32], for a large number of specialists tasks reallocation between them may lead to a significant increase of resource costs of these operations. 3.2. the user interface for developing a conflict-free plan under strict resource restrictions after receiving requests to use control facilities, they are aggregated to one table. this table is a basis for developing a draft of the plan of allocation of control facilities. the draft (candidate) plan can be viewed in a tabular form (e.g., figure 6) as well as in a form of a diagram for user convenience. color indication of conflicts with the possibility to view data about their reasons was implemented. so, the user can view requests that conflict with each other and data about the state of the shared resources which cannot be used in accordance with the requirements of the received requests. 59 boris kucherov, vladimir artyushenko acta polytechnica ctu proceedings figure 6. the main form of the program for developing conflict-free plan when new requests on using resources are received, the indication about existing not-processed data is carried out by color highlighting these data and showing total number of records to be processed. colors used for highlighting not-processed data as well as conflicts are quite important for information perception by the specialists of planning department. on the one hand, colors for alarms (e.g., conflicts) should attract attention to the highlighted data. on the other hand, color indication can be shown during quite long time, so it shouldn’t be annoying or cause fatigue of the specialists. also, various colors should be used for conflicts caused by different reasons (e.g., conflict with another communication session and conflict with maintenance of control facility). as the result of practical use of the developed software, colors with not very high saturation were chosen (hues of red for alarms, hues of blue for not-processed data). the specialist can resolve conflicts in manual mode as well as in automated mode (using special software for conflicts resolution), or using both of them. he/she chooses appropriate mode after analysing conflicts and reasons of their formation. advisability of solving conflicts in manual mode in some situations could be caused by small number of conflicts or by simplicity of solution (e.g., moving a communication session to another control facility without changing its time). time costs of solving conflicts in manual and automated modes can be comparable in such case. the resolution of conflicts in typical situations where the decisions are already known and stored in the corresponding database should also be mentioned. candidate solutions of conflicts can be developed using visualization of plan in the diagram containing available times of using each resource for each consumer. such times can be considered as possible solutions of the conflicts. also, a user can view data about possible solutions of the conflicts. such view of data representation is more intuitive and can make user’s work easier. however, it makes sense to use software for automated conflicts resolution (developing conflict-free plans) in many cases. a possibility to use such external (third-party) software is provided to ensure resolving conflicts in automated mode. in such case, all necessary data, including a draft of the plan of allocation control facilities, data about existing resource restrictions and reference datais sent to software for automated development of a conflict-free plan. note that the specialist could adjust the settings of developing conflict-free plans. for example, the specialist can mark certain communication sessions as mandatory to be included in the plan. also, the specialist can resolve some conflicts in manual mode before sending a draft of the plan to the software for automated development of a conflict-free plan. in addition, the specialist can make changes in the draft of the plan generated by such software. when a conflict-free plan is developed, it is sent into the reverse direction (from software for automated developing conflict-free plan to developed software for allocation of control facilities for spacecrafts). automated conflicts resolution can be carried out using, for example, methods of solving srs discussed in [4, 5, 12–18]. when all conflicts were resolved (if they have arisen), the plan of allocation of control facilities is approved. as soon as it was done, an extract from the plan for each subscriber is generated and sent. it should be noted that specialists of planning department have to prepare a large number of documents in hard copy after developing or changing the plan. the batch printing of documents on the results of a developing plan is provided to reduce time of this operation. the list of the documents to be printed is dynamically generated according to the content of the plan or its correction. to develop a conflict-free plan of allocation of control facilities as well as to solve other tasks of planning department it is necessary to have various data about the current situation (e.g., data about state of control facilities). its perception by the specialists can influence on the efficiency and quality of their decisions. so, its representation is also one of important issues of human-machine interaction in solving tasks of the planning department. 4. the variants of informative representation of operative and statistical data specialists of planning department need compact and informative representation of data about the current situation as well as the results of analysis of using shared resources to perform prompt evaluation and analysis of it. data about current situation include such parameters as current state of control facilities and spacecrafts, requirements of spacecrafts, and can 60 vol. 12/2017 human-machine interaction in solving tasks of the planning department be considered as operative data. the results of analysis of using control facilities for spacecrafts include such data as a number of planned and performed communication sessions, a number of troubles when communication sessions take place and its effects, statistical characteristics of repairing control facilities with typical malfunctions, etc. one of the most informative and convenient for the users ways to represent operative data is to use interactive schematic form and to represent the results of analysis of using control facilities is to use statistics. 4.1. representation of operative data compact and informative representation of operative data can be reached by presenting data in an interactive schematic form with the possibility to drill down to the desired level (e.g., figure 7). in this example pictograms of shared resources (control facilities) are schematically shown on geographical map in accordance with their locations. color indication of the status of control facilities for spacecrafts is carried out both in terms of serviceability and in terms of current usage. detailed reference and operational data can be viewed for each shared resource. also, the pictograms of consumers (spacecrafts) are shown at the top part of the interactive scheme. the indication of status and existence of current communication sessions for spacecrafts is implemented. detailed reference and operational data can be viewed for each consumer. also, a set of allowed shared resources is shown for each consumer (a set of control facilities which are included in ground control complex of each spacecraft is shown). the progress of performing the plan is showed in tabular form for each control facility at the top of interactive scheme. moreover, a separated tabular form to visualize the current progress of performing the plan of control facilities allocation for spacecrafts with color indication of state of communication sessions is provided. in addition, the data about the state of spacecrafts constellation are displayed using 3d-model of spacecrafts flights on near-earth orbit (e.g., figure 8). space dynamics calculations in the developed model are performed using sgp4 model (sgp simplified general perturbations) for spacecrafts on low-earth orbit and sdp4 model (sdp simplified deep space perturbations) for other spacecrafts. the possibility to manage progress of simulated time is provided. it can be normal or accelerated. also, a progress of simulated time can be stopped (it would be mean showing the results of modelling at fixed time). it should be noted that one of the directions of further development is integration between a 3d-model and interactive geographical map. it will have positive influence on the efficiency of evaluating the current situation. figure 7. the operative presentation data about the current situation in the schematic form (cf control facility, sc spacecraft, cmp control and measurement point) figure 8. example of visualization of data about state of spacecrafts constellation it is important to note that data about current situation is obtained as a result of collecting and processing a large amount of data, such as results of communication sessions and reprimands to them, data about occurrence and parrying malfunctions of control facilities, maintenance of control facilities, etc. much of this data, e.g. reprimands to communication sessions, can occur many times. so, using a list of typical reprimands is proposed. it favors classification data and improvement of quality of processing data by standardization of definitions. moreover, it allows increasing the efficiency of input data about reprimands by choosing its description from the list instead of manual input. possibility to view collected data in summary table for selected time interval was implemented to use in creating reports and further analysis of the data. the data in such table can be filtered and grouped flexibly to concentrate user’s attention on a part of the data which should be processed at the present. 4.2. representation of statistical data as it was mentioned above, the allocation of shared resources should take into account the results of analysis of their usage. specialists of planning department need various statistical data to perform such analysis. 61 boris kucherov, vladimir artyushenko acta polytechnica ctu proceedings statistical data manipulation can be done for various periods and various data slices (e.g., consumers, resources, results of resources usage, time intervals, etc.). the flexible generation of reports in accordance with current requirements of users is provided. in addition, there should be an opportunity to calculate new statistical indicators based on the basic ones with applying to them predefined functions and groups. statistical data manipulation is implemented both on server-side using features of oracle database and on client-side. server-side implementation is done using aggregate and analytical sql (structured query language) functions. client-side implementation is done using components quantumgrid and pivotgrid from devexpress vcl. use of such components provides flexible filtering and grouping statistical information. it helps to increase efficiency of analysis of using control facilities. also, a user can view data in the standard as well as in a customizable view while working with pivot tables, which are implemented by pivotgrid component. it should be noted that this current view of pivot table can be printed. flexibility of data representation in pivot tables, achieved by changing their view through moving headers of fields into different table areas, allows to generate reports promptly according to actual requirements of the specialists of the planning department. data from these tables can also be presented in charts. it ensures increasing not only clearness of data visualization, but also clearness of reports prepared by the specialists of the planning department. 5. conclusions thus, the analysis of specific features of humanmachine interaction in solving the tasks of planning department under strict resource restrictions using advanced information technology has been performed. the proposed approaches to developing user interface provide concentrated attention of specialists of planning department on the most important data requiring priority processing. the system of visual and sound notification about important events was developed to increase the efficiency of specialists’ response on changes of the current situation. specific features of user interface for developing conflict-free plan have been noted. the variants of informative presentation of actual information about the current situation on the interactive scheme and flexible presentation of statistical data have been proposed. 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[30] orekit. www.orekit.org. [31] norad two-line element sets current data. http://celestrak.com/norad/elements/. [32] t. de jong. cognitive load theory, educational research, and instructional design: some food for thought. instructional science 38(2):105–134, 2010. doi:10.1007/s11251-009-9110-0. 63 http://dx.doi.org/10.1109/taes.2009.5259176 http://dx.doi.org/10.1109/aero.2013.6496849 http://dx.doi.org/10.1007/s10951-008-0066-8 http://dx.doi.org/10.1109/estel.2012.6400125 http://dx.doi.org/10.1109/aero.2015.7119277 http://dx.doi.org/10.1145/1718918.1718926 http://dx.doi.org/http://dx.doi.org/10.1016/j.intcom.2011.05.006 http://dx.doi.org/http://dx.doi.org/10.1016/j.intcom.2008.04.004 http://dx.doi.org/http://dx.doi.org/10.1016/j.ijhcs.2015.02.001 http://dx.doi.org/10.1145/2254556.2254607 www.orekit.org http://celestrak.com/norad/elements/ http://dx.doi.org/10.1007/s11251-009-9110-0 acta polytechnica ctu proceedings 12:56–63, 2017 1 introduction 2 the increasing efficiency of response of the planning department's specialists on changing the current situation 3 developing a conflict-free plan under strict resource restrictions 3.1 prediction workload of specialists of planning department 3.2 the user interface for developing a conflict-free plan under strict resource restrictions 4 the variants of informative representation of operative and statistical data 4.1 representation of operative data 4.2 representation of statistical data 5 conclusions references acta polytechnica ctu proceedings doi:10.14311/app.2016.5.0069 acta polytechnica ctu proceedings 5:69–73, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app deployment of ertms in czech republic jiří vopava∗, mária jánešová, radek kratochvíl ctu in prague, czech technical university in prague – faculty of transportation sciences, konviktská 20, 110 00, prague ∗ corresponding author: jiri.vopava@gmail.com abstract. the article describes current situation and expected deployment of international standard for automatic rail vehicle protection in czech republic for period 2014 – 2020. article introduces expected status in 2020 and subsequent implementation of commitments until 2026. it introduces expected result of gradual implementation for tracks and vehicles. it also displays brief deployment overview of european rail traffic management system in european union countries for each level of european train control system. keywords: ertms, etcs, gsm-r, interoperability. 1. introduction the ertms is automatic train protection which represents basic part of interoperability in european rail system. the term is abbreviation of "european rail traffic management system" and it was defined to synchronize nationals systems to the one common compatible system. urgency of the unification and cooperation between european countries caused an increase in freight which had negative impact for environment and ecology. the implementation of interoperability and automatic train protection across european countries allows competition to air and car freight. implementation of the standard is business initiative that transforms the operation of the tracks, enhance safety, capacity, performance and reliability. it also have impact on reduce of cost of operation and maintenance. ertms is divided into two basic components. the first one is etcs "european train control system" and second gsm-r "global system for mobile communication for railway". the ertms allow one compatible system for crossborder traffic what reduce cost for implementation several regional stand-alone systems. the synchronization of automatic train protection increase competitiveness of the european rail sector. gsm-r "global system for mobile communications – railway" is a radio system based on gsm standard for providing of voice and data communication between vehicle and track. etcs "european train control system", is an automatic train protection system to replace the existing national systems. the etcs replaces about twenty different automatic train protections across european track. it can be configured to operate in one of the following application levels to enable etcs equipped vehicles to operate in not etcs equipped system where the safe movement of the vehicle is controlled by the default national control system: figure 1. etcs l1 [1] • level 0 – etcs equipped vehicles operating on lines without etcs system, • level 1 – an conventional line-side signal is passed to the train via a switched transmitter on the track, repeating the indication from the conventional signalling system, which continues to be used to support safe train separation. it is the figure 1, • level 2 – movement authority is passed by the gsm-r radio network from a radio block centre to the train. conventional train detection systems are utilized in conjunction with interlocking systems used to enforce safe train separation. it is the figure 2, • level 3 – it builds on level 2, but increases safe train separation using critical data from the train. it is the figure 3. 2. deployment of ertms in czech republic the czech republic contributing to the fulfillment of legal solutions arising from following documents: • directive 2008/57/ec of the european parliament and of the council 69 http://dx.doi.org/10.14311/app.2016.5.0069 http://ojs.cvut.cz/ojs/index.php/app j. vopava, m. janesova, r. kratochvil acta polytechnica ctu proceedings figure 2. etcs l2 [1] figure 3. etcs l3 [1] of 17 june 2008 on the interoperability of the rail system within the community • decisions 2012/88/eu, commission decision of 25 january 2012 on the technical specification for interoperability relating to the control-command and signalling subsystems of the trans-european rail system (2012/696/eu a 2015/14/eu) • regulation (eu) no 1315/2013 of the european parliament and of the council of 11 december 2013, on union guidelines for the development of the transeuropean transport network and repealing decision no 661/2010/eu • regulation (eu) no 1316/2013 of the european parliament and of the council of 11 december 2013, establishing the connecting europe facility, amending regulation (eu) no 913/2010 and repealing regulations (ec) no 680/2007 and (ec) no 67/2010 the deployment is defined in document "národní implementační plán ertms" released by ministry of transport. the document defines maximum amount of payloads for each project gsm-r and etcs l2 with respect to co-financing from ertms funds. it also defines expected deployment schedule of each project. between 2005 and 2014 was equipped 1132 km of tracks across of the czech republic. it is connected to figure 4. map of gsm-r implementation [2] figure 5. map of etcs implementation [2] the gsm-r sždc, db, öbb, prorail and the home network operator. there are now mobile terminals equipped with gsm-r all čd vehicles used in regular operation. almost all čd vehicles used in regular operation are now equipped with gsm-r terminals. the first stage with fully deployed etcs system at 2021 will be track "praha – česká třebová – brno – břeclav". following tables 1, 2, 3 display figures for expected schedule of deployment of gsm-r, etcs l2 and vehicle on-board equipment for period 2014 – 2020 (– 2026). the figure 6 below visualizes data from tables above. it displays total amount of deployments for each year until 2020. figure 6. total amount of expected deployments 70 vol. 5/2016 deployment of ertms in czech republic no. track distance [km] deployment 1 uzel praha (beroun – praha – benešov u prahy – lysá nad labem) 120 2014-2015 2 české velenice st. hr. rakousko – české budějovice – horní dvořiště st. hr. rakousko 110 2015-2016 3 plzeň – české budějovice 136 2015-2016 4 kolín – havlíčkøuv brod – křižanov – brno 195 2014-2016 5 benešov – votice 20 2015-2016 6 beroun – plzeň – cheb st. hr. německo 169 2014-2016 7 cheb – vojtanov st. hr. německo 20 2015-2016 8 znojmo – šatov st. hr. rakousko 13 2015-2016 9 ústí nad orlicí – lichkov st. hr. polsko 35 2015-2016 10 votice – české budějovice 100 2016-2017 11 hranice na moravě – horní lideč st. hr. slovensko 67 2016-2017 12 ústí nad labem – oldřichov u duchcova/úpořiny – most – karlovy vary – cheb 212 2017-2018 13 pardubice – hradec králové 22 2019-2020 14 zábřeh na moravě – šumperk 13 2019-2020 15 praha – letiště v. havla ruzyně – kladno 31 after 2020 16 brno – přerov 90 after 2020 17 plzeň – domažlice st. hr. německo 72 after 2020 18 velký osek – hradec králové – choceň 96 after 2020 total 1521 table 1. expected track deployment with gms-r [3] no. track distance [km] deployment 1 kolín – břeclav st. hr. rakousko/slovensko 277 2012-2016 2 kralupy nad vltavou – praha – kolín 110 2016-2017 3 st. hr. německo – dolní žleb – kralupy 112 2017-2019 4 petrovice u karviné st. hr. polsko – přerov – břeclav 206 2015-2017 5 praha-uhřiněves – votice 54 2016-2017 6 votice – české budějovice 101 2017-2018 7 česká třebová – přerov 110 2016-2018 8 plzeň – cheb st. hr. německo 117 2016-2018 9 beroun – plzeň 70 2016-2018 10 dětmarovice – mosty u jablunkova st. hr. slovensko 53 2017-2019 11 české velenice st. hr. rakousko – české budějovice – horní dvořiště st. hr. rakousko 112 2017-2019 12 ústí nad orlicí – lichkov st. hr. polsko 37 2018-2020 13 kolín – nymburk – mělník – děčín východ – děčín-prostřední žleb 159 after 2020 14 kolín – havlíčkøuv brod – brno 200 after 2020 15 praha – lysá nad labem 35 after 2020 16 praha – letiště v. havla ruzyně – kladno 31 after 2020 17 praha – beroun 43 after 2020 18 plzeň – domažlice st. hr. německo 72 after 2020 19 pardubice – hradec králové 22 after 2020 20 plzeň – české budějovice 136 aftre 2020 21 brno – přerov 90 after 2020 22 hranice na moravě – horní lideč st. hr. slovensko 67 after 2020 23 uzel praha 40 after 2020 24 český těšín – ostrava-svinov 41 after 2020 25 velký osek – hradeck králové – choceň 96 after 2020 26 cheb – karlovy vary – chomutov 111 after 2020 27 ústí nad labem – chomutov, ústí nad labem – bílina 101 after 2020 total 2603 table 2. expected deployment of equipment upgrade ertm/etcs [3] 71 j. vopava, m. janesova, r. kratochvil acta polytechnica ctu proceedings no. track distance [km] deployment 1 kolín – břeclav st. hr. rakousko/slovensko 250 2015-2019 2 kralupy nad vltavou – praha – kolín 100 2016-2019 3 st. hr. německo – dolní žleb – kralupy 100 2017-2019 4 petrovice u karviné st. hr. polsko – přerov – břeclav 130 2015-2020 5 praha-uhřiněves – votice 40 2016-2020 6 votice – české budějovice 50 2017-2020 7 česká třebová – přerov 50 2016-2020 8 plzeň – cheb st. hr. německo 40 2016-2020 9 beroun – plzeň 40 2016-2020 10 dětmarovice – mosty u jablunkova st. hr. slovensko 20 2017-2020 11 české velenice st. hr. rakousko – české budějovice – horní dvořiště st. hr. rakousko 50 2017-2020 12 ústí nad orlicí – lichkov st. hr. polsko 20 2018-2020 13 kolín – nymburk – mělník – děčín východ – děčín-prostřední žleb 100 after 2020 14 kolín – havlíčkøuv brod – brno 100 after 2020 15 praha – lysá nad labem 30 after 2020 16 praha – letiště v. havla ruzyně – kladno 20 after 2020 17 praha – beroun 30 after 2020 18 plzeň – domažlice st. hr. německo 40 after 2020 19 pardubice – hradec králové 20 after 2020 20 plzeň – české budějovice 50 after 2020 21 brno – přerov 60 after 2020 22 hranice na moravě – horní lideč st. hr. slovensko 30 after 2020 23 uzel praha 20 after 2020 24 český těšín – ostrava-svinov 20 after 2020 25 velký osek – hradec králové – choceň 40 after 2020 26 cheb – karlovy vary – chomutov 50 after 2020 27 ústí nad labem – chomutov, ústí nad labem – bílina 50 after 2020 total 1550 table 3. expected track deployment of etcs l2 [3] after 2020 will be deployed around 250 km tracks and 150 vehicles every year until 2026. strategies transition from the current national system vz ss to european interoperable system class a – etcs consists a combination of investment in track equipment and train equipment. in the first phase will be equipped only international traffic trains. during migration will vehicles equipped with etcs parallel with vz ls that allow operation of both systems together. etcs should be fully migrated for first and second rail corridor and the track přerov – česká třebová at the latest to 2030. after the migration period will be completely decommissioned national systems vz ls and fully deployed etcs system. in some cases can be deployed new special sections equipped solely with etcs, which will be designed to operate only vehicles equipped with etcs even before end of migration period. i.e. a railway connection václav havel airport prague and prague center. 3. deployment of ertms in other european countries unification of europe requires to all transport systems operates without restrictions and time losses, especially when crossing borders. the deployment started in most of european union countries. following countries started participation on deployment of the ertms standard: austria, belgium, bulgaria, croatia, czech republic, denmark, finland, france, germany, greece, hungary, italy, luxembourg, netherlands, poland, romania, slovakia, slovenia, spain, sweden and united kingdom. the figure 7 displays amount of kilometers contracted tracks for each country. the figure 8 displays covering of the ertms divided by level of tracks. the figure 9 displays amount of deployed on-board equipment of vehicles for each country. the figure 10 displays levels of on-board equipment implemented in vehicles. 72 vol. 5/2016 deployment of ertms in czech republic figure 7. ertms contracted tracks [km] in eu figure 8. tracks in eu separated by level 4. conclusions by 2020 the gsm-r will cover major sections of the rail freight corridors in the czech republic. the system will be further deployed progressively on all 3700 km of national routes in order to create comprehensive operational tracks. etcs deployment priority by 2020 is rail freight corridor 7, partially corridors 8, 9, 5 and the track přerov – česká třebová. by 2020, it is necessary to ensure the development of the etcs about 1350 kilometers of tracks and 890 vehicles, ie. for additional six years, around 250 km of tracks and 150 vehicles every year, but this is conditional on the timely implementation of the modernization infrastructure. this requires the necessary financial resources for the trackside and on-board ertms and creating mofigure 9. global ertms vehicles contracted in europe figure 10. vehicles in eu separated by level tivational factors and efficient financial support equipping vehicles with on-board equipment of gsm-r and etcs. references [1] the european rail traffic management system, portál ertms [online]. [2016-02-12], http://www.ertms.net/?page_id=42. [2] národní implementační plán ertms 2014-2020, portál acri [online]. [2016-02-12], http://www.acri.cz/uploads/acri-akademie/15-06% 20etcs/2015_cech,%20varadinov.pdf. [3] národní implementační plán ertms, portál ministerstva dopravy [online]. [2016-02-12], http://www.mdcr.cz/nr/rdonlyras/ 7ff4faf1-1ebe-4116-bf90-808ec7306e04/0/ nipertmsnpweb.pdf. 73 http://www.ertms.net/?page_id=42 http://www.acri.cz/uploads/acri-akademie/15-06%20etcs/2015_cech,%20varadinov.pdf http://www.acri.cz/uploads/acri-akademie/15-06%20etcs/2015_cech,%20varadinov.pdf http://www.mdcr.cz/nr/rdonlyras/7ff4faf1-1ebe-4116-bf90-808ec7306e04/0/nipertmsnpweb.pdf http://www.mdcr.cz/nr/rdonlyras/7ff4faf1-1ebe-4116-bf90-808ec7306e04/0/nipertmsnpweb.pdf http://www.mdcr.cz/nr/rdonlyras/7ff4faf1-1ebe-4116-bf90-808ec7306e04/0/nipertmsnpweb.pdf acta polytechnica ctu proceedings 5:69–73, 2016 1 introduction 2 deployment of ertms in czech republic 3 deployment of ertms in other european countries 4 conclusions references acta polytechnica ctu proceedings doi:10.14311/app.2015.1.0045 acta polytechnica ctu proceedings 2:45–50, 2015 © czech technical university in prague, 2015 available online at http://ojs.cvut.cz/ojs/index.php/app impact assessment of image feature extractors on the performance of slam systems taihú pirea,∗, thomas fischera, jan faiglb a university of buenos aires, intendente güiraldes 2160, ciudad autónoma de buenos aires, argentina b department of computer science, faculty of electrical engineering, czech technical university in prague, technická 2, 166 27, prague, czech republic ∗ corresponding author: tpire@dc.uba.ar abstract. this work evaluates an impact of image feature extractors on the performance of a visual slam method in terms of pose accuracy and computational requirements. in particular, the s-ptam (stereo parallel tracking and mapping) method is considered as the visual slam framework for which both the feature detector and feature descriptor are parametrized. the evaluation was performed with a standard dataset with ground-truth information and six feature detectors and four descriptors. the presented results indicate that the combination of the gftt detector and the brief descriptor provides the best trade-off between the localization precision and computational requirements among the evaluated combinations of the detectors and descriptors. keywords: image features, visual slam, stereo vision. 1. introduction during the last decade, the simultaneous localization and mapping (slam) problem has been one of the main research interests in mobile robotics. particularly, the use of cameras as the main sensors has been given a special attention [1] [2] [3] [4] because of their benefits such as low-cost and passive sensing. in vision-based slam approaches, local image features are used to build a map and simultaneously estimate the robot pose using the environment landmarks represented as the image features. in this way, the map is represented as a sparse point cloud, where each point results from triangulating salient points (image features) matched from a pair of stereo images. currently, there exist several local image feature extractors in the literature. a feature extractor is a combination of a salient point (called keypoint) detection procedure and a computation of a unique signature (called descriptor) for each such a detected point. the most commonly used detectors are sift [5], surf [6], star [7], gftt [8], fast [9], and relatively recently proposed orb [10], while among the most used descriptors we can mention sift, surf, orb, brief [11], and brisk [12]. in visual slam systems, the feature extraction process has a huge impact on the accuracy of the whole system. on one hand, the precision of the robot localization is heavily correlated to the sparsity of features in images and the ability to track them for a long period during the robot navigation, even from different points of view. on the other hand, if the number of points in the map grows too quickly, it may slow down the whole system. to be able to keep the response of the system under real-time constraints, images have to be dropped or other parts of the system, like optimization routines, need lower computational requirements. in this work, we evaluate the impact of different state-of-the-art feature extractors on the performance of the visual slam localization method. in particular, the evaluation is based on the stereo visual slam approach s-ptam introduced in [4]. the presented results indicated that the combination of the gftt detector and brief descriptor is the most reliable choice for our slam system among the other evaluated combinations. the rest of the paper is organized as follows. section 2 presents overview of the related work while section 3 summarizes the most used feature detectors and descriptors in the visual slam literature. section 4 briefly comments the considered stereo visual slam system using for the evaluation. in section 5, we present the evaluation of the features extractors and the achieved results. section 6 is dedicated to the conclusions and future work. 2. related work several evaluations of features extractors can be found in literature. each of them is driven by the particular application or issue at the hand they are aimed to address. for example, in [13], authors evaluate several features extractors in the context of autonomous navigation in outdoor environments under seasonal changes. they came to a conclusion that the best performing method is the star–brief combination of the detector–descriptor, which outperforms sift by more than thirty percentage points. in addition, they argued that the star–brief extractor is also less computationally demanding than other extractors and thus it seems to be the most suitable feature 45 http://dx.doi.org/10.14311/app.2015.1.0045 http://ojs.cvut.cz/ojs/index.php/app t. pire, t. fischer, j. faigl acta polytechnica ctu proceedings detector–descriptor for navigational purposes. on the other hand, authors of [14] provide a performance comparison of feature extractors against illumination changes in outdoor scenes in the context of the visual navigation. they concluded that the configuration of the fast–surf is the optimal in their setup. besides, they report that this combination provides an effective computational time per image, which is favorable for the real-time vision-based navigation application. the work [15] compares contemporary point features detector and descriptor pairs in order to determine the best combination for the robot visual navigation. the authors concluded that the fast– brief combination is a good choice when processing speed is an important parameter of the system setup. they also argued that under camera movement conditions, additional computational cost—needed for the descriptors and detectors that are robust to in-plane rotation and large scaling— seems to be unjustified. however, they do not tested the method in a real slam application. regarding the aforementioned evaluation of the detectors and descriptors, the work presented in this paper is within the context of the full 6dof slam. 3. local image features an image feature extractor consists of detection and description phases. the feature detector serves to locate salient areas of the image while the feature descriptor captures information about the local neighborhood of the detected area. here, we provide a brief overview of the considered feature extractor and descriptor algorithms in this evaluation study. sift – scale invariant feature transform [5]. an established feature detector with a high precision and good robustness, which is known to be computationally demanding. surf – speeded up robust features [6] is a similar to sift, but it is computationally less demanding due to approximations. star – a modified version of the censure (center surrounded extrema) [7] detector, which is computationally less demanding at the expense of a lower precision. brief – binary robust independent elementary features [11] is a descriptor that describes an image area using a number of intensity comparisons of random pixel pairs. it is saved as a binary string, which reduces the computational complexity of the subsequent matching. fast – features from accelerated segment test [9] is a feature detector focused on lowering the computational cost. brisk – binary robust invariant scalable keypoints [12] is a scale and rotation invariant version of brief, but unlike brief, it uses a deterministic comparison pattern. orb – oriented fast and rotated brief [10] is another attempt to achieve a scale and rotation invariant brief, as a computationally efficient alternative to sift and surf. it uses the fast detector to achieve low computational requirements. gftt – a detector focused on selecting features relevant to motion tracking by analyzing the amount of information they provide for that particular task [8]. the surf and sift descriptors rely on the their own detectors, which are also considered in the presented evaluation. however, for the brief and brisk binary descriptors the considered detectors are the gftt, fast and star which results in the additional six combinations of the detector–descriptor pairs in the presented evaluation. 4. overview of s-ptam s-ptam [4] is a stereo visual slam method for a large scale map navigation based on the monocular parallel tracking and mapping (ptam) method introduced in [1]. the method consists of two processes working in parallel: 1) the tracking of the detected features and; 2) creating a map of the features (mapping). during a robot navigation, the method works as follows. s-ptam extracts features from the incoming stereo images to match and construct a virtual map of the environment. the newly extracted feature descriptors are matched against descriptors of the points stored in the map according to the estimated field of view. the matches may then be used to refine the estimated camera pose using an iterative least squares minimization method, e.g., using the levenberg-marquardt algorithm. the particular stereo matches between the features that cannot be matched to the map are triangulated and inserted as new map points, for the tracking of future frames. in parallel, a map refinement algorithm is running. it is also based on the levenberg-marquardt optimization that continuously performs the bundle adjustment on the current local portion of the map. in [4], s-ptam uses the gftt feature detector and the brief descriptor extractor. in this work, we consider other combinations of the detector–descriptor to evaluate an impact of the combination to the performance of the localization and mapping processes. 5. evaluation the kitti vision benchmark suite [16] is used to evaluate s-ptam for each type of considered detector– descriptor configuration. in particular, we present the results obtained for the sequence 00, shown in figure 1. the sequence records the stereo camera frames captured by a moving car in an urban scenario for almost 4 km long path. the particular parameters of 46 vol. 2/2015 impact assessment of image feature extractors on slam the evaluated feature extractors have been selected in such a way that allows s-ptam to run without ever loosing localization. they have been tuned from a strong restrictive value and then relaxed until the method completes the whole sequence. the parameters are listed in table 1. detector / parameter valuedescriptor sift noctavelayers 1 l2normthreshold 100 surf hessianthreshold 1000 noctaves 1 l2normthreshold 0.2 star responsethreshold 20 brief bytes 32 hammingthreshold 25 fast threshold 60 brisk hammingthreshold 100 orb nfeatures 2000 nlevels 1 hammingthreshold 50 gftt nfeatures 2000 mindistance 15.0 table 1. parameters used for feature detectors and descriptors. the parameters which do not appear in the list use the default value in the opencv implementation. in the case of the binary descriptors, the hamming distance is used to compute the valid matches while the l2 norm is used for the surf and sift descriptors. the evaluation has been performed using an intel core i7 processor with 4 cores running at 2.2 ghz. although s-ptam strongly exploits parallelism, the experiments were run in a sequential fashion that allow us to simulate ideal conditions and abstract from the limitations of the available computational power. this ensures that no frames are dropped and that the iterative optimization routines always converge or reach a maximum threshold of iterations. nevertheless, the tracking process performs pose optimization using an iterative algorithm; so, the less time is used in the features extraction, the more iterations the method can compute. figure 2 shows a characterization of the total tracking time for each pair of frames, as achieved by using the evaluated extractors. moreover, the iterative least-squares optimization, which is utilized in the mapping and tracking processes, depends linearly on the number of tracked points (the density of the map). thus, regarding the computational burden, the map should be as small as possible while the map points should contain strong enough features to support a robust tracking of the figure 1. path tracked by every method run under different extractors, against the ground truth. the path is nearly 4 km long. the shown distances at the axes are in meters. figure 2. total tracking time achieved by each configuration frames. table 2 shows the final number of points contained in the map after finishing each trial for a particular combination of feature detector and descriptor. in figure 3, we can see how the map size impacts directly on the temporal performance of the tracking process. combinations of the detector–descriptor that build the most dense maps also take the longest time to compute. differences in the map size for the evaluated descriptor in the feature extractors with the same detector can have two reasons. the first reason is that new 47 t. pire, t. fischer, j. faigl acta polytechnica ctu proceedings figure 3. tracking time without taking into account feature extraction points are created from the stereo features only if these features are not matched to the map. the second reason is that the points marked as outliers during the refinement processes are discarded. in the first case, this can be caused by descriptors that are not robust enough to be matched to the map for a long time. in the second case, the descriptor matching may be too permissive and it allows bad matches that are later discarded as outliers. extractor final map size gftt / brief 990 455 gftt / brisk 1 314 356 sift / sift 1 581 876 star / brief 1 893 372 surf / surf 2 059 879 fast / brief 2 420 652 star / brisk 2 447 418 fast / brisk 3 207 003 orb / orb 5 192 885 table 2. the number of points contained in the map after completing the sequence for each evaluated extractor, in ascending order. since the goal of this work is to assess the impact of the feature extractor choice also on the accuracy of the slam method, the achieved performance is presented as two independent relative errors for each estimated pose: εt for the translation error and; εθ for the orientation. let xk be the estimated pose at the frame k, which can be decomposed as the translation tk and the rotation rk. let x∗k be the reference pose, which can be decomposed in the same fashion. the aforementioned errors are computed as εt,k+1 = ‖(tk tk+1) ( t∗k t∗k+1 ) ‖, εθ,k+1 = angle ( (rk rk+1) ( r∗k r∗k+1 )) , where is the inverse of the standard motion composition operator. for pure translations, we can rewrite t1 t2 = t2− t1, and for the pure rotations as r1 r2 = rt1r2. ‖x‖ stands for the euclidean norm and angle (r) extracts the magnitude of the rotation. the computed errors are shown in figure 4 and figure 5, respectively. although the angular deviation to the ground truth, shown in figure 5, seems to be similar in all methods, the same is not true for the translation error, as it can be seen in figure 4. the brisk descriptor seems to be a more reliable with the fast detector, while the same holds for the brief descriptor with the gftt detector. figure 4. relative translation error figure 5. relative orientation error for completion, the absolute errors ε′t,k = ‖tk t∗k‖ ε′θ,k = angle (rk r∗k) are shown in figure 6 and figure 7. 48 vol. 2/2015 impact assessment of image feature extractors on slam figure 6. absolute translation error figure 7. absolute orientation error 6. conclusions in this paper, we present an evaluation of the impact of different state-of-the-art image feature extractors on the performance of the slam method proposed in [4]. the kitti benchmark suite dataset with a ground truth is used to evaluate the achievable precision of the method for different feature extractors. based on the presented results, the main conclusion is that the gftt detector is the most suitable choice for the best performance in the evaluated dataset. the gftt (accompanied with the brief or brisk descriptors) outperforms the other methods in terms of the required computational time and the map quality. although the map density is far smaller, the computed translation error is similar, even slightly better, than the one achieved by other extractors. this insight can be interpreted as the most useful features (regarding the navigation) are extracted while the descriptor also support efficient matching resulting in a more precise localization. recently, a novel stereo feature extractors have been proposed, e.g., [17], which motivates us to consider them in s-ptam. an evaluation of the novel extractors is a subject of our future work. acknowledgements this work is a direct result of the bilateral cooperation program between the czech and argentinian republics support by the argentinian project arc/14/06 and travel support of the czech ministry of education under the project no. 7amb15ar029. the work of j. faigl is supported by the czech science foundation (gačr) under the research project no. gj15-09600y. references [1] g. klein, d. murray. parallel tracking and mapping for small ar workspaces. 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[7] m. agrawal, k. konolige, m. blas. censure: center surround extremas for realtime feature detection and matching. in eccv, vol. 5305 of lecture notes in computer science, pp. 102–115. springer berlin heidelberg, 2008. doi:10.1007/978-3-540-88693-8_8. [8] j. shi, c. tomasi. good features to track. in cvpr, pp. 593–600. 1994. doi:10.1109/cvpr.1994.323794. [9] e. rosten, t. drummond. machine learning for highspeed corner detection. in eccv, vol. 3951 of lecture notes in computer science, pp. 430–443. springer berlin heidelberg, 2006. doi:10.1007/11744023_34. [10] e. rublee, v. rabaud, k. konolige, g. bradski. orb: an efficient alternative to sift or surf. in iccv, pp. 2564–2571. 2011. doi:10.1109/iccv.2011.6126544. [11] m. calonder, v. lepetit, c. strecha, p. fua. brief: binary robust independent elementary features. in eccv, vol. 6314 of lecture notes in computer science, pp. 778–792. springer berlin heidelberg, 2010. doi:10.1007/978-3-642-15561-1_56. [12] s. leutenegger, m. chli, r. siegwart. brisk: binary robust invariant scalable keypoints. in iccv, pp. 2548–2555. 2011. doi:10.1109/iccv.2011.6126542. 49 http://dx.doi.org/10.1109/ismar.2007.4538852 http://dx.doi.org/10.1007/s11263-010-0361-7 http://dx.doi.org/10.1109/tro.2015.2463671 http://dx.doi.org/10.1023/b:visi.0000029664.99615.94 http://dx.doi.org/10.1007/11744023_32 http://dx.doi.org/10.1007/978-3-540-88693-8_8 http://dx.doi.org/10.1109/cvpr.1994.323794 http://dx.doi.org/10.1007/11744023_34 http://dx.doi.org/10.1109/iccv.2011.6126544 http://dx.doi.org/10.1007/978-3-642-15561-1_56 http://dx.doi.org/10.1109/iccv.2011.6126542 t. pire, t. fischer, j. faigl acta polytechnica ctu proceedings [13] t. krajník, p. de cristóforis, m. nitche, et al. image features and seasons revisited. in european conference on mobile robotics (ecmr). 2015. (to appear). [14] dzulfahmi, n. ohta. performance evaluation of image feature detectors and descriptors for outdoor-scene visual navigation. in acpr, pp. 872–876. 2013. doi:10.1109/acpr.2013.159. [15] a. schmidt, m. kraft, m. fularz, z. domagala. comparative assessment of point feature detectors in the context of robot navigation. journal of automation, mobile robotics and intelligent systems 7(1):11–20, 2013. [16] a. geiger, p. lenz, c. stiller, r. urtasun. vision meets robotics: the kitti dataset. ijrr 32(11):1231– 1237, 2013. doi:10.1177/0278364913491297. [17] r. arroyo, p. alcantarilla, l. bergasa, et al. fast and effective visual place recognition using binary codes and disparity information. in iros, pp. 3089–3094. 2014. doi:10.1109/iros.2014.6942989. 50 http://dx.doi.org/10.1109/acpr.2013.159 http://dx.doi.org/10.1177/0278364913491297 http://dx.doi.org/10.1109/iros.2014.6942989 acta polytechnica ctu proceedings 2:45–50, 2015 1 introduction 2 related work 3 local image features 4 overview of s-ptam 5 evaluation 6 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2016.5.0017 acta polytechnica ctu proceedings 5:17–21, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app design parameters of buffer stops petr guziur brno university of technology, faculty of civil engineering, veveří 331/95, 602 00 brno correspondence: guziur.p@fce.vutbr.cz abstract. paper discuses reasons of building buffer stops and situations that may occur in railway station leading to build safety tracks. also discusses parameters of buffer stops that enter its design, such as collision speed and kinetic energy absorbing capacity. furthermore, presents categories of buffer stops depending on principles of absorbing the kinetic energy and points pros and cons of each structure. keywords: buffer stop, kinetic energy, braking force, dead-end track. 1. introduction buffer stop is a device at the end of dead-end track or closed track with a purpose to stop the rolling stock. in czech republic it is allowed to use three types of buffer stops (according to national regulation čd ž9 [1]). all three types are fixed (rigid) construction, yet there are numerous designs of buffer stops used abroad. we can divide buffer stops in categories depending on the principles of absorbing the kinetic energy, which is the most important parameter of buffer stops. as basic categories we can name fixed buffer stops, hydraulic buffer stops and friction buffer stops. every type has its pros and cons and suitable place to be installed (depending on circumstances). 1.1. flank protection one of the places, where buffer stop has to be installed, is the end of safety track which represents direct flank protection of train paths. there are two types of flank protection of train path: • direct flank protection – protection of rolling stock from non-permitted ride of rolling stock from side approaching track – flank protection switch or derail is used, • indirect flank protection – protection of rolling stock from non-permitted ride of rolling stock from side approaching track – signals with prohibiting signal is used. and there are different conditions for flank protection of train path with speed up to 120 km.h−1 and above this speed. direct flank protection of train path with speed higher 120 km.h−1 is required: • from all sidings, • from all service tracks. in this case, rolling stock arriving from siding or service track should head to the safety track and probably has low speed at its end (by the buffer stop). another situation with possibility of higher impact speeds may occur on safety tracks from running tracks (see chapter 1.1.1). 1.1.1. mutually excluded train path amongst other conditions, safety and signalling plant of second or higher category has to forbid the simultaneous setting of train path for which the train path with higher speed than 120 km.h−1 meets, crosses or overlaps with continuation of another train path. this condition is crucial for direct flank protection. if there is no direct flank protection of the train path with speed higher than 120 km.h−1, one of train paths is not allowed to be set or the speed is restricted up to 120 km.h−1. speed restriction depends on possibilities of main signals (what speed can be signalled). in railway station, where restricted speed is used, the restriction brings speed to lower level, than in railway station, where no restriction is needed (with speed of 120 km.h−1). this issue causes regular delay of trains on daily bases, since not even system like kango is able to cope with this situation. the only result is to build flank protection switches not only from sidings and service tracks but even from running tracks where threat of the train path with speed higher than 120 km.h−1 occurs. 2. buffer stop’s design parameters as a crucial parameter for designing buffer stop is its kinetic energy absorbing capacity, thus stopping a rolling stock of certain mass with a certain collision speed. there are various situations of buffer stop’s location, therefore it is needed to approach the design individually. whether the buffer stop is at the end of a dead-end track in station by platform, or ends a safety track (either from sidings, service track or even running tracks). each situation gives us different speed and different type of train (its mass) that can run into a buffer stop. as mentioned above, amount of kinetic energy that buffer stop is able to absorb is the crucial parameter for its design. kinetic energy of moving rolling stock can be calculated as sum of the kinetic energy of transitional motion and kinetic energy of rotating parts of the rolling stock (1.). 17 http://dx.doi.org/10.14311/app.2016.5.0017 http://ojs.cvut.cz/ojs/index.php/app petr guziur acta polytechnica ctu proceedings vehicle groups vehycle types ρ[-] trains regular passengers or freight trains 0,06 electric motor unit 0,15 0,20 cars cars with mechanical traction transition 0,12 0,15 cars with traction motors 0,20 0,025 passengers cars 0,04 0,06 full freight cars 0,04 0,05 empty freight cars 0,1 0,12 locomotives steam 0,08 0,10 electric 0,20 0,30 motor 0,15 0,30 table 1. coefficient of rotating parts [2] speed [km.h−1] speed [m.s−1] impact mass [t] 100 200 300 400 500 600 700 800 900 1000 10 2,78 386 773 1159 1546 1932 2319 2705 3091 3478 3864 15 4,17 869 1739 2608 3478 4347 5217 6086 6956 7825 8694 table 2. examples of kinetic energy [kj] (1.) ekin,c = ekin,p + ekin,r (2.) ekin,p = 1 2mv 2 (3.) ekin,r = 1 2iω 2 with substitution equation (2.) and (3.) into equation (1.) and following modification it is possible to calculate kinetic energy of moving rolling stock, using equation (4.). (4.) ekin,c = 1 2m(1 + ρ)v2 • ekin,c ... total kinetic energy [j]; • ekin,p ... kinetic energy of transitional motion [j]; • ekin,r ... kinetic energy of rotating parts [j]; • m ... weight of rolling stock [kg]; • v ... collision speed [m.s−1]; • i ... moment if inertia [kg.m2]; • ω ... angular speed [s−1]; • ρ ... coefficient of rotating parts [-]. examples of kinetic energy are given in table 2 for buffer stop, as a device (structure) that has to work properly and must ensure high level of safety and reliability, we need to involve a safety coefficient in calculations. therefore, the buffer stop’s kinetic energy absorbing capacity has to be determined as follows: r >= ekin,ck • r ... buffer stop’s kinetic energy absorbing capacity [j]; • ekin,c ... total kinetic energy [j]; • k ... safety coefficient [-]. in table 3 are shown examples of safety coefficient graded by the level of protection and type of train according to austrian standards [3]. 2.1. collision speed the collision speed is defined as the maximum permissible speed in which trains may travel when colliding with buffer stop. there are various approaches, how to determine collision speed. german standard ds 800 01 [4] use the collision speed based on train type: • passengers trains: 15 km.h−1 • freight trains: 10 km.h−1 austrian standard dv b 53 [3] use the collision speed based on track type: • main line trains: 15 km.h−1 • empty passengers trains or shunting: 10 km.h−1 take an example how the collision speed can be calculated. driver is responsible to make a proper braking according to signals. by error he overlooks a presignal and has no information about decelerating the train. he starts to decelerate at the point of signal with prohibiting signal using the emergency brake. table 4 displays braking distances (using operating brakes and emergency brake) and speeds of trains at the end of dead-end track (model situation: assuming the distance between signal with prohibiting signal and buffer stop is 100 m). parameters for table 4: • * train will stop before the buffer stop, • os deceleration – 0,50 m.s−2 (2x unit 451/452) [5], • r, ex, ic deceleration – 0,45 m.s−2 (locomotive 363 + 8 cars type y) [5], 18 vol. 5/2016 design parameters of buffer stops type of train and security level k [-] passengers trains 1,5 freight trains and shunting 1,2 freight trains and shunting, when it is necessary to protect various systems which are located behand or nearby buffer stop 1,5 freight trains and shunting, in cases where there are traffic zones, structures or residential houses located behind or nearby buffer stop 1,8 preventing the fall of any train or rolling stock into abyss 2,0 table 3. safety coefficient [3] speed [km.h−1] braking distance [m] speed at the end of dead-end track [km.h−1] os r, ex, ic emergency braking os r, ex, ic emergency brake 50 192,90 214,33 40,19 35 37 * 60 277,78 308,64 57,87 48 49 * 70 378,09 420,10 78,77 60 61 * 80 493,83 548,70 102,88 71 72 13 90 625,00 694,44 130,21 82 83 43 100 771 857,34 160,75 93 94 61 table 4. deceleration of trains buffer stop type 6 cars of 15 t 1 car of 80 t rail buffer stop 1,0 km.h−1 1,6 km.h−1 concrete type "sudop" 0,7 km.h−1 1,1 km.h−1 concrete type "dsb" 1,0 km.h−1 1,6 km.h−1 table 5. resistances of buffer stops used in czech republic [1] • emergency brake deceleration – 2,40 m.s−2. 3. types of buffer stops 3.1. fixed buffer stops with mechanical bumpers fixed (rigid) buffer stop is one of the most used types of buffer stops considering its history as an oldest one. construction of fixed buffer stop consists of a block or frame fixed rigidly to the rails or the ground. as other constructions, fixed buffer stop has its pros and cons. one of advantages is that it can be placed at the end of the dead-end track, thus it does not reduce the usable length of the track. however, in this case cons prevail, such as low resistance and manner of deceleration. resistances (as a state of usability) of fixed buffer stops used in czech republic are shown in table 5. if the mass or speed is higher, either the buffer stop or the train is destroyed. assuming both buffer stop and rolling stock frame will be reinforced significantly, and therefore cannot deform, the deceleration figure 1. example of hydraulic buffer stop (oleo comp.) [7] is unacceptable (see table 6). 3.2. hydraulic buffer stop (fixed buffer stop with hydraulic bumpers) hydraulic buffer stops are similar in construction to fixed. consist of a block or frame fixed rigidly to the rails or the ground. hydraulic buffer stops absorb kinetic energy in gradual manner (depends on the type of the hydraulic bumpers). if the energy is higher than the bumper is able to absorb, buffer stop is destroyed. parameters of the buffer stop on figure 1: • kinetic energy absorbing capacity: 2688 kj, • bumpers stroke: 2400 mm. 3.3. friction buffer stop friction buffer stop is the most effective way to stop moving rolling stock. the way of absorbing the kinetic energy, thus decelerating the rolling stock is the most efficient and safe. not only the train decelerates in 19 petr guziur acta polytechnica ctu proceedings impact speed [km.h−1] impact speed [m.s−1] stroke of mechanical bumpers [mm] [6] 75 105 decelartion [m.s−2] overload decelartion [m.s−2] overload 5 1,39 6,43 0,66g 4,59 0,47g 10 2,78 25,72 2,62g 18,37 1,87g 15 4,17 57,87 5,90g 41,34 4,21g table 6. deceleration of train and overload on passengers on impact the fixed buffer stop figure 2. length needed for buffer stop placement and to ensure braking distance [8] gradual manner over a longer distance (time period), but the kinetic energy absorbing capacity could be very high. friction buffer stop generally consist of rigid steel frame with buffers, connected to rails using arresting devices (friction jaws). in case of collision, kinetic energy is transformed into heat by means of friction. therefore, energy absorbing capacity of friction buffer stop depends on the number of friction jaws, friction coefficient resp. braking force of jaws and length of braking. nevertheless, there is a disadvantage. friction buffer stop needs a braking distance, therefore cannot be placed at the end of the deadend track and shortens its usable length. moreover the track behind the buffer stop needs to be horizontally straight and contain no welds and joints or other obstacles over rails. notes for figure 2: • lv ... length needed for buffer stop placement and to ensure braking distance; • lb ... buffer stop length; • lw ... maximum braking distance. three types of friction buffer stops can be named: • friction buffer stop (without additional brakes), see figure 3; • friction buffer stop with additional brakes, see figure 4; • friction buffer stop with hydraulic bumpers (with/without additional brakes). notes for figure 3: (1.) collision triangle; (2.) breaking devices; (3.) buffers; (4.) device for returning the buffer stop to working position after collision; (5.) reinforcement; figure 3. friction buffer stop without additional brakes [8] figure 4. friction buffer stop with additional brakes [8] (6.) reinforcement. notes for figure 4: (1.) additional arresting devices for added braking; (2.) steel profile below rails for reinforcement of the track; (3.) jointed connection belts between arresting devices; (4.) lateral connection between arresting devices. 3.3.1. braking force braking force is the determining factor of friction buffer stop. as mentioned above, buffer stop must absorb high amount of kinetic energy. calculation of breaking force in case of friction buffer stops depends on numbers of arresting devices, braking force of each arresting device and maximum braking distance. r = nbfblw • r ... buffer stop’s kinetic energy absorbing capacity [j]; 20 vol. 5/2016 design parameters of buffer stops figure 5. rawie 16 zeb, stopping distance/impact speed/impactmass diagram, safety coefficient 1,0 and 1,5 [9] • nb ... number of arresting devices [-]; • fb ... braking force of a single arresting device [n]; • lw ... maximum braking distance [m]. braking force of friction buffer stop with additional brakes comes from formula up there. formula is modified considering braking force of additional brakes while braking distance of each additional arresting device is included separately. r = nz∑ i=1 2fbilw i • r ... buffer stop’s kinetic energy absorbing capacity [j]; • nz ... number of a pair of additional arresting devices [-]; • fbi ... braking force of a single arresting device, based on a braking distance [n]; • lw i ... length of braking distance of a pair of arresting devices [m]. an example of friction buffer stop’s braking effectiveness is shown in figure 5 (friction buffer stop without additional brakes with absorbing capacity of 640 kj.m−1). 4. conclusion many aspects have to be taken in account while designing buffer stop. one has to consider its location – ending of dead-end track in railway station, ending safety track from sidings, service track or running track. every scenario brings different requirements such as type of train, collision speed, impact mass etc. in general, three types of buffer stops are used, depending of the principle of absorbing the energy. fixed buffer stops are more than useless for higher collision speeds considering its manner of deceleration and its resistances. however, using fixed buffer stops is justified e.g. in shunting yards, where are low speeds and no passengers on board. as more appropriate ending of dead-end track is usage of hydraulic or friction buffer stop. resistances of those types are much higher than fixed buffer stops. both this construction decelerates train in gradual manner and no harm to the rolling stock or buffer stop itself is done if the design was precise. acknowledgements the paper was created with support of the project no. lo1408 "admas up advanced materials, structures and technologies" supported by the ministry of education, youth and sports within the targeted support of program "national program for sustainability i". references [1] čd ž9 železniční spodek, vzorový list železničního spodku, zarážedla. české dráhy, s.o., divize dopravní cesty, o. z. praha, 2001. in effect from: 2002-04-01. [2] j. široký. mechanika v dopravě i âăş kolejová vozidla [online]. updated 2003, [2016-01-13], http://homen.vsb.cz/~s1i95/mvd/skr_mvd.pdf. [3] ’́obb: dv b 53. die gestaltung von oberbauanlagen. [4] db: ds 800 01. bahnanlagen entwerfen allgemeine entwurfsrichtlinien. [5] l. fiala. provozní dopady aplikace ochranných vzdáleností podle tnž 34 2620 master thesis. university of pardubice, pardubice. supervisor pavel drda, 2010. [6] tnž 28 2605 kolejová vozidla – železniční. trubkové nárazníky s korýtkovým vedením. typy, základní parametry, technické požadavky, zkoušení. nymburk: čsd, 1991. in effect from: 1991-07-01. [7] oleo end stops. oleo international [online]. updated 2015-07-09, [2015-11-07], http://www.oleo.co.uk/products/end-stops. [8] israel railways ltd. railway buffer stops planning guidlines [online], 2009. updated 2013, [201511-10], http://www.iroads.co.il/sites/default/ files/imce/ir_buffer_stops_guidelines.doc. [9] rewie bahntechnik strassenbahn. rawie gmbh & co. kg [online]. updated 2015-08-20, [2015-11-07], http://www.rawie.de/index.php/de/bahntechnik/ strassenbahn. 21 http://homen.vsb.cz/~s1i95/mvd/skr_mvd.pdf http://www.oleo.co.uk/products/end-stops http://www.iroads.co.il/sites/default/files/imce/ir_buffer_stops_guidelines.doc http://www.iroads.co.il/sites/default/files/imce/ir_buffer_stops_guidelines.doc http://www.rawie.de/index.php/de/bahntechnik/strassenbahn http://www.rawie.de/index.php/de/bahntechnik/strassenbahn acta polytechnica ctu proceedings 5:17–21, 2016 1 introduction 1.1 flank protection 1.1.1 mutually excluded train path 2 buffer stop's design parameters 2.1 collision speed 3 types of buffer stops 3.1 fixed buffer stops with mechanical bumpers 3.2 hydraulic buffer stop (fixed buffer stop with hydraulic bumpers) 3.3 friction buffer stop 3.3.1 braking force 4 conclusion acknowledgements references 128 acta polytechnica ctu proceedings 2(1): 128–132, 2015 128 doi: 10.14311/app.2015.02.0128 investigating long-term behaviour of x-ray binaries using archival data m. m. kotze1,2, p. a. charles2,3 1south african astronomical observatory, p.o. box 9, observatory 7935, south africa (sa) 2astrophysics, cosmology and gravity centre (acgc), astronomy department, university of cape town, rondebosch 7701, sa 3school of physics & astronomy, university of southampton, southampton so17 1bj, uk corresponding author: marissa@saao.ac.za abstract long term modulations have been detected in a wide variety of both low and high-mass x-ray binaries. the all sky monitor on board the rossi x-ray timing explorer provides the most extensive (∼15 years) and sensitive x-ray archive for studying such behaviour. since those variations were often intermittent and/or aperiodic, we used a time-dependent dynamic power spectrum method to examine how the modulations themselves vary with time in a systematic way. some were found to be remarkably stable, while others show a range of properties, from even longer variability time-scales to quite chaotic behaviour. keywords: accretion discs x-ray binaries. 1 introduction kotze & charles (2012) contains the results of our timedependent period analysis on 25 x-ray binaries (xrbs) with reported long term variability. for the purpose of these conference proceedings, some of those results are reproduced herein to illustrate the importance of such an approach when dealing with varying periodic and/or aperiodic signals. we also use this opportunity to present some of the highlights contained in our previously published results. 2 data analysis 2.1 rxte/asm archival data the massachusetts institute of technology (mit) operated an all sky monitor (asm) on board the rossi x-ray timing explorer (rxte) from 1996 to 2012. the asm observed the x-ray sky with 3 rotating scanning shadow cameras (ssc) which scanned ∼80% of the sky during ∼90 min orbits. data were reduced and compiled weekly by the asm team and made publicly available 1 as dwell-by-dwell or one-day-averages in four energy bands, which includes a sum-band (1.5-12 kev). one-day-average data 2 are the dwell-by-dwell data binned into 1-day bins. archival asm datasets contain the lightcurves of all xray sources in the rxte catalogue. for full details see levine et al. (1996). 2.2 time-dependent period analysis periods are typically found by variability analysis of time-series/lightcurve datasets. while this approach may allow distinction between periodic and quasiperiodic behaviour, it contains no information regarding the variation or consistency of aperiodic/quasi-periodic signals. clarkson et al. (2003) presented results from their time-dependent periodic analysis on 4 x-ray binaries in the form of dynamic power spectra (dps). the method requires the datasets to be split into windows that are of sufficient length to allow detection of the maximum period considered. transition from one independent window to the next is smoothed (i.e. increased resolution) by adding sliding windows between the positions of adjacent independent data windows. lomb-scargle (l-s; lomb 1976 & scargle 1982) periodograms were produced for every data window and the results of all the periodograms for a source were plotted together in a density map, using the l-s power for each frequency plotted at every window’s mid-point along the time-axis. the frequency domain allowed appropri1http://xte.mit.edu/ and http://xte.mit.edu/asmlc.html 2i have made all their plots available on: http://www.saao.ac.za/∼marissa/lc/lc.html 128 http://dx.doi.org/10.14311/app.2015.02.0128 investigating long-term behaviour of x-ray binaries using archival data ate coverage over frequencies associated with previously reported periodic behaviour (table 1). since the dps method requires a significant number of computations, its application has been limited until recent advances in desktop technology allowed it to be employed more readily. figure 1: accretion disc stability to radiation-driven warping in xrbs, as functions of q and rb ( [ gm1 c2 ] ), adapted from ogilvie & dubus (2001) to include only xrbs with known super-orbital periods and updated with their latest system parameters (see table 1). squares indicate low-mass xrbs (lmxbs) and circles high-mass xrbs (hmxbs). tidally-induced disc precession (sec 3.4) may occur left of the dashed line. 3 results several mechanisms have been proposed to account for the super-orbital variations (psup) observed in xrbs. we list our results according to the mechanisms that have been considered most likely candidates for the cases included here. please refer to kotze & charles (2012) for more details. 3.1 radiation-induced disc warp/tilting ogilvie & dubus (2001) provided stability predictions for xrb accretion discs against radiation-driven warping/tilting. therein the binary separation (rb) and mass ratio (q = m2/m1) determine the location of a source on their predictive diagram, which is divided into zones where stable warps (between the dashed and solid line), chaotic warps (above the dashed line) or no warps (below lower solid line) are expected. a source near the transition boundary between the stable warp zone and the chaotic warp zone, may experience instability that could result in variable warps. table 1: system parameters for included xrbs source psup porb q rb/106 [days] [days] [m2 m1 ] [gm1 c2 ] her x-1 33-37 [1] 1.700 [2] 1.56 3.1 smc x-1 50-70 [3] 3.89 [4] 11.0 8.9 lmc x-4 30 [5] 1.41 [6] 10.6 4.5 cyg x-2 60-90 [7] 9.844 [8] 0.34 8.0 x1820-303 171 [9] 0.008 [10] [0.1] 0.1 ss433 162 [11] 13.10 [12] [1.0] [3.0] x1916-053 5 [13] 0.035 [14],[15] [0.1] 0.2 199 [16] [1] leahy & igna (2010), [2] tananbaum et al. (1972), [3] clarkson et al. (2003), [4] schreier et al. (1972), [5] lang et al. (1981), [6] chevalier & ilovaisky 1977, [7] clarkson et al. (2003), [8] cowley et al. (1979), [9] chou & grindlay (2001), [10] stella et al. (1987), [11] margon (1984), [12] crampton et al. (1980), [13] homer et al. (2001), [14] walter et al. (1982), [15] white & swank (1982), [16] priedhorsky & terrell (1984) figure 2: her x-1: this steady super-orbital period have been associated with a stable radiation-driven warp. 129 m. m. kotze, p. a. charles figure 3: smc x-1: the super-orbital period that is evolving dramatically over an even longer time-scale, may be associated with a radiation-driven warp that is variable. figure 4: lmc x-4: the steady long-term period may be produced by a stable radiation-driven warp. figure 5: cyg x-2: the unstable/chaotic behaviour may be associated with chaotic warping. 3.2 third body zdziarski et al. (2007) performed a comprehensive analysis of the triple system scenario and how binary eccentricity oscillations could modulate mass transfer through l1, finding agreement between theoretical and observed lightcurves for x1820-303. figure 6: x1820-303. 3.3 precessing relativistic jets ss433 is the prototypical microquasar. its precessing relativistic jets and their resulting ∼ 162 day superorbital period was obtained by hjellming et al. (1981) and margon (1984) from variations in the radial velocity measurements from balmer and he i emission lines. figure 7: ss433. 3.4 tidally-induced disc precession whitehurst & king (1991) described how tidal interactions with the donor may excite resonances in the accretion disc, causing it to precess and produce quasi130 investigating long-term behaviour of x-ray binaries using archival data periodic variations in the lightcurve. essentially the disc becomes elliptical, expanding beyond its critical radius while remaining within its roche-lobe radius, so that disc precession is effectively the result of changes in the orientation of this elliptical accretion disc with respect to the donor. figure 8: x1916-053. tidal disc precession depends on the mass ratio (q = m2 m1 ) and will only occur if q < 0.25 − 0.33, producing so-called “superhumps”, which have been detected in the su uma sub-class of cataclysmic variables (cvs). the vertical dashed line on fig. 1 indicates this boundary, to the left of which xrbs are expected to be susceptible to tidal disc precession (e.g. x1916-053 and x1820-303). 4 discussion the composite figure for each source contains a wealth of information to assist interpretation. the lightcurves are shown in the top panels and density maps with the dps results form the main panels, for which the scales are indicated to the right. the 99.9%-confidence white noise levels (green lines), together with the l-s for the entire datasets, are shown in the left panels. all included sources show significant (exceeding the white noise levels) periodic signals in their dps. previously reported periodicities (listed in table 1), indicated by red bars, are clearly present in the dps panels and often also in the l-s (left-hand) panels along with additional variability. 5 conclusions quasi-periodic or aperiodic signals should be investigated using time-dependent period analysis techniques. while these examples focussed on long-term superorbital behaviour of xbs, it should be immediately apparent how useful such a technique would be for investigating short-term quasi-periodic oscillations in cvs. acknowledgement asm results were provided by the asm/rxte teams at mit and at the rxte science operations facility and guest observer facility at nasa’s goddard space flight center (gsfc). this work formed part of my phd thesis, supervised by prof. phil charles and co-supervised by prof. brian warner, at the university of cape town (uct) and was funded by the national research foundation (nrf) of south africa. references [1] chevalier c., ilovaisky s. a. : 1977, a&a, 59, l9 [2] chou y., grindlay j. e. : 2001, apj, 563, 934 doi:10.1086/324038 [3] clarkson, w. i., charles, p. a., coe, m. j., laycock, s. : 2003, mnras, 343, 1213 doi:10.1046/j.1365-8711.2003.06761.x [4] cowley a. p., crampton d., hutchings j. b. : 1979, apj, 231, 539 doi:10.1086/157216 [5] crampton d., cowley a. p., hutchings j. b. : 1980, apj, 235, l131 doi:10.1086/183176 [6] hjellming, r. m., & johnston, k. j. : 1981, nature, 290, 100 doi:10.1038/290100a0 [7] homer l., charles p. a., hakala p., muhli p., shih i.-c., smale a. p., ramsay g. : 2001, mnras, 322, 827 [8] kotze, m. m., charles, p. a. : 2012, mnras, 420, 1575 doi:10.1111/j.1365-2966.2011.20146.x [9] lang f. l., et al. : 1981, apj, 246, l21 [10] leahy d. a., igna c. d. : 2010, apj, 713, 318 doi:10.1088/0004-637x/713/1/318 [11] levine, a. m., bradt, h., cui, w., et al. : 1996, apjl, 469, l33 doi:10.1086/310260 [12] lomb, n. r. : 1976, apss, 39, 447 [13] margon, b., anderson, s. f., aller, l. h., downes, r. a., & keyes, c. d. : 1984, apj, 281, 313 [14] ogilvie, g. i., & dubus, g. :2001, mnras, 320, 485 131 http://dx.doi.org/10.1086/324038 http://dx.doi.org/10.1046/j.1365-8711.2003.06761.x http://dx.doi.org/10.1086/157216 http://dx.doi.org/10.1086/183176 http://dx.doi.org/10.1038/290100a0 http://dx.doi.org/10.1111/j.1365-2966.2011.20146.x http://dx.doi.org/10.1088/0004-637x/713/1/318 http://dx.doi.org/10.1086/310260 m. m. kotze, p. a. charles [15] priedhorsky w. c., terrell j. : 1984, apj, 280, 661 [16] scargle, j. d. : 1982, apj, 263, 835 [17] schreier e., giacconi r., gursky h., kellogg e., tananbaum h. : 1972, apj, 178, l71 doi:10.1086/181086 [18] stella l., priedhorsky w., white n. e. : 1987, apj, 312, l17 doi:10.1086/184811 [19] tananbaum h., gursky h., kellogg e. m., levinson r., schreier e., giacconi r. : 1972, apj, 174, l143 [20] walter f. m., mason k. o., clarke j. t., halpern j., grindlay j. e., bowyer s., henry j. p. : 1982, apj, 253, l67 [21] whitehurst, r., & king, a. : 1991, mnras, 249, 25 [22] white n. e., swank j. h. : 1982, apj, 253, l61 doi:10.1086/183737 [23] zdziarski, a. a., pooley, g. g., & skinner, g. k.: 2011, mnras, 412, 1985 discussion koji mukai: can you clarify what you saw in x1916? it is a low q system, but i thought the disc precessesion period was about 5 days, while your plot showed only longer periods. marissa kotze: our dps analysis for this source show no significant periodic behaviour below 10 days. but this is not unexpected, since the 5 day period associated with tidal disc precession in x1916-053 was not determined from x-ray flux variations, but rather from optical variability and changes in the structure of the x-ray dips, which our dps analysis of rxte asm data is unable to detect. 132 http://dx.doi.org/10.1086/181086 http://dx.doi.org/10.1086/184811 http://dx.doi.org/10.1086/183737 introduction data analysis rxte/asm archival data time-dependent period analysis results radiation-induced disc warp/tilting third body precessing relativistic jets tidally-induced disc precession discussion conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0069 acta polytechnica ctu proceedings 7:69–71, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app performance of steel fiber reinforced concrete – comparability of tests according to dafstb-guideline "stahlfaserbeton" and en 14651 steffen anders∗, melanie schovenberg institute of structural engineering, bergische universität wuppertal, pauluskirchstr. 11, 42285, wuppertal, germany ∗ corresponding author: baustoff@uni-wuppertal.de abstract. for the determination of the performance of steel-fiber reinforced concrete (sfrc), the post-peak flexural strengths are used. in different national and european standards, different test-setups are defined, resulting in double efforts for testing for the manufacturers. in addition, the german national guideline "stahlfaserbeton (dafstb)" on sfrc is well established european-wide, but the test standard is specifically national, demanding a four-point-bending tests using unnotched beams. contrarily, the european standard en 14651 as well as the model code 2010 [1] demand three-point bending tests using notched specimens. applying the national guideline is obligatory in germany for structural use of sfrc. therefore, it is essential to standardize the performance evaluation of sfrc based on commonly applied international guidelines. in the following, an approach is presented especially dealing with the problem of random occurrence of cracks in the four-point-bending tests. it is shown, that neglecting the point of crack can systematically under-estimate the performance of sfrc especially at deformations. keywords: steel-fiber reinforced concrete, performance classes, post-peak flexural strength. 1. introduction in order to get permission to distribute and sell steelfibers in europe, a ce-certificate is obligatory. therefore, it is necessary to determine the performance of the steel-fibers in concrete, depending on the type of steel fibers as well as the fiber contents. in this case, the en 14651 [2] is the relevant standard, demanding a test using third-point loading on notched specimens. in order to get the permission to sell steel-fiber reinforced concrete e.g. as ready mixed concrete the performance of sfrc has to be evaluated according to the german national guideline "stahlfaserbeton (dafstb)" [3]. this guideline demands tests on unnotched specimens in a 4-point bending set-up. in both guidelines, performance of sfrc is measured in terms of post-peak flexural strengths. seen from the mechanical point of view the evaluation of post-peak flexural strengths is a fracture mechanical problem, demanding determination of strengths and load bearing capacities directly in the crack. this precondition is fulfilled only by en 14651 but not by the german guideline, because the crack can occur anywhere in the mid third of the beam due to the four-point-loading scheme. in order to overcome the problem of mechanical incorrectness as well as achieving international standardization, establishing a connection between the two test methods would be advantageous to facilitate the conversion of results from one method to another. one important aspect in this context is to include the point of crack into the evaluation according to the guideline "stahlfaserbeton". this aspect will be dealt with in the following. 2. test methods and evaluation of post-peak flexural strengths the most important difference between the national guideline "stahlfaserbeton (dafstb)" and the european standard en 14651 is the test set-up as shown in fig. 1. in the four-point loading test, which is demanded by the guideline "stahlfaserbeton (dafstb)", the crack should occur randomly in the mid third between the two loads due to lacking of a notch. the deflection of the beam is measured using transducers at mid-span. as described, due to this distance the testing method is not consistent from a fracture mechanical point of view. the method given in en 14651 uses a notched beam and just one load exactly above the notch at mid-span. thus, deflection and cracking are in-line. the evaluation of the post-peak flexural strength in the guideline "stahlfaserbeton (dafstb)" uses the mid-span deflection δ. in this guideline, the post-peak flexural strength is calculated from the load at two defined deflections of δ = 0.5 mm and δ = 3.5 mm at mid-span (see fig. 2-up). seen from point of view of fracture mechanics, the deflection at the point of crack is always higher than the deflection at mid-span, resulting in a systematic underestimation of the postpeak flexural strength, provided a strain softening behavior of the steel-fiber reinforced concrete. 69 http://dx.doi.org/10.14311/app.2017.7.0069 http://ojs.cvut.cz/ojs/index.php/app steffen anders, melanie schovenberg acta polytechnica ctu proceedings figure 1. comparison of test set-ups on the other hand, the en 14651 standard uses the crack mouth opening displacement (cmod) being directly correlated to the mid-span deflection [4]. to specify the post-peak flexural behavior, strength values at four different points are defined in terms of cmod (see fig. 2-down). the deflection at δ = 0.47 mm at cmod1 correlates well to the german guideline. cmod4 at a deflection of δ = 3.02 mm shows a difference of about 0.5 mm for the evaluation point. additionally, the cross-sections differs either, for the notch reduces the height of the cross section (both beams are produced with a cross-section of 150 × 150 mm). the approach of the en 14651 is consistent with respect to fracture mechanics, because the deflection is measured directly in the cracked crosssection. the shown differences in testing and calculating make it nearly impossible to compare the results of the guidelines. a special problem being the random cracking with german test set-up. 3. calculation approach to adjust the results taken during the tests according to the guideline "stahlfaserbeton (dafstb)" the point of the first crack has to be measured. if this is done the deformations measured at mid-span, can be transferred to the cracked cross-section by simply using theorem of intersecting lines applied on the larger part of the beam, assuming both parts of beam are not deformed themselves. fig. 3 shows that the deflection in the cracked cross-section is always larger than deflection at mid-span. the consideration of the point of the crack results in an increased stretching of the force-deflection curve. the correction of the curve increases with an increasing deflection during the test as well as with an infigure 2. evaluation of post-peak flexural strengths at different points. up dafstb-guideline "stahlfaserbeton", down en 14651 figure 3. calculation approach for taking the point of crack into account using the theorem of intersecting lines creasing distance of the crack from the middle of the beam. in fig. 4, the increased stretching can be easily seen especially at higher deflections. figure 4. change of mid-span deflection in case of strain hardening material at low deflections and strain softening at high deflections 70 vol. 7/2017 performance of steel fiber reinforced concrete depending on the effectiveness of the fibers (and on the fiber content), generally two different material behaviors are distinguished. either the material is strain hardening, meaning that the transferred load increases with an increasing deflection or the material is strain softening, showing decreasing transferable loads with increasing deflections. in fig. 4 the postpeak flexural strength for low deflections of about δ = 0.5 mm shows strain hardening. in case of strain softening, as can be seen at a deflection higher than about 1 mm a correction of the load-deflection curve leads to increasing post-peak flexural strengths. 4. results and discussion after measuring the point of crack of about 360 fourpoint bending tests, the resulting distribution of the point of crack is given in fig. 5. the displayed distance of the crack from mid-span does not differ whether the crack occurred left or right from the mid of the beam. assuming a perfectly homogeneous concrete, the crack should theoretically occur between the loads. an analysis of the point of the first crack shows, that only 50 % of all cracks occur in a distance less than 4 cm around the mid of the beam. at distances of less than 2 cm from mid-span, less than 25 % of all cracks occur. figure 5. distance of point of crack from mid-span applying the correction approach for the point of crack on several beams, the post-peak flexural strength values are affected as well. the larger the distance of the crack from mid-span the higher the correction, strain softening assumed. most of the beams have shown force-deflection curves comparable to fig. 4. as mentioned, these beams often show little strain hardening at low deflections. because the correction at δ = 0.5 mm is small, the post-peak flexural strength values are unaffected for a large number of beams. due to the slight strain hardening, the post-peak flexural strength values decrease for a number of beams. at larger deflections of δ = 3.5 mm the correction is higher, because of the higher deflection in combination with the strain softening. the mean increase ranges at about 0.15 n · mm−2, which is half a performance class. figure 6. effect of correction of post-peak flexural strength due to random cracking of beams tested according to dafstb guideline "stahlfaserbeton" 5. conclusions for the determination of performance of sfrc, different testing and evaluation approaches are used in germany and in europe. from a point of view of fracture mechanics, the german approach is incorrect, due to a random occurrence of the cracks predominantly in the mid-third. this leads to a systematic underestimation of the deflection in the cracked cross-section. therefore, it is essential to take the point of the first crack into account, leading to a stretching of the forcedeflection curve. two different modes of behavior can occur. for strain hardening, which is often found at low deflections and at higher fiber contents, the postpeak flexural strength can decrease, and for strain softening behavior, usually found for concrete having lower fiber contents as well as at higher deflections, the post peak flexural strength increases. taking the point of crack into account leads to an increase of about half a performance class on an average. in further steps, the results should directly be related to results from tests according to en 14651. additionally, the different geometries caused by the notches have to be taken into account. references [1] din en 14651: prüfverfahren für beton mit metallischen fasern bestimmung der biegezuggfestigkeit (proportionalitätsgrenze, residuelle biegezugfestigkeit) 2004. [2] deutscher ausschuss für stahlbeton (dafstb): dafstb-richtlinie stahlfaserbeton 2012. [3] fédération international du béton (fib): modelcode for concrete structures 2010. [4] b. barr, et al. round-robin analysis of the rilem tc 162-tdf beam-bending test: part 2 application of delta from the cmod response. materials and structures 36(263):621–630, 2003. doi:10.1617/13954. 71 http://dx.doi.org/10.1617/13954 acta polytechnica ctu proceedings 7:69–71, 2017 1 introduction 2 test methods and evaluation of post-peak flexural strengths 3 calculation approach 4 results and discussion 5 conclusions references acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0097 acta polytechnica ctu proceedings 4:97–101, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app quench front propagation in the annular channel jan štěpánek∗, vaclav bláha, vaclav dostál faculty of mechanical engineering, czech technical university in prague, technická 4, prague, czech republic ∗ corresponding author: j.stepanek@fs.cvut.cz abstract. understanding the quench front propagation during bottom core reflooding is crucial for the effective cooling during the loca accident. the results presented in this paper were obtained on an experimental loop with an annular test section. the test section consists of a vertical electrically heated stainless steel tube with outer diameter 9 mm and length of 1.7 m. the heated tube is placed inside a glass tube with the inner diameter 14.5 mm. water mass flux during the reflooding is in the range from 100 kg m−2 s−1 up to 140 kg m−2 s−1 and the initial wall temperature of the stainless steel tube is in the range from 250 ◦c up to 800 ◦c. the presented results show the influence of the initial conditions on the quench front propagation and the complexity of the phenomenon. keywords: quench front, rewetting, loca. 1. introduction cooling of very hot surfaces is still not satisfactorily described area. the main difficulty of this kind of cooling is that coolant can’t reach the hot surface because of a thin vapor layer generated between the hot surface and the coolant. this vapor layer acts as a thermal insulating gap and it prevents effective cooling. heat transfer in this gap is much lower than in rewetted area. as the surface cools down, the vapor layer collapses and coolant rewetts the surface. a high heat transfer rate takes place at this moment. the location where coolant, for example water, rewetts the surface is called the quench front. because of rapid cooling at the quench front, a heat accumulated in front of the quench front is conducted towards the rewetted area. this heat conduction accelerates the cooling of dry surface and it helps the quench front to advance forward [1]. the speed of this rewetting advance is called the quench front velocity. quenching takes place in many technical applications such as steel hardening, cryogenic technology and many others. one of the most crucial applications is a nuclear reactor safety. this phenomenon is dominant for safety during core reflooding phase of loca (loss-of-coolant accident). the temperature of the fuel cladding rapidly rises up (over 1200 ◦c [2]) after blow-down phase. then emergency core cooling system (eccs) starts to pump relatively cold water into the core. as the water reaches the hot fuel rods quenching appears [3]. this complicates effective core cooling. the quenching phenomenon has been solved analytically in many studies based on experimental data [4]. in these studies cooled geometry is usually divided into several regions. the most common approach divides the geometry into two regions. one region is dry region in front of the quench front. in this region a heat transfer coefficient is assumed as zero, i.e. adiabatic boundary condition. the second region is wet or rewetted region, where a heat transfer coefficient is taken as constant number [5]. this problem is then usually solved using wiener-hopf technique or heat balance integral method (hbim). there were many experimental efforts in the second half of 20th century. but many of these experiments were done for short geometries with limited range of initial wall temperatures [6]. the main goal of upcoming experiments is to cover wide range of initial wall temperatures, water mass flow rates and to describe effects of accumulated heat (different wall thickness and uneven tube heating) and geometrical elements such as spacer grids. in this paper a first set of experimental data is presented. 2. experimental loop for the purpose of quench front phenomenon investigation an experimental loop has been built. the loop consists of test section, dc power source, data acquisition system and variable hydraulic circuit. the test section is assembled from inner electrically heated steel tube and from outer glass tube. the steel tube is 1.7 m high and it is equipped with set of k-thermocouples (see tc1, tc2 and tc3 in fig. 1). these thermocouples are in contact with inner surface of the heated tube. the thermocouples in the wall are not calibrated and its precision is then ±2.5 ◦c but the precision of these thermocouples is not important because temperature time gradient is measured. the spacing between thermocouples is 0.5 m. the outer diameter of the steel tube is 9 mm, its wall thickness is 0.5 mm and the tube is made of x6crniti18 stainless steel. the outer glass tube has inner diameter of 14.5 mm and its wall thickness is 1.75 mm. it gives annular flow cross-section of 100 mm2. the test section is situated between lower and upper chamber. in these chambers are situated pressure sensors with accuracy of 0.5 % fso and calibrated class 2 k-thermocouples. initial wall temperature, water mass flow rate, lower chamber 97 http://dx.doi.org/10.14311/ap.2016.4.0097 http://ojs.cvut.cz/ojs/index.php/app j. štěpánek, v. bláha, v. dostál acta polytechnica ctu proceedings pressure, inlet temperature, power input and outer temperature of the glass tube (tcgl in fig. 1) are scanned during the experiment. the water mass flow rate is continuously measured by turbine flow meter. the precision of the flow meter is ±3 %. p tin tc1 tc3 tc2 q + tcgl figure 1. simplified experimental loop scheme. 3. setup the initial wall temperature of the experiment was in range from 250 ◦c up to 800 ◦c with step of 50 ◦c, the initial flow rate was set to 130 kg m−2 s−1 and its actual values are dependent on hydraulic characteristics of the test section during the experiment. this initial flow rate is adjusted in short circuit of the loop. firstly the steel tube is heated up to desired temperature. the thermocouple on the glass tube is used as an indicator of the stationary state. when the temperature of this thermocouple is constant, the reflooding begins. once the water reaches upper chamber, the experiment is finished. collected information are then evaluated on the pc. 4. quench front velocity in experimental studies quench front velocity is usually identified in several ways. one of these approaches is usage of time dependence of measured temperature on the cooled geometry. another approach for example uses optical methods such as high speed cameras. the quench front velocity was obtained as the distance between thermocouples (0.5 m) overcame in measured time. time, when a thermocouple has been rewetted is identified via maximum value of the first derivative of the measured temperature. this derivative value also represents position of the quenching temperature. when all rewetting times for each thermocouple are obtained, the quench front velocity can be calculated. 5. results each experiment was repeated five times. the measured temperatures and other experimental data were interpolated using piecewise cubic hermite interpolation polynominal (pchip). the quenching temperature has been calculated as an average from valid experimental data. in fig. 2 we can see the quenching temperatures for each initial wall temperature level and for each thermocouple. as can be seen this dependence is almost linear. the rewetting temperature of the first thermocouple behind the inlet is highest and for the last thermocouple is this temperature the lowest of all. this temperature drop is caused by two-phase mixture propelled by steam generated at the quench front. this mixture precools dry region of the heated tube and this precooled surface is then rewetted at lower temperature. initial wall temperature also strongly influences the value of the quench front velocity. higher wall temperature generates more steam at the quench front. on the one hand this steam helps to cool down the dry region but on the other hand this steam generates higher pressure drop and this leads to lower quench front velocity. but the most significant slowdown is caused by evaporated fraction of the inlet water mass flux. this dependence can be seen in fig. 3. from fig. 3 we can see, that quench front velocity drop is very significant between initial wall temperature levels 250 ◦c and 300 ◦c. from 300 ◦c this dependence is almost linear. for 300 ◦c the quench front velocity is 7.6 cm s−1 and for 800 ◦c 2.6 cm s−1. this velocity difference represents about 70 % velocity drop in this temperature range. with higher wall temperatures a significant pressure bump can be observed when the water meets the hot surface in the test section. this prompt pressure increase is caused by rapid steam generation at the quench front. the steam moves at high speed along the hot surface and the steam is then slightly overheated. these conditions lead to high pressure drop along the test section and it slows the quench front down. the pressure drop can be observed from initial wall temperature of 400 ◦c and it grows from 2 kpa up to 17 kpa at 800 ◦c wall temperature level. the value of the pressure bump was calculated as a difference between maximum pressure and uninfluenced pressure at lower wall temperatures in the lower chamber. this dependence is plotted in fig. 4. the maximum value of pressure bump at 800 ◦c represents nearly 90 % of pressure drop of the fully reflooded test section. also heat transfer rate at the quench front has been calculated. this heat transfer rate is calculated using first derivative of the wall temperature and material characteristics of the heated tube such as 98 vol. 4/2016 quench front propagation in the annular channel figure 2. rewetting temperature on initial wall temperature. figure 3. quench front velocity on initial wall temperature. heat capacity and electric resistance. using known difference of accumulated heat and known value of electric current a heat transfer rate at the quench front can be enumerated. when the heat transfer rate is known, the heat transfer coefficient can be also obtained from this heat transfer rate and from known quenching temperature and temperature of saturated water. resulting values of heat transfer coefficient are plotted in fig. 5. 6. experiment and real nuclear reactor the heated tube diameter corresponds to dimension of fuel rod of pressurized water reactor and its length is approximately halved. the results from the experiment give us the basis for estimating the quench front velocity as a local process. in a real nuclear reactor this process goes into complex spatial process. on the other hand a material used for the heated tube 99 j. štěpánek, v. bláha, v. dostál acta polytechnica ctu proceedings figure 4. pressure bump on initial wall temperature. figure 5. heat transfer coefficient at the quench front on initial wall temperature. also affects the quench front propagation. the use of zirconium alloy will probably significantly slow down the quench front propagation along the heated surface due to exothermic reaction of the zirconium and steam vapour approximately above 800 ◦c [7]. inclusion of this phenomenon is necessary for experimental efforts at very high temperatures in the future. the heat generation along the tube is constant in this effort but also an uneven heat generation will be investigated in the upcoming experimental work. this unevenness will affect the quench front velocity as well. 7. conclusions the presented results in this paper show the complexity of the quenching phenomenon for one coolant mass flux level and for range of initial wall temperature from 250 ◦c up to 800 ◦c in the annular channel. from these results can be concluded, that quenching velocities and rewetting temperatures are strongly dependent on the initial wall temperature. with increasing initial wall temperature the quench front velocity rapidly decreases. moreover increasing initial 100 vol. 4/2016 quench front propagation in the annular channel wall temperature goes with significant pressure bumps. these pressure bumps strongly influence the hydraulic characteristic of the heated channel and this leads to a big pressure drop in the channel. these effects can lead to unevenness of water flow through the core during loca. the unevenness can lead to cooling water flowing around the central area of the core, where the surface temperature is lower, and the central area of the core can be cooled down distinctly later. on the other hand, geometrical elements, such as spacer grids, create secondary quench fronts moving along the fuel rod [8]. due to these secondary quench fronts, the last rewetted point can’t be clearly determined. in other words, the water presence above the core doesn’t mean that the rest of the core is rewetted and cooled down. all these weaknesses of the quenching phenomenon should be uncovered for better handling of nuclear reactor accident. more experimental efforts will be done in the future. in these efforts a wide range of water mass flux will be covered. references [1] e. elias, g. yadigaroglu. a general one dimensionalmodel for conduction-controlled rewetting of a surface. nuclear engineering and design 42 (1977), 185–194. [2] m. billone, y. yan, t. burtseva, r. daum. cladding embrittlement during postulated loss-of-coolant accidents. u.s. nuclear rerulatory commision nureg/cr-6967, anl-07/04, 2008. http://www.nrc.gov/docs/ml0821/ml082130389.pdf [3] h.c. yeh. analysis of rewetting of a nuclear fuel rod in water reactor emergency core cooling. nuclear engineering and design 34 (1975), 317–322. [4] s.k. sahu, p.k. das, s. bhattacharyya. analytical and semi-analytical models of conduction controlled rewetting: a state of the art review. thermal science 19 (2015), 1479–1496. doi:10.2298/tsci121231125s. [5] s. olek. on the two region model with a step change in the heat transfer coefficient. nuclear engineering and design 108 (1988), 315–322. [6] a.k. saxena, v. venkat raj, v. govardhana rao. experimental studies on rewetting of hot vertical annular channel. nuclear engineering and design 208 (2001), 283–303. doi:10.1016/s0029-5493(01)00356-9. [7] j. belle, m.w. mallett. kinetics of the high temperature oxidation of zirconium. j. electrochem. soc. 101 (1954), 339–342. doi:10.1149/1.2781278. [8] j. stepanek, v. blaha, v. dostal, p. burda. the effect of spacer grid’s elements on the rewetting velocity. in proceedings of international conference on nuclear engineering (icone23). new york: asme, 2015. isbn 978-4-88898-256-6. 101 http://www.nrc.gov/docs/ml0821/ml082130389.pdf http://dx.doi.org/10.2298/tsci121231125s http://dx.doi.org/10.1016/s0029-5493(01)00356-9 http://dx.doi.org/10.1149/1.2781278 acta polytechnica ctu proceedings 4:97–101, 2016 1 introduction 2 experimental loop 3 setup 4 quench front velocity 5 results 6 experiment and real nuclear reactor 7 conclusions references acta polytechnica ctu proceedings doi:10.14311/app.2017.11.0070 acta polytechnica ctu proceedings 11:70–73, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app the detailed priority of international freight expresses in the overlapping section of rfc 7 and rfc 9 kolín – choceň přemysl šrámek∗, tatiana molková university of pardubice, jan perner transport faculty, department of transport technology and control, studentská 95, 532 10 pardubice, czech republic ∗ corresponding author: premysl.sramek@student.upce.cz abstract. the main goal of this article is to research the optimal priority of international freight expresses, especially on european freight corridors. this article shows this problem in the context in the overlapping section of rfc 7 and rfc 9 kolín – choceň. there is solved changing priority of freight expresses in detail, whereas other train priorities are the same. keywords: capacity, freight expresses, freight corridors, timetable stability. 1. introduction one of the aims of european transport policy is to redirect capacity of road freight traffic to other modes of transport, where rail transport is an interesting and environmentally friendly alternative, especially in terms of speed, availability and amount of transported cargo. on the other hand, by customers is required delivery time is guaranteed by carriers, what is unfortunately not always possible, especially due to high utilization of european rail infrastructure. the solution is the construction of new lines, increasing the capacity of existing lines through construction and reconstruction measures or through operational measures. among the operational measures may be included alternative routing of trains as well as changing priorities of a particular type of train, e.g. train category fex (freight express) [1]. the aim of this article is to find the optimal priority of international freight expresses to satisfy the customers required delivery times due to optimization of train priority. 2. materials and methods there are mentioned some information about european freight corridors rfc and the simulation method with using of simulation tool simut (average delay increment (adi) calculation). 2.1. rail freight corridors (rfc) on the basis of the european parliament and the eu council no. 913/2010 for competitive freight and no. 1316/2013, which is created the connecting europe facility (cef), is the gradual establishment of rail freight corridors rfc (rail freight corridors). the main aim of the operation of these corridors is to strengthen the competitiveness of railways synergies between rail systems and harmonization of allocation interstate freight routes by national infrastructure managers [2]. czech republic, respectively czech railway infrastructure administration (cria), as the infrastructure manager and allocator of capacity, is a member of rfc 5 (baltic – adriatic), rfc 7 (orient / eastmediterranean), rfc 8 (north sea – baltic) and rfc 9 (czechoslovak corridor). each corridor is operated on the basis of the corridor information document (cid); each corridor has a single point of contact (c oss) and allows carriers to apply international prearranged train paths facilitated freight via c-oss. the request must be filed by information system rne pcs and must include the cross-border section. this paper deals with the model study of common section of rfc 7 and rfc 9 kolín choceň. 2.1.1. rfc 7 rfc 7 – the orient corridor runs from central europe to easternand southern-europe connecting 7 member states – czech republic, austria, slovak republic, hungary, romania, bulgaria and greece. the total length of main lines is approx. 3900 km and the length of alternative and connecting lines is almost 2500 km altogether. most limiting factors of rfc 7 are low capacity, speed limit, limited length of trains, limited axle load, not electrified sections and lack of adequate safety equipment (signalling track circuits with 25 hz frequency, etcs, gsm-r, etc.). the railway infrastructure managers and capacity allocation companies responsible for establishing and running rfc7 are committed to offer reliable, high-quality, competitive transport services in order to increase the market demand, to operate the infrastructure costeffectively on the long run through harmonization of technical and procedural conditions and to facilitate the environmentally sustainable development of the european economy and the achievement of a better quality of life for its people (3). in capacity analysis, published in implementation plan of rfc 7 [3], there are found lines with capacity utilization higher than 90 %. the longest sections with this high capacity 70 http://dx.doi.org/10.14311/app.2017.11.0070 http://ojs.cvut.cz/ojs/index.php/app vol. 11/2017 the detailed priority of international freight expresses utilization are situated in the czech republic, concretely sections poříčany – pardubice (65 km) and choceň – česká třebová (25 km). 2.1.2. frc 9 rfc 9 – the czech-slovak rail freight corridor (cs corridor) runs from prague to čierna nad tisou (slovak-ukrainian border) connecting 2 member states – czech republic and slovak republic. the total length of main lines is 972 km and the length of alternative and connecting lines is 276 km altogether. most limiting factors of rfc 9 are the same as in rfc 7. in capacity analysis, published in implementation plan of rfc9 [4], there are found lines with capacity utilization higher than 90 %. 2.2. the simulation method in this part is said something about the simulation method in context of the transit of international freight express trains (fex) in the overlapping section of rfc 7 and rfc 9 kolín – choceň. in this section there are a total amount of 10 railway stations, in which it is possible overtaking trains (double track line). interstation sections are divided by an automatic block into track sections; all crossing safety devices are equipped with gates. for simulation was used simulation tool simut, developed by pavel krýže, phd. from cria. the simulation tool simut is developed in visual basic, therefore it can run on every pc with microsoft office. it has to be input the option of a simulation, then railway stations and their shortcuts, station tracks for each railway station, line tracks, connection of station and line tracks, length of interstation departments and amount of line departments, type of train for priority, type of train for each number of a train and the path of each train. the simulation program simut can put new paths in a daily timetable with the solution for arisen path conflicts [1]. it was used daily timetable 2016, which included the amount of 384 trains. the similar topic was solved in (1), but not so exactly, in the evaluation there were used for fex only the importance values 0.5; 1.7; 1.9 and there was created periodic timetable. in the table 1 are displayed the importance values of trains, which remain the same, and the importance value of fex is increasing from 0.5 to 2.0 through step 0.1. therefore, it was solved 16 simulations, every simulation had 365 simulation runs (whole timetable period). about train types in table 1 – en means euronight train, sc is supercity train, ec – eurocity train, ic – intercity train, r is fast train, sp – speed-up passenger train, os – stop passenger train. the remaining train types are types of railway cargo transport – nex is here fex and its importance value is variable (the research object). pn is normal cargo train and mn means slow cargo trains servicing e. g. sidings. within the simulation program was established the average delay increment (adi). the average delay figure 1. adil in the relation with fex importance value. increment was calculated by dividing the difference between total output and total input delay and the total number of trains. this indicator was calculated as an ongoing basis for each simulation run, so the total for the entire graph (all simulation runs). the indicator was also calculated for different types of transport, i.e. for long-distance passenger transport (adil), regional passenger transport (adir) and freight transport (adif). as part of the simulation was set for all simulation runs random entry delay based on the exponential probability distribution. there were solved conflicts of station tracks, freight trains were allowed to ride before their schedule time (in the case of free capacity) [1]. 3. results and discussion in the table 2 there are displayed timetable stability indicators (adi, adil, adir, adif) in the relation with changing importance value of fex. all timetable stability indicators have unit min/train, it means every train of the category should get this delay in minutes. the timetable stability indicators are in the relation with fex importance value compared on the figure 1 (adil), figure 2 (adir), figure 3 (adif) and figure 4 (adi). adil is with increasing fex importance value just always increasing and it is logical – cargo transport has more and more preference. in the case, when fex importance value is the same as the ex importance value, it means 2.0, is adil strongly rising to 9.31 min/train. against fex important value 1.9 (4.39 min/train) is twofold value – the result is fex can’t have higher or the same priority as ex. on the figure 1 there is created the linking curve with the equation and reliability. for adil has the highest reliability exponential linking curve. on the figure 2 there is displayed adir – in this case is evaluation very difficult. the linking curve reliability is the best for polynomial linking curve. over 1.5 fex importance value is adir affirmative, the best compromise is for fex importance value 1.3 – adir is – 0.27 min/train. the result is fex should 71 přemysl šrámek, tatiana molková acta polytechnica ctu proceedings train type en sc ec ic ex r sp os sv nex pn mn lv importance value 2.5 1.8 3.0 2.8 2.0 1.8 1.5 1.0 0.3 var. 0.1 0.03 0.08 table 1. the train importance values. fex importance value adil adir adif adi 0.5 1.04 -0.54 1.19 0.84 0.6 1.19 -0.61 1.63 1.07 0.7 1.36 -0.37 1.21 1.02 0.8 1.42 -0.30 1.12 1.02 0.9 1.47 -0.51 1.31 1.09 1.0 1.88 -0.31 0.46 0.97 1.1 2.02 -0.08 0.31 1.01 1.2 2.22 -0.12 0.39 1.12 1.3 2.60 -0.27 -0.38 0.96 1.4 2.50 -0.06 0.79 1.42 1.5 3.05 0.05 0.25 1.47 1.6 3.08 0.01 0.57 1.60 1.7 3.00 0.06 -0.17 1.28 1.8 4.46 0.31 -0.36 1.89 1.9 4.39 0.01 -0.72 1.67 2.0 9.31 0.53 -1.44 3.66 table 2. timetable stability indicators in the relation of changing fex importance value. figure 2. adir in the relation with fex importance value. have higher priority than regional passenger trains, especially than stop passenger trains. the linking curve reliability for adif is the best for polynomial linking curve. from 1.7 fex importance value is adif always negative and decreasing, but negative is for 1.3 fex importance value, too. the result is here not so clear. on the figure 4 there is displayed average delay increment for whole timetable. in every case is the timetable unstable, adi is affirmative, the output delay is higher than the input delay. the linking curve has really high reliability for polynomial. for 2.0 fex importance value is adi getting really high due to increasing adil. less than 1 min/train is adi only in 3 cases – for fex importance values 0.5, 1.0 and 1.3. the best adi is for 0.5 (0.84 min/train), but figure 3. adif in the relation with fex importance value. figure 4. adi in the relation with fex importance value. it is in contrast with higher fex priority than regional passenger trains priority. the second best adi is for 1.3 (0.96 min/train), adil is 2.60 min/train, adir is – 0.27 min/train and adif is – 0.38 min/train. according to previous results the total result for best possible timetable stability is to set the fex importance value for chosen timetable to 1.3. and it corresponds the rules of prescription cria d1 [5], where the fex trains have importance between stop and speed-up passenger trains (1.0 – 1.5). 4. conclusions it was checked in detail the relation between the importance of fex trains and timetable stability. there were made 16 simulation variants in simulation program simut and then compared results. the research result is clear – for timetable 2016 in the overlapping section rfc 7 and rfc 9 kolín – choceň is necessary for best possible timetable stability to set the fex importance value (priority) to 1.3, it means between stop passenger trains priority and speed-up passenger trains priority. it corresponds in the czech republic 72 vol. 11/2017 the detailed priority of international freight expresses the contemporary prescription statement – it suffices only to keep it. acknowledgements this paper is supported by sgs. references [1] p.šrámek, t.molková. the priority of international freight expresses in the overlapping section of rfc 7 and rfc 9 kolín – česká třebová. studentská vědecká konference interoperabilita v železniční dopravě iricon 2016 – sborník, 2016. isbn 978-80-01-05939-5. [2] r.čech, m.šlachtová. železniční nákladní koridory rfc. železniční magazín czech raildays, m-presse plus, s. r. o., 2015. issn 1212-1851. [3] rfc 7 orient corridor, implementation plan of rail freight corridor 7 orient corridor [online], 2015. [cit. 2015-20-11]. [4] rfc 9 cs corridor, implementation plan of rail freight corridor 9 [online], 2013. [cit. 2015-23-11]. [5] sždc. d1 dopravní a návěstní předpis. sždc, s. o., 2013. 73 acta polytechnica ctu proceedings 11:70–73, 2017 1 introduction 2 materials and methods 2.1 rail freight corridors (rfc) 2.1.1 rfc 7 2.1.2 frc 9 2.2 the simulation method 3 results and discussion 4 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.12.0013 acta polytechnica ctu proceedings 12:13–23, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app affective computing and augmented reality for car driving simulators dragoş datcua,∗, leon rothkrantzb,c a twnkls, groothandelsgebouw, stationsplein 45, rotterdam, the netherlands b intelligent interaction, delft university of technology, mekelweg 4, delft, the netherlands c faculty of transportation sciences, czech technical university in prague, konviktská 20, prague 1, czech republic ∗ corresponding author: email@dragosdatcu.eu abstract. car simulators are essential for training and for analyzing the behavior, the responses and the performance of the driver. augmented reality (ar) is the technology that enables virtual images to be overlaid on views of the real world. affective computing (ac) is the technology that helps reading emotions by means of computer systems [1][2][3], by analyzing body gestures, facial expressions, speech and physiological signals. the key aspect of the research relies on investigating novel interfaces that help building situational awareness and emotional awareness, to enable affect-driven remote collaboration in ar for car driving simulators. the problem addressed relates to the question about how to build situational awareness (using ar technology) and emotional awareness (by ac technology), and how to integrate these two distinct technologies [4], into a unique affective framework for training, in a car driving simulator. keywords: affective computing, augmented reality, serious gaming, car driving simulator. 1. introduction due to its capability to improve perception of reality, to support collaboration, a visual display of virtual objects, and to enable transitions between real and virtual environments, augmented reality (ar) technology can be used to create novel interfaces for face-to-face and remote collaboration for training [5][6]. affective computing-based technologies for car driving simulators have capability to lower the cost of accessing the expertise (by reducing a need to move trainers to where their expertise is needed), and to increase availability of expertise. this applies primarily to multi station driving simulators. ar technology can support new types of visualization and can help to develop new learning experience for the trainee. the whole driving simulation can be rendered using ar, using ar glasses, screens or windshield projections. by using augmented reality, the trainee can be presented various stimuli taking the form of virtual representations. in addition, visual notifications can be presented, as generated automatically by the system or as specifically instructed by expert. in addition to augmented reality, reading driver’s affect by affective computing technology has capability to adapt the simulation given the affect state of the trainee. 1.1. augmented reality augmented reality [7] is a technology that enables virtual images to be overlaid on views of the real world. due to its capability to improve the perception of reality, to support teamwork, visual display of virtual objects, and to enable transitions between real and virtual environments, the augmented reality can be used to create novel interfaces for face-to-face and remote collaboration. for example, ar enables users to see virtual representations of remote people in front of them and have spatial interactions with them, as if being there in person. wearable computers and cameras can be combined with augmented reality information display to support remote collaboration and to significantly improve performance on physical tasks. however, new research on interaction paradigms, presence and situational awareness needs to be conducted to create an augmented reality system that naturally enhances collaboration and establishes virtual co-location. in this case, situational awareness is defined as perception of given situation, its comprehension and prediction of its future state. 1.2. affective computing affective computing (ac) is a technology that "relates to, arises from, or deliberately influences emotions" [8]. emotions guide cognition to enable adaptive responses to the environment, and can have a major impact on the perception, attention, memory and decisionmaking. also, affect can have a significant impact on the driving behavior [9]. the affect reading by computer systems [1][2][10][3] is realized through the analysis of body gestures, facial expressions, speech and physiological signals. 13 http://dx.doi.org/10.14311/app.2017.12.0013 http://ojs.cvut.cz/ojs/index.php/app dragoş datcu, leon rothkrantz acta polytechnica ctu proceedings figure 1. ar trainee using the car driving simulator figure 2. training session including one trainer and two trainees. 1.3. hybrid ar-ac for car driving simulations the research aims to find solutions to specific challenges regarding integration of the affective computing technology with the augmented reality technology, with application in car driving simulations. the motivation of this approach comes from lack of understanding on emotional awareness models in arbased interactions between trainees and trainers, in a computer supported collaborative setup. previous studies [4], [11] indicate advantages of combined ar/vr and ac for different scenarios. the research aims to address the following questions: • what are the best means for sensing and collecting affect data from the car drivers engaged in driving training sessions? three sensing hardware will be investigated first, namely e-health sensor [12], cortrium [13] and empatica e4 wristband [14]. multimodal approaches for affect recognition will be studied. • which models and (contact and non-contact) sensors are best suited for affect reading in car driving simulators? • how can existent models be adapted in a data-fusion approach?, considering: . physiological sensors (i.e. heart rate, galvanic skin response, respiration rate, temperature, etc.), . facial expressions (from environmental cameras), with occlusion of the eye region by ar headset, . emotion in speech (prosody). • how to build emotional awareness among trainees and the expert/the trainer? how to integrate and maintain emotional awareness? • how to integrate and maintain emotional awareness and operation-specific situational awareness? • what performance oriented model can be built to automatically adapt the ar system support (such as user interface, etc.) for a human-to-human interaction in virtual co-location, given the emotional awareness? • in which way can (free-hands) hci for ar/vr headsets benefit from emotional awareness, targeting the individual performance during collaboration? • how to adapt existent interaction models? • which is the appropriate affect multimodal framework to support remote collaboration in ar/vr? • how to adapt shared memory spaces to support affect-driven virtual environments? • how to store, transfer and represent audio-video data and affect data, in a multi-user secure environment, with robustness to network breakdowns? • what data-fusion models are to integrate multiple (marker-less) tracking (slam) independent systems for ar? • what driving performance model can be built to automatically adapt the ar system support (such as the user interface, etc.) given the emotional awareness? using this, for instance the ar-based simulation can be dynamically adapted according to the trainee’s affect state, so that to increase drive learning performance. • how to improve the (marker-less) tracking in the shared virtual environment to cope with rather high operational pace of security teams, and with large illumination variation? . rgb-d tracking models section 2 presents a previous research on remote collaboration by augmented reality. section 3 presents the model that integrates affective computing technology and an augmented reality technology. section 4 details on aware, an affect-driven collaboration framework to support car driving simulations in augmented reality. section 5 presents hardware and software components for affect reading during car driving simulation. the last section emphasizes on conclusions and future work for the research on combined augmented reality and affective computing technologies. 14 vol. 12/2017 affective computing and augmented reality for car driving simulators 2. related work there have been car driving simulator-related approaches for rule-based systems that predicts in real-time the driver’s intent [15] or for driver vigilance monitoring [16][17] applied to enhance safe driving experience. moeslund et al. [18] propose arthur, an ar meeting system that permits multiple users wearing hmds at a round table, to interact with objects specific to architecture and an urban planning domain. the interaction with augmented world is in two ways, using physical objects placeholder objects and a wand, and by hand gestures. dong et al. [19] propose arvita, an advanced collaborative ar tool with problem solving capabilities to be applied in classroom and in professional practice. in these scenarios, multiple users wearing hmds and sitting around a table are able to perform interaction and to visualize dynamic simulations of engineering processes overlaid on the surface of the table. the work of wang and dunston [17] advances two ar based systems for remote collaboration and a face-to-face co-located collaboration in the scenario of detecting design errors. jailly et al. [20] presents an ar system for enhancing the comprehension of the manipulated remote devices in distance learning domain that allow for communication between both students and teachers. ferrise et al. [21] tackle the domain of maintenance operations of industrial product. in addition to using vr technology to support an operator to learn performing maintenance operations by combining traditional instruction manuals with simulation, the ar technology is employed to extend the scenario to tele-assistance. a vr-based skilled operator guides from the distance a trainee that is equipped with ar technology already displaying instructions on top of real product. nilsson et al. [22] propose an ar tool to improve collaboration between actors from different organizations such as the rescue services, the police and military personnel in a crisis management scenario while the same time sustaining individual needs. yabuki et al. [23] present a system in the early phase of development, aiming at supporting the cooperation between people working outdoor on environmental issues. the information provided to the users wearing hmds relates to 3d representations of temperature distribution and wind distribution, velocity and direction. alem et al. [24] propose remote, a remote guiding system that integrates non-mediated hand gesture communication in the mining industry. the work scenario of the system implies the expert remotely assisting a worker using the hands to point to certain locations and to show specific manual procedures. testing and validation of four early user interface design iterations aimed at maintenance tasks for repairing a photocopy machine, removing a card from a computer mother board and assembling a lego toy. wichert [25] describes a mobile collaborative ar environment that uses web technologies. the collaborative environment allows a 3d game like tetris to be played in real time by several users wearing hmds. the players can be located in the same room, with possibility for extending the collaboration with a remote player. the game setup provides support for studying the two types of ar based collaboration: the co-located cooperative interaction with skilled workers, each having a different view of the ar world and the indirect interaction with remote expert that has the same view as the skilled worker. in a similar way, datcu et al. [4][5] propose an ar based scenario of playing a game collaboratively, to study complex problem solving by physically co-located and virtually co-located participants. within the game, the goal of jointly building a tower of coloured blocks represents an approximation of a shared task. individual expertise is modelled as possibility to move blocks of a distinct colour and shared expertise is modelled by possibility of all players to move blocks of same colour. by scaling down real-life, more complex problems, the study compares presence, workload and situational awareness in real world and ar collaboration scenarios. additionally, datcu et al. [6][7] developed a platform for tele-collaboration by ar for supporting teams in the security domain. schnier et al. [26] focus on studying the issues around establishing joint attention toward the same object or referent, in a physically co-located collaboration ar environment. gu et al. [27] conduct a study on the impact of 3d virtual representations and use of tangible user interfaces as support for synchronous design collaboration using the ar technology. the results indicate that the change from a physically co-located working environment to the virtual co-located scenario encourages the ar users to smoothly move between working on the same tasks and working on different tasks or different aspects of the design process. the current state of the art on collaboration in ar provides relevant examples for ar based models that support a synchronous collaboration among users either being physically or virtually co-located, using free-hands or tangible interaction, static or mobile, or either using hmds or other display devices. these research outcomes, however, have to be still investigated in car driving simulation domain, especially with regard to remote visualization, spatial interaction and remote authoring in training scenarios. 3. model augmented reality systems are not limited to use of head-mounted devices and mainly have to combine real and virtual objects be interactive in real-time 15 dragoş datcu, leon rothkrantz acta polytechnica ctu proceedings and to register objects within the 3d. due to the capability: • to improve perception of reality, • to support teamwork process, • to support manual annotation by virtual objects, • to support an interaction between virtual and augmented environments, the technical solutions based on augmented reality have the potential to enhance novel interfaces for a computer-aided collaborative process, in face-to-face and remote collaboration scenarios. augmented reality systems can be used to establish the experience of being practically co-located by means of simulated presence. augmented reality systems have been used to allow experts to spatially collaborate with others at any other place in the world without traveling and thereby creating the experience of being virtually co-located, e.g. in the field of a crime scene investigation [6],[28]. the affective computing technology makes use of measurements from (contact and non-contact) physiological body sensors to automatically recognize in real-time, the affect of the field personnel. the affect data is further on used to automatically: • improve interaction in augmented reality (for the field personnel), • increase immersion and situational awareness for spatially distributed users in the virtual reality [29] and augmented reality [30]. from the hardware point of view, a solution is to use a microsoft hololens ar head mounted device (hmd) (see figure 3) that has a depth sensor already integrated. figure 3. standalone hololens ar device [31]. the investigation first considers a closed-loop arac model for the virtual reality, proposed by wu et al. [11]. next, the closed-loop model is adapted for augmented reality. 3.1. closed-loop architecture according to the yerkes-dodson law, the performance in mental tasks is dependent on arousal in the form of a non-monotonic function (figure 4). the performance increases with arousal, given arousal is at low levels, reaches the peak at a given arousal level and decreases after that optimal level. figure 4. yerkes-dodson-law the closed-loop system consists of three components namely affect recognition component, affect-modeling component and affect control component. these components are displayed in figure 5. the affective computer-aided collaboration approach based on augmented reality for car driving simulators, consists of three components namely: • the affect recognition component, • the affect-modeling component, and • the affect control component. figure 5. closed-loop affective computing architecture for augmented reality. 3.1.1. affect recognition the affect recognition component performs the assessment of the user’s affect by analyzing different body signals such as psychophysiological signals and facial expressions, emotion in speech, etc. ideally, these techniques to sense the trainee’s affect state should be working in real-time, should be automatic, noncontact, non-invasive and should have a high accuracy. multi-modal approaches aggregate data from different types of sensors to decrease the error over estimated affect states. 16 vol. 12/2017 affective computing and augmented reality for car driving simulators 3.1.2. affect modeling the second component, the affect modeling creates a relationship between the trainee’s affect and the features of the user’s environment. this component determines how the trainee’s affect should be changed, given her/his profile, the known arousal level for the optimal learning performance. this mapping is further used to identify car driving simulation parameters including the ar settings and the scenario and training session stimuli. 3.1.3. affect control the third component, the affect control provides the means for adapting the environment in such a way to get the trainee to the target affect state. this component can be semi-automatic, especially in scenarios including a human expert, such as in car driving simulation when the trainer can change the course of the training session with new stimuli that fit better the learning procedure. given the car driving simulation parameters previously determined, this component applies selected changes. the aim is by applying these changes, the trainee’s affect is changed towards the arousal state that is associated with optimal learning performance. in order to optimize the car driving performance, the three components of sensing, modeling and control adjust the functionality of the car driving simulator according to the trainee’s affect state. 4. affective framework for augmented reality virtual co-location relies on the augmented reality technology [32][33] to create spaces in which the trainer, the trainees and the objects are either virtually or physically present: it allows people to engage in spatial remote collaboration. an affect-driven collaboration framework supports the virtual co-location technique for the trainee and for the trainer, the collection and processing (especially the data fusion) from the low/sensory level to the high semantic levels. in the following text, the trainee is referred to as the local user and the trainer is referred to as the remote expert. the framework is called affective framework for augmented reality aware. the aware framework has been developed with the goal to support computational demands and multi-modal data streams among running applications and data processing modules. aware is a highly scalable, modular and parallel environment for a distributed collaboration using ar (the diagram in figure 6). it is developed to support virtual co-location of multiple users playing different roles in well-defined scenarios. the following text describes aware in detail. figure 6. aware framework for adaptive ar training. 4.1. local and remote user applications aware is based on a centralized architecture. it contains different applications for local and remote users. the applications have different user interfaces which are created using the unity game engine. the application for the local user is adapted for hmds (standalone hololens optical see-through hmd in figure 3). the application for the remote user runs on a desktop computer or laptop. thus, the remote user gets a screen-based visualization and can interact with the system by using the keyboard and a standard mouse device. 4.2. directions by the trainer aware supports the collaboration process by providing the trainer (remote user) with tools to give directions in form of spatial annotations. the annotations appear in the view of the trainee (local user). the remote user can augment the view of the local user with the following elements: • 3d-aligned objects (arrow/cube/sphere), • 2d-screen aligned content (text, photo and video), • dialog boxes for introducing text for the graphical objects and also for colours of some visual elements, • screen aligned counter and text, • screen aligned (flashing) panic button in the form of a text with the frame, • screen aligned image and colour border (to show info about a person), and 17 dragoş datcu, leon rothkrantz acta polytechnica ctu proceedings • virtual stickers (indicating scanning area at the crime scene). all annotations are encoded as distinct data messages and events that pass through shared memory system. updates are automatically sent to each software module or application (such as the software application of the local user or the software application of the remote user) by using a notification and a push system of events and data. 4.3. consistency of actions the consistency of actions is a critical aspect for establishing a virtual co-location. for that purpose, local updates are processed only when data and events are received as a feedback from the aware shared memory space module. consequently, the application for the trainer (remote user) does not execute user input updates in the graphical user interface immediately. such updates are applied only after the data and events of the user input are available in the shared memory space. the flow of data and event notifications are illustrated in the diagram in figure 7. figure 7. diagram of data and event notifications for user actions between aware modules and user applications. 4.4. data and event notifications through aware the data communication is established via the shared memory mechanism of aware. the shared memory mechanism handles parallel connections from different users located in different physical environments, and allows data sharing across different types of devices, including mobile ar hmd systems. in aware, the network communication is implemented using both tcp/ip standard for the data transfers between the server and software modules running on hardware devices linked via network cables, and udp standard for data transfers between software modules connected via wireless links. in case of the udp-based network communication, each frame from video sequence is encoded as a compressed image (using vga resolution and jpeg encoding) into a udp packet. 4.5. shared visualization virtual co-location is enabled by sharing a video channel from the hmd of the trainee (local user) with the trainer (remote user). the shared video stream, thereby, forms basis for the shared work environment. the shared memory mechanism provides functionality for synchronizing the video frames with the updates from the hmd camera tracking and with the manual annotations made by the remote user. via a graphical user interface, the remote user can modify the ar content, which is visible on the screen. the ar system has also capability to record, store and display a photo and video content. the aware framework provides functionality to store data remotely, not only locally. such data are persistent as long as the aware server is up and running. especially for videos, this mechanism ensures synchronization of the display: at a time moment, the same video frame is played for both the local and the remote user. the photos and videos are stored in separate files using standard formats, such as .png, .jpg and .avi. the transmission of video streams makes use of the motion jpeg mjpeg video compression format. each frame of the video sequence is compressed and transferred as a jpeg image. the automatic process of event and data notification takes place only for the software modules and applications that register for the specific type of data. in this way, for instance the application for the local user does not have to receive, via the network, video from its own camera (it has a direct access to this video). 4.6. communication decoupling aware achieves decoupling of communication by supporting both local user’s and remote user’s applications to access updates through a shared memory space. this functionality is tightly coupled to the virtual co-location paradigm that enables multiple users at different physical locations to work collaboratively according to their roles in a well-defined scenario. collaboration at a distance is possible as long as both users have a network connectivity to the aware server. 4.7. local user tracking in the physical environment the local user’s motion in the physical environment is automatically tracked in an augmented reality by using a slam system. a slam system (simultaneous localization and mapping) generates and updates a map of an unknown physical environment while simultaneously keeping track of a user’s location within it. 18 vol. 12/2017 affective computing and augmented reality for car driving simulators aware can run different slam systems. one of them is rdslam [34], a real-time marker-less monovision slam more suited for indoor environments developed at zhejiang university in hangzhou, china. another slam is lsd-slam [35], a real-time marker-less slam running on semi-dense depth maps. a third slam system is orb-slam2 [36], a real-time system for monocular, stereo and rgb-d cameras that computes camera trajectory and a sparse 3d reconstruction. the tracking module is integrated as a module of the aware framework and can run on computer of the trainer (local user) or on a separate hardware system. in addition to tracking the hmd position and orientation, slam performs a mapping of the physical environment (of the trainer) and generates an internal 3d representation of the physical world. the physical world is represented in terms of data structures related to key points discovered during the tracking, and to recordings of a camera position and orientation with respect to the key-points. such data are mainly used internally by the slam during the tracking process. the tracking procedure identifies a set of key points (as natural visual features) from each frame of the video sequence. estimation of the camera parameters (location and orientation) keeps track of all the key points during the time. this means newly discovered key points are stored in the system memory and already-known key-points are tracked when detected. as a part of the aware functionalities, the tracking module stores all detected key-points in the current frame of the digital video sequence, the camera location and orientation data in the shared memory space. once these data are stored on the shared memory space, all the system modules are notified on the updates so that the data can be further read, if necessary. this mechanism is illustrated in figure 7. the result of a markerless tracking provides the hmd camera location and orientation while the mapping result provides a representation of the physical world in form of a sparse cloud of 3d points. 4.8. selection and positioning of 3d virtual objects the sparse cloud of 3d points represents visual key-points, which connect the augmented world to the physical world and further act as virtual anchors supporting annotation by ar markers. the remote user can attach a virtual 3d object by using the user interface. after choosing a desired type of augmentation (by selecting a specific icon) from the bar of icons on the top-left side of the user interface, the remote user proceeds by directly mouse-clicking on the screen showing the current frame of the video sequence. the mouse click event associates the 2d coordinates of the mouse cursor on the laptop screen. in order to attach the selected 3d virtual object, the 2d mouse cursor location has to be converted to 3d coordinates, related to the reference system of the slam tracking. this conversion is done by requesting the slam module via the shared memory space implemented in aware, to map the 2d coordinate in the current video frame to the 3d coordinate. the mapping implies searching for the closest key point from the equivalent 3d location of the 2d point of the mouse click event generated through the user interface of the remote expert. once computed, the closest 3d point in the coordinate reference system of slam is sent back to the expert system application via the shared memory space. this is illustrated in the diagram in figure 8. figure 8. diagram of data and event notification for user actions within aware modules and applications. once attached to key point, a 3d-aligned virtual object is correctly rendered in the next video frames on the user interfaces for both local and remote conditions during run-time, the generation of graphical content being consistent with the hmd camera motion (figure 4, the upper part of the diagram). 5. setup 5.1. hardware the affect adaptive aware framework for training supports hardware equipment for the augmented reality and physiological sensors. such equipment includes microsoft hololens headset (figure 3), and physiological sensors such as: physiological ehealth kit (figure 9), heart rate detector cortrium (figure 10) and empatica e4 (figure 11). the e-health sensor shield v2.0 [12] (figure 9) can perform a real-time body monitoring for biometric and medical applications by using 10 different sensors including: pulse, oxygen in blood (spo2), airflow (breathing), body temperature, elec19 dragoş datcu, leon rothkrantz acta polytechnica ctu proceedings trocardiogram (ecg), glucometer, galvanic skin response (gsr sweating), blood pressure (sphygmomanometer), patient position (accelerometer) and muscle/eletromyography sensor (emg). figure 9. ehealth platform [12]. cortrium [13] (figure 10) can assess body surface temperature, activity, and respiration rate and it also contains a high-performance three-channel ecg for screening and diagnostics of cardiological diseases. figure 10. cortrium heart rate monitor [13]. empatica e4 [14] (figure 11) is a real-time wristband monitor of the physiological signals. the device incorporates a photoplethysmography sensor to measure blood volume pulse (providing estimations on the heart rate, heart rate variability and other cardiovascular features). in addition, it has a 3-axis accelerometer, and an infrared thermopile that reads peripheral skin temperature. an built-in electrodermal activity sensor measures the sympathetic nervous system arousal and derives features related to stress, engagement, and excitement. 5.2. affect recognition 5.2.1. non-contact heart rate detection non-contact analysis of physiological indicators has a major impact on several application domains making use of live monitoring of the people’s faces, in realistic scenarios involving working, playing and resting. photoplethysmography represents a noncontact, noninvasive and low-cost method that makes use of variations of transmitted or reflected light to determine figure 11. empatica e4 wristband physiological signal monitoring [14]. cardiovascular blood volume. considering normal ambient light as illumination source, allows for using video cameras and even regular webcams as heart rate detection sensors. according to the previous study [37], specific face skin areas provide enough information to estimate the heart rate, by using computer vision techniques only, including the viola&jones object detector and active appearance models. the results of such a non-contact face analysis method for the heart rate detection are depicted in figure 12. the tests have proved that the whole face area does not necessarily provide optimal region of interest for the pulse detection, the best being the cheek and forehead regions. the findings can be used to optimize the scanning of the face region which in turn leads to shorter computation times and more accurate results for the heart rate detection. in addition, lower face features can be used to sample color information for the analysis while the trainee in the car driving simulator wears an augmented reality hmd such as hololens. 5.2.2. bi-modal emotion recognition the assessment of emotional levels from speech can be naturally done by identifying patterns in the audio data and by using them in a classfication setup. the features we extract are the energy component and 12 mel-frequency cepstral coeffcients together with their delta and the acceleration terms. hmms models makes use of gaussian mixtures with different number of components. the evaluation indicates the most effcient hmm model makes use of 4 states and 40 gaussians per mixture. the accuracy of this hmmbased classifier is 55.90% [38] (table 1). making facial expression recognizers with hidden markov models and local binary pattern features (lbps) implies the identification of the optimal model parameters. finding the best number of states, the best number of gaussian mixture components and the best set of local binary patterns, is not a trivial task. we start from the results of the adaboost.m2 classifiers. for evaluation of the facial expression recognition, we have generated hmm models for each 20 vol. 12/2017 affective computing and augmented reality for car driving simulators figure 12. box plots of heart rate median errors together with the 25th and 75th percentiles, for each face region. emotion category. the best facial expression recognition model uses 268 distinct features that correspond to a selection of 45 features from each facial expression category. the accuracy of this classifier is 37.71% [38] (table 2). the recognition of emotions based on a decision level fusion implies the combination of final classification results obtained by each modality separately. for this, we take into consideration four sets of unimodal classification results namely from the speech-oriented analysis and from the separate lbp-oriented analysis which use visual features from the whole face image from specific face regions. we use these sets together with a weight function that allows for setting different importance levels for each set of unimodal results. this weight-based semantic fusion models asynchronously the emotion in visual and auditory channels. the best model obtained in this way has the accuracy of 56.27% [38]. 6. conclusions this is the first research to study a role of the affect in an augmented reality for the car driving simulation. the augmented reality technology for a remote collaboration by virtual co-location, is used to support the trainer and the trainee during the car driving training session. in order to improve learning performance during training, the affective computing technology is used to sense the trainee’s affect state and to further update semi-automatically car driving simulator parameters. the affect recognition consists of a multimodal technique that processes inputs from contactbased physiological sensors, from facial expressions readings and from the emotion in speech. the way of using the affective computing technology to further control 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[34] w. tan, h. liu, z. dong, et al. robust monocular slam in dynamic environments. in mixed and augmented reality (ismar), 2013 ieee international symposium on, pp. 209–218. 2013. doi:10.1109/ismar.2013.6671781. [35] j. engel, t. schöps, d. cremers. lsd-slam: large-scale direct monocular slam, pp. 834–849. springer international publishing, cham, 2014. doi:10.1007/978-3-319-10605-2_54. [36] r. mur-artal, j. m. m. montiel, j. d. tardós. orb-slam: a versatile and accurate monocular slam system. ieee transactions on robotics 31(5):1147–1163, 2015. doi:10.1109/tro.2015.2463671. [37] d. datcu, m. cidota, s. lukosch, l. rothkrantz. noncontact automatic heart rate analysis in visible spectrum by specific face regions. in proceedings of the 14th international conference on computer systems and technologies, compsystech ’13, pp. 120–127. acm, new york, ny, usa, 2013. doi:10.1145/2516775.2516805. [38] d. datcu. multimodal recognition of emotions. phd. thesis. delft. delft university of technology, 2009. 23 http://dx.doi.org/10.1186/s13388-015-0025-9 http://dx.doi.org/10.1007/s10606-013-9190-x http://dx.doi.org/10.1145/2702613.2732839 http://dx.doi.org/10.1109/38.963459 http://dx.doi.org/10.1162/pres.1997.6.4.355 http://dx.doi.org/10.1109/ismar.2013.6671781 http://dx.doi.org/10.1007/978-3-319-10605-2_54 http://dx.doi.org/10.1109/tro.2015.2463671 http://dx.doi.org/10.1145/2516775.2516805 acta polytechnica ctu proceedings 12:13–23, 2017 1 introduction 1.1 augmented reality 1.2 affective computing 1.3 hybrid ar-ac for car driving simulations 2 related work 3 model 3.1 closed-loop architecture 3.1.1 affect recognition 3.1.2 affect modeling 3.1.3 affect control 4 affective framework for augmented reality 4.1 local and remote user applications 4.2 directions by the trainer 4.3 consistency of actions 4.4 data and event notifications through aware 4.5 shared visualization 4.6 communication decoupling 4.7 local user tracking in the physical environment 4.8 selection and positioning of 3d virtual objects 5 setup 5.1 hardware 5.2 affect recognition 5.2.1 non-contact heart rate detection 5.2.2 bi-modal emotion recognition 6 conclusions references 261 acta polytechnica ctu proceedings 2(1): 261–263, 2015 261 doi: 10.14311/app.2015.02.0261 properties of recurrent nova t pyxidis based on 2011 outburst k. tanabe1 1faculty of bioshere-geoshere science,okayama university of science,okayama 700-0005 japan corresponding author: tanabe@big.ous.ac.jp abstract we reexamine the properties of the recurrent nova t pyxidis based on our own spectroscopic data accompanying with the photometric ones by vsolj (variable star observers league in japan) during 2011 outburst. one of the purpose of this paper is whether a missing outburst could be happen around 1988-1989. comparing the 2011 outburst data with previous ones, we may conclude that any essential difference can not be found. accordingly it is difficult to deny a small possibility of a ”missing” outburst from 1988 to 1989, taking into account the seasonal gap in its observation for northern hemisphere observers . the problem whether im normae belongs to be a member of t pyx subclass or not is to be postponed by its next outburst taking into account of t pyx’s peculiar spectral behavior. keywords: cataclysmic variables recurrnt novae t pyxidis optical spectroscopy photometry. 1 introduction recurrent novae (rne hereafter), whose definite total number is just 10 (see warner (2008) for example), are divided into three distinct subclass, namely t pyx subclass, u sco subclass and t crb subclass. among these three, t pyx subclass has only one member, t pyxdis itself and has a quite unique property of very short orbital period (1.8 h). t pyxidis is the only galactic nova belonging to the southern constellation pyxis. outburst of this object was discovered by h. leavitt in 1902 photographically. this rn has experienced 5 outbursts (1902, 1920, 1944, 1966) including 1890 detected on the harvard archival plate, before 2011 outburst. while detailed photometric observations were performed before 2011 outburst (see schaefer (2010)), spectroscopic observations performed from early time were rather fragmentary. moreover this rn accompanies nebulosity. the 2011 outburst of the rn t pyxidis was detected after 45 year of absence (twice as long as recurrence period) by linnolt on april 14.2931(ut), 2011(waagen(2011)). im mediately after discovery we started low-resolution spectroscopy and obtained detailed feature of this rn before maximum light. the obtained results is reported in the paper by imamura and tanabe (2012). on the other hand the results of the photometric observations are based on the results performed by the members of vsolj (variable star observers league in japan). in section 2, we summarize the spectroscopic observational results by imamura and tanabe (the present author), including both the basic properties of t pyx obtained before 2011 outburst and the essentials of socalled tololo classification scheme. in section 3, we try to compare the photometric observations by vsolj during 2011 outburst with the template light curve by schaefer (2010) based on its previous outbursts. then we discuss a possibility of ”missing outburst” to be expected in 1988-1989 by comparing 2011 outburst with the previous ones by using the schaefer’s template light curve (schaefer (2010)). also we mention about the problem whether im normae can be another member of t pyx subclass. at the end of this section we summarize our results. 2 summary of low-resolution optical spectroscopy 2.1 basic properties of t pyxidis based on pre-2011 outburst as it is mentioned above, t pyx is a quite unique rn for its very short orbital period (1.83 hour) compared with other rne. photometric behavior is characterized by slow rise and slower decline. its position is (α,δ)=(9h04m41.47,-32deg22.0min) and (λ,β)=(150deg,-46deg). this latter ecliptic coordinate makes its seasonal gap (almost half a year) the for northern hemisphere observers. the observed spread of magnitude is b=6.4-15.4. in addition the inclination is about 10 degree (for example, utas et al (2010)). the distance had not been known; recent value by sokoloski(2013) is 4.8±0.5kpc. 261 http://dx.doi.org/10.14311/app.2015.02.0261 k. tanabe 2.2 spectral classification of novae modern and phenomenological spectral classification of classical novae(we denote cne hereafter) is established by williams (so-called tololo classification system). according to this system, spectra of cne are divided into two classes, namely fe ii class and he/n class. the former corresponds to slow evolution novae and the latter to fast ones. as this phenomenological scheme is thought to be a reflection of the physical stage of nova ejecta, it seems to be applicable not only to cne but also to rne. 2.3 spectral evolution of t pyxidis in its early stage of 2011 outburst we started our low-resolution (r∼400) spectroscopy, using dss-7 spectrograph with st-402 ccd camera (both of them of sbig (santa barbara instrumental group)) production attached to a 28 cm schmidt cassegrain telescope (celestron production) at tanabe’s personal observatory(tpo) located in the north west edge of okayama city in japan (many photometric data obtained at tpo on dwarf novae are published by vsnet collaboration team). this site is quite suitable for astronomical observation because of its fine weather and good seeing. the okayama astrophysical observatory (oao) of national observatory in japan (naoj) is located at 40 km west from tpo. figure 1: spectral evolution of t pyxidis. upper panel denotes earlier stage,which shows he/n feature. on the contrary lower panel is later stage that shows typical feii spectral phase. the date after maximum light (minus means before maximum) are denoted on the right shoulder on each spectrum. spectral observations started at two days after discovery (april 16th and ended at 14th of may due to its position close to the sun. total observation are 13 nights, among which 9 nights are before the maximum light. details of the results are reported in imamura and tanabe (2011). here we only summarize the peculiarity about the pre-maximum behavior that the spectral evolution is not only hybrid but opposite direction from he/n phase to fe ii one. this feature is quite exotic (see figure 1). according to the obtained p cygniprofle, the expansion velocity turns from decreasing to increasing. such a transition seems to cause this extraordinary evolution from he/n to fe ii phase. the relation between this evolutional feature and the temporal change of physical state as a binary system will be discussed in a separate paper. 3 discussion 3.1 ”missing” outburst? as is shown in figure 2, the photometric behavior of t pyx during its 2011 outburst seems to be essentially the same as the template curve combined by previous outbursts (schaefer (2010)). taking into account that 45 year interval is twice as averaged interval from those 5 outburst records, we feel temptation to find out evidence of outburst around 1988-1989. in addition we can find no incompatible feature on our spectra with past fragmentary spectral data. hence it is plausible that the structure of the t pyx system does not change in binary structure after 45 years absence from outburst. therefore it is worth seeking the possibility of ”missing” outburst around 1988-1899. we tried to search the photometric data in vsolj database and found several records from the end of 1988 to 1989 with visual magnitude of 13 mag. however, unfortunately, these records were by a single observer and no distinct light variation could be seen. so this cannot be a strong evidence for missing outburst. figure 2: light curve obtained by vsolj members during 2011 outburst. smooth curve denotes a template light curve by schaefer (2010) based on previous photometric (b magnitude) data. we can see coincidence between two and conclude that no essential difference exist. 262 properties of recurrent nova t pyxidis based on 2011 outburst 3.2 is im normae a real member of t pyx subclass? recurrent nova im normae is a possible member of t pyx subclass from the point of view of light curve and its orbital period (schaefer (2010)). however taking into account of the spectroscopic properties based on 2011 outburst, spectral evolution of t pyx subclass is to posses such a property as the inverse change of normal transition from fe ii phase to he/n one. to confirm that im nor really belongs to t pyx subclass, it is necessary for us to wait the next outburst (some 80 years) for obtaining a new data on its spectral evolution. 3.3 conclusions 1) during the early stage of outburst, t pyx shows the hybrid spectral transition from he/n phase to fe ii. 2) light curve obtained by vsolj which seems to be identical to the schaefer’s template curve suggests the missing 1988-1989 outburst. but no strong evidence exists during these years. 3) without spectroscopic data, the problem whether im normae really a member of t pyx subclass is not settled. acknowledgement the author thanks vsolj members (leader seiichiro kiyota) for permitting us to make use of photometric data. minako ogi, my graduate student, helped me for her assistance of making a figure 2. the author also thanks naoko tanabe for her preparation of the instruments during our spectroscopic observations. references [1] leavitt,h.1913,harvard college obs.cir.179,1 [2] imamura,k and tanabe,k.: 2012 pasj 64,l9 [3] schaefer,b. : 2010, apjs, 187, 275 doi:10.1088/0067-0049/187/2/275 [4] utas et al. 2010,mnras, 409,237 doi:10.1111/j.1365-2966.2010.17046.x [5] sokoloski et al. 2013,apjl 770,l33 doi:10.1088/2041-8205/770/2/l33 [6] waagen,e.et al. 2011,cent.bur.electron.telegram,2700 [7] warner, b. 1995, in cataclysmic variable stars (new york: cambridge university press) doi:10.1017/cbo9780511586491 [8] warner, b. 2008, in classical novae, ed. bode, m. f. & evans, a. (new york: cambridge university press) [9] williams, r. e. 1992, aj.104, 725 [10] williams, r. e. 2012,aj 144, 98 discussion ashley pagnotta: there was no missed eruption in the year of 1980s.too many observers were working.brad schaefer has worked at all possibble archival amateuer’s data looking for trails hasn’t forward anything. kenji tanabe: i asked recently the observer t.kato for his 1988-1989 vsolj data whether the value of 13 magnitudes data indicating this rn’s high state is reliable or not.his answer was of little confidence. he said that the telescope used was 20cm and visual observation at his early day of vs observations. at first i thought this was performed using 60cm telescope of kyoto university. 263 http://dx.doi.org/10.1088/0067-0049/187/2/275 http://dx.doi.org/10.1111/j.1365-2966.2010.17046.x http://dx.doi.org/10.1088/2041-8205/770/2/l33 http://dx.doi.org/10.1017/cbo9780511586491 introduction summary of low-resolution optical spectroscopy basic properties of t pyxidis based on pre-2011 outburst spectral classification of novae spectral evolution of t pyxidis in its early stage of 2011 outburst discussion "missing" outburst? is im normae a real member of t pyx subclass? conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.11.0016 acta polytechnica ctu proceedings 11:16–21, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app railtopomodel and railml 3 in overall context adam hlubuček ctu in prague, faculty of transportation sciences, konviktská 20, prague, czech republic correspondence: hlubuada@fd.cvut.cz abstract. this paper aims to provide a brief insight into the uic railtopomodel and railml initiative. concerning the railml exchange format, mainly the current form of forthcoming third edition, involving especially the infrastructure schema, based on the railtopomodel modelling principles, is taken into account. when rewarding, the comparison between railml 3 and the previous railml 2.3 version is given. at the end, the author focuses on selected issues of possible applicability of these tools for the needs of such systems as the automatic train control, automatic train operation, prediction of train etc. if essential, some extensions of the structures are proposed. keywords: railtopomodel, railml, railway infrastructure, information systems. 1. introduction railml [1] is an open source exchange format used in the railway branch to ensure a data transfer among different software applications. the railway markup langue, based on xml, was originally designed to enable data exchange in the scope of timetabling. later on, the specifications [2] were extended to the subsystems of rolling stocks and infrastructure. in these days, also the schema of interlocking is being developed in relation to oncoming railml 3 release. another milestone, as regards the railml 3, is a significant reedition of the infrastructure concept. whereas the principles of modelling of the railway topology were rather casually defined within the previous versions, railml 3 is supposed to be strongly founded on the uic railtopomodel [3] which provides the rules how to describe the infrastructure in predefined way, nevertheless, allowing all kinds of user-specific extensions. the railtopomodel initiative was introduced in 2013 [4] in order to create a common standard in railway infrastructure modelling. the generic railway topology model aims to meet multiple needs in the field of railway data exchange, ensured by the means of the railml 3 format. in 2016, the railtopomodel was released in the form of uic international railway standard 30100 [5]. 2. the railtopomodel overview the uic railtopomodel [3] is a topological model of railway infrastructure, based on a „connexity graph“. describing a railway topology, two basic types of elements can be taken into account: the linear elements (e.g. tracks and lines) and nonlinear elements (e.g. operational points). these elements allow describing the infrastructure at different levels of detail, in order to be suitable for different specific purposes. regarding the “connexity graph”, the elements of both these categories are supposed to be modelled as the nodes, whereas the edges in the node-edge diagram represent the physical connections between these particular interconnected net elements. the linear elements shall have their orientation defined. therefore, when concerning the (again orientated) relation between two of them, it should be in both cases apparent, whether the beginning or the end of the net element is taken into account. this generic principle is illustrated in the figure 1 considering the tracks to be the nodes. in order to express the fact, whether a train is able to pass from one net element to another, additional information is necessary to be given. for this reason, the relations between net elements shall be described also by the navigability attribute, besides, concerning the direction of allowable train movement. [5] in this way, a feasible passage through a switch from one track to another can be modelled as well as the line change when passing through an operation control point. currently, the model enables to express the topology including positioning and location of net entities to be projected to the topological layer taking into account different views. there are several predefined levels of detail (macro, meso, micro) at which a railway network can be described. a user may utilize (or start with) any of them, depending to his specific use case. furthermore, he is authorised to create own levels, to be appropriate for his needs (e.g. nano or corridor level). these levels of detail should be vertically interconnectable by the means of aggregation and disaggregation principles. therefore, when passing from one level to another, sometimes an extra transition level is needed. except the different views of the topology, the particular level enables to deal with particular entities in different ways. for instance, it allows displaying a certain entity as a section at a detailed level, as a spot at a less detailed level and not to include it to the least detailed level at all. [5–7] 16 http://dx.doi.org/10.14311/app.2017.11.0016 http://ojs.cvut.cz/ojs/index.php/app vol. 11/2017 railtopomodel and railml 3 in overall context figure 1. an application of the railtopomodel principles on an example of a railway station with five simple turnouts and one single slip modelled by the means of positioned net relations. later on, the model together with railml 3 should be extended so as to enable digital continuity for infrastructure life cycle and operation supporting bim development and using railml 3 for web services as well. it should be able to provide a unique continuous network description, not only taking into account past, current and future states, but also involving the project management aspect of the lifecycle dimension. [6] concerning the objects being modelled, expressing their validities (active / non active), variants (alternative current states) and versions (states evolving over time) should be possible. [4] 3. railtopomodel packages 3.1. base currently, the railtopomodel consists of four packages. concerning the uml class diagram designed to express its structure, there is a base network domain consisting of the base object, network, level network and network resource data classes, defining the general overview of the network being modelled, including the modelling principles used. the classes of the other subsystems are mostly some kind of extensions of the network resource class, eventually of the base object class itself. the base object class specifies the fundamental attributes to be common for all the derived xml elements (in order to express its unique id, name and validity). as regards the id, especially the uuid should be used. [5, 8] 3.2. topology the topology package is especially based on the net elements and relations which are modelled by the means of node-edge diagram. the aggregation principle (of net elements) is managed within the topology domain as well. particular net elements can be grouped to larger units, creating new net elements, which are supposed to be used to express the topology at less detailed level. for instance, several tracks (linear net elements in the scope of micro-topology) can be aggregated in order to form a station area, further regarded to be an operational point (a nonlinear element in the scope of macro-topology). nevertheless, the railtopomodel defines the data classes using the most general approach (not yet specifying the particular elements of infrastructure). [5, 8] 3.3. positioning the positioning package enables to define several positioning systems (linear as well as geometric – both the geographical and these ones used to display particular entities on a monitor) as well as the corresponding coordinates. to a particular net element, several of these positioning systems can be associated, nevertheless every positioning net element involves own intrinsic positioning system, whose coordinates takes values in the range of <0;1> referring to a relative position within the element. [5, 8] in order to be able to express the intrinsic position in absolute terms, the attribute of length related to the oriented net element would have to be specified in addition. 3.4. net entities the last subsystem deals with net entities. the net entities represent these object and characteristics of the infrastructure, which can be connected to the undelaying topology layer using positioning systems. differently from the previous railml versions, enabling only to link these object to a one certain track forming its data substructure, the railtopomodel (as designed for railml 3) allows them to be handled separately without relation to the topology (for instance to describe an asset, which has not been fitted to the infrastructure yet). closer specification of these net entities is provided by the railml 3 infrastructure schema. together with the entities, their location in relation to net elements and positioning systems is managed. an entity location can be a spot location, linear location or area location, while an entity is allowed to have several locations (including both different and the same types). [5, 8] 17 adam hlubuček acta polytechnica ctu proceedings figure 2. illustration of different approaches in locating of entities in the scope of railml 2 and railml 3. 4. railml evolving over time currently, railml 3 is available for testing purposes only. in 2016, the railml 3.0.is4 alpha version was released containing xsd files (defining allowable structure of particular xml documents) especially regarding the railtopomodel schema (introduced with the railml 3 release) and the infrastructure schema. [8] the railml 3.0 releases are designed for possible railml 3 users, who are asked to compare it to their needs and to formulate a “use case” defining what kind of data they intend to exchange. these “use cases” [9] serve as the basis for further development of the railml 3 infrastructure schema. by means of that approach, the creators want to avoid accumulation of such data items which no one needs. the railml 3 infrastructure schema, as regards the 3.0.is4 release, consists of following subsections: the topology, the coordinates, the operation, the geometry, the assets and the infrastructure parameters (while the last one was removed with the 3.0.5 version). [8] 4.1. topology concerning the previous railml versions, [10] topology information is stored within the particular track elements using mutual connectors situated at the track ends and track begins or within switch points. the points defining a switch are allowed to be situated both at the track begin and at a certain distance from the track begin. such approach makes the model ambiguous, as it is not clear how to segment the tracks, not to mention confusing manner in which railml 2 describes the branching tracks of a switch. [7, 10] starting from the third version, the topology is considered separately and based on the abovementioned principles of railtopomodel. concerning the micro level, a connection between tracks is allowed to be situated at the track begin or at the track end only, which admits the values (expressed in relative units) of either 0 or 1. [8] among others, lengths of tracks are not necessary to be given in order to describe “the pure topology” properly. the same approach may be used for any other level of detail. nevertheless, there are still some questions under discussion within the railml community. railml 3 should support precious description of the track geometry. it has not been decided yet, whether the geometry will be considered separately or if it should depend on the topology. [6] 4.2. positioning systems and coordintes in railml 3, the positioning systems are managed in the scope of the coordinates subsection. previous versions are only able to express position from the beginning of a track completed with information of absolute position and geographical coordinates. these are expressed as the attributes or subelements of the elements representing the object being placed. [10] the absolute position should represent traditional mileage, which indicated values are not guaranteed to correspond to real distances. it happens for historical reasons (due to reconstructions of railway lines) and it is caused by different lengths of parallel tracks in horizontal curves and in the rail branching areas. in railml 2, there is a mileage change element enabling to express mileage jumps and overlaps being a part of the track topology assigned to a particular track. within railml 3, the issue is addressed in more complex way, following the railtopomodel principles again. a user is allowed to define different linear and geometric positioning systems using line, geometric and screen coordinates. the mileage irregularities are resolved by the means of binding different linear positioning systems. regarding the intrinsic positioning system, inseparably associated to given net element, as already mentioned, the position is measured in relative values from 0 to 1). [6, 8, 10] 18 vol. 11/2017 railtopomodel and railml 3 in overall context 4.3. net entities: operational entities, geometry entities and assets the most of particular subsections of the railml 3 infrastructure schema deal with located net entities, to be fit to the topological layer. these are the operational entities, geometry entities and assets (in railml 3.0.is4 mostly representing technical facilities of railway and with 3.0.5 version renamed to functional assets in order to be distinguished from physical assets). as regards railml 3.0.is4, there are following entities included, while users can add any others (not to be a part of the common basis) to meet their needs. [6, 8] in terms of further releases, the lists are expected to be extended, based on the “use cases”. [9] • operational entities . line . operational point . border . speed profile . speed restriction . track • geometry entities . horizontal curve . gradient curve . superelevation curve . track geometry point • assets . bridge . buffer stop . derailer . isolation rail joint . level crossing . platform . platform edge . service section . signal . stop post . switch . train detection element . train protection element . tunnel for comparison, there are two major groups of entities (the track elements group and the ocs elements group) in railml 2 creating data substructures of each track element. their location within their parent track shall be given by means of the position attribute, expressing the distance from the beginning of a track in metres. in the case of linear character of the entity being placed, railml 2 uses two different approaches how to represent it; either to determine the spots where the data change (e.g. the radius changes, speed changes. . . ), or to determine the spot location of the object itself, possibly completed with the attribute of length (e.g. the platform edges, bridges, level crossings. . . ). in some cases, it is essential to determine the considered direction. [10] the railml 2 way of description, indeed, sometimes implies data inconsistency. the data could be misunderstood. the fact that all entities are strictly allocated to one specific track may cause some difficulties concerning the infrastructure description. for instance, how to define and describe track circuits when only their borders can be marked out? structural object as bridges, tunnels and level crossings often belong to more than one track. in the scope of railml 2, every affected track needs to involve an extra instance of related data classes, although the original real world object is always the same (as seen in the figure 2). [7, 10] railml 3, building on the railtopomodel principles, offers solutions of these issues. not only that it enables spot, linear and aggregated location of net entities, but it also allows them to be multiply located (see again the figure 2). locating of all the net entities is managed in the same way, no matter what kind of entity it is. [8] every xml element representing a net entity can contain unlimited amount of spot, linear and aggregated location elements involving location spots and linear sections expressing different locations of the entity. regarding the aggregated location, it can be expressed both by spots and linear sections defining an area within the railyard. the location can be also represented by point and linear types of coordinates. their definition is taken from the gml geometry schema. it means that the net entities are already not necessarily assigned to one specific track. [7, 8] the xml elements describing the entities of the same type are included in common container elements within relevant subsection. in some cases, more complex substructure is used (especially as regards the signals, nevertheless, some of their items could be possibly managed within the interlocking schema). concerning the assets, their operating time, constriction time and blocked time is possible to be expressed, in addition. prospectively, a link of these functional assets with physical assets to be a part of inventory management is intended to be ensured. [6, 8] 4.4. infrastructure paramteres the last category, also enabling to describe characteristics of railway infrastructure, used in railml 3.0.is4 is the subsection of infrastructure parameters. the following (again extendable) list of the parameter classes is given, as regards the 3.0.is4 release. [8] • infrastructure parametres . track gauge . speed electrification . weight limit . train protection . clearance gauge . train radio . track alignment 19 adam hlubuček acta polytechnica ctu proceedings in railml 2, the most of these parameters can be expressed in two different ways: through infrastructure attribute groups (to be assigned to a certain track) or as track elements (changes within a track). [10] the railml 3.0.is4 approach is closer to the first attitude mentioned. the infrastructure parameters are managed in rather different way than the net entities. every net element (as be a part of the topologic layer) can refer to unbounded number of infrastructure parameters representing specific track conditions. besides, it means that the parameters are valid for the relevant net entity (e.g. a track or line section) as a whole. except they cannot be positioned, the related xml elements are handled in the same manner as the net entities. [8] apparently, there was an effort to remove the redundancy. unfortunately, it would mean that these global parameters cannot be changed within a particular net element. indeed, in some cases it is not essential; however, for example, as regards the electrification, it could cause serious difficulties. for that reason, based on discussions within the railml community, [11] the infrastructure parameters subsection was cancelled with railml 3.0.5 (released in march 2017) and the entities included was moved to the functional assets group (thereby becoming net entities). at the same time, the network location was introduced in order to represent the intended function of the cancelled subsection. [8] 5. selected application issues the railml 3 exchange format is supposed to find application in interconnection of such it systems as infrastructure registers, maintenance systems, evidences of assets, construction projects, visualisation of railway infrastructure (georeferenced documents, gis applications, schematic track plans, longitudinal sections), simulations of railway operation, calculations of energy consumption, capacity planning, information systems for operative control, predictions of train running, automatic routing, automatic train control, automatic train operation and many others. apparently, it is big challenge for developers to meet all the multiple needs. certainly, the alpha release does not cover all the desired aspects, as surely as it will be gradually complemented reflecting particular use cases. [9] 5.1. railml for atc? as the infrastructure description used by railml is essentially based on real track lengths, not only to use absolute mileage which can be misleading, railml seems to be very useful tool to provide data for such applications that operate with actual distance travelled by a train. among other applications, it is essential for the ertms / etcs [12] as an automatic train control system using balises to be reference points for measuring the distance travelled. the balises and balise groups are included in the railml 2 specifications, nevertheless, railml 3 have not been saturated with such entities yet. perhaps, it is caused by the unresolved issue in which way to perform referencing between the balises and balise groups elements. [8, 10] except the balise locations, other additional data are needed, including locations of important objects, speed restrictions, slopes, track conditions (change of traction systems, powerless sections, non stopping areas, sound horn commands...) road suitability parameters (loading gauge, traction system, axle load category...). many of them have already been included into the railml 3 infrastructure schema, nevertheless, some of them should be added or revised. [8, 11] 5.2. transfer times planning concerning predictions of train running (and in some cases capacity planning as well), not only the railway infrastructure itself must be taken into account, but also some related facts are important. for instance, when ensuring correspondences among trains, transfer times are often critical. among others, they depend on parameters of the paths connecting the platform edges. when there are platforms with level access, the transferring passengers are influenced by passing trains (and conversely). this fact shall be taken into account when assigning the platform edges and tracks to the trains as well (for instance, not to allow a passing train run over the foot level crossing being used by passengers). not to mention the vital importance of the foot level crossing location register for such application as the automatic train operation because of the need to ensure human safety. to cope with these cases, the model and the exchange format would need to be significantly extended. 6. proposal of a rtm based passenger movement model the abovementioned issue is more complex, as the passenger routes (connecting particular platforms together and with station building and other important locations in a station) consist of different elements (e.g. platform ramps, stairways, lifts, underpasses, overpasses, foot level crossings, footpaths). all these facilities could be expressed using railml 3 as net entities (although the railml 3 alpha release, for instance, enables to express the existence of a lift on a platform by the means of its attribute only). these platform accessories and related facilities should be interconnectable and describable by such attributes expressing their usability by persons with reduced mobility and other important parameters so as to enable searching suitable routes connecting particular “passenger access nodes” (in the sense of significant spots assigned to platforms, station building and other net entities). even such situations as a lift being out of service should be taken into account. 20 vol. 11/2017 railtopomodel and railml 3 in overall context figure 3. an author’s proposal of railtopomodel application in the scope of passenger routing issue exemplified for the case of a railway station equipped with platforms with level access. there are several possible solutions how to meet these needs. one of them is to apply railtopomodel again, this time not to connect pieces of railway infrastructure but the abovementioned “passenger access nodes”, henceforth to be considered as a new sort of the net elements (see the figure 3). this approach, in general, would also enable to model emergency access roads to railway tunnels, for instance, and to cope with other related issues. 7. conclusions railtopomodel and the corresponding data exchange format railml 3 have a great opportunity to become very useful tools in describing railway infrastructure and ensuring the rail data sharing. involving also the schemas of timetable, rolling stocks and prospectively interlocking, the railml language covers almost the whole range of the railway branch. although the railway system is based on relatively similar principles across the whole europe, there are many nationally specific details that should be addressed in a coordinated manner in order to make the constantly evolving railml system universal enough to enable different software application to consistently communicate with each other. to make the system as usable as possible, the potential users should formulate their “use cases” [9] and be in contact with the railml community creating the specifications. then they should be able to influence the final form of the railml 3 first public release in order to be suitable for their needs. nevertheless, the very special matters can be solved individually by the means of user-specific extensions. within this document, some of possible extensions were outlined as well. references [1] railml. railml [online]. https://www.railml.org/. [2] railml. the railml subschemas [online]. https://www.railml.org/en/user/subschemes.html. [3] railtopomodel. railtopomodel [online]. http://www.railtopomodel.org//. [4] uic. feasibility study uic railtopomodel and data exchange format [pdf], 2013. http://www.railtopomodel.org/files/download/ railtopomodel/270913_trafit_ finalreportfeasibilitystudyrailtopomodel.pdf. [5] uic. uic international railway standard [pdf], 2016. http://www.railtopomodel.org/files/download/ railtopomodel/270913_trafit_ finalreportfeasibilitystudyrailtopomodel.pdf. [6] railml, uic. 7th railtopomodel and 30th railml conference, paris, 2016. [7] v. p. kolmorgen, c. rahmig. railml/rtm explanation session, prague, 2017. [8] railml. railml schema version 3.0.is4 [xsd], 2016. [9] railml. use cases [online]. https://www.railml.org/en/user/use-cases.html. [10] railml. railml schema version 2.3 [online], 2016. https://www.railml.org/files/download/schemas/ 2016/railml-2.3/documentation/railml.html. [11] m. karlsson, c. rahmig. [railml3|alpha] modelling of track conditions [online], 2016. http://www.railml. org/forum/index.php?t=msg&th=474&start=0&. [12] ertms. the european traffic management system [online]. http://www.ertms.net. 21 https://www.railml.org/ https://www.railml.org/en/user/subschemes.html http://www.railtopomodel.org// http://www.railtopomodel.org/files/download/railtopomodel/270913_trafit_finalreportfeasibilitystudyrailtopomodel.pdf http://www.railtopomodel.org/files/download/railtopomodel/270913_trafit_finalreportfeasibilitystudyrailtopomodel.pdf http://www.railtopomodel.org/files/download/railtopomodel/270913_trafit_finalreportfeasibilitystudyrailtopomodel.pdf http://www.railtopomodel.org/files/download/railtopomodel/270913_trafit_finalreportfeasibilitystudyrailtopomodel.pdf http://www.railtopomodel.org/files/download/railtopomodel/270913_trafit_finalreportfeasibilitystudyrailtopomodel.pdf http://www.railtopomodel.org/files/download/railtopomodel/270913_trafit_finalreportfeasibilitystudyrailtopomodel.pdf https://www.railml.org/en/user/use-cases.html https://www.railml.org/files/download/schemas/2016/railml-2.3/documentation/railml.html https://www.railml.org/files/download/schemas/2016/railml-2.3/documentation/railml.html http://www.railml.org/forum/index.php?t=msg&th=474&start=0& http://www.railml.org/forum/index.php?t=msg&th=474&start=0& http://www.ertms.net acta polytechnica ctu proceedings 11:16–21, 2017 1 introduction 2 the railtopomodel overview 3 railtopomodel packages 3.1 base 3.2 topology 3.3 positioning 3.4 net entities 4 railml evolving over time 4.1 topology 4.2 positioning systems and coordintes 4.3 net entities: operational entities, geometry entities and assets 4.4 infrastructure paramteres 5 selected application issues 5.1 railml for atc? 5.2 transfer times planning 6 proposal of a rtm based passenger movement model 7 conclusions references 90 acta polytechnica ctu proceedings 2(1): 90–93, 2015 90 doi: 10.14311/app.2015.02.0090 simultaneous ubvri observations of the ae aquarii blobs g. latev, r. zamanov, s. boeva, k. stoyanov 1institute of astronomy and national astronomical observatory, bulgarian academy of sciences, 72 tsarighradsko shousse blvd., 1784 sofia, bulgaria corresponding author: glatev@astro.bas.bg abstract we summarize the results of our study of the cataclysmic variable ae aqr on the basis of simultaneous ubv ri observations. for the flares, we estimated the average risetime of about 300 sec, and colours (u −b)0 ∼ 1.1 and (b − v )0 ∼ 0.1. we also calculated temperatures, sizes, masses and expansion velocities of a few individual fireballs. in a single night (16.08.2012), we detected ∼ 8 min quasi-periodic modulation. keywords: stars: individual: ae aqr novae, cataclysmic variables binaries: close stars: flare. 1 introduction ae aquarii is a fascinating magnetic cataclysmic variable (cv) with orbital period of 9.88 h. like the typical cvs, it consists of a k4 iv/v star which transfers material toward a magnetic fast spinning white dwarf (wd). ae aqr has a relatively long orbital period and is one of the largest cvs having semimajor axis a = 2.33±0.02 r�, wd mass mwd = 0.63±0.05 m�, secondary mass m2 = 0.37 ± 0.04 m� (the quantities obtained with high-dispersion time-resolved absorption line spectroscopy by echevarŕıa et al. 2008). a review of ae aqr was presented by p. meintjes (this volume). ae aqr has radio and millimeter synchrotron emission (bastian, dulk & chanmugam 1988), and could be source of tev γ-rays (oruru & meintjes 2012 and references therein). however, magic does not detect γ−ray emission from ae aqr (aleksić et al. 2014). wynn, king & horne (1997) demonstrated that the wd is acting as magnetic propeller and is ejecting most of the matter transferred through the inner lagrangian point in the form of blobs (‘fireballs’). the spitzer infrared spectrum above 12.5 µm can be interpreted as synchrotron emission from electrons accelerated to a power-law distribution in expanding clouds (dubus et al. 2007). ae aqr hosts a rapidly rotating white dwarf. its spin period is p = 33.08 s and spin down rate – 5.64 × 10−14 s s−1 (patterson 1979, mauche et al. 2011), corresponding to a spin-down luminosity of 6×1033 erg s−1. a part of this spin-down power goes for ejection of the blobs. the magnetospheric propeller is effective and only a small fraction (∼3%) of the trasferred mateial eventually accretes on to wd (oruru & meintjes 2012). 2 observations our observations of ae aqr were started in 1998 with an electophotometer in v-band and are now extended to simultaneous multicolour (ubv ri) observations with the telescopes of the national astronomical observatory rozhen (2.0m rcc, 50/70 cm schmidt and 60 cm telescope) and the belogradchick astronomical observatory (60 cm telescope). the observational sessions can be summarized as follow: (i) 1998 1999: v-band electrophotometric observations. (ii) aug 2010 aug 2011: simultaneous multicolor (ubv ri) ccd observations. (iii) sep 2011 aug 2013: new simultaneous multicolor ccd observations. observational methods and data reduction are described in zamanov et al. (2012). 3 photometric behavior strong flickering and flaring activity was noted by henize (1949). on time-scales of about 10 minutes, the light curve of ae aqr displays flares with an amplitude up to ≈ 1 mag (see fig.1 and fig.2). multicolour optical photometry was performed by chincarini & walker (1981) in ubv bands. later van paradijs, van amerongen, & kraakman (1989), reported five-colour (in walraven bands) observations and showed that the flares have rise time ∼ 100 − 200 s and occur throughout the whole orbit. in fig.2 we plot the orbital light curve of ae aqr using the orbital period of 0.411655530 d and the zeroorbital phase jd0 = 2449281.4222200 (casares et al. 1996). in this figure a part of our data obtained in august 2013 are shown. the quiescent flux curve is recognizable as smooth orbital variation with two maxima and two minima per orbital cycle. 90 http://dx.doi.org/10.14311/app.2015.02.0090 simultaneous ubvri observations of the ae aquarii blobs figure 1: optical light curve of ae aqr obtained on september 27, 2011 in the bv ri bands. figure 2: the b band light curve of ae aqr (august 2013) folded with the orbital period (9.8797 h). 3.1 the flares as expanding fireballs pearson, horne & skidmore (2003, 2005) formulated analytic expressions for the spectral evolution and continuum light curves of flickering and flaring variability that occur over a wide range of astrophysical objects. they applyed these expressions to the observations of the cataclysmic variables ae aqr and ss cygni, and of the supernova sn 1987a, deriving physical parameters for the material involved. they have shown that the observed flare spectrum and evolution of ae aqr is reproducible with an isothermal fireball with population ii abundances. the interested reader is directed to their papers for a full discussion. the basic assumptions are: (i) the flares of ae aqr are due to the appearance and expansion of fireballs (blobs); (ii) the blobs are isothermal; (iii) they represent spherically symmetric expansion of a gaussian density profile with radial velocity proportional to the distance from the center of the expansion. figure 3: upper panel: dereddened fluxes of a fireball at the maximum of the flare. the solid line is a black body fit. lower panel: time evolution of the flare in the v band. the (red) solid line represents the isothermal fireball model. following pearson et al. (2005), the dimensionless time β is defined as β = 1 + h(t − tpk), where tpk is the time of the peak of the flare, h is an “expansion constant” setting the speed of the expansion. the dimensionless time β is also the expansion factor being the constant of proportionality between the current and peak scale length apk: β ≡ a/apk. the central density of the fireball is ρ = m (πa2)3/2 , (1) where m is the total mass of the material involved in the expansion (the fireball mass). the speed of expansion at a is v = ha. the optical depth parallel to the 91 g. latev et al. observer’s line of sight is τ(y) = − ∫ −∞ ∞ κ dx = τ0 e −2( y a )2 (2) where y is the impact parameter (the distance from the fireball center perpendicular to the line of sight), κ1 is the linear absorption coefficient, ε is the correction for stimulated emission, ε = 1 − e(hν/kt ). here t is the fireball temperature, a is the length scale (which we call the fireball size). the optical depth on the line of sight through the center of the fireball (y = 0) is τ0 = κ1 ε m 2 21/2 t 1/2 0 ν3 π5/2 a5 . (3) the emission of the fireball is: fν = π a2 bν(t ) 2 d2 s(τ0), (4) where s(τ0) is the ”saturation function” (see fig. 1 of pearson et al. 2005). to calculate the fireball parameters t,m, a,h, ρ and v, we performed the following: 1. we compute the peak flux of the fireball, fpk, in the five optical bands (ubv ri). an example is given in fig.3, where the calculated peak fluxes (corrected for the reddening) are plotted. 2. we derive the temperature of the fireball with a black body approximation applying iraf nfit1d routine. 3. we evaluate the size of the blob at the peak, apk, using τ0 = 6.8202 and eq.4. 4. we calculate the mass of the fireball (eq.3). the calculations are done adopting population ii abundances (κ1 = 1.27 × 1052 m−1). 5. fitting the v band light curves, we derive the expansion constant h. an example is given in fig.3 lower panel) . 6. we derive the speed of expansion and the central density. part of the calculated parameters are given in table 1. we reach lovely agreement between between the model and the light curves of the optical flares using fireballs with a temperature t ∼ 15000 k and mass m ∼ 1020 g. blobs are detected in two other close binaries containing white dwarfs (the recurrent nova rs oph and the symbiotic star ch cyg). in future it will be interting to understand is it the same mechanism (magnetic propeller), which generates the blobs. figure 4: a) light curve (in johnson b band) of ae aqr obtained on august 16, 2012. quasi-periodic oscillations are visible. b) power spectrum of the light curve. the maximum indicates a period of about 8 min. 4 unusual behaviour on august 16, 2012 usually, ae aqr has light curve as shown in fig.1. however, in our observation obtained on august 16, 2012 (see fig.4) a clear periodicity is visible. the power spectrum has a maximum corresponding to t = 7.5 ± 0.2 min. possible explanations of this unusual behavior are: (1) beat modulation between the orbital period and the wd spin period (e.g. as supposed for bg cmi, fig.7.3 of warner 1995). the equation 1/pbeat = 1/pspin − 1/porb (5) gives pbeat = 33.03 s, which is too short in comparison with the observed value. (2) blob rotating with keplerian velocity at the border of the magnetosphere: rblob = (2π)−2/3 (gmwd)1/3 t 2/3, (6) the period t = 7.5 min corresponds to keplerian rotation at distance rblob ≈ 0.11 r�. the magnetospheric radius is estimated as rm ≈ 4−8rwd ≈ 0.05−0.10 r� (zamanov et al. 2012 and references therein). in our opinion, we had the chance to observe a blob rotating at the magnetosphere boundary. 92 simultaneous ubvri observations of the ae aquarii blobs table 1: the computed parameters of the fireballs. the time is in format yyyymmdd hh:mm. in the table are given as follows: rise time in seconds, colours of the peak emission of the fireball (corrected for the interstellar reddening), temperature of the fireball, its mass and size (at the peak of the flare). quantity 20100813 23:40 20100814 19:20 20100814 19:48 20100814 20:10 20110831 21:43 rise time [sec] 260±20 230±25 290±30 440±20 260±30 (u −b)0 -1.36±0.06 -1.43±0.03 -0.93±0.04 -0.80±0.05 -1.02±0.07 (b − v )0 0.24±0.03 0.23±0.03 0.17±0.03 0.19±0.03 0.03±0.06 temperature t [k] 14 545±1000 27 292±1500 10 856±150 9 527±100 13 395±200 mass m [1019 g] 9.6±1.5 6.8±1.5 39 ±6 78±12 97±15 size apk [109 cm] 3.0±0.3 2.5±0.3 5.3±0.3 7.1±0.4 7.7±0.4 5 conclusions using 4 telescopes, we performed simultaneous observations in 5 bands (ubv ri) of the flare activity of the cataclysmic variable ae aqr. adopting the model of an isothermically expanding ball of gas, we calculated parameters (temperature, size, mass) of a few individual fireballs. in a single night, we detected ∼ 8 min quasiperiodic modulation, which might be due to a blob rotating at the magnetosphere boundary. in future we intent to measure more blobs and to search for correlations between their physical parameters. also, we will try to do a follow-up study of the qpos phenomenon. acknowledgement the authors are very grateful to the anonymous referee for useful notes and comments. this work was supported in part by the op ”hrd”, esf and the bulgarian ministry of education and science (bg051po0013.3.06-0047). references [1] aleksić, j., ansoldi, s., antonelli, l. a., et al. 2014, a&a, 568, aa109 [2] bastian, t. s., dulk, g. a., & chanmugam, g. 1988, apj, 324, 431 doi:10.1093/mnras/282.1.182 [3] casares, j., mouchet, m., martinez-pais, i. g., & harlaftis, e. t. 1996, mnras, 282, 182 [4] chincarini, g., & walker, m. f. 1981, a&a, 104, 24 doi:10.1111/j.1365-2966.2008.13248.x [5] dubus, g., taam, r. e., hull, c., watson, d. m., & mauerhan, j. c. 2007, apj, 663, 516 [6] echevarŕıa, j., smith, r. c., costero, r., zharikov, s., & michel, r. 2008, mnras, 387, 1563 doi:10.1111/j.1365-2966.2012.20410.x [7] henize, k. g. 1949, aj, 54, 89 [8] oruru, b., & meintjes, p. j. 2012, mnras, 421, 1557 doi:10.1046/j.1365-8711.2003.06079.x [9] patterson, j. 1979, apj, 234, 978 doi:10.1086/426582 [10] pearson, k. j., horne, k., & skidmore, w. 2003, mnras, 338, 1067 [11] pearson, k. j., horne, k., & skidmore, w. 2005, apj, 619, 999 [12] van paradijs, j., van amerongen, s., & kraakman, h. 1989, a&as, 79, 205 [13] warner, b. 1995, cambridge astrophysics series, 28 doi:10.1002/asna.201211718 [14] wynn, g. a., king, a. r., & horne, k. 1997, mnras, 286, 436 [15] zamanov , r. k., latev, g. y., stoyanov, k. a., et al. 2012, astronomische nachrichten, 333, 736 discussion ashley pagnotta: what is the timescale of the short unexplained flares superimposed on the orbital modulations? georgi latev: sampling every 10 seconds, average time from peak to peak is about 8 minutes simone scaringi: given the simultaneous multi-color photometry can anything be said about color evolution of ae aqr? g. latev: we will try to do this in our future work. 93 http://dx.doi.org/10.1093/mnras/282.1.182 http://dx.doi.org/10.1111/j.1365-2966.2008.13248.x http://dx.doi.org/10.1111/j.1365-2966.2012.20410.x http://dx.doi.org/10.1046/j.1365-8711.2003.06079.x http://dx.doi.org/10.1086/426582 http://dx.doi.org/10.1002/asna.201211718 introduction observations photometric behavior the flares as expanding fireballs unusual behaviour on august 16, 2012 conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.11.0006 acta polytechnica ctu proceedings 11:6–11, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app development of the municipal noise-absorbing screen and test section construction technology ondřej bret∗, petra čížková czech technical university in prague, faculty of civil engineering ∗ corresponding author: ondrej.bret@fsv.cvut.cz abstract. the article presents the development and construction technology of the municipal noise-absorbing screen (mnas) – in czech "městská protihluková clona" (mphc). the municipal noise-absorbing screen is a new acoustical element developed in cooperation of the department of railway structures, faculty of civil engineering, ctu in prague and the montstav cz s.r.o. company. it is characterised by very small dimensions – its height is only ca 0.3 metre above the top of rail. the element serves to attenuate the noise induced by rail traffic arising at the wheel-rail contact. the municipal noise-absorbing screen consists of individual, mutually interlocked units, placed one after another, made of bound recycled rubber. the article describes the major limiting conditions for the placement, shape and execution of the municipal noise-absorbing screen. it also describes the construction of the test section situated on a tram track in prague and sums up the experience obtained after the first year of operation. keywords: municipal noise-absorbing screen, noise pollution, tram traffic, tram cars, recycling, rubber granulate. 1. introduction the present-day requirements for admissible noise levels induced by both road and railway traffic in builtup residential areas have been increasingly growing. this issue is a subject of long-term discussions not only among professionals, but more and more frequently also within the public media space. the problem arising during the approval of reconstructed tram tracks in 2017 can serve as an example [1]. traffic induced noise can be limited by active or passive noise reduction measures. active noise reduction measures on the railway track in construction terms include, above all, a high-quality and well-maintained roadway, appropriate track construction design, rail fastening, application of rail absorbers and elimination of rail corrugation [2]. active noise reduction measures also include measures performed on vehicles. these are, above all, the wheel profile maintenance, bogie-mounted plates and other modifications of bogies. even the application of suitable combinations of active measures, however, comes up against the ceiling of its potential and passive measures are necessary. passive noise reduction measures include, for example, classic noise barriers, applied not only in rail transport, but also in road transport. the latest efforts are aimed at developing smaller-size elements, placed closed to the source of noise taking the form of various low noise-absorbing screens [3]. low noise-absorbing screens are elements or building units placed along tram tracks, railway tracks or other rail guided transport systems whose application results in the reduction of undesirable effects of noise arising during the passage of rail traffic [2]. low noiseabsorbing screens are placed as close as possible to the structure gauge set by a technical standard. thanks to their dimensions, they can be installed much closer to the source of noise as compared to classic noise barriers being thus able to attenuate the dominant noise arising at the wheel-rail contact (rolling noise) and the bogie noise [4, 5]. depending on the material from which they are produced, they can have absorption or reflection properties. 2. municipal noise-absorbing screen the municipal noise-absorbing screen (hereinafter also referred to as "mnas") is a noise-absorbing element developed in cooperation of the department of railway structures, faculty of civil engineering, ctu in prague and the montstav cz s.r.o. company, engaged in the recycling and production of rubber elements. the operational verification runs in cooperation with the prague public transit company (pptc). mnas serves for the attenuation of the noise induced by rail traffic, arising at the wheel-rail contact. the characteristic height of the screen is ca 30 cm above the top of rail (tr). the screen is placed in the immediate vicinity of the vehicle gauge and thus it effectively reduces the arising noise. the municipal noise-absorbing screen is characterised by the material used – a composite based on recycled rubber granulate, bound by a polyurethane binder. the rubber granulate is a secondary raw material that can be used in railway construction in different applications [6], either in a bound [7, 8] or unbound state [9]. unlike other similar elements, mnas is easily demountable, which is a great advantage in the case of e.g. a nec6 http://dx.doi.org/10.14311/app.2017.11.0006 http://ojs.cvut.cz/ojs/index.php/app vol. 11/2017 development of the municipal noise-absorbing screen essary intervention of the integrated rescue system for which concrete noise barriers create a significant obstacle to a fast and smooth intervention [10]. the first-generation mnas, which is the subject of this article, is presently being verified under operating conditions and its durability is monitored – due to favourable thermal and technical properties of the rubber granulate [9] mnas is presumed to resist winter conditions and degradation quite well [11]. it is made up of units (segments) manufactured of bound recycled rubber with dimensions of 250 x 600 x 750 mm (width x height x length), which are partially embedded below the ballast bed so that the height of the screen is ca 30 cm above the top of rail depending on the execution. 3. limiting conditions for mnas placement, shape and execution there were many limiting factors for the placement, shape and execution of the municipal noise-absorbing screen emerging already in its design phase. the major limitations are the structure gauge, or the tramway vehicle gauge respectively. the design of the mnas shape and placement was initially based on the vehicle gauge under čsn 28 0318 – "structure gauges of tramway tracks" [12]. according to this standard, the vehicle gauge width in a straight track section is 1300 mm from the rail axis. the reference vehicle considered in the above standard is a three-section tram of the kt8d5n type with a vehicle width of 2.5 m and a length of 30.3 m. in prague, this type is represented by a bi-directional tram of the kt8d5.rn2p type, which originated by the reconstruction of the kt8d5 tram [13, 14]. due to the fact that the vehicle gauge is very significantly extended in directional curves of small radii [12], the installation of mnas is feasible mainly in straight sections and curves with radii from ca 200 m. in straight sections and curves with large radii, it must be placed respecting the vehicle gauge pursuant to čsn 28 0318 [12], or other limitations specific for the respective tram operation. other parameters for the mnas placement on a test section within the prague public transit company (pptc) network included potential passage of the psp-01 bogie snow plough (figure 1). the psp01 snow plough was developed to meet the growing need for clearing snow from the rail space for the use of new low-floor vehicles. due to the low-floor part, these vehicles have a greater width in the lower parts of the body casing than older (high-floor) trams, being, in some cases,equipped with other components in the part close to the top of rail which may cause problems in contact with water (snow). to allow smooth snow removal even in directional curves, the share of the psp-01 bogie plough has a greater width than standard operated trams. its total width is 2.6 m – i.e. 1.3 metres from the rail axis. based on the need to preserve the possibility of the plough passage, this parameter must also be taken into account in figure 1. psp-01 snow plough [15]. prague and the screen must be placed with some reserve slightly further away from the rail axis than would be necessitated by the tram vehicle gauge. based on consultations with pptc representatives over designs taking into account the above limitations, a question arose concerning a potential passenger escape exit from the tram in case of emergencies (accidents, vehicle failures, etc.,...) with respect to the screen placement. while older trams and their retrofits usually have four-section folding doors (opening in the inside direction) and modern trams are, as a rule, fitted with ejecting doors (opening in the outside direction, but only to a distance of several cm from the body casing), the possibility of opening tilting doors in the t6a5 type trams appeared as potentially problematic interfering with the screen placement. as seen in figure 2, while opening the door the door leaves move along a circular trajectory getting to a distance of up to 360 mm from the body casing (1610 mm from the rail axis). therefore, when placing mnas to the right in the riding direction, the opening of the t6a5 tram door must be allowed, which can be achieved in two ways: 1) move the municipal noise-absorbing screen further way from the rail axis, to a distance exceeding 1610 mm – which is a solution totally inappropriate it terms of the acoustic effectiveness of the mnas element, or 2) select such a height of the screen above the top of rail allowing the tilting of the door – due to the height of the door at the maximum admissible wheel wear this level is at a height of 28 cm above tr – which is a solution feasible without problems. in placing the screen in the test section, this issue did not need to be solved as mnas is placed to the left of the rail axis there, i.e. on the side without a door where it does not affect a potential evacuation of the passengers. it should be added that t6a5 trams are gradually discarded from traffic operation in prague and replaced with new vehicles in which the door opening is solved by the above mentioned ejection of leaves, so that this limitation in placing mnas on the door side will no longer apply in the future. based on the above conditions and limitations, a 7 ondřej bret, petra čížková acta polytechnica ctu proceedings figure 2. t6a5 tram – cross section, including the tilting door movement – plotting in a type drawing [16]. figure 3. mounting of mnas prototypes – vandal resistance test. design of the mnas placement in characteristic sections was developed and verified by the production and mounting of three prototype segments. 3.1. verification of prototypes the trial placement of the prototypes was carried out on 23. 3. 2016 on a tram track close to the pptc central workshops, in a section between ústřední dílny dopravního podniku – na homoli stops. both the team of the department of railway structures fce ctu and the representatives of pptc, tt (tram track) administration section and dct (tram traffic route) special structures participated in the test. apart from the construction / installation test, the verification included the compatibility and interaction of individual units and their vandal-resistance was tested – resistance to the displacement of individual segments of the screen (figure 3). based on local investigation, the final design of the placement and shape was developed and the connection of mnas units was optimized. 3.2. selection of a section for trial installation the test section for the placement and verification of the acoustic properties of the municipal noiseabsorbing screen (mnas) was selected in cooperation with the prague public transit company (pptc) again. tracks with an open track structure were considered (even though mnas can also be installed in a section with vegetation cover) of which the final choice fell on a tram track in prague 4, direction sídliště modřany, the section pobřežní cesta – přístaviště in the prague district of braník. the double track tram line in the respective section is led parallel to modřanská street, on a separate body with an open ballast bed. grooved rails of the nt1 shape on tb93 concrete sleepers with w14 elastic baseplateless fastening are used there. the rail is executed as continuous welded rail. the screen was installed on the centre-bound track, to the left of the riding direction (i.e. in the inter-track space). the mnas position was selected with regard to the subsequent technical noise level measurement aimed at identifying the acoustic effectiveness of the designed noise reduction measure. the sound level meter microphone was located at a distance of 7.5 metres from the monitored track, on the side more distant from the road to eliminate the effect of passing car traffic. the characteristic section at the point of the noise-absorbing screen placement is shown in figure 4. the selected distance of the screen face from the rail axis was 1420 mm, and its height was 300 mm above the top of rail. 3.3. test section construction the test section was established on 9. 4. 2016 in coordination with a one-day tram operation lockout in the dvorce – sídliště modřany section, planned for the overhaul and maintenance of traction wires. in the morning before the lockout, accurate measurement and marking of the site for the placement and installation of the municipal noise-absorbing screen plus other preparatory works had been performed. immediately after the start of the lockout, the mhs two-way excavator made a groove in the ballast bed for the installation of mnas units (figure 5). successive work was done manually, without machinery. the site construction camp and vehicle parking were established near pobřežní cesta stop, by the exit of the link road from barrandov bridge onto modřanská street, ca 200 m from the established test section. from there, the mnas segments, tools and other material were transported by a track trolley. the width of the previously excavated groove necessary for mounting the mnas segments and the depth related to the top of rail (tr) were checked and further extended as necessary. before the installation of units, the gravel bearing surface was compacted with a manual petrol powered vibrating plate (figure 6). individual mnas units were gradually mounted onto the compacted surface, proceeding step by step from the start of the section towards přístaviště stop. the position of installed units in relation to the rail was continuously checked – their distance from the rail axis (structure gauge) and their height above tr (figure 7). mounted units were gradually backfilled 8 vol. 11/2017 development of the municipal noise-absorbing screen figure 4. characteristic section at the point of the noise-absorbing screen placement. figure 5. groove excavation for mounting mnas using the mhs two-way excavator. figure 6. compaction of groove surface prior to the screen placement. with gravel, which was compacted, both manually and using machinery. individual units were mutually interlocked by wooden laths placed on the upper side of the screen (figure 8) – this ensures the interaction of the whole screen (necessary e.g. to resist vandalism) and also secures its permanent position. figure 7. checking the screen distance and height from the rail axis and tr. an atypically chamfered unit preventing the crash of tram units into the front of the screen in case of emergency (e.g. displacement of screen units due to vandalism) was mounted onto the front of the municipal noise-absorbing screen in the riding direction (i.e. in the direction from pobřežní cesta stop) (figures 89). after the final check of the position of all units, final modifications of the ballast bed profile were made and the gravel around the installed mnas was compacted with a manual petrol powered vibrating plate. a total of 32 mnas units were installed, the test section being 24 metres in length. 3.4. screen modification following noise measurement monitoring the state after the mnas construction, the screen was modified to improve the acoustic effectiveness of the noise reduction measure used. this modification consisted in adding boards of recycled rubber, 25 mm in thickness, to the upper screen wall, which created an overlap, 9 ondřej bret, petra čížková acta polytechnica ctu proceedings figure 8. mnas seen from the start of the section – chamfered first unit is evident in the front. figure 9. detail of modified mnas execution. 70 mm in length, at the screen face to further reduce the arising noise. thanks to the board overlap, the screen face was shifted towards the track, from the original distance of 1.42 m from the rail axis to 1.35 m after the modification. the modification is evident from figure 9. the screen was modified under traffic operation on 26.4.2016. the modification was performed using boards of recycled rubber, pre-cut to the necessary dimensions. the boards were fastened to individual mnas segments with 0.5 m spacing by means of dowels into polystyrene – this solution proved to be the most convenient based on tests. after the installation of additional boards providing the overlap of the screen towards the track, the measurement of noise was carried out to verify the effectiveness of modified mnas. the solved section with completed mnas, including the modification, is presented in figure 10. 4. conclusion the designed and implemented noise reduction measure proved to be an effective alternative for the attenuation of noise induced by tram traffic. the measured data served to establish the average energy value for all measured passages of tram units. the resulting reduction due to the municipal noise-absorbing screen (mnas) application after its modification identified figure 10. municipal noise-absorbing screen after modification. was 3.9 db. some types of trams (in relation to the body casing shape at the bogie level) even reached higher noise reduction levels. more detailed information about the mnas effectiveness will be published in the professional peer-reviewed journal, akustika, in autumn 2017 (www.akustikad.com). the test section is currently subjected to continuous monitoring and different parameters are surveyed on it on a long-term basis. after the first year of operation and the first winter season, the municipal noise-absorbing screen does not show any signs of mechanical damage, degradation or other defects. in 2016, the industrial property protection agency awarded the municipal noise-absorbing screen the industrial and utility model certificate. in the following phases of research and development, further monitoring of the first-generation mnas test section, described in this article, and the construction and verification of the second-generation mnas test section or sections is presumed where structural improvements, designed on the basis of experience obtained from the construction and monitoring of the first-generation test section, will be applied. references [1] k. frouzová. praha musí řešit hlučné tramvaje na opravených tratích. hrozí omezení nebo zrušení desítky spojů / prague must solve noisy trams on repaired tracks. there is a threat of limitation or cancellation of ten lines, in: www.ihned.cz: hospodářské noviny [online]. [cit. 2017-03-10] http://domaci.ihned.cz/c1-65569370-praha-musi-resithlucne-tramvaje-na-opravenych-tratich-hrozi-omezeninebo-zruseni-desitky-spoju. [2] p. čížková. the acoustic effectiveness of low height noise barrier. in: kropp, w, ed. proceedings of the 45th international congress on noise control engineering. inter-noise 2016, hamburg, 2016-08-21/2016-08-24. berlin: german acoustical society (dega), 2016. isbn 978-3-939296-11-9. [3] j. smutný, l. pazdera, v. tomandl. assessment of the effectiveness od low noise barrier brens barrier in tetčice village. in: eisereich, j.e., ed. rychlost s tichostí. rychlost s tichostí 2015, plzeň. praha: powerprint, 2015. isbn 978-80-87994-28-3. 10 vol. 11/2017 development of the municipal noise-absorbing screen [4] p. čížková, l. lomoz. the effectiveness of a low height noise barrier. in: 14th geoconference on ecology, economics, education and legislation. 14th international multidisciplinary scientific geoconference sgem 2014, albena, 2014-06-17/2014-06-26. sofia: stef92 technology ltd., 2014. issn 1314-2704, isbn 978-619-7105-18-6, doi 10.5593/sgem2014/b52/s20.094. [5] p. čížková, l. lomoz. comparison of efficacy of low and hight acoustic screens. akustika, 2014. issn 1801-9064. [6] m. lidmila. nové perspektivy využití recyklovaných materiálů v železničním stavitelství / new perspectives of using recycled materials in railway construction, in: udržitelná výstavba. čvut v praze, 2011. isbn 978-80-01-04961-7. [7] l. horníček, h. krejčíková, m. lidmila, et al. antivibrační rohože v železničním stavitelství v čr / antivibration mats in railway construction in the czech republic. české vysoké učení technické v praze, fakulta stavební, 2011. isbn 978-80-01-04963-1. [8] j. makuch. maty wibroizolacyjne we wrocławskich torach tramvajowych. in: xiv konferencja naukowo-techniczna "drogi kolejowe 2007" [online], 2007. [cit. 2017-03-7] http://www.zits.pwr.wroc.pl/makuch/art38.pdf. [9] m. lidmila, v. lojda, o. bret. laboratory models of a railway track with the subgrade layer based on rubber granulate in: advances and trends in engineering sciences and technologies ii: proceedings of the 2nd international conference on engineering sciences and technologies, 29 june – 1 july 2016, high tatras mountains, tatranské matliare, slovak republic. boca raton: crc press, 2016. isbn 9781138032248. [10] protihlukové stěny hluku nezabrání a jsou bezpečnostní komplikací / noise-absorbing walls do not prevent noise being an obstacle to safety, želpage [online]. [cit. 2017-03-10] http://www.zelpage.cz/zpravy/8188?lang=cs. [11] o. bret. determination of rubber granulate frost protection. in: juniorstav 2017, 19. odborná konference doktorského studia. brno: vysoké učení technické v brně, fakulta stavební, 2017. isbn 978-80-214-5473-6. [12] čsn 28 0318. průjezdné průřezy tramvajových tratí a obrysy pro vozidla provozovaná na tramvajových dráhách / structure gauges and vehicle gauges for vehicles operated on tram tracks. praha: český normalizační institut, 2015. [13] katalogový list tramvajového vozu kt8d5. skd trade, a.s. / catalogue sheet of t6a5. tram car of skd trade a.s. [online]. [cit. 2017-03-18] http://www.skd.cz/tramvaje/kt8d5.htm. [14] r. mara. pražské tramvaje. praha: pavel malkus dopravní vydavatelství, 9/2012. isbn 978-80-87047-28-6. [15] archives of the prague public transit company. [16] katalogový list tramvajového vozu t6a5. skd trade a.s. / catalogue sheet of t6a5. tram car of skd trade a.s. [online]. [cit. 2017-03-18] http://www.skd.cz/tramvaje/t6a5.htm. 11 acta polytechnica ctu proceedings 11:6–11, 2017 1 introduction 2 municipal noise-absorbing screen 3 limiting conditions for mnas placement, shape and execution 3.1 verification of prototypes 3.2 selection of a section for trial installation 3.3 test section construction 3.4 screen modification 4 conclusion references acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0102 acta polytechnica ctu proceedings 4:102–106, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app activation analysis of historical samples and neutron spectrum determination at vr-1 training reactor jan šturma∗, milan štefánik department of nuclear reactors, faculty of nuclear sciences and physical engineering, czech technical university in prague, břehová 7, 115 19 praha, czech republic ∗ corresponding author: sturmja2@fjfi.cvut.cz abstract. vertical irradiation channel of the vr-1 training reactor of the department of nuclear reactors ctu was used for activation analysis of historical samples from the 14th to the 19th century. for determination of mass fractions of materials such as copper, gold and silver in irradiated samples, the relative method of activation analysis was used. further, a set of 24 activation detectors of 12 various materials served for the determination of neutron spectrum of the vr-1 reactor using analytical method; moreover the analytical solution was compared to unfolded spectrum obtained from sand-ii deconvolution program. keywords: activation analysis, reaction rate, neutron spectroscopy, historical samples, westcott formalism. 1. introduction research reactors can be used as a significant source of radiation, especially neutrons. there are several ways of neutron applications from medical purposes such as the boron capture therapy to material testing, or transmutation technologies et cetera. one possible application is also a radioanalytical method called the neutron activation analysis. this method is based on intentional production of radionuclides in studied materials through the neutron interactions; it is an exact tool that can be used to qualitatively and quantitatively determine composition of various samples. the pool-type light water training reactor vr-1 of the department of nuclear reactors ctu is frequently used for purposes of neutron activation analysis especially due to its experimental equipment such as vertical and horizontal irradiation channels. presented project aims to determine the composition of historical samples and neutron spectrum of vr-1 training reactor by using the neutron activation technique. 1.1. neutron activaton analysis measuring the characteristic radiation of the sample, usually gamma or beta particles, produced in radionuclide decays, the saturated activity of irradiated sample can be determined as asat = λtreal s(eγ) tlive εfep(eγ) iγ(eγ)( 1 − e(−λta) ) e(−λtc) ( 1 − e(−λtreal) ) ∏ i ci, (1) where λ is the decay constant of measured radionuclide, treal is the real time of the gamma spectrum measurement, tlive is the live time of the measurement, s(eγ) is number of counts in the full energy peak at energy eγ , εfep is the detector efficiency for full energy peak, iγ is the probability of gamma emission, ta is the irradiation time and tc is the cooling time. possible corrections, e.g. the correction for reactor power fluctuation, self-shielding of gamma radiation or the correction for gamma coincidences, are represented by factors ci. for determination of sample composition, the relative method of the activation analysis is standardly used. studied samples are irradiated together with the activation standards of known composition. the amount of investigated material in the sample can be determined as follows ast mst = asp msp , (2) where ast and asp are the saturated activities of produced radionuclide in standard or in sample, and mst and msp are the masses of investigated material in standard foil or in sample. other technique of neutron activation analysis is the absolute method, where the amount of material in sample is defined as msp = aspm naφσa , where m is the molar mass of examined material, na is the avogadro’s number, φ is the integral neutron flux and σa is the spectrum averaged microscopic activation cross-section. 1.2. neutron spectrum determination by activation detectors methods of neutron activation analysis can be also used for measurement of neutron flux using activation detectors of various materials. the response of the 102 http://dx.doi.org/10.14311/ap.2016.4.0102 http://ojs.cvut.cz/ojs/index.php/app vol. 4/2016 activation analysis and neutron spectrum determination at vr-1 reactor detector to the neutron field per one nuclei, called reaction rate, can be calculated as rr = asat n0 , (3) where n0 is the number of target nuclei in the activation detector. reaction rates obtained by irradiating the set of various detectors together with the cadmium cover as well as some threshold interactions make possible to reconstruct the neutron field using analytical methods. the analytical expression of neutron flux is φ(en) = φt(en) + φe(en)∆1∆2 + φf(en). (4) neutron flux in thermal energy region, φt(en), is for well moderated reactors defined according to the westcott formalism as [1] φt(en) = en (ktn)2 e− en ktn rt r g(tn)σ0 , where en is the energy of neutrons, k is the boltzmann constant, tn is the thermodynamic temperature of neutrons, rt r is the response of detector to thermal neutrons, g(tn) is the deviation of the activation cross section from the law 1/v in thermal energy region and σ0 is the activation cross-section for energy en = 0.0253 ev. the activation detector in cadmium cover is activated mostly by neutrons of energies associated with the energy of most significant resonance in crosssection, and therefore it is suitable to determine the epithermal neutron flux. discrete values of neutron flux for resonance energies eres of activation materials are defined as [2] φt(eres) = repi r k∫ e2 e1 σ(en) den , where repi r is the response of the detector in cadmium cover to the neutron field, k is the proportional representation of the most significant resonance in the cross-section in epithermal energy region, and e1 or e2 represents the lower or upper boundary of resonance. experimentally obtained discrete values of neutron flux can be fitted using the expected shape of epithermal reactor spectrum in the form of a/exn , and consequently it can be smoothly connected to the thermal and fast analytical solution of neutron spectra using the joining functions ∆1 and ∆2 defined as ∆1 = 1 1 + ( 4.95ktn en )7 , ∆2 = exp ( − en 3 · 105 ) . threshold activation detectors are serving to express the reaction rates rf r of activation detectors to the fast neutron region. in fast region, the differential neutron flux is described as φf(en) = rf r σt s(en), where σt is the spectrum averaged threshold crosssection and the s(en) is the fission neutron spectrum. 2. materials and methods 2.1. activation experiments of historical samples the vertical irradiation channel of vr-1 training reactor was used to perform the activation experiments of historical coins; the main purpose was to determine the qualitative and quantitative composition by employing the relative method of neutron activation analysis. in 2014, six historical coins were irradiated together with the reference standards of expected materials. in particular, kurush-1923, pfennig-1745, kreutzer-1843, parvus-14.century, centessimo-1852, and heller-1854 were studied, and copper, gold, silver, and nickel foils were used as activation standards in two sets. in 2015, another three coins (korona-1893, kreutzer-1861, and pfennig-1776) together with the silver and copper standards in the form of foils were irradiated. figure 1. first set of historical samples with reference materials. figure 2. third set of historical coins analyzed using activation analysis. figure 3. hpge detector in pb shielding. each set of samples was irradiated twice. the first irradiation at low reactor power was performed to disprove the presence of inappropriate isotopes, such as 59co. because after irradiation of such isotope, the long term radionuclide is produced, and it is inconvenient. gamma lines of 116min were observed in the spectrum of one sample, and due to this fact, the 103 jan šturma, milan štefánik acta polytechnica ctu proceedings indium reference activation standard was added to the set before main irradiation at the nominal power. during the second irradiation, the reactor was operated at power-level of 1 kw, and the irradiating time was set to 15–30min. after the main irradiation, the gamma-ray spectra of irradiated samples were measured by the semiconductor hpge detector. for all radionuclides observed in spectra, the saturated activity was determined by using the equation (1). 2.2. irradiationg of activaction detectors altogether 24 activation detectors made of 12 various materials (al, ag, au, cu, fe, in, lual, mn, mo, nacl, u and w) in the form of thin foils (nacl detector had a form of tablet) were irradiated in the vertical irradiation channel at mid-height of reactor core of vr-1 reactor. irradiating time was 15–45min at the reactor-power of 1 kw. activation materials were chosen with respect to the activation cross-sections in order to cover all energy regions of reactor spectrum; therefore the cadmium cover and some threshold detectors were used. after irradiation, the gamma spectra of detectors were measured. for each observed reaction, the reaction rates were determined using the expression (3). figure 4. set of activation detectors. reaction t1/2 rr [s−1] dev [s−1] 197au(n,γ)198au 2.70 days 1.77 · 10−13 4.04 · 10−15 197au(n,γ)198au cd 2.70 days 3.70 · 10−14 2.61 · 10−16 63cu(n,γ)64cu 12.70 hours 7.89 · 10−15 1.62 · 10−16 63cu(n,γ)64cu cd 12.70 hours 3.51 · 10−16 5.50 · 10−18 186w(n,γ)187w 23.72 hours 9.05 · 10−14 7.77 · 10−16 186w(n,γ)187w cd 23.72 hours 1.56 · 10−14 1.20 · 10−16 98mo(n,γ)99mo 65.94 hours 8.46 · 10−16 2.12 · 10−17 98mo(n,γ)99mo cd 65.94 hours 5.61 · 10−16 1.46 · 10−17 115in(n,γ)116min cd 54.29min 4.06 · 10−14 2.13 · 10−16 115in(n,n’)115min 4.47 hours 1.44 · 10−16 3.76 · 10−18 115in(n,γ)116min 54.29min 2.19 · 10−13 1.79 · 10−15 238u(n,γ)239u 23.45min 8.70 · 10−15 3.23 · 10−17 238u(n,γ)239u cd 23.45min 4.99 · 10−15 1.45 · 10−17 23na(n,γ)24na cd 14.96 hours 2.64 · 10−17 4.01 · 10−19 27al(n,p)27mg 9.46min 7.77 · 10−18 3.12 · 10−19 27al(n,α)24na 14.96 hours 5.29 · 10−19 4.12 · 10−20 56fe(n,p)56mn 2.58 hours 1.10 · 10−18 2.72 · 10−20 109ag(n,γ)110mag cd 249.79 days 1.79 · 10−15 7.59 · 10−18 55mn(n,γ)56mn cd 2.58 hours 9.25 · 10−16 6.14 · 10−18 55mn(n,γ)56mn 2.58 hours 2.37 · 10−14 5.28 · 10−16 176lu(n,γ)177lu cd 6.73 days 6.89 · 10−14 1.85 · 10−15 176lu(n,γ)177lu 6.73 days 5.70 · 10−12 5.05 · 10−14 23na(n,γ)24na 14.96 hours 7.65 · 10−16 7.82 · 10−18 37cl(n,γ)38cl 37.24min 7.01 · 10−16 9.07 · 10−18 table 1. reaction rates of irradiated activation detectors. 3. results 3.1. analysis of historical coins composition the relative method of neutron activation analysis was used to determine the quantitative composition of five materials in all irradiated historical coins using equation (2). measured mass and mass fractions wi are listed in table 2. sample material m [mg] wi [%] kurush au 1 052.64± 12.54 58.44± 0.70 pfennig ag 17.97± 0.16 5.62± 0.05 (1745) cu 265.72± 5.49 83.17± 1.72 kreutzer cu 3 682.40± 96.71 94.95± 2.49 (1843) parvus ag 49.11± 0.43 13.67± 0.12 cu 194.81± 4.65 54.22± 1.29 centessimo cu 1 312.61± 11.46 99.95± 0.87 in (12.34± 0.58)·10−3 (76.10± 4.42)·10−5 heller ag 2.01± 0.31 0.04± 0.01 cu 4 797.12± 77.15 93.83± 1.51 pfennig ag 37.48± 0.99 12.82± 0.34 (1776) cu 265.88± 6.71 90.96± 2.29 korona ag 2 674.09± 3.097 54.98± 0.64 cu 448.64± 11.9 9.22± 0.42 kreutzer cu 2 889.20± 71.95 92.89± 2.31 (1861) table 2. determined composition of irradiated coins [3]. parameters of radioactive decays from [4], such as the half-life period, energy and intensity of gamma radiation, were used to assign the observed gamma lines in measured spectra to specific radionuclides. then according to the neutron energies reached in thermal nuclear reactors, cross-sections, and natural isotopic composition, the observed radionuclides were assigned to considered materials. qualitative analysis of composition was carried out in this way for the coin heller. except the contribution of natural background, the gamma spectrum of heller (see fig. 5) contains the gamma lines of 64cu, 110mag marked in blue color, and then 122sb, 124sb, 76as and 24na as well. observed radionuclides referred to presence of antimony, arsenic, mercury, silver and sodium in irradiated samples. figure 5. analyzed gamma spectrum of heller. 104 vol. 4/2016 activation analysis and neutron spectrum determination at vr-1 reactor 3.2. neutron spectrum reconstruction reaction rates of interaction observed in used activation detectors through produced radionuclides covered all the energy regions of neutron spectra for typical thermal reactor. the use of cadmium cover enabled to separate the contributions of thermal and epithermal neutrons. threshold interactions served to determine the response of detector to the fast neutron. using nuclear data from endf/b-vii.1 [5], the neutron spectrum was determined according to equation (4). the irradiation position in the fuel cell dummy with the overmoderated neutron spectrum allowed to utilize the westcott formalism. separately described energy regions of neutron spectrum together with the discrete points of neutron flux, associated with the most significant resonances in activation cross-sections, and total neutron flux, determined using analytical methods, are depicted in fig. 6 and fig. 7 respecitvely. figure 6. analytic description of neutron flux regions. figure 7. total neutron flux determined by analytical methods. results obtained by analytical methods were compared to numerical solution using the unfolding procedure of sand-ii code [6]. as the input (guess) neutron spectrum requested for the deconvolution process, the analytical spectrum was used. in the 5th iteration and using nuclear data from the endf/bvii.1 data library and experimentally determined reaction rates, the neutron spectrum in 36 energy bins from 10−12 mev to 101 mev was successfully unfolded. comparison of determined numerical and analytical neutron spectrum in the mid-height of reactor core of vr-1 training reactor is in fig. 8. calculated ratios c/e, representing calculated over experimental reaction rates rations, as a parameter of spectrum unfolding, are listed in table 3. figure 8. comparison of analytical and unfolded spectrum. reaction c/e [–] reaction c/e [–] 197au(n,γ)198au 0.92 56fe(n,p)56mn 0.99 63cu(n,γ)64cu 0.87 55mn(n,γ)56mn 0.84 115in(n,γ)116min 1.18 176lu(n,γ)177lu 1.06 23na(n,γ)24na 1.03 37cl(n,γ)38cl 0.92 27al(n,α)24na 1.06 238u(n,γ)239u 1.01 table 3. c/e ratios of reactions used for the spectrum unfolding. 4. conclusions according to the experiences and results of activation experiments, the vr-1 reactor is suitable for analyzing of composition of historical samples, especially coins. table 2 clearly shows the possibilities of determination of all materials commonly used in coin production, such as gold, silver, or copper. main advantages of vr-1 training reactor is the possibility of easy way of inserting samples into irradiating position in vertical channel and relatively low reactor power, comparing to others research reactors in czech republic, so it is hard to produce emitters of very high activities. the first time used method of analytical spectrum description in full energy range showed the new possibility of neutron spectrum determination using the activation detectors at vr-1 reactor. moreover, the analytical spectrum corresponds to expectations, but compared to results of numerical solution using the sand-ii unfolding code appears slightly undervalued in the thermal energy region. this brings a new way of potential further specifying of the analytical spectrum description. results illustrated in this paper are a summary of outcome achieved within the bachelor’s thesis in 2013– 2014 and the master’s degree project in 2015–2016. references [1] c. westcott, w. walker, t. alexander. effective cross sections and cadmium ratios for the neutron spectra of thermal reactors. tech. rep., atomic energy of canada ltd., 1959. conference: 2. united nations international conference on the peaceful uses of atomic energy, geneva (switzerland), 1958. http://www.osti.gov/scitech/biblio/4279663. [2] h.-l. pai, p.-y. ma, s.-c. wang, w. s. lee. measurement of epithermal neutron spectra by 105 http://www.osti.gov/scitech/biblio/4279663 jan šturma, milan štefánik acta polytechnica ctu proceedings resonance detectors. nuclear science and engineering 9(4):519–520, 1961. [3] j. šturma. neutronová aktivační analýza historických předmětů na školním reaktoru vr-1. bachelor’s thesis, kjr fjfi, české vysoké učení technické v praze, 2014. [4] s. chu, l. ekström, r. firestone. the lund/lbnl nuclear data search, version 2.0, february 1999. http://nucleardata.nuclear.lu.se/toi/. [5] national nucelar data center. endf/b-vii.1 evaluated nucelar data library. http://www.nndc.bnl.gov/endf/b7.1/. [6] p. griffin, j. kelly, j. vandenburg. user’s manual for snl-sand-ii code. tech. rep. sand93-3957, sandia national laboratories, 1994. http://prod.sandia. gov/techlib/access-control.cgi/1993/933957.pdf. 106 http://nucleardata.nuclear.lu.se/toi/ http://www.nndc.bnl.gov/endf/b7.1/ http://prod.sandia.gov/techlib/access-control.cgi/1993/933957.pdf http://prod.sandia.gov/techlib/access-control.cgi/1993/933957.pdf acta polytechnica ctu proceedings 4:102–106, 2016 1 introduction 1.1 neutron activaton analysis 1.2 neutron spectrum determination by activation detectors 2 materials and methods 2.1 activation experiments of historical samples 2.2 irradiationg of activaction detectors 3 results 3.1 analysis of historical coins composition 3.2 neutron spectrum reconstruction 4 conclusions references acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0007 acta polytechnica ctu proceedings 7:7–11, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app comparison of virtual fields method, parallel network material model and finite element updating for material parameter determination florian dirisamer∗, umut d. çakmak, imre kállai, martín machado, zoltán major institute of polymer product engineering, johannes kepler university linz, altenbergstrasse 69, 4040 linz, austria ∗ corresponding author: florian.dirisamer@jku.at abstract. extracting material parameters from test specimens is very intensive in terms of cost and time, especially for viscoelastic material models, where the parameters are dependent of time (frequency), temperature and environmental conditions. therefore, three different methods for extracting these parameters were tested. firstly, digital image correlation combined with virtual fields method, secondly, a parallel network material model and thirdly, finite element updating. these three methods are shown and the results are compared in terms of accuracy and experimental effort. keywords: dic, finite element updating, parallel network model, vfm. 1. introduction elastomers are often used as damping elements and undergo, depending on their constraints, uniand multiaxial loadings in tension, compression and shearing [1–4]. the nonlinear inherent viscoelastic material behaviour of the epdm shore a 50 with a maximum elongation of several hundred percent makes it further complicated to extract material parameters for the whole range of time (frequency), temperature and environmental conditions relevant for the application [5, 6]. therefore a large number of tests at different temperatures and loading velocities have to be performed (75 tests [7] for the standard method (std)). to circumvent these difficulties and to extract the material parameters sufficiently, three different and well-known methods were used here for comparison purposes. the motivation is the biaxial characterization of elastomers for different applications (sealing, damping, etc.). firstly, a combined methodology based on digital image correlation (dic) [8] and virtual fields method (vfm) [9]. in this method, a heterogeneous strain field is introduced in order to acquire more than one parameter in a single test. this leads to drastically reduced time and costs. secondly, a parallel network material model (pnmm) with the procedure of bergström [10] (mcalibration and polyumod), where a test procedure including hysteretical and relaxation behaviour at certain temperatures, velocities, as well as test conditions leading to the modeling of the viscoelastic behaviour. thirdly, a finite element updating (feu) procedure using the abaqussolver [11] is utilized. measured force-displacement signals are compared to the simulated ones and the material parameters are updated until these two signals fit sufficiently within a defined tolerance. finally, these three methods are compared in terms of accuracy 36 80 120 r22 (a) . specimen 0 100 200 300 400 500 6000 5 10 15 20 25 30 35 40 45 50 55 time in s d isp la ce m en t in m m 0.1 mm s−1 1 mm s−1 10 mm s−1 hyst. & res. (b) . displacement-time diagram. figure 1. biaxial test specimen with dimensions in mm and displacement-time diagram for 0.1 mm s−1, 1 mm s−1, 10 mm s−1 and with the procedure including hystereses and relaxation for the experiments. and experimental effort and the advantages as well as disadvantages are summarized for each method. 2. description of the methods the biaxial test specimens (figure 1a) were tested with a biaxial test frame [2] at 20 °c in a temperature chamber (cts gmbh, jennersdorf, aut), loaded by an 1.5 kn actuator and measured with a 4.5 kn load cell (bose electroforce systems group, mn, usa). the optical strain measurement was performed with a dic-camera system (aramis, gom mbh, braunschweig, d) and a cold light source (dedocool, dedotec usa inc., ma, usa) and a speckle pattern was manually applied to the biaxial test specimen. the further workflow for each of the three methods, dic combined with vfm (figure 4), pnmm with the procedure of bergström (mcalibration and polyumod) (figure 7) and feu (figure 10), is explained in detail in the subsections 2.12.3. 7 http://dx.doi.org/10.14311/app.2017.7.0007 http://ojs.cvut.cz/ojs/index.php/app f. dirisamer, u.d. çakmak, i. kállai et al. acta polytechnica ctu proceedings (a) (b) (c) (d) (e) (f) εxx εyy εxy εmajor εminor εres = εminor εmajor legend εxx legend εyy legend εxy legend εmajor legend εminor legend εres -0.1 0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 -0.1 0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 -0.2500 -0.1875 -0.1250 -0.0625 0.0000 0.0625 0.1250 0.1875 0.2500 0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.000 0.025 0.050 0.075 0.100 0.125 0.150 0.5 0.6 0.7 0.8 0.9 1.0 figure 2. digital image correlation results at max strains in εxx (a), εyy (b) and εxy (c) and calculated results for εmajor (d), εminor (e) and εminor/εmajor (f). 0 10 20 30 40 500 1 2 3 strain in % st re ss in m pa 0.1 mm s−1 1 mm s−1 10 mm s−1 figure 3. stress-strain diagram for 0.1 mm s−1, 1 mm s−1 and 10 mm s−1. 2.1. digital image correlation (dic) and virtual fields method (vfm) the workflow for the vfm is shown in figure 4. displacement controlled tests at velocities of 0.1 mm s−1, 1 mm s−1 and 10 mm s−1 (figure 1b) were performed with optical strain measurement and the loaddisplacement data for each of the three velocities, as well as the optical images were recorded. these image series are evaluated via dic (ncorr, georgia institute of technology, ga, usa) to generate the strain fields εxx, εyy and the shear field εxy (figure 2a-c). afterwards εmajor (figure 2d) and εminor (figure 2e) were calculated according to equation 1. εmajor/minor = εxx + εyy 2 ± √( εxx + εyy 2 )2 − ( εxx · εyy − ε2 xy ) (1) the equibiaxial area is the region, where εmajor and εminor are “equal”, therefore, εres = εmajor/εminor (figure 2f) was calculated and the equibiaxial area was extracted in the range of εres ≥ 0.5. that area perform test capture images image series matlab (dic) strain field matlab major/minor strain matlab stress-strain data load-displacement data figure 4. workflow for the virtual fields method (vfm). was afterwards converted to an equibiaxial diameter and the biaxiality ratio φ, the biaxial stress σ was calculated by dividing the measured force with the equibiaxial diameter and the thickness and the strain ε was calculated for each image series (figure 3). 8 vol. 7/2017 comparison of vfm, pnmm and feu 0 10 20 30 40 50 600 1 2 3 strain in % st re ss in m pa 0 20 40 601. 45 1. 75 time in s s tr es s in m p a 0 20 40 601. 95 2. 3 time in s s tr es s in m p a 0 20 40 602. 2 2. 55 time in s s tr es s in m p a 0 20 40 602. 35 2. 75 time in s s tr es s in m p a figure 5. stress-strain diagram for load with hystereses and relaxation with marked relaxation areas. parameter value parameter value bulk modulus 106.59 lock stretch 4.0841 pressure dependence of flow −0.129 temp. exp. flow resistance 0 temp. factor for stiffness 0 therm. expansion coefficient 0 thermal expansion ref. temp. 293 flow resistance a 0.1743 shear modulus a 7.9898 stress exponential a 11.499 final shear modulus b 0.9803 flow resistance b 1.4018 initial shear modulus b 2.0318 norm. evolution rate of µb 10.212 stress exponential b 10.156 relative contribution of i2 c 9.3e-05 shear modulus c 1.3068 table 1. parameter table for three network material model. 2.2. parallel network material model (pnmm) the workflow for the pnmm is shown in figure 7. for the procedure of bergström (mcalibration and polyumod), tests which include hysteresis and relaxation domains (figure 1b) was performed. the hysteresis and relaxation domains are necessary to model the viscoelastic behaviour with one material test at a certain temperature and velocity. as a material model, the three parallel network model [12] was chosen. it consists of: 1st network: temperature-dependent 8-chain model [13, 14], power-law flow rate, hydrostatic pressure dependence, power-law temperature dependence strain in % 0 10 20 30 40 500.0 0.5 1.0 1.5 2.0 2.5 3.0 st re ss in m pa experimental predicted figure 6. experimental and predicted stress-strain diagram. perform test load-displacement data abaqus stress-strain data mcalibration & polyumod material model material model parameter figure 7. workflow for the parallel network material model (pnmm). 2nd network: temperature-dependent 8-chain model, shear modulus evolution with plastic strain, power-law flow rate, hydrostatic pressure dependence, power-law temperature dependence 3rd network: 8-chain model with first order i2 (second invariant of deformation tensor) dependence. with a simulation, the stress-strain data (figure 5) was calculated, which is imported and processed in mcalibration. the material parameters are calculated analytically by comparing the predicted results to the experimental ones and updating these parameters until the results fit. in that way, the material parameters are generated (table 1) and the experimental as well as predicted strain-stress curves are shown in figure 6. 9 f. dirisamer, u.d. çakmak, i. kállai et al. acta polytechnica ctu proceedings 0 10 20 30 40 500 50 100 150 200 250 displacement in mm lo ad in n 0.1 mm s−1 1 mm s−1 10 mm s−1 experimental predicted figure 8. experimental and predicted forcedisplacement diagram with the mooney-rivlin model. velocity c10 c01 d[ mm s−1] [mpa] [mpa] 0.1 0.5849 0.0856 0 1 0.5924 0.1016 0 10 0.5979 0.1506 0 table 2. parameter table of the received mooneyrivlin model-parameters. 2.3. finite element updating (feu) the workflow for the feu is shown in figure 10. tests with velocities of 0.1 mm s−1, 1 mm s−1 and 10 mm s−1 (figure 1b) were performed and the load-displacement data were recorded (figure 8, solid lines). these data were imported separately to matlab [15] and a custom-made feu-script is executed. this prepares the input file for abaqus automatically, executes the solver, performs a numerical simulation and extracts the simulated results. it compares the simulated (predicted) results to the experimental ones, updates the material parameters in the input file and repeats that procedure until the load-displacement curve fit within a defined tolerance. the gained material parameters are liste in table 2 and the compared load-displacement data are shown in figure 8. furthermore, the evolution of the parameters c10 and c01 are visualized in figure 9. 3. results and discussion in order to analyze the difference of the three terms of accuracy and experimental effort, the advantages as well as the disadvantages are summarized individually. 10−1 100 101 0.58 0.59 0.6 velocity in mm s−1 c 10 in m pa c10 0.06 0.11 0.16 c 01 in m pa c10 c01 figure 9. evolution of c10 and c01 over the velocity. perform test load-displacement data matlab abaqus material model parameter figure 10. workflow for the finite element updating (feu). • virtual fields method (vfm) the stress-strain data were calculated by vfm, in which the actual full-field strain data is considered. this full-field data includes some information about the sliding of the clamping system, elastic extension of the machine due to the force and some other small effects, which cause deviation between the measured and applied length. therefore, these effects can be taken into account and excluded. furthermore, more than one material parameter can be analyzed by generating inhomogeneous strain fields (different loading states) in one test and specimen. however, there are difficulties in finding the right equations for the virtual strain field of each loading condition and its specific (geometric) constraints to receive the right parameters and dic data is needed, which cause higher effort for acquisition and a huge amount of computational power. • parallel network material model (pnmm) the result of pnmm are the nonlinear material model parameter which include here (but is not limited to) viscoelastic, relaxation and cyclic behaviour, which gives the whole range of velocity dependence at a certain temperature and loading configuration with one test. stress-strain data must be evaluated by a simulation and the analytical calculation of the material model parameters is time consuming. furthermore, different parameter combinations of the same material model and the same test data can be received by choosing different initial parameters. therefore, the results have to be examined carefully. the selection of the material model is important for the characteristics and the accuracy. 10 vol. 7/2017 comparison of vfm, pnmm and feu std vfm pnmm feu 0 0.5 1 1.5 2 2.5 1 0.33 0.2 11 2 1.5 0.5 eff or t manual experimental computational figure 11. manual experimental and computational effort of virtual fields method (vmf), parallel network material model (pnmm) and finite element updating (feu) normalized to the standard method (std). • finite element updating (feu) the result of feu are the nonlinear material model parameters. therefore, results from specimen, as well as component tests can be taken to create a simulation. to receive the appropriate results, it is necessary to create a detailed simulation with the proper boundary conditions. furthermore, the selection of the material model is essential for the results. however, there are different parameter combinations for the same material model and simulation just by choosing different initial parameters. careful analyses of the results at various loading rates are required. the comparison of the manual and computational experimental effort of the three methods vfm, pnmm and feu, normalized to the standard method (std) (cf. section 1) is shown in figure 11. the manual experimental effort for the standard test consists of three test procedures (uniaxial, pure shear, equibiaxial), five temperatures and five test velocities, which leads to 75 tests (section 1). through the inhomogeneous strainfield of the vfm, the three test procedures can be minimized to one, which gives 25 tests, however, because of dic, the computational effort is more than doubled compared to std. for the pnmm, the whole range of velocity data for a certain temperature is included in one test, this cause 15 tests altogether, but the computational effort is by 50% greater than std. this is caused by the desired stress-strain data and the analytical calculations. the feu has no benefit on the reduction of the number of tests, nevertheless, the computational effort for small fem-simulations can be minimized, as the force-displacement data is selected directly. acknowledgements the research for this paper was performed within the framework of ffg 7th call of “produktion der zukunft” (project number: 848620). references [1] l. treloar. the elasticity and related properties of rubbers. reports on progress in physics 36(7):755, 1973. [2] u. d. çakmak, z. major. experimental thermomechanical analysis of elastomers under uniand biaxial tensile stress state. experimental mechanics 54(4):653–663, 2014. [3] u. d. çakmak, i. kallaí, z. major. temperature dependent bulge test for elastomers. mechanics research communications 60:27–32, 2014. [4] e. leiss-holzinger, u. d. çakmak, b. heise, et al. evaluation of structural change and local strain distribution in polymers comparatively imaged by ffsa and oct techniques. express polym lett 6:249–256, 2012. [5] n. w. tschoegl, w. g. knauss, i. emri. the effect of temperature and pressure on the mechanical properties of thermoand/or piezorheologically simple polymeric materials in thermodynamic equilibrium–a critical review. mechanics of time-dependent materials 6(1):53–99, 2002. [6] u. d. çakmak. experimental studies on time-temperature-dependent bulk and surface behavior of soft composite materials. ph.d. thesis, johannes kepler university, 2014. [7] a. grambow. bestimmung der materialparameter gefüllter elastomere in abhängigkeit von zeit, temperatur und beanspruchungszustand. ph.d. thesis, bibliothek der rwth aachen, 2002. [8] ncorr. ncorr. http://www.ncorr.com, 2016. [9] f. pierron, m. grédiac. the virtual fields method: extracting constitutive mechanical parameters from full-field deformation measurements. springer science & business media, 2012. [10] j. bergström. polyumod user’s manual. veryst engineering, llc, needham, ma 2009. [11] hibbett, karlsson, sorensen. abaqus/standard: user’s manual, vol. 1. hibbitt, karlsson & sorensen, 1998. [12] j. bergström, j. bischoff. an advanced thermomechanical constitutive model for uhmwpe. the international journal of structural changes in solids 2(1):31–39, 2010. [13] e. m. arruda, m. c. boyce. a three-dimensional constitutive model for the large stretch behavior of rubber elastic materials. journal of the mechanics and physics of solids 41(2):389–412, 1993. [14] j. bergström, m. boyce. large strain time-dependent behavior of filled elastomers. mechanics of materials 32(11):627–644, 2000. [15] c. moler, et al. matlab user’s guide. university of new mexico, 1982. 11 http://www.ncorr.com acta polytechnica ctu proceedings 7:7–11, 2017 1 introduction 2 description of the methods 2.1 digital image correlation (dic) and virtual fields method (vfm) 2.2 parallel network material model (pnmm) 2.3 finite element updating (feu) 3 results and discussion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2015.1.0040 acta polytechnica ctu proceedings 2:40–44, 2015 © czech technical university in prague, 2015 available online at http://ojs.cvut.cz/ojs/index.php/app planning and coordination in driving simulation martin schaefer department of computer science, fee, ctu in prague, czech republic correspondence: martin.schaefer@fel.cvut.cz abstract. we present an overview of coordination and planning tasks that we face with during the development of the agentdrive simulation platform. we particularly describe an integration of the agentdrive with a driving simulator opends. we demonstrate how the planning and coordination mechanisms can be applied in a driving simulator for automated driving applications or realistic traffic generation. we emphasize particular planning and/or coordination methods that were already developed using agentdrive platform. keywords: autonomous driving, driving simulation, automated driving, adas, automotive, multiagent systems, agent-based simulation, multi-agent coordination. 1. introduction safety and efficiency of the road traffic transport systems are common goals in the related research areas. automotive industry keeps producing safer and more efficient cars to reach these goals. there is a boom of intelligent solutions to make driving safer, efficient and comfortable. there are passive safety systems followed by active ones in modern cars. active safety systems are represented by a scale of driver assistance systems as emergency braking systems, lane-assist system, automated parking features, etc. these, so called advanced driver assistance systems (adass), are possibly just a step to a fully automated driving. the concept of the fully autonomous car, mostly advertised by google, is well known. the increasing automation in driving should bring the desired safety and efficiency of the road traffic. the road traffic efficiency from traffic perspective is often optimized by controlling traffic flows centrally in the road network. differently, the safety, apart the high-level precautions, is mostly assured individually by on-board systems of each single vehicle. the distribution of the responsibility over vehicles is natural with regards to the distributed physical manner of the domain. the road traffic is a multi-agent system. the distributed agents have usually several common desires, e.g, the safety. on the other hand, there is a competition for the limited resources, i.e., the road network capacity. the private properties of the individual cars and also their heterogeneity motivate multi-agent paradigm to be suitable. verification of such a complex and critical multiagent system is difficult. coordination mechanisms are not directly applicable in the real world traffic. the cost of the experiments with a real hardware is high. the simulation is a tool to be used to evaluate the concepts before the real world deployment. we will describe several particular coordination and planning tasks in this domain on the particular example of the integration of agentdrive and opends. figure 1. opends simulator view, highway scenario the agentdrive platform is being developed to allow to design, prototype and evaluate agent-based coordination mechanisms [1]. opends is an open sourced driving simulator (see figure 1). the agentdrive platform is introduced in [1]. the driver assistance system developed on the top of the integration of agentdrive and opends is described in [2]. in this paper, we will refer to the integration of agentdrive and opends as the simulation platform. 2. simulation platform the integration of agentdrive with a driving simulator is motivated by the need to involve the human factor into the simulation of autonomous road traffic. the driving simulation brings the capability to let a human driver to be a part of the simulation, i.e., human-in-the-loop simulation. also, the driving simulation works as a physics simulator for the agentdrive simulation. on the other hand the agentdrive brings the functionality of a traffic simulation (map data based scenarios, demand modelling, road network structures, etc.). and mainly, it allows to develop agent-based coordination mechanisms on the top of the traffic and the driving simulation. the figure 2 shows the components of the simulation platform. in the following sections, we present the main task 40 http://dx.doi.org/10.14311/app.2015.1.0040 http://ojs.cvut.cz/ojs/index.php/app vol. 2/2015 planning and coordination in driving simulation driving simulation physical sim. hmi 3d vis. human driver sumo osm scenario traffic analysis2d visualization road network multi-agent coordination coordination module srtm 3d model driving simulation figure 2. simulation platform architecture, the driving simulation module represents opends part and the module on right is the agentdrive platform. note, we use openstreetmap data for the road traffic generation. that simulation platform is ready to perform. the tasks are overlapping in several aspects. moreover, combinations of the tasks are also possible to be done. we present the categories for better organization and readability. 2.1. traffic studies the simulation is reasonable if it is able to reflect the important features of the studied real world situation. in the context of the road traffic we aim to instantiate the traffic so it corresponds to the real one. the defining aspects are: amount of vehicles on the road, distribution of the origin and the destination locations and the local behaviour of the vehicles/drivers. this can be achieved by a static routing and scheduling of the traffic. having such a traffic generated, we can study, for example, the effects of different local behaviour of the vehicles/drivers on the global traffic flow. as the local behaviour can have significant effect on the traffic, the original static routing and road utilization can become irrelevant. this usually leads to the usage of a mobility demand model instead of the static traffic instantiation. the mobility demand model describes the origin and the destination locations of trips in time. in this case, online routing and driver models are needed to perform the simulation. 2.2. human factors studies it is important to consider the human factor when a new technology is about to be deployed. nowadays, drivers are fully responsible for controlling the cars. all the technologies that are about to penetrate the road traffic need to be acceptable for the human drivers. moreover, the technologies should help drivers, not to distract them, nor to make them be less aware of the driving. the driving simulators are used to study human factors. also, in our simulation platform the opends is used to incorporate the human into the simulation 3. the opends also allows the researcher to analyse the experiment in the analyser part of the simulator. the external devices to track driver’s behaviour, e.g, stress, attention, can be used. the opends provides the researchers with a possibility to export the experiment outputs directly into the reports. our main interest is particularly in the human factors in automated driving or driving with the advanced driver assistance systems. such studies require (apart the mentioned driving simulator features) the automated driving or adas support respectively. we dedicate a separate section to both of these wide areas. 2.3. driver assistance system studies assistance systems are one of the ways to bring automation into the traffic. driver assistance systems should help drivers to observe the traffic situation by sensors and eventually warn the driver of the danger. active systems, e.g., emergency braking systems, can even intervene in case of emergency. there are several aspects of adas to research. first, it is the development or prototyping of such a system. later on, it is important to study the effects of such a system on the driver’s behaviour and in consequence on the safety. also, we can refer to the studies of the effects on traffic discussed in 2.1. there is a significant effect on the traffic flow even with only few vehicles equipped with adas (published in [3]). 41 martin schaefer acta polytechnica ctu proceedings figure 3. the basic human-in-the-loop simulation setting for human factor studies the simulation platform needs to provide a researcher with a human-in-the-loop simulation and support for adas functionality support. the humanin-the simulation features are similar to the ones described in the human factors section. on the top of it, the external dashboard availability is desired for the implementation of the adas interface. the adas functionality support means that the simulation platform has to offer a way to implement the particular functionality of the system. usually, it means to provide sensory data and an interface for the presentation of the outputs of the system to the driver. the interface can be an already mentioned output to the external dashboard or a human-machine interface (hmi) directly in the simulation visualization. in case of active adas, it is needed to provide a mechanism how the adas can intervene into the controlling of the vehicle. the logic of the assistance system is often in the scope of sensor processing, sensor fusion, reasoning and eventually the control theory. the first two phases related to sensors can be replaced by a model of a sensor in the simulated environment. if there are no real sensory data, it is possible to present a sensor model with a defined uncertainty instead of applying sensor processing on the artificial data. the mentioned reasoning stands for motion planning, trajectory prediction, pathfinding, etc.. the reasoning is then in the focus of our interest, it is where the coordination and planning is applicable. 2.4. connected car studies connected cars term stands for vehicles that are equipped with communication devices that allow them to communicate with other vehicles (v2v), infrastructure (v2i) or with manufacturer, emergency services and others (v2x). the communication device can be approached as a sensor. then, the communication sensor can be used for collective localization or world mapping. the communication sensor is providing the reasoning unit with an additional information that can be used for the reasoning. connectivity is well utilized in the cooperative setting. here, the communication channel is used as an infrastructure for cooperative protocols. more advanced cooperative techniques can be beneficial but the high demands on the connection is often a drawback of such approaches. 2.5. autonomous driving studies autonomous or driver-less vehicles is a wide research field. it offers also many cooperative and planning solutions to be applied. the agentdrive platform is primary designed to support a development of the multi-agent coordination and planning algorithms. driving simulation is not explicitly needed for autonomous driving as there is no driver any more. nevertheless, the driving simulation is useful for many purposes in the autonomous driving related studies. it is not realistic that all the vehicles become driver-less overnight. so, there will be a period of time when there are human-driven vehicles and driver-less cars on the road at the same time. also, the autonomous driving could be firstly applied to only controlled areas or situations (e.g., highways), so the driver will need to share the responsibility with the computer. completely different application of autonomous driving is in automated traffic generation for a driving simulation. mostly, if the traffic is present in the driving simulation, it is scripted to perform just a really basic model of a reactive traffic. then, the algorithms to control an autonomous vehicle can be used to generate a more realistic and autonomous traffic for a better driving simulation experience. 3. planning and coordination applications the integration of opends and agentdrive is built on the idea to perform studies described in the previous section. it shows, that the planning and coordination applications play a key role in our simulation platform. this section presents the particular already developed applications of coordination and planning. such applications form a toolbox for the previously mentioned studies. 3.1. routing and navigation routing is the shortest path planning problem on the road network graph. the problem is well known and a simple dijkstra’s or a* algorithm are applicable on the problem. the graph edges can be weighted according to the travelling speed and the occupation of the roads. this allows the vehicles to optimize the routing according the actual traffic as it is commonly done nowadays in navigation application. also, the online rerouting is applicable if it is desired. the routing algorithm from the current location is used in this case. 42 vol. 2/2015 planning and coordination in driving simulation the navigation is a routing on the finer graph. the routing is performed on the level of lanes in this case. it is used for proper lane navigation, so that the vehicle is able to get into the desired lane changing lanes. 3.2. driver assistance systems we have already developed several solutions related to the adas. the applications are all related to the highway driving. highways are the simpler domain for assistance systems like an adaptive cruise control (acc) or lane change assists (lca). we can consider only longitudinal dimension to be continuous, the lanes are considered to be discrete in the highway domain. in [2] we demonstrate how the agentdrive is suitable for adas development. the integrated cooperative adaptive cruise control and cooperative lane change assist was developed and presented in [4] and [5]. we employed a safe-distance method originally designed in [6] to provide a driver with an assistance. the driver with the assistance was advised to change speed or to change lane by the assistance system. the results show that the drivers claimed the decreased cognitive load with the activated assistance system. another interesting extension of the acc is presented in [7]. the author claims that the acc functionality for linear space (i.e., vehicles in line) could be extended for in junction coordination. it is possible if we are able to project the junction situation (i.e., vehicles approaching from different directions) into the linear space. 3.3. local coordination algorithms the purpose of such algorithms is to control vehicles so that the vehicles follow their desired paths while avoiding collisions with each other. the algorithms can be applied to the fully controlled vehicles, i.e., autonomous driving, or to feed the advanced driver assistance systems. there are several approaches to the road traffic coordination. the basic approach is a reactive mechanism, where an agent representing a vehicle observes the neighbourhood and reacts to it. the safe-distance method presented in [6] is an example of a such approach. the main idea of the method is in the maintaining a safe distance between the vehicles. an action that an agent performs must result into a safe state. a vehicle is in a safe state when the vehicle can perform a sequence of actions that leads the vehicle to stop without any collision. the method is described in detail in [6] or its generalization is in [8]. the generalization allows to use the method on the general road network with junctions, not only on the highway without crossings as it was constrained in the original work. the inspiration for the generalization is in the lane merging when the vehicles must merge into a single lane. the vehicles must create a gap for a vehicle in the next lane. the similar concept can be applied in the junctions, we can imagine a junction as the single lane we need to figure 4. visualization of junction passing using the orca algorithm merge into. the gaps are virtually created when approaching the junction and the junction is then passed smoothly. the same core algorithm is also mentioned in section 3.2 in the context of the generalized acc. another reactive coordination method is based on the optimized reciprocal collision avoidance (orca) [9]. we applied the state-of-the art algorithm for the multi-robot collision avoidance in the road traffic domain (see 4. in contrast to the previous safe-distance method, the orca is a free ride algorithm based on the velocity obstacles. the advantage of that is that it is independent of the lanes on the road, but at the same time it can be its disadvantage. the application into the driving simulation shows that the orca could perform better in utilization of the road capacity. on the other hand it is not compatible with the current traffic as it does not respect the lanes and behaves unpredictably for the human drivers. junctions and coordination on the junction is often a separate problem in the road traffic coordination. the setting with the traffic lights is simple, the vehicles must follow the instructions of the central authority through the traffic lights. the optimization of the timing and similar studies are in scope of pure traffic simulations. the junctions without the centralized coordination are in practice controlled by the rules defining who gives a way to who. we already presented the generalized safe-distance method that can serve as a coordination method in junctions in our simulations. there is no give a way sign or concept of main street, the priority comes from the position to the junction. also, the multi-agent planning is able to maintain collision free junction passing. the asynchronous decentralized prioritized planning (adpp) method for road vehicles coordination was proposed and applied 43 martin schaefer acta polytechnica ctu proceedings in [10] and in detail in [11]. the prioritized planning is a good approach to reduce computation complexity of the multi-agent planning, however, the priority assignment is an open problem. the static priority assignment is a simple but not convenient and compatible solution with the current traffic rules, the dynamic priority assignment is a challenge for the future research. the cited work on adpp for the road traffic already presented several adjustments of the algorithm so that it is applicable in the highly dynamic traffic domain. as an example, we can mention dynamic constraints introduced to model dynamism of the road vehicles. another cooperative technique based on the peer-topeer algorithm was researched in [12]. the approached suffered from the excessive peer-to-peer communication in case of a conflict in plans. the cooperation in sense of plan sharing was adopted also in works related to the platooning. the platooning is a concept of vehicle trains. the advantages of the platoons are fuel reduction, road utilization efficiency and reduction of driver load. platooning is mostly spelled in context of the commercial truck transportation. the control theory aspects with the presence of the communication was studied in [13]. the focus on formations of the vehicles and the effects of the platoons on the traffic flow was described in [14]. the coordination algorithms form the core of the simulation platform. the simulation platform is designed to allow a wide range of in terms of computation resources usage, empirical solution quality or subjective user experience. 4. conclusions we presented the integration of agentdrive and opends. we presented the main areas that the simulation platform can be used in. we emphasize the requirements of each of the areas. we identify that the integrated simulation platform contains several planning and coordination applications. the applications were listed, categorized and presented to show the work done using the simulation platform. also, we mention open issues in the related research fields. the content gives a view on the application possibilities of the simulation platform. acknowledgements this work was supported by the grant agency of the czech technical university in prague, grant no. sgs15/209/ohk3/3t/13. references [1] m. schaefer, j. vokrinek. agentdrive: towards an agent-based coordination of intelligent cars. in advances in practical applications of agents, multi-agent systems, and sustainability: the paams collection, pp. 211–224. springer international publishing, 2015. doi:10.1007/978-3-319-18944-4_18. [2] m. schaefer, j. vokrinek. developing agent-based driver assistance systems using agentdrive. in advances in practical applications of agents, multi-agent systems, and sustainability: the paams collection, pp. 312–315. springer, 2015. doi:10.1007/978-3-319-18944-4_35. [3] a. kesting, m. treiber, m. schönhof, et al. jam-avoiding adaptive cruise control (acc) and its impact on traffic dynamics. in traffic and granular flow 05, pp. 633–643. springer, 2007. doi:10.1007/978-3-540-47641-2_62. [4] j. vokrinek, m. schaefer, d. pinotti. multi-agent traffic simulation for human-in-the-loop cooperative drive systems testing. in proceedings of the 2014 international conference on autonomous agents and multi-agent systems, pp. 1691–1692. international foundation for autonomous agents and multiagent systems, 2014. [5] m. schaefer, j. vokrinek, d. pinotti, f. tango. multiagent traffic simulation for development and validation of autonomic car-to-car systems. in autonomic road transport support systems. birkhauser basel, in print. [6] m. schaefer. noncooperative collision avoidance of road vehicles, 2011. [7] d. kubeša. autonomous cruise control for general collision avoidance of road vehicles. in proceedings of the 19th international scientific student conferenece poster 2015. czech technical university in prague, 2015. [8] d. kubeša. collision avoidance on general road network, 2015. bachelor’s thesis. [9] m. schaefer. collision avoidance of highway traffic. master’s thesis, czech technical university in prague, 2014. [10] m. vavřinec, m. schaefer. prioritized planning for road vehicles coordination. in proceedings of the 19th international scientific student conferenece poster 2015. czech technical university in prague, 2015. [11] m. vavřinec. asynchronous decentralized prioritized planning for cooperative vehicles, 2015. bachelor’s thesis. [12] p. janovský. cooperative collision avoidance of road vehicles, 2011. [13] m. švandrlík. convoy platooning using vehicle to vehicle communication. master’s thesis, české vysoké učení technické v praze. vypočetní a informační centrum., 2015. [14] o. borovec. cooperative formations on highway, 2015. bachelor’s thesis. 44 http://dx.doi.org/10.1007/978-3-319-18944-4_18 http://dx.doi.org/10.1007/978-3-319-18944-4_35 http://dx.doi.org/10.1007/978-3-540-47641-2_62 acta polytechnica ctu proceedings 2:40–44, 2015 1 introduction 2 simulation platform 2.1 traffic studies 2.2 human factors studies 2.3 driver assistance system studies 2.4 connected car studies 2.5 autonomous driving studies 3 planning and coordination applications 3.1 routing and navigation 3.2 driver assistance systems 3.3 local coordination algorithms 4 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.11.0001 acta polytechnica ctu proceedings 11:1–5, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app comparison of language subset and language extension by safe related information approach to safe system development tomáš brandejský∗, vít fábera department of applied informatics in transportation, faculty of transportation sciences, ctu in prague ∗ corresponding author: brandejsky@fd.cvut.cz abstract. presented contribution is dedicated to discussion of two different approaches into increase of programming language safety. they are language subset and extension of original safety mechanisms. as examples we used misra c/c++ subset and spark language builded on the base of ada language. in the last chapters we discuss novel approaches based on application of programmable hardware which is described in vhdl language, which is also modification of ada language. especially spark and vhdl languages represents novel approaches to safe system development which are now discussed in relation to new railway sw projects. keywords: misra, ada, spark, vhdl, programmable hardware, software safety. 1. introduction nowadays we can observe two opposite approaches to modification of programming languages to be more suitable to safe system development. the first is the reduction of chosen programming language expressions to safe subset, like misra c/c++ [1, 2] and this approach is also supported by today standards of safe software development like iso61508 [3] or en50128 [4]. in the last few years, novel and partially opposite development is expanded. it is based on extension of original language by additional explanations containing description of such aspects of software, that are not described enough by original language. typical example is spark [5] language precisiating original ada one [6] even though it was originally designed as language specialized to safe control system development. 2. misra c/c++ misra c (motor industry software reliability association) c language subset was developed in 1998, latter it was updated and also there was developed analogical support for c++ (misra c++). misra c/c++ defines itself as guidelines. it defines language subset in the form of rules partially suggesting good practice solutions, frequently warning programmers away of wrong application of the language. especially valuable of misra guideline are parts explaining why was each rule formed, explaining what is the subject of possible future problem. applying of this rules allows to write robust code with decreased probability of malfunction. now it is possible to apply compilers and source code checkers implementing misra guidelines to allow automatic static analysis of code. even, there exists free software tool clang-misracpp2008 [7] but the development of this tool probably stopped before two years. from the practical viewpoint, misra guidelines checker implemented in compiler is also very interesting. it is even better than standalone checker because checking in compiler runs in each code making and does not require additional checking operation step. many companies producing compilers for development of embedded systems based especially on single chip micro-controllers, for example keil software company which is widely used by railway control system developers community in our country. there exists effort to implement misra rules into gnu c/c++ compilers because these compilers are free, proven in use and supports many processors and micro-controllers. one of the first works in this areas was [8], where authors describe its checker for gnu c which is written in ciao prolog language into which misra rules they were transformed. ciao prolog is similar to gnu prolog and is also free and compatible with gnu one but it seems to be more advanced than gnu prolog in its design. this project probably is not active now. there was also european project within the frame of itea3 call for development of gcc fork called ggcc [9] with aim to implement misra rule checking into gcc compiler. this project probably newer started or produced no reasonable result. thus it is possible to conclude that now there is no applicable support of misra for gnu c compilers and that gnu compilers development effort now focuses rather to support of parallel (super-)computers, like implementation of acc extension of standard c/c++ languages. misra c specification is not public domain and this fact might also cause small interest of gnu community to implement this subset. there exist also similar subset called high integrity c++ [10] by programming research, but also this specification is not public domain as well as checking tools. 1 http://dx.doi.org/10.14311/app.2017.11.0001 http://ojs.cvut.cz/ojs/index.php/app tomáš brandejský, vít fábera acta polytechnica ctu proceedings 3. ada language origin of ada language falls into falls into 80’s of previous century. this language was developed for us army applications as safe, strong typing programming language supporting parallelism, inter-process safe communication and defensive programming style preventing programmers errors and decreasing the need of testing. this pascal (or algol) like language was adopted in avionics and nuclear industry and it is referred by safe software system development standards [3, 4]. because the language was designed with respect to extremely large scale control system design operated by us ministry of defence, it was designed to eliminate maximum of programmers errors, ability to detect large percentage of them during compilation of code and with ability to operate in distributed environment with respect to possible communication errors and system component faults. the language was equipped by specific typing mechanism supporting defensive programming to support ability of error detection by compiler. defensive programming is related to strong typing, which means, that magnitudes between variables of different types cannot be shared without explicit conversion. because mainstream programming languages like c offer limited list of types (integer, real, character), the use of type control is able to discover only limited number of programmer errors when such languages are used. on the opposite side, ada language offers ways how to define new data types e.g. by constraining of definition domain of sample type (e.g. type secondfloornumbers is range 200..253; defines data type which magnitudes are constrained to really existing scale of numbers and allows to compiler to identify each impossible magnitude caused by programmer or communication error, e.g. 0). because strong typing might be exhausting, when it is required in situations when it brings to benefit, in ada it is possible to define subtypes, which magnitudes are transformed automatically without explicit type conversions between original type and all its subtypes. all data structures use closing clause unambiguously defining its end to prevent mistakes caused by wrong understanding of nested structures in the time of development, testing and maintenance. on the end of function and procedure definition it is supported its name stating. for many years, in mainstream programming languages the support of concurrent programming was extraordinary. ada language contains it from its origin in 70’s. ada allows not only define processes, but it contains strong support of safe inter-process communication and process synchronization called rendezvous. each process has defined so called entries to accept messages sent by other processes and is able to send messages to entries of other ones. but not only. it is possible to choose, which messages will be accepted in given state of process and it is possible to define reactions to unexpected situations, especially to fact, that given message was not received for given time. each process might define its local variables and separate itself from others. due to its real time orientation, ada language supports exception handling to solve unexpected situation without program fail. there is present concept of modular programming which applied templates (modules without precisely defined types, operators, procedures and functions which might be precisiated later in the time of final program linking. it allows e.g. to write sorting algorithm library without knowledge of sorted data type. such library si then applicable to any data type implementing assignment and comparison operators. latter ada adopted object oriented programming concept but it is not widely used as e.g. c/c++, java and some other languages, especially due to high price of commercial compilers and need of specific education of programmers. similarly like for c/c++, also for ada language there was effort to develop safe subset to increase its (high) safety. also standards [3, 4] refers this subset but in reality nothing such exists. the improving of ada language was moving different way and tends to spark language, especially due to impossibility do make such simple programmers errors as they are solved by misra for c/c++. significant part of such errors can not occur in standard ada and thus its improvement is much difficult, because even original (full scale) ada operates on different (much higher) level of safety than e.g. c. there exist support of ada language based on gnu compiler collection, but it means that there are supported especially versatile operating systems like linux and common purpose processors. there is also interesting, that compiler is not named ada compiler, but by acronym gnat. it is caused by licensing, when ada compiler term can be used only for compiler satisfying large (and thus expensive) verification, which is out of scope of gnu community. spark language is not pure subset. it also extends ada code by additional information to eliminate potential ambiguities and insecurities hidden in ada source codes. the main changes to standard ada language are the following: • the use of access types and allocators is not permitted (term access in ada denotes pointer – more frequent term known from the other programming languages, its misuse might cause significant errors hard to discover by testing). • all expressions (including function calls) are free of side-effects. this improvement was reached by incorporating of additional description of use of variables and symbols visible from neighborhood to prevent e.g. mistaking of global and local variable of the same name. • aliasing of names is not permitted in general but the renaming of entities is permitted as there is a static 2 vol. 11/2017 comparison of language subset and language extension relationship between the two names. in analysis all names introduced by a renaming declaration are replaced by the name of the renamed entity. this replacement is applied recursively when there are multiple renames of an entity. • the goto statement is not permitted. • the use of controlled types is not currently permitted. • tasks and protected objects are permitted only if the ravenscar profile (or the extended ravenscar profile) is specified. ravenscar profile denotes set of pragmas influencing compiler work to prevent some possibly unsafe construction in ada code. ravenscar profile is available in standard ada too, in spark is is not option but he standard. • raising and handling of exceptions is not currently permitted (exceptions can be included in a program but proof must be used to show that they cannot be raised). misra c/c++ especially eliminates confusing structures which might be understand differently by compiler, programmer and structures which are differently understand by different compilers, especially due to vague language definition (it is especially problem of c language, c++ in its last version was significantly improved, precisiated). for example if there is used condition ((x==a)&&(y==b)), there is not defined in language specification if the sub-expression (x==a) is evaluated as the first or the second. it is no problem until we do modification of this condition to form ((x()==a)&&(y()==b)). in this new condition x and y are not static objects (variables), but they are function calls and functions might contain so-called side effects, in this case they might operate the same global variable and thus the results of calls of functions x() and y() might be influenced by call order. this subset has also many rules eliminating confusing structures causing misunderstandings by programmers and testers. misra subsets contain tens such confusing structures. e.g. it is possible to mention constants starting with zero (they are understood by compilers as octal numbers by definition), problem of nested structures if-else which might not contain else branch and no terminal symbol stopping this structure is defined in the language and so on. 4. spark spark language introduces explicit description of use of global objects (and commonly objects defined on higher level of visibility) called dependencies. the use of these additional descriptions is known from design by contract methodology, which was on the origin of such languages as eiffel [11]. this methodology prescribes that software designers should define formal, precise and verifiable interface specifications for software components, which extend the ordinary definition of abstract data types with preconditions, postconditions and invariants. preconditions are conditions which must be satisfied to enter the following section. opposite postcondition must be satisfied on the end of the block and the invariant must be valid inside the block. 5. vhdl vhdl (vhsic hardware description language) [12] is now frequently used in programming of field-programmable gate arrays. it describes structure and/or behaviour of digital hardware. vhdl is similar to ada language both in concept and syntax (parallel processes, subtypes, ...). it was primarily proposed for simulation, now the vhdl description is an input for synthesis tool instead of schematic diagram to produce final design. the interesting question is, if the similarity of vhdl and ada languages cannot be used to description of both sw a fpga implementation of systems with high requirements to reliability, applicability, maintenance and safety. simulation of system described by vhdl language is not straightforward due to need to respect signal and not process oriented nature of fpga. this nature caused presence of sensitivity list in vhdl code. in vhdl, the proces statement has an part called sensitivity list. the syntax is as follows: [process_label:]process[(sensitivity_list)] declarative_part begin statement_part end process[process_label]; example: andgate1: process (a,b) begin y <= a and b after 5 ns; end process; the sensitivity list consists of input signal identifiers separated by commas. sensitivity list is important at the moment of the simulation. during the initialization phase of simulation, the process runs and it assigned initial values of signals and variables (signal y in our case). then the process is suspended. if the any signal listed in the sensitivity list is changed, the process is resumed and executed. the sensivity list after the process keyword is syntactically optional, but we can really say that is mandatory. the sensitivity list placed after the process keyword can moved at the end ot the process section and written like the wait on statement: andgate1: process begin y <= a and b after 5 ns; wait on a, b; end process; 3 tomáš brandejský, vít fábera acta polytechnica ctu proceedings figure 1. corresponding schematic diagrams to vhdl code related to simulation. the process having sensitivity list after process keyword must contain no wait on statement. if some signal is missing in the list, it affects naturaly the simulation. for example, signal b is missing: andgate1: process (a) begin y <= a and b after 5 ns; end process; let consider the set of simulus: both signals are set to 0 at time 0ns, a signal is changed to 1 at 10ns, b signal is changed to 1 at 20 ns. the result of simulation in isim (a part of xilinx ise design pack) is constant zero signal y, because the process in not activated at the time 20 ns due to missing signal b in the sensitivity list. while process andgate1 really describes combinational and, andgate2 process has sequential behavior. we show one more example of code and corresponding schematic diagrams to simulation (fig. 1). multiplexor1: process (s, i0, i1) begin if s = ’0’ then y <= i0; else y <= i1; end if; end process; multiplexor2: process (s) begin if s = ’0’ then y <= i0; else y <= i1; end if; end process; in simulation, the output y of multiplexor2 process changes only if event on s occurs. it means that output y follows the value of i0 at the moment of falling edge on s and value of i1 at the moment of rising edge on s. 6. synthesis processes andgate2 and multiplexor2 have sequential behaviour during the simulation with isim. how process these codes synthesis tools xilinx ise 12.4? if a signal is missing in the sensitivity list, tools writes a warning like "i0 should be on the sensitivity list of the process". if signal y is listed in the sensivity and it y an output of the entity, the vhdl compiler writes an error "y with mode ’out’ cannot be read". if y is an internal signal, it can state in the sensitivity list without warning or error. but all variants of code lead to the same rtl (register transfer level) – combinational logic – and gate and multiplexor. syntesis tool decides if it uses combinational logic or flip-flop according to typical vhdl code structures (if clk’event and clk = ’1’ then for flip-flops). so, if we forget to put a signal in the sensitivity list and if we ignore warnings, the simulation of the code and the behavioral of the target design can be different. the reason is: to put all input signal in the sensitivity list and or use a variant of the sensitivity list with keyword all, which was added into new specification of the language. the gcc compiler has -wall switch, that cause to stop compiling also if a warning occurs. switch -wall is recomended in c language if we create a safety software. synthesis tools (xilinx ise) have usually no switch like -wall, vivaldo design suite from xilinx makes possible to change severity from warning to errors. as seen, vhdl, although declared as language with safety properties, has also some weak points. a question is: wouldn’t it be suitable to extend vdhl compilers in the sense of -wall switch and to add a variable list like in sparc, espetially, if vhdl is speculated as a language for railway systems? by the way, rules for safety design using vhdl was presented in [13]. 7. discussion vhdl language uses control structures and programming methodology analogical to original ada language. it is the subject of future research, if it is possible to modify it in the way analogical to spark to increase its safety and analysis if such extension could bring significant increase to safety due to influence of hardware (gate array) to it. 8. conclusion the presented paper brings analysis of impact of two basic methods to increase language safety to cover safety requirements of systems working on high safety integrity levels, e.g. on railways. it is not only focused to comparison of ada and spark languages but it is illustrated on problems bring by implementation of vhdl simulator designed with respect to describe safe system by single language without need to distinguish if this system will be implement by hw or sw. references [1] guidelines for the use of the c language in critical systems, march 2013. isbn 978-1-906400-10-1 (paperback), isbn 978-1-906400-11-8 (pdf). 4 vol. 11/2017 comparison of language subset and language extension [2] guidelines for the use of the c++ language in critical systems, june 2008. isbn 978-906400-03-3 (paperback), isbn 978-906400-04-0 (pdf). [3] iec 61508 – electronic functional safety package. [4] en50128: railway applications – communications, signaling and processing systems – software for railway control and protection systems, 2011. [5] iso/iec 8652:2012(e). ada reference manual. copyright ©1992, 1993, 1994, 1995. [6] spark 2014 reference manual. copyright ©2013-2016. [7] "https://github.com/rettichschnidi/clangmisracpp2008". [8] g. marpons. a coding rule conformance checker integrated into gcc [online]. "babel.ls.fi.upm.es/ gmarpons/pubs/prole08codingrules.pdf". [9] ggcc reseny mandrivou v ramci itea3. [10] "http://www.codingstandard.com/section/index/". [11] eiffel language [online]. "http://www.ecmainternational.org/publications/standards/ecma367.htm". [12] ieee standard vhdl language reference manual, 2000. [13] t.musil. návrh metodiky pro vývoj a verifikaci bezpečných algoritmů implementovaných v dynamicky rekonfigurovatelných fpga (methodology for design and verification of algorithms with demands for safety on dynamically reconfigurable fpga), doctoral thesis. czech technical university, 2015. 5 acta polytechnica ctu proceedings 11:1–5, 2017 1 introduction 2 misra c/c++ 3 ada language 4 spark 5 vhdl 6 synthesis 7 discussion 8 conclusion references acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0017 acta polytechnica ctu proceedings 7:17–21, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app numerical discretisation of built structures assumption and reality m. gutermann∗, c. schröder university of applied sciences bremen, institute for experimental static, neustadtswall 30, bremen, germany ∗ corresponding author: marc.gutermann@hs-bremen.de abstract. the second half of the 20th century was affected by the introduction of electronic data processing. the numerical methods appeared to be capable of solving every engineering problem. however, dealing with real problems, an appropriate numerical discretization of built structures is in many cases a difficult task, since fundamental input data concerning the actual properties of the structure, material and mechanical boundary condition couldn’t always be met. typical difficulties are an incomplete documentation, unknown effects of structural faults and uncertain material properties. in this paper our experience in experimental assessment of structures is described and the outcome of experimental versus numerical results is compared in several examples. this paper summarizes finally both prospects and limitations of numerical simulations of built structures and shall show that the identified load bearing capacity is strongly bound to the quality of the numerical structural model. keywords: numerical discretisation, hybrid static, load tests, bridge, foundation, carousel. 1. introduction “a mathematical or mechanical model may be almost perfect it stays a model”. this citation from prof. opitz (tu dresden) points to the fact that many students and even some engineers believe in computational results without reflection since a computers calculation seems always correct. the truth is that the results are as good as their assumptions which lay hopefully always on the safe side. more and more existing structures have to be assessed according their serviceability and load carrying safety. the common procedure and solution strategies are shown in fig. 1. but even numerical assessment requires input data concerning actual material and structural properties as well as mechanical boundary conditions. these preconditions could not always be met so that not any calculated proof is successful. possible reasons are an incomplete documentation, unknown effects of structural faults and uncertainties in the modelling of the structural system with appropriate boundary conditions. another problem occurs if the structures have a historic design: the current technical recommendations are made for building of (new) structures and does not meet the requirements to assess historic designs. figure 1. solution strategies to asses load carrying capacity of built structures a parallel application of computational and experimental methods allows improving the numerical model and leads mostly to a much higher assessment of load carrying capacity, since the calibrated discretisation predicts the structural behaviour in a more realistic way (so called hybrid static fig. 1). on the basis of the experimental observation, the input parameters required for the analysis are obtained, e.g. to assess a railway bridge (see fig. 2). the modelling of boundary conditions as well as material parameters were calibrated using experimental results and led to a more realistic folded-plate-discretisation (see fig. 3). all loadings, recommended by guidelines, could be calculated using this model and sufficient load bearing capacity was proved. the advantage of subsequent extrapolating analysis is its totally non-destructive character. however, the disadvantage is the remaining uncertainty concerning the correctness of a numerical extrapolation. parametric studies or the consideration of large safety margins are means for handling these uncertainties. 17 http://dx.doi.org/10.14311/app.2017.7.0017 http://ojs.cvut.cz/ojs/index.php/app m. gutermann, c. schröder acta polytechnica ctu proceedings figure 2. measurements during operation figure 3. fe-model, parameters calibrated by measurements the following chapters give some examples how experimental data supplement numerical assessment and which advantages result hence. 2. case studies 2.1. masonry arch bridge “clevertorbrücke”, hanover the stone masonry arch bridge crosses the river leine in the center of hanover to transfer a multi-lane principal road. a recurring inspection revealed several open joints, where the mortar has been deeply washed out. an engineering office measured the actual shape of the three-center arch as well material properties. first numerical discretisation, taking only the arch into account as load-carrying member, showed that the bridge should have collapsed under its self-weight already. it seemed obvious that the chosen assumptions did not fit the actual load transfer so that a second calculation took backfill into account [1, 2]. this showed a higher load carrying capacity, but revealed two aspects: first, the proven load-carrying capacity was still too low for high frequented roads; second, the load carrying transfer was a theoretical assumption and could not be proven without experimental confirmation. since load carrying behaviour of backfill may be non-linear, we chose test loading with a special vehicle [3] (see fig. 4). figure 4. belfa test loading of stone masonry arch bridge, hanover the results showed, that there was an effective load transfer in the backing and that this influence stays constant even at higher load levels including partial safety factors (see tab. 1). with the experimental results it was possible to calibrate finite elements models afterwards, even simple beam-spring-models, since it was possible to choose all unknown parameters as spring stiffness or boundary conditions. in summary many influences (e.g. back filling, effective constraints, ...) supports in fact the load carrying system [4], but cannot be considered in calculations without experimental evaluation, especially if their load carrying behaviour may be non-linear at higher stress levels. 2.2. reinforced concrete foundations of wind energy converters in the first decade of this century several reinforced concrete foundations of onshore wind energy converters showed defects as cracks and spalling at concrete surface. some defects had simple causes as shrinkage or creeping but some defects were more severe and led to shut-down of sites (see fig. 5). one incorrect approach had been, that the foundation was preliminary constructed as a foundation of an immobile structure. in fact a wind energy converter is more likely a machine than an immobile construction. an experimental assessment of several affected construction showed under operation movements of several millimetres (f ≤ 2.3 mm) between foundation surface and steel built-in-part. a simple post-calculation by hand confirmed the assessed dimension, although they contain only deformation caused by elongation of concrete or steel as well as materials effects (shrinkage or creeping). poor workmanship may cause even higher deformations. our investigations showed clearly that in case of machine foundations, not only forces but also deformations should be taken into account, especially constructing connections between different materials. 18 vol. 7/2017 numerical discretisation of built structures results calculation measurement (fe-model with backing) strain deflection strain deflection action ε[µm/m] f[mm] ε[µm/m] f[mm] drive through of crane 19 0.33 5 0.35 (g = 48 t) test load bk 16/16 56 0.92 35 0.7 (incl. γ and crane) test load bk 30/30 97 1.57 85 1.2 (incl. γ and crane) table 1. comparison of results at arch crown (fe-model with backing vs. measurement) figure 5. double flange built-in part and observed defect mechanism 2.3. carousel, wuhan (china) after erection of a carousel the local authorities surveyed the construction by measuring strain at one of the main beams and compared these results with the submitted structural analysis of the construction. unfortunately these values differ more than 200 %. we were invited to conduct additional measurements to investigate this deviation. we measured strains at the main beam at several positions (see tab. 2) and compared the results with both simple bar model and 3d-fe-model (see fig. 6). the results showed that the upper sensors close to the weld (d1tk d3tk) measured much higher strains, caused to the influence of the nearby joint. sensor d4tk was situated out of the joints influence, removed more than half of the beam diameter (see fig. 6). as a result this sensor showed appropriate values compared to both bar and 3d-fe-model. figure 6. barand 3d-fe-model model incl. sensor positions in summary an experimental evaluation of calculations has to take into account which assumption had been made for the structural analysis. otherwise the comparison will fail without being well founded. 2.4. steel truss bridge, lomé (togo) the state togo built a steel truss bridge in the year 1960 to transport phosphates from inland to seaport (see fig. 7). in the last decades more and more steel girders showed increasing deterioration by corrosion, obviously caused by the rough environmental conditions (high humidity, salt water, phosphates). it was decided to rehabilitate the bridge by replacing top and bottom chord during train operation. fatigue had to be proven for the remaining girders, e.g. diagonals and support grid. a calculation had not given satisfactory results, so that additional information should be collected by on-site experiments and measurements including the verification of rehabilitation success. figure 7. steel truss bridge crossing the lac togo and tested fields the results were diverging: individual parts showed even higher values, but most stress levels were lower than calculated. the maximum reduction of more than 50 % was reached at the grid beams. the following proof of fatigue showed that almost all members had a sufficient remaining live time of 20 years. 19 m. gutermann, c. schröder acta polytechnica ctu proceedings sensor average measured strain interference cal. strain min [µm/m] max [µm/m] [µm/m] [µm/m] d1tk -147 129 ±40 ∼190 d2tk -196 89 ±50 ∼143 d3tk -259 68 ±50 – d4tk -95 128 ±30 ∼100 d5tk -62 56 ±25 – vb1 -30 21 ±1 26–47 table 2. relative deformation between foundation surface and steel built-in part (double flange system) figure 8. influence of discretisation: a) simple spatial framework b) detailed dispersed truss the experimental results were used afterwards to investigate the influence of calculational assumption on the stress level of truss members and consequentially on their remaining lifetime [5]. in the process the main emphasis was led on the discretisation of static system (see fig. 8) and load application. this showed that the chosen loading (single load, partial distributed load) varied the results of grid beams for several ten percent, as measured and analysed. this was actually an exceptional outcome, all other investigated parameters, as • connection of truss members as hinge or rigid joints • consideration of sheet plates between truss members • realistic discretisation of boundary conditions • joint stiffness between longitudinal and cross beams showed much lower influence, so that they can be generally neglected. in summary the investigations showed, that a more detailed spatial discretisation and especially a realistic load application can lead to much better results, even without experimental assessment. a simple analysis and discretisation of built structure is sufficient as a first approximation. 3. conclusions if we want to describe the physical reality using numerical discretisation we need additional information that may be gained by experiments, e.g. non-destructive testing, monitoring or load-tests. this may be cost and time consuming, but sometimes a little effort may have a great benefit. our experiences, documented in this paper, are summarized with the following statements: • a numerical model stays model, even if it seems perfect. concomitant experimental analysis helps to improve significantly both model and results. • experimental evaluation should meet calculation assumptions. otherwise they could not be compared. • many influences (e. g. back filling, effective constraints, ...) support in fact the load carrying system, but cannot be considered in calculations without experimental evaluation, especially if their load carrying behaviour may be non-linear at higher stress levels. • the calculated result is dependent on both system and boundary assumptions (especially in cases of arches and fatigue proof). change of system parameters may vary the results by 100 % or more. • discretisation of machine foundation should take (tolerable) deformations into account. an analysis as static and stiff system may not be sufficient and may lead to severe defects. acknowledgements we want to send special thanks to the university of applied sciences bremen and all involved parties, which enables us to have done more than 300 successful investigations in the field of analysing load carrying safety of built structures. references [1] d. proske, p. lieberwirth, p. h. van gelder. sicherheitsbeurteilung historischer steinbogenbrücken. mauerwerk 11(4):186–189, 2007. doi:10.1002/dama.200700327. [2] z. orbán, m. gutermann. assessment of masonry arch railway bridges using non-destructive in-situ testing methods. engineering structures 31(10):2287–2298, 2009. doi:dx.doi.org/10.1016/j.engstruct.2009.04.008. [3] m. gutermann, c. schröder. loading vehicle belfa development and experience gained in 10 years of practice. bridge structures 11(1,2):19–31, 2015. doi:10.3233/brs-150081. [4] m. gutermann. an article on experimental assessment of structural safety of solid bridges. proceedings of icem12-12th international conference on experimental mechanics 28, 2004. 20 http://dx.doi.org/10.1002/dama.200700327 http://dx.doi.org/dx.doi.org/10.1016/j.engstruct.2009.04.008 http://dx.doi.org/10.3233/brs-150081 vol. 7/2017 numerical discretisation of built structures [5] w. malgut, k. ammermann, t. sander, m. gutermann. pont lagunaire, togo experimentelle tragwerksanalyse einer stahlfachwerkbrücke zum nachweis der restnutzungszeit. 8 symposium "experimentelle untersuchungen von baukonstruktionen" 2015. 21 acta polytechnica ctu proceedings 7:17–21, 2017 1 introduction 2 case studies 2.1 masonry arch bridge "clevertorbrücke", hanover 2.2 reinforced concrete foundations of wind energy converters 2.3 carousel, wuhan (china) 2.4 steel truss bridge, lomé (togo) 3 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2015.1.0034 acta polytechnica ctu proceedings 2:34–39, 2015 © czech technical university in prague, 2015 available online at http://ojs.cvut.cz/ojs/index.php/app on traversability cost evaluation from proprioceptive sensing for a crawling robot jakub mrva∗, martin stejskal, jan faigl dept. of computer science, czech technical university in prague, technická 2, 166 27 prague, czech republic ∗ corresponding author: jakub.mrva@fel.cvut.cz abstract. traversability characteristics of the robot working environment are crucial in planning an efficient path for a robot operating in rough unstructured areas. in the literature, approaches to wheeled or tracked robots can be found, but a relatively little attention is given to walking multi-legged robots. moreover, the existing approaches for terrain traversability assessment seem to be focused on gathering key features from a terrain model acquired from range data or camera image and only occasionally supplemented with proprioceptive sensing that expresses the interaction of the robot with the terrain. this paper addresses the problem of traversability cost evaluation based on proprioceptive sensing for a hexapod walking robot while optimizing different criteria. we present several methods of evaluating the robot-terrain interaction that can be used as a cost function for an assessment of the robot motion that can be utilized in high-level path-planning algorithms. keywords: terrain traversability, proprioceptive sensing, walking robot. 1. introduction exteroceptive sensing is widely analyzed and summarized in the survey [1], where authors conclude that the most favored method is to assess the traversability characteristics before actually driving the robot into the respective region. such an assessment is based on a terrain model created from exteroceptive sensors like laser range finder or stereo camera. however, the difficulties a robot has while traversing rough terrain (e.g., slippages, softness of the ground, energy consumption, etc.) cannot be foreseen in advance. one has to actually walk through the terrain to feel and measure the interaction between the robot and the ground using proprioceptive sensors like accelerometers, force and torque sensors, etc. according to the survey that provides a study of unmanned ground vehicles (ugv), the generic capability of a robot to negotiate the terrain is the most commonly called as the traversability (along with occasional terms like terrainability, trafficability, mobility, etc.). based on that, we follow this established term and refer to its value as to the traversability cost. although the cost is a common name, its meaning varies among researchers. regarding the mission the robot is requested to accomplish, we need to balance between the time or the distance traveled, the energy consumption, the stability, the danger along the path, etc. having a terrain model, a common method of optimizing the traversability cost is to prefer a smooth and obstacle-free path, but a usage of proprioceptive sensors as indicators of the expected cost does not have such a common direction. in this paper, we report on existing approaches for traversability assessment based not only on exteroceptive sensors but we rather focus on proprioceptive sensors. moreover, instead of wheeled robot, we consider legged robots. the rest of the paper is organized as follows. we identify the main components of the terrain traversability analysis in section 2. first, we provide a brief overview of the exteroceptive sensing based methods for a comparison. next, we follow with an overview of known approaches using proprioceptive sensing. we formulate the main objectives in the view of the terrain traversability evaluation in section 3 and propose traversability evaluation methods for walking robots while focused on utilizing proprioceptive sensors in section 4. finally, a discussion about possible future approaches is given in section 5. 2. related work a great progress in the field of autonomous, perception-based, off-road navigation in robotic unmanned ground vehicles (ugv) was influenced by the darpa learning applied to ground vehicles (lagr) program [2], which ran from 2004 until 2008. the challenge evoked several solutions [3–5] with different approaches of robot sensing which can be divided into two groups as: 1) exteroceptive; 2) and proprioceptive sensing. 2.1. exteroceptive sensing it is reasonable to have information about the terrain prior to traversing it. laser scanner and camera are examples of exteroceptive sensors mostly used in the case of acquiring terrain characteristics. the terrain scan can provide an elevation map for a proper foothold planning [6] and estimation of its traversability [7] using a laser scanner. characteristic features can be obtained from a far-field scan (color image, stereo camera, etc.) and classified based on a model learned from near-field [3, 4, 8] where more data are 34 http://dx.doi.org/10.14311/app.2015.1.0034 http://ojs.cvut.cz/ojs/index.php/app vol. 2/2015 available. with data source getting closer to the robot, we get more precise models of the terrain, but usage of only exteroceptive sensors does not provide much information about the real interaction between the robot and the terrain being traversed and thus the robot can hardly learn from its experience. 2.2. proprioceptive sensing on the other hand, the robot needs to receive a feedback from the terrain to utilize learning from experience. proprioceptive sensors measure the modalities of the terrain that affect the robot motion directly. in the path planning task, the robot plans according to estimated traversability costs. however, the estimation can change when the robot actually encounters the terrain, as it has been applied in the previous approaches [3, 4, 8] using wheeled robot with bumpers, wheel encoders for a slip measurement or imu with gyros and accelerometers for measuring the roughness of the terrain. for example, a tall-grass area can be estimated as a non-traversable using only a range measurement, but it turns out that the robot can go through it without a significant difficulty. the traversability cost assessment is closely related to the terrain classification (or discrimination) assuming that the terrains of the same kind provide the same conditions for traversing. based only on proprioceptive sensors, the classification can be done using accelerometers [9] (the faster the speed, the better the accuracy) or yaw-angle variations [10] on a wheeled robot, or using servo drives feedback on a hexapod walking robot [11, 12]. focusing now mainly on legged robots, an early analysis of terrain traversability for legged locomotion using active perception was proposed by krotkov back in 1990 [13] studying the terrain stiffness and surface friction upon foot contact on a planetary rover – the ambler robot. however, the final path of the ambler robot is computed on a grid terrain elevation map avoiding occluded cells [14], i.e., without the possible knowledge gained from the proprioceptive sensors. a more matured solution [15] utilizes a biologically inspired gait on a hexapod crawler. carrying a lot of proprioceptive sensors, the robot was able to negotiate small obstacles using few hard-coded reflexes which ensured quality footholds during the motion. however, the estimation of the traversability cost relies only on exteroceptive sensors and the shape of the terrain. regarding our focus, we consider the work of hoffmann et al. as the most related to our approach. they presented how different sensory modalities affect the accuracy of the terrain discrimination using a quadruped puppy robot [16]. they also studied the relationship between the gait used and the classifier accuracy [17] including using sequences of different gaits to get better results. 3. problem statement the terrain sensing and the evaluation of the traversability cost of the robot motion fits into the scope of path planning. assuming we have a map of the environment in terms of positions of untraversable obstacles or regions, we can build a weighted graph on top of the map. although we consider evaluation of the cost for path planning, the planning itself is out of the scope of this paper. therefore, we consider the planning problem can be solved using optimal planners like a* [18] or d* [19] on a graph with known weights, i.e., the costs on the edges. the path consists of a sequence of actions (the robot moves along an edge using a particular gait) that have some cost—the traversability cost—which can be computed from various sources based on different criteria and different tasks the robot is performing. in general, we can distinguish sources of information the robot receives (terrain-sensor modalities) and the outcomes of the resulting robot motion (cost modalities) as can be seen in fig. 1. proprioceptive exteroceptive sensors terrain gait control f(s) evaluation c cost terrain-sensor modalities cost modalities figure 1. schema of the robot perception module. the input modalities represent different sensor measurements of the terrain which are used in a function f to evaluate the traversability cost c. the cost is multimodal in general but usually only one modality is used for planning (e.g., the robot speed). we can imagine that a terrain can be described by several characteristic features: shape, consistency, temperature, friction, etc. which can be measured by various sensors. each such a feature can be viewed as a modality that is either directly measured or remains hidden. each sensor refers to different modalities and combined together, we get a set of observable modalities on the input side of the robot perception module generating a multidimensional vector of sensor data. in general, we can say that more modalities— and hence more information—about the terrain we have, the better the estimation of its traversability cost we can get. notice that some of the modalities may provide more useful information (regarding the cost evaluation) than others. the output side of the module is also multimodal although it is not as obvious because usually only one modality is used for the traversability cost estimation (e.g., the robot speed while traversing the terrain). 35 j. mrva, m. stejskal, j. faigl acta polytechnica ctu proceedings the main problem is the middle part (of the schema in fig. 1) that consists of an evaluation function f which transforms the sensory measurement into a single (albeit multimodal) cost. the methodology how to extract a single cost from a lot of data in time, frequency or other domain is not a straightforward task and hence results vary among researchers from the simple and obvious findings to more and more sophisticated methods. 3.1. terrain-sensor modalities the input modalities refer to the robot-terrain interaction from which we can gather the sensory data. however, we can gather such data only from the observable modalities. for example, without a camera image, we can hardly determine the color of the terrain. a (certainly not complete) list of terrain-sensor modalities should include following terrain features: • shape (surface) – the 3d shape of the terrain or obstacles is useful for precise motion planning and it is usually scanned by exteroceptive sensors but can also be inferred from an advanced touch sensor. • color – a color camera image of the terrain area can enhance the terrain discrimination (e.g., flat sand vs. concrete). • consistency – a gravel, snow or sand is not a solid terrain and its surface is usually changed during and after the robot motion while leaving trace or marks on such terrain. this can be measured by sensible touch sensors or by comparing the surface shape before and after the motion referring to the terrain changeability or granularity. • softness – differences between solid (e.g., concrete) and soft (e.g., carpet) terrains can affect greatly the robot performance. this modality is measurable only by proprioceptive (e.g., force) sensors. • compliance – a terrain can look stiff (e.g., grass or small branch) but does not resist to the robot motion and usually regains its shape afterwards; so, a compliant terrain is penetrable. this is also measurable only by proprioceptive sensors. • adhesion – an adhesive terrain offers better friction and hence better traction which is crucial to ensure stable footholds and permit high accelerations. a force sensor or slippage analysis is needed to measure the adhesion with respect to the robot leg shape and material. • temperature – in some cases, e.g., on a volcano, a robot might need to avoid hot surfaces in order not to damage itself. the temperature (scanned by a thermal camera) can also be used for a better estimate of terrain traversability by analysing the relations between the terrain granularity (compactness) and thermal transients [20]. as it is shown in fig. 1, the values of input modalities measured by exteroceptive sensors are (in general) dependent on the terrain being scanned and also on the gait that drives the robot. the sensor readings can be affected when using a different gait— e.g., a fast tripod gait causes shaky motion of the robot and the images taken can be blurred. similarly, when measuring by proprioceptive sensors, some of the terrain-sensor modalities can change its value depending on the robot motion. for example, the terrain can seem solid and adhesive while traversing slowly, and crumbling or slippery when accelerating (on gravel or ice). another example for a wheeled vehicle is a sand (desert) that can be traversable until a small change in the control is applied and then it become completely untraversable. focusing on proprioceptive sensors and legged robots, the most important terrain-sensor modalities are those which directly affect the robot motion and hence its performance: shape, consistency, softness, compliance, and adhesion. 3.2. cost modalities in general, the outcome (or the cost) of the robot motion does not have a single scalar value. for example, answering a question: “how was the robot going?” with “5” looks like some information has been lost. instead, for example, we would like to know that it went fast but spent a lot of energy and hit several obstacles along the way. the crucial part is then to balance the trade-off between all of the possible outcomes—the cost modalities— of our interest. the outcomes (cost modalities) can be the following (again, we do not claim it is a complete list): • average speed (time) – the overall time and speed has to be evaluated relatively to the robot capabilities. either a reliable odometry or external motion capture system is needed for a proper evaluation. • energy consumption – a robot might have a limited energy capacity to fulfill its task, and therefore, it needs to care about the energy consumption (e.g., to switch to a more energy-efficient gait [21]). • maximal torque – in very rough terrains, the balance in exploiting all motors the same can be impaired and very high torque values of some motors can cause overheating or damage of servos and the robot itself. • uncertainty of localization – continuous robot body motion—if not smooth enough—can negatively affect the reliability of range sensors or camera-based visual localization. • stability risk – the robot posture can be close to its stability margins during the motion, which increases the risk of falling and should be counted in further path planning. • damage risk – a precise terrain analysis can unveil risky areas where the robot can be damaged (e.g., after a small slip), and therefore, these areas should be either avoided or at least considered. 36 vol. 2/2015 notice that the aforementioned cost modalities are dependent not only on the terrain the robot is traversing but also on the gait that is used to control the robot (except the risk of damage from a prior terrain analysis to avoid such a terrain). the traversability cost is usually evaluated using only a single modality when a robot is performing a simple task. however, if the robot has to perform a long-term mission and meanwhile learn from its own experience to achieve better results, a single modality is not enough and the other modalities have to be considered. a robot can then optimize its decisions in order to keep a high performance in a long period. 4. use case the proposed discussion of multiple modalities on both the terrain-sensor interface and the evaluation of the traversability cost can be applied on almost every mobile robot. however, each robot has different set of sensors and thus it can measure different terrain features and thus measure different cost modalities. here, we present an example—a use case—for a hexapod walking robot operating in a rough terrain with limited proprioceptive sensory data. the platform, used methodology, and testing scenarios are described in the following parts. in section 4.4, achieved results are presented. 4.1. used hexapod platform we used an affordable platform phantomx hexapod mark ii with an adaptive gait [22] that enables this robot to traverse uneven terrains and negotiate small obstacles. the gait is a periodic-based (in terms of alternating the legs in a given order) but alters and reacts on the underlying terrain surface. the robot utilizes its servo drives feedback for the tactile sensing of the ground and servo drives are also the only sensory information the robot has (i.e., the robot is technically blind). 4.2. methodology of cost evaluation following the set of possible traversability cost modalities listed in section 3.2 and the sensors available, we consider only the speed, energy (power) consumption, and maximal torque. the speed is given from the running time of the experiments and known distance of the traversed path. the energy consumption is estimated very roughly using several approximations. firstly, the instantaneous energy consumed (the power) is proportional to the drawn current assuming a constant voltage (p ∝ i). secondly, the current is proportional to the torque of the servomotor (i ∝ τ). thirdly, the torque is (according to the servo manufacturer) proportional to the servo drive controller position error e, (τ ∝ e). therefore, the power consumption (in a small discrete time step) can be inferred from the sum of absolute values of servo position errors p ∝ 18∑ i=1 |ei|. (1) for simplicity, we leave the units and scale because we only need to know the relative changes in the energy consumption under different conditions. finally, the maximal torque is computed similarly as τmax ∝ max e. (2) 4.3. testing scenarios the traversability cost evaluation was tested on three different terrains shown in fig. 2. the office floor is perfectly flat while the wooden blocks include obstacles with height about 5 cm (for comparison, the leg femur-tibia and tibia-foot links are 7 cm, resp. 13 cm long). the third terrain contains free wooden obstacles (2 cm high) that are not fixed to the floor and thus can be shifted during the robot traversal. the trajectory during experiments was equally long on all of the terrains and the robot was driven by adaptive gait [22] under 3 different configurations (pentapod, tetrapod and tripod). office floor movable obstacles wooden blocks figure 2. terrains traversable by the adaptive gait 4.4. results the measured experimental results are shown in table 1. as can be seen from the speed comparison, the robot is not slowed by obstacles and hence the used gait (in each of the three configurations) is very adaptive. nevertheless, its speed is slow even on the flat office floor and there can surely be found a faster gait for flat terrains which, however, may not be able to traverse other terrains. terrain office movable blocks gait 5/4/3 5/4/3 5/4/3 speed [mm/s] 9/15/22 9/15/22 9/15/22 work [e/mm] 45/28/19 52/32/23 47/28/21 power [e/s] 39/42/43 45/48/51 42/43/48 max torque 47/45/44 53/48/65 62/60/66 table 1. different cost modalities experimentally evaluated on different terrains for the same traveled distance using adaptive gait with different number of legs in support phase. three values in each cell stand for pentapod / tetrapod / tripod gait. 37 j. mrva, m. stejskal, j. faigl acta polytechnica ctu proceedings if we look at the traversability cost regarding different modality—the energy consumption, we can see that traversing the flat terrain is the least energy consuming. however, the other terrains have no more than about 10% increase in power consumption. traversing movable obstacles causes the highest energy consumption, which can be explained considering friction and leg configurations. when a leg slide sideways on a floating obstacle, a more momentum is created on the joints and thus more torque is needed to counteract this behavior. naturally, it is easier to walk with legs under the body than with legs straddled. another perspective of the evaluation is by comparing the maximal torque in the servo drives measured during the robot motion. we can see that the highest torque was measured when traversing the blocks. this indicates that such a terrain causes legs to be occasionally more loaded than others (e.g., after a small slip on the edge of a block), which is projected also into the average energy consumption (which is based on torque values). regarding the maximal torque values measured, we can also see that the tetrapod gait suffers less from high torque values (caused mainly by slippages), such that the impact after a slippage is not as big as for the pentapod or tripod gait. 5. conclusion we have shown that the evaluation of traversability cost, which is an important part needed for pathplanning, depends on the modality of sensory data as well as on the modality of the cost itself. each cost modality represents a different perspective of evaluating the robot performance and we show how sensory data can be transformed into the traversability cost estimation. while different situations need different cost modalities to be considered, in general, we need to find a trade-off between them to assess the cost more appropriately. we present a use case of the proposed idea in realexperimental evaluation with a hexapod walking robot traversing terrains with various difficulty. using only a single gait for all terrains might look appropriate according to the measured speed, but considering another perspective can unveil the potential risk of servo damage and switching to another gait (slower, but not the slowest) would be a more suitable solution. getting more into the problem of traversability cost estimation in the future work, we would like to take into account another modality—a gait modality. combined all modalities together, we can better model the perception of the robot which is a key factor in assessing the traversability costs to different terrain areas. moreover, the perception can be connected to learning and mapping between the terrain features and corresponding costs can be found automatically. acknowledgements the presented work has been supported by the czech science foundation (gačr) under research project no. 1509600y. the work of jakub mrva has been also supported by the grant agency of the czech technical university in prague, grant no. sgs15/208/ohk3/3t/13 references [1] p. papadakis. terrain traversability analysis methods for unmanned ground vehicles: a survey. engineering applications of artificial intelligence 26(4):1373–1385, 2013. doi:10.1016/j.engappai.2013.01.006. 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[18] p. hart, n. nilsson, b. raphael. a formal basis for the heuristic determination of minimum cost paths. ieee transactions on systems science and cybernetics 4(2):100–107, 1968. doi:10.1109/tssc.1968.300136. [19] a. stentz. optimal and efficient path planning for unknown and dynamic environments. technical report cmu-ri-tr-93-20, carnegie mellon robotics intitute, 1993. [20] c. cunningham, i. nesnas, w. whittaker. terrain traversability prediction by imaging thermal transients. in ieee international conference on robotics and automation (icra), pp. 3947–3952. 2015. doi:10.1109/icra.2015.7139750. [21] n. kottege, c. parkinson, p. moghadam, et al. energetics-informed hexapod gait transitions across terrains. in ieee international conference on robotics and automation (icra), pp. 5140–5147. 2015. doi:10.1109/icra.2015.7139915. [22] j. mrva, j. faigl. tactile sensing with servo drives feedback only for blind hexapod walking robot. in proceedings of the 10th international workshop on robot motion and control (romoco), pp. 240–245. 2015. doi:10.1109/romoco.2015.7219742. 39 http://dx.doi.org/10.1177/027836499601500204 http://dx.doi.org/10.1016/j.robot.2014.07.006 http://dx.doi.org/10.1109/tssc.1968.300136 http://dx.doi.org/10.1109/icra.2015.7139750 http://dx.doi.org/10.1109/icra.2015.7139915 http://dx.doi.org/10.1109/romoco.2015.7219742 acta polytechnica ctu proceedings 2:34–39, 2015 1 introduction 2 related work 2.1 exteroceptive sensing 2.2 proprioceptive sensing 3 problem statement 3.1 terrain-sensor modalities 3.2 cost modalities 4 use case 4.1 used hexapod platform 4.2 methodology of cost evaluation 4.3 testing scenarios 4.4 results 5 conclusion acknowledgements references 99 acta polytechnica ctu proceedings 2(1): 99–102, 2015 99 doi: 10.14311/app.2015.02.0099 suzaku view of magnetic cataclysmic variables t. yuasa1 1institute of space and astronautical science (isas), japan aerospace exploration agency (jaxa), 3-1-1 yoshinodai, chuo, sagamihara, kanagawa 252-5210, japan corresponding author: yuasa@astro.isas.jaxa.jp abstract results of magnetic cataclysmic variable studies performed with the suzaku satellite are reviewed in this article. particular emphasis is placed on the recent update of x-ray spectral model of intermediate polars, possible kinematically redshifted fluorescent fe k emission lines, and the magnetic cv contribution to the galactic ridge x-ray emission. keywords: cataclysmic variables intermediate polars x-rays. 1 introduction magnetic cataclysmic variables emit hard x-rays from hot plasma with temperatures of 108−9 k contained in the post-shock accretion column on the magnetic pole(s) of a white dwarf. japan’s x-ray observatory satellite suzaku , providing x-ray ccd coverage below 10 kev and hard x-ray response up to 50 kev with the si-pin diode, has been actively observing magnetic cvs, particularly, intermediate polars through its initial observation phase to following ao phases. as of 2013, more than 20 intermediate polars have been observed, and main results have been reported in [11], [15], [13], and [3]. in the following sections, we review major results reported in these articles. 2 x-ray spectral model of intermediate polars in [15], we have constructed, based on the previous study by [10], an x-ray spectral model of the postshock plasma of intermediate polars, by numerically solving the three conservation equations (mass, momentum, and energy) with a newly reported plasma cooling function [9]. since the shock temperature depends on the gravitational potential depth, this model contains a mwd/rwd ratio as a free parameter, and by combining the mwd/rwd ratio with a theoretical mwd − rwd ratio (e.g. by [5]), one can estimate mwd and rwd from observed spectra. figure 1 shows an example of spectral fitting with the multi-temperature model. a single-temperature model apparently fails to reproduce the observed spectrum, especially in the fe k emission line region (1 upper panels). this can be understood as follows; the hard x-ray continuum requires hotter temperature (due to emission from hot plasma close to the shock) although the apparent he-like and h-like fe kα emission line ratios require much cooler plasma temperatures (the model underestimates the he-like fe kα line and overestimate the h-like fe kα line). figure 1: suzaku spectra of tv col fitted with a single-temperature model (upper panels) and our model [15] with emissivity gradient (lower panels). crosses and red curves are observed source count rates and response-convolved model count rates. right panels present blow-up view of the fe emission line region. note that in both cases, 6.4 kev fe k fluorescent line was modeled with a single gaussian of which normalization was allowed to freely vary. our multi-temperature model, on the other hand, successfully reproduces the fe k emission lines as well as the over-all spectral shape. the best fit parameters give acceptable fit statistics, and a wd mass estimate of 0.91(0.83−1.00) m�. figure 2 summarizes estimated wd masses of 17 ips compared with the average wd masses of isolated and non-magnetic accreting systems. 99 http://dx.doi.org/10.14311/app.2015.02.0099 t. yuasa 2.1 recent updates [2] has recently reported an updated version of the intermediate polar spectral model that takes into account several aspects in the model geometry and the numerical calculation; (i) the new model can have a dipolar accretion column geometry as well as a cylindrical column, (ii) conservation equations are set for ions and electrons separately, and (iii) the accretion rate can be variable. figure 3 illustrates the accretion geometry which was considered in their paper. the two-fluid treatment is to account for the delayed increase of the electron temperature after the shock where ions are first heated, and electrons are collisionally heated relatively slowly. figure 2: distribution of estimated masses of wds in 17 nearby intermediate polars [15]. average wd masses are shown for isolated wds [4] and non-magnetic cvs [8]. broad-band spectra calculated by [2] are shown in figure 4 together with ratios between different specific accretion rates at the shock. major differences are expected, in particular, in lower accretion rates with dipolar geometry. based on this, the authors expect that the estimated wd mass could have been artificially reduced in systems like ex hya which has a low accretion rate. 3 spin modulation of centroid energy of fluorescent fe kα emission line [3] analyzed suzaku data of v1223 sgr and found a spin modulation of the centroid energy of the fluorescent fe kα emission line as shown in the third panel of figure 5. the maximum energy shift in terms of centroid energy of a single gaussian was ∼ 20 ev. when the fluorescent line is fitted with two gaussians, one at 6400 ev and the other having freely varying centroid energy, the minimum of the centroid energy of the second component is 6.29+0.10 0.11 kev. figure 3: dipolar and cylindrical geometry of the post-shock accretion region that was assumed in [2]. figure 4: upper panels: model spectra calculated for mwd = 0.7 m� with various specific accretion rates a and (a) cylindrical and (b) dipolar accretion geometry. lower panels: ratio spectra normalized by that for a = 100 g cm−2 s−1. the authors attributed this red-ward shift to the kinematic doppler shift caused by reflection from the rapidly falling pre-shock accretion matter (vff ∼ a few×1000 km s−1), and interpreted that the spin modulation is caused by the changing viewing angle (timedependent radial velocity of the accreting pre-shock material). although the detection of the second (redshifted) component is marginal in suzaku data, the near future astro-h observatory will definitively detect this with splendid energy resolution of ∼ 5 ev 100 suzaku view of magnetic cataclysmic variables (fwhm), and will provide a new technique to estimate the gravitational potential depth of a wd from the magnitude of the energy shift. figure 5: spin-modulation of count rates, and best-fit parameters of absorption column density, centroid energy of fluorescent fe kα emission line, and its equivalent width. adopted from [3] with additional labels. 4 serendipitous discoveries although suzaku x-ray telescope has a tightly collimated field of view of ∼ 18 arcmin× 18 arcmin, several new magnetic cvs are identified with their intense three fe kα emission lines as presented in figure 6. figure 6: suzaku/xis spectra of serendipitous sources that are thought to be magnetic cvs. adopted from [6], [12], and [1]. as claimed and spectroscopically confirmed in [7] and [14], respectively, magnetic cvs (more precisely intermediate polars) are the major contributors of the galactic ridge x-ray emission (grxe), so there should be enormous number of magnetic cvs in the field. these findings partially support this idea of omnipresence of hard x-ray emitting magnetic cvs in the galaxy. figure 7 shows a fit result of the broad-band grxe spectrum with the ip model and an additional lower temperature component (which is attributed to superposition of a number of dim coronal sources). figure 7: broad-band spectral fitting of the grxe using the intermediate polar spectral model [14]. 5 conclusion suzaku will continue to observe several magnetic cvs, for example, in 2013 (ao-8), v1223 sgr will be reobserved for 180 ks to reconfirm the spin modulation of the centroid energy of the fluorescent fe kα emission line. the forthcoming astro-h mission will provide a great step forward in understanding the accretion geometry, post-shock region, reflection, and many other physical processes taking place in magnetic cvs. references [1] bernardini, f. et al., 2012, a&a, 542, a22 [2] hayashi, t., & ishida, m. 2013, arxiv e-prints [3] hayashi et al., 2011, pasj, 63, 739 [4] kepler, s. o. et al., 2007, mnras, 375, 1315 doi:10.1111/j.1365-2966.2006.11388.x [5] nauenberg, m. 1972, apj, 175, 417 doi:10.1086/151568 [6] nobukawa, m., koyama, k., matsumoto, h., & tsuru, t. g. 2009, pasj, 61, 93 [7] revnivtsev, m., sazonov, s., gilfanov, m., churazov, e., & sunyaev, r. 2006, a&a, 452, 169 [8] ritter, h., & kolb, u. 2003, a&a, 404, 301 101 http://dx.doi.org/10.1111/j.1365-2966.2006.11388.x http://dx.doi.org/10.1086/151568 t. yuasa [9] schure, k. m., kosenko, d., kaastra, j. s., keppens, r., & vink, j. 2009, a&a, 508, 751 [10] suleimanov, v., revnivtsev, m., & ritter, h. 2005, a&a, 435, 191 [11] terada, y. et al. 2008, pasj, 60, 387 [12] uchiyama, h. et al., 2011, pasj, 63, 865 [13] yuasa, t. 2013, suzaku studies of white dwarf stars and the galactic x-ray background emission, springer theses ser. (springer) [14] yuasa, t., makishima, k., & nakazawa, k. 2012, apj, 753, 129 doi:10.1088/0004-637x/753/2/129 [15] yuasa, t. et al., 2010, a&a, 520, a25 discussion s. balman: have you checked any correlation between m�, temperature, and luminosity in your paper on the suzaku sample? t. yuasa: there was no correlation for any parameter such as m�, temperature, or luminosity. s. scaringi: does the geometry of the post-shock region affect the wd mass estimation? t. yuasa: yes, it affects it as explained in [2]. quantitatively, the dipolar case poses geometrical compression which leads to increased emissivity and therefore lower apparent plasma temperature compared to the cylindrical case. 102 http://dx.doi.org/10.1088/0004-637x/753/2/129 introduction x-ray spectral model of intermediate polars recent updates spin modulation of centroid energy of fluorescent fe k emission line serendipitous discoveries conclusion 1 acta polytechnica ctu proceedings 1(1): 1–12, 2014 1 doi: 10.14311/app.2014.01.0001 old and new from multifrequency astrophysics franco giovannelli1, lola sabau-graziati2 1inaf istituto di astrofisica e planetologia spaziali, area di ricerca di tor vergata, via fosso del cavaliere, 100 i00177 roma, italy 2intadpt. cargas utiles y ciencias del espacio, c/ra de ajalvir, km 4 e28850 torrejón de ardoz, madrid, spain corresponding author: franco.giovannelli@iaps.inaf.it abstract in this short review paper we comment on some the most important steps that have been made in the past decades for a better understanding of the physics governing our universe. the results we discuss come from the many groundand-space-based experiments developed for measuring astrophysical sources in various energy bands. these experimental results are discussed within the framework of current theoretical models. because of the limited length of this paper, we have selected only a few topics that, in our opinion, have been crucial for the progress of our understanding of the physics of cosmic sources. keywords: multifrequency astrophysics. 1 introduction with the advent of space-based experiments, it has been demonstrated that cosmic sources emit energy practically across the entire electromagnetic spectrum, albeit from different physical processes. several observations stand as witness to these processes. since the observed fluxes from cosmic sources can be highly variable in time and frequency, it follows that the physical processes from which they originate are in themselves highly variable. therefore simultaneous multifrequency observations are strictly necessary in order to understand the actual behaviour of cosmic sources. indeed, space experiments have opened practically all of the electromagnetic “windows” on the universe. a discussion of the most important results coming from multifrequency photonic astrophysics experiments will provide new inputs for the advance of our knowledge of physics, very often in the most extreme physical conditions. we remark on the sheer magnitude of the high quality data across practically the whole electromagnetic spectrum that has become available to the scientific community since the beginning of the space era. with these data, we are attempting to explain the physics governing the universe, and, moreover, its origin, which has been and still is a matter of the greatest curiosity for humanity. we know for certain that the universe has an absolute power limit lmax ∼ εpl/tpl ∼ c5/g ∼ 3.6×1059 erg s−1, where εpl and tpl are the planck energy and planck time, respectively, c the light velocity and g the gravitational constant. this amount of power is produced in different kind of cosmic sources, namely, the early universe (eu), quasars (qsos) and active galactic nuclei (agns), supernovae (sne), neutron stars (nss), and black holes (bhs), all types of galaxies with their stars and interstellar medium (ism), and intergalactic medium (igm) (e.g., lipunov, 1995). they radiate particles and photons at different levels of energy across the entire electromagnetic spectrum from their origins. however, the cosmic particle radiation arriving near earth, with energies from ∼ 106 to ∼ 1020 ev, is nearly isotropic, because of the galactic magnetic field, which cancels any particular directionality in the galaxy. such cosmic particle radiation apparently includes the nuclei of all known elements, as well as electrons, positrons, and antiprotons. so in spite of the cosmic rays being carriers of rich astrophysical information, it is very difficult to understand their message clearly. indeed, although it is evident that they must originate in different sources, it is at the same time extremely difficult to separate the different contributions. for more complete discussions, the reader can note the substantive books on this topic, containing excellent reviews, published by the italian physical society (giovannelli & mannocchi, 1989, 1991, 1993, 1995, 1997, 1999, 2001, 2003, 2005, 2007, 2009, 2011), by the italian astronomical society (giovannelli & sabau-graziati, 1996; 1999, 2002a, 2002b, 2010a, 2012a), by the chinese journal of astronomy and astrophysics (giovannelli & sabau-graziati, 2003, 2006, 2008), and by acta poly1 http://dx.doi.org/10.14311/app.2014.01.0001 franco giovannelli, lola sabau-graziati technica (giovannelli & mannocchi, 2013; giovannelli & sabau-graziati, 2014). with “passive” physics experiments (.i.e., observations) we view our universe, while with active physics experiments we try to reproduce some of the physical conditions and processes occurring somewhere in the universe. both kinds of experiments converge to the knowledge of the physics governing the universe. in this paper we will discuss what seem to us some of the most relevant results obtained in the recent past that significantly improve our knowledge of the physics governing our universe. deeper discussions about astroparticle physics can be found in the review papers by giovannelli (2007, 2009, 2011, 2013). giovannelli & sabau-graziati (2010b, 2012b), and de angelis, mansutti & persic (2008) discussed in their review papers the multifrequency behaviour of high energy cosmic sources, and very high energy (vhe) γ-ray astrophysicsal sources. 1.1 astroparticle physics development the subject of high energy astrophysics is generally approached through the study of cosmic rays. the reason for this is historical in nature. since the discovery of this extraterrestrial radiation by victor hess (1912), the scientific research involved in trying to discover the nature nature of these sources has been extensive. as a result, many separate research fields have been developed. before particle accelerators came into operation, high energy cosmic rays were the laboratory tools for investigations of elementary particle production, and to date they are still the only source of particles with energies greater than 1012 ev. the research into the composition of the radiation led to the developing study of the astrophysical environment using the information in the charge, mass, and energy spectra; this field is also known as particle astrophysics. now, the large hadronic collider (lhc), described by straessner et al. (2011), is able to reach tev energies for p-p interactions, and has attained energyies of 7 tev, in order to search for the higgs’ boson with the atlas detector (aad et al., 2012). no significant excess of events over the expected background is observed and limits on the higgs boson production cross section are derived for a higgs boson mass in the range 110 gev < mh < 300 gev. the observations exclude the presence of a standard model higgs boson with a mass 145 < mh < 206 gev at 95% confidence level. of great importance was the discovery of high energy photons near the top of the earth’s atmosphere. this originated the development of new astronomical fields such as the x-ray or γ-ray astronomy. but many of these high energy photons have their origin in the interactions of the high energy charged particles with cosmic matter, light, or magnetic fields. the particle astrophysics and the astronomical research fields have found in this fact a bond to join their efforts in trying to understand the high energy processes which occur in astrophysical systems. a summary on the status of the search for the origin of the highest energy cosmic rays has been published by biermann (1999). he mentioned several competing proposals, such as the supersymmetric particles. biermann notes that gamma ray bursts must also give rise to energetic protons, interacting high energy neutrinos and cosmological defects. in his paper, biermann discussd the propagation of these particles, assuming that they are charged, and concluding that the distribution of arrival directions of the highest energy particles on the sky ought to reflect the source distribution as well as the propagation history. he remarked that the present status of our observations can be summarized as inconclusive. however, he concluded as follows: if we can identify the origin of the events at the highest energies, beyond 5× 1019 ev, the greisen–zatsepin–kuzmin cutoff due to the microwave background, near to 1021 ev, and if we can establish the nature of their propagation through the universe to us, then we will obtain a tool to do physics at eev energies. the arrival directions of ≥ 60 eev ultra-high-energy cosmic rays (uhecrs) cluster along the supergalactic plane and correlate with active galactic nuclei (agn) within ≈ 100 mpc (abraham et al., 2007, 2008). the association of several events with the nearby radio galaxy cen a supports the paradigm that uhecrs are powered by supermassive black-hole engines and accelerated to ultra-high energies in the shocks formed by variable plasma winds in the inner jets of radio galaxies. the gzk horizon length of 75 eev uhecr protons is ≈ 100 mpc, so that the auger results are consistent with an assumed proton composition of the uhecrs. in this scenario, the sources of uhecrs are fr ii radio galaxies and fr i galaxies like cen a with scattered radiation fields that enhance uhecr neutral–beam production. radio galaxies with jets pointed away from us (i.e., more toward the plane of the sky) can still be observed as uhecr sources due to deflection of uhecrs by magnetic fields in the radio lobes of these galaxies. a broadband ∼ 1 mev–10 eev radiation component in the spectra of blazar agn is formed by uhecr–induced cascade radiation in the extragalactic background light. this emission is too faint to be seen from cen a, but could be detected from more luminous blazars (dermer et al., 2009). recent evidence from the pierre auger observatory suggests a transition, at 5 eev-10eev in the composition of ultra high energy cosmic rays (uhecrs), from protons to heavier nuclei such as iron (abraham et al., 2010). piran (2010) considered the implications of 2 old and new from multifrequency astrophysics the heavier composition on the sources of uhecrs. he concluded that with typical reasonable parameters of a few ng for the extra–galactic magnetic field (egmf) intensity and a coherence distance of a mpc the distance that nuclei uhecr above the gzk energy traverses before photodisintegrating is only a few mpc. in spite of the significantly weaker limits on the luminosity, cen a is the only currently active potential source of nuclei uhecrs within this distance. the large deflections erases the directional anisotropy expected from a single source. if indeed the composition of above gzk– uhecrs is iron and if the egmf is not too small then cen a is the dominant source of observed nuclei uhecrs above the gzk limit. in summary, charged cosmic rays are influenced in their propagation through space by the magnetic fields in the galaxy, and for the lowest energy particles also in the solar system. the result is that the distribution of arrival directions as the radiation enters the earth’s atmosphere is nearly isotropic. it is not possible to identify the sources of the cosmic rays by detecting them. however, in the high energy interactions produced at the source, electrically neutral particles such as photons, neutrons, and neutrinos are also produced and their trajectories are not deviated, being directed from their point of origin to the observer. owing to their short lifetime, neutrons cannot survive the path length to the earth (decay length ∼ 9 pc at 1 pev) and neutrinos do not interact efficiently in the atmosphere. it is in this context that the gamma ray astronomy has demonstrated itself to be a powerful tool. the observations made to date have detected γ-rays from many astronomical objects such as neutron stars, interstellar clouds, the center of our galaxy and the nuclei of active galaxies (agns). one might expect very important implications for high energy astrophysics from the observations at energies greater than 1011 ev of extragalactic sources (e.g., hillas & johnson, 1990). the fluxes of γ-rays at these energies are attenuated because of their interactions with the cosmic radio, microwave, infrared and optical radiation fields. measurements of the flux attenuation can then provide important information on the distribution of such fields. for instance, the threshold energy for pair production in reactions of photons with the 2.7 k background radiation is reached at 1014 ev and the absorption length is of the order of ∼ 7 kpc. for the infrared background the maximum absorption is reached at energies greater than 1012 ev. the qualitative problem of the origin of cosmic rays is practically solved, while the quantitative problem in determining the fraction of them coming from the different possible sources is still open. 2 very high energy sources the most exciting results of the last decade have been obtained in the field of vhe astrophysics from different experiments (e.g. cgro/egret, wipple, hegra, cangaroo, celeste, stacee, tibet, hess, veritas, milagro, magic) that detected many vhe cosmic sources. the high energy sky. with the exception of crab nebula, vela x, and 3c 273, was empty until middle nineties. “fast forward” to 19th april 2012, the vhe sky (e > 100 gev) is populated by 107 cosmic sources: 46 out of 107 extragalactic and 61 galactic (http://www.mppmu.mpg.de/∼rwagner/sources/ or http://tevcat.uchicago.edu). one of the most interesting results has been the determination of the spectral energy distribution (sed) of the crab nebula, thanks to many measurements obtained by different he–vhe experiments (albert et al., 2008b). another exciting result has been the detection of the first variable galactic tev source, namely the binary pulsar psr b1259-63 (aharonian et al., 2005). they found that the radio silence occurs during the time in which the pulsar is occulted by the excretion disk of the be star. the many detected sources, representing different galactic and extragalactic source populations, are supernova remnants (snrs), pulsar wind nebulae (pwne), giant molecular clouds (gmcs), star formation regions (sfrs), compact binary systems (cbss), and active galactic nuclei (agns). paredes & persic (2010) reviewed the results from magic cherenkov telescope for most of the former class of sources. models of tev agns have been discussed by lenain (2010). 3 diffuse extragalactic background radiation after the big bang, the universe started to expand with a fast cooling. the cosmic radiation observed now is probably an admixture of different components which had their origin in different stages of the evolution as the results of different processes. this is the diffuse extragalactic background radiation (debra), which, if observed in different energy ranges, allows the study of many astrophysical, cosmological, and particle physics phenomena (ressell & turner, 1990. debra is the witness of the whole history of the universe from the big bang to present time. such history is marked by three main experimental witnesses supporting the big bang theory (e.g. giovannelli & sabau-graziati, 2008): the light element abundances (burles, nollett & turner, 2001); the cmbr temperature at various redshifts as determined by srianand, petitjean & ledoux (2000), and 3 franco giovannelli, lola sabau-graziati the references therein; the cmb at z = 0 as result of cobe (tcmbr(0) = 2.726 ± 0.010 k), which is well fitted by a black body spectrum (mather et al., 1994). at z' 2.34, the cmbr temperature is: 6.0 k < tcmbr(2.34) < 14.0 k. the prediction from the hot big bang: tcmbr = tcmbr(0) × (1 + z) gives tcmbr(2.34) = 9.1 k, which is consistent with the measurement (srianand, petitjean & ledoux, 2000). 4 reionization of the universe after the epoch of recombination (last scattering) between ≈ 3.8 × 105− ≈ 2 × 108 yr (z ≈ 1000 − 20), the universe experienced the so–called dark ages, where the dark matter halos collapsed and merged until the appearance of the first sources of light. this ended the dark ages. the ultraviolet light from the first sources of light also changed the physical state of the gas (hydrogen and helium) that fills the universe from a neutral state to a nearly fully ionized one. this was the reionization era where the population iii stars formed, and consequently, the first sne and grbs. this occurred between ≈ (2− 5)× 108 yr (z ≈ 20− 10). soon after population ii stars started to form and probably the second wave of reionization occurred and stopped at ≈ 9 × 108 yr (z ≈ 6) after the big bang, and then the evolution of galaxies started (e.g. djorgovski, 2004, 2005). quasars – the brightest and most distant objects known – offer a window on the reionization era, because neutral hydrogen gas absorbs their ultraviolet light. reionization drastically changes the environment for galaxy formation and evolution and in a hierarchical clustering scenario, the galaxies responsible for reionization may be the seeds of the most massive galaxies in the local universe. reionization is the last global phase transition in the universe. the reionization era is thus a cosmological milestone, marking the appearance of the first stars, galaxies and quasars. recent results obtained by ouchi et al. (2010) give an important contribution for solving such a problem. indeed, from the the lyα luminosity function (lf), clustering measurements, and lyα line profiles based on the largest sample to date of 207 lyα emitters at z = 6.6 on the 1 deg2 sky of subaru/xmm-newton deep survey field, ouchi et al. (2010) found that the combination of various reionization models and observational results about the lf, clustering, and line profile indicates that there would exist a small decrease of the intergalactic medium’s (igm’s) lyα transmission owing to reionization, but that the hydrogen igm is not highly neutral at z = 6.6. their neutral-hydrogen fraction constraint implies that the major reionization process took place at z >∼ 7. the w. m. keck 10-m telescope has shown the quasar sdss j1148+5251 at a redshift of 6.41 (≈ 12.6× 109 yr ago). this is currently the most distant quasar known (djorkovski, 2004). this measurement does not contradict the result found for the epoch of reionization. however, the search of the epoch of reionization is still one of the most important open problems for understanding the formation of the first stars, galaxies and quasars. 5 clusters of galaxies the problems of the production and transport of heavy elements seems to have been resolved. indeed, thermally driven galactic winds, such as from m82, have shown that only active galaxies with an ongoing starburst can enrich the icm with metals. the amounts of metals in the icm is at least as high as the sum of the metals in all galaxies of the cluster (e.g. tozzi et al., 2003). several clusters of galaxies, having strong radio emission, have been associated with egret sources. this is an important step in clarifying the nature of many unknown egret sources (colafrancesco, 2002). however, in the first 11 months of operations of the fermi lat monitoring program of cgs no γ-ray emission from any of the monitored cgs has been detected (ackermann et al., 2010b). in spite of many important results coming from satellites of the last decade, the hierarchical distribution of the dark matter, and the role of the intergalactic magnetic fields in cgs are still open. simultaneous multifrequency measurements with higher sensitivity instruments, in particular those in hard x-ray and radio energy regions and optical-to-near infrared (nir) could solve such problems. 6 dark energy and dark matter by using different methods to determine the mass of galaxies it has been found a discrepancy that suggests ∼ 95% of the universe is in a form that cannot be seen. this form of unknown content of the universe is the sum of dark energy (de) and dark matter (dm). colafrancesco (2003) deeply discussed about new cosmology. the discovery of the nature of the dark energy may provide an invaluable clue for understanding the nature and the dynamics of our universe. however, there is ∼ 30% of the matter content of the universe which is dark and still requires a detailed explanation. baryonic dm consisting of machos (massive astrophysical compact halo objects) can yield only some fraction of the total amount of dark matter required by cmb observations. wimps (weakly interacting massive particles) (non-baryonic dm) can yield the needed cosmological amount of dm and its large scale distribution provided that it is “cold” enough. several options have been proposed so far like: i) light neutrinos with mass in 4 old and new from multifrequency astrophysics the range mν ∼ 10−30 ev, ii) light exotic particles like axions with mass in the range maxion ∼ 10−5−10−2 ev or weakly interacting massive particles like neutralinos with mass in the range mχ ∼ 10− 1000 gev, this last option being favored at present (see, e.g., ellis 2002). eros and macho, two experiments based on the gravitational microlensing, were developed. two lines of sight have been probed intensively: the large (lmc) and the small (smc) magellanic clouds, located 52 kpc and 63 kpc respectively from the sun (palanque-delabrouille, 2003). with 6 years of data towards the lmc, the macho experiment published a most probable halo fraction between 8 and 50% in the form of 0.2 m� objects (alcock et al., 2000). most of this range is excluded by the eros exclusion limit, and in particular the macho preferred value of 20% of the halo. among experiments for searching wimps as dark matter candidates, there is pamela, an experiment devoted to a search for dark matter annihilation, antihelium (primordial antimatter), new matter in the universe (strangelets?), the study of cosmic-ray propagation (light nuclei and isotopes), electron spectrum (local sources?), solar physics and solar modulation, and terrestrial magnetosphere. a comparison of the expected pamela results with many other experiments has been discussed by morselli (2007). bruno (2011) discussed some results from pamela. the search for dm is one of the main open problems of today’s astroparticle physics. 7 the galactic center the galactic center (gc) is one of the most interesting places for testing theories in which frontier physics plays a fundamental role. there is an excellent review of mezger, duschl & zylka (1996), which discusses the physical state of stars and interstellar matter in the galactic bulge (r ∼ 0.3–3 kpc from the dynamic center of the galaxy), in the nuclear bulge (r < 0.3 kpc) and in the sgr a radio and gmc complex (the central∼ 50 pc of the milky way). this review reports also a list of review papers and conference proceedings related to the galactic center with bibliographic details. in the review paper by giovannelli & sabau-graziati (2004, and the references therein) the multifrequency behaviour of the galactic center has been also discussed. larosa et al. (2000) presented a wide-field, high dynamic range, high-resolution, long-wavelength (λ = 90 cm) vla image of the galactic center region. this is the most accurate image of the gc. while highly obscured in optical and soft x-rays; it shows a central compact object (a black hole candidate) with m ∼ 3.6× 106 m� (genzel et al., 2003a), which coincides with the compact radio source sgr a∗ [r.a. 17 45 41.3 (hh mm ss); dec.: -29 00 22 (dd mm ss)]. sgr a∗ in x-rays/infrared is highly variable (genzel et al., 2003b). the gc is also a good candidate for indirect dark matter observations. moreover, the detected excess of he γ-rays at gc would be produced by neutralino annihilation in the dark matter halo. such an excess could be better measured by the fermi observatory. 8 gamma-ray bursts the many theoretical descriptions of gamma-ray bursts (grbs) show that the origin of these sources is still an open and strongly controversial topic. fireball (fb) model (meszaros & rees, 1992; piran, 1999), cannon ball (cb) model (dar & de rújula, 2004), spinninprecessing jet (spj) model (fargion, 2003a,b; fargion & grossi, 2006), fireshell (izzo et al., 2010) model — directly coming from electromagnetic black hole (embh) model (e.g. ruffini et al. 2003 and the references therein) — are the most popular, but each one against the others. important implications on the origin of the highest redshift grbs are coming from the detection of the grb 080913 at z =6.7 (greiner et al., 2009), grb 090423 at z ∼ 8.2 (tanvir et al., 2009), and grb 090429b (cucchiara et al., 2011). this means that really we are approaching to the possibility of detecting grbs at the end of dark era, where the first pop iii stars appeared. izzo et al. (2010) discussed successfully a theoretical interpretation of the grb 090423 within their fireshell model. wang & dai (2009) studied the high-redshift star formation rate (sfr) up to z ' 8.3 considering the swift grbs tracing the star formation history and the cosmic metallicity evolution in different background cosmological models including λcdm, quintessence, quintessence with a time-varying equation of state and brane-world models. λcdm model is the preferred which is however compared with other results. although great progress has been obtained in the last few years, grbs theory needs further investigation in the light of the experimental data coming from old and new satellites, often coordinated, such as bepposax or batse/rxte or asm/rxte or ipn or hete or integral or swift or agile or fermi or maxi. 9 extragalactic background light space is filled with diffuse extragalactic background light (ebl) which is the sum of starlight emitted by galaxies through the history of the universe. high energy γ-rays traversing cosmological distances are expected to be absorbed through their interactions with the ebl by: γvhe + γebl −→ e+ e−. then the γ-ray flux φ is suppressed while travelling from the emission 5 franco giovannelli, lola sabau-graziati point to the detection point, as φ = φ0e−τ(e,z), where τ(e,z) is the opacity. the e–fold reduction [τ(e,z) = 1] is the gamma ray horizon (grh) (e.g. blanch & martinez, 2005; martinez, 2007). the direct measurement of the ebl is difficult at optical to infrared wavelengths because of the strong foreground radiation originating in the solar system. however, the measurement of the ebl is important for vhe gamma-ray astronomy, as well as for astronomers modelling star formation and galaxy evolution. second only in intensity to the cosmic microwave background (cmb), the optical and infrared (ir) ebl contains the imprint of galaxy evolution since the big bang. this includes the light produced during formation and reprocessing of stars. current measurements of the ebl are reported in the paper by schroedter (2005, and references therein). he used the available vhe spectra from six blazars. more recently, the redshift region over which the gamma reaction history (grh) can be constrained by observations has been extended up to z = 0.536. upper ebl limit based on 3c 279 data have been obtained (albert et al., 2008a). the universe is more transparent to vhe gamma rays than expected. thus many more agns could be seen at these energies. indeed, abdo et al. (2009a) observed a number of tev-selected agns during the first 5.5 months of observations with the large area telescope (lat) on–board the fermi gamma-ray space telescope. redshift– dependent evolution is detected in the spectra of objects detected at gev and tev energies. the most reasonable explanation for this is absorption on the ebl, and as such, it would represent the first model–independent evidence for absorption of γ-rays on the ebl. abdo et al. (2010b) by using a sample of γ-ray blazars with redshift up to z ∼ 3, and grbs with redshift up to z ∼ 4.3, measured by fermi/lat placed upper limits on the γ-ray opacity of the universe at various energies and redshifts and compared this with predictions from well–known ebl models. they found that an ebl intensity in the optical-ultraviolet wavelengths as great as predicted by the ”baseline” model of stecker, malkan & scully (2006) that can be ruled out with high confidence. 10 relativistic jets relativistic jets have been found in numerous galactic and extragalactic cosmic sources at different energy bands. the emitted spectra of jets from cosmic sources of different nature are strongly dependent on the angle formed by the beam axis and the line of sight, and obviously by the lorentz factor of the particles (e.g. bednarek et al., 1990 and the references therein; beall, guillory & rose, 1999, 2009; beall, 2002, 2003, 2008, 2009; beall et al., 2006, 2007). so, observations of jet sources at different frequencies can provide new inputs for the comprehension of such extremely efficient carriers of energy, like for the cosmological grbs. the discovered analogy among µ–qsos, qsos, and grbs is fundamental for studying the common physics governing these different classes of objects via µ–qsos, which are galactic, and then apparently brighter and with all processes occurring in time scales accessible by our experiments (e.g. chaty, 1998). chaty (2007) remarked the importance of multifrequency observations of jet sources by means of the measurements of grs 1915+105. dermer et al. (2009) suggest that ultra-high energy cosmic rays (uhecrs) could come from black hole jets of radio galaxies. spectral signatures associated with uhecr hadron acceleration in studies of radio galaxies and blazars with fermi observatory and ground–based γ-ray observatories can provide evidence for cosmic-ray particle acceleration in black hole plasma jets. also in this case, γ-ray multifrequency observations (mev–gev–tev) together with observations of pev neutrinos could confirm whether black-hole jets in radio galaxies accelerate the uhecrs. despite their frequent outburst activity, microquasars have never been unambiguously detected emitting high-energy gamma rays. the fermi/lat has detected a variable high-energy source coinciding with the position of the x-ray binary and microquasar cygnus x-3. its identification with cygnus x-3 is secured by the detection of its orbital period in gamma rays, as well as the correlation of the lat flux with radio emission from the relativistic jets of cygnus x-3. the γ-ray emission probably originates from within the binary system (abdo et al., 2009b). also the microquasar ls 5039 has been unambiguously detected by fermi/lat being its emission modulated with a period of 3.9 days. analyzing the spectrum, variable with the orbital phase, and having a cutoff, abdo et al. (2009c) conclude that the γ-ray emission of ls 5039 is magnetospheric in origin, like that of pulsars detected by fermi. this experimental evidence of emission in the gev region from microquasars opens an interesting window about the formation of relativistic jets. 11 cataclysmic variables the detection of cvs with the integral observatory (barlow et al., 2006) have recently renewed the interest of high energy astrophysicists for such systems, and subsequently involving once more the low–energy astrophysical community. the detection of cvs having orbital periods inside the so-called period gap between 2 and 3 hours, which separates polars (apparently generating gravitational radiation) from intermediate polars (which suffer magnetic braking) renders attractive 6 old and new from multifrequency astrophysics the idea of the physical continuity between these two classes. further investigations are necessary for solving this important problem. for a recent review on cvs see the paper by giovannelli & sabau-graziati (2012c). 12 high mass x-ray binaries for general reviews see e.g. giovannelli & sabaugraziati (2001, 2004) and van den heuvel (2009) and references therein. hmxbs are young systems, with age ≤ 107 yr, mainly located in the galactic plane (e.g., van paradijs, 1998). a compact object — the secondary star —, mostly a magnetized neutron star (x-ray pulsar) is orbiting around an early type star (o, b, be) — the primary — with m ≥ 10 m�. the optical luminosity of the system is dominated by the early type star. such systems are the best laboratory for the study of accreting processes, thanks to their relatively high luminosity in a large part of the electromagnetic spectrum. because of the strong interactions between the optical companion and collapsed object, low and high energy processes are strictly related. in x-ray/be binaries the mass loss processes are due to the rapid rotation of the be star, the stellar wind and, sporadically, to the expulsion of casual quantity of matter essentially triggered by gravitational effects close to the periastron passage of the neutron star. the long orbital period (> 10 days) and a large eccentricity of the orbit (> 0.2) together with transient hard x-ray behavior are the main characteristics of these systems. among the whole sample of galactic systems containing 114 x-ray pulsars (johnstone, 2005), only few of them have been extensively studied. among these, the system a 0535+26/hde 245770 is the best known thanks to concomitant favorable causes, which rendered possible thirty eight years of coordinated multifrequency observations, most of them discussed by e.g. giovannelli & sabau-graziati (1992, 2008), burger et al. (1996). accretion powered x-ray pulsars usually capture material from the optical companion via stellar wind, since this primary star generally does not fill its roche lobe. however, in some specific conditions (e.g. the passage at the periastron of the neutron star) and in particular systems (e.g. a 0535+26/hde 245770), it is possible the formation of a temporary accretion disk around the neutron star behind the shock front of the stellar wind. this enhances the efficiency of the process of mass transfer from the primary star onto the secondary collapsed star, as discussed by giovannelli & ziolkowski (1990) and by giovannelli et al. (2007) in the case of a 0535+26. giovannelli & sabau-graziati (2011) discussed the history of the discovery of optical indicators of high energy emission in the prototype system a0535+26/hde 245770≡ flavia’ star, updated to the march–april 2010 event when a strong optical activity occurred roughly 8 days before the x-ray outburst (caballero et al., 2010) that was predicted by giovannelli, gualandi & sabaugraziati (2010). this event together with others occurred in the past allowed to giovannelli & sabaugraziati (2011) to conclude that x-ray outbursts occur ∼ 8 days after the periastron passage. giovannelli, bisnovatyi-kogan & klepnev (2013) developed a model for explaining such a delay by the time of radial motion of the matter in a non–stationary accretion disk around the neutron star, after an increase of the mass flux in the vicinity of a periastral point in the binary. this time is determined by the turbulent viscosity, with the parameter α = 0.1− 0.3. however how x-ray outbursts are triggered in xray pulsars constitute one important still open problem giving rise to controversy within astrophysicists. important news are coming also from gev observations of hmxbs. indeed, abdo et al. (2009e) present the first results from the observations of lsi + 61◦303 using fermi/lat data obtained between 2008 august and 2009 march. their results indicate variability that is consistent with the binary period, with the emission being modulated at 26.6 days. this constitutes the first detection of orbital periodicity in high–energy γ-rays (20 mev-100 gev). the light curve is characterized by a broad peak after periastron, as well as a smaller peak just before apastron. the spectrum is best represented by a power law with an exponential cutoff, yielding an overall flux above 100 mev of ' 0.82×10−6 ph cm−2 s−1, with a cutoff at ∼ 6.3 gev and photon index γ ∼ 2.21. there is no significant spectral change with orbital phase. the phase of maximum emission, close to periastron, hints at inverse compton scattering as the main radiation mechanism. however, previous very high-energy gamma ray (> 100 gev) obser vations by magic and veritas show peak emission close to apastron. this and the energy cutoff seen with fermi suggest that the link between he and vhe gamma rays is nontrivial. this is one open problem to be solved in future. 12.1 obscured sources and supergiant fast x-ray transients relevant are integral results about a new population of obscured sources and supergiant fast x-ray transients (sfxts) (chaty & filliatre, 2005; chaty, 2007; rahoui et al., 2008; chaty, 2008). the importance of the discovery of this new population is based on the constraints on the formation and evolution of hmxbs: does dominant population of short-living systems – born with two very massive components – oc7 franco giovannelli, lola sabau-graziati cur in rich star-forming region? what will happen when the supergiant star dies? are primary progenitors of ns/ns or ns/bh mergers good candidates of gravitational waves emitters? can we find a link with short/hard γ-ray bursts? 13 ultra–compact double–degenerated binaries ultra-compact, double-degenerated binaries (ucd) consist of two compact stars, which can be black holes, neutron stars or white dwarfs. in the case of two white dwarfs revolving around each other with an orbital period porb ≤ 20 min. the separation of the two components for a ucd with porb ≈ 10 min or shorter is smaller than jupiter’s diameter. these ucd are evolutionary remnants of low–mass binaries, and they are numerous in the milky way. the discovery of ucd is foreboding interesting hints for gravitational–wave possible detection with lisa observatory. 14 magnetars the discovery of magnetars (anomalous x-ray pulsars – axps – and soft gamma-ray repeaters – sgrs) is also one of the most exciting results of the last years (mereghetti & stella, 1995; van paradijs, taam & van den heuvel, 1995; and e.g. review by giovannelli & sabau-graziati, 2004 and the references therein). indeed, with the magnetic field intensity of order 1014 − 1015 g a question naturally arises: what kind of sn produces such axps and sgrs? are really the collapsed objects in axps and sgrs neutron stars? (e.g. hurley, 2008). with such high magnetic field intensity an almost ‘obvious’ consequence can be derived: the correspondent dimension of the source must be of ∼ 10 m (giovannelli & sabau-graziati, 2006). this could be the dimension of the acceleration zone in supercompact stars. could they be quark stars? ghosh (2009) discussed some of the recent developments in the quark star physics along with the consequences of possible hadron to quark phase transition at high density scenario of neutron stars and their implications on the astroparticle physics. important consequences could be derived by considering the continuity among rotation-powered pulsars, magnetars, and millisecond pulsars. such continuity has been experimentally demonstrated (kuiper, 2007). however, the physics underlying that observational continuity is not yet clear. 15 neutrino astronomy for a short discussion about neutrino astronomy, see for instance the paper by giovannelli (2007 and the references therein), as well as all the papers of the session neutrino astronomy, which appeared in the proceedings of the vulcano workshops 2006, 2008, and 2010 (giovannelli & mannocchi, 2007, 2009, 2011). however, it is important to remark that several papers have appeared about: i) the sources of he neutrinos (aharonian, 2007) and diffuse neutrinos in the galaxy (evoli, grasso & maccione, 2007); ii) potential neutrino signals from galactic γ-ray sources (kappes et al., 2007); iii) galactic cosmic-ray pevatrons with multi-tev γ-rays and neutrinos (gabici & aharonian, 2007); iv) results achieved with amanda: 32 galactic and extragalactic sources have been detected (xu & the icecube collaboration, 2008); diffuse neutrino flux from the inner galaxy (taylor et al., 2008); discussion about vhe neutrino astronomic experiments (cao, 2008). important news and references can be found in the proceedings of the les rencontres de physique de la vallée d’aoste (greco, 2009, 2010). news about the neutrino oscillations have been reported by mezzetto (2011). the angle θ13 is different than zero: sin2 θ13 = 0.013. this result opens the door to cp violation searches in the neutrino sector, with profound implications for our understanding of the matter–antimatter asymmetry in the universe. 16 conclusions and reflections it is becoming increasingly clear that the energy régime covered by vhe γ-ray astronomy will be able to address a number of significant scientific questions, which include: i) what parameters determine the cut-off energy for pulsed γ-rays from pulsars? ii) what is the role of shell-type supernovae in the production of cosmic rays? iii) at what energies do agn blazar spectra cut-off? iv) are gamma blazar spectral cut-offs intrinsic to the source or due to intergalactic absorption? v) is the dominant particle species in agn jets leptonic or hadronic? vi) can intergalactic absorption of the vhe emission of agn’s be a tool to calibrate the epoch of galaxy formation, the hubble parameter, and the distance to γ-ray bursts? vii) are there sources of γ-rays which are ‘loud’ at vhes, but ‘quiet’ at other wavelengths? it appears evident the importance of multifrequency astrophysics. there are many problems in performing simultaneous multifrequency, multienergy multisite, multiinstrument, multiplatform measurements due to: i) objective technological difficulties; ii) sharing common scientific objectives; iii) problems of scheduling and budgets; iv) politic management of science. in spite of the many ground-based and space-based experiments providing an impressive quantity of excellent data in different energy regions, many open problems still exist. we believe that only by drastically 8 old and new from multifrequency astrophysics changing the philosophy of the experiments will it be possible to solve most of the present open problems. for instance, in the case of space–based experiments, small satellites, dedicated to specific missions and problems, and having the possibility of scheduling very long time observations, must be supported because of their relative faster preparation, easier management and lower costs with respect to medium and large satellites. we strongly believe that in the next decades “passive” physics experiments in space, as well as groundbased, and perhaps lunar-based observatories will be the most suitable probes in sounding the physics of the universe. probably the active physics experiments have already reached the maximum dimensions compatible with a reasonable cost/benefit ratio, with the obvious exception of the neutrino astronomy experiments. acknowledgement we wish to thank the soc of the karlovy vary 10th integral/bart workshop for inviting us to discuss this review during the workshop, and the loc for logistical support for one of us (fg). this research has made use of nasa’s astrophysics data system. references [1] aad, g. et al. 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(icecube collaboration): 2008, n. phys. b 175-176, 401. 12 http://dx.doi.org/10.1063/1.1587092 http://dx.doi.org/10.1086/431173 http://dx.doi.org/10.1038/35050020 http://dx.doi.org/10.1038/nature08459 http://dx.doi.org/10.1063/1.3076687 http://dx.doi.org/10.1086/376731 introduction astroparticle physics development very high energy sources diffuse extragalactic background radiation reionization of the universe clusters of galaxies dark energy and dark matter the galactic center gamma-ray bursts extragalactic background light relativistic jets cataclysmic variables high mass x-ray binaries obscured sources and supergiant fast x-ray transients ultra–compact double–degenerated binaries magnetars neutrino astronomy conclusions and reflections 161 acta polytechnica ctu proceedings 2(1): 161–164, 2015 161 doi: 10.14311/app.2015.02.0161 study of photometric variability of selected su uma dwarf novae i. voloshina1, v. metlov1 1sternberg astronomical institute, lomonosov moscow state university, moscow, russia corresponding author: vib@sai.msu.ru abstract in this work we present time-resolved photometry of several poorly-studied dwarf novae during recent superoutbursts. observations were made with a ccd, mounted on 50and 60-cm telescopes of the sternberg astronomical institute in crimea in april may and october 2012 and june july 2013. superhumps were detected in light curves of all the dwarf novae. the amplitudes and periods of detected light variations were calculated. superhumps evolution was also followed up for all systems and classification is improved. keywords: cataclysmic variables dwarf novae su uma stars outbursts photometry light curves periods. 1 introduction su uma stars represent one of the three sub-types of dwarf novae. besides the frequent normal outbursts, they could show outbursts of larger amplitudes and much longer duration than the normal ones,superoutbursts. during superoutbursts they exhibit socalled superhumps,an increase of system brightness on the small part of the orbital light curve, that repeats with a period a few percents longer than the orbital one. the amplitudes of superhumps are around 0m.3. the orbital periods of su uma stars are about 80-180 min. there are two small subtypes of dwarf novae inside of this group: wz sge stars with short superhumps period and very long time of outburst recurrence and er uma stars with very short intervals between superoutbursts. it was found from observations that evolution of the superhumps period consists of 3 stages: early evolutionary stage with a longer period of superhumps (stage a), middle stage with systematically varying superhumps period (stage b) and the last stage with a shorter, stable period of superhumps (stage c). all stages are most distinct in wz sge systems. the superhumps, seen during the early stages of wz sge dwarf novae, are double-wave humps and their periods are close to the orbital ones (kato, 2002), the ordinary superhumps are one-wave humps. they have the largest amplitude of periodicity and period slightly longer than the orbital period. according to the tidal-thermal model of osaki (1996) superhumps arise as a result of accretion disk precession triggered by gravitational disturbances from the secondary component. the period of superhumps is beat period between the precession period pprec and orbital period porb. the present paper is aimed at investigating of superhumps phenomenon in selected su uma stars. 2 program stars the stars for our study were chosen from the vsnet list of dwarf novae undergoing superoutbursts during our observational sets. the criteria for our choice were, first of all, the brightness of an object limited by telescope power and relatively rare superoutbursts (and therefore poorly studied). they are: css 121004: 205146-035827 (j2051), v844 her, pnv j19150199+0719471 (j1915), sdss j150240.98+3334239 (j1502). 3 observations the main part of our observations was obtained at the 60-cm telescope with ccd apogee 47 (528 × 512 pxl, pixel size 12×12µm) in v,r and rc bands and partly at the 50-cm telescope with a new ccd apogee alta-8300 (3326×2504 pxl, pixel size 5.4 × 5.4µm) in v band in crimea. the duration of observational sets varied from 3 to 6 h. the accuracy is 2 − 3% for r band, but is less for v band 4−5%. the reference stars were taken mostly from aavso list. if we used the local standard star from the vicinity of a program star special high precision observations with ubv photometer at the 60-cm telescope were conducted during the nights with good weather conditions for the standard calibration. ccd data were reduced using the maxim dl standard package, ubv data with software developed by v. lyuty. 161 http://dx.doi.org/10.14311/app.2015.02.0161 i. voloshina, v. metlov 3.1 v844 her the dwarf nova v844 her underwent a superoutburst in may, 2012 (vsnet-alert 14525). this object showed frequent outbursts during 2009–2011, but was relatively inactive next year. the superoutburst that we followed up occurred 370 days after the last superoutburst of 2011. our first observation of v844 her was conducted on april 22 when this nova was in quiescence (∼ 18m) but restarted later after receiving information about the outburst and lasted practically until the end of the outburst when v844 her returned to its pre-outburst brightness. figure 1 show the evolution of superhumps in v844 her. 6052.40 6052.45 6052.50 6052.55 13.1 12.9 12.7 6053.40 6053.45 6053.50 6053.55 13.2 13.0 12.8 6054.40 6054.45 6054.50 6054.55 13.4 13.2 13.0 jd 2450000+ 04.05.2012 05.05.2012 06.05.2012 v v v figure 1: v844 her light curves obtained at the beginning of the outburst. decreasing of superhumps which is clearly seen on the light curve at the bottom indicates that a new stage is approaching. 3.2 sdss j150240.98+3334239 the discovery of outburst of this dwarf nova was reported by vsnet on april 2, 2012. its optical magnitude ranges from 13m.7 to 19m.6 during quiescent and outburst phases, respectively. usno photometry reveals a deep (2.5 mag) eclipse occurring at a period of 84.24 minutes (szkody et al., 2006) which evidence that it is a high inclination system. our observations of j1502 cover 6 nights from april 23 to june 2, 2012. observational light curves for three of them are presented in figure 2. they show deep eclipses besides superhumps. our analysis was restricted by consideration of superhumps phenomenon in this system. figure 2: light curves of high inclination system j1502 showing both superhumps and eclipses. 3.3 css 121004: 205146-035827 the object was discovered by crts on october 4, 2012. observations provided by dr. maehara on october 8 (vsnet-outburst 14685) demonstrate superhumps with figure 3: stage b superhumps in the light curves of dwarf nova j2051. an amplitude of 0m.2 and with a short period of 0d.056 in the light curves of this object. we started our observations later, on october 10 because of the bad sky conditions before this date. at this moment the brightness of j2051 was 14m.9. the object started to fade rapidly on october 20 with rate 0.37m · d−1 and became too faint for observations on october 22 (∼ 18m). our observations of dwarf nova j2051 in v band are shown in figure 3. 162 study of photometric variability of selected su uma dwarf novae 3.4 pnv j19150199+0719471 on june 1, 2013 e.de miguel (vsnet-outburst 15466) reported discovery of an outburst of this transient with magnitude ∼ 10m.8. the next day he reported about detection of early superhumps in the light curve of this object with a possible period of 0d.0641(2) (probably stage a). on june 9 the double-peaked superhumps with an average amplitude of 0m.1 and psh ∼ 0d.0569, were detected by several observers. spectroscopic observations provided by echevarria et al.(2013) suggested the high inclination and low massive component,brown dwarf. our observations of this nova started on june 4, 2013 and lasted until the middle of july 2013. during our observations the brightness of j1915 dropped from 11m.47 at the beginning to 18m (v) at the end of the superoutburst. the light curves of j1915 obtained at the different moments of 2013 superoutburst as an example are shown in figure 4. 6449.3 6449.4 6449.5 11.8 11.7 11.6 11.5 11.4 r c a 6457.3 6457.4 6457.5 12.5 12.4 12.3 12.2 r c b 6467.3 6467.4 6467.5 13.0 12.9 12.8 12.7 r c c 6482.3 6482.4 6482.5 16.0 15.9 15.8 15.7 r c jd2450000 + figure 4: evolution of superhumps in dwarf nova j1915: a beginning of stage a superhumps; b stage b superhumps; c transition from b to c stage; d post-fading stage superhumps. scale is the same for all panels. 4 results for data analysis and search of periodicities we used a special code period98 (sperl, 1998) and period04 (lenz & breger, 2004). the analysis was firstly done for every observational night and later the mean values for different stages of each star were calculated. for v844 her although stages a-c were observed, the period of stage a superhumps was not determined, due to limited observations during this stage. pdot for stage b was positive, as seen in other superoutbursts of this object. in the light curves of dwarf nova j2051 the stages b and c can be distinguished. the superhumps period variations suggests that the object more resemble ordinary su uma-dwarf novae than wz sge-stars. the numerous observations obtained for j1915 (about 6000 images at all) permitted us to follow up superhumps evolution in detail beginning from the first night of our observations, june 4. no superhumps were detected in the light curve of j1915 on this particular night. subsequent observations provided on the next night, june 5, recorded a periodic variation in the light curve of j1915. we suggest that it could be beginning of the stage a. the superhumps period for different stages was determined. the absence of recorded outburst in the past, large amplitude of present outburst, values of parameters (like ε, pdot and other) and the pattern of superhumps period variation are typical for wz sge-stars. so we conclude that the recently discovered dwarf nova j1915 belongs to the wz sge-subtype. some of the power spectra calculated for each star as an example are shown in figures 5–8. figure 5: one of the v844 her power spectra as an example. figure 6: the power spectrum of j1502, calculated for all 6 nights of our observations. 163 i. voloshina, v. metlov figure 7: the power spectrum of j2051. figure 8: the power spectrum of j1915. the periods which were determined in frame of this study are collected in table 1. the orbital periods were taken from the literature. table 1: determined periods. object psh(stage b) psh(stage c) porb v844 her 0.05590 ± 2 0.05587 ± 3 0.054643 j2051 0.05715 ± 5 0.05680 ± 6 — j1502 0.05891 ± 2 — 0.06944 j1915 0.05833 ± 2 0.05800 ± 3∗ 0.06164 * for j1915 the period in the second column represent the post-fading superhumps period. 5 summary the main results of our study of su uma dwarf nova photometric variability can be summarized as follows: • the time-resolved photometry in v and r bands was obtained for several su uma-type dwarf novae whose superoutbursts were observed during the 2012–2013 season: – for v844 her 10 nights, ∼ 1400 images in v and rc bands; – for css 120004: 205146-03582 8 nights, ∼ 1000 images in v and r bands; – for pnvj19150199+0719471 13 nights, about 6000 images both in v and rc bands; – for sdss j150240.98+3334239 6 nights, ∼ 750 images in v band. • the individual light curves of all program stars were constructed on the base of these numerous observations. superhumps were detected in the light curves all of them and their evolution during the outbursts was followed up. • the superhumps periods and amplitudes were determined from our data and mean superhumps periods were obtained for each nova (see table 1). • the amplitude of outburst, phase-averaged profile of superhumps and superhumps period variations for css 121004: 205146-035827 suggest that this object more resemble ordinary su uma-stars than wz sge-dwarf nova. • on the base of its outburst properties, the recently discovered nv j19150199+0719471 was classified as a dwarf nova of wz sge subtype. the obtained results are preliminary and reflect the work in progress. they may be slightly improved by using more sophisticated methods and thorough subsequent analysis. acknowledgement i. voloshina gratefully acknowledges professor f. giovannelli for the invitation to take part in this conference as well as his kind hospitality in palermo. the authors thank a. bykov for helping with observations in crimea in 2012. this work was supported in part by the program of state support of russian federation leading scientific schools through grant 2374.2012.2. references [1] lenz, p., breger, m.: 2005, coast 146, 53l. [2] sperl, m.: 1998, coast 111, 1. [3] szkody, p., et al.: 2006, astron. j. 131, 973. doi:10.1086/499308 [4] osaki, y.: 1996, pasp 108, 39. doi:10.1086/133689 [5] . kato, t., et al.: 2012, pasj 64, 21. [6] kato et al.: 2013, pasj 65, 23. (survey iv) 164 http://dx.doi.org/10.1086/499308 http://dx.doi.org/10.1086/133689 introduction program stars observations v844 her sdss j150240.98+3334239 css 121004: 205146-035827 pnv j19150199+0719471 results summary acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0008 acta polytechnica ctu proceedings 4:8–12, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app post critical heat transfer and fuel cladding oxidation vojtěch caha∗, jakub krejčí department of nuclear reactors, faculty of nuclear sciences and physical engineering, czech technical university in prague, czech republic ∗ corresponding author: vojtech.caha@fjfi.cvut.cz abstract. the knowledge of heat transfer coefficient in the post critical heat flux region in nuclear reactor safety is very important. although the nuclear reactors normally operate at conditions where critical heat flux (chf) is not reached, accidents where dryout occur are possible. most serious postulated accidents are a loss of coolant accident or reactivity initiated accident which can lead to chf or post chf conditions and possible disruption of core integrity. moreover, this is also influenced by an oxide layer on the cladding surface. the paper deals with the study of mathematical models and correlations used for heat transfer calculation, especially in post dryout region, and fuel cladding oxidation kinetics of currently operated nuclear reactors. the study is focused on increasing of accuracy and reliability of safety limit calculations (e.g. dnbr or fuel cladding temperature). the paper presents coupled code which was developed for the solution of forced convection flow in heated channel and oxidation of fuel cladding. the code is capable of calculating temperature distribution in the coolant, cladding and fuel and also the thickness of an oxide layer. keywords: heat transfer, post dryout, cladding oxidation, isolated channel. 1. introduction the post critical heat flux heat transfer is encountered when the surface temperature becomes too high to maintain a continuous liquid contact, and the surface becomes covered by a continuous vapour blanket. it results in coverage of the heated surface by a continuous vapour film in the case of film boiling regime, or an intermittent vapour film in the case of transition boiling regime. the boundary between these post dryout heat transfer boiling regimes is the minimum of film boiling temperature, or leidenfrost temperature. the typical boiling curve is depicted in figure 1. post dryout heat transfer is initiated as soon as the critical heat flux condition is reached and it remains until rewetting or quenching of the surface takes place. the post critical heat flux heat transfer regimes in boiling flow can be divided as: (1.) transition boiling regime, (2.) flow film boiling regime, (a) inverted annular film boiling, (b) slug flow film boiling, (c) dispersed flow film boiling. the transition boiling is a combination of unstable film boiling and unstable nucleate boiling consecutively existing at a given location on a heating surface. whereas, film boiling is generally defined as a boiling where only the vapour phase is in contact with the heated surface. inverted annular film boiling is characterized by a vapour layer separating the continuous liquid core from the heated surface and usually encountered at void fractions below 40 %. while dispersed flow film boiling is characterized by the existence of figure 1. typical boiling curve [1]. discrete liquid drops entrained in a continuous vapour flow; normally encountered at void fractions above 80 %. the transition between these two cases is the slug flow film boiling. the existence of film boiling depends on flow conditions and surface temperature. the main parameters influenced heat transfer in post dryout region are pressure, equilibrium quality and mass flux. severe non-equilibrium conditions between liquid and vapour phase can occur and must be taken into account in calculation during low coolant mass flux. it is important to point out that post dryout transition behaviour is reliant on independent boundary condition. if heat flux is the independent boundary condition, the transition boiling regime does not occur. in contrary, when wall temperature is an independent variable, each post dryout flow regime can succeed. as a consequence, the nucleate boiling regime is immediately followed by film boiling regime in the nuclear reactor core [1]. 8 http://dx.doi.org/10.14311/ap.2016.4.0008 http://ojs.cvut.cz/ojs/index.php/app vol. 4/2016 post critical heat transfer and fuel cladding oxidation 2. basic equations first, the main objective of the project was to develop a program for the thermo-hydraulic calculation of nuclear reactor core or experimental electrically heated tubes and rod bundles cooled by light water. the temperature profile of the fuel cladding and fuel with the influence of oxide layer was also included. eventually, the program was used for a comparative assessment of different heat transfer coefficient correlations in the post dryout region and also for evaluation of fuel cladding oxidation correlations. as a conservative approach for the solution of this calculation is used a method of isolated channel model. the calculation can be conducted for stationary states as well as for transients (pseudo-stationary model). it is possible to input nonuniform power distribution and also local resistance (spacer and mixing grids). the program considers homogeneous equilibrium model (hem) which respects thermodynamic imbalance between phases. the calculation can be run at constant pressure or with respect to pressure drops. there are included pressure drops caused by friction, spacer and mixing grids, change of elevation and change of coolant density. pressure drops related to friction between coolant and wall are determined by fiolenko correlation [2]. the wall temperature correction is set by protopov correlation [2] and two phase region correction is calculated by armand’s model [2]. the calculation is based on the solution of equation h = ∫ l 0 q(z) dz. (1) the thermo-physical properties of light water are evaluated by a library using iapws-if97 definition. the program also contains equations and correlations for real quality, slip ratio, void fraction etc. during the development, the code was aimed to a simplicity of input data entering and an ability of easy addition of new models and correlations. 3. heat transfer the fuel cladding surface temperature is very important parameter in operation and safety of nuclear reactors. that is influenced by a local boiling regime and by a suitable correlation for heat transfer from wall to the coolant. in the subcooled liquid region the calculation of nusselt number is conducted by dittus-boelter equation [2] nu = 0.023re0.8pr0.4. (2) whereas nucleate boiling occurs when wall temperature exceeds coolant saturation temperature by jenslottes difference [2] ∆tjl = 0.791 exp ( − p 6.201× 106 ) q0.25. (3) the beginning of bulk boiling is defined by saturation temperature of coolant and then thom correlation is used [2] tw = tsat + 22.52 √ q exp ( p 8.6875 ) . (4) the wall temperature in the transitional region is linearly approximated. the post critical heat flux heat transfer correlation is used immediately after dnbr decreases below one. the user can choose pg-t [3] or bezrukov [2] critical heat flux correlation. eventually, if equilibrium quality is greater or equal one, convection to superheated steam region is set – sieder-tate correlation nu = 0.021re0.8pr0.4 ( pr prw )0.25 . (5) 3.1. post critical heat flux heat transfer due to a large number of post critical heat flux heat transfer correlations, it was necessary to carefully select suitable one for use in pressurized light water reactors. the main criterion for selection was validity range of correlation. finally, it was chosen seven correlations for the post critical heat flux heat transfer. a list of chosen post chf heat transfer correlations and their validity ranges are shown in table 1. it is obvious that all correlations are valid in wide ranges and covered most of operational and emergency states of pwr. most of them consider thermo-dynamic equilibrium between the phases, i.e. it assumes that the temperature of vapour phase is equal to the temperature of saturation. in general, these correlations have similar form to dittus-boelter correlation. correlations which respects thermo-dynamic imbalance between the phases, consider superheated steam which coexists with liquid drops. the difference between them is the heat flux calculation using wall temperature and superheated steam temperature. the typical correlation which consider thermo-dynamic imbalance is groeneveld-delorme correlation. correlation p g x [mpa] [kg m−2 s−1] [–] bishop 4.08–21.9 700–3140 0.07–1 groeneveld 5.7 0,07–21,5 130–4000 −0,12–3,09 groeneveld 5.9 3,4–21,5 700–5300 0,1–0,9 miropolskiy 3,9–21,6 800–4550 0,06–1 groe.-delorme 0,7–21,5 130–5200 −0,12–3,09 condie-beng. 0,42–21,5 16,5–5234 −0,2–1,73 pdo tables 0,1–20,0 0–7000 −0,2–2,0 table 1. validity range of used post chf correlations. the first correlation considering thermo-dynamic equilibrium is bishop correlation (6), [1]. the calculation of heat transfer coefficient is applied to the temperature of vapour blanket on the heated surface which can be obtained as the average of wall and 9 vojtěch caha, jakub krejčí acta polytechnica ctu proceedings saturation temperature. this correlation is used for example in vipre or fraptran codes. nu = 0.0193re0.8 vf pr1.23 vf ( %v %l )0.068( x+ %v %l (1− x) )−0.68 (6) the next usually used equation is groeneveld correlation (7), [4]. the user can find to versions (5.7 and 5.9) in the program. the versions differ in coefficients and validity ranges. this correlation is used in cobra-flx and fraptran codes. the temperature of vapour and liquid are related to the saturation temperature. nu = c1 ( gxdh αλv )aprbw( 1− 0.1 (( %l %v − 1 ) (1− x) )0.4 )−c (7) the program also contains miropolskiy correlation (8), [5]. it is also correlation which respects thermodynamic equilibrium between the phases. but it is valid only for 0.23 ≤ q ≤ 1.16mw/m2 and 8 ≤ dh ≤ 24 mm. nu = 0.023 ( gdh λv )0.8pr0.8 w ( x+ %v %l (1− x) )0.8( 1− 0.1 (( %l %v − 1 ) (1− x) )0.4 )−1 (8) groeneveld-delorme correlation (9), [6] is a typical example of correlation which considers thermodynamic imbalance. it is used for example in fraptran code. nu = 0.008348pr0.6112 vf( gdh µvf ( xa + %v %l (1− xa) ))−0.8774 (9) the last correlation which was used in the program is condie-bengston correlation (10), [6]. it is an empiric correlation that respects thermo-dynamic equilibrium between the phases. α′ = 5.345× 10−5pr2.2598 w re(0.6249+0.2043 ln(x+1)) v (103λv)−0.4593d0.8095 h (x+ 1)2.0514 . (10) moreover, groeneveld’s look-up post dryout tables [7] are included in the program. its advantage is in the wide range of validity due to the large experimental database which is used and simply searching of heat transfer according to pressure, mass flux equilibrium quality and wall and saturation temperature difference. besides, basic table model includes corrections for hydraulic diameter, cold wall, narrow gap or local resistances. these tables are used for example in assert-pv code. 4. temperature profile and cladding oxidation the module solving fuel temperature profile and cladding oxidation is also included. first, the coolant and wall temperature calculation is performed. an increase of cladding oxide layer and its influence on cladding temperature calculation is followed. then, a conduction in the cladding is solved. heat transfer in fuel-cladding gap calculation is the next step. finally, the temperature profile in fuel is found. all used models consider a cylindrical geometry. the temperature increase caused by lower thermal conductivity of zro2 compared to cladding depends on oxide thickness and its thermal conductivity (function of temperature) ∆tox = qdox λox . (11) the growth of the oxide layer greatly depends on the temperature, cladding material and chemical composition of coolant. the current version of the program contains correlation for low temperature oxidation [8] from matpro library, but is prepared for addition another formulae ∆dox = 0.175 exp ( − 14080 t ) t. (12) heat conduction in the cladding is provided with standard equation of fourier’s law in cylindrical geometry. the calculation of the heat transfer coefficient in fuel-cladding gap is the most complicated part in the temperature profile determination. state of gap depends on many parameters. the program solves it as a sum of three parts – heat conduction in gas, in fuel-cladding contact and thermal radiation. all parts contain several models and many constants. a detailed description can be found in [9]. the fourier’s law is used also for calculation of temperature profile in the fuel [9]. the heat source is considered radially uniform. thermal conductivity in fuel respects dependency on temperature, porosity, burnup, cracking, composition etc. 5. post chf experiments there were carried out a whole range of experiments in post dryout region in tubes as well as in rod bundles which most of them are unavailable due to their commercial utilization. available experiments were carried out at different input parameters (pressure, mass flux, power) and geometries. a comprehensive research was done in [1]. a comparative analysis of post dryout heat transfer coefficient correlations described in section 3.1 were performed. owing to wide range of experimental parameters were chosen experiments measured at the royal institute of technology in stockholm [3]. in these experiments which were carried out over 500 were gained more than 15000 points in post chf region. the experimental equipment was connected to light water loop and was in the shape of a vertical round tube that was electrically heated. there were 10 vol. 4/2016 post critical heat transfer and fuel cladding oxidation also placed 49 thermocouples on the outer wall at different elevation. the axial power distribution was uniform. ranges of experimental parameters are given in table 2. heated length [m] 7.0 inner diameter [m] 0.0100, 0.0149, 0.0247 inlet coolant subc. [◦c] 5 ± 1, 10 ± 3 pressure [mpa] 3, 5, 7, 10, 12, 14, 16, 18, 20 mass flux [kg m−2 s−1] 500, 1000, 1500, 2000, 2500, 3000 heat flux [mw m−2] 0.10–1.25 quality (pdo) [-] 0.03–1.60 table 2. range of experimental parameters and geometry. 6. post chf experiments results the comparison of all described post chf heat transfer coefficient correlation was performed on the group of 120 experiments which were chosen carefully to satisfy validity ranges of all correlations (table 1). the calculation found wall temperatures which were compared with experimentally obtained values in the post chf region. an example of one experiment results is given in figure 2. the figure shows a dependence of wall temperature on the axial length. immediately after chf conditions are reached the rapid increase in wall temperature is observed. then, the wall temperatures differ due to used correlation. figure 2. dependence of calculated and experimental wall temperature on axial length. another capability of developed program is shown in figure 3. the graphical module is able to draw any important calculated parameter in time (transient calculations) and also temperature profiles of coolant, cladding and fuel in each time step. the best results were obtained with groeneveld’s look-up pdo tables. statistical evaluation is given in table 3 where ∆i = tw,calc,i − tw,exp,i tw,exp,i , (13) figure 3. coolant, cladding and fuel temperature profile. ∆̄ = 1 n n∑ i=1 ∆i, (14) σ̄ = √√√√ 1 n − 1 n∑ i=1 (∆i − ∆̄)2. (15) correlation ∆̄ [%] σ̄ [%] bishop 2.22 8.69 groeneveld 5.7 0.19 8.3 groeneveld 5.9 −4.93 7.37 miropolskiy 12.58 22.37 groe.-delorme 92.01 12.08 condie-beng. 13.73 13.69 pdo tables 2.82 5.67 table 3. statistical evaluation of post chf correlations. figure 4 shows a comparison of experimental and calculated wall temperatures achieved with groeneveld’s look-up pdo tables. figure 4. groeneveld’s look-up pdo tables results. 11 vojtěch caha, jakub krejčí acta polytechnica ctu proceedings 7. conclusion a thermo-hydraulic program based on isolated channel model was developed. it includes the wide range of heat transfer correlations for different one phase and two phase flow regimes. great attention was paid to the post chf boiling regime. the program also includes the module for evaluation of temperature profile in fuel and cladding which contains influence of oxide layer. the program is prepared for the addition of new oxidation model correlations which are being developed for different cladding tubes materials and temperature ranges. all calculated results can be shown in 3d graphs created by post-processing module using python mayavi library. a comparative analysis of different heat transfer correlations in the post chf region was done. the analysis included a comparison of seven post chf heat transfer correlations with experimental data which were obtained on electrically heated tube. the best results were achieved with groeneveld’s look-up pdo tables. the continue of this work should aim to verify this results on different experimental data set with axially nonuniform power distribution, on transient experiment with the return from post chf region and on rod bundle experiment. list of symbols g mass flux [kg/m2s] h enthalpy [k/kg] l length [m] q heat flux [w/m2] q linear power [w/m] nu nusselt number [–] p pressure [pa] pr prandtl number [–] re reynolds number [–] t time [s] t temperature [k] x quality [–] α void fraction [–] λ heat transfer coefficient [w/m2k] µ dynamic viscosity [pa s] % density [kg/m3] acknowledgements this work was supported by the grant agency of the czech technical university in prague, grant no. sgs14/156/ohk4/2t/14. references [1] thermohydraulic relationships for advanced water cooled reactors. tech. rep. iaea-tecdoc-1203, international atomic energy agency, 2001. http://www.iaea.org/inis/collection/ nclcollectionstore/_public/32/024/32024154.pdf. [2] n. e. todreas, m. kazimi. nuclear systems volume i: thermal hydraulic fundamentals. crc press, 1989. [3] k. m. becker, c. h. ling, s. hedberg, g. strand. an experimental investigation of post dryout heat transfer. tech. rep. kth-nel-33, royal institute of technology, stockholm, sweden, 1983. http://www.iaea.org/inis/collection/ nclcollectionstore/_public/15/049/15049472.pdf. [4] d. c. groeneveld. post-dryout heat transfer at reactor operating conditions. in national topical meeting on water reactor safety. 1973. http://www.iaea.org/inis/collection/ nclcollectionstore/_public/04/089/4089010.pdf. [5] n. hammouda. subcooled film boiling in non-aqueous fluids. ph.d. thesis, university of ottawa, 1996. http://hdl.handle.net/10393/9949. [6] s. k. moon, s. y. chun, s. cho, et al. an experimental study on post-chf heat transfer for low flow of water in a 3x3 rod bundle. nuclear engineering and technology 37(5):457–468, 2005. [7] d. c. groeneveld. look-up table for fully developed film-boiling heat-transfer coefficients for light water. university of ottawa, 2001. [8] j. krejčí, v. vrtílková, d. gajdoš, d. rada. proposal of new oxidation kinetics for sponge base e110 cladding tubes material. in topfuel2015 – conference proceedings, pp. 466–473. 2015. http://www.euronuclear.org/ events/topfuel/topfuel2015/transactions/ topfuel2015-transactions-poster.pdf. [9] j. krejčí, v. caha. ube-postchf. tech. rep., čvut, praha, 2015. 12 http://www.iaea.org/inis/collection/nclcollectionstore/_public/32/024/32024154.pdf http://www.iaea.org/inis/collection/nclcollectionstore/_public/32/024/32024154.pdf http://www.iaea.org/inis/collection/nclcollectionstore/_public/15/049/15049472.pdf http://www.iaea.org/inis/collection/nclcollectionstore/_public/15/049/15049472.pdf http://www.iaea.org/inis/collection/nclcollectionstore/_public/04/089/4089010.pdf http://www.iaea.org/inis/collection/nclcollectionstore/_public/04/089/4089010.pdf http://hdl.handle.net/10393/9949 http://www.euronuclear.org/events/topfuel/topfuel2015/transactions/topfuel2015-transactions-poster.pdf http://www.euronuclear.org/events/topfuel/topfuel2015/transactions/topfuel2015-transactions-poster.pdf http://www.euronuclear.org/events/topfuel/topfuel2015/transactions/topfuel2015-transactions-poster.pdf acta polytechnica ctu proceedings 4:8–12, 2016 1 introduction 2 basic equations 3 heat transfer 3.1 post critical heat flux heat transfer 4 temperature profile and cladding oxidation 5 post chf experiments 6 post chf experiments results 7 conclusion list of symbols acknowledgements references 246 acta polytechnica ctu proceedings 1(1): 246–250, 2014 246 doi: 10.14311/app.2014.01.0246 the x-ray binary ks 1731–260: possible analogy with her x-1 vojtěch šimon1,2 1astronomical institute, academy of sciences of the czech republic, 25165 ondřejov, czech republic 2czech technical university in prague, fel, prague, czech republic corresponding author: simon@asu.cas.cz abstract the x-ray binary with the neutron star (ns), ks 1731–260, displays superorbital cycle similar to that in her x-1. the accretion disk had the memory of the cycle-length even when this modulation sometimes disappeared in the main outburst of ks 1731–260, and during anomalous low state in her x-1. the disk still existed during such seasons. although irradiation of the disk by x-rays is a viable explanation for the disk precession and warping (see model of foulkes et al.), the mechanisms which give rise to the observed x-ray modulation are quite different for each of these systems. variable absorption can explain this cycle only in her x-1. we propose a variable mass accretion rate onto the ns in ks 1731–260 due to a highly variable impact of the inflowing mass stream with the changing phase of the cycle. keywords: radiation mechanisms accretion, accretion disks x-rays: binaries optical x-rays. 1 introduction ks 1731–260 (e.g. [2, 32]) and her x-1 (e.g. [10]) are mass exchanging x-ray binary systems, with the neutron star (ns) accreting matter from a low (or medium)-mass companion. they can be considered specific type of transient systems as regards their activity (on/off transients in the notation of [13] (rapid rise, very long (years) lasting state of activity, rapid return to the inactive state)). their active x-ray states were accompanied by intense brightenings by more than a magnitude in the optical [12] and near infrared bands [21, 32]. both these systems display cyclic modulation of xray intensity during the active state (her x-1: the cyclelength pc ≈ 35 d [28], ks 1731–260 pc ≈ 38 d [22]). this modulation is superorbital (about 20 times longer than the orbital period porb) in her x-1 because its porb is only 1.7 d [28]. since the observations of ks 1731– 260 in quiescence showed that the donor is of type g5v (with a contribution of a synchrotron jet) [32], it is possible that the cycle is superorbital, too, if this star fills its roche lobe. 2 observations the data from asm/rxte [15] (one-day means) were used. they contain the intensities isum (1.5–12 kev) and ia (1.5–3 kev), ib (3–5 kev), ic (5–12 kev). the hardness ratios are hr1 = ib/ia and hr2 = ic/ib. the optical data of her x-1 come from the aavso international database (massachusetts, usa) [11]. 3 active state in ks 1731–260 in ks 1731–260, the x-ray active state with a complicated evolution lasted for about 12.5 years [4]. after return to quiescence, the luminosity is very similar to that of the other quiescent ns systems [31]. the end of the active state was accompanied by a decrease of brightness by about 1.7 mag(h) in the infrared [21, 32]. asm/rxte monitored part of the active state. it consisted of two segments of a largely different activity. in the scenario of [24] using the model of [6], the whole disk was thermally stable in the hot (ionized) state during the main outburst. the rapid end of the main outburst was followed by a series of the echo outbursts, ascribed to a thermally unstable disk with a series of recurrently propagating cooling and heating fronts. the x-ray light curve observed by asm/rxte is shown in fig. 1a. moving averages (ma) of isum with the filter half-width q = 5 d enhance the visibility of the modulation on a timescale of days. to determine the long-term evolution of isum averaged over these fluctuations, the data were fitted with the code hec13. it was written by prof. p. harmanec using the method of [30]. the changes of isum are not accompanied by the variation of hr1 in the sense expected if absorption is the cause of the modulation (using the coefficients of [18]) (fig. 1b). the same is true for hr2. search for the cycle-length in ma from fig. 1a was carried out with the weighted wavelet z-transform (wwz) developed by [7]. this method enables one to determine the period and amplitude of unevenly sam246 http://dx.doi.org/10.14311/app.2014.01.0246 the x-ray binary ks 1731–260: possible analogy with her x-1 pled time series. wwz indicates whether or not there is a periodic fluctuation at a given time at a given frequency f (fig. 2a). a similar result was obtained for the one-day means of isum. it emerges that neither the period of the modulation, pc, nor its amplitude are stable. pc is not conclusively detected in some segments. this is caused by a real, abrupt change of the light curve. figure 1: (a) x-ray light curve of ks 1731–260 during the main outburst. ma of isum (q = 5 d) enhance the visibility of the modulation. the smooth curve shows the main trend (the hec13 fit). the time interval around the conjunction with the sun is marked. (b) time variation of hr1. the smooth line represents ma for q = 8 d. the errors of ma are the standard errors. the big error bar and arrow in panel b mark the influence of absorption. three prominent extrema of isum and their hr1 are marked. see sect. 3 for details. adapted from [25]. fig. 2b shows the best pc, determined from f that has the biggest value of wwz at a given time (only the segments in which the amplitude is larger than 50 percent of its peak value). see [25] for details. the recurrence time tc of the echo outbursts is about 51 days [24], which is quite different from pc in the main outburst (see also [22]). absorption of x-rays would influence mostly ia. however, the variations of soft x-ray intensity during the cycle suggest intrinsic changes of emission at unchanged absorption (fig. 1b). the echo outbursts after the main outbursts in some transients are helpful in investigating the nature of the above-mentioned cycle in ks 1731–260. the recurrence time tc of the echo outbursts is significantly longer for the systems with longer porb [24]. in this regard, we present arguments in favor of the superorbital nature of the cycle in the main outburst of ks 1731–260. if pc of 38 d were close to porb, the expected tc of the echo outbursts would be at least 800 days, much longer than observed. figure 2: (a) wwz-transform of the moving averages of ks 1731–260 from fig. 1a. (b) the best cycle-length. see sect. 3 for details. adapted from [25]. 4 activity in her x-1 the x-ray light curve of her x-1 displays only two segments (discrete spikes) of the on state (main-on and short-on) during the 35 d cycle (e.g. [28, 14]). on and off-states do not form a clear profile of the long-term light curve in the asm/rxte data; only two anomalous low states als1 and als2 in which isum was below the detection limit can be resolved. instead of the light curve, the activity was therefore studied using the fluence of each main-on spike (fig. 3a). this fluence was determined by an integration of isum over the profile of the main-on state. the scatter of fluences of the individual spikes is real. their time evolution is emphasized by the hec13 fits. they reveal a cycle of about 400 d. evolution the 35 d cycle, measured by the turn-on times of the main-on state, is correlated with that of the spin period of the ns. this suggests the evolution of the transfer of angular momentum from the disk to the ns [27]. the 35 d cycle-length is always unstable, but the largest changes coincide with als. als thus represents an episode of the largest change of the mass flow through the disk onto the ns. the disk remembers the conditions for the 35 d cycle-length and its phase 247 vojtěch šimon (mainly after als2). figure 3: (a) time evolution of fluence of main-on states (1.5–12 kev) in her x-1. each episode of this state represents a point in the curve. the smooth lines represent the fits to the time evolution. (b) smoothed evolution of the optical orbital modulation of her x-1 with time. see sect. 4 for details. the profile of the unique optical emission plays an important role in distinguishing between the character of the active and inactive states in her x-1. dominant part of the optical emission in the active state is due to reprocessing off x-rays from the close vicinity of the ns on the part of the photosphere of the donor facing the ns (e.g. [10]). occasional inactive states in which the orbital modulation remained flat and the optical emission faint occurred only before the x-ray astronomy era (e.g. [12]). they were caused by temporary decreases of this irradiation. a heavy smoothing of the aavso optical data enabled to study the time evolution of the orbital modulation, hence of the x-ray irradiation of the donor (fig. 3b). this revealed a relation between the optical and x-ray long-term activity. in spite of a decrease of the optical brightness accompanying the fall of x-ray flux in als1, the x-ray irradiation remained. this implies that accretion continued even during als1. this event was therefore not a real low state like those in the pre-x-ray astronomy era. a similar situation was the als in 1983 when the optical modulation of her x-1 remained comparable to that in the active state [5]. however, the observations by the astron satellite revealed very large differences between the x-ray spectra obtained in this als and after recovery from this low state (1984) [26]. intense cyclotron emission of the ns dominated during normal main-on state of the 35 d cycle (aug 25, 1984). on the contrary, the x-ray spectrum obtained in als in the phase when main-on state was expected (june 30, 1983) showed a combination of a faint cyclotron emission of the ns and reflection of the donor. both the orbital modulation in the optical band and the reflection of the donor in the x-ray band confirmed that the mass accretion continued during als. als1 in fig. 3a appears to be extreme in the sense that both the change of the 35 d cycle of the disk and the increase of the spin period of the ns had the largest amplitude among the episodes of als [27]. the decrease of the optical brightness in als1 (fig. 3b) then suggests that these changes of the disk were also accompanied by a decrease of the x-ray irradiation of the donor. 5 conclusions the modulation of x-ray emission in ks 1731–260 was first attributed to the precession of the accretion disk by [22]. its pc ≈ 38 d in the main outburst is quite different from tc ≈ 51 d of the echo outbursts. the series of the echo outbursts in ks 1731–260 [24] can be used as an independent method for determining its porb to be about 0.5 − 1 d [24]. since the length of porb is by more than an order of magnitude shorter than pc, ks 1731–260 became a new member of the family of x-ray binary systems with superorbital cycles. the superorbital cycle of ks 1731–260 cannot be caused by transitions of the disk between the hot and the cool state because it occurred only during the phase of the hot (ionized) state of the disk (see also [25]). the disk had the memory of the cycle as regards the length of pc in ks 1731–260 even when this modulation sometimes disappeared in the main outburst, and in her x-1 during als. nevertheless, the disk still existed even during these phases, which is suggested by the intense x-ray emission in ks 1731–260 and the reprocessing off x-rays in the optical band in her x-1. intense irradiation of the disk by x-rays is a viable explanation for the disk precession and warping (see models of [8, 9]). indeed, ks 1731–260 and her x-1 are strong emitters (lx ≈ 1.8 × 1037 erg s−1 in the main outburst of ks 1731–260 [20], lx ≈ 2× 1037 erg s−1 in the main-on state of her x-1 [17]). this is about 0.1 of the eddington luminosity. however, it is necessary to find how this precession gives rise to the modulation of the observed x-ray intensity. in her x-1, absorption causes x-ray variations during the cycle [23]. however, 248 the x-ray binary ks 1731–260: possible analogy with her x-1 this explanation is not applicable to ks 1731–260. we propose an alternative explanation for the modulation in ks 1731–260. the models of [8, 9] show that the stream of matter inflowing from the donor reaches quite different impact regions of the tilted and warped disk during the cycle. this impact can occur deep in the inner disk region in some phases. this therefore affects the mass flow in the inner disk during the individual phases. in this scenario, the true cycle-length can be twice as long if the profile is double-wave. the almost constant hr1 and hr2 during the cycle can be explained if the spectral components [4] and their intensities vary with a variable mass accretion rate onto the ns. the number of mechanisms for the modulation during superorbital cycle therefore increases in this family of systems. in ks 1731–260, the atoll shifts on a timescale of less than a day [3] are superimposed on the superorbital cycle. according to [1], atoll type shifts are caused by variations of the mass accretion rate onto the ns. this suggests that the accretion is due to the contributions of various simultaneous flows of matter. magnetic flux density b of the ns is important for the emission mechanism in the x-ray band. is there any relation between this mechanism and the superorbital cycle? her x-1 contains a pulsar with the spin period of 1.24 s (0.806 hz) [28] and b ≈ 5 × 1012 gauss [29]. it produces cyclotron emission (e.g. [16]). on the other hand, ks 1731–260 is a millisecond pulsar with the spin period of 524 khz [19]. in the main outburst, its emission is a combination of an optically thick comptonization component and a blackbody component [20]. this suggests b of the ns much smaller than in her x-1. all this implies that the superorbital cycle can operate even for such largely different mechanisms of x-ray emission, hence for the largely different b and the accretion flows near the ns. acknowledgement this research has made use of the observations provided by the asm/rxte team. i used the aavso international database (massachusetts, usa). this study was supported by the grants 102/09/0997 and 13-33324s provided by the grant agency of the czech republic. i made use of the code developed by dr. g. foster and available at http://www.aavso.org/data/software/wwz.shtml. i thank prof. petr harmanec for providing me with the code hec13. the fortran source version, compiled version and brief instructions how to use the program can be obtained via http:// astro.troja.mff.cuni.cz/ftp/hec/hec13/. references [1] bloser, p.f., et al.: 2000, apj, 542, 1000 doi:10.1086/317019 [2] barret, d., et al.: 1998, a&a, 329, 965 [3] barret, d., et al.: 2000, apj, 533, 329 doi:10.1086/308651 [4] chelovekov, i. v., et al.: 2006, astl, 32, 166 [5] delgado, a. j., et al.: 1983, a&a, 127, l15 [6] dubus, g., et al.: 2001, a&a, 373, 251 [7] foster, g.: 1996, aj, 112, 1709 [8] foulkes, s.b. et al.: 2006, mnras, 366, 1399 doi:10.1111/j.1365-2966.2005.09910.x [9] foulkes, s.b., et al.: 2010, mnras, 401, 1275 doi:10.1111/j.1365-2966.2009.15721.x [10] gerend, d., boynton, p. e.: 1976, apj, 209, 562 [11] henden, a.: 2011, aavso database [12] hudec, r., wenzel, w.: 1976, baicz, 27, 325 [13] king, a.r.: 2006, in compact stellar x-ray sources, cambridge univ. press [14] leahy, d. a.: 2002, mnras, 334, 847 doi:10.1046/j.1365-8711.2002.05547.x [15] levine, a. m., et al.: 1996, apj, 469, l33 [16] lewin, w. h. g., et al.: 1995, x-ray binaries, camb. astr. s., vol.26 [17] mccray, r. a., et al.: 1982, apj, 262, 301 [18] morrison, r., mccammon, d.: 1983, apj, 270, 119 [19] muno, m. p., et al.: 2000, apj, 542, 1016 doi:10.1086/317031 [20] narita, t., et al.: 2001, apj, 547, 420 doi:10.1086/318326 [21] orosz, j.a., et al.: 2001, atel 75 [22] revnivtsev, m., sunyaev, r.: 2003, a&a, 399, 699 [23] roberts, w.j.: 1974, apj, 187, 575 doi:10.1086/152667 [24] šimon, v.: 2010, a&a, 513, a71 [25] šimon, v.: 2012, newa, 17, 697 doi:10.1016/j.newast.2012.04.006 [26] sheffer, e. k., et al.: 1992, sva, 36, 41 249 http://dx.doi.org/10.1086/317019 http://dx.doi.org/10.1086/308651 http://dx.doi.org/10.1111/j.1365-2966.2005.09910.x http://dx.doi.org/10.1111/j.1365-2966.2009.15721.x http://dx.doi.org/10.1046/j.1365-8711.2002.05547.x http://dx.doi.org/10.1086/317031 http://dx.doi.org/10.1086/318326 http://dx.doi.org/10.1086/152667 http://dx.doi.org/10.1016/j.newast.2012.04.006 vojtěch šimon [27] staubert, r., et al.: 2009, a&a, 494, 1025 [28] tananbaum, h., et al.: 1972, apj, 174, l143 doi:10.1086/180968 [29] truemper, j., et al.: 1978, apj, 219 l105 doi:10.1086/182617 [30] vondrák, j.: 1969, baicz, vol.20, 349 [31] wijnands, r., et al.: 2001, apj, 560, l159 doi:10.1086/324378 [32] zurita, c., et al.: 2010, a&a, 512, a26 250 http://dx.doi.org/10.1086/180968 http://dx.doi.org/10.1086/182617 http://dx.doi.org/10.1086/324378 introduction observations active state in ks 1731–260 activity in her x-1 conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.11.0097 acta polytechnica ctu proceedings 11:97–102, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app analysis of dynamic effects acting on railway crossings daniela vukušičová institute of railway structures and constructions, faculty of civil engineering, brno university of technology, brno, czech republic correspondence: vukusicova.d@fce.vutbr.cz abstract. the paper is focused on measurement and analysis of dynamic effects on railway turnouts. two same-type turnouts with different fastening elasticity were chosen. attention was focused mainly on the crossing part of the turnout, where the highest dynamic impacts occur. the point of the paper is the assessment of influence of soft rail pads on spread of dynamic energy through the construction. keywords: turnout, crossing part, dynamic effects, vibrations. 1. introduction switches and crossings are the key part of a railway track. in terms of dynamic effects they belong to the most loaded constructions on the railway infrastructure especially crossing part with common crossing. they are not only the places where wheel moves from wing rail to frog (or vice versa), but also places where the stiffness changes. however the length of track with switches and crossings constitutes just a small part of the railway network, maintenance of the crossings generates relatively high cost. [1] it is primarily caused by complex forces action which is induced by passage of the train through the crossing and also by the need of maintenance of many turnout components. the study of dynamic effects will help us to clarify some regularities which may be used for future optimisation of the construction and it should lead to its service life extension. 2. aims the main aim is a comparison of dynamic behaviour of two constructions which different fastening system elasticity. the comparison is based on evaluation of transmission of vibration through these constructions. it is required to repeat measurements several times in reasonable time periods to compare the constructions in terms of increasing dynamic effects in time, as well. one of important things to do is also a choice of suitable mathematic apparatus for evaluation of dynamic effects in time, frequency and time-frequency domain. 3. stress of a crossing part the most important place of a crossing part in terms of dynamic effects is the area of transition from a wing rail to crossing nose, where the dynamic impact occurs. this impact is transmitted through the bearers to ballast which is then extremely stressed and it leads to abrasion of gravel particles on contact with a bearer. due to this stress, degradation of ballast shape under the bearer happens and it causes inadequate support of the turnout. if a turnout is not supported appropriately, the geometry of transmission forms a wing rail to crossing nose collapses and the whole degradation process accelerates. the crossing part is stressed more and more which can cause damage of a frog. 4. mechanism of wheel transition from the wing rail to the crossing nose mechanism of wheel transition from the wing rail to the crossing nose is a very complex spatial problem. the wheel passes three phases during the transition of the frog. at first, it goes on the wing rail, then it goes through a transition zone on both wing rail and crossing nose and at last it goes on crossing nose and related rail. this mechanism is shown in fig. 1 in ideal case of geometry of transition a wheel passes from the wing rail to a crossing nose continuously without dynamic impacts. this complex problem is often simplified. the simplification consists in the fact that a wheel runs on the wing rail, which deviates from the axis of the track to create a space for a crossing nose. due to the geometry of the wheel and the wing rail the wheel often descends slightly at an angle α1. after impact on the crossing nose a wheel rises again at an angle of a crossing nose α2, as long as it does not reach the starting position at the end of the transition zone. this could be seen on the simplified model of the wheel movement through the crossing part shown in fig. 2. from fig. 2 it is evident, that the total angle, at which wheels impact the crossing nose is α = α1 +α2, in this angle the influence of transition geometry on dynamic effects is simplified described. 97 http://dx.doi.org/10.14311/app.2017.11.0097 http://ojs.cvut.cz/ojs/index.php/app daniela vukušičová acta polytechnica ctu proceedings figure 1. schematic representation of the wheel set crossing over the frog – view from above [2]. figure 2. simplified model of wheel movement through the crossing part [3]. 5. measuring location and description of measured turnouts the measurements were carried out at the railway station usti nad orlici on main lines turnouts no. 3 and 4 (fig. 3). maximum speed on main line is 130 km.h−1 (160 km.h−1) for tilting vehicles, such as pendolino). both chosen constructions are the same except elasticity of the fastening system. description of the turnouts: • part of single crossover • rails profile uic 60 • fastening system (ribbed baseplate with vossloh tension clamp skl 24), turnout no. 3 has new ribbed baseplates with different rail pads – reduce overall stiffness of the track. • monoblock crossing from manganese steel • concrete sleepers • ballasted track • crossing angle 1:12 and radius 500 m • used almost exclusively in trailing direction three measuring campaigns were made on both above figure 3. turnout no. 4 and single crossover with turnout no. 3. mentioned turnouts. 6. methodology of the measurement the certified methodology of the measurement was used [4]. measurement methodology is designed for in-situ measurement in condition of full operation and was certified by the ministry of transport of the czech republic. the certified methodology consists of bearers displacements measurements, vibration acceleration measurements (on crossing, bearers and into the ballast), and pressure measurements (in two levels into railway substructure). for the purposes of this paper only small part of vibration acceleration measurement is described, only the part which is used below in evaluation part of the paper. the focus is on vibration transition from the crossing trough bearer to the ballast. the three-axis accelerometer was placed on flange of the wing rail (fig. 4) and one-axis sensor was placed on bearer nearest to the crossing nose. piezoelectric vibration acceleration sensors on wing rail and on bearer were attached to plastic handles and glued to the cleaned surface of the measured structure. 98 vol. 11/2017 analysis of dynamic effects acting on railway crossings figure 4. the three-axis accelerometer placed on flange of the wing rail. for measurement into the ballast the measuring stone was developed. the three-axis accelerometer was inserted into the measuring stone which was placed into the ballast directly under the crossing nose. 7. mathematical apparatus when dynamic action from railway traffic is measured in-situ it is necessary to describe and evaluate stochastic signal. this is rather difficult. in order to get necessary information and compare the dynamic action on each construction it is possible to evaluate stochastic signal from three different perspectives. first perspective is time domain. the calculated value is area under the curve of moving rms (rms stands for root mean square). thanks to this time perspective it’s possible to determine total dynamic action on construction. for detailed analysis of the dynamic actions above described method is not sufficient because frequency composition is unknown. for this reason it is useful to transform signal from time domain to frequency domain. for this transformation we use fourier transformation method. in frequency domain it is possible to determine which parts of signal are the strongest ones. for detailed analysis it is useful to use third perspective, which evaluate signal from time-frequency domain [5]. with this perspective we can see not only frequency composition but also its occurrence in time. 8. the welch method the welch method is certain modification of the fast fourier transformation. digital signal x[n] (n = 0, 1, 2, ..., n − 1) is divided into k segments each of them with length m (xi[m], i = 0, 1, ..., k − 1,m = 0, 1, ...,m − 1). segments are either placed in row one by one then n = k∗m or they overlap. each segment is weight by function w[m]. after transformation and following calculations periodograms components sj[k] are created. these components put together represent approximate spectral density s[k]. this estimation is described by following formulas. component of periodograms is determined by formula 1 [6]. sj [k] = 1 u ∗m ∗ [m−1∑ m=0 x[m+i∗m ]∗w[m]∗ε( −j2πmk m ) ]2 (1) where u = 1 m ∗ m−1∑ m=0 w2[m] (2) is vector’s standard of window function, w[m] is window function. resultant estimation is done by averaged component periodogram. s = 1 k ∗ k−1∑ i=0 sj [k] (3) 9. short time fourier transform (stft) stft provides compromise between time and frequency signal representation [7]. its integral definition is stft (ω) x (t′, f) = ∫ ∞ −∞ [ x(t)∗g(t−t′) ] ∗ε−i2πf(t−t′)∗dt (4) where g is window function, ’*’ complex conjunction, t′ is time displacement of window, x(t) its time representation of signal and stft (ω) x (t′, f) is its timefrequency representation [7]. 10. evaluation of vibration acceleration evaluation of vibration acceleration is divided to three sections: time domain, frequency domain and timefrequency domain. for time analysis comparable trains that passed over both turnouts were chosen. for detailed frequency analysis were chosen locomotive type 380 and two multiple units (leo express and pendolino) because they passed over both turnouts the maximum line speed. the most interesting is transmission of vibration from wing rail (a4z) through bearer (a3z) to the ballast (a33z). the evaluated signals are identified as follows: first letter a indicates vibration acceleration, number in the middle is a measuring channel number and the last letter indicates direction (z is vertical direction). 11. evaluation in time domain from many graphs and tables i chose the one which best represents results of my analysis. table 1 represents areas under the curve of moving rms on both turnouts calculated from vibration signals measured from selected trains and their comparison in all measurements campaigns. red colour typifies percentage loss of dynamic energy by transmission from rail to bearer and to ballast. value of the area under the 99 daniela vukušičová acta polytechnica ctu proceedings curve of moving rms on rail (a4z) is thought as 100% and it is calculated how many percent of this value is transmitted to bearer (a3z) and to ballast (a33z). it is obvious that values on wing rail (a4z) are increasing especially from third campaign on turnout no. 4. this fact is apparently caused by degradation of transition geometry, as the turnout no. 4 has bigger bearer displacement. on the bearer (a3z) there are also increasing values from third measuring campaign, but the increase is not significant in either of turnouts. on the turnout no. 4 there is slight increase of the percentage of dynamic energy transfer to the bearer, while on turnout no. 3 not, which is interesting. into the ballast both turnouts are comparable, but from overall point of view more dynamic energy is transferred from turnout no. 4. if we put into account all measurement campaigns on turnout no. 3, approximately 24% of dynamic energy is transmitted to the bearer, while on turnout no. 4 it is about 35%. into the ballast almost 5% of dynamic energy is transmitted from turnout no. 3 and 6,6% from turnout no. 4. the positive contribution of new fastening system on turnout no. 3 is shown in these results. 12. evaluation in frequency domain very important information can be obtained from frequency spectrum of the evaluated signal. for better comparison frequency curves were converted to numbers by calculating the areas under the curve. the area under frequency curve was divided into two frequency bands. first frequency band (150 – 600 hz) is the band where high frequency contact impact force occurs. this high frequency impact cases especially plastic deformation on the crossing nose and that is the reason why these high frequencies are not transferred into the bearer. second frequency band (0 – 150 hz) is the band where low frequency bending process occurs. these low frequencies are responsible for bearer displacements and ballast bed bending. based on the above mentioned on the wing rail both frequency bands were evaluated while on the bearer and in into the ballast only second frequency band (0 – 150 hz) was evaluated [8]. two multiple units (pendolino and leo express) and locomotive type 380 were selected for comparison of the turnouts (table 22). it is obvious that between second and third measurement campaign all values except that into the ballast are increased. lower values into the ballast can be explained by the fact that space between the bearer and ballast occurred. the bearer has worse support which resulted in bigger displacements. bigger bearer displacements are on the turnout no. 4, this is reflected in the values from the bearer (a3z). on the wing rail (a4z) especially on the frequency band 150 – 600 hz bigger values are on turnout no. 3, bud the difference between turnouts decreases. this fact can be caused by bigger wear of the turnout no. 3. difference decreases because of displacement on turnout no. 4 bearers are more significant than on turnout no. 3. based on above mentioned evaluation it is obvious that it is possible to valorise the wear of the crossing or bearer displacement only on the basis of vibration acceleration measurements. this is an important fact. 13. evaluation in time-frequency domain time-frequency method can be used for confirmation of conclusions from frequency and time analysis. the advantage of this method is that it can display time and value of frequency action in one chart. as an example i present time-frequency graph calculated for signal detected on bearer when pendolino train passed the crossing. as we can see on figure 5 there is time on horizontal axis and frequency on vertical axis. figure 5 shows the fact that the densest frequencies were detected in time when train wheel sets were passing the measuring point. maximum frequency range is from 70 to 80 hz and about 50 hz. 14. conclusion and recommendation within three measurement campaigns two turnouts with different fastening elasticity were compared. the comparison was based on measurement of dynamic effects in-situ. according to evaluation it is possible to declare that the new fastening system on turnout no. 3 appears to be perspective. it has a positive influence in reduction of dynamic effects on bearer and ballast. i would like to recommend observation of both measured turnouts and realize more measurements on them with use of the certified methodology at least once a year. if the positive influence of new fastening system confirmed, i would recommend its installation on more turnouts. references [1] a. m. zarembski. factors involved in turnout maintenance. railway track & structures, 1995. issn 0339016. [2] r. müller, b. nelain, j. nielsen, et al. description of the vibration generation mechanism of turnouts and the development of cost effective mitigation measures. 2013. report from project rivas, code: rivas_uic_wp3-3_d3_6_v02, version 2. [3] fischer, oberaigner, daves, et al. the impact of a wheel on a crossing. die stosswirkung eines rades auf das herzstück einer weiche. zev rail glasers annalen 129, 2005. issn 1618-8330. [4] j. smutný, l. pazdera, i. vukušič. hodnocení dynamických účinků na výhybky. certifikovaná metodika. ministerstvo dopravy – odbor kosmických aktivit a its, 2014. 124/2014-710-vv/1. 100 vol. 11/2017 analysis of dynamic effects acting on railway crossings area under curve of moving [m/s] measurement train a4z on crossing no. a3z on crossing no. a33z on crossing no. 3 4 3 4 3 4 1 loko 380 49 43 12 13 3 3 24 31 6 6 2 loko 380 45 34 8 10 3 3 18 29 7 10 3 loko 380 64 40 11 14 4 3 17 35 6 8 1 leo express 123 93 31 34 4 4 26 36 3 5 2 leo express 121 89 27 30 5 6 22 33 4 6 3 leo express 152 105 32 37 4 4 21 35 3 4 1 pendolino 217 308 74 116 11 13 34 38 5 4 2 pendolino 264 229 74 76 15 14 28 33 6 6 3 pendolino 312 239 85 104 16 23 27 44 5 10 average 149,7 131,1 39,4 48,1 7,1 8,1 24,1 34,8 4,9 6,6 table 1. area under curve of moving rms and the percentage transfer of dynamic energy from rail to sleeper and to ballast. area under curve of frequency spectrum hz * m/s2 measurement train a4z on crossing no. a3z on crossing no. a33z on crossing no. 3 4 3 4 3 4 0150hz 150600hz 0150hz 150600hz 0150hz 0150hz 0150hz 0150hz 1 loko 380 1735 6413 1340 4555 988 986 328 344 2 loko 380 1206 5854 1438 4688 621 855 314 391 3 loko 380 1620 6428 1747 4635 864 1311 199 153 1 leo express 675 3461 500 2463 502 448 72 75 2 leo express 449 2402 489 1932 293 379 66 90 3 leo express 604 3463 616 2750 421 604 47 32 1 pendolino 1018 3731 737 2718 634 816 96 135 2 pendolino 1000 3615 853 3074 642 626 132 126 3 pendolino 1085 3985 991 4008 794 1175 83 72 average 1044 4372 968 3425 640 800 149 158 table 2. area under frequency curve divided in to two frequency bands. 101 daniela vukušičová acta polytechnica ctu proceedings figure 5. time-frequency spectrogram calculated by stft method, turnout no. 3, pendolino train, third measurement campaign. [5] j. smutný, l. pazdera, m. bajer, i. moll. the analysis of dynamic effects in turnout structures by the method of quadratic time and frequency invariant transformations. proceedings of the sixth international symposium "computatuonal civil engineering 2008" iasi. societatea academica matei – teiu botez, iasi, romania, 2008. isbn 978-973-8955-41-7. [6] j. smutný. the modern method of the noise and vibration analysis applied on railway traffic. thesis of the doctoral dissertation. vut brno. isbn 80-214-0988-6. [7] j. smutný, l. pazdera. time-frequency analyses of real signals. 2003. isbn 80-86433-23-4. [8] i. vukušič. analýza dynamických účinků ve výhybkách. disertační práce. vysoké učení technické v brně, fakulta stavební, ústav železničních konstrukcí a staveb, 2005. vedoucí práce prof. ing. jaroslav smutný, ph.d. 102 acta polytechnica ctu proceedings 11:97–102, 2017 1 introduction 2 aims 3 stress of a crossing part 4 mechanism of wheel transition from the wing rail to the crossing nose 5 measuring location and description of measured turnouts 6 methodology of the measurement 7 mathematical apparatus 8 the welch method 9 short time fourier transform (stft) 10 evaluation of vibration acceleration 11 evaluation in time domain 12 evaluation in frequency domain 13 evaluation in time-frequency domain 14 conclusion and recommendation references acta polytechnica ctu proceedings doi:10.14311/app.2016.5.0041 acta polytechnica ctu proceedings 5:41–43, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app modernization of railway stations česká lípa and karlovy vary with the expected co-financing from european funds form opd2 radek kratochvíl∗, maria janešová, jiří vopava ctu in prague, czech technical university in prague faculty of transportation sciences, konviktská 20, 110 00, prague 1, czech republic ∗ corresponding author: kratochvil.radek@seznam.cz abstract. the article describes the planned modernization of railway stations in česká lípa and karlovy vary, their scope and financing. the emphasis is laid on the expected co-financing of these projects from european structural and investment funds planned for the years 2016-2020. it is case of the operational program transport opd2. the study compares the two projects from many aspects, in particular from the economic and structural-urban planning points of view. keywords: modernization, railway station, opd2, construction costs. 1. european structural and investment funds opd2 on 12 may, 2015 the european commission approved operační program doprava pro období 2014-2020 – the newly designated as opd2. in the past, the transport operational program designed for the years 2007 – 2013 was used the czech republic. this opd2 program will provide the czech republic with the possibility to draw from the eu funds the amount of almost eur 4.7 billion, in particular for the development of road and rail infrastructure. general allocation of opd2: 5 524 434 631eur, including the european share: 695 769 435eur programming document opd2 (2014cz16m1op001) contains detailed information about co-financing projects in various areas of transportation. we will within this article deal with the issue of rail transport. here, there are some important and interesting facts contained in this document relating to the modernization of rail and multimodal transport: currently approximately 9,500 km of railway tracks are operated in the czech republic, which makes it considering the total area of the czech republic one of the densest rail networks in the world. the big problem of the railway network in the czech republic is its low technical level (insufficient track speed and frequent speed drops, low capacity, lack of interoperability, insufficient parameters for freight transportation, particularly the length of tracks in stations and terminals for multimodal transport), poor condition and lack of amenities of transport terminals, railway stations and stops and the related low comfort for passengers, resulting in low competitiveness in comparison with the road transport in most important directions and aspects. co-financing of the rail transport within opd2 is possible under the priority axis 1, where inter alia, the following objectives are determined: • point 1.1 improving the infrastructure for increased competitiveness and greater use of rail transport for this priority axis is the support of the eu is set in the amount of eur 2,395,964,680. the share of overall eu support in the operational program is 51.02% it is clear from table 2 (overview of investment strategy of the operational program) [1] 2. modernization of the railway station in česká lípa the main railway station česká lípa [2] is located in the liberec region. the railway station is located in the south-western part of the town of česká lípa. this is the crossroads of four railway lines, see the specification below. the railway junction česká lípa is the second largest rail hub in the liberec region (just behind liberec). specifications: ids: idol (liberec) list of numbers of tracks: 080, 081, 086, 087 [2] gps of the railway station: n 50◦40′31, 302; e 14◦31′59, 46 the railway station should undergo a complete modernization. the railway infrastructure administration [3], hereinafter referred to as sždc (as the main investor) and skanska a.s. (as the contractor / builder) have officially concluded the contract for this modernization. funds will be provided by the state fund for transport infrastructure and the construction is designed for co-financing from the european structural and investment funds – 41 http://dx.doi.org/10.14311/app.2016.5.0041 http://ojs.cvut.cz/ojs/index.php/app r. kratochvil, m. janesova, j. vopava acta polytechnica ctu proceedings figure 1. modernization of the česká lípa railway station the architectural design of the construction project (14-334-201) [5] operational program transport – opd2. at this railway station in česká lípa a new terminal building will be built for passengers and at the same time the existing station building is to be reconstructed so that it can accommodate the new safety equipment technology. a new underpass subway and three new platforms with steel roofing and elevators will be built at the station. furthermore, two bridges are to be remodelled and several other alterations shall be made within this construction project. basic information on the construction project: name: modernizace žst. česká lípa investor: správa železniční dopravní cesty, státní organizace (sždc) contractor/builder: skanska a.s. [4] designer: sudop praha a.s. construction period: november 2015 – may 2017 construction costs: 1 006 416 679 czk not including vat according to the statement of så¡dc the eu usually contribute up to 80% of the total eligible costs. the project documentation prepared by sudop praha a.s. indicates that the construction project of the modernization of the česká lípa railway station will fundamentally affect the transport in the whole česká lípa county. in addition to rebuilding the railway station the project also involves the revitalization of some connecting sections, on which the speed of trains will be increased consequently. the aim of the changes is a new configuration of the track so that it can accommodate multilevel platforms, increasing the speed from 40-60 to 65-100 km/h on most tracks for passenger trains and elimination of non-essential parts of the track. the railway station of česká lípa has been negatively affected by the division into two disjointed parts. as a result of this the station is confusing for passengers, too large and not very comfortable for a train change. the construction adjustments will unite the two parts of the railway figure 2. modernization of the česká lípa railway station the architectural design of the construction project (14-334-201) [5] figure 3. modernization of the česká lípa railway station the architectural design of the construction project (14-334-201) [5] station and the passenger area will move closer to the town center by about 250 m. 3. modernization of the railway station in karlovy vary the railway station of karlovy vary [2] is located in the karlovy vary region. the railway station (unofficially called the ”upper station”) is a transport hub of the city karlovy varyboth for the passenger and freight rail transport. the station is located on a major route cheb chomutov, track 140. specifications: ids: duk (ústí nad labem), idok (karlovy vary) list of numbers of tracks: 140, 141, 142 [2] gps of the railway station: n 50◦14′7, 737; e 12◦52′, 647 the railway station should undergo a complete modernization. sždc (as the main investor) and skanska (as the contractor/builder) have agreed on this modernization. the construction project has been designed to be co-financed from the european structural and investment funds – operational program transport – opd2. the new railway station with optimum passenger handling capacity will be 42 vol. 5/2016 modernization of railway stations česká lípa and karlovy vary figure 4. visualization of the railway station of karlovy vary, the project by sudop praha a.s. [5] built by skanska a.s. without interrupting the train service. to ensure the functionality of the station the eastern part of the existing building will be retained, which will perform the basic functions of the railway station during the construction period. after the construction project completion also this eastern part of the station building will be demolished. consequently, platform adjustments will be implemented. the new building will have one above ground and one underground floor. it will be dominated by the hall with a glass roof, which passes through both floors and divides the building into two halves. basic information on the construction project: name: modernizace žst. karlovy vary investor: správa železniční dopravní cesty, státní organizace (sždc) contractor/builder: skanska a.s., division pozemní stavitelství západ [4] designer: sudop praha a.s. construction beginning: 22.4.2015 construction costs: 75 800 000 czk not including vat 4. conclusion this article has compared two different projects on modernization of railway stations. the two projects vary greatly in terms of their scope of works and, of course, in terms of the related budgets. the planned modernization of the railway station of česká lípa is much broader and includes, for example reconstruction figure 5. the modernization of the railway station of karlovy vary station building, a cross-section b-b, project (14-217.240) [5] žel. st. česká lípa 1 006,4 žel. st. karlovy vary 75,8 table 1. construction costs of projects (czk million excluding vat) of two bridges, construction of 19 railway crossings and 32 switches on the 33 km long track. both construction projects have the same investors, designers and construction contractors and both have been designed to be co-financed from european structural and investment funds operational program transport opd2. this is a very important parameter of the project, because it would be very difficult to finance the projects of this size without the eu support. references [1] portál sždc [online]. evropské strukturální a investiční fondy, operační program doprava. [2016-02-10], http://www.opd.cz. [2] portál čd [online]. české dráhy a.s. informace o nádražích. [2016-02-10], http://www.cd.cz/cd-online/stanice.php. [3] portál opd [online]. správa železniční dopravní cesty, s.o. spolufinancování z eu. [2016-02-10], http://www.szdc.cz/modernizace-drahy/ spolufinancovani-z-eu/op-doprava.html. [4] portál společnosti skanska a.s. [online]. skanska. [2016-02-10], http://www.skanska.cz. [5] portál sudop praha [online]. sudop praha a.s. [2016-02-10], http://www.sudop.cz. 43 http://www.opd.cz http://www.cd.cz/cd-online/stanice.php http://www.szdc.cz/modernizace-drahy/spolufinancovani-z-eu/op-doprava.html http://www.szdc.cz/modernizace-drahy/spolufinancovani-z-eu/op-doprava.html http://www.skanska.cz http://www.sudop.cz acta polytechnica ctu proceedings 5:41–43, 2016 1 european structural and investment funds opd2 2 modernization of the railway station in ceská lípa 3 modernization of the railway station in karlovy vary 4 conclusion references acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0001 acta polytechnica ctu proceedings 4:1–7, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app study of identification of two-phase flow parameters by pressure fluctuation analysis ondrej burian∗, vaclav dostal, ladislav vesely faculty of mechanical engineering, czech technical university in prague, technická 4, praha 6, czech republic ∗ corresponding author: ondrej.burian@fs.cvut.cz abstract. this paper deals with an identification of a parameters of simple a pool boiling in a vertical rectangular channel by analysis of pressure fluctuation. a small experimental facility about 9 kw power, which was used for simulation of apool boiling phenomena and creation of steam-water volume in this work is introduced. a several pressure fluctuations measurements and differential pressure fluctuations measurements at various were carried out. main changed parameters were a power of heaters and a hydraulics resistance of a channel internals. a measured pressure data were statistically analysed and compared with goal to find dependencies between parameters of a two-phase flow and statistical properties of pressure fluctuation. at the end of this paper are summarized final results and applicability of this method for parameters determination of two phase flow for pool boiling conditions at ambient pressure is discused. keywords: two-phase flow, pressure fluctuation measurement, void fraction. 1. introduction boiling of liquids is a high dynamic phenomena, which is characterized as a phase change of a liquid phase to a gaseous phase. the most common example of that is boiling of water to water steam, which occurs in many facilities in our life. it may exist in wide range of parameters and regiments, which includes pressure, temperature, heat flux, bulk temperature etc. the one of the key parameters is a void fraction which represents a share of steam fraction in overall volume. the knowledge of this parameter is key for identification other parameters of boiling and operational parameters of facilities which operate with boiling phenomena like steam boilers, boiling water reactors or steam generators. one of a perspective method for identification a key parameters of boiling and two-phase flow phenomena, which is focused on analysis of measured differential pressure and its a time fluctuation, is described in this work. this method is based on fact that differential pressure between two measured locations in a two-phase mixture located in some distance at above is dependent on the void fraction. void fraction in volumetric form is defined as a ratio of a steam fraction volume to overall a two-phase volume, see (1). the density of a two-phase mixture can be expressed by (2), where ρl is density of liquid fraction and ρg is density of steam fraction. α = vg v (1) ρm = ρl(1− 〈α〉) + ρg〈α〉 (2) second assumption is that the value of this differential pressure is not stable in stable state, but it fluctuated around some mean value. this dependency is a result of influence of the void fraction on a hydrostatic pressure at measured locations – a measurement points. hydrostatic pressure of a two-phase volume about some void fraction is value between hydrostatic pressure of a liquid volume and a steam volume, which decreases with increasing a void fraction. a pressure fluctuation is a result of a process of a bubble generation and its flow throw the measured section. if we find dependency between void fraction and measured differential pressure, which is measured between two measurement points located at above in some distance, we can use it like fundamental of a method for determination of the void fraction. however more interesting may be an information about boiling and two-phase flow parameters which we can get from statistical analysis of fluctuation of measured differential pressure. research of this method, identification advantages and disadvantages of this method is subject of this research work which will be introduced in this paper. due to a boiling and a two-phase flow are complicated phenomenas, is impossible to determinate an analytical solution with physical model of dependency between void fraction and differential pressure. they are complex phenomenas which are affected many external and internal influences. from that reasons as described at above was chose experimental way which should give empirical view of scope to this problem. using differential pressure as a parameter is more useful than point pressure, because we do not know position of a level of a two-phase mixture up the measured points. the beginning phase of this research project is focused on an experimental research at an ambient pressure conditions. the aim of this phase is a verification an initial assumptions, assessment a general values of 1 http://dx.doi.org/10.14311/ap.2016.4.0001 http://ojs.cvut.cz/ojs/index.php/app title:workshop on the golden age of cataclysmic variables and related objects � ii. editors: franco giovannelli, inaf istituto di astro�sica e planetologia spaziali, area di ricerca di tor vergata, roma, italy lola sabau-graziati, inta dpt. cargas utiles y ciencias del espacio, madrid, spain co-published by: czech technical university in prague (ctu), zikova 4, 166 36 prague 6, czech republic, and astronomical institute of the czech academy of sciences, fri£ova 298, 251 65 ond°ejov, czech republic. editorial o�ce: ctu � central library, technická 6, 160 80 praha 6, czech republic. acta@cvut.cz i�: 68407700. head of the editorial board: v. petrá£ek. editorial board � internal members: robin arthur healey, rectorate of ctu, department of external a�airs, ctu, czech republic ta´ána jaro²íková, faculty of biomedical engineering, department of natural sciences, ctu, czech republic milan jirásek, faculty of civil engineering, department of mechanics, ctu, czech republic jitka jírová, faculty of transportation sciences, department of mechanics and materials, ctu, czech republic petr jizba, faculty of nuclear sciences and physical engineering, department of physics, ctu, czech republic pavel kalina, faculty of architecture, department of theory and history of architecture, ctu, czech republic zuzana masáková, faculty of nuclear sciences and physical engineering, department of mathematics, ctu, czech republic jan píchal, faculty of electrical engineering, department of physics, ctu miroslav sýkora, klokner institute, department of structural reliability, ctu, czech republic radek �ulc, ctu, faculty of mechanical engineering, department of process engineering, ctu, czech republic editor-in-chief: i. adlerová. graphic design and typesetting: v. neºerka, m. somr. cover: m. r·ºi£ková, j. jílek. print: ctu publishing house, zikova 4, 166 36 prague 6, czech republic. [date of issue] april 20, 2015 in: acta polytechnica ctu proceedings(2),1, http://ojs.cvut.cz/ojs/index.php/app isbn 978-80-01-05688-2 (�vut v praze) isbn 978-80-905129-3-1 (astronomický ústav av �r, v.v.i.) issn 2336�5382 the publication of these proceedings was �nancially supported by the czech academy of sciences. c© czech technical university in prague and astronomical institute of the czech academy of sciences, 2015. reprinting is allowed only with the agreement of the editorial o�ce and with citation of the source. palermo workshop 2013 the second international workshop on the golden age of cataclysmic variables and related objects ii palermo, italy, september 9 – 14 edited by franco giovannelli & lola sabau-graziati 1 doi: 10.14311/app.2015.02.9001 organizing institutions inaf – istituto di astrofisica e planetologia spaziali, roma – inaf-iaps, roma, italy inta – dpt. de cargas utiles y ciencias del espacio, inta-dcuce, madrid, spain czech republic academy of sciences – astronomical institute, ascr-ai, ondřejov, czech republic czech technical university, ctu in prague, czech republic department of physics, technion, haifa, israel russian academy of sciences – institute of astronomy, ras-ia, moscow, russia inaf osservatorio astronomico di capodimonte, inaf-oac, napoli, italy department of astronomy, university of washington, seattle, wa, usa scientific organizing committee dmitry bisikalo, ras-ia, moscow (russia) massimo della valle, inaf-oac, napoli (italy) franco giovannelli, inaf-iaps, roma (italy) (chairperson) rené hudec, ascr-ai., ondřejov (czech republic) lola sabau-graziati, inta-dcuce, madrid (spain) giora shaviv, department of physics, technion, haifa (israel) paula szkody, department of astronomy, university of washington, seattle, wa, usa local organizing committee franco giovannelli, inaf-iaps, roma, italy (chairperson) daniela giovannini, cnr-ibcn, roma, italy francesco reale, cnr-isc, roma, italy iv foreword new results coming from the new generation satellites, especially in the hard x–ray and γ–ray regions, renewed the interest of scientific community about cvs. this, together with the new developments in searching for the progenitors of type ia supernovae was the main reason for organizing this workshop on the golden age of cataclysmic variables and related objects. after the great success attained with the first 2011 edition, we decided to organize, in agreement with the scientific community, this second meeting of a series with biennial cadence in palermo in the beautiful mondello bay. we are completely convinced that a deep discussion about cvs and related objects, mostly through the physical processes occurring inside those systems, is the most powerful way for a better and faster development of our knowledge just of the cataclysmic processes, rather usual in the universe. for this purpose, we invited distinguished colleagues representative the most important space– and ground–based experiments of the present generation. they painted the whole panorama on the experimental results and on their interpretation by using current models and/or developing new ideas for a better comprehension of the detected phenomena. during the discussion of a lot of new results, obtained along most of the electromagnetic spectrum, we have learned that the astrophysics of galactic sources is still extremely interesting and unavoidable. indeed it provides crucial information on the same physical processes occurring also in the extra–galactic sources, with obvious different scale factors. many thanks to the authors, which accepted our reminders recalled at the beginning of the workshop, for keeping to schedule. however, in spite of the accurate respect of the dead line of a number of authors, we still suffer a delay in publishing these proceedings because of the laziness of a considerable part of other authors. in spite of this, these proceedings will appear within one year from the workshop date. this is the second edition of the workshop, whose proceedings are published by the ‘acta polytechnica ctu proceedings’, an international refereed journal of the czech technical university in prague (czech republic). we would like to thank all participants and especially the speakers for their active contributions in rendering this workshop updated with their talks, alive with their discussions, and friendly with their attitudes. particular thanks to mr francesco reale for his excellent assistance for informatics in roma, during the preparation of the workshop, and for his faultless assistance in palermo. a very special thank to dr daniela giovannini for her precious help in managing the workshop. we are grateful to the pianist maestra valentina usai, to the violinist maestro alessandro perpich and to the actresses lisa colosimo and flavia giovannelli for their wonderful performance ”hic habitat felicitas: mozarterie from the kingdom behind” staged in the suggestive atmosphere of the splendid la torre hotel. v many thanks to: i. the director of the istituto di astrofisica e planetologia spaziali, roma of the istituto nazionale di astrofisica (iaps-inaf) (dr pietro ubertini); ii. the caen s.p.a. (viareggio) who partially supported the organization of this workshop. particular thanks to the plan nacional de i+d+i of spain for partially supporting the publication of this book. finally, we would like to thank mr daniele inzerillo, the chef of the splendid la torre hotel, who delighted us with his creations during our stay and to the whole staff of the hotel for their professionalism and kindness. the editors franco giovannelli & lola sabau-graziati vi list of participants arai akira, nishi-harima astronomical observatory, university of hyogo, japan arai@nhao.jp balman solen, middle east technical university, turkey solen@astroa.physics.metu.edu.tr baptista raymundo, universidade federal de santa catarina (ufsc), brazil raybap@gmail.com bisikalo dmitry, institute of astronomy ras, russia bisikalo@inasan.ru blondin stéphane, service d’astrophysique, cea saclay, france stephane.blondin@oamp.fr breytenbach hannes, university of cape town, south africa johbenbrey@gmail.com buckley david, southern african large telescope, south africa dibnob@saao.ac.za cannizzo john, umbc/nasa/gsfc, usa john.k.cannizzo@nasa.gov carter philip, department of physics, university of warwick, uk philip.carter@warwick.ac.uk chochol drahomir, astronomical institute of the slovak academy of sciences, slovakia chochol@ta3.sk de bianchi silvia, tu dortmund, germany silvia.debianchi@tu-dortmund.de della valle massimo, capodimonte astronomical observatory, inaf-napoli & icranet, pescara, italy dellavalle@na.astro.it ederoclite alessandro, centro de estudios de f́ısica del cosmos de aragón, spain aederocl@cefca.es gilmozzi roberto, european southern observatory, garching, germany rgilmozz@eso.org giovannelli franco, inaf – iaps, roma, italy franco.giovannelli@iaps.inaf.it vii gonzalez-riestra rosario, xmm–newton science operations ctr, esac, villafranca del castillo, villanueva de la cañada, madrid, spain rosario.gonzalez@sciops.esa.int hachisu izumi, university of tokyo, japan hachisu@ea.c.u-tokyo.ac.jp henze martin, xmm–newton science operations ctr, esac, villafranca del castillo, villanueva de la cañada, madrid, spain martin.henze@sciops.esa.int hernandez santisteban juan venancio, university of southampton, uk j.v.hernandez@soton.ac.uk hudec rené, astronomical institute as–ondřejov & ctu–prague, czech republic rene.hudec@gmail.com idan irit, technion israel institute of technology, israel idan@technion.ac.il isern jordi, institut for space sciences ice-csic/ieec, barcelona, spain isern@ieec.cat ishida manabu, the institute of space and astronautical science/jaxa, sagamihara, japan ishida@astro.isas.jaxa.jp izzo luca, sapienza university of rome and icranet, roma, italy luca.izzo@gmail.com kajikawa tomoyo, kyoto sangyo university, kyoto, japan kajikawa@cc.kyoto-su.ac.jp kato mariko, keio university, yokohama, japan mariko@educ.cc.keio.ac.jp katysheva nataly, sternberg state astronomical institute, moscow, russia natkat2006@mail.ru kawakita hideyo, koyama astronomical observatory kyoto, sangyo university, kyoto, japan kawakthd@cc.kyoto-su.ac.jp knigge christian, university of southampton, uk c.knigge@soton.ac.uk kononov dmitriy, institute of astronomy ras, moscow, russia dkononov@inasan.ru kotze marissa, south african astronomical observatory, cape town, south africa marissa@saao.ac.za viii kotze enrico, south african astronomical observatory, cape town, south africa ejk@saao.ac.za latev georgi, institute of astronomy and national astronomical observatory, sofia, bulgaria glatev@astro.bas.bg martino bruno luigi, associated iaps-inaf, roma, italy brunolmartino@gmail.com mason paul, university of texas at el paso, usa pmason@nmsu.edu meintjes pieter, university of the free state, bloemfontein, south africa meintjpj@ufs.ac.za mikolajewska joanna, n. copernicus astronomical center–pan, warsaw, poland mikolaj@camk.edu.pl mukai koji, nasa/gsfc/cresst and umbc, greenbelt, md, usa koji.mukai@umbc.edu nagashima masayoshi, kyoto sangyo university, kyoto, japan g0837714@gmail.com naito hiroyuki, nagoya university, nagoya, japan naito@phi.phys.nagoya-u.ac.jp nebot ada, observatoire astronomique de strasbourg, france ada.nebot@astro.unistra.fr ness jan-uwe, xmm–newton science operations ctr, esac, villafranca del castillo, villanueva de la cañada, madrid, spain juness@sciops.esa.int neustroev vitaly, university of oulu, finland vitaly.neustroev@oulu.fi odendaal alida, university of the free state, bloemfontein, south africa winka@ufs.ac.za orio marina, inaf–osservatorio astronomico di padova, italy marina.orio@oapd.inaf.it pagnotta ashley, american museum of natural history, new york, ny, usa pagnotta@amnh.org parisi pietro, inaf – iaps, roma, italy pietro.parisi@iaps.inaf.it ix patterson joseph, columbia university, new york, ny, usa jop@astro.columbia.edu poggiani rosa, dipartimento di fisica, università di pisa, italy rosa.poggiani@df.unipi.it potter stephen, south african astronomical observatory, cape town, south africa sbp@saao.ac.za pretorius margaretha, university of southampton, uk m.pretorius@soton.ac.uk qian shengbang, yunnan astronomical observatory, kunming, china qsb@ynao.ac.cn reale francesco, cnr – isc, italy francesco.reale@sic.rm.cnr.it reinsch klaus, universität göttingen, institut für astrophysik, germany reinsch@astro.physik.uni-goettingen.de ritter hans, max-planck-institut für astrophysik, germany hsr@mpa-garching.mpg.de sabau-graziati lola, instituto nacional de técnica aeroespacial (inta) — departamento de cargas utiles y ciencias del espacio (dcuce), torrejón de ardóz, madrid, spain sabaumd@inta.es scaringi simone, k.u. leuven, the netherlands simone.scaringi@ster.kuleuven.be schmidtobreick linda, eso, santiago, chile lschmidt@eso.org schreiber matthias r., universidad de valparaiso, chile matthias.schreiber@uv.cl sekeras matej, astronomical institute of slovak academy of sciences, tatranska lomnica, slovakia msekeras@ta3.sk semena andry, space research institute (iki)–ras, moscow, russia san@iki.rssi.ru shaviv giora, technion – israel institute of technology, haifa, israel giora@shaviv.org šimon vojtěch, astronomical institute, academy of sciences, ondřejov, czech republic vojtech.simon@gmail.com x sion edward, villanova university, pa usa edward.sion@villanova.edu skopal augustin, astronomical institute of slovak academy of sciences, tatranska lomnica, slovakia skopal@ta3.sk smith robert, department of physics & astronomy, university of sussex, brighton, uk r.c.smith@sussex.ac.uk stoyanov kiril, institute of astronomy and national astronomical observatory, sofia, bulgaria kstoyanov@astro.bas.bg suleimanov valery, institute for astronomy and astrophysics, university of tübingen, germany suleimanov@astro.uni-tuebingen.de szkody paula, university of washington, wa, usa szkody@astro.washington.edu tanabe kenji, okayama university of science, okayama-shi, japan tanabe@big.ous.ac.jp tappert claus, dpto de f́ısica y astronomı́a, facultad de ciencias, universidad de valparaiso, chile claus.tappert@uv.cl ubertini pietro, inaf – iaps, roma, italy pietro.ubertini@iaps.inaf.it uemura makoto, hiroshima university, higashi-hiroshima, japan uemuram@hiroshima-u.ac.jp voloshina irina, sternberg astronomical institute, moscow state university, moscow, russia vib@sai.msu.ru yuasa takayuki, jaxa, sagamihara, japan yuasa@astro.isas.jaxa.jp zemko polina, sternberg astronomical institute, moscow state university, moscow, russia polina.zemko@gmail.com zharikov sergey, instituto de astronomı́a, unam, ensenada, mexico zhar@astrosen.unam.mx zhu liying, yunnan astronomical observatory, kunming, china zhuly@ynao.ac.cn xi xii 329 acta polytechnica ctu proceedings 1(1): 329–331, 2014 329 doi: 10.14311/app.2014.01.0329 concluding address franco giovannelli1 1inaf istituto di astrofisica e planetologia spaziali, area di ricerca di tor vergata, via del fosso del cavaliere, 100 i00177 roma, italy corresponding author: franco.giovannelli@iaps.inaf.it abstract before i officially conclude this workshop — far be it from me to attempt to compete with some concluding remarks already delivered at the meeting with various levels of passion by gennady bisnovatyi-kogan, giulio auriemma and sergio colafrancesco — i would like to comment on some of the highlights emerging from our fruitful week of discussions about multifrequency behaviour of high energy cosmic sources, without any pretension of completeness. keywords: photonic astrophysics particle astrophysics neutrino astrophysics. undoubtedly the advent of spacecraft gave a strong impulse to astronomy. starting roughly in the mid 1970s, almost the whole electromagnetic spectrum has been continuously surveyed in a large number of space experiments. astroparticle physics, a new field of physics, was born roughly twenty years ago by joining the efforts of the high energy astrophysics community and the particle physics community. during this relatively short period of time, astroparticle physics has developed strongly through studies of cosmic sources that are emitters of photons, charged particles, and neutrinos. some of the sources could produce gravitational waves that will probably be detectable in the near future with the new generation of ground–based gravitational experiments, such as ligo, and space– based experiments, such as lisa. meanwhile the large hadron collider (lhc) has been producing excellent results on the higgs boson, and in general about the study of pp collisions at tev energies, never obtained before in ground–based laboratories. these results, together with the results coming from the hubble space telescope (hst), with its deep survey of faraway objects of the universe, and with the vhe emission detected from a number of cosmic sources, both galactic and extragalactic, are witnesses of the validity of the big bang theory, described by the standard model. among many experimental and theoretical results discussed during this workshop, i would like to mention a couple of them that, in my opinion, will underpin the future of astroparticle physics. the first is the vhe sky at energies eγ > 100 gev. about 150 tev sources have been detected (see fig. 1, http://tevcat.uchicago.edu/). only 20 years ago, this sky was practically empty. it is expected that over the next decade the ongoing operation of fermi will be accompanied by observations with the current ground– based h.e.s.s., magic, veritas experiments and the planned cta and hawc experiments. data obtained in the very wide energy range from 100 mev to 1 pev will provide very deep insights into a number of problems of high-energy astrophysics and fundamental physics (see the review paper about tev astronomy by rieger, de oña-wilhelmi & aharonian, 2013). figure 1: tev sources catalog (http://tevcat.uchicago.edu/) the second is connected with the reionization epoch of the universe at z ≈ 20 − 30, when the first stars appeared (e.g. lamb & reichart, 2000; ciardi & loeb, 2000; bromm & loeb, 2002). therefore, quasars and grbs could be detectable up to roughly that epoch. type–ia supernovae (sne ia) have been detected up to z ≈ 1.7; the future jwst will be able to detect sn ia in the range 1.7< z < 3 (aldering et al., 2007). quasars have been detected at z = 6.419, 6.43 (fan et al., 2003), and z = 7.085 (mortlock et al., 2011), and grbs up to z = 9.4 (cucchiara et al., 2011). these detections support the theory fixing the reionization epoch to z ≈ 20 − 30 (see fig. 2). 329 http://dx.doi.org/10.14311/app.2014.01.0329 franco giovannelli after this workshop, the importance of multifrequency astrophysics and multienergy astro-particle physics once more appears evident. however, there are many problems in performing simultaneous multifrequency, multisite, multiinstrument, multiplatform and multienergy measurements due to: i) objective technological difficulties; ii) sharing common scientific objectives; iii) problems of scheduling and budgets; iv) political management of science. figure 2: sketch of the evolution of the universe from the epoch of recombination up to the present time. the epoch of reionization is also marked (after dai zhigao, nanjing university). the positions of the highest z quasars and grb are superimposed. during this fruitful workshop, we hope to have demonstrated once more the “vulcano theorem” enunciated in my concluding address in 1984: it is possible to develop science seriously even if smiling. and finally, i would like to conclude with a few wonderful words of dr daisaku ikeda (2001)–president of soka gakkai international (sgi)–reported in the booklet for today and tomorrow the thought for may 30th: “whoever has many friends has greater opportunities for growth. in this way, one both makes society a better place, and lives happier and more satisfied. in all cases, human relations, interpersonal interaction and communication are of vital importance. we must establish and nurture friendship and contacts with many people, both in our environment, and in society in general. in this manner our life will open up and will flourish”. we could go back to early childhood when we were like the little prince. one sees clearly only with the heart. what is essential is invisible to the eye (from the little prince, by antoine de saint exupéry). acknowledgement it is my pleasure to thank: the scientific organizing committee (j.h. beall, th. boller, r. hudec, l. sabau-graziati, a. santangelo); the informatics operator (francesco reale alias figaro, the factotum) for helping with informatics and in solving all related problems during the preparation and development of the workshop, and at the registration desk in palermo; the executive secretary, daniela giovannini, who smoothed any inconveniences that occurred at the registration desk with professionalism and moreover with her nice smile; the directors of inaf-iaps, dcu&ce-inta, mpe, e-o. hulburt ctr-nrl, st. john’s college, iaa/university sand 1, ascr/ai ondřejov & the czech technical university in prague; the actresses lisa colosimo and flavia giovannelli; the violinist alessandro perpich and pianist valentina usai; the staff of the splendid hotel la torre. on behalf of the soc and loc, i am pleased to thank all participants and especially the speakers for their active contributions in updating this workshop with their talks, alive with their discussions, and friendly with their attitudes. my special thanks to three colleagues and friends (gennady bisnovatyikogan, giulio auriemma and sergio colafrancesco), who kindly took on the challenging task of making the concluding remarks of the workshop. finally, on behalf of all participants, i would like to express my warm thanks to the chef, mr daniele inzerillo, who prepared a large number of delicacies for us. i hope to meet all of you once again during our next palermo workshop. references [1] aldering, g. et al.: 2007, astropart. phys. 27, 213. doi:10.1016/j.astropartphys.2006.11.001 [2] bromm, v., loeb, a.: 2000, apj 575, 111. doi:10.1086/341189 [3] ciardi, b., loeb, a.: 2000, apj 540, 687. doi:10.1086/309384 [4] cucchiara, a. et al.: 2011, apj 736, 7. doi:10.1088/0004-637x/736/1/7 [5] fan, x. et al.: 2003, aj 125, 1649. 330 http://dx.doi.org/10.1016/j.astropartphys.2006.11.001 http://dx.doi.org/10.1086/341189 http://dx.doi.org/10.1086/309384 http://dx.doi.org/10.1088/0004-637x/736/1/7 concluding address [6] ikeda, d.: 2001, for today and tomorrow the thought of 30th may, edizioni esperia. [7] lamb, d.q., reichart, d.e.: 2000, aip conf. proc. 526, 658. doi:10.1063/1.1361618 [8] mortlock, d.j. et al.: 2011, nature 474,616. doi:10.1038/nature10159 [9] rieger, f.m., de oña-wilhelmi, e., aharonian, f.a.: 2013, front. phys. 8(6), 714. doi:10.1007/s11467-013-0344-6 331 http://dx.doi.org/10.1063/1.1361618 http://dx.doi.org/10.1038/nature10159 http://dx.doi.org/10.1007/s11467-013-0344-6 acta polytechnica ctu proceedings doi:10.14311/app.2017.13.0035 acta polytechnica ctu proceedings 13:35–38, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app foamed cement composites: detection of the modulus of elasticity using dic analysis and comparison with other methods jakub ďurejea,∗, zdeněk prošeka,b a czech technical university in prague, faculty of civil engineering, thákurova 7, 166 29 prague 6, czech republic b university centre for energy efficient buildings, czech technical university in prague, třinecká 1024, 273 43 buštěhrad, czech republic ∗ corresponding author: jakub.dureje@fsv.cvut.cz abstract. a modulus of elasticity was determined for eight differently foamed cement paste samples. samples were loaded in the laboratory by a hydraulic press. the force acting on the sample was read directly from the laboratory press. digital image correlation (dic) analysis were used to draw deformations. before loading pressure test was applied a random contrast pattern to the samples. samples were captured by the camera in a one-second interval during the loading pressure test. the images were edited in the adobe photoshop lightroom and then evaluated using ncorr software. the result is a vertical and horizontal shift field. on the basis of the results obtained, it was possible to calculate the modulus of elasticity of each sample. keywords: dic analysis, foamed cement paste, field of displacement, static modulus of elasticity, dynamic modulus of elasticity. 1. introduction there are many different methods to detect deformation of the sample during the loading pressure test. the displacement of the crosspiece of the hydraulic press does not correspond to the deformation of the sample in the direction of the force. this is due to the deformation of the exponed parts of the test device. to measure deformations, it is possible to use some type of extensometer and place it directly between the jaws of the press in which the sample is tested and measure the displacement directly between the jaws. thanks to the ever-improving technologies, we can obtain the entire field of displacement by dic analysis by capturing a series of photos during sample testing and subsequent evaluation. the advantage is that, compared to the measurement with an extensometer, we obtain deformations in all directions on the measured surface of the sample [1, 2]. dic analysis is used in many industries, by many companies, including airbus, awe, stresscraft and british energy. it is used, for example, for measuring the heat dissipation and curvature of electronic components, for measuring the 3d shape of the air bags, for monitoring the components of the power plants to determine their status and to reduce their emissions, or for the behavior of building materials during the loading tests [2]. dic analysis is an optical method, to get the most accurate results it is necessary to avoid optical defects. for each lens, the image is distorted towards the edges. depending on the deformation of the square, we distinguish distortions to barrel distortions, pincushion distortions, or a combination of both – wave distortions. lens manufacturers are trying to eliminate these phenomena with the appropriate lens system. the lenses are constructed at certain distances where the distortion occurs least. for this reason, it is necessary to select a suitable lens and capture distance according to the size of the subject to be sensed [3, 4]. 2. materials and samples the sample properties were measured at 28 days of age and the day after manufacture the samples were removed from formwork and stored freely in a laboratory environment at a temperature of 22 ± 1 ◦c and a relative humidity of 50 ± 2%. test beams of dimensions 40×40×160 mm were made, which were broken in half during the previous bend test. the reference mixtures for testing were made of portland cement cem i 42.5r radotin (refc), a combination of portland cement and finely ground concrete recyclate in a ratio of 0.66 : 0.34 (refr). fine-grained recycled concrete was produced by high-speed grinding, from waste generated from drainage concrete blocks. subsequently, the reference mixtures were lightened using foaming additives such as industrial additive from the mapei (m) company or the additive used by firefighters (h). the composition of the individual samples and the bulk density are given in table 1 [5]. 3. experimental methods dic analysis was performed on a total of 10 samples, on two references and eight differently foamed cement pastes. samples were loaded in the laboratory by a 35 http://dx.doi.org/10.14311/app.2017.13.0035 http://ojs.cvut.cz/ojs/index.php/app jakub ďureje, zdeněk prošek acta polytechnica ctu proceedings sample nr. designation cement (c) recyclate (r) weight (c+r) water to mix cement putty (v1) water added to the foam (v2) water (v1+v2) w/c foam bulk density [g] [g] [g] [g] [ml] [ml] [-] [ml] [kg.m−3] 45 c7.5h 750.0 0.0 750 225 75 300 0.40 3.75 603.83 40 c7.5m 750.0 0.0 750 225 75 300 0.40 3.75 677.84 29 c10h 1000.0 0.0 1000 300 50 350 0.35 2.50 1333.10 21 c10m 1000.0 0.0 1000 300 50 350 0.35 2.50 1394.40 24 r7.5h 487.5 262.5 750 225 75 300 0.40 3.75 1177.08 34 r7.5m 487.5 262.5 750 225 75 300 0.40 3.75 895.14 15 r10h 650.0 350.0 1000 300 50 350 0.35 2.50 1603.99 12 r10m 650.0 350.0 1000 300 50 350 0.35 2.50 1457.30 5 refc 1000.0 0.0 1000 350 0 350 0.35 0.00 1646.10 9 refr 650.0 350.0 1000 385 0 385 0.39 0.00 1641.70 table 1. composition of the samples and the bulk density [5]. figure 1. random pattern on a sample in grayscale. hydraulic press heckert model fp100, at a speed of 1 mm per minute. subsequently, a static modulus of elasticity was specified. after that, static modulus of elasticity obtained on the basis of dic analysis, static modulus of elasticity obtained on the basis of the displacement of the hydraulic press and the dynamic elastic modulus obtained by the ultrasonic and resonance method were compared. nondestructive resonance method was used to measure dynamic modules. the brüel & kjær measuring set consists of the figure 2. field of vertical displacement from the ncorr post software. brüel & kjær type 3560-b-120 measuring switchboard, the brüel & kjær type 4519-003 acceleration sensor, the brüel & kjær type 8206 impact hammer and the control laptop. modulus of elasticity obtained from data from crosspiece of the hydraulic press does not correspond to the reality, because the deformation of the test instrument itself is included in the data. also, the values of the dynamic modulus of elasticity are rather inaccurate due to the inappropriateness of the resonant and ultrasonic method on porous systems. dynamic modulus of elasticity should achieve higher values than static modulus of elasticity, because by non-destructive methods we get the tangent modulus 36 vol. 13/2017 foamed cement composites: detection of .... figure 3. results of static and dynamic moduli of elasticity. of elasticity and the secant modulus of elasticity we get from the loading test [6]. 4. princip of dic analysis dic (digital image correlation) is an optical method used to measure displacement on the sample surface. compares the grayscale values of individual groups of points called subsets on the surface of the sample between the pictures taken during the loading test. it is necessary to have a sufficiently contrasting random pattern on the surface of the sample. some materials have this pattern naturally. for other samples, the pattern should be applied appropriately. the software compares shades of gray and their displacement between individual photos (figure 1). the result is the field of displacement between the reference and each picture. the reference picture is usually taken before the start of the test [7, 8]. 5. advantages of dic analysis dic analysis is a cost-effective optic method that can be used in laboratory and outdoor environment. it is used to inspect large important structures (bridges, industrial buildings, power plants) that degrade due to external influences. the capture of large objects can be done directly from the air using drones thanks to advanced technologies. this solution is relatively simple, accurate and financially advantageous [1, 2]. during the measurements in the laboratory, we obtain a field of displacement in the horizontal and vertical directions. we can also measure cracks occurring. during the loading tests, the exact course of cracks can be determined by dic analysis, even those that are not observable by the naked eye. these data are very beneficial for the presumption of the durability of the tested material [2]. 6. sample measurement dic analysis was used on foamed cement paste samples. half of cement paste beams were tested according to csn en 12390-3 test of hardened concrete part 3: compressive strength of test samples [9]. a random contrast pattern of black and white spray was applied to the samples. during the testing, images were taken with canon eos 70d on a tripod from a distance of approximately 300 millimeters. the images were taken in a one-second sequence during loading. for each sample, 50 − 100 photos were taken. the photos were edited in adobe lightroom for higher contrast, and then the dic analysis was performed in ncorr version 1.2.1. the results were scaled and the virtual extensometer was placed in the field of displacement in the ncor_post software (figure 2). the results of the individual displacement were assigned to the respective forces using the extractforces software. subsequently, a static modulus of elasticity in microsoft excel was calculated from the results. 7. results and discussions samples ref c and ref r were references. the other eight samples were differently foamed. samples 37 jakub ďureje, zdeněk prošek acta polytechnica ctu proceedings c 7.5 h, c 7.5 m, and r 7.5 m were foamed too much therefore it was not possible to measure the dynamic modulus of elasticity by the resonance method because it was not possible to capture the response from the impact hammer. the results of the other modulus of elasticity in these three samples, because of their high foaming, are not very accurate. in the case of the compression test, these three samples were observed (especially for samples c 7.5 h and c 7.5 m), as the material collapsed successively on the floors. it was not about the flexible behavior that is assumed to acquire the modulus of elasticity. therefore, the results of the measurements of these samples should be considered inaccurate, and due to their poor mechanical properties, do not use this highly foaming cement paste for practical use in the building industry. the static modulus of elasticity for all samples obtained from the displacement of the hydraulic press crosspiece are very low. this is due to the deformation of the test rig itself together with the sample deformation. for this reason, it makes no sense to further consider the static modulus of elasticity thus obtained. measurement of c 10 m, r 10 h and r 10 m samples were expected, static moduli of elasticity are slightly less than dynamic. for samples r 7.5 h, ref c, and ref r, the static moduli of elasticity are approximately half that of the dynamic moduli of elasticity. on the other hand, the static modulus of elasticity is higher than the dynamic for c 10 h sample (figure 3). this is due to the inaccuracy of measuring the dynamic modulus of elasticity because of the inappropriateness of the resonant and ultrasonic method on porous systems. 8. conclusion for this type of samples, the most accurate method is dic analysis. measurement by ultrasonic method or resonance method is not accurate in porous systems. measurement of deformation directly from the hydraulic device is very inaccurate as it involves deformation of the hydraulic device itself. the results show that the less or no foamed samples without recyclate have a higher modulus of elasticity than samples with recyclate, but with more foamed samples, it is the opposite. furthermore, it is noticeable that the less foamed samples with a foaming additive used by firefighters have a higher modulus of elasticity than samples with a foaming additive for industrial use, but with more foamed samples, this is the opposite. acknowledgements this outcome was supported by the czech technical university in prague under no. sgs16/201/ohk1/3t/11 and no. sgs17/060/ohk1/1t/11 and by the ministry of education, youth and sports within national sustainability programme i, project no. lo1605. the authors also thank the center for nanotechnology in civil engineering at the faculty of civil engineering, czech technical university in prague, and the joint laboratory of polymer nanofiber technologies of the institute of physics, academy of science of czech republic, and the faculty of civil engineering, czech technical university in prague. references [1] p. k. rastogi, e. hack. optical methods for solid mechanics: a full-field approach. john wiley & sons, 2012. [2] n. mccormick, j. lord. digital image correlation. materials today 13(12):52–54, 2010. [3] jasar. optické vady a vlastnosti objektivu. http: //photo.mysteria.cz/clanky/objekt2.html#aberace, 2002. [4] l. jelinek. darktable: korekce objektivu a odstranění skvrn. https://www.linuxexpres.cz/praxe/ darktable-korekce-objektivu-a-odstraneni-skvrn, 2015. [5] v. růžička. mechanické vlastnosti pěnových cementových pas. master’s thesis, czech technical university in prague, prague, 2017. [6] m. ballon. porovnaní modulů pružnosti stavebních materialů. master’s thesis, brno university of technology. faculty of civil engineering, brno, 2014. [7] m. a. sutton, j. j. orteu, h. schreier. image correlation for shape, motion and deformation measurements: basic concepts, theory and applications. springer science & business media, 2009. [8] s. yoneyama, g. murasawa. digital image correlation. experimental mechanics 2009. [9] čsn en 12390-3–zkoušení ztvrdlého betonu–část 3: pevnost v tlaku zkušebních těles. úřad pro technickou normalizaci, metrologii a zkušebnictví 10, 2009. 38 http://photo.mysteria.cz/clanky/objekt2.html#aberace http://photo.mysteria.cz/clanky/objekt2.html#aberace https://www.linuxexpres.cz/praxe/darktable-korekce-objektivu-a-odstraneni-skvrn https://www.linuxexpres.cz/praxe/darktable-korekce-objektivu-a-odstraneni-skvrn acta polytechnica ctu proceedings 13:36–39, 2017 1 introduction 2 materials and samples 3 experimental methods 4 princip of dic analysis 5 advantages of dic analysis 6 sample measurement 7 results and discussions 8 conclusion acknowledgements references 174 acta polytechnica ctu proceedings 2(1): 174–177, 2015 174 doi: 10.14311/app.2015.02.0174 application of total variation minimization to doppler tomography m. uemura1, t. kato2, d. nogami3, r. mennickent4 1hiroshima astrophysical science center, hiroshima university, kagamiyama 1-3-1, higashi-hiroshima, hiroshima 739-8526, japan 2department of astronomy, kyoto university, kitashirakawa-oiwake-cho, sakyo-ku, kyoto 606-8502, japan 3kwasan and hida observatories, kyoto university, yamashina-ku, kyoto 607-8471, japan 4universidad de concepción, departamento de astronomı́a, casilla 160-c, concepción, chile corresponding author: uemuram@hiroshima-u.ac.jp abstract we have developed a new model of the doppler tomography using total variation minimization (dttvm). we demonstrated that this method can reconstruct localized and non-axisymmetric profiles possibly having sharp edges in the doppler map. we apply this model to the real data of the dwarf nova, wz sge in superoutburst. dttvm can reproduce the observed spectra with a high precision, while the previous models fail to reproduce localized sources. keywords: cataclysmic variables dwarf novae optical spectroscopy individual: wz sge. 1 introduction doppler tomography (dt) is a widely-used method in the field of cataclysmic variables (cvs) [1]. dt is an ill-posed inverse problem in most cases. a filtered backprojection method provides a way to solve the problem. it masks high frequency components in the doppler maps in order to uniquely determine the solution. the other way is to introduce regularization terms in addition to the likelihood term. the maximum entropy method (mem) has been used to regularize the dt problem. the dt with mem determines the solution by maximizing the information entropy over the default image. the comparison between the back-projection method and mem is reported in [2]. those dt methods tend to smeared out the localized and sharp-edge profiles in the doppler map. on the other hand, such profiles are expected to appear in accretion disks of cvs, such as spiral shocks and hot spot. it has been reported that there are significant residuals between the observed and model spectra that are obtained from dt (e.g. [3]). it is, however, unclear if the residuals indicate real emission components that are not reproduced by the model. in this paper, we introduce a new dt by total variation minimization (tvm), which is described in [4]. tvm has received attention in the field of image reconstruction because it can reconstruct sharp-edge features by making image sparse in its gradient domain. 2 doppler tomography by total variation minimization 2.1 model suppose there are m data given by d = {d0, d1, · · · , dm}. the i-th element of d, di, is the flux at a radial velocity vr,i and phase φi. also suppose n × n = n points in the doppler map given by s = {s0,0, s0,1, · · · , sn,n}. the j-th element in the map has the coordinate of (vx,j , vy,j) and intensity of sj . the goal of dt is to estimate ŝ from the observation d according to ŝ = arg min s { 1 m ‖d−as‖22 + λ n φ(x) } . (1) the first term in the right side is a least-square term, and the second term is a regularization term which consists of a hyperparameter λ and a function φ. a is a m × n matrix whose element depends on the phase, radial velocity, and instrumental response. for the response function, we assumed a gaussian profile with a variance σ2, where σ corresponds to the velocity resolution of the observed spectra. an element of a, aij is then given by aij = 1√ 2πσ2 exp { − (vr,i − vr,ij) 2 2σ2 } . (2) tvm provides a method to solve ill-posed problems. 174 http://dx.doi.org/10.14311/app.2015.02.0174 application of total variation minimization to doppler tomography the isotropic total variation φtvm,iso is defined as φtvm,iso(s) = ∑ i,j √ (si+1,j − si,j)2 + (si,j+1 − si,j)2. (3) φtvm,iso is used as φ in equation (1) in our model. we use the twist algorithm to estimate ŝ in equation (1) [5, 6].1 the calculation code of dttvm can be available at our web site.2 2.2 demonstrations using artificial data we show an example of the results of dttvm using artificial data sets in figure 1. first, we made the assumed doppler maps, then simulated observations of line-profile variations, and reconstructed the maps using dttvm. we calculated three doppler maps from the simulated spectra with different values of λ in equation (1). we assumed the original doppler map containing three spot structures, as shown in the upper leftmost panel of figure 1. the upper two spots have sharp-edge and flat-top profiles of different size and intensity. the lower left spot has a gaussian profile. dttvm reproduced the original map in all three cases. in case (a), the edges of the flat-top spots are slightly smeared out compared to cases (b) and (c). in addition, the peak intensity of the gaussian spot is underestimated in case (a). these smearing effects are less prominent for smaller values of λ. the model spectra and residuals are also shown in figure 1. the residuals are smaller for smaller λ. these results demonstrate that dttvm can reconstruct both sharp-edge and smooth profiles in a doppler map. 2.3 application to the data of wz sge we apply dttvm to the data of the dwarf nova, wz sge taken on the 10th day of the superoutburst in 2001 [7]. figure 2 presents the doppler maps and model spectra. the results were computed using log10 λ of (a) −2.2, (b) −3.2, and (c) −5.2. all doppler maps exhibit a disk feature having non-axisymmetric distribution of intensity. the peak intensity of the localized bright regions is lower in case (a) than the others. as a result, the residuals are large in case (a), compared with the other cases. the model spectra reproduce the observed one without any prominent residuals in cases (b) and (c). figure ?? shows the result of the doppler tomography using the same data of wz sge calculated with mem. we used the calculation code presented in [8].3 the calculation code defines α as a hyperparameter of the model. cases (a), (b), and (c) in figure ?? were calculated with logα = −1.0, −2.0, and −3.0, respectively. in cases (a) and (b), smooth two-armed structures appear on a weak sign of a disk feature. in case (c), patchy structures appear, but they are evidently artifacts. in all cases of (a), (b), and (c), there are significant residuals of the spectral data at −500 km s−1 for phase 1.75 and at +500 km s−1 for phase 1.60. both features have counterparts at phases shifted by 0.5, which indicate they are rotating components with the orbital period. these rotating residuals definitely arise from localized structures in the doppler map, which can be successfully reconstructed by dttvm: the former one corresponds to the feature at (vx, vy) ∼ (0, 500) and the latter one to the lower right region in figure 2. 3 summary as demonstrated above, dttvm can reconstruct both sharp-edge and smooth profiles in a doppler map. hence, this model is advantageous for the reconstruction of highly localized or edge structures in the doppler map, such as the emission from the secondary star, hot spot, or shock wavefront. the doppler map of wz sge obtained by dttvm is surprisingly different from that built with the mem method. the difference in the regularization term could cause the different maps especially when the data sample is small. dttvm can reproduce the observed spectra with a high accuracy, even in the case that the mem method generate significant residuals in spectra. this indicates that tvm is probably a suitable regularization method for real doppler map, compared with mem. acknowledgement this work was supported by jsps kakenhi grant number 22540252 and 25120007. we appreciate comments and suggestions from dr. shiro ikeda. rem acknowledges support by fondecyt grant 1110347 and the basal centro de astrofisica y tecnologias afines (cata) pfb–06/2007. 1〈http://www.lx.it.pt/˜bioucas/twist/twist.htm〉 2〈http://home.hiroshima-u.ac.jp/uemuram/dttvm/〉 3〈http://www.mpa-garching.mpg.de/˜henk/〉 175 m. uemura et al. references [1] marsh, t. r. & horne, k. 1988, mnras, 235, 269 doi:10.1093/mnras/235.1.269 [2] marsh, t. r. 2001, in astrotomography, indirect imaging methods in observational astronomy, ed. h. m. j. boffin, d. steeghs, & j. cuypers (springer-verlag), 1 [3] tappert, c., mennickent, r. e., arenas, j., matsumoto, k., & hanuschik, r. w. 2003, a&a, 408, 651 [4] uemura, m., kato, t., nogami, d., & mennickent, r. e. 2013, pasj, submitted [5] bioucas-dias, j. m. & figueiredo, m. a. 2007b, in image processing, 2007. icip 2007. ieee international conference on vol. 1 (ieee), pp i–105 [6] bioucas-dias, j. m. & figueiredo, m. a. 2007a, image processing, ieee transactions on, 16, 2992 [7] nogami, d. & iijima, t. 2004, pasj, 56, 163 [8] spruit, h. c. 1998, arxiv:astro-ph/9806141 discussion dmitry kononov: 1. it’s nice that your method can restore flat features. 2. it’s in a sense incorrect to compare two results of inverse-problem solving methods if you have no physical basics under the structures you are trying to explain. makoto uemura: as you pointed out, both tvm and mem have no physical meaning. but, i think the comparison still makes a sense. we can select a better model based on residuals between observations and model. in the case of wz sge, the residuals obtained with our method are much smaller than those with mem. the mem method fails to reproduce the localized structures of the line profile, while our method can reproduce them. dmitry bisikalo: is it possible to use tvm in 3d doppler tomography? makoto uemura: yes, it is. the 3d doppler tomography is also a linear problem, so it is easy to apply the method to it. vx (km s−1) v y (k m s −1 ) −1000 0 +1000 − 10 00 0 + 10 00 original − 1 5 10 −1000 0 +1000 − 10 00 0 + 10 00 (a)logλ=−1.0 −1000 0 +1000 (b) logλ=−2.0 −1000 0 +1000 (c) logλ=−3.0 rv (km s−1) o rb ita l p ha se −2000 0 +2000 0. 0 0. 2 0. 4 0. 6 0. 8 1. 0 −2000 0 +2000 0. 0 0. 2 0. 4 0. 6 0. 8 1. 0 0 +2000 0 +2000 0 +2000 0 +2000 0 +2000 figure 1: results of dttvm using an artificial map having three spots. the artificial map is depicted in the upper left-most panel. the simulated spectra from the map is shown in the lower left-most panel. three sets of results are shown with different λ, which is indicated by the top of the figure. for each set, the estimated doppler map is shown in the upper panel. the lower left and right panels are the model spectra and residuals between the original and model spectra, respectively. 176 http://dx.doi.org/10.1093/mnras/235.1.269 application of total variation minimization to doppler tomography vx (km s−1) v y (k m s −1 ) −1000 0 +1000 − 10 00 0 + 10 00 (a) logλ=−2.2 vx (km s−1) v y (k m s −1 ) −1000 0 +1000 − 10 00 0 + 10 00 (b) logλ=−3.2 vx (km s−1) v y (k m s −1 ) −1000 0 +1000 − 10 00 0 + 10 00 (c) logλ=−5.2 rv (km s−1) o rb ita l p ha se −2000 0 +2000 1. 0 1. 5 2. 0 2. 5 rv (km s−1) −2000 0 +2000 1. 0 1. 5 2. 0 2. 5 rv (km s−1) −2000 0 +2000 1. 0 1. 5 2. 0 2. 5 rv (km s−1) −2000 0 +2000 1. 0 1. 5 2. 0 2. 5 rv (km s−1) −2000 0 +2000 1. 0 1. 5 2. 0 2. 5 rv (km s−1) −2000 0 +2000 1. 0 1. 5 2. 0 2. 5 figure 2: results of dttvm for the data of wz sge. upper panels: the doppler maps. lower left and right panels: the model spectra and residuals between the model and observed spectra, respectively. the three sets of the panels were calculated with different λ, which are indicated in the figure. vx (km s−1) v y (k m s −1 ) −1000 0 +1000 − 10 00 0 + 10 00 (a) logα=−1.0 vx (km s−1) v y (k m s −1 ) −1000 0 +1000 − 10 00 0 + 10 00 (b) logα=−2.0 vx (km s−1) v y (k m s −1 ) −1000 0 +1000 − 10 00 0 + 10 00 (c) logα=−3.0 rv (km s−1) o rb ita l p ha se −2000 0 +2000 1. 0 1. 5 2. 0 2. 5 rv (km s−1) −2000 0 +2000 1. 0 1. 5 2. 0 2. 5 rv (km s−1) −2000 0 +2000 1. 0 1. 5 2. 0 2. 5 rv (km s−1) −2000 0 +2000 1. 0 1. 5 2. 0 2. 5 rv (km s−1) −2000 0 +2000 1. 0 1. 5 2. 0 2. 5 rv (km s−1) −2000 0 +2000 1. 0 1. 5 2. 0 2. 5 figure 3: as in figure 2, but for the mem case. 177 introduction doppler tomography by total variation minimization model demonstrations using artificial data application to the data of wz sge summary 143 acta polytechnica ctu proceedings 2(1): 143–147, 2015 143 doi: 10.14311/app.2015.02.0143 model atmosphere spectrum fit to the soft x-ray outburst spectrum of ss cyg v. f. suleimanov1,2, c. w. mauche3, r. ya. zhuchkov2, k. werner1 1institute for astronomy and astrophysics, kepler center for astro and particle physics, eberhard karls university, sand 1, 72076 tübingen, germany 2kazan (volga region) federal university, kremlevskaya str. 18, 42008 kazan, russia 3lawrence livermore national laboratory, l-473, 7000 east ave., livermore, ca 94550, usa corresponding author: suleimanov@astro.uni-tuebingen.de abstract the x-ray spectrum of ss cyg in outburst has a very soft component that can be interpreted as the fast-rotating optically thick boundary layer on the white dwarf surface. this component was carefully investigated by mauche (2004) using the chandra letg spectrum of this object in outburst. the spectrum shows broad (≈ 5 å) spectral features that have been interpreted as a large number of absorption lines on a blackbody continuum with a temperature of ≈ 250 kk. because the spectrum resembles the photospheric spectra of super-soft x-ray sources, we tried to fit it with high gravity hot lte stellar model atmospheres with solar chemical composition, specially computed for this purpose. we obtained a reasonably good fit to the 60–125 å spectrum with the following parameters: teff = 190 kk, log g = 6.2, and nh = 8 · 1019 cm−2, although at shorter wavelengths the observed spectrum has a much higher flux. the reasons for this are discussed. the hypothesis of a fast rotating boundary layer is supported by the derived low surface gravity. keywords: cataclysmic variables dwarf novae radiation transfer x-rays individual: ss cyg ≡ bd+42◦ 4189a. 1 introduction ss cyg is one of the brightest cataclysmic variables (cvs), one of the best-studied dwarf nova stars (warner 1995), and was the first cv discovered in x-ray radiation (rappaport et al. 1974). the properties of the x-ray radiation of this close binary system have been extensively investigated, and are observed to be dramatically different in quiescence and in outburst. in quiescence, the x-ray spectrum is hard and can be described by an optically thin hot (kt ≈ 20 kev) plasma with an observed flux ≈ 2 · 10−10 erg s−1 cm−2. in outburst, this hard component decreases by a factor of ten, the plasma temperature is reduced to ∼ 6–8 kev, and an additional soft component appears with a blackbody temperature ≈ 200–300 kk (córdova et al. 1980; mcgowan et al. 2004; ishida et al. 2009). it is commonly accepted that the x-ray radiation of non-magnetic cvs arises in the boundary layer (bl) between the white dwarf (wd) and the accretion disc (pringle & savonije 1979; tylenda 1981; patterson & raymond 1985a, b; kley 1991), which are optically thick at high accretion rates (ṁ > 1016 g s−1) and optically thin at lower accretion rates. the soft x-ray spectrum of ss cyg in outburst was carefully investigated by mauche (2004) using a highresolution spectrum obtained with the chandra letg. he phenomenologically described the observed 40–130 å spectrum by a blackbody with temperature t ≈ 250 kk and numerous broad absorption features of ions of cosmically abundant o, ne, mg, si, s, and fe. the bl luminosity and wd spin were also evaluated in this work. on the other hand, this spectrum looks like the photospheric spectra of super-soft x-ray sources (lanz et al. 2005; rauch et al. 2010; van rossum 2012), so it probably could be described using the spectra of hot stellar model atmospheres. boundary layers possibly rotate with almost keplerian velocities and could have reduced (in comparison with wd) surface gravities close to the local eddington limit. therefore, we consider close to eddington limit models in the present work. here we present our attempt to fit the chandra letg spectrum of ss cyg using such model spectra. we also make estimates of the bl parameters in the context of our model fits. 2 model atmospheres the version of the lte computer code atlas (kurucz 1970; 1993), modified by us to deal with high temperatures (ibragimov et al. 2003; suleimanov & werner 2007), was used to model high temperature at143 http://dx.doi.org/10.14311/app.2015.02.0143 v. f. suleimanov et al. mospheres. in this code, local thermodynamic equilibrium (lte) is assumed and the pressure ionization effects using the occupation probability formalism (hummer & mihalas 1988) as described by hubeny et al. (1994) are taken into account. coherent electron scattering together with the free-free and bound-free transitions of all ions of the 15 most abundant elements using cross-sections from verner & yakovlev (1995) were adopted for the continuum opacity. line blanketing is also included using ∼ 25000 spectral lines from the chianti, version 3.0, atomic database (dere et al. 1997). 140 160 180 200 220 240 260 5.6 5.8 6.0 6.2 6.4 6.6 6.8 g < g edd lo g g t eff , kk 10-5 10-4 10-3 10-2 10-1 1 10 102 0 1 2 3 4 5 6 7 8 9 10 11 12 g ra d / g column density, g cm-2 t eff = 200 kk, log g = log g edd + 0.2 = 6.28 t eff = 200 kk, log g = log g edd + 0.4 = 6.48 t eff = 250 kk, log g = log g edd + 0.2 = 6.67 figure 1: top panel: positions of the computed model atmospheres in the teff–log g plane. the dashed curve demarcates the eddington limit (log g = log gedd). bottom panel: the relative radiation force vs. depth for various model atmospheres. twenty-two model atmospheres with solar chemical composition were computed using the described code. the effective temperatures of the models range between 150 kk and 250 kk with a step of 10 kk. two values of the surface gravity for each effective temperature, namely log g = log gedd +0.2 and log g = log gedd +0.4, were used. here log gedd = log(σe σsbt 4 eff/c) = 4.88 + 4 log(teff/105k) is the surface gravity that has an equal radiation pressure force for a given teff , and σe ≈ 0.34 cm2 g−1 is the electron scattering opacity for the assumed solar chemical composition. the positions of the computed models on the teff–log g plane are shown in fig. 1 (top panel). for the considered model atmospheres, a radiation pressure force grad due to spectral lines becomes larger than the surface gravity at the upper atmospheric layers (see fig. 1, bottom panel). to enforce hydrostatic equilibrium, we took a gas pressure equal to 10% of the total pressure (pgas = 0.1ptot) at all atmospheric layers where grad > g. as shown in fig. 2, the computed emergent spectra are dominated by a forest of absorption lines, and have to be convolved with the letg spectral resolution and the interstellar gas transmission to be compared with the observed spectrum of ss cyg (see fig. 3). the spectra of models with different surface gravities are sufficiently different to discriminate them from a comparison with the observed spectrum (see fig. 2, bottom panel). 40 60 80 100 1011 1012 1013 1014 1015 1016 1011 1012 1013 1014 1015 1016 log g = log g edd + 0.2 = 6.28 log g = log g edd + 0.4 = 6.48 t eff = 200 kk h , er g cm -2 s-1 a -1 wavelength, a t eff = 150, 200, 250 kk log g = log g edd + 0.2 h , er g cm -2 s-1 a -1 figure 2: top panel: emergent spectra of three model atmospheres with the same log g = log gedd + 0.2 and various effective temperatures: 150 kk (solid curves), 200 kk (dashed curves), and 250 kk (dotted curves). bottom panel: emergent spectra of two model atmospheres with the same effective temperature (200 kk) and different log g. 3 results the model spectra convolved with the chandra letg spectral resolution ∆λ = 0.05 å were used to fit the observed soft x-ray spectrum of ss cyg. the interstellar absorption (with the hydrogen column number den144 model atmosphere spectrum fit to the soft x-ray outburst spectrum of ss cyg sity nh as a fitting parameter) was also taken into account. the observed spectrum was fitted in the 60–125 å wavelength range because at the shorter wavelengths our model spectra could be incorrect (see next section). the best-fit model parameters are teff = 190 kk, nh = 8·1019 cm−2, and normalization k = 7.82·10−26, and correspond to the models with the lower surface gravity log g = log gedd + 0.2. the reduced χ2 = 3.9 is relatively large, hence the formal parameter errors are large, too, and we have not attempted to determine them. the best-fit model spectrum together with the observed spectrum is shown in fig. 3. the contours of χ2 on the teff–lognh parameter plane are shown in fig. 4. the normalization can be expressed as k = fr2 wd/d 2 where d is the distance to ss cyg and f is the wd fractional area occupied by the bl, which can be expressed as the relative bl extension along the wd surface f ≈ (2πrwd 2hbl)/(4πr2 wd) = hbl/rwd. the basic properties of the bl can be derived from the obtained fit parameters. using the same system and wd parameters as used by mauche (2004) — mwd = 1 m�, rwd = 5.5 · 108 cm (therefore, model log g = 8.46), d = 160 pc, and an accretion disk bolometric luminosity in outburst ldisk = 1035 erg s−1 — we obtain the fractional area of the bl f = 6.3 · 10−2 (5 · 10−3), the bolometric bl luminosity lbl = 1.8 · 1034 (5 · 1033) erg s−1, and the relative bl luminosity lbl/ldisk = 0.18 (0.05), where the best-fit parameter values obtained by mauche (2004) are shown in parentheses for comparison. the spin period of the wd in ss cyg is 12 (9) s as inferred using the relation between the bl and accretion disk luminosities (kluźniak 1987; kley1991) lbl/ldisk = [1 − ωwd/ωk(rwd)]2, (1) where ωk(rwd) is the kepler angular velocity at the wd radius. the accepted model gravity on the wd surface in ss cyg (log gwd = 8.46) is more than two orders of magnitude higher than the obtained bl effective surface gravity log geff = 6.2. the surface gravity of the bl can be reduced only by fast rotation of the accreting matter geff = gwd − ω2 blrwd (2) = gwd (1 − [ωbl/ωk(rwd)]2). therefore, a relative bl angular velocity ωbl/ωk(rwd) ≈ 0.98 was obtained using this relation. figure 3: the chandra letg spectrum of ss cyg in outburst (thick black curve) and the best-fit model atmosphere spectrum with teff = 190 kk, log g = 6.2, and lognh = 19.9 (thin red curve). the fitting was performed in the 60–125 å wavelength range. the model spectrum at shorter wavelengths is shown by the dashed red curve. figure 4: position of the best-fit model in the teff–lognh parameter plane and contours of χ2 = [1.5, 3, 6]χ2 min. 4 discussion and conclusion we present here the results of fitting the ss cyg chandra letg spectrum in outburst with model atmosphere spectra. the obtained best fit model spectrum does not describe the observed spectrum at short wavelengths (< 60 å) and in the 82–90 å wavelength region and, therefore, it is not statistically acceptable (χ2/dof = 3.9). these deficiencies can be connected with model shortcomings: the most important ignored effect is atmosphere expansion due to a spectral linedriven stellar wind. this expansion can be significant 145 v. f. suleimanov et al. because grad > g at the outer layers of our model atmospheres (see also van rossum 2012). in addition, non-lte effects could be important (see, e.g., rauch et al. 2010), the chemical composition may differ from solar, and, finally, the atomic data are almost certainly neither complete nor entirely accurate. the second important shortcoming is connected with a likely complicated bl structure with a distribution of effective temperatures and surface gravities over its surface. therefore, a simple one-zone bl model presented here is most probably insufficient and more sophisticated bl models have to be considered. nevertheless, the spectral modeling presented here supports a bl in ss cyg that is, to first approximation, a hot (≈ 190 kk), fast rotating [ωbl ≈ 0.98 ωk(rwd)], narrow (hbl ≈ 0.063rwd) belt on the wd surface. acknowledgement this work is supported by the dfg sfb / transregio 7 “gravitational wave astronomy” (v.s.) and the russian foundation for basic research (grant 12-02-97006r-povolzhe-a) (r.zh.). c.w.m.’s contribution to this work was performed under the auspices of the u.s. department of energy by lawrence livermore national laboratory under contract de-ac52-07na27344. references [1] córdova, f. a., chester, t. j., tuohy, i. r., & garmire, g. p. 1980, apj, 235, 163 [2] dere, k. p., landi, e., mason, h. e., monsignori fossi, b. c., & young, p. r. 1997, a&ass, 125, 149 [3] hubeny, i., hummer, d. g., & lanz, t. 1994, a&a, 282, 151 [4] hummer, d. g., & mihalas, d. 1988, apj, 331, 794 doi:10.1086/166600 [5] ibragimov, a. a., suleimanov, v. f., vikhlinin, a., & sakhibullin, n. a. 2003, astronomy reports, 47, 186 doi:10.1134/1.1562213 [6] ishida, m., okada, s., hayashi, t., nakamura, r., terada, y., mukai, k., & hamaguchi, k. 2009, pasj, 61, 77 [7] kley, w. 1991, a&a, 247, 95 [8] kluźniak, w. 1987, ph.d. thesis, stanford univ. [9] kurucz, r. l. 1970, sao special report, 309 [10] mauche, c. w. 2004, apj, 610, 422 [11] mcgowan, k. e., priedhorsky, w. c., & trudolyubov, s. p. 2004, apj, 601, 1100 doi:10.1086/380758 [12] patterson, j., & raymond, j. c. 1985a, apj, 292, 535 doi:10.1086/163187 [13] patterson, j., & raymond, j. c. 1985b, apj, 292, 550 doi:10.1086/163188 [14] pringle, j. e., & savonije, g. j. 1979, mnras, 187, 777 doi:10.1093/mnras/187.4.777 [15] rauch, t., orio, m., gonzales-riestra, r., nelson, t., still, m., werner, k., & wilms, j. 2010, apj, 717, 363 doi:10.1088/0004-637x/717/1/363 [16] rappaport, s., cash, w., doxsey, r., mcclintock, j., & moore, g. 1974, apj, 187, l5 doi:10.1086/181378 [17] suleimanov, v., & werner, k. 2007, a&a, 466, 661 [18] tylenda, r. 1981, acta astr., 31, 267 [19] van rossum, d. r. 2012, apj, 756, 43 [20] verner, d. a., & yakovlev, d. g. 1995, a&ass, 109, 125 [21] warner, b. 1995, cambridge astrophysics series, 28 discussion dmitry kononov: what is a reason to initially use the solar chemical composition instead of chemical compositions for stars of later spectral type? valery suleimanov: unfortunately, we do not know the chemical composition of the secondary in ss cyg. therefore, we started from the most conservative case, which is the solar chemical composition. jan-uwe ness: the assumed wd mass in the model (1 m�) seems discrepant from the mass given in the introduction (0.55 m�), a factor 2. this suggest that all parameters of the model may be discrepant from reality, so what do we learn? valery suleimanov: sorry, you mixed up the white dwarf mass with the mass of the secondary (0.55 m�). dmitry bisikalo: how can you discriminate between a boundary layer and a pseudo-photosphere or a hot disk halo? 146 http://dx.doi.org/10.1086/166600 http://dx.doi.org/10.1134/1.1562213 http://dx.doi.org/10.1086/380758 http://dx.doi.org/10.1086/163187 http://dx.doi.org/10.1086/163188 http://dx.doi.org/10.1093/mnras/187.4.777 http://dx.doi.org/10.1088/0004-637x/717/1/363 http://dx.doi.org/10.1086/181378 model atmosphere spectrum fit to the soft x-ray outburst spectrum of ss cyg valery suleimanov: the observed soft xray luminosity is a discrimination factor. any pseudophotosphere or an optically thick hot disk halo with this low surface gravity (log g ≈ 6.2) and the derived effective temperature (≈ 190 kk) would have a radius that is tens of times larger than the white dwarf radius, and the luminosity would be hundreds of times larger than the observed luminosity. 147 introduction model atmospheres results discussion and conclusion acta polytechnica ctu proceedings doi:10.14311/app.2017.10.0065 acta polytechnica ctu proceedings 10:65–68, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app landslide reclamation in šárka valley martin vaníček geosyntetika s.r.o., nikoly tesly 3, prague 6, czech republic correspondence: mvanicek@geosyntetika.cz abstract. housing development in šárka’s valley is situated in former brickworks borrow pit for brick-clay. on its north side the borrow pit cutting is up to 8m high with main road on top. this slope was suffering from progressive landslide mainly due to weathering and surface erosion. the reclamation works proposed and afterwards executed consisted of stabilizing the slope by combination of soil nailing and connecting reinforced slope with surcharge bench at its toe. the final reinforced soil structure nicely merged into the surrounding environment. keywords: landslide reclamation, muralex stone facing system, reinforced soil structure. 1. introduction main task of this project was to design and later to execute the reclamation of landslide below the edge of horoměřická street. the slope is part of housing development project top residence šárecké údolí. this development project is situated in the area of former brickworks. the slope that has been progressively collapsing was up to 8m height with the slope as steep as 1:1. the progressive collapse was initiated by climatic degradation of brick clay and surface erosion on the steep slope. 2. geotechnical conditions in the area of the whole development project the geotechnical investigation has been performed. several boreholes and trial pits have been used to determine the geological structure of the area. as is typical for such projects the soil properties have been suggested from the index tests performed on few disturbed samples taken and from the description of soils encountered during exploratory works. in the area of landslide additional gi was undertaken, however again without determination of shear strength of encountered soils. based on the above information simple geotechnical model was determined. on site bedrock from weathered clayey shales was found, categorised as r5 based on czech code of practise. the depth to weathered bedrock was indicated between 1 and 4 m with respect to the borehole location within the slope. the shales were overlaid by clayey sandy silt (brick clay), based on classification cs sandy clay firm to stiff consistency. near the surface a layer with organic content was present. shear strength properties of soils have been selected with respect to eurocode 7 guidelines as very cautious value from tabled values of soil properties in discontinued czech code of practise čsn 731001. for the construction of new earth structure body, it was in the design assumed to use local soils from basement excavation for houses. also for recompacted soils from excavations the tests for determination of shear strength haven’t been performed, therefore their characteristic properties have been selected as very cautious values from tabled soil properties in čsn 752410, czech code of practise for earth dams. selected characteristic soil properties for reinforced soil structures are presented in table 1 below. based on above mentioned investigation typical cross section through land slide has been created and assumed location of slip surface together with individual soil layers has been indicated in fig. 1. ground water level has been found under the slope relatively shallow, about 1m below ground level. in the borehole 5.5 m deep from top of the slope, ground water hasn’t been found. this indicates that ground water level does not copy the ground surface and is rather naturally gradual. 3. proposed solution in accordance with proposed development project the bottom line of reclamation is defined by edge of unbound cycleway. in order to guarantee required stability of the reclaimed slope, it’s inclination is proposed at 1:1.75 1:2.00 with reinforcement in 1 m spaced layers. due to limited space, the slope has to be ended by retaining wall with max. height of 1.6 m. based on main architect requirement the retaining wall should have gabion facing. at the top edge of the slope, it was not possible to do any large excavations, as there is situated highly trafficked street horoměřická. in order to cut through the potential slip surface, driven soil nails in 1m vertical and 1.5 m horizontal spacing inclined by 60° from horizontal have been proposed. these soil nails from 50 × 6.3 mm steel pipe with 1. 5m length have been located into the steps in existing slope excavations created for better connection with new slope. stability of the new slope is maintained by reinforcing geogrids fortrac® mpt, with vertical spacing of 0.5 m or 1 m depending on the position in the slope. 65 http://dx.doi.org/10.14311/app.2017.10.0065 http://ojs.cvut.cz/ojs/index.php/app martin vaníček acta polytechnica ctu proceedings table 1. characteristic soil properties assumed. figure 1. cross section of collapsed slope with indicated assumed geotechnical layers and slipped surface. the length of geogrids is given between slope face and steps in existing ground, where they are connected to the soil nails by nail heads. the base retaining wall with vertical gabion type facing was designed as muralex® stone system. above the base retaining wall drainage channel was created to drain the surface water from the slope. on eastern side the reclamation is framed by the underpass under the horoměřická street with brick cladding of the steep slope above the underpass portal (see visualization on fig. 2). slope above portal wing wall is again retained by max. 3 m high retaining wall with muralex® stone system. the western side of slope reclamation is framed by newly planned staircase. the level difference between existing slope and reclaimed slope towards the planned staircase is proposed as reinforced steep slope (4:1) with muralex® green system, which provides vegetated surface. figure 2. visualization of reclaimed slope integration into the existing terrain design solution has been developed in accordance to eurocode 7, namely based on experience. typical cross section through reclaimed slope is shown in fig. 3. 66 vol. 10/2017 landslide reclamation in šárka valley figure 3. typical cross section through the reclaimed collapsed slope 4. reclamation execution next to design solution the developer and main contractor of the whole housing development asked us to also take care about the execution of reclamation works. the actual conditions have proven the design assumptions, except the shallower depth of weathered shales close to slope base, where we have some problems with nails driving. this issue was easily solved by shortening of the nails, which does not influence the overall stability. in the upper part the soil nails have been driven well behind the assumed slip surface, along which the slope most probably earlier collapsed. another emerged issue in lack of locally available soil was again easily solved by importing of the suitable soil. this imported soil was tested in lab for shear strength and compaction efficiency by proctor standard test including the optimal moisture content for compaction. reclamation was executed according to plan also due to highly permitting weather. wall from reinforced soil was build using wrap around technique, when individual layers have been compacted against mobile formwork (see fig. 4). at each geogrid layer, anchoring elements have been installed for future connection of muralex® facing elements. at these layers were also installed driven figure 4. formwork for proper compaction of reinforced soil structure with wrap-around facing in the facing area. soil nails and connected to the geogrids strips with help of nail heads (see fig. 5). above the base retaining wall new slope was built with the inclination in between 1:1.75 and 1:2.00 based on space availability. the soil was compacted by plate and ditch roller and compaction quality was tested by light dynamic plate test. once the slope was built and ramp for machinery access removed, attached front facing muralex® system was installed (see fig. 6). in locations with vertical facing, the system was filled with stones 63/125 mm and in locations with 4:1 slope facing, sieved organic soil filling was used. lastly the slope 67 martin vaníček acta polytechnica ctu proceedings figure 5. connection of reinforcing geogrids fortrac® mpt and driven soil nails figure 6. attached front facing system muralex® before 63/125 mm stone filling was covered with topsoil and temporary erosion protection mesh from coconut fibres. afterwards the whole slope surface was covered by grass seeds. already figure 7. overall view on the finished reclaimed slope, where grassing can be seen after couple of days the slope started to be nicely grassed (see fig. 7). 5. summary finally it can be concluded that even at confined conditions it is possible to reclaim collapsed slope by appropriate combination of soil reinforcement techniques soil nailing and soil reinforcement by fortrac® mpt geogrids. the final visual perception nicely implemented the reclaimed slope into high standard housing development. the system of attached front facing muralex® creates aesthetic element, which can be during the lifetime of reinforced soil structure repaired or modified from whatever reasons (e.g. accident, change of aesthetic feeling, . . . ) without compromising the main retaining soil structure. 68 acta polytechnica ctu proceedings 10:65–68, 2017 1 introduction 2 geotechnical conditions 3 proposed solution 4 reclamation execution 5 summary 152 acta polytechnica ctu proceedings 2(1): 152–155, 2015 152 doi: 10.14311/app.2015.02.0152 evolution and outbursts of cataclysmic variables s.-b. qian1,2,3, l.-y. zhu1,2,3, e.-g. zhao1,2, e. fernández lajús4,5, j. zhang1,2, g. shi1,2, z.-t. han1,2 1yunnan observatories, chinese academy of science, p. o. box 110, 650011 kunming, china 2key laboratory for the structure and evolution of celestial objects, chinese academy of sciences, 650011 kunming, china 3university of the chinese academy of sciences, yuquan road 19#, sijingshang block, 100049 beijing, china 4facultad de ciencias astronómicas y geof́ısicas, universidad nacional de la plata, 1900 la plata, buenos aires, argentina 5instituto de astrofisica de la plata (cct la plata conicet/unlp), argentina corresponding author: qsb@ynao.ac.cn abstract mass transfer and accretion are very important to understand the evolution and observational properties of cataclysmic variables (cvs). due to the lack of an accretion disk, eclipsing profiles of polars are the best source to study the character of mass transfer in cvs. by analyzing long-term photometric variations in the eclipsing polar hu aqr, the property of mass transfer and accretion are investigated. the correlation between the brightness state change and the variation of the ingress profile suggests that both the accretion hot spot and the accretion stream are produced instantaneously. the observations clearly show that it is the variation of mass transfer causing the brightness state changes that is a direct evidence of variable mass transfer in a cv. it is shown that it is the local dark-spot activity near the l1 point to cause the change of the mass transfer rather than the activity cycles of the cool secondary star. our results suggest that the evolution of cvs is more complex than that predicted by the standard model and we should consider the effect of variable mass accretion in nova and dwarf nova outbursts. keywords: cataclysmic variables polars photometry individual: hu aqr, dp leo, mn hya, and v2301 oph. 1 introduction cataclysmic variables (cvs) are semi-detached binaries where a low-mass (spectral types of k and m) component star transfers mass to a white dwarf (e.g., warner 1995). according to the standard theory of cvs, the evolution of long-period (p > 3 hours) cvs are driven by angular momentum loss (aml) via magnetic braking (mb), and the ”period gap” (the apparent scarcity of cvs in the period range from 3 to 2 hours) was explained as the cessation of the mb at the period of 3 hours when the secondary component becomes completely convective (e.g., rappaport et al. 1983; spruit & ritter 1983). cvs below the ”period gap” are governed by gravitational radiation. cvs as a mass transferring binary, the aml should keep the secondary filling the critical roche lobe and transferring mass to the white dwarf continuously. in this way, cvs will evolve from a higher mass secondary with longer period to a lower mass secondary with shorter period. mass transfer and accretion in cvs are very important to understand their evolution and observational properties (e.g., the novae and dwarf-novae outbursts). most cvs (e.g., polars and some dwarf novae and novalike cvs) usually show brightness changes in high state, intermediate and low states. the most possible reason to cause these changes is the variation of mass transfer. however, direct evidence is lacking because of the influence of an accretion disk in a normal (non-magnetic) cv. in a polar (magnetic cv), the magnetic field of the white dwarf is very strong to prevent the formation of an accretion disk (e.g., giovannelli & sabau-graziati 2012). the transferred material from the secondary is quickly and directly accreted onto the white dwarf. during the eclipses, light components from the accretion stream and spot on the white dwarf can be isolated. therefore, eclipsing polars can provide invaluable information on the character of mass transfer. the changes of eclipsing profiles directly reflect the variations in the mass-transfer rate. the results will shed light on our understanding of several key astrophysical problems such as the high and low brightness state 152 http://dx.doi.org/10.14311/app.2015.02.0152 evolution and outbursts of cataclysmic variables changes and dwarf nova outbursts. however, only a few polars were monitored photometrically including the brightest polar am her (e.g., hessman et al. 2000; kafka & honeycutt 2003, 2005; wu & kiss 2008), no eclipsing polars were monitored for a long time (e.g., up to several years) before. on the other hand, the eclipse times of eclipsing polars can be determined with a high precision because the accretion stream and the hot spot on the white dwarf can be isolated during the eclipses. very smallamplitude cyclic changes in the observed-calculated (oc) diagram can be detected. therefore, they are also good targets to search for planets and brown dwarfs orbiting cvs by analyzing the light travel time effect. some substellar objects were recently discovered to be orbiting the polars dp leo and hu aqr (qian et al. 2010a, 2011). by using the same method, planets orbiting other evolved binaries were discovered. some examples discovered by our group are those orbiting the detached white-dwarf binaries qs vir and rr cae (qian et al. 2010b, 2012a) and the subdwarf b-type binary ny vir (qian et al. 2012b). 2 targets and observations we have selected ten eclipsing polars, dp leo, ep dra, v2301 oph, ek uma, hu aqr, uz for, v1432 aql, mn hya, v1309 ori, and sdss j015543.40+002807.2, for monitoring photometrically. we monitored those sample stars since 2009 by using the 2.4-m and 1.0m telescopes at yunnan observatories in china and the 2.15-m jorge sahade telescope at complejo astronomico el leoncito (casleo), san juan, argentina. more than 100 eclipse profiles of the selected polars were observed. the eclipse profile for the eclipsing polar, v2301 ophshown in fig. 1. it was obtained on feb. 15, 2012 by using the 2.4-m telescope in lijiang observational station of yunnan observatories. during the observation, no filters were used. among the selected eclipsing polars, we pay more attention to hu aqr. it is one of the brightest eclipsing polars at both optical and x-ray wavelengths. this polar is a total eclipsing binary with an orbital inclination of i = 87◦ and has only one accretion pole (e.g., schwope et al. 2001). all these make it the most ideal target to investigate the properties of mass transfer through the long-term photometry. we have monitored it since 2009 and nearly 70 eclipse profiles were obtained. 3 direct evidence for mass transfer and accretion two of white-light eclipse profiles of hu aqr obtained at high and low brightness states are shown in fig. 2. as shown in the figure, the eclipses start with the limb of the red-dwarf component eclipsing the hot spot (accretion region), and the primary is also eclipsed nearly at the same time. then the accretion stream is the dominant source of the brightness with a small contribution of the secondary, and the distortion in the ingress profile is visible. finally, only the red dwarf is visible and provides a constant contribution at the bottom of the eclipse. 73.440 73.443 73.446 73.449 73.452 73.455 73.458 3.0 2.5 2.0 1.5 1.0 0.5 0.0 -0.5 -1.0 figure 1: white-light photometric observations of v2301 oph obtained on feb. 15, 2012 by using the 2.4m telescope in lijiang observational station of yunnan observatories. solid dots refer to the magnitude differences between v2301 oph and the comparison star, while open circles to those between the comparison and the check stars. -0.10 -0.05 0.00 0.05 0.10 0.15 0.20 4.0 3.5 3.0 2.5 2.0 1.5 1.0 0.5 0.0 figure 2: comparison of two eclipse profiles for hu aqr at high and low brightness states, respectively. the two eclipse profiles were obtained in 2011 by using the 2.4-m telescope in yunnan observatories. the sequence of the egress process is approximately reversed. as displayed in fig. 2, the egress profile of hu aqr is rather stable. therefore, the mid-egress times were used to detect two planetary objects orbiting this binary star by analyzing the light travel time 153 s.-b. qian et al. effect (qian et al. 2011) and the new eclipse times will be used to revise the parameters of the circumbinary planets. as shown in fig. 2, when hu aqr is at a high brightness state, the distortion in the ingress profile is visible. these properties suggest that there is an accretion stream from the secondary to the white-dwarf component and at the same time we see a hot spot on the white dwarf. both the existences of the accretion stream and the hot spot indicate a high mass accretion rate at high brightness state. on the other hand, at a low brightness state, the distortion in the ingress profile disappeared and the eclipse profiles are symmetric. these can be explained as the results that no hot spots on the white dwarf and no accretion streams are seen between the component indicating that no mass transfers and accretions between both components. the brightness variation is correlated with the change of the eclipse profile suggesting that both the hot spot and the accretion stream are produced instantaneously. this is a direct evidence of variable mass transfer and accretion in the cv. two eclipse profiles at high brightness states are plotted in fig. 3. the two eclipse profiles were observed on may 29 and 31,2011 with the 2.15-m jorge sahade telescope in argentina. as displayed in the figure, both the brightness before the eclipse and the ingress profile are variable in two days. other two eclipse profiles obtained in 2010 by using the 1.0-m telescope in yunnan observatories are displayed in fig. 4. it is shown in the figure that hu aqr is on the way from a high state to a low state indicating that the rate of mass transfer is decreasing. 4 discussion and conclusions the observations in previous section give a direct evidence for variable mass transfer and accretion in cvs. the orbital period of hu aqr is about 2.08 hours, just below the cv period gap. non-magnetic cvs with orbital periods in this range are usually dwarf novae (dn). two dwarf novae, ir com and dv uma, have the nearly same orbital period as that of the eclipsing polar hu aqr. they show dn outbursts (a sudden increase of brightness up to 2-7 magnitudes) at usually irregular intervals (nogami et al., 2001). their dn outbursts are explained as the disc instability (cannizzo 1993). however, it is not clear that the outbursts are pure disc phenomena that occur without some contribution of variable mass transfer from the secondary (livio & verbunt, 1988; duschl & livio, 1989). our conclusions suggest that we should consider the contribution of mass transfer in the model of cv outbursts (e.g., cannizzo 1993). the evolution of cvs may be more complex than that predicted by the standard model. -0.20 -0.15 -0.10 -0.05 0.00 0.05 0.10 0.15 0.20 4.5 4.0 3.5 3.0 2.5 2.0 1.5 1.0 oct 22, 2010 figure 3: white-light eclipse profiles observed with the 1.0-m telescope in yunnan observatories. open circles refer to the data obtained on oct. 22, 2010, while solid dots to those obtained on oct. 30. some physical mechanisms, such as irradiationdriven mass transfer and star-spots cause (e.g., wu et al., 1995; livio & pringle 1994), have been proposed to explain the changes of mass transfer in cvs. to solve this question, we analyzed the brightness variation around phase 0.5. it is discovered that the brightness from phase 0.3 to 0.65 usually shows a large dip at low states when the mass transfer rate is very low. two of the light curves obtained at low states are shown in fig. 5 where a large dip is seen around phase 0.5. these brightness dips can be explained by the presence of dark spots near the l1 point on the cool secondary star. this conclusion indicates that it is the coverage of dark spots near l1 point that produce the decrease of the mass transfer rate. 3.52 3.53 3.54 3.55 3.56 3.57 3.58 3.59 3.60 4.5 4.0 3.5 3.0 2.5 2.0 1.5 1.0 0.5 4.51 4.52 4.53 4.54 4.55 4.56 4.57 4.58 4.59 4 3 2 1 figure 4: two light curves of hu aqr observed at low brightness states with the 2.15-m jorge sahade telescope in argentina. it is shown that the brightness around phases 0.5 shows a large dip. the light curve in the left was obtained on nov. 11, 2011, while that in the right was obtained on nov. 12. at the bottom of the eclipse, all of the hot spot, the white dwarf, and the accretion stream are eclipsed by 154 evolution and outbursts of cataclysmic variables the secondary. only the red-dwarf component is visible and provides a constant contribution. therefore, it is the only chance to measure the brightness change of a mass donor in a cv. a cyclic variation in the brightness of the secondary is discovered that can be explained as the dark-spot activity cycle. it is the first time to detect an activity cycle for a fast-rotating mass donor in a cv. our results reveal that the variable mass accretion is not caused by magnetic activity cycles of the fast-rotating red dwarf. acknowledgement this work is supported by chinese natural science foundation through a key project (no.11133007). new ccd photometric observations of those eclipsing polars were obtained with the 2.4-m and 1.0-m telescopes at yunnan observatories (yno) in china and the 2.15-m ”jorge sahade” telescope in argentina. references [1] cannizzo, j. k., 1993, apj 419, 318 [2] duschl, w. j. & livio, m., 1989, a&a 209, 183 [3] giovannelli, f. & 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lajus, e., baume, g. l., 2012a, mnras 422, l24 doi:10.1111/j.1745-3933.2012.01228.x [14] qian s.-b., zhu l.-y., dai z.-b., fernández lajús, e., xiang f.-y., and he, j.-j., 2012b, apj 745, l23 doi:10.1088/2041-8205/745/2/l23 [15] rappaport, s., verbunt, f., joss, p. c., 1983, apj 275, [16] schwope, a. d., schwarz, r., sirk, m., howell, s. b., 2001, a&a 375, 419 [17] spruit, h. c., & ritter, h., 1983, a&a 124, 267 [18] warner, b., 1995, cataclysmic variable stars, cambridge univ. press, cambridge [19] wu, k. & kiss, l. l., 2008, a&a 481, 433 [20] wu, k., wickramasinghe, d. t., warner, b., 1995, pasa 12, 60 discussion k. reinsch: which filters did you use for your photometry? could you see a colour dependence in the orbital variation as would be expected for a light curve contribution originating from the secondary? qian shengbang: since we need high time resolution for our data, the exposure time is only a few seconds. therefore, no filters were used during the observations. 155 http://dx.doi.org/10.1086/174202 http://dx.doi.org/10.1093/mnras/232.1.1p http://dx.doi.org/10.1046/j.1365-8711.2001.04114.x http://dx.doi.org/10.1088/2041-8205/708/1/l66 http://dx.doi.org/10.1111/j.1745-3933.2009.00780.x http://dx.doi.org/10.1111/j.1745-3933.2011.01045.x http://dx.doi.org/10.1111/j.1745-3933.2012.01228.x http://dx.doi.org/10.1088/2041-8205/745/2/l23 introduction targets and observations direct evidence for mass transfer and accretion discussion and conclusions 139 acta polytechnica ctu proceedings 1(1): 139–145, 2014 139 doi: 10.14311/app.2014.01.0139 latest results from the fermi gamma-ray telescope aldo morselli1 1infn roma tor vergata corresponding author: aldo.morselli@roma2.infn.it abstract can we learn about new physics with astronomical and astro-particle data? since its launch in 2008, the large area telescope, onboard of the fermi gamma-ray space telescope, has detected the largest amount of gamma rays in the 20 mev 300 gev energy range and electrons + positrons in the 7 gev1 tev range, opening a new observational window on a wide variety of astrophysical objects. keywords: gamma ray gamma ray detectors dark matter. 1 introduction the fermi observatory carries two instruments onboard: the gamma-ray burst monitor (gbm) [1] and the large area telescope (lat) [2]. the lat is a pair conversion telescope for photons above 20 mev up to a few hundreds of gev. the field of view is ∼2.4 sr and lat observes the entire sky every ∼ 3 hours (2 orbits). these features make the lat a great instrument for dark matter (dm) searches. the operation of the instrument through the first three years of the mission was smooth at a level which is probably beyond the more optimistic prelaunch expectations. the lat has been collecting science data for more than 99% of the time spent outside the south atlantic anomaly (saa). the remaining tiny fractional down-time accounts for both hardware issues and detector calibrations [4], [5]. more than 650 million gamma-ray candidates (i.e. events passing the background rejection selection) were made public and distributed to the community through the fermi science support center (fssc) 1. over the first three years of mission the lat collaboration has put a considerable effort toward a better understanding of the instrument and of the environment in which it operates. in addition to that, a continuous effort was made to in order to make the advances public as soon as possible. in august 2011 the first new event classification (pass 7) since launch was released, along with the corresponding instrument response functions (and a release of a new event class ’pass 7 reprocessed’ is planned for the near future). compared with the prelaunch (pass 6) classification, it features a greater and more uniform exposure, with a significance enhancement in acceptance below 100 mev. the fermi lat results on the extragalactic sky will be covered by benoit lott [3]. here we will present the main results regarding the indirect dark matter searches and the origin of cosmic rays. 2 indirect dark matter searches one of the major open issues in our understanding of the universe is the existence of an extremely-weakly interacting form of matter, the dark matter, supported by a wide range of observations including large scale structures, the cosmic microwave background and the isotopic abundances resulting from the primordial nucleosynthesis. complementary to direct searches being carried out in underground facilities and at accelerators, the indirect search for dm is one of the main items in the broad fermi science menu. the word indirect denotes here the search for signatures of weakly interactive massive particle (wimp) annihilation or decay processes through the final products (gammarays, electrons and positrons, antiprotons) of such processes. among many other ground-based and spaceborne instruments, the lat plays a prominent role in this search through a variety of distinct search targets: gamma-ray lines, galactic and isotropic diffuse gamma-ray emission, dwarf satellites, cr electrons and positrons. 2.1 galactic center the galactic center (gc) is expected to be the strongest source of γ-rays from dm annihilation, due to its coincidence with the cusped part of the dm halo density profile [10], [11], [12]. a preliminary analysis of the data, taken during the first 11 months of the fermi satellite operations is presented in [13], [14]. 1the fssc is available at http://fermi.gsfc.nasa.gov/ssc 139 http://dx.doi.org/10.14311/app.2014.01.0139 aldo morselli figure 1: derived 95% c.l. upper limits on wimp annihilation cross sections in the milky way halo, for the muon (left) and tau (right) annihilation channels. the purple and blue contours show pamela and fermi positron excess dm interpretation constraint regions. the diffuse gamma-ray backgrounds and discrete sources, as we know them today, can account for the large majority of the detected gamma-ray emission from the galactic center. nevertheless a residual emission is left, not accounted for by the above models [13], [14]. improved modeling of the galactic diffuse model as well as the potential contribution from other astrophysical sources (for instance unresolved point sources) could provide a better description of the data. analyses are underway to investigate these possibilities. 2.2 galactic halo in order to minimize uncertainties connected with the region of the galactic center, analysis [15] considered a region of interest consisting of two off-plane rectangles (5◦ ≤ |b| ≤ 15◦ and |l| ≤ 80◦) and searched for continuum emission from dark matter annihilation or decay in the smooth galactic dark matter halo. they considered two approaches: a more conservative one in which limits were set on dm models assuming that all gamma ray emission in that region might come from dark matter (i.e. no astrophysical signal is modeled and subtracted). in a second approach, dark matter source and astrophysical emission was fit simultaneously to the data, marginalizing over several relevant parameters of the astrophysical emission. as no robust signal of dm emission is found, dm limits are set. these limits are particularly strong on leptonic dm channels, which are hard to constrain in most other probes (notably in the analysis of the dwarf galaxies, described below). this analysis strongly challenges dm interpretation [16] of the positron rise, observed by pamela [17] and fermi lat [18, 19] (see figure 1). 2.3 dwarf galaxies dwarf satellites of the milky way are among the cleanest targets for indirect dark matter searches in gamma-rays. they are systems with a very large mass/luminosity ratio (i.e. systems which are largely dm dominated). the lat detected no significant emission from any of such systems and the upper limits on the γ-ray flux allowed us to put very stringent constraints on the parameter space of well motivated wimp models [20]. a combined likelihood analysis of the 10 most promising dwarf galaxies, based on 24 months of data and pushing the limits below the thermal wimp cross section for low dm masses (below a few tens of gev), has been recently performed [21]. the main advantages of the combined likelihood are that the analysis can be individually optimized and that combined limits are more robust under individual background fluctuations and under individual astrophysical modelling uncertainties than individual limits. the derived 95% c.l. upper limits on wimp annihilation cross sections for different channels are shown in figure 2 (top). the most generic cross section (∼ 3 · 10−26cm3s−1 for a purely s-wave cross section) is plotted as a reference. these results are obtained for nfw profiles [22] but for cored dark matter profiles the j-factors for most of the dsphs would either increase or not change much so these results includes j-factor uncertainties [21]. with the present data we are able to rule out large parts of the parameter space where the thermal relic density is below the observed cosmological dark matter density and wimps are dominantly produced non-thermally, e.g. in models where supersymmetry breaking occurs via anomaly mediation for the mssm model [20]. future improvements (apart from increased amount of data) will include an improved event selection with a larger effective area and photon energy range, and the inclusion of more satellite galaxies. in figure 2 (bottom) are shown the predicted upper limits in the hypothesis of 10 years of data instead of 2; 30 dsphs in140 latest results from the fermi gamma-ray telescope stead of ten (supposing that the new optical surveys will find new dsph); spatial extension analysis (source extension increases the signal region at high energy e ≥ 10 gev,m ≥ 200 gev). figure 2: derived 95% c.l. upper limits on wimp annihilation cross sections for different channels. down: predicted 95% c.l. upper limits on wimp annihilation cross sections in 10 years for bbar channel. other complementary limits were obtained with the search of possible anisotropies generated by the dm halo substructures [23], the search for dark matter satellites [24] and a search for high-energy cosmic-ray electrons from the sun [25]. 2.4 gamma-ray lines a line at the wimp mass, due to the 2γ production channel, could be observed as a feature in the astrophysical source spectrum [12]. such an observation would be a “smoking gun” for wimp dm as it is difficult to explain by a process other than wimp annihilation or decay and the presence of a feature due to annihilation into γz in addition would be even more convincing. no significant evidence of gamma-ray line(s) has been found in the first two years of data from 7 to 200 gev [26] (see also [27]). recently, the claim of an indication of line emission in fermi-lat data [28, 29] has drawn considerable attention. using an analysis technique similar to [27], but doubling the amount of data as well as optimizing the region of interest for signal over square-root of background, [28] found a (trial corrected) 3.2 σ significant excess at a mass of ∼ 130 gev that, if interpreted as a signal would amount to a cross-section of about < σv >∼ 10−27cm3s−1. figure 3: dark matter annihilation 95% cl cross section upper limits into γγ for the einasto profile for a circular region of interest (roi) with a radius rgc = 16◦ centered on the gc with |b| < 5◦ and |l| > 6◦ masked. the signal is found to be concentrated on the galactic centre with a spatial distribution consistent with an einasto profile [30]. this is marginally compatible with the upper limit presented in [26]. in the analysis of the 4 year data the fermi lat team has improved over the two year paper in three important aspects: i) the search was performed in five regions of interest optimized for dm search under five different assumptions on the morphology of the dm signal, ii) new improved data set (pass 7 reprocessed) was used, as it corrects for loss in calorimeter light yield due to radiation damage during the four years of the fermi mission and iii) the energy dispersion was improved by adding a 2nd dimension to the previously used triple gaussian probability distribution function (pdf) model, leading to a so called ’2d’ pdf (such procedure is shown to increase the sensitivity to a line detection by 15%).. in that analysis [31] no globally significant lines have been fond and new limits to this dm annihilation channel were set (see figure 3). in a close inspection of the 130 gev feature it was found that indeed there exist a 135 gev signal at 4.01σ local significance, when a ’1d’ point spread 141 aldo morselli function (psf) and old data sets were used (consistently with what [28, 29] have found). however, the significance drops to 3.35σ (local, or ≤ 2σ global significance once trials factors are taken into account). in addition, a weaker signal is found at the same energy in the control sample (in the earth limb), which might point to a systematics effectpresent in this data set. in order to examine this possibility weekly observations of the limb are scheduled, and a better understanding of a nature of the excess in the control sample should be available soon. a new version of the event-level reconstruction and analysis framework (called pass 8 ) is foreseen soon from the fermi lat collaboration. with this new analysis software we should increase the efficiency of the instrument at high energy and have a data set based on independent event analysis thus gaining a better control of the systematic effects. 2.5 the cosmic ray electron spectrum the experimental information available on the cosmic ray electron (cre) spectrum has been dramatically expanded with a high precision measurement of the electron spectrum from 7 gev to 1 tev by the fermi lat [18], [19]. the spectrum shows no prominent spectral features and it is significantly harder than that inferred from several previous experiments. recently the fermi-lat collaboration performed a direct measurement of the absolute e+ and e− spectra, and of their fraction [35]. as the fermi-lat does not carry a magnet, analysis took advantage of the fact that due to its magnetic field, the earth casts a shadow in electron or positron fluxes in precisely determined regions. as a result, this measurement confirmed a rise of the positron fraction observed by pamela, between 20 and 100 gev and determined for the first time that it continues to rise between 100 and 200 gev (see figure 4). these measurements show that a new component of e+ and e− are needed with a peak at ∼ 1 tev. the temptation to claim the discovery of dark matter from detection of electrons and positrons from annihilation of dark matter particles is strong but there are competing astrophysical sources, such as pulsars, that can give a strong flux of primary positrons and electrons (see [16] and references therein). at energies between 100 gev and 1 tev the electron flux reaching the earth may be the sum of an almost homogeneous and isotropic component produced by galactic supernova remnants and the local contribution of a few pulsars with the latter expected to contribute more and more significantly as the energy increases. if a single nearby pulsar gives the dominant contribution to the extra component a large anisotropy and a small bumpiness should be expected; if several pulsars contribute the opposite scenario is expected. so far no positive detection of cre anisotropy was reported by the fermi-lat collaboration, but some stringent upper limits were published [34] and the pulsar scenario is still compatible with these upper limits. energy (gev) 1 10 210 p os itr on f ra ct io n −110 fermi 2011 pamela 2009 ams 2007 heat 2004 figure 4: positron fraction measured by the fermi lat and by other experiments [32, 33, 17]. the fermi statistical uncertainty is shown with error bars and the total (statistical plus systematic uncertainty) is shown as a shaded band. after the conference the ams-02 collaboration presented the result on the positron fraction [36] that confim the positron ratio rise observed by pamela and fermi and extend it up to 350 gev. forthcoming measurements from ams-02 and calet are expected to reduce drastically the uncertainties on the propagation parameters by providing more accurate measurements of the spectra of the nuclear components of cr. fermi-lat and those experiments are also expected to provide more accurate measurements of the cre spectrum and anisotropy looking for features which may give a clue of the nature of the extra component. 3 origin of cosmic rays cosmic rays are particles (mostly protons) accelerated to relativistic speeds. despite wide agreement that supernova remnants (snrs) are the sources of galactic cosmic rays, unequivocal evidence for the acceleration of protons in these objects is still lacking. when accelerated protons encounter interstellar material they produce neutral pions, which in turn decay into gamma rays. this offers a compelling way to detect the acceleration sites of protons. the identification of pion-decay gamma rays has been difficult because high-energy electrons also produce gamma rays via bremsstrahlung and inverse compton scattering. we detected the characteristic pion-decay feature in the gamma-ray spectra of two snrs, ic 443 and w44, with the fermi large area 142 latest results from the fermi gamma-ray telescope telescope. this detection provides direct evidence that cosmic-ray protons are accelerated in snrs. energy (ev) 810 910 1010 1110 1210 ) -1 s -2 d n /d e ( er g cm 2 e -1210 -1110 -1010 best-fit broken power law fermi-lat veritas (acciari et al. 2009) magic (albert et al. 2008) agile (tavani et al. 2010) -decay0π bremsstrahlung bremsstrahlung with break ic 443 energy (ev) 810 910 1010 1110 1210 ) -1 s -2 d n /d e ( er g cm 2 e -1210 -1110 -1010 best-fit broken power law fermi-lat agile (giuliani et al. 2011) -decay0π bremsstrahlung bremsstrahlung with break w44 figure 5: (a and b) gamma-ray spectra of ic 443 (a) and w44 (b) as measured with the fermi -lat [37] . color-shaded areas bound by dashed lines denote the best-fit broadband smooth broken power law (60 mev to 2 gev), gray-shaded bands show systematic errors below 2 gev due mainly to imperfect modeling of the galactic diffuse emission. at the high-energy end, tev spectral data points for ic 443 from magic [38] and veritas [39] are shown. solid lines denote the best-fit pion-decay gamma-ray spectra, dashed lines denote the best-fit bremsstrahlung spectra, and dash-dotted lines denote the best-fit bremsstrahlung spectra when including an ad hoc low-energy break at 300 mev c−1 in the electron spectrum. these fits were done to the fermi lat data alone (not taking the tev data points into account). magenta stars denote measurements from the agile satellite for these two snrs, taken from [40] and [41], respectively. figure 5 shows the spectral energy distribution obtained for ic 443 and w44 through maximum likelihood estimation. the normalizations of the fluxes of ic 443 and w44 and those of neighboring sources and of the galactic diffuse model, were left free in the fit for each bin. to determine whether the spectral shape could indeed be modeled with accelerated protons, we fit the lat spectral points with a π0-decay spectral model, which was numerically calculated from a parameterized energy distribution of relativistic protons. the measured gamma-ray spectra, in particular the low-energy parts, matched the π0-decay model (fig.5) [37]. the π0-decay gamma rays are likely emitted through interactions between “crushed cloud” gas and relativistic protons, both of which are highly compressed by radiative shocks driven into molecular clouds that are overtaken by the blast wave of the snr unless we introduce in an ad hoc way an additional abrupt break in the electron spectrum at 300 mev c−1 (fig.5 dash-dotted lines), the bremsstrahlung models do not fit the observed gamma-ray spectra. if we assume that the same electrons are responsible for the observed synchrotron radiation in the radio band, a lowenergy break is not expected to be very strong in the radio spectrum and thus the existing data do not rule out this scenario. the introduction of the low-energy break introduces additional complexity and therefore a bremsstrahlung origin is not preferred. finding evidence for the acceleration of protons has long been a key issue in attempts to elucidate the origin of cosmic rays. our spectral measurements down to 60 mev enable the identification of the π0-decay feature, thus providing direct evidence for the acceleration of protons in snrs. the proton momentum distributions, well-constrained by the observed gamma-ray spectra, are yet to be understood in terms of acceleration and escape processes of high-energy particles. 4 conclusions fermi turned four years in orbit on june, 2012, and it is definitely living up to its expectations in terms of 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[40] m. tavani, et al., [agile coll.], apj 710, l151 (2010). doi:10.1103/physrevlett.110.141102 [41] a. giuliani, et al., [agile coll.], apj 742, l30 (2011). doi:10.1126/science.1231160 145 http://dx.doi.org/10.1103/physrevd.82.092003 http://dx.doi.org/10.1103/physrevlett.110.141102 http://dx.doi.org/10.1126/science.1231160 introduction indirect dark matter searches galactic center galactic halo dwarf galaxies gamma-ray lines the cosmic ray electron spectrum origin of cosmic rays conclusions 42 acta polytechnica ctu proceedings 1(1): 42–48, 2014 42 doi: 10.14311/app.2014.01.0042 lhc, astrophysics and cosmology giulio auriemma1,2 1università degli studi della basilicata, potenza,italy 2infn sezione di roma, rome, italy corresponding author: giulio.auriemma@cern.ch abstract in this paper we discuss the impact on cosmology of recent results obtained by the lhc (large hadron collider) experiments in the 2011-2012 runs, respectively at √ s = 7 and 8 tev. the capital achievement of lhc in this period has been the discovery of a spin-0 particle with mass 126 gev/c2, very similar to the higgs boson of the standard model of particle physics. less exciting, but not less important, negative results of searches for supersymmetric particles or other exotica in direct production or rare decays are discussed in connection with particles and v.h.e. astronomy searches for dark matter. keywords: hep physics cosmology dark matter dark energy. 1 introduction on july 4th 2012 the atlas[1] and cms[2] collaboration has announced the discovery of a new massive boson, which subsequentely was shown to look like the standard model higgs bosonn. this was possible only after the 2012 runs of lhc at √ s = 8 tev. the two central experiment atlas & cms have collected during 2011 and 2012 an integrated luminosity of ≈ 40 fb−1. several reason support the general belief that this boson could be the long expected higgs boson [3], in particular • it is definitively a boson with spin 6= 1 because decays in γ-γ channel (h → γγ). quantum numbers jp = 0+,predicted by sm are strongly favored [4, 5] ; • the pdg averaged mass is [6] : mh = 125.9 ± 0.4(stat) ± 0.4(syst) gev/c2 consistent with ew precision measurements that requires mh = 102−24 −20 gev/c2 [7]; • production cross section σpp→h agrees well inside the errors to the prediction of sm, that are affected by the uncertainty of 15%. • branching ratios to leptons, hadrons and gauge bosons are close enough to the sm predictions, with some tension in the channels h → γγ (µ ' 2) and h → bb (µ < 1) for atlas data. • angular distribution is slightly in favor of spin 1, but only with more data this could be confirmed, analyzing the decay h →ww → 2`2ν. at present, from february 2013 to november 2014, lhc is engaged in the first long shutdown aimed at the consolidation of the accelerator for running at the full design c.m.s. energy √ s = 14 tev. after this point, hopefully, supersymmetry (susy) hunting will be open. 2 supersymmetric higgs from the supersymmetry theory is expected a relation between the half-integer spin fermions to the integer spin bosons, introduced initially on a purely mathematical ground [8]. the real appeal of this theoretical framework is that it incorporates not only the three gauge fields of the sm but also gravity [9, 10]. figure 1: mssm model higgs masses, the hatched area indicates the decoupling susy parameters space ma > 2mz (adapted from ref. [11]). 42 http://dx.doi.org/10.14311/app.2014.01.0042 lhc, astrophysics and cosmology the particle spectrum of susy is extremely more crowded then the particle spectrum of sm. the present universe is constituted by matter fermions and force fields mediated by bosons, no susy particles has been identified. it means that at a time m−1 pl ≤ tsusy ≤ tew the supersymmetry has been broken, in the sense that masses of susy partners became m̃susy � msm . for this reason the lightest neutral supersymmetric particles are excellent candidates for dark matter [12]. the higgs sector of susy theories is more complicated then in the sm. in the minimal supersymmetric extension of the sm, the higgs sector is schematically:( h0 u h− ) ( h+ h0 d ) a0 (1) namely a cp-odd pseudo scalar field a0 and two doublets of scalar cp-even fields. whose neutral components have v.e.v., assumed to be 〈 h0 u 〉 = vu and〈 h0 d 〉 = vd normalized to the value of fermi constant v2 u + v2 d = √ 2gf , with a ratio parameterized as vu/vd = tanβ. the physical fields detectable at accelerator h and h are mixed states of the neutral components of the doublets with masses mh < mh , although it was never discarded the possibility to detect also the other states, especially the charged ones. if the mass of the pseudo-scalar ma and tanβ are taken as free parameters, the masses of the other four are fixed by the equations [13]: m2 h± = m2 a +m2 z + ∆m2 h± m2 h,h = 1 2 ( m2 a +m2 z ) + ∓ √ m2 a +m2 z − (2mamz cos 2β) 2 + ∆m2 h,h (2) where ∆m2 h±and ∆m2 h,h are the appropriated radiative corrections. fig. 1 shows the predictions of eq. (2) in which is clear that the light susy higgs mass saturates in the limit of decoupling ma � mz to mh → mz |cos 2β| + ∆m2 h. the actual value of this limit, that depends strongly from the radiative corrections, is estimated to be in the range 130-150 gev/c2 [15, 16]. fig. (2) from cms [14] shows the result of the search of higgs like particles decaying to pairs of gauge bosons, giving evidence that a susy high mass higgs with mass lower than 700 gev/c2 is excluded. in facts the total production cross sections for the neutral susy higgs is essentially the same of that expected in sm, but the dominant decay channels are h → (w±, z) with vector bosons in final state [11]. fig. 2 shows the results of the cms search of higgs with mh > 200 gev/c2 [14], that clearly excludes any mass mh ≤ 600 gev/c2 at 95% cl. figure 2: observed (solid line) and expected (dashed line) 95% cl upper limit on the ratio of the product of production cross section and branching ratio to the sm expectation for the higgs boson (from ref. [14]). 3 higgs boson in cosmology inflation is nowadays a well accepted paradigm in cosmology. the only problems is what is physically the “inflaton”. the original field considered as inflaton by guth was actually the higgs field [17], whose potential v (φ) = 1 4λφ 4 can naturally produce inflation if λ is small [18]. but this model predicts that the amplitude of density perturbation is δρ/ρ ∼ √ λ. therefore, in order to explain the observed δρ/ρ ∼ 10−4, it should be λ ∼ 10−10, absolutely irreconcilable with an higgs mass mh = √ 2λv, with v = (√ 2gf )− 1 2 given by the strengths of the weak interactions. a solution could be a coupling of the higgs field with the gravity [19], with a lagrangian density lgr+sm = ( 1 2 m2 pl + ξφ2 ) r+ 1 2 |∂µφ|2 − vsm (φ) (3) where mpl = (8πgn ) −1 is the reduced planck mass, r the ricci scalar, vsm (φ) = 1 4λ ( φ2 − v2 )2 is the potential of the sm higgs field and ξ 6= 0 its coupling to the gravity. applying a rescaling of the metric g̃µν = ( 1 + 2ξφ2/m2 pl )−1 gµν [20] the potential of the field becomes veff (φ) = λ 4 ( φ2 − v2 )2( 1 + 2ξφ2 m2 pl )2 (4) for the present small value of the higgs field φ � mpl/ √ 2ξ we have ṽ (φ) 'v(φ), while for φ & mpl/ √ 2ξ the effective potential of eq. (4), has a 43 giulio auriemma plateau that allows a successful slow-roll inflation. a first constraint on the coupling ξ is obtained from the amount of expansion of the universe reached at the end of the inflationary phase. the number of e-folding, defined from a(tf ) = a(ti) exp(−n) is predicted to be, using the slow-roll approximation [21], the higgs field that varies in the expansion from an initial value φi to a final one φf ≈ mpl/ √ 2ξ. the ratio is φi/φf ≈ √ 8n/3 for ξ � 1. the amplitude of anisotropy depends on the mass of the higgs boson, which fixes the value of the quartic coupling λ. the predicted scalar amplitude is δρ/ρ ≈ n π √ 18 √ λ/ξ. in order to justify the observed δρ/ρ ≈ 10−4 a strong coupling ξ & 104 is required. more refined calculations, including the non negligible radiative corrections to the higgs potential due the coupling with heavy quarks [22, 23], show that mh =126 gev/c2 is compatible with the spectral index of the power law for scalar perturbations ns = 0.962± 0.002 and the upper limit for the tensor-to-scalar ratio r < 0.11 (95% c.l.) measured by planck [24]. theoretical studies have confirmed that susy inflation is possible, in many different scenarios [25] either with minimal [26] or non-minimal coupling [27]. as noted by linde [28] we can expect that due to the rich structure of the higgs sector in susy theories, the effective potential of the superfield will show several minima, interleaved by maxima where v ′(φ)� v (φ), suitable for slow-roll inflation in the minimal coupling case ξ = 0. the case of a non minimal coupling ξ > 0, is shown in ref. [27]. in a recent paper nakayama & takahashi [29] examined a susy model in which the lightest neutral higgs boson could be identified with the sm-like one. figure 3: planck best-fit value of the spectral index and mh = 126 gev/c2 from lhc fits very well mssm inflaton model with small β (adapted from ref. [29]). 4 dark matter cosmological non-baryonic dark matter with ωdmh 2 = 0.120 ± 0.003(stat) ± 0.03(syst) has been estimated by planck [30]. figure 4: status of experimental direct search for wimps. the 68% cl region of possible positive detection are shown as filled area, while solid line represents 95% cl upper limits. the type of relics that can supply this density at “freeze out” should have a thermally averaged rate of annihilation at “freeze-out” (tf ' mdm/20) : 〈σav〉tf ' 2× 10−26 ( 0.12 ωdmh2 ) cm3s−1 (5) for mdm > 10 gev/c2 [31]. it is worth noticing that the dm particles will be non-relativistic at freeze-out with β ≈ 4 × 10−2, that is dubbed “cold dark matter” (cdm). in addition the annihilation cross section that produces a rate comparable to the one of eq. (5) is close to the weak scale σ ≈ g2 fm 2/16π for an hypothetical weakly interacting massive particle (wimp), not existing in the sm. the density of wimp’s in the solar neighborhood is estimated to be ρdmlocal = 0.39± 0.03 gev/cm3 and is flowing with a velocity ≈ 200 km/s. wimp of mass 10 gev/c2, scattering against nucleons with a cross section σsi ≈ 10−40 cm2, give 0.5 interactions/100 kgday in a suitable detector[32]. the present controversial status of the direct searches is summarized in fig. 4. this figure shows that the claims for positive detections [33, 34, 35] seem to cluster around a “low” mass value mwimp ≈ 10 gev/c2 and a “high” elastic scattering cross section σsi ≈ 0.5× 10−40 cm2/nucleon. particularly tantalizing is the claimed observation of a yearly modulation of the detected signal [36], that could be a clear signature of the association of the detected particles with the galactic halo. but unfortunately fig. 4 shows also that all but dama/libra experiments do not show evidence of a similar signal, even if it should be well inside their sensitivity [37]. 44 lhc, astrophysics and cosmology indirect searches for dm are based on the detection of radiation produced in the annihilation and decay of relic wimp’s. neutrino, gamma and antimatter astronomy are the basic tools of this search. from the eq. 5 it is possible to derive an order of magnitude of the annihilation rate. it is worth to stress however that this estimate is an average of σav over the thermal velocity distribution at tf � 1 gev, while annihilations in a galactic environment will take place at much lower temperature. moreover the source function of the astrophysical radiation will be qk = 〈σav〉 bkρ2/m2 in photons cm−3s−1 being bk the inclusive branching ratio to the sm particle k, ρ and m respectively the local energy in gev/c2 cm−3 and the mass of the wimp in gev/c2. the spectrum of the γ-rays (or neutrinos) produced is composed by a continuum, extending up to the kynematical limit eγ . m and several monochromatic lines, each corresponding to a two body final states. the latter very attractive signature was proposed since 1988 by the compton gamma ray obsevatory [38]. in facts the first indication of a possible dm component in the diffuse galactic γ-rays from the galactic plane was given by the egret spark-chamber calorimeter [39], that found a significant excess on the galactic plane for eγ ≥ 1 gev. the poor energy resolution of the egret calorimeter for hard γ-rays did not allowed any search for lines, but the intensity and distribution in the galactic frame of this radiation was found to be close to what expected for annihilation or decay of particles with mass in the range 50-100 gev/c2. in the case of wimp’s the γ inclusive annihilation rate is σγv ≈ 10−26 cm3s−1 [40]. the diffuse γ−rays emission from selected regions on the galactic plane has been measured with high energy resolution (∼ 8% in the range 1-300 gev) by the csi scintillator trackercalorimeter of the fermi-lat instrument [41, 42]. the observed γ-rays spectrum is fitted with a single power law e−αγ for eγ ≥ 12.6 gev, with α = 2.44±0.01. narrow lines of width compatible with the instrumental resolution have been searched using background+signal max-likelihood method. fermilat has not detected any statistically significant γ-ray line in the range from 5 to 300 gev. an upper limit of the rates σ2γv ≤ 0.02 − 3.6 × 10−27 cm3s−1, for wimp’s masses 5 ≤ m ≤ 200 gev/c2, can be estimated from the flux upper limit at 95% c.l., applying the most optimistic galactic halo wimp density profile from n-body simulations [43]. if a simple isothermal profile is assumed, the limit increases by 50%. this limit starts to be close to the predicted rate for susy dm candidates [44]. unfortunately with this new data the claimed line at ≈130 gev [45, 46] corresponding to σ2γv ≈ (1.1± 0.5) × 10−27 cm3s−1 has not gained statistical significance (≈ 3.3σ). an excess of positrons in the energy range 4 ≤ ee ≤ 50 gev in cosmic rays, was discovered by a balloonborne instrument launched in 1974 from palestine, tx, in the heroic age of astroparticle physics [47]1. it is remarkable that after about 40 years we have a high precision mesurement of the positron flux covering the range 0.5 ≤ ee ≤ 350 gev from the 8.5 tons particle’s spectrometer ams-02 installed on the international space station [48]. the ams-2 positron fraction vs. energy is first decreasing from 8.42% at 1 gev to a minimum of 5.1% at 7 gev then increasing up to ' 15% at 260 gev. an excellent fit to this behaviour can be obtained either from pair emission by pulsar[49] or wimps annihilation [50]. in the latter case the mass of the wimp should be in the range 750 gev ≤ m ≤ 1.5 tev and inclusive annihilation rate 10−23 ≤ σe+v ≤ 10−22 cm3s−1[52] significantly larger then the one of eq. 5 ref. [51]. the discriminating observation is definitively the detection of an excess in the antiproton flux, because in the annihilation to lepton pair and quarks one is strongly correlated. up to now the pamela data [53] do not support any deviation from cosmic rays secondary production. alternatively, by assuming that the excess of positrons is all due to astrophysical sources, ref. [54] finds an upper limit to the annihilation rate that varies from 10−26 cm3s−1 at m = 10 gev/c2 to 10−23 cm3s−1 at m = 1 tev/c2, assuming that the dominant annihilation channel is µ+µ−. 5 lhc search for dark matter candidates the lower mass state of the four spin 1 2 neutralinos χ0 1, χ 0 2, χ 0 3, χ 0 4, predicted in r-parity conserving susy models, is a good candidate for the role of wimp. other candidates do exists, as for example the superpartner of the graviton, the spin 3 2 gravitino, that would be a superwimp because it couples with ordinary matter only via the gravitational interaction, making direct dm detection practically impossible [55]. at hadronic colliders such as lhc only wimps that couple with protons, such as the neutralino, can be directly produced. the production of neutralino candidate can be tested, quasi-model independently, using the process: pp→ ( χ0 1χ̄ 0 1 ) +x (6) wherex can be one (or more) hadronic jet, hard leptons or photons, while the neutralino pair (if r-parity is conserved) do not interact with the detector, but uppears in the kinematics of the event as missing trans1note that the young member of this slac team will be the nobel laureate of 2006 for cobe. 45 giulio auriemma verse energy emisst [56]. the dominant sm physical background for the reaction (6) is pp → w±/z0 → ``, where the leptons are neutrinos or are not detected, that can be subtracted and/or reduced by optimized kinematical cuts. figure 5: upper limits on σsi (left) and σ2γv (right) inferred from monojet+emisst atlas data [57]. considering the simpler case that x is a single hadronic jet the cross section for neutralino pairs production, that contributes to process (6), will be σqq→χχ̄ ≈ αsg 2 χg 2 qp jet t /m4 ∗ where αs = 0.64 is the qcd constant, gχ, gq the susy couplings being q = q, q̄ or g and finally m∗ � pt is suppressing mass scale. the detection of a number of events significantly larger the the calculated sm background would be strong indication of a wimp candidate, whose mass could be inferred from the missing energy distribution. in addition a comparison with direct dm search experiments, discussed in the previous section, would be possible because the scattering cross section, from the same coupling, is predicted to be σsi ≈ g2 χg 2 qµ 2/m4 ∗ being µ the reduced mass of the wimp-nucleon system [58]. moreover the same suppression factor m−4 ∗ enters, together with phase space factor depending only from the masses, in the annihilation rate of the neutralino (see for example eq. (10) and (11) of ref. [59]) that allows comparison with the dm relic density and the indirect searches. fig. (5) shows the potentiality of this type of searches at lhc [57, 60]. figure 6: lhcb signal for b0 s → µ+µ− [62] (left) and presently cmssm allowed region (green) on the plane (m0,m1/2) [55] (right). important constraints on the supersymmetries, beyond the effective field theories discussed before, that can also set limits to the wimp candidates properties, are given by the search for rare decays of heavy neutral mesons like the b0 d and b0 s decays, copiously produced at lhc [61], performed by the lhcb experiment as well as the cms experiment. lhcb is the lhc experiment devoted to flavor physics. both lhcb and cms have measured the br(bs → µµ) which is an important test bench for new physics, because it strongly suppressed in the minimal smit is enhanced by susy. limit at 95% cl is br(bs → µµ)susy < br(bs → µµ)sm . 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[63] d. bauer, et al. in ”report prepared for the community summer study”, (snowmass) 2013 arxiv: 1305.1605. 48 http://arxiv.org/abs/1007.0821 http://arxiv.org/abs/1309.2570 http://dx.doi.org/10.1103/physrevlett.105.121101 http://arxiv.org/abs/1304.1414 http://arxiv.org/abs/1008.1783 http://arxiv.org/abs/1210.4491 http://dx.doi.org/10.1103/physrevd.82.116010 http://arxiv.org/abs/1005.3797 http://arxiv.org/abs/1109.4398 http://arxiv.org/abs/1207.7315 http://arxiv.org/abs/1307.5024 http://arxiv.org/abs/1307.5024 http://arxiv.org/abs/1305.1605 http://arxiv.org/abs/1305.1605 introduction supersymmetric higgs higgs boson in cosmology dark matter lhc search for dark matter candidates summary 274 acta polytechnica ctu proceedings 1(1): 274–277, 2014 274 doi: 10.14311/app.2014.01.0274 multiscale modeling of astrophysical jets james h. beall1,2,3, john guillory* 3, david v. rose4, michael t. wolff2 1st. johns college, annapolis, md 2space sciences division, naval research laboratory, washington, dc; 3college of sciences, george mason university, fairfax, va; 4voss scientific, albuquerque, nm; corresponding author: beall@sjc.edu abstract we are developing the capability for a multi-scale code to model the energy deposition rate and momentum transfer rate of an astrophysical jet which generates strong plasma turbulence in its interaction with the ambient medium through which it propagates. we start with a highly parallelized version of the vh-1 hydrodynamics code (coella and wood 1984, and saxton, et al., 2005). we are also considering the pluto code (mignone et al. 2007) to model the jet in the magnetohydrodynamic (mhd) and relativistic, magnetohydrodynamic (rmhd) regimes. particle-in-cell approaches are also being used to benchmark a wave-population models of the two-stream instability and associated plasma processes in order to determine energy deposition and momentum transfer rates for these modes of jet-ambient medium interactions. we show some elements of the modeling of these jets in this paper, including energy loss and heating via plasma processes, and large scale hydrodynamic and relativistic hydrodynamic simulations. a preliminary simulation of a jet from the galactic center region is used to lend credence to the jet as the source of the so-called the fermi bubble (see, e.g., su, m., & finkbeiner, d. p., 2012) *it is with great sorrow that we acknowledge the loss of our colleague and friend of more than thirty years, dr. john ural guillory, to his battle with cancer. keywords: jets active galaxies blazars intracluster medium non-linear dynamics plasma astrophysics. 1 introduction recent high-resolution (vlba) observations of astrophysical jets (see, e.g., lister et al. 2009) reveal complex structures apparently caused by ejecta from the central engine as they interacts with both surrounding interstellar material such as broad-line region (blr) and narrow-line region (nrl) clouds, and ejecta from prior episodes of activity. a particularly trenchant example of these complex interactions is also shown by the galactic microquasar, sco x-1 (fomalhaut, geldzahler, and bradshaw, 2001). such observations can be used to inform models of the jet-ambient-medium interactions. based on an analysis of these data, we posit that a significant part of the observed phenomena come from the interaction of the ejecta with prior ejecta as well as interstellar material. 2 scales of jet interactions with the ambient medium large scale hydrodynamic simulations of the interaction of astrophysical jets with the ambient medium through which they propagate can be used to illuminate a number of interesting consequences of the jets’ presence. these include acceleration and entrainment of the ambient medium, the effects of shock structures on star formation rates, and other effects originating from ram pressure and turbulence generated by the jet (see, e.g., basson and alexander, 2002; zanni et al. 2005; and krause and camenzind 2003; perucho, et al. 2012). we have presented results for large scale hydrodynamic simulations and initial relativistic hydrodynamic simulations in previous works (beall et al., 1999, 2003, 2006). as noted in those papers, magneto-hydrodynamic (mhd) and (rmhd) simulations neglect important species of physics: the microscopic interactions that occur because of the effects of particle-particle interactions and the interactions of particles with the collective effects that accompany a fully or partially ionized ambient medium (i.e. a plasma). while the physical processes (including plasma processes) in the ambient medium can be modeled in small regions by pic (particle-in-cell) codes for some parameter ranges, simulations of the larger astrophysical jet structure with such pic codes are not possible with current or foresee274 http://dx.doi.org/10.14311/app.2014.01.0274 multiscale modeling of astrophysical jets able computer systems. for this reason, we have modeled these plasma processes in the astrophysical regime by means of a system of coupled differential equations which give the wave populations generated by the interaction of the astrophysical jet with the ambient medium through which it propagates. a detailed discussion of these efforts can be found, variously, in scott et al. (1980), rose et al. (1984), rose et al. (1987), beall (1990), and beall et al. (2003). the scales of these interactions range from kilometers to kiloparsecs. 2.1 energy loss, energy deposition rate, and momentum transfer from plasma processes the system of equations used to determine the normalized wave energy densities is very stiff. scott et al. (1980) estimated the equilibrium solution of this system of equations for heating of clusters of galaxies, and rose et al. (1984) and beall (1990) showed dynamical solutions that confirmed the stability of the equilibrium solutions. solving the system of equations yields a time-dependent set of normalized wave energies (i.e., the ratio of the wave energy divided by the thermal energy of the plasma) that are generated as a result of jets interaction with the ambient medium. these solutions can yield an energy deposition rate (de/dt), an energy deposition length (de/dx), and ultimately, a momentum transfer rate (dp/dt (1/vb) ∗ (de/dt) that can be used to estimate the effects of plasma processes on the hydrodynamic evolution of the jet. for this part of the analysis, we suppose that a portion of the jet is composed relativistic particles of either e±, p − e−, or more generally, a charge-neutral, hadron-e− jet, with a significantly lower density than the ambient medium. the primary energy loss mechanism for the electron-positron jet is via plasma processes, as beall (1990) notes. kundt (1987, 1999) also discusses the propagation of electron-positron jets. beall et al., (2006) illustrate two possible solutions for the system of coupled differential equations that model this mode of the jet-ambient medium interaction: a damped oscillatory and an oscillatory solution. the landau damping rate for the two-temperature thermal distribution of the ambient medium is used for these solutions. the average energy deposition rate, < d(αε1)/dt >, of the jet energy into the ambient medium via plasma processes can be calculated as < d(αε1)/dt >= npkt < w > (γ1/ωp)ωpergs cm −3s−1, where k is boltzmann’s constant, t is the plasma temperature, < w > is the average (or equilibrium) normalized wave energy density obtained from the wave population code, γ1 is the initial growth rate of the two-stream instability, and α is a factor that corrects for the simultaneous transfer of resonant wave energy into nonresonant and ion-acoustic waves. the energy loss scale length, deplasma/dx = −(1/nbvb)(dαε1/dt), can be obtained by determining the change in γ of a factor of 2 with the integration ∫ dγ = − ∫ [d(αε1)/dt]dl/(vbnbm ′ c2) as shown in rose et al., 1978 and beall 1990, where m ′ is the mass of the beam particle. thus, lp = ((1/2)γcnbmc 2)/(dαε1/dt) cm is the characteristic propagation length for collisionless losses for an electron or electron-positron jet, where dαε1/dt is the normalized energy deposition rate (in units of thermal energy) from the plasma waves into the ambient plasma. in many astrophysical cases, this is the dominant energy loss mechanism. we can therefore model the energy deposition rate (de/dt) and the energy loss per unit length (de/dx), and ultimately the momentum loss per unit length (dp/dx) due to plasma processes. figure 1: simulation using a highly-parallelized version of the vh-1 hydrodynamics code. the figure shows the transverse cross-section (figure 1a) and the detail of the jet head in the y-z cross-section (figure 1b) for a fully 3-dimensional hydrodynamic simulation of jet with v = 1.5x109 cm/sec. the cross section at z = 300 for a jet with v = 1.0x1010 cm/s. the cross section represents approximately 2 kiloparsecs from the jet origin. we have used the 5123 simulation in this representation for ease of presentation, given the size and difficulty of displaying the 20483 data. note the well-developed rayleigh-taylor instabilities at the jet-ambient medium boundary in figure 1a. beall, guillory, and rose (2009) have compared the results of a pic code simulation of an electronpositron jet propagating through an ambient medium of an electron-proton plasma with the solutions obtained by the wave population model code, and have found good agreement between the two results (see figure 1 from that paper). at the same time, that paper demonstrates that the ambient medium is heated and entrained into the jet. that analysis also shows that a relativistic, low-density jet can interpenetrate an ambient gas or plasma. initially, and for a significant fraction of its propagation length, the principal energy loss mechanisms for such a jet interacting with the ambient medium is via plasma processes (rose et al. 1984, beall 1990). 275 james h. beall et al. as part of our research into the micro-physics of the interaction of jets with an ambient medium, we continue to investigate the transfer of momentum from the jet, and expect to present these results shortly. in order to proceed to a more detailed analysis of the issue of momentum transfer, we have used modern pic code simulations to study the dynamics of caviton formation, and have confirmed the work of robinson and newman (1990) in terms of the cavitons’ formation, evolution, and collapse. 2.2 results of hydrodynamical calculations figure 1 shows two views of a simulation for an astrophysical jet for parameters appropriate to a seyfert galaxy, using a highly-parallelized version of the vh1 hydrodynamics code. the figure shows the transverse cross-section (figure 1a) and the detail of the jet head in the y-z cross-section (figure 1b) for a fully 3-dimensional hydrodynamic simulation of jet with v = 1.5x109 cm/sec. the cross section at z = 300 for a jet with v = 1.0x1010 cm/s. the cross section occurs at approximately 2 kiloparsecs from the jet origin. figure 2: simulation using the vh-1 code of a supersonic jet with parameters appropriate to the galactic center region. in this simulation, also, we use the vh-1 code for a supersonic jet in the x-y pressure cross section (1a) and with an x-y density cross section (1b) for a supersonic jet with v = 2.0x108 cm/s. such a jet originating from the supermassive black hole at the center of the milky way could account for the production of the gamma-ray structure known as the galactic center bubble found by the fermi satellite. the vertical scale of the jet represents approximately 2 kiloparsecs from the jet origin. we have used the 5123 simulation in this representation for ease of presentation, given the size and difficulty of displaying the 20483 data figure 2 shows a simulation of a supersonic jet for parameters appropriate to the galactic centre region. in this simulation, also, we use the vh-1 code for a supersonic jet in the x-y pressure cross section (1a) and with an x-y density cross section (1b) for a supersonic jet with v = 2.0x108 cm/s. such a jet originating from the supermassive black hole at the center of the milky way could account for the production of the gamma-ray structure known as the galactic center bubble found by the fermi satellite. the vertical scale of the jet in figure 2a represents approximately 2 kiloparsecs from the jet origin. we have used the 5123 simulation in this representation for ease of presentation. the detail of the jet-head structure (figure 2b) shows complex, transverse shock structures at the leading edge of the jet. the simulations we have run using 20483 cells confirm these features. 3 concluding remarks the effects of collective and particle processes, including plasma effects, can have observational consequences. beall (1990) has noted that plasma processes can slow the jets rapidly, and beall and bednarek (1999) have shown that these effects can truncate the low-energy portion of the γ-rays spectrum (see their figure 3), a similar effect will occur for particle-particle productions of neutrinos, pions, and (perhaps) neutrons. this could also reduce the expected neutrino flux from agn. the presence of plasma processes in jets can also greatly enhance line radiation species by generating high-energy tails on the maxwell-boltzmann distribution of the ambient medium, thus abrogating the assumption of thermal equilibrium. an analytical calculation of the boost in energy of the electrons in the ambient medium to produce such a high energy tail, with ehet ∼ 30 − 100kt, is confirmed by pic-code simulations. aside from altering the landau damping rate, such a high-energy tail can greatly enhance line radiation over that expected for a thermal equilibrium calculation (see beall et al. 2006, and beall, guillory, and rose (1999) for a detailed discussion). we are in the process of setting up runs for the pluto code (mignone et al. 2007) in order to benchmark its results with our results of the vh-1 code in appropriate parameter ranges. acknowledgement jhb and mtw gratefully acknowledge the support of the office of naval research for this project. thanks also to colleagues at various institutions for their continued interest and collaboration, including kinwah wu, curtis saxton, s. schindler and w. kapferer, and s. colafrancesco. references [1] basson, j. f., and alexander, p., 2002, the longterm effect of radio sources on the intracluster medium, mnras, 339, 353. 276 multiscale modeling of astrophysical jets [2] beall, j. h. et al., 1978, radio and x-ray variability of the nucleus of centaurus a (ngc 5128), ap.j., 219, 836. doi:10.1086/155845 [3] beall, j. h. and rose, w. k., 1981, on the physical environment in the nucleus of centaurus a(ngc 5128), ap.j., 238, 539 (also see erratum, 1981, ap.j., 248, 883). [4] beall, j. h. and bednarek, w., 1999, on the hadronic beam model for gamma-ray production in blazars, ap.j., 510, 188. [5] beall, j. h., guillory, j., and rose, d. v., 1999, observational signatures in jet-cloud interactions, mem. s. a. it., 70, 1235. [6] beall, j. h., guillory, j., and rose, d. v., 2003, agn jet interactions with the intracluster medium, c.j.a.a., 3(suppl.), 137. [7] beall, j. h., guillory, j., rose, d. v., schindler, s., colafrancesco, s., 2006, energetics of jet interactions with the intracluster medium, c.j.a.a., 6(suppl. 1), 283. [8] beall j. h., 1990, energy loss mechanisms for fast particles in an ambient medium, in physical processes in hot cosmic plasmas, w. brinkmann, a. c. fabian, and f. giobannelli, eds. (kluwer academic, london), p. 341. doi:10.1007/978-94-009-0545-0 20 [9] colella, p., and woodward, p. r. 1984, the piecewise parabolic method (ppm) for gasdynamical simulations, j. comp. phys., 54, 174. doi:10.1016/0021-9991(84)90143-8 [10] fomalont, e. b., geldzahler, b. j., and bradshaw, c. f., 2001, scorpius x-1: the evolution and nature of the twin compact radio lobes, ap.j., 558, 283. doi:10.1086/322479 [11] kaplan, s. a., and tsytovich, v. n., 1973 plasma astrophysics, (pergamon press, oxford). [12] krause, m., and camenzind, m., 2003, paarameters for very light jets of cd galaxies, new astron. rev., 47, 573. doi:10.1016/s1387-6473(03)00096-4 [13] kundt, w., 1987, the sources and their models, in astrophysical jets and their engines, ed. w. kundt (reidel, dordrecht, netherlands), p. 1. [14] kundt, w. 1999, ss 433, mem. s. a. it., 70, 1097. [15] lister, m. l. et al., 2009, astronom. j., 137, 3718. doi:10.1088/0004-6256/137/3/3718 [16] mignone, a. et al., 2007, ap.j. suppl., 170, 228. [17] newman, d. l., winglee, r. m., robinson, p. a., glanz, j., and goldman, m. v., 1990, simulation of the collapse and dissipation of langmuir wave packets, phys. fluids b, 2, 2600. doi:10.1063/1.859385 [18] perucho, m., 2012, jets in high-mass microquasars, mem. s. a. it., 83, 297. [19] rose, w. k., guillory, j., beall, j. h., and kainer, s., 1984, the interaction of relativistic chargedparticle beams with interstellar clouds, ap.j., 280, 550. [20] rose, w. k., beall, j. h., guillory, j., and kainer, s., 1987, radiation from relativistic beams interacting with interstellar gas, ap.j., 314, 95. doi:10.1086/165042 [21] saxton, c. j., bicknell, g. v., sutherland, r. s., and midgley s., 2005, interactions of jets with inhomogeneous cloudy media, mnras, 359, 781. doi:10.1111/j.1365-2966.2005.08962.x [22] scott, j. h., holman, g. d., ionson, j. a., and papadopoulos, k., 1980, the heating of gas in clusters of galaxies by relativistic electrons collective effects, ap.j., 239, 769. [23] su, m., and finkbeiner, d. p., 2012, evidence for gamma-ray jets in the milky way, ap.j., 753, 61. doi:10.1088/0004-637x/753/1/61 [24] zanni, c. et al., 2005, heating groups and clusters of galaxies: the role of agn jets, astron. astrophys., 429, 399. discussion manel perucho could you comment on the viscosity of the bow shock in your 3-d simulations? what is causing it? jim beall the viscosity is likely due to turbulence generated by the jet-ambient medium interaction and from internal shock structures within the jet and in the jet interface with the interstellar medium. gennady bisnovatyi-kogan was a magnetic field included in your numerical simulations? jim beall the vh-1 code we are using is a hydrodynamic code with no capability for the inclusion of magnetic fields. we can estimate the magnetic field strength by assuming equipartition with the gas pressure, but this is not entirely satisfactory. we want to explore the pluto code, which has an mhd capability, in the near future. 277 http://dx.doi.org/10.1086/155845 http://dx.doi.org/10.1007/978-94-009-0545-0_20 http://dx.doi.org/10.1016/0021-9991(84)90143-8 http://dx.doi.org/10.1086/322479 http://dx.doi.org/10.1016/s1387-6473(03)00096-4 http://dx.doi.org/10.1088/0004-6256/137/3/3718 http://dx.doi.org/10.1063/1.859385 http://dx.doi.org/10.1086/165042 http://dx.doi.org/10.1111/j.1365-2966.2005.08962.x http://dx.doi.org/10.1088/0004-637x/753/1/61 introduction scales of jet interactions with the ambient medium energy loss, energy deposition rate, and momentum transfer from plasma processes results of hydrodynamical calculations concluding remarks acta polytechnica ctu proceedings doi:10.14311/app.2017.13.0039 acta polytechnica ctu proceedings 13:39–42, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app on development of the interactive design tool based on isogeometric analysis edita dvořáková∗, bořek patzák czech technical university in prague, faculty of civil engineering, thákurova 7, 166 29 prague 6, czech republic ∗ corresponding author: edita.dvorakova@fsv.cvut.cz abstract. isogeometric analysis is a new concept of finite element method which has been proposed to bridge the gap between the cad systems and the fem solvers. in isogeometric analysis, the same basis functions, typically splines or nurbs, are used for geometry description as well as for approximation of unknowns and thus the same model can be shared between cad and iga systems. this results in a higher accuracy and overall efficiency of the analysis. many isogeometric elements have been already proposed and implemented into the existing finite element solvers, but the automatic connection with a cad system is usually missing. our goal is to develop such a connection and to provide a tool which would interactively run the analysis when the model changes. this approach can enormously enhance the design process as it can provide the basic knowledge about the structural behavior already in conceptual design phase. keywords: curved beam element, discrete shear gap, interactive design, isogeometric analysis. 1. introduction finite element solvers are the integral part of a nowadays structural design. once the architectural model is developed in cad (computer-aided design) system, the structure is further analyzed in fem (finite element method) solver. there are two independent models (cad model and fem model) and thus when one of them changes during the design process the other has to be correspondingly (and usually manually) adjusted, leading to the higher time-consumption. moreover, the inaccuracies in geometry description are usually introduced as the cad and fem models use different functions for geometry representation. the standard finite element method usually uses polynomial basis functions, while the cad systems are based on splines. the use of spline functions for geometry and unknown approximations in finite element analysis enables to share one model between architectural design and structural analysis. this idea has been proposed by huges et al. [1] and it is called isogeometric analysis (iga). since 2005, when isogeometric analysis has been introduced, many researchers have been focusing on its development and the results proved the advantages of iga over standard fem in many fields. our focus is placed on its application for the analysis of curved beams as the curved geometries can especially benefit from the isogeometric approach. we use the formulation of curved beam element presented by bouclier et al. [2] with the locking treatment based on discrete shear gap (dsg) method [3, 4]. the element has been implemented into oofem finite element solver [5] and our main goal is to develop a connection between cad system and the solver to provide a tool encapsulating the analysis within the architectural design environment. 2. curved beam element the presented two-dimensional curved beam element is based on timoshenko beam theory. it has three independent unknowns, axial displacement ut, transverse displacement un and rotation θ. a strain-displacement matrix b defined as ε = br, (1) where ε = {εm, γs, χb}t and r = {ut, un, θ}t , is derived from the relations for membrane strain εm, transverse shear strain γs, and bending strain χb εm = u′t − un r , γs = ut r + u′n − θ, χb = θ′, (2) where s ∈ 〈0, l〉 runs along the midline of a beam and prime indicates a derivative with respect to s. by omitting the terms which are divided by radius of curvature r the straight beam formulation is obtained. a material matrix d results from n = eaεm, q = kgaγs, m = eiχb, (3) where n,q and m are axial force, transverse shear force and bending moment, respectively. young’s modulus e, shear modulus g, shear coefficient k, area a and moment of inertia i are the material and 39 http://dx.doi.org/10.14311/app.2017.13.0039 http://ojs.cvut.cz/ojs/index.php/app edita dvořáková, bořek patzák acta polytechnica ctu proceedings cross-section characteristics. a stiffness matrix is then calculated as k = ∫ l 0 bt db ds. (4) to evaluate the stiffness matrix the gaussian quadrature involving p+ 1 gauss points over each knotspan is used, where p is a degree of approximation. 2.1. nurbs-based formulation in case of iga, the langrange polynomial basis functions used in fem are replaced by splines. the presented element is formulated using non-uniform rational b-splines (nurbs) [6], which is the most widespread and developed technology in cad industry. a nurbs curve is defined by its degree, control points with weights, and knotvector. nurbs basis functions are generated by weighting the b-splines functions, which are piecewise polynomial functions and are a special subset of nurbs functions. nurbs curve is given as the linear combination of basis functions and control points coordinates. the knotvector is a set of non-decreasing parametric coordinates (knots) which influence the mapping. the knots divide a parametric space into knotspans (usually referred to as “elements” in iga) and each knotspan is influenced only by limited number of control points. therefore the knotspan defines which control points affect particular part of the domain. see figure 1 for an example of a nurbs curve geometry. very important aspect of isogeometric analysis is a non-interpolatory nature of the basis functions, as the nurbs do not satisfy kronecker-delta property. another distinct feature of the nurbs basis functions is the higher inter-element continuity. while only c0 continuity is provided by traditional polynomial functions, in case of iga up to cp−1 continuity can be achieved. by repeating knots in a knotvector, the continuity at that knot can be artificially reduced. 2.2. locking treatment shear locking is a well-known problem of standard timoshenko beam elements and this phenomena persists also in isogeometric formulation. this problem occurs because the displacements and rotation are treated independently and approximated by the functions of the same order. from eq. 2 for shear and bending strains it can be seen that formula for bending strain results in lower order term than formula for shear strain, but actually this should be vice-versa. also the field inconsistency within the term for shear strain causes that zero shear strain cannot be satisfied along entire patch when the same order interpolation of unknowns is used. several locking removal techniques have been proposed to unlock isogeometric beam element including reduced integration, b̄-method, dsg method, see [2, 3] for the references. in this study, the dsg-based formulation is used. while this method can increase computational cost (as well as b̄-method), it has a big advantage over reduced integration: for the reduced integration the recovered strains can be evaluated only at gauss points, dsg method enables to evaluate them along the entire patch. discrete shear gap method has been originally developed for the standard finite elements [3] but echter and bischoff [4] have extended its use also for isogeometric analysis. the approach can be divided into several steps yielding the modified b matrix. the idea is not to satisfy the equation γs = ut r + u′n − θ (5) pointwise, but in integral sense. the shear contribution uγhi n (called “shear gaps”) to the deflection is obtained by integration of eq. 5 as uγ hi n = ∫ si 0 γhs ds = ∫ si 0 ut r + u′n − θ ds = bdsgr, (6) at collocation points si calculated as greville abscissa of the control points [6]. modified transverse displacements are interpolated using nurbs basis functions ni uγ modh n = n∑ i=1 niũ γhi n . (7) please note, that discrete shear gaps ũγhi n are noninterpolatory in isogeometric analysis. to expressed the discrete shear gaps by values at the control points the transformation matrix a is derived{ uγ h n } = a { ũγ h n } , aij = nj(si), (8) where { uγ h n } are interpolatory values of shear gaps at control points and nj(si) is the jth-basis function evaluated at ith-collocation point. the modified shear strain is then given as γmod h s = n∑ i=1 n ′i ũ γhi n . (9) combining eqs. 6-9 results in the modified straindisplacement matrix b b = n ′a−1bdsg, (10) which is used to evaluate stiffness matrix k (eq. 4). 3. interactive design tool thanks to the isogeometric formulation, the presented element can be easily connected to cad system. the possibility of seamless connection between cad and fea is the major benefit of iga. this goal can be achieved even without use of isogeometric approach (see e.g. [7]), nevertheless the costly transformations 40 vol. 13/2017 on development of the iga based interactive design tool knots control points s = l s = 0 s ξ ξ1 = 0 ξ2 = 0 .5 ξ3 = 1 knot span patch y x figure 1. description of nurbs geometry. between cad and fem are necessary in such a workflow. firstly, the geometrical model is completed by analysis data, such as loads, boundary conditions and material characteristics, then the model is transformed into suitable computational model and the analysis mesh is generated, and finally the analysis is performed in fem solver. to visualize the results within the cad system the model has to be transformed back to the original model. with the use of isogeometric analysis, once the model is completed with analysis data, the analysis can be performed directly [8] and no transformation is needed for both the analysis and the visualization. for our purposes, the use of cad system rhinoceros (rhino) [9] has been chosen. the geometry representation of rhino is based on nurbs, moreover rhino enables plug-in development and use of built-in tool grasshopper [10]. grasshopper is a visual programming interface within rhino which can directly access nurbs geometry. in addition, visual programming is intelligible even to a user with no programming background, so the user can define additional analysis data at this level. the workflow of the tool is illustrated in figure 2. firstly, the nurbs geometry specified by a user in rhino is passed to the grasshopper, where the model is completed with boundary conditions and material and crosssection characteristics. currently, these data are provided in the text format similar to one used in oofem, but in the next phase of the development, the special plug-ins can be developed. once all the analysis data are collected, the python script within grasshopper together with other available grasshopper tools directly passes these data to oofem and run the analysis. when the analysis is finished, the output file is uploaded back to the grasshoper, where the visualization of the results is carried out. schematic illustration of grasshopper environment with results visualized in rhino can be seen in figure 3. very important feature of the developed tool is, that the grasshopper (and in turn also oofem) recomputes the results immediately when something changes. no matter whether the user adjusts the geometry model results analysis data geometry material, crosssection boundary conditions analysis results visualisation rhinoceros 3d grasshopper grasshopper oofem figure 2. interactive design tool. geometry or changes the boundary conditions, the results are interactively updated. this provides the immediate knowledge about behaviour of the designed structure and eases the process of finding optimal design. in the future work the designer will receive graphical indication of sections where load-bearing capacity or stability limits are achieved. such an approach would allow to establish viable conceptual design from both architectural and structural point of view without the necessity of understanding details of structure behaviour. 4. conclusions the formulation of the curved beam element with locking treatment has been presented and the element has been implemented into oofem finite element code. thanks to the isogeometric formulation, the automatic connection of cad system and the analysis has been provided or modified. the developed tool enables to display the results in rhino immediately 41 edita dvořáková, bořek patzák acta polytechnica ctu proceedings figure 3. schematic illustration of grasshopper environment with results visualized in rhino. the example corresponds to a cantilever circular arc beam (black) subjected to horizontal and vertical load at its tip. the deformed geometry is in red and the bending moment is in blue. after the geometry and analysis data are provided. this gives the user instant knowledge about behaviour of the designed structure and enables to see differences of alternative designs. acknowledgements the financial support of this research by the grant agency of the czech technical university in prague (sgs project no. sgs17/043/ohk1/1t/11) is gratefully acknowledged. references [1] t. j. r. hughes, j. a. cottrell, y. bazilevs. isogeometric analysis: cad, finite elements, nurbs, exact geometry and mesh refinement. comput methods appl mech engrg 194:4135–4195, 2005. [2] r. bouclier, t. elguedj. locking free isogeometric formulations of curved thick beams. comput methods appl mech engrg 245-246:144–162, 2012. [3] k. bletzinger, m. bischoff, e. ramm. a unified approach for shear-locking-free triangular and rectangular shell finite elements. computers and structures 75:321–334, 2000. [4] r. echter, m. bischoff. numerical effiency, locking and unlocking of nurbs finite elements. comput methods appl mech engrg 199:374–382, 2010. [5] b. patzák. oofem project home page, 2017. http://www.oofem.org. [6] l. piegl, w. tiller. the nurbs book. springer-verlag berlin heidelberg, new york, 1997. [7] l. svoboda, j. novák, l. kurilla, j. zeman. a framework for integrated design of algorithmic architectural forms. advances in engineering software 72:109–118, 2014. [8] m. hsu, c. wang, a. herrema, et al. an interactive geometry modeling and parametric desigh platform for isogeometric analysis. computers and mathematics with applications 70:1481–1500, 2015. [9] rhinoceros, 2017. http://www.rhino3d.com/. [10] grasshopper, 2017. http://www.grasshopper3d.com/. 42 http://www.oofem.org http://www.rhino3d.com/ http://www.grasshopper3d.com/ acta polytechnica ctu proceedings 13:40–43, 2017 1 introduction 2 curved beam element 2.1 nurbs-based formulation 2.2 locking treatment 3 interactive design tool 4 conclusions acknowledgements references 13 acta polytechnica ctu proceedings 1(1): 13–19, 2014 13 doi: 10.14311/app.2014.01.0013 γ-rays, ν’s and particle astronomy as messengers of the universe maurizio spurio1 1dipartimento di fisica e astronomia università di bologna and infn corresponding author: spurio@bo.infn.it abstract observations of charged cosmic-rays, γ-rays and neutrino are possible thanks to the availability of new detectors coming from technologies typical of experimental particle physics. in conjunction with more traditional techniques used by astronomers, these multimessenger correlations of experimental data are opening a new scenario in astrophysics. we review some of the more recent developments in the field. keywords: cosmic-rays γ-rays neutrinos satellites ground-based experiments neutrino telescopes. 1 introduction the multimessenger inter-correlation between cosmic rays (crs), γ-rays and neutrinos is of fundamental importance for a deeper comprehension of high energy (he) processes in astrophysical sources. one of the main questions in astrophysics is the origin and nature of crs (§2), whose energy spectrum extends up to above 1020 ev. there are many indications of the galactic origin of the cr bulk (protons and other nuclei up to ∼ 1016 ev). due to the influence of galactic magnetic fields, charged particles detected on earth do not point to the sources. gamma-rays and neutrinos do not suffer the effect of magnetic fields: they represent the decay products of accelerated charged particles but cannot be directly accelerated. the possibility of particle astronomy rely on the detection of these neutral probes, or to the detection of the highest component of charged crs (see castellina, these proceedings). recent advances on gev and tev γ-ray astronomy by satellites and ground-based experiments (§3) have led to the discovery of different classes of galactic and extragalactic objects that can be shed light on the cr acceleration mechanisms. most objects observed in the γ-rays (see fig. 1) are known sources from measurements of their electromagnetic emission at different wavelengths, in particular in the radio and in the x-rays. accelerated protons will interact in the surroundings of the crs emitter with photons predominantly via the ∆+ resonance: p+ γ → ∆+ → πo + p or → π+ + n (1) protons will interact also with ambient matter (protons, neutrons and nuclei), giving rise to the production of charged and neutral mesons. the relationship between sources of γ-ray and neutrinos is the meson-decay channel. neutral mesons decay in πo → γγ while charged mesons decay in neutrinos: π+ → νµ + µ+ ↪→ µ+ → νµ + νe + e+ π− → νµ + µ− ↪→ µ− → νµ + νe + e− (2) in particular circumstances, the energy escaping from the source is distributed between crs, γ-rays and neutrinos. only the coincident measurement of neutrinos (§4) from the source would give a uncontroversial proof of the discovery of the galactic acceleration sites of protons and nuclei. figure 1: sketch of the production of crs, neutrinos, γ-rays and lower energy photons from an astrophysical jet. the highest energy crs are probably originated from extragalactic sources. if they are protons with e > 5 × 1019 ev, they could interact with the cosmic microwave background radiation. this process restricts the origin of highest energy protons seen on earth to a small fraction of the universe, a sphere of the order of 13 http://dx.doi.org/10.14311/app.2014.01.0013 maurizio spurio 100 mpc (the greisen-zatsepin-kuzmin suppression). the prediction of a diffuse flux of he neutrino of extra-galactic origin is a direct consequence of the ultra he cr observations. this connection between crs, neutrinos and γ-rays was used to put upper bounds on the expected neutrino flux from extragalactic sources, since the neutrino energy generation rate will never exceed the generation rate of high energy protons. in this paper, we will review some of the recent updates in these fields. 2 crs and antimatter figure 2: cr intensity as a function of the energy from 1010 to 1020 ev. below few gev, the contribution of particles coming from the sun is not negligible. the energy range of the flux measured by direct experiments is reported as blue line; that measured by indirect experiments as red line crs are mainly protons (fig. 2) and heavier nuclei which are constantly hitting the upper shells of the earth’s atmosphere (blümer et al, 2009). up to energies of ∼ 1014 ev, the cr spectrum is directly measured above the atmosphere. stratospheric balloons and satellites have provided the most relevant information about the composition of crs. above ∼ 1014 ev, cr measurements are only accessible from groundbased large area arrays. recent observations of tev photons seem to confirm the diffusive shock acceleration (dsa) model, where the shocks powered by supernova explosions in our galaxy provide the iterative scattering mechanism for crs acceleration up to ∼ 1016 ev (see hillas, 2005). the key feature of this process is that an energy powerlaw spectrum of the type ∼ e−2 is produced. the dsa model is consistent with the balance between the energy transferred to the accelerated particles and the energy loss due to the escape of crs out of the galaxy. the e−2 emission at sources, when corrected for energydependent leakage from the galaxy, is in agreement with the observed cr energy spectrum. the details of acceleration mechanism and propagation of cosmic rays at higher energies are not completely understood. an important open item is the presence of antimatter in the radiation. equal amounts of matter and antimatter should have been produced at the beginning of the universe. the fact that there seems to be only matter around us is one of the major open problems in cosmology and in particle physics. the antiprotons, as well as the positrons, are a component of the cosmic radiation being produced in the interaction between crs and the interstellar matter. being exactly the same as particles except for their opposite charge sign, antiparticles are readily distinguished as they bend in opposite directions in magnetic field. magnetic spectrometers provide a clear and simple particle/antiparticle separation and probe the existence of antimatter in our galaxy. figure 3: the positron ratio measured by the pamela, fermi and ams-02 as presented in the first public presentation of ams-02 results. the expectation from the production of positrons as secondary particles is shown as dashed line. the discrepancy below 10 gev is explained by different phases of solar activity when data were collected. from http://ams.cern.ch/ an important feature in the e+ spectrum was observed by the pamela satellite and confirmed with the high precision measurement of ams-02. launched in 2011, the ams-02 experiment started immediately to take date on the international space station (iss). it is the largest particle physics detector never carried outside the earth atmosphere. the first results were presented in april, 2013 and refer to the measurement of positron in the crs. the e+ fraction in the e− + e+ flux found in the cosmic radiation increases steadily be14 γ-rays, ν’s and particle astronomy as messengers of the universe tween 10 gev to ∼ 250 gev, see fig. 3. at energies above 250 gev, the spectrum appears to flatten but to study the behavior at higher energy more statistics is required. the positron fraction spectrum exhibits no spatial anisotropy, structures or time dependence. these measurements have stimulated a large debate, as they cannot in fact be understood by models describing the production of secondary crs during propagation in the galaxy (see dashed line in fig. 3). several explanations have been proposed to interpret the observed excess: an astrophysical origin, such as nearby pulsars or microquasars, or exotic sources, as for instance the annihilation of dark matter particles in our galaxy. the p/p ratio (∼ 10−5 ÷ 10−4) shows that the antiproton flux is in overall agreement with a pure secondary component: antiparticles are produced during the interaction of crs with the interstellar matter. on the contrary, the ratio e+/e− ∼ 0.1 seems indicate that most of the detected electrons are of primary origin. due to energy loss processes, the majority of he electrons must be originated by sources closer than a few hundred pc. he electrons really probe cr production and propagation in the nearby region of our galaxy. in the next years, the ams-02 experiment will undoubtedly be the leading experiment for a systematic study of the crs through direct measurements, for the searches of antimatter in space, and for the searches for particles originated by dark matter annihilations. 3 high energy γ-rays he astrophysical processes producing relativistic particles are in most cases associated with the production of γ-rays in a wide range of energies. starting from the egret satellites in the ’90th, a new window has been opened in the observation of photons above ∼ 100 mev 1. the egret catalog consists of about 270 galactic and extragalactic objects. the present generation of space-based gamma ray telescopes, agile and lat, has opened a new era with thousands of galactic and extragalactic sources. the large number of sources and the high data quality are producing a deeper insight into the understanding of the processes of acceleration and radiation of non-thermal particles in the universe at sub-tev energies. as the flux of γ-rays decreases with increasing energy, space-based observations of most sources are limited to less than 100 gev. gamma-rays above 100 gev 2 are detected on ground, using extensive air shower (eas) particle detectors or the imaging atmospheric-cherenkov technique (iact). tev γ-rays are absorbed when reaching the earth atmosphere, and the absorption process proceeds by creation of a cascade of secondary particles. these emit cherenkov radiation, at a characteristic angle in the visible and uv range, which passes through the atmosphere. as a result of cherenkov light collection by a suitable mirror in a camera, the showers can be observed on the surface of the earth. the comparisons between the main features of space-based, iacts, eas and neutrino telescopes (§4) are presented in table 1. table 1: characteristic of space-based, iacts, eas and neutrino telescopes. from the top raw: energy range; effective area; the background rejection power; the angular and energy resolutions; the characteristic aperture of the telescopes; the duty cycle. space iact eas ν-tel energy (tev) 10−4-0.3 0.5-100 0.5-50 1-1000 area (m2) 1 104 104 0.1-300 bck rejec. > 99% > 99% 95% 99% angular resol. 0.5◦ 0.05◦ 0.7◦ 0.5◦ ∆e/e 10% 15% 50% 40% aperture (sr) 2.7 0.003 1.8 2π duty cycle 85% 10% 95% 95% 3.1 he γ-rays on satellites the large area telescope (lat) on the fermi satellite (launched in june 2008) is a γ-ray detector designed to distinguish photons in the energy range 20 mev to more than 300 gev from the high background of energetic charged particles. the γ-ray sky (unlike at other wavelengths) is strongly dominated by diffuse radiation originating in our galaxy by cr interactions with the interstellar gas and photon fields through the processes of inelastic nucleon scattering, bremsstrahlung, and inverse compton scattering. the lat mapping of the galactic γ-rays offers a way to derive information about the spatial distribution of crs and matter. the second catalog of high-energy γ-ray sources (2fgl) detected by the lat (nolan p.l. et al., 2012) derives from data taken during the first 24 months of the science phase of the mission, which began on 2008 august 4. the 2fgl catalog contains 1873 sources detected and characterized in the 100 mev to 100 gev. it includes source location regions, energy dependence of the flux in terms of a power-law with an exponentially cutoff and light curves on monthly intervals for each source. among the 1873 sources, 127 are firmly identified and 1171 reliably associated with counter1we indicate with he γ-rays the photons between 0.02-100 gev 2we indicate with vhe γ-rays the photons between 100 gev-100 tev 15 maurizio spurio parts of known or likely γ-ray producing source classes, see fig. 4. agn, and in particular blazars, are the most prominent class of associated sources: 917 sources are associated, of which 894 are blazars, 9 are radio galaxies, 5 seyfert galaxies. normal galaxies are now established as a class of γ-ray emitters and 7 2fgl sources are associated with such objects. pulsars have been traditionally studied through radio astronomy methods, with about 1800 pulsars found beaming radio waves. however, most of their radiation (a few percent of their spin-down power) is emitted at high-energies. in the last few years, the number of pulsars detected in the γ-ray has increased from half a dozen to more than 150 thanks to the agile satellite and the fermi-lat. among the pulsar, the crab plays a fundamental role, as it is the strongest γ-ray source in our field of view. the crab was since recently thought to be a steady source of radiation, from optical to tev energies. agile unexpected has discovered in 2010 (tavani et al., 2011) strong and rapid γ-ray flares from the crab nebula over daily timescales. this observation have changed the understanding of this cosmic object, and challenged emission models of pulsar wind and particle acceleration processes. pulsed γ-ray emission above 100 gev and up to 400 gev was recently detected from the crab with the veritas and magic iacts. figure 4: fermi-lat 2fgl full sky map (top) and blowup of the inner galactic region (bottom) showing sources by source class. identified sources are shown with a red symbol, associated sources in blue. about 70 sources of the 2fgl catalog are associated with pulsar wind nebulae. supernova remnants are a special class because a substantial number of the known objects are sufficiently extended to be potentially resolved with the lat. these objects are particularly interesting because they can represent regions of cr acceleration. in total, twelve sources in the catalog are modeled as spatially extended. 3.2 vhe γ-rays at ground one of the most recent and remarkable achievements in astrophysics is the discovery of more than 110 galactic and extragalactic sources of vhe radiation (see for a review rieger et al., 2013). at present, seven shell-type snrs have been firmly identify as vhe γ-ray emitters the pioneering ground based γ-ray experiment was built by the whipple collaboration. during the last decade, several ground-based γ-ray detectors were developed, both in the north and south earth hemisphere. at present, the new generation apparatus are the h.e.s.s. and veritas telescope arrays and the magic telescopes. these iacts have produced a catalogue of tev γ-ray sources which is continuously updated and available at http://tevcat.uchicago.edu/. electron can produce he γ-rays through the socalled leptonic model. synchrotron radiation from radio to the x-ray band is originated by accelerated electrons moving in the source magnetic fields. these particles can also produce gev-tev γ-rays through inverse compton scattering on the produced radiation field, or on external radiation fields. therefore, measurements of the synchrotron x-ray flux from a source can constrain the predictions on the accompanying γ-rays produced in leptonic processes. accelerated hadrons could either produce γ-rays via interaction with ambient matter or photon fields with sufficient high density. in this case, γ-rays are produced by the decay of neutral mesons while ν’s are produced by the decay of charged mesons. this γ-rays and neutrino production refer to a so-called astrophysical hadronic model. in this framework, the energy spectrum of secondary γ and ν particles follows the same power law of the progenitor crs. both the leptonic and the hadronic models, or a combination of them, could provide an adequate description of the present experimental situation. if high energy photons are produced in the hadronic models, high energy neutrinos will be produced as well. most of observed tev γ-ray galactic sources have a power law energy spectrum e−αγ , where αγ ∼ 2.0÷ 2.5. the values of the spectral index are very close to the expected spectral index of cr sources, αcr. this lead to the conclusion that sources of tev γ-rays can also be the sources of galactic crs. 16 γ-rays, ν’s and particle astronomy as messengers of the universe 4 neutrino astrophysics the main detection signatures for neutrinos in a neutrino telescope (see chiarusi & spurio, 2010) are long, straight tracks and approximately spherical cascades. the former are created by neutrino-induced muons while the latter are produced by neutrino-induced electromagnetic and/or hadronic showers. charged particles emit cherenkov light. from the measured arrival time of the cherenkov light, the direction of the neutrino can be derived. the accurate measurement of the νµ direction (up to 0.3o in water) could allows the association with (known) sources. because the mechanisms that produce crs can produce also neutrinos and γray, potential neutrino sources are in general also γ-ray emitters. due to the production mechanism (eq. 2), the flavor ratio at sources is νe : νµ : ντ = 1 : 2 : 0, which is changed by the neutrino oscillations to 1 : 1 : 1 on earth. figure 5: neutrino telescopes searches for an excess of events over the irreducible background of atmospheric neutrinos. the points represent the measurements of atmospheric νµ spectrum by three telescopes. the red curve represent the still unmeasured contribution of prompt neutrinos from charmed mesons decay. the green lines are the waxman& bahcall (1999) upper bound from diffuse flux of neutrinos from extragalactic sources. the blue line the possible contribution of ν from the gzk effect. some of the most promising candidate neutrino sources in our galaxy are extremely interesting, due to the recent results from tev γ-ray detectors. a neutrino telescope in the mediterranean sea is looking at the same southern field-of-view as the h.e.s.s. including the galactic center. the small interaction cross section of neutrinos allows them to come from far away, but it is also a drawback, as their detection requires a large target mass. assuming the present boundaries arising from γ-rays sources, the challenge to detect galactic neutrinos is open for a multi kilometer-scale apparatus, see fig. 5. also the extragalactic crs-neutrinos connection sets the scale of the detectors to 1 km3. icecube (http://icecube.wisc.edu/) is a 1 km3-scale neutrino detector buried in the antarctic ice. it comprise 86 strings, with 5160 photomultiplier tubes (pmt). each string includes 60 digital optical modules. the deepcore infill array to icecube reduces the energy threshold of icecube to energies as low as 10 gev. in water the antares collaboration (ageron et al, 2011) has completed in 2008 the construction of the largest neutrino telescope (∼ 0.1 km2) in the northern hemisphere. galactic sources. although much smaller than icecube, antares is advantaged by its geographical location for the study of galactic sources. to give a figure of merit, the tev photon flux from a possible neutrino candidate source as rx j1713.7-3946 is e2 γφγ ' 10−11 tev cm−2 s−1. assuming the same flux from neutrinos and no he cutoff, few events/year are expected in a 1 km3 telescope over the background of atmospheric neutrinos in a ∼ 1◦ search cone. the sensitivity of antares for 1000 days of livetime is ∼ e2 νµφsensνµ ' (3 − 8) × 10−11 tev cm−2 s−1 in the declination range from δ = −90◦ to +43◦. in total 51 possible neutrino sources have been studied. none of them shows a significantly excess of tev events over the expected background. figure 6: expected neutrino spectra from full numerical neucosma (red) and simply analytic guetta (blue) models. limits on these predictions are shown in the energy ranges where 90% of the flux (dashed lines) is expected. the icecube limit on the neutrino emission (black dashed) is based from 300 grbs. the antares limit on 296 grbs (red dashed) takes into account the neutrino oscillation effect. ν from grbs. gamma-ray bursts (grbs) are short and very intense flashes of he γ-rays, which occur unpredictably and isotropically over the sky. in model describing the γ-ray emission, protons can also be shockaccelerated, yielding secondary emission of he ν’s accompanying the electromagnetic signal. the detection of neutrinos in coincidence with a grb would be unambiguous proof for hadronic acceleration in cosmic sources. 17 maurizio spurio fig. 6 shows the result from these searches. the stringent icecube limit (black dashed line, abbasi et al., 2012) was a factor of 3.7 below the predictions made using the guetta et al. (2004) model (blue line in fig. 6), creating tension between the nonobservation of a signal and the prevailing models for neutrino emission from grbs. this could either indicate the need for rejection of these models or for more detailed modeling of the neutrino emission. the ν prediction from an advanced numerical calculation of grb (neucosmahümmer et al., 2012), including the full photohadronic interaction cross-section, independent losses of secondary particles, and flavor mixing, is shown as read line. the new predicted flux is about an order of magnitude below than the previous analytic approach, and thus it is still compatible with the limit as published by icecube. figure 7: declination vs reconstructed energy of the he cosmic neutrino candidates in the icecube detector (whitehorn at wipac 2013) diffuse he neutrinos. recently icecube reported on the observation of two he particle shower events discovered in a search for pev neutrinos (aartsen et al., 2013). these events (reconstructed as downward going) are of much higher energy than expected from the background of atmospheric neutrinos, fig. 5. stimulated by these two events, almost during the same time of this frascati workshop, the icecube announced the results of a dedicated search for downward going neutrino-induced events in a restricted fiducial volume. here, 28 events (7 muon-like and 21 shower-like) were discovered, with an expected background of 12.1 events (from atmospheric and prompt neutrinos, and atmospheric muons). the distribution of the declination and deposited energy for these events is shown in fig. 7. the collaboration asserts that the events seems to be neutrinos, with flavor ratios consistent with the expected 1 : 1 : 1 and compatible with an isotropic flux. 5 conclusions multimessenger astrophysics becomes more and more important to obtain a complete picture of non-thermal processes in the universe. this program can be achieved by combining pieces of information from all three messengers: photons, charged crs and ν’s. the implications extend from the origin of crs to the origin of dark matter, from processes of acceleration of particles by strong shock waves to the magnetohydrodynamics of relativistic jets, from distribution of matter in the interstellar medium to the intergalactic radiation and magnetic field distributions. the strong impact of he and vhe γ-rays discoveries on several topical areas of modern astrophysics and cosmology are recognized and of fundamental importance for the astronomical communities. in the near future, the role of ams-02 is of overwhelming importance for direct measurement of crs. finally, the recent multi-tev excess of neutrino events may be a first hint of an astrophysical he neutrino flux, opening the field of neutrino astronomy for the next decade. references [1] aartsen m.g. et al., 2013. accepted by prl [2] abbasi, r. et al.: 2012, nat, 484, 351 doi:10.1038/nature11068 [3] ageron, m. et al.: 2011, nim a, 656, 11 doi:10.1016/j.nima.2011.06.103 [4] blümer j. et al: 2009, prog.part.nucl.p. 63, 293 doi:10.1016/j.ppnp.2009.05.002 [5] chiarusi t, spurio m.: 2010, epj. c65, 649 [6] guetta, d. et al.: 2004, astr. phys., 20, 429 doi:10.1016/s0927-6505(03)00211-1 [7] hillas a. m.: 2005, j. phys. g 31, 39. doi:10.1088/0954-3899/31/5/r02 [8] hümmer, s. et al.: 2012, prl 108, 231101 doi:10.1103/physrevlett.108.231101 [9] nolan p.l. et al.: 2012 apjs 199 31 doi:10.1088/0067-0049/199/2/31 [10] rieger f.m. et al.:arxiv:1302.5603 [11] tavani m. et al.: 2011, science vol. 331 doi:10.1126/science.1200083 [12] waxman e., bahcall j.: 1999, prd59:023002 18 http://dx.doi.org/10.1038/nature11068 http://dx.doi.org/10.1016/j.nima.2011.06.103 http://dx.doi.org/10.1016/j.ppnp.2009.05.002 http://dx.doi.org/10.1016/s0927-6505(03)00211-1 http://dx.doi.org/10.1088/0954-3899/31/5/r02 http://dx.doi.org/10.1103/physrevlett.108.231101 http://dx.doi.org/10.1088/0067-0049/199/2/31 http://dx.doi.org/10.1126/science.1200083 γ-rays, ν’s and particle astronomy as messengers of the universe discussion arnon dar: concerning the icecube events, the quoted error on the atmospheric neutrino background seems to be very small. maurizio spurio: in my opinion the main uncertainty could arise not from atmospheric neutrinos, but from the vetoing efficiency estimate for surviving atmospheric muons. there are some peculiarity of the events which are intriguing and only a detailed publication can clarify. for instance, the fact that (after background subtraction) the muon neutrinos are fewer than the expected from the quoted 1 : 1 : 1 ratio; that a cutoff energy at ∼1 pev should be present; that the upgoing signal (4 events) is compatible with the background (3 events). for these reasons, if there is no underestimated contamination from atmospheric muons, the signal seems to be more likely of galactic origin than diffuse extragalactic. 19 introduction crs and antimatter high energy -rays he -rays on satellites vhe -rays at ground neutrino astrophysics conclusions 107 acta polytechnica ctu proceedings 2(1): 107–110, 2015 107 doi: 10.14311/app.2015.02.0107 broad-band variability in accreting compact objects s. scaringi1,2 1instituut voor sterrenkunde, k.u. leuven, celesijlaan 200d, leuven, belgium 2max planck institute fur extraterrestriche physik, d-85748 garching, germany corresponding author: simo@mpe.mpg.de abstract cataclysmic variable stars are in many ways similar to x-ray binaries. both types of systems possess an accretion disk, which in most cases can reach the surface (or event horizon) of the central compact object. the main difference is that the embedded gravitational potential well in x-ray binaries is much deeper than those found in cataclysmic variables. as a result, x-ray binaries emit most of their radiation at x-ray wavelengths, as opposed to cataclysmic variables which emit mostly at optical/ultraviolet wavelengths. both types of systems display aperiodic broad-band variability which can be associated to the accretion disk. here, the properties of the observed x-ray variability in xrbs are compared to those observed at optical wavelengths in cvs. in most cases the variability properties of both types of systems are qualitatively similar once the relevant timescales associated with the inner accretion disk regions have been taken into account. the similarities include the observed power spectral density shapes, the rms-flux relation as well as fourier-dependant time lags. here a brief overview on these similarities is given, placing them in the context of the fluctuating accretion disk model which seeks to reproduce the observed variability. keywords: cataclysmic variables x-ray binaries optical timing photometry individual: mv lyrae individual: lu cam. 1 introduction cataclysmic variables (cvs) are close interacting binary systems where a late-type star transfers material to a white dwarf (wd) companion via roche lobe overflow. with an orbital period ranging from hours to minutes, the transferred material from the secondary star forms an accretion disc surrounding the wd. as angular momentum is transported outwards in the disc, material will approach the innermost regions close to the wd in the absence of strong magnetic fields, and eventually accrete on to the compact object. x-ray binaries (xrbs) are also compact interacting binaries which are similar to cvs in many ways, but where the accreting compact object is either a black hole (bh) or a neutron star (ns). both cvs and xrbs, as well as active galactic nuclei (agn; accreting supermassive bhs), have been shown to display strong aperiodic variability on a broad range of time-scales as well as in different wavelength ranges. xrbs have shown variability ranging from milliseconds to hours, whilst for cvs this ranges from seconds to days. this difference can be mainly attributed to the fact that the innermost edges of the accretion discs in cvs sit at a few thousand gravitational radii, whilst for xrbs it can reach down to just a few gravitational radii. the fact that material can get deeper within the gravitational potential of xrbs, as compared to cvs, also explains why they are more luminous and emit predominantly in x-rays, compared to cvs, which emit predominantly at optical/uv wavelengths. aperiodic broad-band variability (also referred to as flickering) has extensively been studied in x-rays for xrbs over several decades in temporal frequency (see for example terrell 1972; van der klis 1995; belloni et al. 2000; homan et al. 2001; belloni, psaltis & van der klis 2002). as cvs emit mostly at optical/uv wavelengths, timing studies of these objects had to rely on optical observing campaigns from earth, which are inevitably hindered by large interruptions, poor cadence, and in many cases poor signal-to-noise ratios. furthermore, the key time-scales to probe in cvs are much longer than in xrbs, requiring long, uninterrupted observations. recently, cv timing studies have been facilitated thanks to the advent of the kepler satellite (gilliland et al. 2010; jenkins et al. 2010), which is able to provide long, uninterrupted and high-precision light curves in the optical light from space. thanks to these capabilities it is now possible to probe over four orders of magnitude in temporal frequency in cvs. more importantly, it is now possible to compare the aperiodic variability properties observed in xrbs to those 107 http://dx.doi.org/10.14311/app.2015.02.0107 s. scaringi observed in cvs after taking into account the relevant timescale and wavelength “translations”. 2 broad-band aperiodic variability in accreting white dwarfs one important discovery relating the flickering properties observed in cvs to those observed in xrbs has come from studying the kepler lightcurve of the nova-like cv mv lyrae displaying typical flickering behaviour as observed in other cvs. specifically, scaringi et al. 2012a have reported the discovery of the so-called rms(root-mean-square)-flux relation within the kepler lightcurve of mv lyrae, where the rms-variability power linearly correlates with the mean cont rate of the source. this relation has been previously observed in a number of xrbs and agn (uttley & mchardy 2001; uttley et al. 2005), and, together with the observed log-normal flux distributions, rules out simple additive processes as the source of flicker noise (e.g. superposition of many independent shots), and instead strongly favours multiplicative processes (e.g. coupling of masstransfer variations travelling from the outer to inner disc for the latter) as the source of variability. more importantly, the fact that very similar rms-flux relations are found within all different types of accreting compact objects (bhs, nss, wds) on all scales strongly suggests that the driving mechanism responsible for the observed aperiodic variability is the same in all systems, irrespective of mass, size or type. additionally to displaying the rms-flux relation, scaringi et al. 2012b have reported that the power spectral density (psd) of mv lyrae is also qualitatively similar to those observed at x-ray wavelengths in xrbs. specifically, all psds display single or multiple quasi-periodic osscillations (qpos) as well as a high frequency break. both the psds of xrbs and cvs can be qualitatively modelled with a combination of lorentzian shaped functions, with the main difference arising from the characteristic frequencies involved. for example, xrbs display aperiodic variability on a wide range of timescales with high-frequency breaks at ≈ 100 − 101 hz (belloni et al. 2005), whilst cvs display very similar psd, but scaled to lower frequencies such that the high frequency break occurs at ≈ 10−3 hz. the difference between the psds in xrbs and cvs can be mainly attributed to the fact that material within the accretion disk can fall deeper within the embedded gravitational potential well of xrbs as opposed to cvs. this will result in xrbs displaying variability on shorter timescales than in cvs, and furthermore, will result in xrbs emitting most of their radiation at x-ray wavelengths as opposed to cvs emitting mostly at optical/uv wavelengths. 3 fourier-dependent time-lags in cvs similarities between the flickering properties of xrbs and cvs are not only limited to single-band observations. it has been known for over a decade that xrbs display high levels of coherence between two simultaneously observed x-ray lightcurves in different energy bands (vaughan & nowak 1997; nowak et al. 1999). associated to this, fourier-dependent time-lags are also observed at x-ray wavelengths, where hard xray photons are delayed with respect to the soft photons, with larger delays at the lowest temporal frequencies (known as hard lags). a natural explanation for hard lags in xrbs comes from the fluctuating accretion disk model (see arevalo & uttley 2006 and references therin), where the coupling of fluctuations in the mass-transfer rate at different accretion disk radii is responsible for the observed variability. as matter propagates from the cooler outer regions of the disk towards the hotter inner ones, the observed variability in two different energy bands will be delayed with respect to each other as a result of the temperature gradient in the accretion disk and fluctuations moving inwards. using the ultracam instrument (dhillon et al. 2007) mounted on the 4.2 meter william herschel telescope, scaringi et al. 2013 have obtained simultaneous optical lightcurves in the u′, g′ and r′ bands on the two nova-like systems mv lyrae and lu cam. the results from this observing campaign show that both systems display soft lags (where blue photons are observed before the red ones) at the lowest observed frequencies, with larger lags at low frequencies. soft-lags have also been observed at x-ray wavelengths in xrbs, as well as agn, and have been explained as photoionising reflection of hard-x-ray photons originating from the inner regions of the disk (possibly the corona) onto the outer regions. in this case, the lag delay would be the lighttravel time from the emitting region to the reflecting region. the soft lags observed in scaringi et al. 2013 are however too large (on the order of ≈ 10 seconds for lu cam) to be explained by light-travel time delay. nevertheless, it might still be that photons from the hot inner regions are being reprocessed by the cooler outer disk, possibly on the thermal timescale. 4 a physical model for the flickering variability the observed flickering properties in xrbs have been modelled in the context of the fluctuating accretion disk model (see arevalo & uttley 2006 and references therin). ingram & done (2011,2012) have shown how this model can be successfully applied to reproduce the observed psd shapes in xrbs. in the most recent at108 broad-band variability in accreting compact objects tempt by ingram & van der klis (2013), the authors have demonstrated how the model can be implemented analytically (rather than numerically), thus reducing the computation time of specific models from hours to seconds. in scaringi 2013 a simplification of the ingram & van der klis (2013) model has been applied to the kepler lightcurve of the cv mv lyrae by removing general relativistic effects which are negligible in accreting wds. the model prescription employed allows to fit the high-frequency psd of mv lyrae by associating the observed flickering to the viscous timescale at specific disk radii. assuming the accretion disk extends all the way to the wd surface, the model allows to fit for the disk outer edge, as well as for α(h/r)2, where α is the viscosity parameter and h/r the disk scale height (shakura & sunyaev 1973). a qualitatively good fit to the data is achieved (with reduced χ2 ≈ 1.2). the model parameters resulting from the fit are displayed in table 1, and suggest that the observed high-frequency flickering is driven by a geometrically thick disk extending from r ≈ 0.12r� all the way to the wd surface. table 1: best-fit parameters with associated (1σ) errors for the fluctuating accretion disk model applied to the kepler lightcurve of mv lyrae (scaringi 2013). mwd(m�) ≡ 0.73 rin(r�) ≡ 0.0105 rout(r�) 0.117+0.029 −0.020 γ 0.853+0.047 −0.041 α(h/r)2 0.705+0.289 −0.182 fvar 0.220+0.001 −0.001 although the observed emission at optical wavelengths in cvs is though to originate from a cold, geometrically thin outer disk, the results from this analysis seem to suggest that the flickering is driven by a geometrically thick inner disk. it is thus possible that the geometrically thin outer disk is reprocessing photons from the geometrically thick inner one, allowing to explain the inferred results. similar geometric configurations have also been inferred in xrbs. both x-ray timing and spectral analysis suggest that geometrically thick disk exists close to the compact object (optically thin, referred to as the corona), possibly sandwiching the geometrically thin, optically thick disk. if a similar configuration is confirmed in cvs, then it is possible that the physics responsible for generating the inner geometrically thick disks in cvs might be the same as that in xrbs. 5 conclusion both cvs and xrbs, as well as agn, are observed to display aperiodic broad-band variability. this variability can be associated to the accretion disks in these systems. as the accretion disks in xrbs can fall much deeper within the embedded gravitational potential well as opposed to cvs, most of their emission will occur at x-ray wavelengths as opposed to optical/ultraviolet. furthermore, the timescales associated with the disk inner edge are a few orders of magnitude higher in temporal frequency than those of cvs. here, a brief overview of the broad-band variability properties observed in cvs has been presented. in particular, the aperiodic properties discussed (psd shapes, rms-flux relations and fourier-dependent time-lags) are in many ways similar to those observed at x-ray wavelengths in xrbs once the relevant temporal scaling has been taken into account. the fluctuating accretion disk model which seeks to explain the observed variability in xrbs has also been briefly discussed in the context of cvs. this model associates the observed variability to the viscous timescale at specific disk radii. in this respect, applying this model to the kepler lightcurve of the nova-like cv mv lyrae suggests the existence of a geometrically thick disk close to the wd responsible for driving the observed high-frequency flickering. acknowledgement the author wishes to acknowledge funding from the fwo pegasus marie-curie fellowship program, as well as useful and insightful discussions with christian knigge, elmar koerding, phil uttley and tom maccarone. references [1] terrell 1972: apj, 174, l35. [2] van der klis 1995: x-ray binaries. cambridge: cambridge univ. press; 1995. p. 252. [3] belloni et al. 2000: a&a, 355, 271. [4] homan et al. 2001: apjs, 132, 377. doi:10.1086/318954 [5] belloni et al. 2002: apj, 572, 392. [6] gilliand et al. 2010: apj, 713, l160. [7] jenkins et al. 2010: apj, 713, l87. doi:10.1088/2041-8205/713/2/l87 [8] scaringi et al. 2012a: mnras, 427, 3396. doi:10.1111/j.1365-2966.2012.22022.x [9] uttley & mchardy 2001: mnras, 323, l26. [10] uttley et al. 2005: mnras, 359, 345. doi:10.1111/j.1365-2966.2005.08886.x 109 http://dx.doi.org/10.1086/318954 http://dx.doi.org/10.1088/2041-8205/713/2/l87 http://dx.doi.org/10.1111/j.1365-2966.2012.22022.x http://dx.doi.org/10.1111/j.1365-2966.2005.08886.x s. scaringi [11] scaringi et al. 2012b: mnras, 421, 2854. doi:10.1111/j.1365-2966.2012.20512.x [12] belloni et al. 2005: a&a, 440, 207 [13] vaughan & nowak 1997: apj, 474, l43. [14] nowak et al. 1999: apj, 510, 874. [15] lyubarskii 1997: mnras, 292, 679. [16] kotov 2001: mnras, 327, 799. [17] arevalo & uttley 2006: mnras, 367, 801. [18] dhillon et al. 2007: mnras, 378, 825. [19] caastella et al. 2012a: mnras, 422, 2407. [20] cassatella et al. 2012b: mnras, 427, 2985. doi:10.1111/j.1365-2966.2012.22021.x [21] de marco et al. 2013: mnras, 431, 2441. doi:10.1093/mnras/stt339 [22] scaringi et al. 2013: mnras, 431, 2535. doi:10.1093/mnras/stt347 [23] ingram & done 2011: mnras, 415, 2323. [24] ingram & done 2012: mnras, 419, 2369 doi:10.1111/j.1365-2966.2011.19885.x [25] ingram & van der klis 2013: mnras, 434, 1476. doi:10.1093/mnras/stt1107 [26] scaringi 2013: mnras, 438, 1233 [27] shakura & sunyaev 1973: apj, 24, 337. [28] narayan & yi 1994: apj, 428, 13. [29] fender et al. 2004: mnras, 355, 1105. discussion linda schmidtobreick: for nls we see a difference in the spectra between low and high inclination systems. low inclination systems show balmer absorption, possibly from an inner optically thick accretion disk which might coincide with your geometrically thick inner disk. does one see a similar relation of the presence of high frequency flickering with inclination? simone scaringi: the current model has only been applied on one system at the moment (mv lyrae, low inclination). future applications of the model on other systems will be able to determine whether the high frequency flickering displays different properties as a function of inclination. solen balman: how do you get an optically thick disk out of α(h/r)2 = 0.7? if α = 0.1 the disk is hot and it is no longer optically thick! simone scaringi: the inference of α(h/r)2 = 0.7 from the modelling of the psd in mv lyrae does not suggest that the disk is optically thick. it might well be that the inner region of the disk inferred here are optically thin as suggested. raymundo baptista: is you α constant with radius? simone scaringi: in the current model prescription α is kept as a constant with radius. however, it is more physical and realistic to allow α to have a radial dependence. this will be explored with the current model in the future. 110 http://dx.doi.org/10.1111/j.1365-2966.2012.20512.x http://dx.doi.org/10.1111/j.1365-2966.2012.22021.x http://dx.doi.org/10.1093/mnras/stt339 http://dx.doi.org/10.1093/mnras/stt347 http://dx.doi.org/10.1111/j.1365-2966.2011.19885.x http://dx.doi.org/10.1093/mnras/stt1107 introduction broad-band aperiodic variability in accreting white dwarfs fourier-dependent time-lags in cvs a physical model for the flickering variability conclusion acta polytechnica ctu proceedings doi:10.14311/app.2017.11.0035 acta polytechnica ctu proceedings 11:35–38, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app level crossing safety in the czech republic martin kobosil∗, jan novák ctu in prague, department of forensic experts in transportation, horská 3, 128 03 prague 2, czech republic ∗ corresponding author: kobosmar@fd.cvut.cz abstract. this paper describes safety threats at level crossings according to the different type of security equipment. initially were explored statistical data, which consist of numbers of level crossings classified by crossing type and numbers of traffic accidents on level crossings. afterwards paper describes specific problems of each individual level crossing type. specifically their causation and consequences, which are being discussed between professional and general public. in conclusion paper describes possible solutions to these problems leading to reducing risks at level crossings. at first is mentioned the statistics number of crossing and number of accidents on the crossing. then paper describes specific problems, which are discussed in professional and general public. they are also solutions of this problems, which brings another point of view and search the actual causes. keywords: railway, level crossing, active safety, visibility splays . 1. level crossings safety in numbers we can classify railway level crossing according to the different type of security equipment. on the 31th december 2016 was in the czech republic total number of 7,961 level crossings. 3,938 of them was equipped only with warning cross (w. cross). on these 49.5 percent of all level crossings it depends only on driver’s decision whether he will enter crossing or not. this decision is based on the level of an attention, driver’s experiences and especially on visibility splays. remaining 4,023 level crossings was secured by on type of an active security equipment. 2,356 of which was equipped with warning lights (w. lights), 1,310 level crossings was equipped with warning lights accompanied by automatic barriers (w. lights with a.b.) and 326 level crossings was equipped with mechanically operated barriers (mech. o.b.). the last 31 level crossings had some other form of protection [1]. 1.1. level crossings accidents rules about how to behave on level crossings are well known. they have been established by the law, taught in driving schools and presented in mass media and in primary schools. theoretically, if these rules would be obeyed, there should be no extraordinary incidents. therefore from legal point of view are traffic accidents on level crossings in majority of cases caused by driver. however in terms of prevention it is essential to examine other consequences and to investigate what factors led to the breaking the law. number of traffic accidents on level crossings according to type of security equipment is shown in table 1. 1.2. specific issues of each type of security equipment each type of above mentioned security equipment is different and has typical safety problems. the security equipment accidents killed injur. w. cross 67 4 27 w. lights 85 25 49 w. lights with a.b. 27 14 3 mech. o.b. 1 0 1 total 180 43 80 table 1. number of traffic accidents on level crossings according to the type of security equipment (2014) [2]. vast majority of these issues is linked to active safety. when we will solve them, we will significantly decrease the number of traffic accidents on level crossings and decrease the economic loss from traffic accidents. according to the rail safety inspection in 2013 there was a loss of 37.5 million czech crowns on railway vehicles, 3.7 million crowns on infrastructure and 19.0 million crowns on other participants involved in traffic accidents. to these figures have to be also added society-wide losses from injuries and deaths [2]. 2. level crossings equipped with warning cross main cause of problems on level crossings equipped only by warning cross are undoubtedly visibility splays, which are very often insufficient. owner of the railway has legal obligation to carry out regular maintenance of vegetation and to remove any other obstructions, which negatively impacts on visibility splays. in particular circumstances, where this cannot be achieved, i.e. due to the difficult ground conditions or due to land ownership disputes, it should be installed signalling equipment ideally in combination with crossing barriers. 35 http://dx.doi.org/10.14311/app.2017.11.0035 http://ojs.cvut.cz/ojs/index.php/app martin kobosil, jan novák acta polytechnica ctu proceedings figure 1. vegetation intruding visibility splays on level crossing (source police czech republic). visibility splays are defined in design standard csn 73 6380, which is legally binding on the basis of regulation no. 177/1995 sb. this standard explains how to correctly determine visibility splays, however it has one issue. according to the paragraph no. 88 of this regulation, above mentioned standard csn 73 6380 is not binding for level crossings, which project documentation was approved before this standard came into effect. vast majority of railway was designed and built in the end of the 19th century and in the first half of the 20th century. visibility splays on these older railways are defined by internal regulation of a railway operator szdc s 4/3. calculations are in the principle similar to methods used in design standards and are based on physical principles, however in the end of the regulation s 4/3 it is allowed to reduce visibility splays by half. this statement is based on the theory of probability and enables to reduce visibility splays in the case of a low probability of a collision, which implies on level crossings with low operational speed on the line along with low traffic volumes. however with this statement cannot be agreed either from the scientific view or from the human view. it is essential to respect physical laws and give driver enough time to decision, reaction and for safe crossing of a level crossing [3, 4]. another problem might be complete overlooking of a level crossing, which comprise of two inconspicuous rail tracks across the road. drivers are notified about presence of a level crossing by three traffic signs a31 complemented by warning cross sign a32, but these are only traffic signs, which is nothing unusual in road traffic and can be overlooked. other vulnerable group are drivers, which are familiar with level crossing, but can simply forget about its presence as well as they forget they are daily driving around memorial. solution to this problem has to be something, which is not as common as traffic signs and should be on the road, where driver is concentrating his attention. road markings could be applied as an optical psychological brake v18. in technical specifications tp 65 ”traffic signs manual” is about traffic sign v5 quoted ”additionally it is used on intersection to mark out where vehicle has to stop to give way, in front of the controlled pedestrian crossing and alternatively also in front of the level crossing” [5]. figure 2. level crossing highlighted by optical psychological brake v18 (source mr sachl). 3. level crossings equipped with warning lights severity of traffic accidents on these level crossings is highest from all of the level crossing types due to the higher operational speed on the line. reasons for disrespecting rules on these level crossings can be overlooking of red warning lights or driver’s risky behaviour. visibility splays on these level crossings does not have to be large, because they are used only when security equipment is out of service. basic rule of this security equipment says: ”do not enter the level crossing, when the red light is flashing.” but what is the reason for disobeying this rule? in mass media the reason is often attributed to the aggressive and undisciplined drivers, but the truth could be somewhere else. hardly will anybody drive in front of the moving train because of the curiosity ’if i will make it’ or because of the desire for adrenaline. first problem could be visibility of the warning lights, which does not comply with the selfexplanatory principle. especially dangerous are level crossings in urban areas, where buildings, foliage, traffic signs or other structures are forming longitudinal lines, which may cause overlooking of a warning lights. in this case it is appropriate to mark and highlight transverse lines by using road markings or ’lights bar’, which is placed on the road as can be seen on figure 3. however it is important to keep in mind that every level crossing has to be assessed individually and that solution of this problem requires cooperation of the railway operator and road maintenance provider. second problem with higher level of risk are drivers, which deliberately enters level crossing despite flashing warning lights. this phenomenon can be seen especially at small cities and villages, where local residents 36 vol. 11/2017 level crossing safety in the czech republic figure 3. level crossing highlighted by ’light bar’ and optical psychological brake (source mr skladany). knows, that it usually takes a long time before the train approaches level crossing after the warning light came on. this situation is particularly dangerous for the next people in a row, because human psychology works like ’he made it, so will i’. these people enter the level crossing following the example they have seen and tragedy is near. another problem, which is typical on level crossings oriented to the west or to the east is also sun and its glare. the intensity of warning lights on these crossings should be increased, e.g. by the use of a led technology. 4. level crossings equipped with warning lights accompanied by automatic barriers this is the safest and the most advanced type of level crossing safety equipment. the barriers are lowered across the road, which makes it clear, that it is forbidden to enter the crossing. on these level crossings is caused only a small number of traffic accidents, but when an accident happens it has usually greater consequences. typical and almost only threat on this type of security equipment is called ’s-manoeuvre’ between the half-barriers as shown on figure 4. these drivers are the biggest gamblers with their lifes. from this reason are some level crossings being equipped with enforcement video cameras, which can record and penalise hazardous drivers [6]. second cause of dangerous situation is when driver is closed between the safety barriers. but this mistake does not have to be fatal. first option is that second passenger can raise the barrier or the barrier can be lifted up by the bonnet of a car. barriers are intentionally balanced, that only a minimal strength is required to raise them. second option is breaking the barrier with a car. every barrier is designed to be easily broken by impacting on it in horizontal direction. it is necessary to raise public awareness about figure 4. s-manoeuvre [6]. this subject and to spread these information between road users. this pack of information is necessary to get to the subconscious mind of general public by enlightenment. the another solution consists of installing detection devices, which can detect trapped vehicle on level crossing. this device send information about trapped car and can give appropriate command to warn or to stop approaching train. the main technical problem of this solution is reliability of the vehicle recognition. low reliability can cause many false alarms and many delays of trains. these detecting systems are already successfully used abroad. figure 5. level crossing with vehicular detectors [7]. 5. how to reduce risk on level crossings we can hear from mass media and between professional and general public that it is drivers who makes mistakes on level crossings. this statements is generally correct, because majority of collisions between motor vehicles and railway vehicles has origin in driver errors, but often as an originator of traffic accidents is considered aggressive behaviour of drivers. it is true that many drivers are speeding, tailgating or making other traffic offences, however on level crossings it is usually simple human errors. driver is concentrating on the road in front of him, but on the road he sees 37 martin kobosil, jan novák acta polytechnica ctu proceedings only two inconspicuous lines across the road. just after double swing of a vehicle he realizes it was rail tracks. by lucky chance it ends up with wiping sweat from a forehead, sometimes it ends up tragically. for effective reducing traffic accident numbers on level crossings it is necessary to change an approach in assessing the whole issue and to focus on genuine causes of traffic accidents. it is essential to make every inconspicuous or hazardous level crossing visible. police has to focus on dangerous evading crossing barriers. additionally it is necessary to shut down duplicate level crossings and level crossings with low usage, to build grade separated railway crossings and to take care of visibility splays by maintaining vegetation and removing other obstructions. equally important is raising of public awareness in driving schools and through mass media and various campaigns of safety organisations. references [1] zeleznicni prejezdy v cislech, cit 2017-02-10. operator of the track szdc [online], http://www.szdc.cz/web/ prejezdy/prejezdy-v-cislech.html. [2] statistika nehodovosti na zeleznicnich prejezdech, 2015. the rail safety inspection office. [3] csn 73 6380 zeleznicni prejezdy a prechody, 2014. czech technical standad. [4] s 4/3 internal regulation, 2014. operator of the track szdc. [5] tp 65 "traffic signs manual", 2013. technical manual. [6] zeleznicni prejezdy budou hlidat kamery, cit 2017-02-10. czech television [online], http://www. ceskatelevize.cz/zpravodajstvi-ostrava/zpravy/ 204475-zeleznicni-prejezdy-budou-hlidat-kamery/ l. [7] i. r. p. .-. [online]. ieee railway projects 2015-2016, cit 2017-02-10. http: //ieeerailwayprojects2015-2016.blogspot.cz/. 38 http://www.szdc.cz/web/prejezdy/prejezdy-v-cislech.html http://www.szdc.cz/web/prejezdy/prejezdy-v-cislech.html http://www.ceskatelevize.cz/zpravodajstvi-ostrava/zpravy/204475-zeleznicni-prejezdy-budou-hlidat-kamery/l http://www.ceskatelevize.cz/zpravodajstvi-ostrava/zpravy/204475-zeleznicni-prejezdy-budou-hlidat-kamery/l http://www.ceskatelevize.cz/zpravodajstvi-ostrava/zpravy/204475-zeleznicni-prejezdy-budou-hlidat-kamery/l http://www.ceskatelevize.cz/zpravodajstvi-ostrava/zpravy/204475-zeleznicni-prejezdy-budou-hlidat-kamery/l http://ieeerailwayprojects2015-2016.blogspot.cz/ http://ieeerailwayprojects2015-2016.blogspot.cz/ acta polytechnica ctu proceedings 11:35–38, 2017 1 level crossings safety in numbers 1.1 level crossings accidents 1.2 specific issues of each type of security equipment 2 level crossings equipped with warning cross 3 level crossings equipped with warning lights 4 level crossings equipped with warning lights accompanied by automatic barriers 5 how to reduce risk on level crossings references acta polytechnica ctu proceedings doi:10.14311/app.2017.10.0056 acta polytechnica ctu proceedings 10:56–60, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app design of subsoil improvement below hall floors peter turček∗, monika súľovská stu bratislava, faculty of civil engineering, radlinského 11, bratislava ∗ corresponding author: peter.turcek@stuba.sk abstract. the construction of an industrial park is now being prepared near the town of nitra. the investor fixed very strict conditions for the bearing capacity and, above all, the settlement of halls and their floors. the geological conditions at the construction site are difficult: there are soft clay soils with high compressibility and low bearing capacity. a detailed analysis of soil improvement was made. stone columns were prepared to be fitted into an approximately 5 m thick layer of soft clay. the paper shows the main steps used in the design of the stone columns keywords: engineering geological investigation, soil improvement, gravel columns, decreasing the settlement, consolidation. 1. introduction the construction of an industrial park was prepared near the town of nitra in 2015. difficult geological conditions, created by a layer of soft to firm quaternary clays approximately 5 m in thickness resulted in unfavourable soil characteristics: low bearing capacity and high settlement. for this reason, it was decided to improve the soil properties. following the evaluation of a preliminary engineering geological investigation, an initial design of stone columns was made during detailed investigation works. before the final design, the efficiency of the stone columns was verified by field tests. three test fields for three various improvement technologies were prepared. penetration tests were applied before and 10 days after the stone columns completion. in test field no. 1, stone columns with a diameter of 500 to 600 mm were prepared using the technology of deep vibrating compaction, and filled with gravel of grain size 4/15 mm, 8/32 mm and 4/32 mm. the stone columns were arranged to form a square and triangular grid. in test field no. 2, dynamic compaction combined with stone columns preparation using a nontraditional technology was used for soil improvement. first, a borehole with a diameter of 600 mm was made and filled with gravel of grain size 0/63 mm or 0/90 mm containing low contents of fine particles. soil particles smaller than 0.063 mm formed less than 5 %. the boreholes were not protected by casing pipes; they had to be filled by gravel as soon as possible to avoid the collapse of boreholes. the next step was compaction of the stone column in two phases by 50 hits. the stone columns were spaced within a square and triangular grid with varied distances from each other. in field test no. 3, dynamic consolidation with a weight of 20 t falling in free fall from a height of 10 m was performed. using this technology created craters approximately 2 m in diameter. this squishy space was filled by stones with grain size 0-400 mm. the content of fine soil was very low. the space of compacted columns formed a square and triangular grid with a spacing of more than 5 m. after the evaluation of data from field experiments [1], dynamic consolidation was rejected, because the results had proved this technology improper for application in local geological conditions. also, the settlement of columns produced by dynamic compaction was higher than by the other technologies. as the depth reached by dynamic compaction was not sufficient for the project requirements, this technology was also rejected. field experiments helped to prepare recommendations which became input data for soil improvement. more halls with different floor loading will be constructed in the industrial park in the near future. the paper focuses on the design of soil improvement for uniform floor load intensity of 60 kpa. 2. design of stone columns various connections of columns to other structural layers were analysed before the design of the stone columns. after removing the topsoil, the separation geotextile was put on the ground level. then, a 500 mm thick gravel layer was laid as a base below the embankment. the 500 mm layer was made up of two layers of crushed stone with grain size 0/125 mm compacted to min. id = 0.85. from this working plane, the stone columns were assembled. after they had been completed, the ground surface was levelled and compacted, as needed, to min. id = 0.85 again. the embankment was built on this base layer. its first three layers levelled the non-horizontal terrain. the main part of the embankment was designed from these layers: 200 mm of the bottom layer of crushed stone 0/125 mm, 300 mm of pit-run gravel with small volumes of fine soil (grain size max. 100 mm), then 56 http://dx.doi.org/10.14311/app.2017.10.0056 http://ojs.cvut.cz/ojs/index.php/app vol. 10/2017 design of subsoil improvement below hall floors again 200 mm of crushed stone 0/125 mm and 300 mm of pit-run gravel with small volumes of fine soil (grain size max. 100 mm). the last 800 mm of the embankment were prepared from a 400 mm layer made up of crushed stone 0/63 mm and two 200 mm layers of crushed stone of grain size 4/32 mm. the main reason for using different types of material was the possibility of their delivery to the site. the length of the construction site was 1380 m. a schematic sectional view of improved subsoil is in fig. 1, while fig. 2 presents an overall view of making the stone columns. one part of the construction site will contain halls whose floors will be loaded by 60 kpa. the investor’s requirement for the settlement of the floors was 10 mm. the thickness of the embankment situated on improved subsoil was 1.5 m. based on a parametric study, a raster of stone columns (sc) 1.8 · 1.8 m in a square grid was selected. the average length of the stone columns was 5.5 m. this length resulted from the requirement that the bottom of the columns would extend into the quarternary gravel layer. it was necessary to verify the bearing capacity, settlement and consolidation of the stone columns for the prepared project. the bearing capacity validation manifested great reserve and it will be not be dealt with this paper. a traditional analytical calculation method was applied for the calculation of settlement and consolidation, partly complemented by priebe’s theory for vertical gravel stone columns. 2.1. traditional calculation of settlement and consolidation after the withdrawal of a humus layer, a 0.5 m thick gravel layer would be prepared on the ground. the stone columns would be built from this level. calculations were made for a simulated model area of 20 · 20 m, as there must a reserve left for transport corridors and, if necessary, a free space for technology in the halls. when a stone column with a diameter of 600 mm is made, the cross-sectional area equal to one stone column is a1 = π r2 = π 0.32 = 0.283 m2 (1) using the distribution of the stone columns in a square grid with a distance between the columns of 1.9 · 1.9 m, 27.67 columns will be placed in an area of 10 · 10 m (5.26 columns fit in a line up to 10 m in length, the distance between the rows is 1.9 m and the 10 m section holds 5.26 columns). therefore, the total area of the columns will be ac = a1 · 27.67 = 0.283 · 27.67 = 7.83 m2 (2) the original soil will occupy the area as = 100− 7.83 = 92.17 m2 (3) the following bedrock model was compiled for the area where a hall with a floor loaded by 100 kpa will be placed: • 3.3 m layer of clay of high plasticity with mainly soft consistency; where edef = 3 mpa; eoed = edef/β = 3/0.37 = 8.1 mpa (4) • 1.2 m thick layer of clayey sand with mainly firm consistency; where edef = 5.95 mpa; eoed = edef/β = 5.95/0.62 = 9.6 mpa (5) • 1.0 m thick layer of silty gravel with medium relative density; where edef = 35 mpa; eoed = edef/β = 35/0.74 = 47.3 mpa (6) • tertiary clay with high plasticity and firm consistency was found below silty gravel; where edef = 4 mpa; eoed = edef/β = 4/0.37 = 10.8 mpa (7) the average oedometric modulus value in a 3.3 m thick clay layer was determined using the equation: eoed = e1 ·a1 + e2 ·a2 a1 +a2 = = 166 · 7.83 + 8.1 · 92.17 100 = 20.46 mpa (8) similarly, for the average value of clayey sand the oedometric modulus determined was eoed = 21.85 mpa, for silty gravel eoed = 56.59 mpa and for tertiary clay eoed = 22.95 mpa. the calculation of settlement was made (as described above) for an area of 20 · 20 m. the embankment layer thickness of 1.5 m acts on the surface of the original ground by a stress with an intensity of 1.5 · 20 = 30 kpa. it was anticipated that a soft clay layer 3.3 m thick with clayey sand and tertiary clay would be compressed after improvement by 5.5 long stone columns in a raster of 1.9·1.9 m (fixing the stone columns 1.0 m into the gravel layer was considered). the calculation is processed in tab. 1. in the same way, the settlement due to a uniform surcharge of the floor by 60 kpa was calculated. the expected settlement under this load is s2 = 9.012 mm. the total estimated settlement (embankment + surcharge of the floor) will reach stot = 4.886+9.012 = 13.898 mm. but the magnitude of this settlement needs to be corrected taking into account consolidation, because part of the settlement will occur during the construction time. the calculation of consolidation in a drainage system consists of two parts: consolidation into vertical elements (stone columns) and consolidation into the horizontal permeable subbase. then, using terzaghi’s theory the average degree of consolidation can be expressed as 57 peter turček, monika súľovská acta polytechnica ctu proceedings figure 1. schematic sectional view of improved subsoil. figure 2. overall view on making stone columns. point no. h z z/b i2 σ2 σor m2 · σor eoed s (m) (m) (kpa) (kpa) (kpa) (mpa) (m) 1 1.6 0.80 0.040 0.98 29.4 16 1.6 20.46 0.002174 2 1.7 2.45 0.122 0.85 25.5 49 4.9 20.46 0.001712 3 1.2 3.90 0.195 0.71 21.3 78 7.8 21.85 0.000741 4 1.0 5.00 0.250 0.62 18.6 100 10.0 56.59 0.000152 5 2.8 6.90 0.345 0.52 15.6 138 13.8 47.30 0.000107 6 2.0 9.30 0.465 0.43 12.9 186 18.6 10.80 7 2.0 11.30 0.565 0.38 11.4 226 22.6 10.80 -∑ s1 = 0.004886 table 1. settlement of the embankment (σ = 30 kpa) after improvement by sc in a raster of 1.9 · 1.9 m. explanatory notes: h thickness of the soil layer; z distance between the footing bottom and the point at which vertical stress is calculated; b width of the foundation; i2 coefficient of stress spreading influence; σ2 vertical stress from the foundation at a depth z; σor original vertical stress at depth z; m2 coefficient of structural strength; eoed oedometric modulus of soil; s settlement of the soil layer with a thickness h. 58 vol. 10/2017 design of subsoil improvement below hall floors u = 1− (1− uh) · (1− uv) (9) where: uh degree of consolidation for horizontal dewatering, uv degree of consolidation for vertical dewatering. firstly, the average degree of subgrade consolidation was determined: eoed = ∑ ei · hi∑ hh = 8.1 · 3.3 + 9.6 · 1.2 3.3 · 1.2 = 8.5 mpa (10) in the calculation of consolidation in the vertical direction, the time factor tv was determined: tv = tvkveoed γwh2 = 1.0368 · 107 · 1 · 10−9 · 8.5 0.01 · 4.52 = 0.435 (11) where: tv duration of vertical consolidation 4 months (4 · 30 · 86400 = 1.0368 · 107 s); kv filtration coefficient in the vertical direction (1 · 10−9 m/s); eoed oedometric modulus of soil (8.5 mpa); γw specific gravity of water (0, 01 mnm−3); h thickness of the drainage layer of soil (4.5 m). from terzaghi’s consolidation graph, we obtained the degree of consolidation uv = 83 %. these boundary conditions have been taken into account for the calculation of consolidation in the horizontal direction: de = 1.13 · d = 1.13 · 1.9 = 2.147 (where d is the axial distance of drains). the time factor th for determining the degree of consolidation uh is: th = thkheoed γwd2 e = 1.0368 · 107 · 1 · 10−9 · 8.5 0.01 · 2.1472 = 1.91 (12) where: th duration of horizontal consolidation 4 months (4 · 30 · 86400 = 1.0368 · 107 s); kv filtration coefficient in the horizontal direction (1 · 10−9 m/s); for n = de d1 = 2.147 0.60 = 3.58 ⇒ in this case, auxiliary graphs yielded uh = 99 %. the resulting average degree of consolidation is then u = 1−(1−uh)·(1−uv) = 1−(1−0.83)·(1−0.99) = = 0.9983 ≈ 100 % (13) thus, it can be concluded that as long as the floor is not loaded earlier than 4 months after the completion of embankment bodies, the consolidation below the embankment will be finished. the measurable settlement of the hall structure, therefore, should only be the component induced by the operating load in the hall. the value of this part of settlement is 9.012 mm. 2.2. calculation of settlement using partially priebe’s theory the solution comes from the definition of the equivalent diameter of the cell de. auxiliary magnitudes: equivalent diameter: de = 1.13 · 1.9 = 2.147 m cross sectional area of the stone column: ac = πr2 = π · 0.322 = 0.283 m2 area of a cell with a diameter de: as = πr2 = π · 1.07352 = 3.62 m2 ratio of the column area to the cell area: ac = ac/as = 0.283/3.62 = 0.078 stress in the foundation base of the floor: σ = 60 kpa the basic design parameter is the so-called concentration ratio of stresses n = ec es = 180 3 = 60 (14) where: ec is young’s modulus of the stone column, es is young’s modulus of soil around the stone column. the settlement of subsoil with reinforcement by stone columns is expressed by the parameter β this parameter represents the ratio of the reinforced soil to original soil settlement. the parameter β can be approximately determined using the equation β = 1 1 + (n− 1) · ac = = 1 1 + (60− 1) · 0.078 = 0.1785 (15) the calculation of settlement caused by a 1.5 m high embankment (σ = 30 kpa) without improvement and by the floor followed. the expected settlement of the embankment was s3 = 11.854 mm and the floor settlement due to loading by 60 kpa was s4 = 20.150 mm. then, the total settlement without improvement is stot = 11.854 + 20.150 = 32.004 mm. using priebe’s theory the assumed settlement of the stone columns is reduced to the value s = sn · β = 32.004 · 0.1785 = 5.713 mm (16) comparing both theoretical methods we obtained the difference: 9.012 mm against 5.713 mm. this 59 peter turček, monika súľovská acta polytechnica ctu proceedings difference can be explained in this way: in classical theory medium stiffness of subsoil was assumed, while in priebe’s theory the load is carried by the stone columns to a greater extent. according to both methods, the investor’s requirement was fulfilled: the settlement was less than 10 mm. 3. conclusion the extremely exposed construction of an industrial park near the town of nitra required improving an approximately 5 m thick layer of soft and firm quaternary clays. in the first step, the suitable technology of soil improvement was selected. to this end, a field experiment in a 1:1 scale was carried out. deep vibrating compaction was evaluated as the most suitable technology. in the second step, the design of stone columns spacing was made. the paper shows the procedure of the design of soil improvement below the floors exposed to uniform loading by 60 kpa. after the accomplishment of subsoil improvements of the whole area of the industrial park, the construction of halls started. 4. acknowledgements the paper presents part of the results from a research project supported by the slovak vega agency no. 1/0882/16 “the influence of boundary conditions on limit states of geotechnical structures”. [2] [3] references [1] k. ströhle, a. tomozei. execution of soil improvement in the trial area. construction project jaguar land rower, nitra, slovakia. zt-ströhle, wien, 2015. [2] j. soták, et al. project darwin. final report of detailed engineering-geological investigation (in slovak). tech. rep., tpa, s.r.o. bratislava, 2015. [3] p. turčekm, m. súľovská. rough landscaping and design of subsoil improvement using stone columns in an industrial park near the town of nitra (in slovak). t-g., bratislava, 2015. 60 acta polytechnica ctu proceedings 10:57–61, 2017 1 introduction 2 design of stone columns 2.1 traditional calculation of settlement and consolidation 2.2 calculation of settlement using partially priebe's theory 3 conclusion 4 acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2016.5.0012 acta polytechnica ctu proceedings 5:12–16, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app on operation of 740 metre long freight trains on czech ten-t railway network michal drábek∗, vít janoš, zdeněk michl department of logistics and management of transport, faculty of transportation sciences, ctu in prague, czech republic ∗corresponding author: xdrabek@fd.cvut.cz abstract. regulation (eu) no 1315/2013 defines actual scope of core and comprehensive ten-t network, including both networks for railway freight transport. for the core network, possibility to operate 740 m long freight trains is required. the aim of this paper is to analyse availability of appropriate overtaking tracks for 740 m long freight trains. due to etcs braking curves and odometry, such trains, after etcs implementation, will require 780-800 m long overtaking tracks. for practical reasons (e.g. bypass lines), whole czech railway ten-t network is analysed. the overtaking track, whose occupation means influence on scheduled traffic or threat to boarding passengers, are excluded. the data was collected from station schemes from collection of official requisites for 2015/16 timetable, issued by sždc, czech state infrastructure manager. most of appropriate tracks are over 800 m long, but their density in the network and in particular directions varies considerably. for freight traffic, gradient of the line is important, so in the resulting figure, there are marked significant peaks for particular lines as well. czech ten-t lines are further segmented on the basis of number of tracks and their traffic character. then, specific issues on overtaking or crossing of 740 m long freight trains are discussed. as a conclusion, for long-term development of czech ten-t lines, targeted investment is recommended not only for passenger railway, but also for freight railway. an attractive capacity offer for railway undertakings, which can stimulate freight traffic on european rail freight corridors, can be represented by network-bound periodic freight train paths with suitable long overtaking tracks outside bottlenecks. after the overtaking by passenger trains, a freight train should run without stop through large node station or a bottleneck area. before the sections with high gradients, coupling of additional locomotives should be connected with the overtaking process. next suitable overtaking tracks should be available behind every significant peak of the line. keywords: european freight corridor, long freight train, overtaking track, freight train path, peak . 1. introduction directive 2008/57/ec of the european parliament and of the council of 17 june 2008 on the interoperability of the rail system within the community [1] defines in annex ii infrastructure as a structural subsystem of the rail system, and traffic operation and management as a functional subsystem of the rail system. in the traffic operation and management subsystem, traffic planning is also included. regulation (eu) no 1315/2013 of the european parliament and of the council [2] defines actual scope of core and comprehensive ten-t network, including both networks for railway freight transport. for the core freight railway network, infrastructure requirements are defined. one of them is possibility to operate 740 m long freight trains. regulation (eu) no 913/2010 of the european parliament and of the council of 22 september 2010 concerning a european rail network for competitive freight [3] defined 9 initial rail freight corridors (rfcs) across the eu. according to the regulation, the corridors should provide guaranteed capacity for freight trains – "under good conditions in terms of commercial speed and journey times". the exact scope of each rfc are subject to negotiation by particular member states. three rfcs run directly through the czech republic: rfc 5 baltic-adriatic, rfc 7 orient and rfc 9 czech-slovak. moreover, negotiations about a branch of rfc 8 north seabaltic from germany to ústí nad labem and praha are proceeding. present, as well as planned or negotiated rfcs are displayed in the official presentation of czech ministry of transport by kušnír and ilík [4]. as a result, only few czech ten-t lines of comprehensive network are not included in any present rfc (or negotiated about being included in it). because of possible future changes of rfcs layout, and because of practical need for bypass lines, the whole czech railway ten-t network was included in the analysis. under the term "overtaking track" it is further understood any station track, which does not proceed any railway line in direct direction, i.e., it is not a main station track. for the sake of simplicity, the "not main" station tracks also in single-track lines, which serve mainly for crossing of trains, are referred to as "overtaking tracks". usable length of an overtaking track (further referred to only as "track length") is defined as a distance between last departure main signals, each one for the opposite direction. in the 12 http://dx.doi.org/10.14311/app.2016.5.0012 http://ojs.cvut.cz/ojs/index.php/app vol. 5/2016 on operation of 740 metre long freight trains case of group departure main signals (common for more parallel tracks), or absence of them, distance between last spots is considered, where rolling stock can be located, so that using of neighbouring track by another train is possible. the term "long trains" will be used for freight trains up to 740 m long. the term "long overtaking tracks" will be used for overtaking tracks at least 780 m long. for collection of data on length of overtaking tracks, railway station schemes from sždc (czech state infrastructure manager) collection of official requisites for 2015/16 timetable [5] were used. 2. methods 2.1. rules for determination of available overtaking tracks for 740 m long trains the basic question is, how long overtaking track is sufficient for a 740 m long train. for present czech signalling system and actual sždc regulations on traffic management, a track with additional 12 m length is sufficient. a 10 m distance is required between the locomotive and the departure main signal (in the train direction). the 2 m distance between an insulated gap and the departure main signal for the opposite direction is calculated. brejcha and čech [6] and binko [7] [8], however, state that for the future etcs implementation, a supplementary length of 40 to 60 m to the train length must be added, due to braking curve and inaccuracy of the etcs odometry. on the basis of the facts stated above, the authors have decided to analyse two categories of available long overtaking tracks: • 780 to 799 m long (in figure 1, separate presence of such track or tracks in particular direction is marked in yellow colour) • 800 m long and longer (in figure 1, presence of at least one such track in particular direction is marked in orange colour) presence of the tracks of both categories is marked in orange colour. presence of at least one long overtaking track in particular direction (on the train’s right, which is valid also for single-track lines or sections) is marked by obtuse-angled triangle of particular colour. its obtuse angle lays in direction, which is this track preferably used for. on czech railway network, there is only right-hand operation nowadays. in some recently modernized stations, an amended czech technical standard tnž 34 2620 railway station and line signalling and interlocking systems [9] was implemented. for the through run routes with allowed speed over 120 km/h, if there is no flank protection from the overtaking track and this track is occupied, only "restricted run route" (vco) with maximum speed 100 km/h is allowed. this mandatory function of interlocking systems obviously leads to longer runtime for the fast train than scheduled. so, overtaking of freight trains on vco-affected tracks is not desirable, but not critical. vco-affected long overtaking tracks are marked by pink edge in figure 1. for possible overtaking (or eventual crossing on single-track lines), only such overtaking tracks were considered, that did not lay between any main station track and waiting room (or entrance/exit of the station) in the case of at-grade access to platform (neither footbridge nor underpass). also such overtaking tracks were not considered that were (or were supposed to be, based on actual timetable [5]) occupied by passenger trains to be overtaken, or turned around. in stations with sidings, an expert estimation of need of station tracks for the freight trains that start or terminate here, was carried out. however, even such "occupied" or "reserved" long overtaking tracks were recorded (separately), if they were long enough. but they are neither displayed if figure 1 nor further discussed in this paper. in the case of a station with more yards (even a passenger and a freight yard), or with station tracks divided in the middle by switch region, an individual approach was chosen. if two subsequent tracks can be used by a long freight train without any impact on regular traffic, overall usable length of the resulting track was recorded. the czech ten-t lines will be further segmented into double-track lines, partially double-track lines and single-track lines. a triple-track line poříčany – praha-libeň and rather short triple-track sections bílina – odb české zlatníky and hranice na moravě – drahotuše will be added to double-track lines. the double-track group comprises vast majority of czech ten-t railway network. these groups can be further divided into subgroups on the basis of their traffic character. the presence of absence of appropriate overtaking tracks will be discussed by particular segments of the lines. 2.2. where to stop for overtaking – a soft decision process it is evident that any stop of a freight train in a bottleneck area leads to lower capacity utilization. so, overtakings should preferably be planned outside the bottlenecks. the following attributes of overtaking stations influence the quality of overtaking: • gradient on following line section (acceleration up the hill lengthens runtime of a freight train significantly and increases consumption of traction energy) • maximum allowed arrival speed on overtaking track (from the infrastructure viewpoint – it usually depends on arrival turnouts) • gradient on previous line section (braking downhill increases wear of brakes) • maximum allowable departure speed from overtaking track (usually depends on departure turnouts) • usable length of the longest overtaking track in particular direction 13 m. drabek, v. janos, z. michl acta polytechnica ctu proceedings in the authors’ opinion, it is very difficult (if not impossible) to set an exact order of priorities of the attributes listed above. each line, each passenger timetable and each set of freight trains together make a unique combination of specific conditions. so, a choice of the most suitable station for overtaking is always a soft decision process [10]. because of importance of gradients for freight railway, significant line peaks are also considered and marked in figure 1. 3. results and discussion czech ten-t lines are further segmented on the basis of number of tracks and their traffic character. presence or absence of long overtaking tracks is commented for each line group. for přerov and bohumín node stations, data on track length and on position of main departure signals were not available. some interesting findings occurred. firstly, during the analysis there emerged few theoretically suitable overtaking tracks which were approximately 770 m long. more precise calculations can determine the exact minimum practically usable track length for the long trains after implementation of etcs. secondly, most of the suitable overtaking tracks are over 800 m long. unfortunately, their density in the network varies considerably. 3.1. double-track (or triple-track) lines busy national mainlines with mixed traffic: • praha – česká třebová – olomouc – přerov – ostrava – bohumín (– chalupki) – dětmarovice/petrovice u karviné (– katowice) – třinec – bystřice busy mainlines with significant (or prevailing) freight traffic: • praha – děčín (– dresden), • lysá nad labem – děčín prostřední žleb, • ústí nad labem – úpořiny – bílina, • přerov – břeclav (– vienna/bratislava), • bystřice – mosty u jablunkova (– žilina). busy suburban sections with mixed traffic: • praha – kralupy nad vltavou, • praha – lysá nad labem – nymburk – kolín, • praha – benešov u prahy, • praha – beroun, • brno – tišnov, • brno – skalice nad svitavou, • brno – břeclav. middle-busy mainlines: • ústí nad labem – teplice – bílina – most – chomutov – karlovy vary – cheb (– marktredwitz), • plzeň – beroun, • kolín – kutná hora (station with both ac and dc traction power supply systems) – havlíčkův brod – tišnov, • česká třebová – skalice nad svitavou, • brno – blažovice, • hranice na moravě – horní lideč (– žilina). due to practically exhausted capacity of the line praha – olomouc – ostrava – bystřice, freight trains should be able to run homogeneous train paths with a long-distance passenger train, so their maximum speed should be 120 km/h, in the worst case 100 km/h. the locomotives should be enough powered to accelerate the train to such speed before it has to be overtaken by next fast train. even if such conditions are fulfilled, there are hardly any available train paths in morning and afternoon peaks between praha and česká třebová. because of busy traffic, the actual number of long overtaking tracks is not sufficient at all. moreover, some ones are located in kolín and pardubice, the busiest nodes within the section mentioned above. for a freight train it is extremely complicate to find a train path that enables conflict-free departure from such busy nodes with level crossing of trains in various directions (e.g. fast train praha – havlíčkův brod – brno with non-stop express train ostrava – pardubice – praha). the section kolín – lysá nad labem is busy by suburban traffic, but enables homogeneous train paths even to slower freight trains (e.g. 90 km/h). however, any stop of a freight train in this section is highly undesirable, because the trains run in 5-8 min wide time slots after each other. behind lysá nad labem, passenger traffic is considerably lower, but freight trains mostly do not need to stop because of train path homogeneity. in any case, the long trains should be scheduled early enough before a fast train, so that they could not delay them. most freight trains need rear-end or head-end assistance in line sections with high gradients, e.g. praha – strančice, český těšín – čadca, kutná hora – žďár nad sázavou, brno – žďár nad sázavou, hranice na moravě – horní lideč etc. for the long trains, 800 m long or longer overtaking tracks are desirable, because of length of the additional locomotive. it is appropriate to combine coupling and uncoupling of this locomotive with the overtaking process. due to speed profile of the line kralupy – děčín – dresden, even 100 km/h fast freight trains can run in homogeneous train paths with non-stop eurocity trains. there is lack of long overtaking tracks in the direction from praha. practically, a non-stop train path from praha-holešovice to děčín is required. on another lines of this sub-category, there is mostly almost no reason for the overtaking of freight trains, if the gradients are low. in busy suburban sections with mixed traffic, best capacity utilization means no stop of a freight train, which requires speed bundling (homogeneous train paths) either with suburban or with fast trains. 14 vol. 5/2016 on operation of 740 metre long freight trains figure 1. presence of available long overtaking tracks in czech ten-t railway network. map source: [11] 3.2. partially double-track lines (middle-busy mainlines) • plzeň – české budějovice (with double-track sections nepomuk – horažďovice předměstí and číčenice – zliv), • benešov u prahy – tábor – české budějovice (mostly double-track line, with remaining several single-track sections). it is desirable to avoid crossing of the freight trains with trains of the opposite direction in single-track sections, because of necessity of stop. the line benešov – české budějovice has not much passenger traffic, but three significant peaks. thus, double or triple traction for running through the whole line is worth consideration. 3.3. single-track lines busy national mainlines with mixed traffic: • domažlice – plzeň jižní předměstí, • brno – holubice – nezamyslice – přerov. mainlines with significant freight traffic: • české budějovice – horní dvořiště (– linz). middle-busy mainlines: • cheb – plzeň (there are double-track sections cheb – lipová u chebu and pňovany – plzeň only in ends of the line, so there is a character of a single-track line), • (furth im wald) – domažlice, • ústí nad orlicí – lichkov (– wroclaw). mainlines with little traffic: • české budějovice – české velenice (– gmünd nö). on single-track lines, longer overtaking tracks in almost every station are necessary, because of crossing of a freight train with any train which runs in the opposite direction. the alternative, which may be more efficient, is targeted partial doubling of the line. in the czech republic, most of passenger trains operate in (more or less) periodic timetable. if there are two systems of periodic passenger services with different section runtimes (and hence, with different crossing stations), there usually remains very little usable capacity left for freight trains. so, if there is a demand after a freight train paths approximately every 2 hours or more often, targeted partial doubling of the line is desirable. "targeted" means in the sections where trains from opposite direction cross each other. for the passenger trains in the czech republic, it usually corresponds to "zero symmetry" time, i.e. the minute 00. freight train paths should be, in the authors’ opinion, if possible, designed as periodic with identic symmetry time, and meeting of the freight 15 m. drabek, v. janos, z. michl acta polytechnica ctu proceedings trains of the opposite direction should be designed into the planned double-track section. if the freight traffic is irregular, at least crossing of a freight and a passenger train should be designed there. 3.4. sections and nodes with lack of long overtaking tracks there are listed lines, sections or nodes where additional long overtaking tracks are desirable: • cheb – plzeň, • furth im wald – domažlice – plzeň, • plzeň – české budějovice (a bypass line), • plzeň – beroun – praha (establishment of flank protection for long overtaking tracks can mostly solve the problem), • české budějovice – horní dvořiště (– linz) (a bypass line), • praha – české budějovice (a bypass line. after completed modernization, overtaking by fast trains is likely inevitable), • praha – ústí nad labem – děčín (this direction only), • děčín prostřední žleb – lysá nad labem, • kolín – havlíčkův brod – brno, • brno – přerov (modernization of the whole line is planned), • praha – olomouc (lack of long overtaking tracks outside large nodes), • přerov – ostrava (this direction only), • brno – břeclav (in the middle of the line and břeclav freight yard). 4. conclusion besides sections with high gradients, overtaking of a freight train is sometimes necessary because of fitting into spare time slot in a bottleneck area, or on a neighbouring line with a different timetable pattern. so, even on a line with sufficient capacity and train path homogeneity, a pair of long overtaking tracks is desirable for this reason. another reason is preparedness for traffic disruptions. in the case of higher gradients, such track should lay behind the peak of the line and before beginning of higher gradient uphill section, but neither in busy node nor in suburban or another bottleneck area. the discussion above has shown that for fulfilling eu requirements for enabling operation of 740 m long freight trains, it is not necessary to lengthen overtaking tracks in every station on double-track lines. but such tracks are desirable outside bottleneck areas and, if need be, behind a peak of the line. for the freight railway undertakings, the probably best capacity offer would be system of periodic catalogue freight train paths without unnecessary stops, as proposed by drábek [10], but with overtaking tracks long enough. this is the strategy that is recommended to sždc for long-term infrastructure improvement, as a conclusion of this paper. acknowledgements the authors would hereby like to propose a vote of thanks to sždc for enabling them to use railway station schemes [5] and especially to propose a vote of thanks to its employee dr. pavel krýže, who is the author of clearly arranged official maps of czech railway network [11]. the authors were glad to use the mentioned sources for the research presented in this paper. references [1] european commission. directive 2008/57/ec of the european parliament and of the council of 17 june, 2008 on the interoperability of the rail system within the community [online], 2011. http://eur-lex.europa.eu/legal-content/en/txt/ pdf/?uri=celex:02008l0057-20110322&from=en. [2] european commission. regulation (eu) no. 1315/2013 of the european parliament and of the council of 11 december 2013 on union guidelines for the development of the trans-european transport network and repealing decision no. 661/2010/eu [online], 2013. http://eur-lex.europa.eu/legal-content/en/all/ ?uri=uriserv:oj.l_.2013.348.01.0001.01.eng. [3] european commission. regulation (eu) no.913/2010 of the european parliament and of the council of 22 september 2010 concerning a european rail network for competitive freight [online]. european union, brussels, 2010. http://eur-lex.europa.eu/legal-content/en/ all/?uri=celex:32010r0913. [4] j. kušnír, j. ilík. railway in 2030, keynote speech, in: future of railway passenger transport in the czech republic, czech raildays [online], 2013. ostrava: czech ministry of transport, in czech, http://www.railvolution.net/czechraildays/2013/ seminare/konference-kusnir.pdf. [5] sždc: collection of official requisites for 2015/16 timetable, unpublished, praha: sždc, 2015. [6] r. brejcha, r. čech. operation of freight trains long up to 740 m. in: scientific-technical proceedings of czech railways. vol. 40/2015 [online], 2015. praha: czech railways, in czech, http://vtsb.cd.cz/vts/clanky/vts40/4008.pdf. [7] m. binko. railway infrastructure for freight transport, in czech raildays: adaptation of railway to both actual and future transport needs of passengers and goods [online], 2015. praha: m-presse plus s.r.o., in czech., http://www.railvolution.net/ czechraildays/2015/buletin2015.pdf. [8] m. binko. railway infrastructure for freight transport, keynote speech, in czech raildays conference [online], 2015. ostrava: sždc s.o., [2015-06-16], in czech, http://binko.webzdarma.cz/2015-6b.pdf. [9] czech technical standard tnž 34 2620 railway station and line signalling and interlocking systems, amended, effective since july 1. 2002, unpublished, olomouc: české dráhy, 2002. [10] m. drábek. periodic freight train paths in network, doctoral thesis. 2014. praha: ctu in prague, http://takt.fd.cvut.cz/cargo/drabek_thesis.pdf. [11] p. krýže. maps of railway network [online], 2015. praha: sždc, http://provoz.szdc.cz/portal/ viewarticle.aspx?oid=594598. 16 http://eur-lex.europa.eu/legal-content/en/txt/pdf/?uri=celex:02008l0057-20110322&from=en http://eur-lex.europa.eu/legal-content/en/txt/pdf/?uri=celex:02008l0057-20110322&from=en http://eur-lex.europa.eu/legal-content/en/all/?uri=uriserv:oj.l_.2013.348.01.0001.01.eng http://eur-lex.europa.eu/legal-content/en/all/?uri=uriserv:oj.l_.2013.348.01.0001.01.eng http://eur-lex.europa.eu/legal-content/en/all/?uri=celex:32010r0913 http://eur-lex.europa.eu/legal-content/en/all/?uri=celex:32010r0913 http://www.railvolution.net/czechraildays/2013/seminare/konference-kusnir.pdf http://www.railvolution.net/czechraildays/2013/seminare/konference-kusnir.pdf http://vtsb.cd.cz/vts/clanky/vts40/4008.pdf http://www.railvolution.net/czechraildays/2015/buletin2015.pdf http://www.railvolution.net/czechraildays/2015/buletin2015.pdf http://binko.webzdarma.cz/2015-6b.pdf http://takt.fd.cvut.cz/cargo/drabek_thesis.pdf http://provoz.szdc.cz/portal/viewarticle.aspx?oid=594598 http://provoz.szdc.cz/portal/viewarticle.aspx?oid=594598 acta polytechnica ctu proceedings 5:12–16, 2016 1 introduction 2 methods 2.1 rules for determination of available overtaking tracks for 740 m long trains 2.2 where to stop for overtaking – a soft decision process 3 results and discussion 3.1 double-track (or triple-track) lines 3.2 partially double-track lines (middle-busy mainlines) 3.3 single-track lines 3.4 sections and nodes with lack of long overtaking tracks 4 conclusion acknowledgements references 242 acta polytechnica ctu proceedings 2(1): 242–245, 2015 242 doi: 10.14311/app.2015.02.0242 line evolution of the nova v5587 sgr from early to nebula phase t. kajikawa1, a. arai1,2, m. nagashima1, h. kawakita1, m. yamanaka3,4,5, k. kawabata3, s. kiyota6 1kyoto sangyo university, koyama astronomical observatory 2university of hyogo, nishi-harima astronomical observatory 3hiroshima university 4kyoto university 5konan university 6vsolj corresponding author: kajikawat8@gmail.com abstract the spectral evolution of the nova v5587 sgr has been monitored at koyama astronomical observatory and higashihiroshima observatory, japan, from the early to nebula phase. the nova rebrightened several times. the spectra during the early phase showed emission lines of hα, hβ, o i, he i, he ii, n ii, fe ii. nova v5587 sgr is classified into the fe ii type. the helium abundance of the nova is estimated as n(he)/n(h) = 0.134 ± 0.09. the light curve, the spectral evolution, and the helium abundance in v5587 sgr are similar to those of the nova pw vul. keywords: cataclysmic variables classical novae optical spectroscopy photometry individual: v5587 sgr. 1 introduction photometric observations of novae are usually performed by many observers worldwide. the light curves of the novae have been revealed in detail, and they can be classified into several classes (strope et al. 2010). in contrast, spectroscopic observations of novae are not performed as frequently as photometric observations because (i) the number of available spectrographs (and observers) are limited; (ii) some fraction of novae are too faint to observe by spectrographs in their later phase (or even at the maximum for some novae). as novae show a variety of spectral evolutions, spectroscopic monitoring can provide new insights into the physics and chemistry of novae. for example, recently nagashima et al. (2013) detected molecular absorption bands of c2 and cn in nova v2676 oph. (this is the first detection of c2 in novae and the second for cn.) this detection was performed as a part of long-term spectroscopic observations of this nova. the light curves of novae in some classes (strope et al. 2010) can be successfully reproduced by models (as reviewed by prof. kato at this meeting). however, the light curves in the “jitter”and “oscillation”classes (strope et al. 2010) could not be reproduced well by the models. in this paper, we focus on the “jitter”class and introduce our recent spectroscopic observations of v5587 sgr classified in this class. we discuss the nature of this nova as it is likely that there are differrent types of oscillations (i.e., different physical conditions) of novae in the “jitter”class. different types of novae might 6 8 10 12 14 16 18 0 100 200 300 400 500 v ( m ag ni tu de s) days after discovery (t) v5587 sgr pw vul figure 1: v band magnitudes of v5587 sgr and pw vul. the light curve of v5587 sgr is from higashihiroshima observatory, vsnet, and aavso observations. the light curve of pw vul was refer to the online data of strope et al.(2010). 242 http://dx.doi.org/10.14311/app.2015.02.0242 line evolution of the nova v5587 sgr from early to nebula phase be mixed together in this class. even though there are high-quality photometric and spectroscopic observations for some jitter class novae, the mechanism for their rebrightening is still unclear (tanaka et al. 2011). by frequent spectroscopic observations, we can observe phenomena useful to reveal the physics of the nova. in order to investigate the mechanism for the rebrightening in the “jitter”class novae, we have conducted spectroscopic observations of v5587 sgr in 2011 – 2012. the nova v5587 sgr (= nova sgr 2011 no.1) was discovered on ut 2011 january 25.86 by nishimura (nakano et al. 2011). the first low-dispersion spectrum was obtained on ut 2011 january 28 at koyama astronomical observatory. the spectrum shows prominent emission lines of hα, hβ and o i. these features suggest that this object is a classical nova (arai 2011; imamura 2011). 2 observations our photometric and spectroscopic observations were performed at two sites. one site is koyama astronomical observatory (kyoto sangyo university, kyoto, japan). we used the 1.3m araki telescope with the losa/f2 spectrograph (arai et al., in prep.) for low-dispersion spectroscopy. the wavelength coverage is 400 – 800 nm and the spectral resolving power is r = λ/∆λ ∼ 580 at 600 nm. the other site is higashi-hiroshima observatory (hiroshima university, hiroshima, japan). we used the 1.5m kanata telescope with trispec (triple range imager and spectrograph with polarimeter, shutdown in 2012) for photometry and with howpol (hiroshima one-shot wide-field polarimeter) for spectroscopy. its wavelength coverrage is 400 – 1000 nm, and spectral resolving power is r ∼ 400 at 600 nm. 450 500 550 600 650 700 750 800 850 n or m al iz ed fl ux + c on st . wavelength (nm) +596d +229d +213d +185d +167d +154d +147d +129d +100d +93d +81d +69d +68d +61d +60d +45d +43d +39d +35d +27d +11d +9d +8d h e ii (4 68 .6 ) h β f e ii( 42 ) (4 92 .4 ) f e ii( 42 ) (5 01 .8 ) f e ii( 42 ) (5 16 .9 ) [o ii i] (4 95 .9 ) [o ii i] (5 00 .6 ) n ii ( 56 8. 0) [n ii ] ( 57 5. 5) h e i ( 58 7. 4) [o i] ( 63 0. 0) [o i] ( 63 6. 3) h α h e i ( 66 8. 1) h e i ( 70 6. 5) [o ii ] ( 73 3. 0) o i (7 77 .4 ) figure 2: the normalized spectra of v5587 sgr observed from +8d (= ut 2011 february 2) to +596d (= ut 2012 september 12) after the discovery. these spectra were obtained at koyama astronomical observatory except for the data on +35d and +45d (= ut 2001 march 3 and 12), taken at higashi-hiroshima observatory. 243 t. kajikawa et al. 3 results figure 1 shows light curves of v5587 sgr. since v5587 sgr showed an erratic variation in the light curve, we consider that the nova is classified in the “jitter”class. particularly, v5587 sgr seems to be a member of the sub-class prototyped by pw vul as shown in strope et al. (2010). based on the light curves, we determined the date of the visual maximum as 9 days after discovery and also determined t2 = 12 days and t3 = 108 days. from (b v) at maximum magnitude and at t2, we estimate the color excess by intersterllar extinction; e(b v) = 0.85 – 1.26. the light curve of v5587 sgr is quite similar to that of the “jitter”class nova pw vul as shown figure 1 (schwarz et al. 1997, and references therein). pw vul was discovered on 1984 july 27 (= jd 2445917) by wakuda (kosai 1984). this nova reached its maximum light of 6.3 magnitude in the v band on 1984 aug 4th. we compare v5587 sgr with pw vul from various viewpoints in the next section. 500 550 n or m al iz ed fl ux wavelength (nm) +45d +43d +39d +35d +27d +11d +9d +8d hβ fe ii (42) figure 3: the spectra of v5587 sgr in early phase. the nova never showed any regrowth of a p-cygni profile. figure 2 shows the growth of hα, hβ, he i, he ii, n ii, [n ii], o i, [o i], [o ii], and fe ii emission lines of v5587 sgr. novae that exhibit rebrightening in the early phase often show the regrowth of a p-cygni profile (tanaka et al. 2011, csak et al. 2005) as in v4745 sgr. however, v5587 sgr has never shown this behavior (figure 3). it is considered that the nova entered into the nebula phase between july 11 to july 29 because the [o iii] forbidden emission lines dominated hβ at that time (figure 4). we assume that the electron density in the nebula phase was ne = 106 ∼ 108 cm−3 according to iijima & esenoglu (2003) and iijima (2006), and we estimate the helium abundance of the ejecta based on the data between july 11 and july 29 ; n(he)/n(h) = 0.134 ± 0.09 (for ne = 106 cm−3), n(he)/n(h) = 0.139 ± 0.09 (for ne = 108 cm−3). 450 500 550 600 650 700 750 800 n or m al iz ed fl ux wavelength (nm) +147d +129d h e ii (4 68 .6 ) h β [o ii i] + f e ii( 42 ) n ii ( 56 8. 0) h e i ( 58 7. 4) [o i] ( 63 0. 0) [o i] ( 63 6. 3) h e i ( 66 8. 1) h e i ( 70 6. 5) [o ii ] ( 73 3. 0) o i (7 77 .4 ) figure 4: the spectra of v5587 sgr in nebular phase(+129 days and +147 days after its maximum). an emission line of he ii was recognized in these spectra. 4 discussion & conclusion the decline rates, amplitudes, and intervals of rebrightening observed in v5587 sgr are similar to those of pw vul. this fact suggests that the wd mass and physical parameters related to the explosion of v5587 sgr would be similar to those of pw vul. comparison between the spectra of v5587 sgr and pw vul also lead us to the same conclusion, namely, they are similar to each other, e.g., the late-phase spectra of v5587 sgr (shown in figure 4 in rosino and iijima 1987). figure 5 also shows helium abundances vs t3 in 20 various novae. helium abundance of v5587 sgr seems to be similar to that of pw vul. this figure indicates that helium abundance is not correlated with t3. in summary, we have performed photometric and low-dispersion spectroscopic observations of v5587 sgr from early to nebula phase. the photometry showed erratic variations of the light curve. the spectra during the early phase showed emission lines of hα, hβ, and fe ii (i.e., fe ii type) and v5587 sgr never showed regrowth of a p-cygni profile. the nova entered the nebula phase between july 11 to july 29 (t = 158 to 178days). we estimated that the helium abundance of v5587 sgr is n(he)/n(h) = 0.134 ± 0.09. the nova is very similar to pw vul considering decline rates, spectral features, and helium abundance. we obtained a new sample of the “jitter”class novae. 244 line evolution of the nova v5587 sgr from early to nebula phase -1 -0.5 0 0.5 0.5 1 1.5 2 2.5 3 3.5 lo g 1 0( n (h e) /n (h )) log10t3 v1494 aql(1) v723 cas(2) v2468 cyg(3) cl aql(4) v407 cyg(5) v1500 cyg(6) qu vul(7) v351 pup(8) u sco(9) pw vul(10),(11) v842 cen(11) v827 her(11) qv vul(11) v2214 oph(11) v977 sco(11) v443 sct(11) v1668 cyg(11) v693 cra(11) v1370 aql(11) v5587 sgr figure 5: the helium abundance of 20 novae. references: (1) iijima & esenoglu (2003); (2) iijima (2006); (3) iijima & naito (2011); (4) iijima (2012a); (5) iijima (2012b); (6) ferland (1978); (7) schwarz (2002); (8) saizar (1996); (9) iijima (2002); (10) schwarz et al. (1997); (11) andreä et al. (1994). references [1] andreä, j., drechsel, h., starrfield, s.: 1994, a&a 291, 869. [2] arai, a.: 2011, iauc 9196, 2. [3] chochol, d., et al.: 2012, mmsai 83, 767. [4] ferland, g.j.: 1978, apj 219, 589. doi:10.1086/155818 [5] iijima, t.: 2002, a&a 387,1013. [6] iijima, t., esenoglu, h.h.: 2003, a&a 404, 997. [7] iijima, t.: 2006, a&a 451, 563. [8] iijima, t., naito, h.: 2011, a&a 526a, 73. [9] iijima, t.: 2012a, mmsai 83, 835. [10] iijima, t.: 2012b, a&a 544a, 26. [11] imamura, k.: 2011, iauc 9196, 2. [12] nagashima, m., et al.: 2014, journal?, in press. [13] nakano, s., nishimura, h., kiyota, s., yusa, t.: 2011, iauc 9196, 1. [14] rosino, l., iijima, t.: 1987, ap&ss 130, 157. doi:10.1007/bf00654989 [15] saizar, p., et al.: 1991, apj 367,310. doi:10.1086/169630 [16] saizar, p., et al.: 1996, mnras 279, 280. doi:10.1093/mnras/279.1.280 [17] schwarz, g.j., et al.: 1997, mnras 290, 75. doi:10.1093/mnras/290.1.75 [18] schwarz, g.j.: 2002, apj 577, 940. doi:10.1086/342234 [19] strope, r.j., schaefer, b.e., henden, a.a.: 2010, aj 140, 34. [20] tanaka, j., et al.: 2011, pasj 63, 159. [21] tanaka, j., et al.: 2011, pasj 63, 911. 245 http://dx.doi.org/10.1086/155818 http://dx.doi.org/10.1007/bf00654989 http://dx.doi.org/10.1086/169630 http://dx.doi.org/10.1093/mnras/279.1.280 http://dx.doi.org/10.1093/mnras/290.1.75 http://dx.doi.org/10.1086/342234 introduction observations results discussion & conclusion acta polytechnica ctu proceedings doi:10.14311/app.2017.13.0029 acta polytechnica ctu proceedings 13:29–34, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app synthesized enrichment functions for extended finite element analyses with fully resolved microstructure martin doškářa,∗, jan nováka, jan zemana,b a faculty of civil engineering, czech technical university in prague, thákurova 7/2077, 166 29 prague 6, czech republic b the institute of information theory and automation, academy of sciences of the czech republic, pod vodárenskou věží 4, 182 08 prague 8, czech republic ∗ corresponding author: martin.doskar@fsv.cvut.cz abstract. inspired by the first order numerical homogenization, we present a method for extracting continuous fluctuation fields from the wang tile based compression of a material microstructure. the fluctuation fields are then used as enrichment basis in extended finite element method (xfem) to reduce number of unknowns in problems with fully resolved microstructural geometry synthesized by means of the tiling concept. in addition, the xfem basis functions are taken as reduced modes of a detailed discretization in order to circumvent the need for non-standard numerical quadratures. the methodology is illustrated with a scalar steady-state problem. keywords: wang tiling, microstructure synthesis, microstructure-informed enrichment functions, extended finite element method. 1. introduction all materials exhibit heterogeneous microstructure at certain level of detail. besides the physical properties of microstructural constituents, the overall response is also dictated by their spatial arrangement. with the advance of numerical methods and computational power, there is an emphasis on devising approaches that take the microstructural characteristics into account and propagate knowledge of material composition into upper-scale models. in our contribution, we focus on problems in which the underlying microstructural geometry is explicitly known. we consider problems where the characteristic length of the microstructure is comparable to the dimension of an upper-scale model; hence, the nested numerical homogenization, such as the fe2 method [1], is not applicable because the underlying assumption of the separation of scales is violated [2, and references therein]. this work supplements our previous results regarding efficient modelling of materials with stochastic heterogeneous microstructure, e.g., [3, 4]. the microstructural geometry of a macro-scale model—as well as its finite element discretization—is synthesized using the wang tiling concept, recalled in section 2. here, we present a method to extract dominant responses of a compressed microstructure to prescribed macroscopic loading. we reuse the extracted responses to synthesize a microstructure-informed enrichment basis in order to accelerate the upper scale calculations. the numerical scheme, outlined in section 4, combines extended finite element framework (xfem) [5, 6, and references therein], used for definition of local basis functions, with the reduced order modelling approach [7], allowing for utilization of standard finite element procedures. finally, section 5 illustrates the methodology with a two-dimensional problem of steady-state thermal conduction in an l-shaped domain. 2. wang tiling concept microstructure of random heterogeneous materials is usually represented by means of a periodic finitesize model—appearing in the literature under various names such as statistically optimal representative unit cell, statistically similar representative volume element, or statistically equivalent periodic unit cell (sepuc)—that resembles the material in terms of various spatial statistics. this setting is particularly suitable for the family of fe2 simulations,e.g., [1], in which it is often accompanied with periodic boundary conditions imposed at the micro-scale level. however, when used for microstructure synthesis, this representation introduces unrealistic, spurious periodic correlations. the formalism of wang tiles represents a compromise between the amount of induced correlation and complexity of a microstructure representation. instead of a single cell, microstructural information is compressed into a set of equi-sized wang tiles with pre-defined requirements on mutual compatibility. in the abstract setting, the compatibility constraints are represented by codes assigned to tile edges, illustrated with distinct colours in figure 1. a realization of the compressed microstructure is then synthesized following a simple stochastic algorithm: an empty grid of 29 http://dx.doi.org/10.14311/app.2017.13.0029 http://ojs.cvut.cz/ojs/index.php/app m. doškář, j. novák, j. zeman acta polytechnica ctu proceedings a desired size is sequentially filled with instances of wang tiles such that the adjacent tile edges are compatible. at each position, a tile is randomly chosen from a subset of tiles compliant with previously placed tiles; hence, the algorithm generates stochastic realizations, providing that set of tiles is rich enough such that multiple tiles are admissible at each assembly step; see figure 1 for an illustration. figure 1. the compressed microstructural geometry represented with the set of wang tiles (top) and an illustration of a step in the tiling algorithm with partially assembled microstructure (bottom). procedures designed to compress a given microstructure into a sepuc can be straightforwardly extended to take into account generalized periodicity occurring in the tiling concept, e.g., the standard optimization procedure based on minimizing discrepancy in the two-point probability function was used in [3]. we also adapted a sample-based approach originated in computer graphics in order to address the high computational cost of the optimization-based design [4]. currently, a variety of material microstructures, ranging from particulate media to complex foam-like microstructures, can be represented with the framework of wang tiling. individual realizations of the microstructure are then generated in linear time with respect to the required sample size, which makes the tiling concept appealing for applications where multiple microstructure samples are required, e.g., investigation of the rve size [8]. 3. synthesized enrichments fields the idea of compressing fluctuation fields using the wang tiling concept has been introduced in novák et al. [9], where the microstructural geometry of individual tiles was optimized with respect to (i) meeting prescribed spatial statistics and (ii) minimizing traction discrepancies among congruent edges in an auxiliary tiling. however, the resulting synthesized stress fields exhibited unavoidable discontinuities and the objective function required careful tuning of weight parameters because the two requirements turned to be hard to achieve simultaneously. in contrast, the present method generates continuous fields of the primal unknowns for any existing microstructure compression. we illustrate the methodology with the steady-state heat conduction problem, governed by ∇ · (−k(x) · ∇θ(x)) = 0 , x ∈ ω , (1) where θ denotes the unknown temperature field, k is a local heat conductivity tensor and no heat sources are considered. first, we assume the decomposition of θ into a fluctuation part θ̃, caused by the presence of heterogeneities, and a macroscopic part controlled with a macroscopic temperature gradient h, θ(x) = θ̃(x) + h · x , ∀x ∈ t(i),∀t(i) ∈ s, (2) where t(i) denotes the domain of the i-th tile and s ={ t(i), i = 1 . . . nt } represent the set of nt available tiles. without loss of generality, each tile is assumed centred, i.e., t(i) = [−α, α]2, where 2α is the size of the tile edge. in order to enforce continuity of the extracted fields, all tiles are loaded with the prescribed macroscopic gradient h and solved simultaneously. providing that the tile geometries are discretized with a compatible triangulation—meaning that discretization of the corresponding tile edges is the same across all tiles—the continuity is ensured by associating the corresponding edge unknowns during the localization of an element contribution into the conductivity matrix of the whole set. the resulting system takes the standard form ks θ̃ = f (h) , (3) where ks = at(i)∈s kt(i) is the conductivity matrix and f (h) is a h-dependent loading vector arising from the weak form after plugging eq. (2) into eq. (1). ks has block-diagonal structure similar to primal domain decomposition approaches. in addition, two types of constraints are imposed on the set system. first, we eliminate zero-energy modes of ks by requirement 1 |s| ∫ s θ̃(x) dx = 0 . (4) the second constraint prevents the fluctuation field θ̃ from compensating for the loading induced through h . 30 vol. 13/2017 synthesized microstructure-informed enrichments for xfem analyses inspired in numerical homogenization, e.g. [2], we introduce the second constraint enforcing 1 |ω| ∫ ω ∇θ̃(x) dx = 0 (5) in a chosen domain ω loaded analogously to eq. (2). using green’s first identity, eq. (5) can be recast into a boundary integral∫ ∂ω θ̃(x)n(x) ds = 0 , (6) where n(x) denotes the outer normal of the boundary. in particular, we consider three mutually exclusive types of the second constraint: (k) the first type prescribes zero temperature fluctuations at tile boundaries, θ̃|∂t(i) = 0 , ∀i = 1 . . . nt , (7) where ∂t(i) stands for the boundary of the i-th tile. (p) in the second type, the requirement (6) is posed tile-wise, i.e.,∫ ∂t(i) θ̃(x)n(x) ds = 0 , ∀i = 1 . . . nt . (8) (s) the last type imposes eq. (6) over the whole set,∫ ∂s θ̃(x)n(x) ds = 0 , (9) where ∂s = { ∂t(i), i = 1 . . . nt } . note that (k) corresponds directly to kinematic uniform boundary conditions used in numerical homogenization, while (p) and (s) mimic periodic and statically uniform boundary conditions, respectively. instead of eq. (3), the final fluctuations θ̃ follows from ks ct i ct ii ci 0 0 cii 0 0  θ̃ λi λii  = f(h) 0 0  , (10) where ci and cii matrices represent the discretized versions of eq. (4) and one of eqs. (7), (8), or (9), respectively, and λ• stands for the corresponding vector of lagrange multipliers. while cii straightforwardly eliminates edge unknowns for the constraint type (k), constructing contributions of individual tile separately and localizing them into cii leads to an ill-posed problem for types (p) and (s) from eq. (6), it clearly follows that if two opposite sides of a tile are required to be compatible— hence they feature the same trace of θ̃—the corresponding component of ∇θ̃ average vanishes and so does the tile contribution to the relevant row in cii. in addition, the ill-posedness also stems from the repetition of edge code pairs within the tile set (swapping the order of codes changes only the sign of the edge contribution to eq. (5)). in certain cases, this can even result in zero matrix cii for the least restrictive constraint (s), in which tile contributions are summed together. one way to treat the singularity of cii is to perform singular value decomposition on the constraint and take into account only the non-zero singular values; however, such a procedure is sensitive to numerical precision. thanks to the simple structure of the constraint, the regular part of the constraint can be directly established as a projection of the original matrix cii. first, all nc combinations of edge codes pertinent to either horizontal or vertical edges are identified and enumerated. next, an empty matrix p ∈ r2nt ×nc , for (p) type of the constraint, or p ∈ r2×nc , for (s) type, is created and populated with 1 (or −1) if the tile contains an enumerated pair of codes (or a pair in the inverse order). odd and even rows of the matrix correspond to vertical and horizontal edges, respectively. if p remains empty for (s), cii constraint is discarded entirely. otherwise, the non-singular constraint matrix cii, replacing cii in eq. (10), is obtained from a projection cii = ptcii. the outlined strategy allows to define one enrichment field θ̃ for a prescribed h and the selected type of the second constraint. for the linear problem considered in this work, two mutually orthonormal loading cases h = { 1, 0 }t and h = { 0, 1 }t cover all possible load cases. combined with three types of cii, we can generate up to six enrichment fields. note that unlike the nested numerical homogenization, where the choice of boundary conditions is based on their suitability in capturing effects of a surrounding medium, we combine different types of cii to control cardinality of the set of compressed fluctuations. figure 2. a compressed fluctuation field obtained by prescribing (s) variant of the second constraint and setting h = {1, 0}t. 4. numerical strategy the fields introduced above are employed as enrichments in a upper-scale model whose microstructural geometry is assembled by means of tiling from the set depicted in figure 1. assume a upper-scale problem governed by the same differential equation as in eq. (1), valid in a upperscale domain ω and accompanied by boundary conditions θ(x) = θ̂(x) x ∈ γθ 6= ∅ , (11) (−k(x)∇θ(x)) · n(x) = q̂(x) x ∈ γq , (12) 31 m. doškář, j. novák, j. zeman acta polytechnica ctu proceedings where θ̂ and q̂ are the given temperature and normal heat flux profiles, respectively, prescribed at parts γθ and γq of the domain boundary ∂ω. an approximate numerical solution arises from the weak form of the problem find θ ∈ v such that a(θ, ϑ) = b(ϑ), ∀ϑ ∈ v0 . (13) and substitutes for the analytical solution that is usually intractable. in eq. (13), a(θ, ϑ) and b(ϑ) denote the bilinear and linear form pertinent to eq. (1); v and v0 stand for the space of admissible temperature fields. quality of the approximate solution is governed by suitability of a finite-dimensional subspace vc ⊂ v in which the solution is sought for. in particular, domain discretization must accurately resolve all geometrical details in the standard finite element (fe) setting. this requirement leads to very fine meshes in applications where microstructural geometry of the domain is involved. besides local mesh refinements, the approximation space can be enhanced by incorporating prior knowledge of local character of the solution. concretely, in the extended finite element framework [5, 6], the approximate solution θc ∈ vc takes the form θc(x) = nc∑ i=1 ni(x) θi + nc∑ i=1 ne∑ j=1 ni(x)ψj(x) θji , (14) where the first sum contains the standard finite element shape functions ni(x) and the second term adds ne enrichment functions ψj for each discretization node; θi denotes the regular degree of freedom (dof) associated with finite-element mesh node xi, θji are the additional dofs. in traditional xfem, only patches of the domain are usually enriched with ψj , suited for one geometrical feature. typically, the enrichment provides asymptotic solution near a crack tip or introduces strong/weak discontinuities [6]. here, we add global enrichments that capture collective response of a material microstructure. the original shape functions ni(x) model the macroscopic response of the domain, while products ni(x)ψj(x) cover the fluctuations caused by material heterogeneity. a similar idea was introduced by strouboulis et al. [10], who used numerical “handbook” functions for assemblies of closely packed inclusions, or plews and duarte [11]. however, both approaches solve local boundary value problems defined on subdomains first and subsequently run the analysis of the whole domain. in contrast, we precompute the fluctuations purely “off-line” at the level of microstructure compression. i.e., without any information of the domain geometry or loading, and construct the enrichments as an assembly of the tiledefined fluctuation fields. in our approach, the upper scale discretization is constructed irrespectively of the underlying microstructural geometry of ω. hence, the approximation basis functions in the form of eq. (14) together with fluctuations in material parameters due to the presence of microstructural geometry preclude efficient use of standard numerical procedures for evaluation of the bi-linear form in eq. (13). in order to circumvent this drawback, we construct another, finer domain discretization space vf , assembled from the tile discretization used in the off-line phase for extracting fluctuation fields. the shape functions ni(x), defined at the coarser discretization, are projected onto the fine mesh; enrichments ψj(x) are already defined within the fine discretization by construction. consequently, eq. (14) can be understood as a definition of reduced modes for the fine discretization. let matrix φ comprises individual reduced modes as its columns, computed as an element-wise product of the projectedni(x) and ψj(x) following eq. (14). the range of φ thus defines a subspace of vf corresponding to vc. instead of solving the large, fine-discretization system kfθf = ff , we restrict the fine-discretization unknowns θf via θf = φ a , (15) where a denotes the vector of unknown coefficients pertinent to the reduced modes. the final algebraic system then takes the form φtkfφa = φtff . (16) 5. results we considered the material microstructure of monodisperse elliptical inclusions, shown in figure 1. both phases were assumed isotropic, with the inclusion material being more conductive (k(x) = 100 i) than the matrix phase (k(x) = 1 i). six fluctuation fields in total, discretized with linear triangular elements, were extracted, see figure 2. the microstructure was superimposed to an upperscale problem represented by an l-shaped domain with uniform temperature profiles prescribed at the bottom and right-hand side edges. the initial coarse discretization of the domain is depicted in figure 3. the linear lagrange basis functions were assumed at the coarse level, whilst the fine space comprised the quadratic lagrange approximation arising from the product of linear coarse shape functions and the enrichments. the solution θxfem of eq. (16) was compared against direct numerical simulation (dns) θdns, which was taken as the reference solution. a sequence of five uniformly refined coarse discretizations, the first one shown in figure 3, was investigated. the proximity of the reference (dns) and xfem solutions 32 vol. 13/2017 synthesized microstructure-informed enrichments for xfem analyses θ̂ = 20 10 tx 10 ty θ̂ = 0 10 tx 10 ty figure 3. a scheme of the problem definition. the edge lengths tx and ty of the tiles were set as tx = ty = 6. all quantities are in consistent units. was quantified via relative errors εl2 = ∥∥θdns − θxfem ∥∥ l2 ‖θdns‖l2 and (17) εh1 = ∥∥θdns − θxfem ∥∥ h1 ‖θdns‖h1 , (18) where ‖u‖2l2 = ∫ ω u2(x) dx and (19) ‖u‖2h1 = ∫ ω u2(x) +∇u(x) · ∇u(x) dx . (20) mean and standard deviations of the errors computed for five coarse discretizations and six different tiling realizations are given in figure 4. 10!4 10!3 10!2 xfem/dns dofs 10!2 10!1 0 0 l2 h1 figure 4. convergence of l2 and h1 errors with increasing number of dofs in the coarse discretization. 6. conclusions we have presented a method for extracting continuous fluctuation fields from a microstructure compressed by means of wang tiles. we have also demonstrated utilization of these fields as enrichments in xfem. in order to avoid non-standard quadratures, xfem basis functions were projected onto a discretization arising from assembly of the tile discretization used for computing the fluctuation fields. the proposed methodology was applied to a steadystate heat conduction problem defined in an l-shaped domain with microstructural geometry provided by the tiling concept. only 1.6 % of the original degrees of freedom were sufficient to obtain 2 % relative error compared to dns. on the other hand, the reduction in dofs accelerates only the solution of eq. (16). for more significant time savings, a low-rank additional approximation of kf , e.g. using the idea of hyper-reduction [12], has to be introduced and is the focus of our current work. we have also restricted ourself to the first-order decomposition, eq. (2); higher order expansion of the macroscopic loading can be considered to further enrich the approximation space. acknowledgements m. doškář and j. novák acknowledge the endowment of the ministry of industry and trade of the czech republic under the project no. fv10202. in addition, m. doškář was supported by the grant agency of the czech technical university in prague, project no. sgs17/042/ohk1/1t/11 “numerical methods for modeling uncertainties in civil engineering”. references [1] f. feyel, j.-l. chaboche. fe2 multiscale approach for modelling the elastoviscoplastic behaviour of long fibre sic/ti composite materials. computer methods in applied mechanics and engineering 183(3-4):309–330, 2000. doi:10.1016/s0045-7825(99)00224-8. [2] m. g. d. geers, v. g. kouznetsova, k. matouš, j. yvonnet. homogenization methods and multiscale modeling: nonlinear problems. in e. stein, r. de borst, t. j. r. hughes (eds.), encyclopedia of computational mechanics second edition, pp. 1–34. john wiley & sons, ltd, chichester, uk, 2017. doi: 10.1002/9781119176817.ecm107. [3] j. novák, a. kučerová, j. zeman. compressing random microstructures via stochastic wang tilings. physical review e 86(4):040104(r), 2012. doi:10.1103/physreve.86.040104. [4] m. doškář, j. novák, j. zeman. aperiodic compression and reconstruction of real-world material systems based on wang tiles. physical review e 90(6):062118, 2014. doi:10.1103/physreve.90.062118. [5] t.-p. fries, t. belytschko. the extended/generalized finite element method: an overview of the method and its applications. international journal for numerical methods in engineering 84(3):253–304, 2010. doi:10.1002/nme.2914. 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[12] d. ryckelynck. hyper-reduction of mechanical models involving internal variables. international journal for numerical methods in engineering 77(1):75–89, 2009. doi:10.1002/nme.2406. 34 http://dx.doi.org/10.1016/j.jcp.2006.09.019 http://dx.doi.org/10.1016/j.compstruc.2016.01.003 http://dx.doi.org/10.1088/0965-0393/21/2/025014 http://dx.doi.org/10.1016/s0045-7825(03)00347-5 http://dx.doi.org/10.1002/nme.4703 http://dx.doi.org/10.1002/nme.2406 acta polytechnica ctu proceedings 13:29–34, 2017 1 introduction 2 wang tiling concept 3 synthesized enrichments fields 4 numerical strategy 5 results 6 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.12.0108 acta polytechnica ctu proceedings 12:108–111, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app interactive motion platforms and virtual reality for vehicle simulators evžen thöndel pragolet, s.r.o., director and czech technical university in prague, assistant professor at the department of electric drives and traction correspondence: thoendel.jr@pragolet.cz abstract. interactive motion platforms are intended for vehicle simulators, where the direct interaction of the human body is used for controlling the simulated vehicle (e.g. bicycle, motorbike or other sports vehicles). the second use of interactive motion platforms is for entertainment purposes or fitness. the development of interactive motion platforms reacts to recent calls in the simulation industry to provide a device, which further enhances the virtual reality experience, especially with connection to the new and very fast growing business in virtual reality glasses. the paper looks at the design and control of an interactive motion platform with two degrees of freedom to be used in virtual reality applications. the paper provides the description of the control methods and new problems related to the virtual reality sickness are discussed here. keywords: motion platform, motion cueing, simulator, simulation, virtual reality, vr sickness. 1. introduction interactive motion platforms are intended for a simulation where direct interaction with a human body is required. this type of simulators is e.g. a motorbike or bicycle simulator or other types of vehicles where direct interaction with the human body is used for controlling the vehicle. a simulator with an interactive motion platform is a closed loop system, where a human being is a part of the system. in contrast to standard humanin-the-loop systems[1], the human does not interact with the system through control elements (such as a steering wheel or pedals) but creates forces and torques which are directly measured and used as input to a mathematical model. the structure of the closed loop system is shown in the next picture. the structure and principle of individual blocks are further discussed. 2. motion platform the purpose of a motion platform in simulators is to reproduce motion effects, such as acceleration, and position towards gravity. different types and principles are discussed in the literature[2]. the important parameter of each motion platform is the number of degrees of freedom (dof) and the range of motion in all directions. the most widely used motion platforms today have 2, 3 or 6 dof. in the case of simulators of land vehicles, the dominant motion is rotation around the horizontal axis. this motion can also be used for reproducing linear accelerations (by using a motion cueing algorithm[3]). the second aspect which must be considered, when designing a new motion platform, is the final price which significantly grows with the number of degrees of freedom. a motion platform with two degrees of freedom is the first design and implementation of an interactive motion platform. an extension with a horizontal rotation of 360 degrees is considered in the future, to avoid or to solve a problem connected with virtual reality sickness. the design of the 2dof interactive motion platform is shown in the picture below. figure 1. design of the motion platform. all kinematic and dynamic parameters are summarized in the following table: maximum payload 150 kg tilt angle 16 degrees degrees of freedom 2 (pitch and roll) maximum tilt rate 100 degrees/s maximum tilt acceleration 500 degrees/s2 power supply requirements 230 v/50 hz, 16 a weight 80 kg table 1. kinematic and dynamic properties. 108 http://dx.doi.org/10.14311/app.2017.12.0108 http://ojs.cvut.cz/ojs/index.php/app vol. 12/2017 interactive motion platforms and virtual reality for vehicle simulators figure 2. structure of the system with an interactive motion platform. 3. mathematical model of the dynamic response a mathematical model of the dynamic response reads information about the acting forces and torques and calculates the response of the motion platform. besides the input from the human, the mathematical model of the dynamic response can also read signals from a superior mathematical model where the dynamic response of the simulated vehicle is implemented. an implementation of the mathematical model of the dynamic response is shown in the next picture. this structure applies a motion cueing algorithm as well as a model of direct dynamic response (called stiffness in the following structure). the principle of a motion cueing algorithm is described in detail in the previous author’s publications[4], and will not be discussed here. a model of the direct dynamic response can be any dynamic system which reacts directly to forces measured on the motion platform. one possible use of the interactive motion platform is rehabilitation or fitness where the model can implement a system of the load. one example is presented in the next picture where a simple model of a rubber ball is shown. all mathematical models have been implemented in matlab/simulink and directly compiled to the control hardware. this method of programming is very effective, and it allows the motion platform to also be used in research projects[5]. 4. load sensors as discussed above, the main innovation of the new motion platform is the possibility to measure forces and torques which are created by a person standing or sitting on the motion platform. four load cells, weighing 100 kg each, are used to measure and further calculate the position (center of gravity) and the intensity of the loading force. figure 3. load sensors attachment. 5. the use in virtual reality there has been fast growth in virtual reality over the last two years, especially connected to the use of virtual glasses. new applications and technologies are continuously being researched. the presented motion platform is ideally suited for vehicle simulators where virtual glasses are used to generate visual perception. several designs of applications have been created, and the first real application of a kayak simulator has been finished in 2016[6]. the first test and the response from many users show a promising potential for business success and further technological enhancement of the use of vr glasses because it significantly reduces the occurrence of virtual reality sickness. 6. virtual reality sickness virtual reality sickness is a common problem which is often discussed. any mismatch between what is seen and what is felt can lead to virtual reality sickness. the motion platform can reproduce a wide range of motion effects, and therefore it contributes to the reduction of the probability of occurrence of virtual reality sickness. however, two degrees of freedom do not cover all motion directions. the horizontal rotation especially is often mentioned in relation to this phenomenon, and it is recommended not to rotate the camera in the vr world at all[7] or to use a 109 evžen thöndel acta polytechnica ctu proceedings figure 4. mathematical model of the dynamic response. figure 5. mathematical model of the direct dynamic response – rubber ball. figure 6. application of the motion platform. 110 vol. 12/2017 interactive motion platforms and virtual reality for vehicle simulators motion platform with a rotary axis[8]. the vertical linear acceleration can partially be compensated for by rotating the motion platform. therefore, it is planned to extend the construction with a rotation of 360 degrees. this new design will be an optimal construction for simulators using vr headsets with respect to the range of reproduction of motion effects and the financial costs. 7. conclusion a new interactive motion platform has been presented here. the possibility to measure acting forces and torques makes the motion platform suitable for the use in vehicle simulators where direct interaction with a human body is required (bicycle or motorbike). the main advantage is the enhancement of the experience and the contribution to the reduction of the virtual sickness phenomenon. we plan to extend the motion platform with a rotary axis which further improves the solution of the problem with vr sickness. acknowledgements the research and development of the new interactive motion platform is supported by the company pragolet, s.r.o. member of the center of intelligent drives and advanced machine control (cidam) supported by the technology agency of the czech republic (tacr). references [1] human-in-the-loop. wikipedia, the free encyclopedia. wikipedia, the free encyclopedia, 10 dec. 2016. web. 10 dec. 2016. [2] e. thöndel. design and optimal control of a linear electromechanical actuator for motion platforms with six degrees of freedom. 2011, intelligent automation and systems engineering, springer, 65-77. [3] e. thöndel. design and optimization of a motion cueing algorithm for a truck simulator. 2012, in proceeding of the 2012 european simulation and modeling conference, essen, germany, 165-170. [4] e. thöndel. model predictive motion cueing algorithm for a truck simulator. 2013, in proceeding of the 2013 european simulation and modeling conference, lancaster, united kingdom, 188-192. [5] p. members. vývoj zpětnovazebního rehabilitačního přístroje založenãľho na principu pohybové terapie. research project, https://www.rvvi.cz/cep?ss=detail&h=ta03010313, 2015. [6] p. contributors. 4d vr experience modul. the global association for marketing at retail, popai awards 2016, http://www.popai.cz/files/tinymce/files/ popai%20awards%202016/vyher/20.pdf, 2016. [7] o. contributors. oculus rift vr motion sickness. oculus http: //riftinfo.com/oculus-rift-motion-sickness/ -11-techniques-to-prevent-it, 2016. [8] r. contributors. yaw motion sickness. http://www.rotovr.com, 2016. 111 https://www.rvvi.cz/cep?ss=detail&h=ta03010313 http://www.popai.cz/files/tinymce/files/popai%20awards%202016/vyher/20.pdf http://www.popai.cz/files/tinymce/files/popai%20awards%202016/vyher/20.pdf http://riftinfo.com/oculus-rift-motion-sickness/-11-techniques-to-prevent-it http://riftinfo.com/oculus-rift-motion-sickness/-11-techniques-to-prevent-it http://riftinfo.com/oculus-rift-motion-sickness/-11-techniques-to-prevent-it http://www.rotovr.com acta polytechnica ctu proceedings 12:108–111, 2017 1 introduction 2 motion platform 3 mathematical model of the dynamic response 4 load sensors 5 the use in virtual reality 6 virtual reality sickness 7 conclusion acknowledgements references 71 acta polytechnica ctu proceedings 1(1): 71–78, 2014 71 doi: 10.14311/app.2014.01.0071 clustering measurements of broad-line agns: review and future mirko krumpe1,3, takamitsu miyaji2,3, and alison l. coil3 1european southern observatory, karl-schwarzschild-straße 2, 85748 garching bei münchen, germany 2instituto de astronomı́a, unam, apdo. postal 106, ensenada, bc, méxico 3university of california san diego, cass, 9500 gilman drive, la jolla, ca 92093-0424, usa corresponding author: mkrumpe@eso.org abstract despite substantial effort, the precise physical processes that lead to the growth of super-massive black holes in the centers of galaxies are still not well understood. these phases of black hole growth are thought to be of key importance in understanding galaxy evolution. forthcoming missions such as erosita, hetdex, eboss, bigboss, lsst, and panstarrs will compile by far the largest ever active galactic nuclei (agns) catalogs which will allow us to measure the spatial distribution of agns in the universe with unprecedented accuracy. for the first time, agn clustering measurements will reach a level of precision that will not only allow for an alternative approach to answering open questions in agn and galaxy co-evolution but will open a new frontier, allowing us to precisely determine cosmological parameters. this paper reviews large-scale clustering measurements of broad line agns. we summarize how clustering is measured and which constraints can be derived from agn clustering measurements, we discuss recent developments, and we briefly describe future projects that will deliver extremely large agn samples which will enable agn clustering measurements of unprecedented accuracy. in order to maximize the scientific return on the research fields of agn and galaxy evolution and cosmology, we advise that the community develops a full understanding of the systematic uncertainties which will, in contrast to today’s measurement, be the dominant source of uncertainty. keywords: large-scale structure of universe galaxies: active. 1 introduction large area surveys such as the two degree field galaxy redshift survey (2dfgrs; colless et al. 2001) and the sloan digital sky survey (sdss; abazajian et al. 2009) have measured positions and redshifts of millions of galaxies. these measurements allow us to map the 3d structure of the nearby universe1. galaxies are not randomly distributed in space. they form a complex cosmic network of galaxy clusters, groups, filaments, isolated field galaxies, and voids, which are large regions of space that are almost devoid of galaxies. the current understanding of the distribution of galaxies and structure formation in the universe is based on the theory of gravitational instability. very early density fluctuations became the “seeds” of cosmic structure. these have been observed as small temperature fluctuations (δt/t ∼ 5 × 10−5) in the cosmic microwave background with the cosmic background explorer (smoot et al. 1992). the small primordial matter density enhancements have progressively grown through gravitational collapse and created the complex network seen in the distribution of matter in the later universe. during a galaxy’s lifetime different physical processes, which are still not well understood, can trigger a mass flow onto the central super-massive black hole (smbh). in this phase of galaxy evolution, the galaxy is observed as an active galactic nucleus (agn). after several million years, when the smbh has consumed its accretion reservoir, the central engine shuts down, and the object is again observed as a normal galaxy. the agn phase is thought to be a repeating special epoch in the process of galaxy evolution. in recent years it has become evident that both fundamental galaxy and agn parameters change significantly between low (z < 0.3) and intermediate redshifts (z ∼ 1 − 2), e.g., global star formation density (hopkins & beacom 2006) and accretion rate onto smbhs. for example, the contribution to black hole growth has shifted from high luminosity objects at high redshifts to low luminosity objects at low redshifts (agn “downsizing”; e.g., hasinger et al. 2005). it has also become clear that smbh masses follow a tight relation with the mass or velocity dispersion of the stars in galactic bulges (magorrian et al. 1998; gebhardt et al. 2000; ferrarese & merritt 2000). these observational correlations moti1a visual impression is given in this video: http://vimeo.com/4169279 71 http://dx.doi.org/10.14311/app.2014.01.0071 mirko krumpe, takamitsu miyaji, alison l. coil vate a co-evolution scenario for galaxies and agns and provide evidence of a possible interaction or feedback mechanism between the smbh and the host galaxy. the interpretation of this correlation, i.e., whether and to what extent the agn influences its host galaxy, remains controversial (e.g., jahnke & macció 2011). since agns are generally much brighter than (inactive) galaxies, one major advantage of agn large-scale (i.e., larger than the size of a galaxy) clustering measurements over galaxy clustering measurements is that they allow the study of the matter distribution in the universe out to higher redshifts. at these redshifts, it becomes challenging and observationally expensive to detect galaxies in sufficient numbers. furthermore, as the distribution of agns and galaxies in the universe depends on galaxy evolution physics, large-scale clustering measurements are an independent method to identify and constrain the physical processes that turn an inactive galaxy into an agn and are responsible for agn and galaxy co-evolution. in the last decade the scientific interest in agn large-scale clustering measurements has increased significantly. as only a very small fraction of galaxies contain an agn (∼1%), the remaining and dominating challenge in deriving physical constraints based on agn clustering measurements is the relative small sample size compared to galaxy clustering measurements. however, this situation will change entirely in the next decade when several different surveys come online that are expected to identify millions of agn over ∼80% of cosmic time. we therefore review broad-line agn clustering measurements. a general introduction to clustering measurements is given in sections 2 & 3. in section 4 we briefly summarize how agn clustering measurements have evolved and discuss recent developments. in section 5 we discuss the outlook for agn clustering measurements in future upcoming projects. 2 understanding observed clustering properties in our current understanding, the observed galaxy and agn spatial distribution in the universe – i.e., largescale clustering – is caused by the interplay between cosmology and the physics of galaxy evolution. in the commonly assumed standard cosmological model, lambda-cdm, the universe is currently composed of ∼70% dark energy, ∼25% dark matter (dm), and ∼5% baryonic matter (larsen et al. 2011). dark matter plays a key role in structure formation as it is the dominant form of matter in the universe. baryonic matter settles in the deep gravitational potentials created by dark matter, the so-called dark matter halos (dmhs). the term “halo” commonly refers to a bound, gravitationally collapsed dark matter structure which is approximately in dynamical equilibrium. the parameters of the cosmological model determine how the dmhs are distributed in space (fig. 1, left panel, a-branch) as a function of the dmh mass and cosmic time. different cosmological models lead to different properties of the dmh population. figure 1: current conceptual model of the physical processes involved in large-scale galaxy and agn clustering. left: the two branches (a and b) in the diagram show the primary causes of clustering: (a) the properties of the dark matter halo population, which are based on the cosmological model, and (b) the physics of complex processes in galaxy formation and evolution, which lead to a distinct baryonic population within collapsed dark matter halos. figure adapted from weinberg 2002. right: illustration of the spatial distribution of galaxies within a dark matter halo. the picture maps the galaxy cluster abell 1689, where an optical image showing the galaxy cluster members is superimposed with the distribution of dark matter shown in purple. credit: nasa, esa, e. jullo, p. natarajan, and j-p. kneib. inside dmhs, or within halos inside another dmh, called sub-halos, the baryonic gas will radiatively cool. if the gas reservoir is large enough, star and galaxy formation will be initiated. the gas can also be accreted onto the smbh in the center of the galaxy. on scales comparable to the size of the galaxy, the agn can heat and/or eject the surrounding gas, preventing star formation, and eventually removing the gas fueling the agn itself. all the galaxy evolution processes described here determine how galaxies and agns are distributed within dmhs (fig. 1, left panel, b-branch). this distribution of agn and galaxies within dmhs (fig. 1, right panel) is described by the halo occupation distribution (hod; peacock & smith 2000). in addition to the spatial distribution of agn and galaxies in dmhs, the hod describes the probability distributions 72 clustering measurements of broad-line agns: review and future of the number of agns and galaxies per dmh of a certain mass and the velocity distribution of agns and galaxies within a dmh. the interplay between cosmology and galaxy evolution causes the observed large-scale clustering of galaxies and agns. the goal of agn and galaxy clustering measurements is to reverse the causal arrows in the fig. 1 (left panel), working backwards from the data to the galaxy & agn halo occupation distribution and dmh population properties, in order to finally draw conclusions about galaxy and agn physics, as well as to constrain fundamental cosmological parameters. 3 clustering measurements the most common statistical estimator for large-scale clustering is the two-point correlation function (2pcf; peebles 1980) ξ(r). this quantity measures the spatial clustering of a class of object in excess of a poisson distribution. in practice, ξ(r) is obtained by counting pairs of objects with a given separation and comparing them to the number of pairs in a random sample with the same separation. different correlation estimators are described in the literature (e.g., davis & peebles 1983; landy & szalay 1993). the large-scale clustering of a given class of objects can be quantified by computing the angular (2d) correlation function, which is the projection onto the plane of the sky, or with the spatial (3d) correlation function, which requires redshift information for each object. obtaining spectra to measure the 3d correlation function is observationally expensive, which is the main reason why some studies have had to rely on angular correlation functions. however, 3d correlation function measurements are by far preferable, since the deprojection (limber 1954) of the angular correlation function introduces large systematic uncertainties. despite these large caveats and the already moderately low uncertainties of current 3d correlation measurements, the use of angular correlation functions might still be justified when exploring a new parameter space. however, the next generation multi-object spectrographs (e.g., 4most (de jong et al. 2012), bigboss (schlegel et al. 2011), and weave (dalton et al. 2012)), will make it far easier to simultaneously obtain thousands of spectra over wide fields. hence, measurements of the 3d correlation function will soon become ubiquitous. as one measures line-of-sight distances for 3d correlation functions from redshifts, measurements of ξ(r) are affected by redshift-space distortions due to peculiar velocities of the objects within dmhs. to remove this effect, ξ(r) is commonly extracted by counting pairs on a 2d grid of separations where rp is perpendicular to the line of sight and π is along the line of sight. then, integrating along the π-direction leads to the projected correlation function, wp(rp), which is free of redshift distortions. the 3d correlation function ξ(r) can be recovered from the projected correlation function (davis & peebles 1983). the resulting signal can be approximated by a power law where the largest clustering strength is found at small scales. at large separations of >50 mpc h−1 the distribution of objects in the universe becomes nearly indistinguishable from a randomly-distributed sample. only on comoving scales of ∼100 mpc h−1 can a weak positive signal be detected (e.g., eisenstein et al. 2005; cole et al. 2005) which is caused by baryonic acoustic oscillations (bao) in the early universe. the spatial clustering of observable objects does not precisely mirror the clustering of matter in the universe. in general, the large-scale density distribution of an object class is a function of the underlying dark matter density. this relation of how an object class traces the underlying dark matter density is quantified using the linear bias parameter b. this contrast enhancement factor is the ratio of the mean overdensity of the observable object class, the so-called tracer set, to the mean overdensity of the dark matter field, defined as b = (δρ/〈ρ〉)tracer/(δρ/〈ρ〉)dm, where δρ = ρ− 〈ρ〉, ρ is the local mass density, and 〈ρ〉 is the mean mass density on that scale. in terms of the correlation function, the bias parameter is defined as the square root of the 2pcf ratio of the tracer set to the dark matter field: b = √ ξtracer/ξdm. rare objects which form only in the highest density peaks of the mass distribution have a large bias parameter and consequently a large clustering strength. theoretical studies of dmhs (e.g., mo & white 1996; sheth et al. 2001) have established a solid understanding of the bias parameter of dmhs with respect to various parameters. comparing the bias parameter of an object class with that of dmhs in a certain mass range at the same cosmological epoch allows one to determine the dmh mass which hosts the object class of interest. a halo may contain substructures, but the dmh mass inferred from the linear bias parameter refers to the single, largest (parent) halo in the context of hod models. 3.1 why are we interested in agn clustering? agn clustering measurements explore different physics on different scales. at scales up to the typical size of a dmh (∼ 1 − 2 mpc), clustering measurements are sensitive to the physics of galaxy and agn formation and evolution. constraints on the galaxy and agn merger rate and the radial distribution of these objects within dmhs can be derived. on scales larger than the size of dmhs, the large-scale clustering is sensi73 mirko krumpe, takamitsu miyaji, alison l. coil tive to the underlying dm density field, which essentially depends only on cosmological parameters. consequently, with only one measurement both galaxy and agn co-evolution as well as cosmological parameters can be studied. future high precision agn clustering measurements have the potential to accurately establish missing fundamental parameters that describe when agn activity and feedback occur as a function of luminosity and redshift. since they will precisely determine how dmhs are populated by agn host galaxies, these measurements will also improve our theoretical understanding of galaxy and agn evolution by enabling comparisons to galaxy measurements and cosmological simulations. here, we elaborate on some (though not all) of the critical observational constraints which are provided by agn clustering measurements: • agn host galaxy – agn cannot be more clustered than the type of galaxies they reside in. thus, agn clustering measurements determine the host galaxy type in a statistical sense for the entire agn sample, regardless of the agn’s luminosity. comparing the observed agn clustering to very accurate galaxy clustering measurements, which depend on different galaxy subclasses (morphological, spectral type, luminosity), constrains the agn host galaxy type. • external (mergers) vs. internal triggering – different theoretical models (e.g., fry 1996; sheth et al. 2001; shen 2009) of how agns are triggered predict very different large-scale clustering properties with agn parameters such as luminosity and redshift. moderately precise agn clustering measurements allow us to distinguish between these different models (allevato et al. 2011). furthermore, the validity of different models can be tested for different luminosities and cosmological epochs. • fundamental galaxy/agn physics – agn largescale clustering dependences with various agn properties could potentially be a key source of independent constraints on galaxy/agn physics. comparing the observed agn clustering properties with results from simulations with different inputs for galaxy/agn physics could identify the physics that links the evolution of agns and galaxies. • agn lifetimes – agn clustering measurements allow us to estimate the agn lifetime at different cosmological epochs (martini & weinberg 2001). the underlying idea is that rare, massive dmhs are highly biased tracers of the underlying mass distribution, while more common objects are less strongly biased (kaiser 1984). therefore, if agns are heavily biased they must be in rare, massive dmhs. the ratio of the agn number density to the host halo number density is a measure of the “duty cycle”, i.e., the fraction of the time that the object spends in the agn phase. • cosmological parameters – as agn clustering measurements extend to much higher redshifts than galaxy clustering measurements, they can be used to derive constraints on cosmological parameters (e.g., basilakos & plionis 2009) back to the time of the formation of the first agns. currently, the detection of the bao imprint on clustering measurements at different cosmological epochs is of great interest to constrain the equation of state of dark energy. agn large-scale clustering measurements with very large agn samples can detect the bao signal in a redshift range that is not accessible with galaxy clustering measurements. 4 agn clustering measurements: past and present until the 1980s, studies had to primarily rely on small, optically-selected, very luminous agn samples for clustering measurements. then the main question was whether agns are randomly distributed in the universe (e.g., bolton et al. 1976; setti & woltjer 1977). the extremely small sample sizes did not allow clustering measurements at scales below ∼50 mpc, where a significant deviation from a random distribution is present. thanks to the launch of major x-ray missions in the 1980s and 1990s such as einstein (giacconi et al. 1979) and rosat (truemper 1993), much larger agn samples enabled successful detections of the agn large-scale clustering signal. a detailed review on the history of x-ray agn clustering measurements is given in cappelluti et al. (2012). although agn clustering measurements are far from being as precise as galaxy clustering measurements, some general findings have emerged in recent years. interestingly, over all of studied cosmic time (z ∼ 0 − 3), broad-line agns occupy dmh masses of log (mdmh/[h −1m�]) ∼ 12.0−13.5 and therefore cluster like groups of galaxies. more detailed information about the current picture of broad-line agn clustering is presented in section 6.6 of krumpe et al. (2012). some puzzling questions remain. for example, at z < 0.5 a weak x-ray luminosity dependence on the clustering strength is found (in that luminous x-ray agns cluster more strongly than their low luminosity counterparts, e.g., krumpe et al. 2010; cappelluti et al. 2010; shen et al. 2013). however, at high redshift it seems that high luminosity, optically-selected agns cluster less strongly than moderately-luminous 74 clustering measurements of broad-line agns: review and future x-ray selected agns. whether this finding is due to differences in the agn populations, an intrinsic luminosity dependence to the clustering amplitude, or an observational bias is yet not understood. we note that different studies have used different relations to translate the measured linear bias parameter to dmh mass, as well as different σ8 values. therefore, instead of blindly comparing the derived dmh mass, re-calculating the masses based on the same linear bias to dmh mass relation and the same σ8 is essential when comparing measurements in the literature. 4.1 recent developments in the last few years several new approaches have been used to improve the precision of agn clustering measurements or their interpretation. we summarize these developments below. cross-correlation measurements: auto-correlation function (acf) measurements of broad-line agns often have large uncertainties due to the low number of objects. especially at low redshifts, large galaxy samples with spectroscopic redshifts are frequently available. in such cases, the statistical uncertainties of agn clustering measurements can be reduced significantly by computing the cross-correlation function (ccf). the ccf measures the clustering of objects between two different object classes (e.g., broadline agns and galaxies), while the acf measures the spatial clustering of objects in the same sample (e.g., galaxies or agns). ccfs have been used before to study the dependence of the agn clustering signal with different agn parameters. however, these values could not be compared to other studies as the ccfs also depend on the galaxy populations used and their clustering strength. only recently has an alternative approach (coil et al. 2009) allowed the comparison of the results from different studies by inferring the agn acf from the measured ccf and acf of the galaxy tracer set. the basic idea of this method, which is now frequently used (e.g., krumpe et al. 2010, 2012; mountrichas & georgakakis 2012; shen et al. 2013), is that both populations trace the same underlying dm density field. photometric redshift samples: large galaxy tracer sets with spectroscopic redshifts are not available at all redshifts. some studies therefore rely on photometric redshifts. the impact of the large uncertainties and catastrophic outliers when using photometric redshifts is commonly not considered but it can be essential. the use of the full probability density function (pdf) of the photometric redshift fit, instead of a single value for the photometric redshift, has been used in some studies (e.g., mountrichas et al. 2013). here, photometric galaxies samples are used as tracer sets to derive the ccf between agn and galaxies. each object is given a weight for the probability that it is actually located at a certain redshift based on the fit to the photometric data. figure 2: in the conceptual model of the hod approach, there are two contributions to the pairs that account for the measured correlation function. pairs of objects (black stars) can either be located within the same dmh (pink filled circles), such that their measured separation contributes to the 1-halo term (red solid line in the large dmh), or can reside in different dmhs, such that their separations (green dotted line) contribute to the 2-halo term. agn halo occupation distribution modeling: instead of deriving only mean dmh masses from the linear bias parameter, hod modeling of the correlation function allows the determination of the full distribution of agn as a function of dmh mass. the derived distribution also connects observations and simulations as it provides recipes for how to populate dmhs with observable objects. in the hod approach, the measured 2pcf is modeled as the sum of contributions from pairs within individual dmhs (fig. 2; 1-halo term) and in different dmhs (2-halo term). the superposition of both components describes the shape of the observed 2pcf better than a simple power law. in the hod description, a dmh can be populated by one central agn or galaxy and by additional objects in the same dmh, so-called satellite agn and galaxies. applying the hod approach to the 2pcf allows one to determine, e.g., the minimum dmh needed to host the object class of interest, the fraction of objects in satellites, and the number of satellites as a function of dmh mass. instead of using the derived agn acf from ccf measurements, miyaji et al. (2011) utilize the hod model directly on high precision agn vs. galaxy ccf and achieve additional constraints on the agn and galaxy co-evolution and agn physics. 75 mirko krumpe, takamitsu miyaji, alison l. coil theoretical predictions: only recently have several different theoretical models been published which try to explain the observed agn clustering with different physical approaches (e.g, fanidakis et al. 2013; hütsi et al. 2014). the key to observationally distinguish between these models are their different predictions for the clustering dependences of different agn parameters. in addition to theoretical models of the observed clustering, other very recently developed models predict the halo occupation distribution of agns at different redshifts, e.g., chatterjee et al. (2012). the major challenge presented by all of these models is the urgent need for observational constraints with higher precision than can be provided with current agn samples. in the future, progress in agn physics and agn and galaxy evolution will be achieved through a close interaction between state-ofthe-art cosmological simulations and observational constraints from high precision clustering measurements. simulations which incorporate different physical processes will lead to different predictions of the agn and galaxy large-scale clustering trends and their halo occupation distributions. observational studies will then identify the correct model and consequently the actual underlying physical processes. 5 the future of agn clustering measurements agn clustering measurements from several upcoming projects will significantly extend our knowledge of the growth of cosmic structure and will also provide a promising avenue towards new discoveries in the fields of galaxy and agn co-evolution, agn triggering, and cosmology. for example, erosita (predehl et al. 2010; launch 2015/2016) will perform several all-sky x-ray surveys. after four years the combined survey is expected to contain approximately three million agns. hetdex (hill et al. 2008; start 2015) will use an array of integral-field spectrographs to provide a total sample of ∼20,000 agns without any pre-selection over an area of∼ 450 deg2. the sdss-iv/eboss and bigboss builds upon the sdss-iii/boss project and will use a fiber-fed spectrograph. over an area of 14,000 deg2, it will observe roughly one million qsos at 1.8 < z < 3.5. in addition to these projects, there will be other major enterprises such as lsst (lsst collaboration 2009) and pan-starrs (kaiser et al. 2002) which will detect several million agns but currently lack dedicated spectroscopic follow-up programs. in the following we will focus on erosita, as this mission will compile the largest agn sample ever observed. figure 3 shows that erosita agn detections will outnumber current galaxy samples with spectroscopic redshifts at z > 0.4. using a large number of agns that continuously cover the redshift space, will allow us (in contrast to galaxy samples) to measure the distribution of matter with high precision in the last ∼11 gyr of cosmic time. to fully exploit the erosita potential for agn clustering measurements, a massive spectroscopic follow-up program is needed. several spectroscopic multi-object programs and instruments are currently planned or are in an early construction phase (e.g., sdss-iv/spiders and 4most). figure 3: number of expected erosita agns (red) and currently available galaxies with spectroscopic redshifts (black solid line at z < 0.4 – sdss data release 7; black dotted line – primus (coil et al. 2011); black solid line at z ∼ 1 – deep2 (davis et al. 2003) and vvds (le fèvre et al. 2005)). instead of the full sky area, we consider only the expected number of erosita agns with spectroscopic redshifts from 4most over 14,000 deg2. erosita agn clustering measurements at z ∼ 0.8 − 1 will even allow for the detection of the bao signal. the feasibility of such a measurement can be estimated using the bao detection found with ∼46,000 sdss lrgs (〈z〉 = 0.35) over 3,816 square degrees of sky (0.72 h−3 gpc3) as a standard for comparison (eisenstein et al. 2005). the observed agn x-ray luminosity function (gilli et al. 2007) and the erosita sensitivity determine the number density of erosita agns. in the abovementioned redshift range, the erosita agn area density will be comparable to that of sdss lrgs at lower redshifts. therefore, the comoving volume number density of erosita agns will be five times lower than that of sdss lrgs. since erosita will conduct an all-sky survey, the increased sky area will counterbalance the lower volume density. given the signal-to-noise ratio (s/n) of the bao detection of eisenstein et al. (2005) and an assumed spectroscopic area of 14,000 deg2, we expect a ∼3σ bao detection using erosita agns only in the redshift range of z ∼ 0.8 − 1. this is consistent with 76 clustering measurements of broad-line agns: review and future kolodzig et al. (2013), who use a different approach based on the angular power spectrum for estimating the significance of a bao detection with erosita agns. with the much larger agn datasets that will exist in the future, the statistical uncertainties in clustering measurements will be significantly decreased. systematic uncertainties will then be the dominant source of uncertainty. the impact and level of different systematic uncertainties can only be carefully explored and quantified through simulations. thus far, there has not been a need for such studies because the agn samples to date are i) drawn from surveys that (with exceptions) cover a rather moderate sky area and are therefore likely to suffer from the problem of cosmic variance2 and/or ii) comprised of up to several thousand objects and are consequently poisson noise dominated. both limitations will be removed in future agn clustering measurements with the upcoming extensive agn samples covering extremely large sky areas. however, to derive reliable constraints on agn physics and cosmology, as well as to avoid any possible misinterpretations of future unprecedented high precision agn clustering measurements, we have to fully understand and be able to correctly model the impact of the systematic uncertainties. only then can we maximize the scientific return of future agn clustering measurements and have a major impact in the field of cosmology and galaxy and agn evolution. acknowledgement mk received funding from the european community’s seventh framework programme (/fp7/20072013/) under grant agreement no 229517. tm is supported by unam/papiit in104113 and conacyt 179662. alc acknowledges support from nsf career award ast-1055081. references [1] abazajian et al. 2009, apjs, 182, 543. doi:10.1088/0067-0049/182/2/543 [2] allevato et al. 2011, apj, 736, 99. doi:10.1088/0004-637x/736/2/99 [3] bolton et al. 1976, apj, 210, l1. 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[54] weinberg 2002, aspc, 283, 3. 78 http://dx.doi.org/10.1088/0067-0049/192/2/16 http://dx.doi.org/10.1086/318331 http://dx.doi.org/10.1088/0004-637x/726/2/83 http://dx.doi.org/10.1111/j.1365-2966.2011.20059.x http://dx.doi.org/10.1093/mnras/sts666 http://dx.doi.org/10.1046/j.1365-8711.2000.03779.x http://dx.doi.org/10.1046/j.1365-8711.2001.04006.x introduction understanding observed clustering properties clustering measurements why are we interested in agn clustering? agn clustering measurements: past and present recent developments the future of agn clustering measurements 163 acta polytechnica ctu proceedings 1(1): 163–169, 2014 163 doi: 10.14311/app.2014.01.0163 modelling the multifrequency sed of agn candidates among the unidentified egret and fermi gamma-ray sources pieter j. meintjes1, pheneas nkundabakura2,1, brian van soelen1, alida odendaal1 1department of physics, university of the free state, p.o. box 339, bloemfontein, 9300, south-africa 2kigali institute of education, p.o. box 5039, kigali, rwanda corresponding author: meintjpj@ufs.ac.za abstract of the 271 sources in the 3rd egret catalogue, 131 were reported as unidentified, i.e. not associated with any particular class of point source in the sky. since the largest fraction of the egret sources were extragalactic, a sample of 13 extragalactic unidentified sources have been selected for multi-wavelength follow-up studies. five of the selected egret sources coincide with gamma-ray flux enhancements seen in the fermi-lat data after one year of operation. in this article, we report the multi-wavelength properties of, among others, the 5 sources detected by fermi-lat from our sample of high galactic latitude unidentified egret sources. recent spectroscopic observations with the southern african large telescope (salt) confirmed one of the unidentified egret sources as a possible seyfert 2 galaxy, or alternatively, a narrow line radio galaxy. the detected gamma-ray emission (eγ > 30 mev) of the 5 coinciding egret/fermi-lat sources are fitted with external compton and synchrotron self compton (ssc) models to investigate the energetics required to produce the egret/fermi gamma-ray flux. in all the models the inclination angle of the jet with respect to the observer is θjet ≈ 60◦, between those of seyfert 1 and seyfert 2/radio galaxies. these results confirm the possibility of seyfert and radio galaxies sources are constituting a new class of γ-ray source in the energy range eγ > 30 mev. keywords: radiation mechanisms: non-thermal line: identification techniques: spectroscopic galaxies: jets bl lacertae objects. 1 introduction the energetic gamma ray telescope experiment egret (30 mev 10 gev) provided the highest gamma-ray window on board the compton gammaray observatory (cgro). egret detected 271 gamma-ray sources above 100 mev, 92 % of which were blazars. of the 271 sources detected, 131 remained unidentified, i.e. could not be associated with any specific point source of gamma-ray emission (hartman et al., 1999). the large number of unidentified egret sources above and below the galactic plane inspired a search for possible extra-galactic radio loud active galactic nuclei (agn) counterparts that could possibly be associated with these unidentified sources. to avoid confusion with possible galactic sources, especially molecular cloud distributions, the search for counterparts was restricted to those unidentified sources at galactic latitudes | b | > 10◦. source selection criteria: the candidate counterparts should be inside the error box associated with the egret detection (hartman et al., 1999), confirmed as extragalactic in the nasa extragalactic database (ned), possess a radio brightness above 100 mjy at 8.4 ghz (sowards-emmerd, romani & michelson, 2003), exhibit hard spectra with spectral indices | α | < 0.7 (sowards-emmerd, romani & michelson, 2003) and display variability (e.g. fan, 2005) that may be associated with an inner accretion disc or jet. based upon these criteria, 13 sources have been selected for further follow-up study (meintjes & nkundababura, 2012; nkundabakura & meintjes, 2012). of the 13 candidate sources selected, 5 have confirmed gamma-ray excesses in the fermi-lat catalogue containing the first year’s observations (abdo et al., 2010a). the fermi large area telescope (fermilat) is a pair conversion γ-ray telescope sensitive to photon energies between 20 mev and 300 gev. launched on 11 june 2008, fermi-lat started to collect data in august 2008. the data are made available on a daily basis and can be accessed online at the official website of the fermi science support centre (http://fermi.gsfc.nasa.gov/cgi-bin/ssc /lat/latdataquery.cgi). the results of detections made within the first 24 months of operation were released in june 2011, in the form of the second fermi-lat catalog 163 http://dx.doi.org/10.14311/app.2014.01.0163 pieter j. meintjes et al. (2fgl; see nolan et al., 2012) 1. five sources from our previous sample of unidentified egret sources have been detected with fermilat, namely 2fgl j0727.0-4726, 2fgl j1304.3-4353, 2fgl j1703.2-6217, 2fgl j1709.0-0821 and 2fgl j1815.6-6407, which are counterparts of 3eg j07244713, 3eg j1300-4406, 3eg j1659-6251, 3eg j17090828 and 3eg j1813-6419 respectively. the fermi-lat sources that coincided with the egret sources are presented as circled crosses in fig. 1. the egret (30 mev-10 gev) gamma-ray spectra of our chosen sample of sources that were observed between april 1991 october 1995 (cycles 1, 2 3 and 4 of the mission) have been determined. the photon spectral index distribution is displayed in fig. 2. the spectral distribution of these unidentified sources corresponds remarkably well with the gamma-ray blazar photon spectral index distribution observed by fermilat (abdo et al., 2010a). b=−90° b=+90° l=0° b=+10° b=−10° b=0°,l=+360° b=+30° b=+60° b=−30° b=−60° figure 1: galactic distribution of the unidentified egret sources (circles) and their fermi-lat counterparts (crosses). 1 1.5 2 2.5 3 3.5 4 3eg j0159-3603 3eg j0500+2529 3eg j0702-6212 3eg j0706-3837 3eg j0724-4713 3eg j0821-5814 3eg j1300-4406 3eg j1659-6251 3eg j1709-0828 3eg j1800-0146 3eg j1813-6419 3eg j1822+1641 3eg j1824+3441 γra y ph ot on in de x hsp-bllacs l and isp-bllacs fsrqs γ=2.03 γ=2.38 figure 2: gamma-ray photon spectral indices of the egret sources between 30 mev 10 gev. the gamma-ray spectra of the sample of egret sources with fermi-lat counterparts were determined. the spectra are presented in fig. 3. noticeable is the apparent change in the spectral index between the egret and the fermi-lat gamma-ray data, which may point to a transition in the gamma-ray production process. -100 0 100 10 100 1000 10000 100000r es id ua ls ( % ) e (mev) 1e-15 1e-14 1e-13 e 2 (d n /d e )( w .m -2 ) 3eg j0724-4713 dn(e)=const e-2.6de a.) 3eg j0724-4713 -100 0 100 10 100 1000 10000 100000 1e+06r es id ua ls ( % ) e (mev) 1e-15 1e-14 1e-13 e 2 (d n /d e )( w .m -2 ) 3eg j1300-4606 dn(e)=const e-3.07de c.) 3eg j1300-4406 -100 0 100 10 100 1000 10000 100000r es id ua ls ( % ) e (mev) 1e-15 1e-14 1e-13 e 2 (d n /d e )( w .m -2 ) 3eg j1659-6251 dn(e)=const e-2.83de 1e-15 1e-14 1e-13 e 2 (d n /d e )( w .m -2 ) 3eg j1659-6251 dn(e)=const e-2.83de b.) 3eg j1659-6251 -100 0 100 10 100 1000 10000 100000r es id ua ls ( % ) e (mev) 1e-15 1e-14 1e-13 e 2 (d n /d e )( w .m -2 ) 3eg j1709-0828 dn(e)=const e-3de d.) 3eg j1709-0828 -100 0 100 10 100 1000 10000 100000r es id ua ls ( % ) e (mev) 1e-15 1e-14 1e-13 e 2 (d n /d e )( w .m -2 ) 3eg j1813-6419 dn(e)=const e-2.85de e.) 3eg j1813-6419 figure 3: the gamma-ray spectra of the egret (30 mev 10 gev) and coinciding fermi-lat (20 mev 300 gev) sources. 2 gamma-ray variability the multi-wavelength emission of accretion driven sources like agn is characterized by very high luminosity, assuming isotropic emission, and variability over several time scales (e.g. fan, 2005). this is reconciled with the fact that the bulk of the spectral energy distribution (sed) of these sources is produced in a non-homogeneous and variable jet. gamma-ray flux 1http://fermi.gsfc.nasa.gov/ssc/data/access/lat/2yr catalog/ 164 modelling the multifrequency sed of agn candidates among the unidentified egret... variability has also been confirmed from agn-blazars (mattox et al., 1997). aperture photometry of the fermi-lat data over a time span of 4.6 years (from august 2008 to march 2013) has been performed to investigate possible long term variability. photons in the energy interval 100 mev to 200 gev were counted in an area with a radius of 1 degree centered on the source and monthly averages were determined. two of the sources, 2fgl j1304.3-4353 and 2fgl j1703.2-6217, showed definite signs of variability, quantified in terms of a variability index v (nolan et al., 2012), which implies that for v > 41 there is a < 1% probability of the source being steady. although variability was detected in 2fgl j1304.3-4353 (v = 47) and 2fgl j1703.2-6217 (v = 167) respectively, no periodicity could be detected (see fig. 4). 1e-07 1.5e-07 2e-07 2.5e-07 3e-07 3.5e-07 54500 55000 55500 56000 56500 ph to n fl ux ( ph ot on s. cm -2 .s -1 ) time (mjd) 2fgl j1304.3-4353 (3eg j1300-4406) average a.) 2fgl j1304.3-4353 1e-07 1.5e-07 2e-07 2.5e-07 3e-07 3.5e-07 4e-07 4.5e-07 5e-07 5.5e-07 54500 55000 55500 56000 56500 ph ot on f lu x (p ho to ns .c m -2 .s -1 ) time (mjd) 2fgl j1703.2-6217(3eg j1659-6251) average b.) 2fgl j1703.2-6217 figure 4: the gamma-ray lightcurves of the two fermi-lat sources, 2fgl j1304.3-4353 and 2fgl j1703.2-6217, which displayed variability over a period of 4.6 years. the vertical error bars indicate the 68% confidence level. 3 optical follow-up studies the optical counterparts of two unidentified egret sources have already been identified (meintjes & nkundabakura, 2012; nkundabakura & meintjes, 2012). the spectrum of pks j0820-5705 (3eg j08215814) resembles that of a fsrq at redshift z = 0.06, while the spectrum of pmn j0710-3850 (3eg j0706-3837) shows broad and narrow lines resembling the spectrum of a liner or seyfert i galaxy at redshift z = 0.129. what distinguishes the spectrum of pks j0820-5705 from that of a normal radio galaxy is the shallow k4000 depression of only 8.8 ± 2.5 %, indicating substantial non-thermal activity, while the corresponding value for pmn j0710-3850 is 80 ± 1 % (meintjes & nkundabakura, 2012; nkundabakura & meintjes, 2012), in agreement with the value expected for a liner-seyfert 1 galaxy (e.g. caccianiga et al., 1999). spectroscopic observations of other sources from our sample have been performed with the southern african large telescope (salt) (see fig. 5), equipped with the robert stobie spectrograph (rss), during 2012, in order to determine the redshift and to identify the class of agn. the spectrum of one of the unidentified egret sources, 3eg j 0159-3603, could be determined (see fig. 6), showing distinct narrow emission lines of o ii, o iii and he ii redshifted by z = 0.35. the spectrum resembles that of a typical seyfert 2 galaxy, or alternatively, a narrow line radio galaxy. this implies the possible association of two seyfert galaxies with the unidentified sources 3eg j0706-3837 and 3eg j 0159-3603 respectively. figure 5: the southern african large telescope (salt). −5e−16 0 5e−16 1e−15 1.5e−15 2e−15 4500 5000 5500 6000 6500 7000 7500 f lu x (e rg s− 1 c m − 2 å − 1 ) wavelength (å) [n ei ii] + h ε [o ii] [n ei ii] [o iii ] h γ pmn j0156−3616 (z=0.35) [o iii ] * * * * h ei i figure 6: salt spectrum of the optical counterpart of the unidentified egret source 3eg j0159-3603, showing emission lines redshifted by z=0.35 4 the spectral energy distributions (sed) the spectral energy distributions (seds) of all the counterparts corresponding to the unidentified egret 165 pieter j. meintjes et al. sources have been pieced together through multiwavelength archival data as well as multi-wavelength observations from radio to optical, using the hartebeesthoek radio astronomy observatory (hartrao) 26 m telescope, as well as various optical telescopes at the south african astronomical observatory (saao) in south africa. infrared data were obtained from the two micron all sky survey (2mass) conducted between june 1997 and february 2001. the seds of the sample of egret sources and the associated fermilat counterparts are presented in fig. 7. 1e-18 1e-17 1e-16 1e-15 1e-14 1e-13 1e-12 1e-11 1e+10 1e+15 1e+20 1e+25 νf ν (w m -2 ) ν (hz) radio opt. fermi egret 3eg j0724-4713 a.) 3eg j0724-4713 1e-18 1e-17 1e-16 1e-15 1e-14 1e-13 1e-12 1e-11 1e+10 1e+15 1e+20 1e+25 νf ν (w m -2 ) ν (hz) radio opt. rosat egret 3eg j1300-4406 fermi c.) 3eg j1300-4406 1e-18 1e-17 1e-16 1e-15 1e-14 1e-13 1e-12 1e-11 1e+10 1e+15 1e+20 1e+25 νf ν (w m -2 ) ν (hz) radio opt. nir egret 3eg j1659-6251 fermi iras b.) 3eg j1659-6251 1e-18 1e-17 1e-16 1e-15 1e-14 1e-13 1e-12 1e-11 1e+10 1e+15 1e+20 1e+25 νf ν (w m -2 ) ν (hz) radio opt. egret 3eg j1709-0828 fermi d.) 3eg j1709-0828 1e-18 1e-17 1e-16 1e-15 1e-14 1e-13 1e-12 1e-11 1e+10 1e+15 1e+20 1e+25 νf ν (w m -2 ) ν (hz) radio opt. nir egret 3eg j1813-6419 fermi e.) 3eg j1813-6419 figure 7: the multifrequency seds for the sample of egret sources. the association of some of the unidentified egret sources with seyfert galaxies/liners poses a possibility of non-aligned agn and radio galaxies constituting a new class of gamma-ray sources. before discussing the modeling of the seds presented above, a brief discussion of the gamma-ray properties of some radio galaxies are presented to illustrate that these sources possess the required energetics to produce measurable γ-ray emission in the egret and fermi-lat energy domain 5 non-aligned agn: a new class of gamma-ray source at high energies (he; eγ > 100 mev) fermi-lat reported about ten misaligned radio galaxies (abdo et al., 2010b,c; rieger, 2012a). at very high energies (vhe; eγ > 100 gev), four radio galaxies have been detected, cen a (d ≈ 3.8 mpc), m87 (d ≈ 16.7 mpc) and the perseus cluster (d ≈ 77 mpc; z ≈ 0.018) sources ngc 1275 and ic 310 (e.g. rieger, 2012a). cen a was the only non-blazar detected at mev to gev energies by cgro (see steinle, 2010 for a review). the he emission from cen a reported by fermi-lat seems to come from both the extended radio lobes and the core region (abdo et al., 2010b,c). the detected he gamma-rays from the extended lobe regions suggests that particle acceleration up to vhes occurs in the disrupted jet region (bordas, 2012). the reported tev emission from cen a (aharonian et al., 2009) provided further evidence of a very effective particle accelerator in cen a. the spectrum up to 5 tev is consistent with a power-law with a photon index ∼ 2.7 ± 0.5, with no apparent variability. the he (eγ > 0.2 gev) emission in cen a is explained in terms of inverse compton (ic) upscattering of the cosmic microwave background (cmb) photons (eph = 8 × 10−4 ev) and infrared (ir) background photons by relativistic electrons with lorentz factors γe = 6 × 105, in a jet with bulk flow velocities between βγ ∼ 0.1-0.5. another peculiar aspect of cen a is a rather low, sub-eddington inferred accretion rate, ṁ ∼ 10−3ṁedd, resulting in a rather low bolometric luminosity lb ∼ 1043 erg s−1 (whysong & antonucci, 2004). the inferred equipartition magnetic field in the radio lobes is b ≈ 9 µg (rieger, 2012b), with the equipartition magnetic field near the black hole (bh) ranging between b ∼ 103 − 104 g (rieger, 2012b). the detection of non-aligned agn in the he and vhe regime poses interesting theoretical challenges regarding particle acceleration and associated gammaray emission in the jets of agn. for example, cen a shows that the radio lobes of radio galaxies may possess the required energetics to accelerate electrons to vhes producing the he gamma-rays through ic upscattering the cmb photons, even though the bulk flow lorentz factor of the jet is fairly low. the detection of tev gamma-rays is explained in terms of γe ∼ 107 electrons up-scattering disc photons to the tev domain (rieger & aharonian, 2009). the nuclear sed of cen a, based on non-simultaneous data, shows two peaks, one around∼ 1013 hz and another around 0.1 mev (e.g. chiaberge et al., 2001; abdo et al., 2010c). the sed below a few gev seems to be satisfactorily explained by a one-zone synchrotron self-compton (ssc) model (chiaberge et al., 2001) but the same approach fail to account for the tev emission observed by h.e.s.s. (abdo et al., 2010c). 166 modelling the multifrequency sed of agn candidates among the unidentified egret... the discussion presented above underlines the fact that normal, non-aligned agn do possess the required energetics to accelerate leptons to vhe energies. the production of sub-gev gamma-rays through a ssc process in the nuclear region, combined with the he emission in the radio lobes and tev emission in the inner disc region close to the black hole (bh), presents a new paradigm in particle acceleration and gamma-ray production in agn. with this in mind, the sed of the fermi-lat counterparts of the unidentified egret sources were modelled. this is a first attempt to explain the sed of these sources within the framework of a synchrotron self-compton (ssc) and external compton (ec) model. these sources are all treated as misaligned agn, with a fixed inclination of θjet ≈ 60◦ between jet and observer. 6 sed modelling the multi-wavelength data from radio to gamma-rays have been combined to create the sed over more than 15 decades in energy (fig. 7). the egret and fermilat gamma-ray data are evaluated with the theoretical framework of a single zone synchrotron self-compton (ssc) (e.g. katarczynski, sol & kus, 2001) and external compton (ec) model (e.g. moderski et al., 2003; sikora, begelman & rees, 1994), i.e. where relativistic jet electrons up-scatter infrared (ir) photons from the disc torus and optical photons from the broad emission line (bel) regions to high energies. the model parameters for the ssc and ec models are presented in table 1 (ssc) and table 2 (ec). the corresponding sed model fits are presented in fig. 8. table 1: parameters related to ssc models for the respective sources. source 3eg j0724-4713 3eg j1659-6251 3eg j1709-0828 3eg j1813-6419 parameter units 1 radius (m) 1.5e+14 1.0e+14 1.0e+14 1.0e+14 2 b (t) 7.0e-04 7.5e-04 2.5e-04 2.5e-04 3 p1 -2 -2 -2 -2 4 p2 -3 -2.6 -2.6 -2.6 5 γmax 1.6e+03 6.2e+02 1.6e+03 2.0e+03 table 2: parameters related to the ec models for the respective sources. source r θobs γbr ke νbel αbel νir (1) (2) (3) (4) (5) (6) (7) 3eg j0724-4713 1.0e+17 1 2.0e+03 4.0e+55 10 -1 0.1 3eg j1300-4406 (bel) 1.0e+17 1 2.0e+04 6.0e+53 1 -1 0.1 3eg j1300-4406 (ir) 1.0e+17 1 3.0e+03 4.0e+54 1 -1 0.1 3eg j1659-6251 (bel) 1.0e+17 1 2.0e+03 6.0e+54 10 -1 0.1 3eg j1659-6251 (ir) 1.0e+17 1 2.0e+03 3.0e+55 10 -0.5 0.1 3eg j1709-0828 1.0e+17 1 2.0e+03 3.0e+55 10 -1 0.1 3eg j1800-0146 2.5e+16 1 5.0e+02 3.0e+55 1 -1 0.1 3eg j1813-6419 1.0e+17 1 2.4e+03 1.3e+55 10 -1 0.1 (1): radius of the emitting region (in cm), (2): viewing angle (in radians), (3): electron lorentz factor at spectral break, (4): electron normalization constant, (5): characteristic frequency of bel (in ev), (6): bel distribution photon index, (7): radiation characteristic frequency of ir (in ev). 167 pieter j. meintjes et al. 1e-18 1e-17 1e-16 1e-15 1e-14 1e-13 1e-12 1e-11 1e+10 1e+15 1e+20 1e+25 νf ν (w m -2 ) ν (hz) radio opt. fermi rosat egret 3eg j0724-4713 ec (ir) scc sync scc ec (bel)ic (tot) a.) 3eg j0724-4713 1e-18 1e-17 1e-16 1e-15 1e-14 1e-13 1e-12 1e-11 1e+10 1e+15 1e+20 1e+25 νf ν (w m -2 ) ν (hz) radio opt. rosat egret 3eg j1300-4406 fermi sync scc ic (tot) c.) 3eg j1300-4406 1e-18 1e-17 1e-16 1e-15 1e-14 1e-13 1e-12 1e-11 1e+10 1e+15 1e+20 1e+25 νf ν (w m -2 ) ν (hz) radio opt. nir egret 3eg j1659-6251 fermi iras ec (ir) sync ssc ec (bel) b.) 3eg j1659-625 1e-18 1e-17 1e-16 1e-15 1e-14 1e-13 1e-12 1e-11 1e+10 1e+15 1e+20 1e+25 νf ν (w m -2 ) ν (hz) radio opt. egret 3eg j1709-0828 fermi ec (ir) ssc sync ec (bel) ic (tot) d.) 3eg j1709-0828 1e-18 1e-17 1e-16 1e-15 1e-14 1e-13 1e-12 1e-11 1e+10 1e+15 1e+20 1e+25 νf ν (w m -2 ) ν (hz) radio opt. nir egret 3eg j1813-6419 fermi ec (ir) ssc sync ic (tot) ec (bel) e.) 3eg j1813-6419 figure 8: the modeled seds for the various egret/fermi-lat sources. from these results (see fig. 8) it can be seen that the egret and fermi-lat data are consistent with an ec model, i.e. the ic upscattering of ir photons from the disc and uv/optical photons from the line emitting clouds (broad line regions) to the egret and fermi-lat energy domain. in all the models the electron lorentz factors were γe ∼ few × 103, rather modest in comparison with the lorentz factors required to explain the γ-ray emission from, for example, cen a. 7 conclusions we report the discovery of 13 flat spectrum extragalactic sources within the error boxes of some high galactic latitude, unidentified egret sources. five of these egret sources have been detected with fermi-lat within the first 11 months of operation. in all cases the egret and fermi-lat gamma-ray emission could be successfully explained in terms of the ic upscattering of bel photons, as well as ir photons from the disc, to egret and fermi-lat energies. the adopted electron energy is of the order of γe ∼ few × 103, which is rather moderate compared to the electron energies of γe ∼ 106 − 107, inferred from the he and tev emission from cen a. these preliminary results definitely confirm that seyfert and radio galaxies could be associated with a significant fraction of the still unidentified extragalactic egret and fermi-lat sources. acknowledgement the authors thank the organisers for the invitation to present this work at this conference. some of the observations reported in this paper were performed by the southern african large telescope (salt). the salt observations were performed under the proposal: 20121-rsa-003 (pi: b van soelen). the authors thank dr. petri vaisanen from the salt science team for his guidance with the data reduction. references [1] abdo, a.a., et al.(fermi): 2010a, apj, 710, 1271 doi:10.1088/0004-637x/710/2/1271 [2] abdo, a.a., et al. (fermi): 2010b, science, 328, 725 doi:10.1126/science.1184656 [3] abdo, a.a., et al. (fermi): 2010c, apj, 719, 1433 doi:10.1088/0004-637x/719/2/1433 [4] aharonian, f.a., et al. (h.e.s.s.): 2009, apj, 695, l40 doi:10.1088/0004-637x/695/1/l40 [5] bordas, p.: 2012 in multifrequency behaviour of high energy cosmic sources, vulcano (may 2328, 2011), memorie s.a.it, vol 83 (1), 87 (eds. f. giovanelli & l. sabau-graziati) [6] caccianiga, a., della ceca, r., gioi, i.m., maccacaro, t. & wolter, t.: 1999, apj, 513, 51 [7] chiaberge, m. et al.: 2001, mnras, 324, 33 doi:10.1046/j.1365-8711.2001.04642.x [8] fan, j-h.: 2005, chin. j. astron. astrophys. suppl., 5, 213 doi:10.1088/1009-9271/5/s1/213 [9] hartman, r., et al.: 1999, apjs, 123, 79 [10] katarzynski, k., sol, h. & kus, a.: 2001, a&a, 367, 809 [11] mattox, j., et al.: 1997, apj, 476, 692 [12] meintjes, p.j. & nkundabakura, p.: 2012, in high energy gamma-ray astronomy, proc of the 5th international high energy gamma-ray astronomy meeting, heidelberg (germany), aip conference proceedings, vol. 1505, p. 554 (eds. f.a. aharonian, w. hoffman & f. rieger), publisher, melville (new york) 168 http://dx.doi.org/10.1088/0004-637x/710/2/1271 http://dx.doi.org/10.1126/science.1184656 http://dx.doi.org/10.1088/0004-637x/719/2/1433 http://dx.doi.org/10.1088/0004-637x/695/1/l40 http://dx.doi.org/10.1046/j.1365-8711.2001.04642.x http://dx.doi.org/10.1088/1009-9271/5/s1/213 modelling the multifrequency sed of agn candidates among the unidentified egret... [13] moderski, r., et al.: 2003, a&a, 406, 855 [14] nkundabakura, p. & meintjes, p.j.: 2012, mnras,427, 859 doi:10.1111/j.1365-2966.2012.21953.x [15] nolan, p.l., et al. (fermi): 2011, apj suppl., 199, 31 doi:10.1088/0067-0049/199/2/31 [16] rieger, f. & aharonian, f.a.: 2009, a&a, 506, l41 [17] rieger, f.: 2012a, in high energy gamma-ray astronomy, proc of the 5th international high energy gamma-ray astronomy meeting, heidelberg (germany), aip conference proceedings, vol. 1505, p. 80 (eds. f.a. aharonian, w. hoffman & f. rieger), publisher, melville (new york) [18] rieger, f.: 2012b, in multifrequency behaviour of high energy cosmic sources, vulcano (may 23-28, 2011), memorie s.a.it, vol 83 (1), 127 (eds. f. giovanelli & l. sabau-graziati) [19] sikora, m., begelman, m.c. & rees, m.j.: 1994, apj, 421, 153 [20] sowards-emmerd, d., romani, r.w. & michelson, p.f.: 2003, apj, 590, 109 [21] steinle, h.: 2010, pasa, 27, 431 [22] whysong, d. & antonucci, r.: 2004, apj, 602, 116 169 http://dx.doi.org/10.1111/j.1365-2966.2012.21953.x http://dx.doi.org/10.1088/0067-0049/199/2/31 introduction gamma-ray variability optical follow-up studies the spectral energy distributions (sed) non-aligned agn: a new class of gamma-ray source sed modelling conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.11.0012 acta polytechnica ctu proceedings 11:12–15, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app friction buffer stop design petr guziur institute of railway structures and construction, faculty of civil engineering, brno university of technology correspondence: guziur.p@fce.vutbr.cz abstract. friction buffer stops are the favoured construction of buffer stop, mainly due to its high resistance and variety of layout. last but not least is its manner of deceleration induced upon impact and during the braking what makes it smart solution in railway transport safety. the general approach of designing buffer stops is via usage of the kinetic energy and its conversion into work. paper describes input parameters such as train velocity or buffer stop vicinity which is expressed by the safety coefficient implanted within the calculation. furthermore, the paper shows the principle of calculation the friction buffer stop work, or to be more precise, the work of its braking jaws and optionally the work of additional braking jaws located behind the buffer stop. last section of the paper is focused on the examples of designing friction buffer stops, points out the main complications and shows the charts of relation amongst braking distance, kinetic energy and braking force and the charts of relation between deceleration rate and braking distance. keywords: buffer stop, kinetic energy, braking force, braking jaw. 1. introduction with increasing demands on safety in transportation, every threat needs to be considered. this means to keep safe onboard passengers and anyone who can be endangered in case of an accident. this applies even for buffer stops – especially for buffer stops at the dead-end tracks in stations by platforms with pedestrians. the use of fixed buffer stops has become less suitable due to their low resistance and manner of deceleration, which arises in an order of tens of m.s−2 [1] a clearly unacceptable state. according to the czech standard cd z9 [2], it is allowed to design fixed buffer stop (table 1). using those constructions with very limited resistance is justified in particular cases such as deadend tracks in shunting yard, rolling stock depots etc. recently the motivation is to use more reliable constructions to increase the safety in railway transportation. the friction buffer stop with its high resistance and manner of deceleration is more suitable one. buffer stop type 6 cars of 15 t 1 car of 80 t rail buffer stop 1.0 km.h−1 1.6 km.h−1 concrete type "sudop" 0.7 km.h−1 1.1 km.h−1 concrete type "dsb" 1.0 km.h−1 1.6 km.h−1 table 1. resistances of buffer stops used in czech republic [2]. 2. friction buffer stop friction buffer stops have become the preferred constructions at the end of a dead-end track in railway stations abroad (e.g. switzerland, germany [3, 4]). resistance of a friction buffer stop (work of the buffer stop) could be much higher than a fixed buffer stop, and can be customized for various train mass, train speeds and acceptable deceleration rates. disadvantage of a friction buffer stop is obviously its space requirement due to its braking distance (see figure 1). kinetic energy of moving train and its reduction along the braking distance is the criteria to calculate and design the buffer stop work. to be more precise the objective is to design the number of braking jaws and their braking distances. there are two possibilities how to design the friction buffer stop: • friction buffer stop without additional braking jaws (see figure 1); • friction buffer stop with additional braking jaws (see figure 2). figure 1. friction buffer stop [5]. lv – track length required for friction buffer stop lw – braking distance lb – buffer stop length 12 http://dx.doi.org/10.14311/app.2017.11.0012 http://ojs.cvut.cz/ojs/index.php/app vol. 11/2017 friction buffer stop design 3. buffer stop design 3.1. train kinetic energy defining the precise value of kinetic energy of moving rolling stock is to include rotating parts into calculation. to simplify the calculation of train kinetic energy one can use formula 1 for calculation the kinetic energy of non-rotating object of certain mass and velocity. ekin = 1 2mv2 (1) ekin – train kinetic energy [j] m – train mass [kg] v – train velocity by impact [m.s−1] 3.2. collision speed collision speed is probably the most questionable parameter entering the calculation. in tracks with train control system, which can interfere with driver inappropriate driving (e.g. etcs) – in this case an insufficient braking at the end of dead end track, it is possible to define the collision speed. nevertheless, there are numerous dead-end tracks without any speed controlling system and therefore the driver is responsible for proper braking. collision speeds that could be found in literature are v = 10 km.h−1 or v = 15 km.h−1 (depends on train type or track type) [4–6]. 3.3. safety coefficient for including an inaccuracy entering the calculation of kinetic energy and to ensure the reliability of the design, safety coefficient k has to be counted in calculation. the value of the coefficient varies and depends on type of train, location of dead end track etc. various infrastructure managers approach towards the assessment of the safety coefficient differently. values of safety coefficient usually varies between 1,0 – 2,0 [3, 4, 6]. type of train k [-] freight trains and shunting 1.2 passenger trains, freight trains and shunting, when it is necessary to protect various systems which are located behind or nearby buffer stop 1.5 all trains, where there are traffic zones, structures or residential buildings located behind or nearby buffer stop 1.8 preventing the fall of any train or rolling stock into an abyss 2.0 table 2. safety coefficient [6]. 3.4. buffer stop work in general, the resistance of buffer stop is described as its energy absorbing capacity, therefore the buffer stop work required to stop the train. in case of friction buffer stop, it is the work of braking jaws w with braking forces fb,i,j on braking distances li,j . work of the braking jaws can be obtained using formula 2 and 3. wi = ni ∗ n∑ j=1 fb,i,j ∗ li,j (2) w = s∑ i=1 wi (3) wi – work of i-group of braking jaws [j] ni – number of braking jaws in i-group [-] fb,i,j – braking force of a single braking jaw, based on a braking distance [n] li,j – length of braking distance of i-group of braking jaws, based on lw [m] braking force of each braking jaw decreases along the braking distance [4]. length of braking distance li,j [m] braking force fb,i,j [kn] 0 – 5 40 5 – 8 36 8 – 12 32 12 – 20 28 table 3. braking force of a braking jaw along the braking distance [4]. the design of friction buffer stop (number of braking jaws and their braking distances) is correct if the buffer stop work is equal or higher than the train kinetic energy increased by the safety coefficient: w ≥ ekin ∗ k (4) 3.5. deceleration rate deceleration rate could be the limiting parameter when designing number of braking jaws and their braking distances. the most challenging design comes with dead-end track where parameters of trains vary (mostly the train mass). deceleration rate has to be monitored both upon impact and along the braking distance where additional braking jaws could be designed. fortunately, restriction in deceleration rate applies only to the passenger trains. maximal deceleration rate is set as a = 2.5 m.s−2 [7]. deceleration rate is calculated as follows: amax = fmax m (5) 13 petr guziur acta polytechnica ctu proceedings figure 2. buffer stop with additional braking jaws. amax – maximal deceleration rate [m.s−1] fmax – maximal braking force along the braking distance [n] m – train mass [kg] 3.6. design procedure the design of buffer stop is customized for two types of trains, the lightest one and the heaviest one running on the dead-end track. this approach covers both deceleration rate restriction (usually the limiting factor for light trains) and the highest value of kinetic energy of heavy train (sufficient work of the buffer stop). braking distance for braking jaws on buffer stop is considered as the main braking distance. the tricky part comes with additional jaws behind the buffer stop thus in their braking distances where each pair of additional braking jaws has different braking distance. therefore it is necessary to consider the variable braking force for each pair of additional braking jaws along the braking distance according to table 3. for better understanding, see following examples. 3.6.1. example 1 as it was described in section 3.6, two types of trains were selected for calculation. a light train with mass of 170 t and a heavy train with mass of 300 t. collision speed of trains v = 15 km.h−1, is the same for both of them, and safety coefficient used to increase the kinetic energy k = 1, 8 (see section 3.3). in this situation, the main braking distance is set to 11,3 m (lw – buffer stop) with five pairs of braking jaws and one pair of additional braking jaws with braking distance of 4,0 m (lw – 1. row of additional braking jaws). under those circumstances, the mass of the light train is high enough to design the large number of braking jaws on buffer stop and the limit of deceleration rate is not exceeded. nevertheless, the offset for the first row of additional braking jaws behind the buffer stop must be set. if the light train reaches the additional braking jaws, braking force will increase and therefore the deceleration rate will increase over the limit. for better understanding, see figure 3 and figure 4. figure 3. kinetic energy and braking force along the braking distance (example 1). figure 4. deceleration rate along the braking distance (example 1). 3.6.2. example 2 in this example, the light train with mass of 80 t and the heavy one with mass of 300 t were selected to point the difficulty and variety of design. collision speed of trains v = 15 km.h−1 is the same for both of them and the safety coefficient used to increase the kinetic energy k = 1, 8 was chosen (see section 3.3). in this case, the main braking distance is set to 15,5 m (lw – buffer stop) with just 2 pairs of braking jaws and three rows of additional braking jaws. each row of additional braking jaws consists of 2 pairs of braking jaws. braking distances are designed as follows: 7,0 m (lw – 1. row of additional braking jaws), 5,5 m (lw – 2. row of additional braking jaws) and 4,0 m (lw – 3. row of additional braking jaws). the mass of light train is significantly lower and one has to design fewer braking jaws on buffer stop in order not to exceed the limit of deceleration rate. the offset of first row of additional braking jaws has to be set similarly to example one. 14 vol. 11/2017 friction buffer stop design figure 5. kinetic energy and braking force along the braking distance (example 2). figure 6. deceleration rate along the braking distance (example 2). 4. conclusion the usage of the fixed buffer stops in the railway stations is slowly becoming an anachronism. one can still come across many of those constructions in present railway stations but the latest progression, is to design buffer stops with high resistance and high level of safety. friction buffer stops meet those criteria in every point. the possibilities variety of designing the friction buffer stop is the huge advantage. the range of options varies form light trains with low collision speed, up to heavy trains with high collision speed. the paper discusses the parameters of the buffer stop and shows some examples of design for certain situations. as described above, design buffer stop for some combinations of trains on dead-end track could be challenging while all criteria, such as buffer stop kinetic energy absorbing capacity, restriction of deceleration rate and space options, must be met. acknowledgements the paper was created with support of the project no. lo1408 "admas up – advanced materials, structures and technologies" supported by the ministry of education, youth and sports within the targeted support of program "national program for sustainability i" and student’s grant tender of the faculty of civil engineering, brno university of technology (fast-j-16-3776). references [1] m. bugarín, j.-m. díaz-de-villageas. conception of buffer stop blocks [online]. 2001. [cit. 2016-11-10] "http://www.railway-research.org/img/pdf/329.pdf". [2] c. z9. železniční spodek, vzorový list železničního spodku, zarážedla. české dráhy, s.o., divize dopravní cesty, o.z., praha, 2001. in effect from 1.4.2002. [3] ausführungsbestimmungen zur eisenbahnverordnung / ab-ebv, 2014. artikel: gleisabschluss, bern. [4] db:ds 800 01. bahnanlagen entwerfen – allgemeine entwurfsrichtlinien. [5] i. r. ltd. railway buffer stops planning guidlines [online]. 2009. [cit. 2016-11-05] "http://www.iroads.co.il/sites/default/files/imce/ ir_buffer_stops_guidelines.doc". [6] rve 05.05.31 oberbau, oberbaukonstruktionen, gleisabschlüsse. wien. 2014. [7] guide for the application of tsi loc&pas. version 2.0, 2015. european railway agency, france. 15 acta polytechnica ctu proceedings 11:12–15, 2017 1 introduction 2 friction buffer stop 3 buffer stop design 3.1 train kinetic energy 3.2 collision speed 3.3 safety coefficient 3.4 buffer stop work 3.5 deceleration rate 3.6 design procedure 3.6.1 example 1 3.6.2 example 2 4 conclusion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0076 acta polytechnica ctu proceedings 7:76–78, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app evaluation of the fatigue response of polyester yarns after the application of abrupt tension loads emilio luiz vieira louzadaa,∗, carlos eduardo marcos guilhermea,b, felipe tempel stumpfa,b a programa de pos graduacao em engenharia mecanica, av. italia, km. 8, rio grande, brazil b policab, av. italia, km. 8, rio grande, brazil ∗ corresponding author: emilioluizlouzada@gmail.com abstract. the discovery of oil fields in deeper waters through out the last decades has led the oil industry to the necessity of replacing the mooring systems of offshore platforms from steel to synthetic cables. consequently, both the industry and the academy started to join forces in order to better understand the mechanical behavior of such materials when subjected to different service conditions. this work aims to assess the change in the fatigue life of polyester (pet) yarns if the material is submitted to an abrupt tension load prior to the application of the fatigue cycling. it was found that the fatigue life of the yarns tested are substantially reduced if the specimen is subjected to this kind of abrupt load in comparison to virgin samples. keywords: mooring lines, synthetic cables, offshore platforms. 1. introduction in the course of the last decades, offshore oil fields had been discovered along the brazilian shore in increasingly deeper waters throughout the years, which forced the oil industry to look for mooring systems to substitute the traditional systems based on steel cables. with the increase of the water depth in which the platform will operate, these systems tend to become potentially heavy, to the point where the mooring system weight itself could overcome the platform floating forces, leading to the sinking of the structure [1, 2]. in order to overcome this situation, the oil industry started to look for lighter mooring systems, which meant lighter materials, and the obvious choice was to invest in the development of mooring cables based on polymeric materials. however, there was a lack of understanding regarding these materials’ mechanical response when submitted to the service conditions of an offshore platform, which basically forced the engineers and academics to develop new research in the field [1–3]. in the present days, polyester (pet) is found to be a widely used material in applications such as anchoring cables. its good performance when submitted to cyclic loadings and the fact that its fatigue life is not affected by its submersion in salt water was the main reason it was the first material to be considered by the industry to such application [4]. however, if the maximum tension force is considerably high, the fatigue life of pet is dramastically reduced [5]. it was found that when operating between cyclic tension loads of 10% and 70% of the material’s tension resistance, samples failed after approximately 100,000 cycles [6]. if the maximum load is reduced to 60% of the material’s yarn break load (ybl), fatigue life increases to 1,000,000 cycles [5]. cyclic tension loads, however the main loads to which the cables are submitted during service, are not the only ones. during the installation of the anchoring cables, the launch of the torpedo anchor might eventually be submitted to a sudden stop, caused either by a failure of the launching system or even due to a stop because of heavy weather conditions, which would lead to abrupt axial tension loads in the synthetic cable being launched/installed. it is expected that this kind of sudden (high) tensile load affects the future mechanical behavior of the polymeric material, specially its fatigue life. this paper aims to correlate the change in the behavior of pet under cyclic loadings before and after it was submitted to abrupt axial loads. such study will be based on the material’s diagram relating number of cycles up to failure (log n) and the minimum tension load throughout the cyclic loading. 2. materials and methods the material used was polyester (pet). yarn samples were of 500 mm length with sandwich-type terminals (figure 1) [7]. prior to the application of the impact load, and throughout all the tests, the samples were left 24 hours at controlled temperature of 20±2°c and relative humidity of 65±4%. tension tests were carried out in an emic dl-2000 electromechanic universal testing machine in order to obtain the material’s ybl of virgin samples. using a 500mm/min displacement ramp, and ten specimen, it was found that this pet has an ybl of 165,44n. 76 http://dx.doi.org/10.14311/app.2017.7.0076 http://ojs.cvut.cz/ojs/index.php/app vol. 7/2017 evaluation of the fatigue response of polyester yarns after the application of abrupt tension loads figure 1. sandwich-type terminals. figure 2. impact testing device. a set of virgin samples were taken to the impact testing device (figure 2) and submitted to an axial impact load corresponding to 10% of the material’s ybl. this load is achieved releasing a 1.7 kg dead weight from a 300mm height, which transfers to the sample a potential energy of 5 j. the maximum elongation of the samples were measured using a marker attached to the bottom end of the yarns running along a ruler. after the impact test, each specimen is taken to an instron 8801 servohydraulic unversal testing machine to be submitted to force-controlled cyclic tension loads. a total of eight ranges of tension loads were used during the cyclic tests: 10-90%ybl, 2090%ybl, 30-90%ybl, 40-90%ybl, 50-90%ybl, 6090%ybl, 70-90%ybl, 80-90%ybl. the frequency used was 0.1hz. the same fatigue procedure was applied to virgin samples, in order to compare their behavior with those damaged by the impact. each load range was applied to ten different samples (both virgin and damaged by the impact test), which means that a total of 160 yarn samples were used throughout the fatigue assessment. figure 3. cycles up to failure versus load ranges: superposed results. 3. results 3.1. effect of impact load on the fatigue life of pet figure 3 shows the number of cycles up to failure versus the minimum load of each load range in the case of virgin samples and damaged samples. regardless of the minimum load applied, the virgin samples have a longer fatigue life compared to the ones that were previously submitted to the abrupt tension load. table 1 sumarises the number of cycles up to failure for both cases for each load range. 3.2. effect of impact load on the yarn elongation together with the tests to determine the material’s ybl, data regarding the samples elongation in rupture were collected. that was made in order to compare the elongation in rupture of the samples submitted to the quasi-static tests performed on the universal testing machine with those obtained when the yarns fail due to impact only. it was found that a potential energy of 6.5 j, which corresponds to a tension load of 13% of the material’s ybl, is required to take the yarns to fail by impact only. a set of ten samples were submitted to this condition and a scale was used to get the yarn’s elongation in rupture. results comparing the elongation of the yarns during quasi-static test and dynamic test are shown in table 2. it was found that the samples tend to elongate considerably less in rupture when the load applied is abrupt (51.6mm versus 57.5mm of the quasi-static tests). 4. conclusions the present paper showed a preliminary assessment of the change in the fatigue life of polyester yarns when they are submitted to an abrupt axial load in comparison to the virgin material, and it was found that a sudden load of approximately 10% of the yarn break load is enought to lead the material to a considerable drop on its fatigue resistance. in terms of the yarn’s elongation in rupture, it was also found that quasi-static tests lead to a larger elongation, and it 77 e. l. v. louzada, c. e. m. guilherme, f. t. stumpf acta polytechnica ctu proceedings minimum load [% ybl] 10 20 30 40 50 60 70 80 virgin samples 50 73 108 127 127 141 153 75 after impact 30 34 41 48 57 71 68 44 table 1. number of cycles up to fatigue rupture. elongation in rupture quasi-static test 57.52mm impact test 51.6mm table 2. elongation in rupture for quasi-static and dynamic tests. can be explained basically by the viscoelastic behavior of the material, because during the impact load the material has no time to dissipate the potential energy in terms of heat energy, for example. it is also interesting to notice that a sudden load of only 13% of the material’s yarn break load is sufficient to lead to its rupture by impact, which is considerably low and could be used to warn the industry to take that into consideration when operating with mooring ropes made of polyester. references [1] c. j. m. del vecchio. light weight materials for deep water moorings. phd thesis 1992. [2] m. m. salama. lightweight materials for mooring lines of deepwater tension leg platforms. marine technology 21(3):234–241, 1984. [3] f. e. g. chimisso. the past, the present and the future of policab: the challenge of synthetic mooring ropes anchorages at pre-salt petroleum basin, in brazil. proceedings of the 10th youth symposium on experimental solid mechanics 2011. [4] r. r. rossi. cabos de poliester para ancoragem de plataformas de petroleo em aguas ultraprofundas, in portuguese. msc thesis 2002. [5] f. v. de carmago, c. e. m. guilherme, c. fragassa, a. pavlovic. cyclic stress analysis of polyester, aramid, polyethilene and liquid crystal polymer yarns. acta polytechnica 56(5):402–408, 2016. doi:10.14311/ap.2016.56.0402. [6] r. l. bosman. on the origin of heat build-up in polyester ropes. oceans96 mts/ieee prospects for the 21st century conference proceedings 1996. [7] d. pfarrius, e. duarte, f. e. g. chimisso. theoretical and experimental modeling of a socket sandwich for use in tension tests of synthetic ropes. proceedings of the vith youth symposium on experimental solid mechanics 2007. 78 http://dx.doi.org/10.14311/ap.2016.56.0402 acta polytechnica ctu proceedings 7:76–78, 2017 1 introduction 2 materials and methods 3 results 3.1 effect of impact load on the fatigue life of pet 3.2 effect of impact load on the yarn elongation 4 conclusions references acta polytechnica ctu proceedings doi:10.14311/app.2016.5.0004 acta polytechnica ctu proceedings 5:4–11, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app on efficient operational concept of future high-speed railway in the czech republic michal drábek department of logistics and management of transport, faculty of transportation sciences, ctu in prague, czech republic correspondence: xdrabek@fd.cvut.cz abstract. the aim of this paper is to elaborate a layout of the first operational concept of rapid services with 1 hour system travel time between praha and brno. two basic methods are used – integrated periodic timetable (periodic rendezvous of all services in ipt-nodes) and operational concept economy approach, as defined below by the author. in this paper, three recent high-speed railway concepts for the future so-called rapid services network of the czech republic are followed-up. the first one is an operational traffic planning study by kalčík, janoš et al. on behalf of czech ministry of transport from 2010. the second one is the high-speed railway promoting book high speed rail even in the czech republic by šlegr et al. from 2012, with likely the most detailed concept of rapid services network. the third one is a paper on progress of the official spatial-technical studies for some future czech high-speed lines by šulc from 2014. the importance of achievement of 1 hour travel time between the largest agglomerations is briefly presented. the presented methodological approach, although soft and manager-oriented, comprises some firm principles: segmentation of high-speed train offer, so that more expensive rolling stock is not wasted by operation on long conventional line sections, consideration of system travel times for efficient rolling stock circuit, restriction of need for links from high-speed to conventional lines, and utilization of high-speed lines as a "rail highway". this approach is intended to be particularized iteratively, with every application. so, in this paper, first version of operational concept economy approach is introduced. the key idea is that passengers should be offered such travel times and service intervals (headways) and such number of direct services, which are adequate to their potential demand, but as much synergistic effect as possible should be strived to be achieved for every proposed construction (new or modernized one). such approach goes towards economic efficiency, which is crucial indicator for political decision necessary for building, let alone eu co-funding of the construction. experience shows that in many czech feasibility studies, achievement of sufficient economic efficiency was the most complicated part of the study. results show that an efficient operational concept can be designed not at the expense of runtimes between the largest cities. keywords: high-speed railway, high-speed line, rapid services, integrated periodic timetable . 1. introduction the aim of this paper is to elaborate a layout of the first operational concept of rapid services with 1 hour system travel time between praha and brno. two basic principles are used – integrated periodic timetable, and operational concept economy approach, as defined below by the author. directive 2008/57/ec of the european parliament and of the council of 17 june 2008 on the interoperability of the rail system within the community [1] defines in annex ii infrastructure and rolling stock as structural subsystems of the rail system, and traffic operation and management as a functional subsystem of the rail system. in traffic operation and management subsystem, traffic planning is also included. this paper is organized as follows. after list of abbreviations and list of largest czech cities, recent concepts of high-speed lines network for rapid services, in the context of recent ten-t regulation [2] are introduced. then, significance of 1 hour travel time is summarized, based mostly on revealedpreference data. introduction of used methods follows: integrated periodic timetable and newly developed soft operational concept economy approach. further, scheme of the resulting operational concept is presented, commented and discussed. the paper is closed by conclusion, including recommendation for further studies in this field. for the sake of brevity and clarity, following abbreviations will be used in this paper: • emu – electric multiple unit • hs – high-speed (railway) • hsl – high-speed line • ipt – integrated periodic timetable • put line – public transport line (not to be mistaken with railway line as a built structure) – a group of services which operate all day in regular period, and serve particular sequence of stations and stops • rs – rapid services (czech system of hsls and follow-up uprgraded or new lines, in czech: rychlá spojení) 4 http://dx.doi.org/10.14311/app.2016.5.0004 http://ojs.cvut.cz/ojs/index.php/app vol. 5/2016 on efficient operational concept • sždc – railway infrastructure administration, state organization – czech state railway infrastructure manager ( in czech: správa železniční dopravní cesty ) • ten-t – trans-european transport networks • tsi – technical specification of interoperability • uic – international union of railways 2. list of largest czech cities table 1 displays list of all czech cities over 40,000 inhabitants. these cities can be divided into four subgroups based on their population, as of 1st january 2015. regional capitals are emphasized. note that population of ostrava agglomeration is comparable with praha. these cities build up five largest agglomerations: praha, ostrava region, brno, northwestern bohemia (from děčín to chomutov) and central moravia. 3. ten-t context and recent concepts of hsls for rapid services most of the intended czech hsls are part of ten-t network, but only three of them are involved into the core ten-t network: hsls praha – ústí nad labem and brno – břeclav, and modernization of the line brno – přerov. for the hsl brno – břeclav, there are several alternative directions southward of vranovice. for the hsl praha – wroclaw (in comprehensive network), there are two alternative directions: via liberec or via hradec králové. the author has followed up from three main sources. each one has been carried out for different purpose. the study carried out by kalčík, janoš et al. (including the author) [4] contains, to the author’s knowledge, the only model timetable for the whole rs network up to now. approximate routes for hsls were defined, and, based on their parameters and on available hs rolling stock parameters, model timetables were constructed using timetabling software fbs. one of the results is a netgraph (scheme of put lines with arrival and departure minutes in node stations). šlegr et al. [5] have written and published the book high speed rail even in the czech republic with many hsl drawings in the map. the book introduces european and world best practice in hs railway and, in a detailed manner, presents potential benefits of the rs system for every czech region. as a result, the most detailed concept of rs network (although not officially approved), with qualified estimation of section runtimes, is introduced there. šulc [6] has presented recent progress in five spatial-technical studies of hsls, carried out on behalf on sždc. the aim of these studies is to find suitable hsl routes, so that necessary space for their future construction can be legally protected. for this purpose, simplified timetable layout and cost estimation were carried out. other hsls were already subject of more detailed feasibility studies: praha – liberec and brno – přerov. the latter study recommended the doubling and modernization of present single-track line up to 200 km/h as the best one, although the assessed line is located directly in the corridor brno – ostrava. uic [7] records that hsls for the maximum speed of 350 km/h are in operation in china (1,028 km), and they are planned in portugal (206 km). in the united kingdom, hsls for the maximum speed of 360 km/h (543 km) are planned. thus, such maximum speed is nothing uncommon for the recently built and planned hsls. figure 1 shows the maximalist future czech hsl network as a backbone of rapid services. it does not include possible local new lines or line modernizations. the scheme was created as follows. for each hsl, always the higher maximum speed from šlegr et al. [5] and šulc [6] was chosen. inclusion of each hsl (or its section) into ten-t core, or comprehensive network based on [2] was marked. the actual phase of project preparation (based on šulc [6] and to the author’s knowledge) was also marked. from the possible links to conventional railway network, only the most significant ones were displayed. the stations or stops, which are intended to be built directly on hsls were adopted from šulc [6]. international hsls are strongly dependent on the will of both neighbouring states: the hsl from ústí nad labem to dresden is supported by czech ministry of transport, as well as the government of saxony (although it requires a long tunnel under the mountains), but the hsl from plzeň to bavaria is not quite a priority for the government of bavaria, despite its indisputable european significance. 4. one hour as a breakthrough in travel time the practice has proven that, when the public transport travel time changes to 1 hour or less, and if this travel time is competitive to car, public transport ridership considerably increases, and some people can even commute daily. if the present travel time by cars between two largest czech cities is approximately 2 hours, only 1 hour is fully competitive, because the travel time to and from the station must be added. in switzerland, new line for 200 km/h was built to achieve travel time of 56 min between zurich and berne (swiss largest city and capital). this line was not an isolated project, but a part of targeted investments for implementing bahn 2000 concept. its main aim was to achieve necessary system travel times for the ipt. this new line, as a kind of swiss ”rail highway”, serves also for many other long-distance put lines. the modal-split of railway for the journeys zurich – berne has achieved 88%, for the journeys zurich – st. gallen (1:02 h travel time) it was 73% (voev utp, 2010 [8]). janoš and baudyš [9] state that improvements in 5 michal drábek acta polytechnica ctu proceedings city population city population praha 1,259,079 zlín 75,112 brno 377,440 havířov 75,049 ostrava 294,200 kladno 68,552 most 67,089 opava 57,772 frýdek místek 56,945 karviná 55,985 city population city population plzeň 169,033 jihlava 50,521 liberec 102,562 teplice 50,079 olomouc 99,809 děčín 49,833 ústí nad labem 93,409 karlovy vary 49,781 české budějovice 93,285 chomutov 48,913 hradec králové 92,808 jablonec nad nisou 45,594 pardubice 89,693 mladá boleslav 44,318 přerov 44,278 prostějov 44,094 table 1. list of largest czech cities. data from czech statistical office [3]. figure 1. maximalist czech hsl network 6 vol. 5/2016 on efficient operational concept timetable offer (more frequent and more periodic service) in long-distance railway in the czech republic have led to increase of number of passengers. ”between 2003 and 2005, incomes increased by 7.86%, and number of passengers by 3.63%. however, in some relations, thanks to new supply, the increase of passengers was 40 to 50%. ipt is being further developed. thanks optimal train connections in junctions and synergic effect of linked supply number of passengers raises by 2-10% per year even on lines with no supply change.” the raise of service for timetable 2004/05 was 7%, compared to timetable 2003/04, when new offer (supply) concept was introduced. vichta [10] has also shown figures that justified timetable offer improvement for large enough cities (ústí nad labem and teplice). since 2003/04 timetable, two segments of periodic service between ústí and praha were introduced: a non-stop fast train with travel time slightly above 1 hour and a 120 min interval, and fast train with several stops hourly. since 2008, a non-stop segment has been operated hourly, and every second service connected teplice directly with praha. compared with train ridership from 2002 (100%), the train ridership between ústí and praha grew to 152% in 2006, and to 325% in 2008. compared to the same year, the train ridership between teplice and praha grew to 228% in 2006 and to 369% in 2008. in both cases, only relative changes can be published, to avoid publishing of czech railways’ business sensitive data. kordis jmk, an integrated transport system coordinator of south moravia region, has carried out a stated-preference study of potential ridership of hsl between praha and brno [11]. the study has proved that about 30,000 passengers daily would use the new hsl, majority of them instead of cars. the potential ridership varied depending on train travel time and ticket price. the results for 45 min travel time were only slightly better than the ones for 60 min. the acceptable ticket price was up to 299 czk. for 300 czk and more, the potential ridership fell to approximately 18,000 passengers. a travel time between praha and brno up to 60 min is also supported officially, at least by some departments of czech ministry of transport and sždc – see šulc, page 14 [6] and kušnír and ilík, page 13 [12]. the graph in the latter presentation shows clear intention to ensure better connection not only for the largest agglomerations, but also for the regions, so that their development can be stimulated. however, a more detailed study on potential rs ridership, which should include a transport demand forecasting model and more detailed economic calculations, has to be carried out. sždc has called a bid for so called ”rapid services – study of opportunities”, that had to be cancelled, because only one eligible applicant remained. recently, a new bid for the study is being in progress. 5. methods 5.1. principle of ipt ipt is a special case of periodic timetable, which ensures connections between various put lines in the whole network. for this effect, the following requirements must be fulfilled. all services operate in put lines, in unified interval which is equal to 2k-multiple of basic period (60 min as a rule), where k is an integer. in every put line, services from opposite directions meet each other at the same time (symmetry time). this time repeats after half an interval. should services of two put lines enable mutual connections with an equal changing time for each direction, these two put lines must have equal symmetry time. in european long-distance railways, symmetry time slightly before the minute 00 is common. this is called zero symmetry axis. in practice, symmetry times in the minute 57 to 01 are used, which, in the case of hourly interval, implies another symmetry time in the minute 30. for the 30 min interval, additional symmetry times in the minutes 15 and 45 occur. an ipt-node is a railway station where connections with services from other put lines can be ensured, because the symmetry time is reached there. to achieve connections in every ipt-node, system travel time between them must be ensured. it is an integer multiple of half period. it consists of sum of regular runtimes between two iptnodes, sum of dwell times and waiting times between them, and of proportional part of dwell, changing or waiting times in mentioned ipt-nodes (it depends which time is limiting in each particular case) [13]. it is obvious that two put lines with equal runtimes, which operate on long enough common line section and do not need to be connected for the passenger transfer, can be interposed into a half interval. this interposition is used for more attractive timetable offer. on the other hand, if the transfer is desirable, the trains of two put lines run as close as possible after each other (so that they reach the same ipt-node, e.g., in berne). 5.2. operational concept economy approach the presented methodological approach, although soft and manager-oriented, comprises some firm principles, which will be explained as follows. this approach is intended to be particularized iteratively, with every application. so, in this paper, first version of operational concept economy approach is introduced. the key idea is that passengers should be offered such travel times and service intervals (headways) and such number of direct services, which are adequate to their potential demand, but as much synergistic effect as possible should be strived to be achieved for every proposed construction (new or modernized one). such approach goes towards economic efficiency, which is a crucial indicator for political decision necessary for building, let alone eu co-funding of the construction. 7 michal drábek acta polytechnica ctu proceedings experience shows that in many czech feasibility studies, achievement of sufficient economic efficiency was the most complicated part of the study. travel times should correspond to system travel times according to ipt rules. of course, system travel time is always considerably larger than a corresponding runtime, because of times for changing between services in the ipt nodes, and necessary time supplement for the sake of timetable stability. because of high-speed railway dynamics, such supplement should be larger here than by the conventional railway. runtime calculations are not subject of this paper, but it is obvious, that for approx. 200 km distant cities praha and brno and for system travel time 60 min between them, maximum speed of 200 km/h is totally insufficient. so, higher speed, e.g. 350 km/h, is considered. moreover, in city centres, only lower speed is possible due to densely built-up areas and probably one more stop in praha before the centre (zahradní město) [6]. if a new hsl is justified by the potential demand, it should be at the same time used by as many trains as possible, to make faster as many connections as possible. thus, at least central parts of the hs network should serve as ”rail highways” for fast enough long-distance, or even fast regional, put lines. this idea leads to requirements for junctions to connect a hsl with conventional rail network. a recent concept of rs of czech ministry of transport [12] corresponds to such idea, because of ensuring fast railway service also for czech regions. but, because of economy, there should be less junctions with as much put lines using one junction as reasonable. as a rule of thumb, every junction from hs line should be used by minimum 1 pair of trains hourly. the design of put lines themselves should also be in compliance with economy. for high-speed railway, a hierarchy in the form of following segments of offer can be defined: • fastest put lines (hs-a) for the speed up to 350 km/h, with dedicated emus. in figure 2, such put lines are marked in red colour. • long-distance put lines (hs-b1) which operate on long sections of fast high-speed lines, so the rolling stock should be able to run 230 to 250 km/h to avoid frequent overtaking by trains of higher segment. rolling stock can vary from emu to classical trainset, or push-pull units hauled by a locomotive (e.g. railjet). in figure 2, such put lines are marked in violet colour, and in pink colour, in the case of tilting trains. • long-distance put lines (hs-b2) which operate on short sections of fast high-speed lines, or they are overtaken by hs-a trains. thus, for the rolling stock the maximum speed of 200 km/h is sufficient. rolling stock can vary from emu to classical trainset. in figure 2, such put lines are marked in blue colour. • fast regional put lines (hs-c), which can achieve significantly lower travel time to the agglomeration centre by using of hsl section. the rolling stock should run at least 160 km/h and be interoperable with tsis required for high-speed railway (for the other segments, this is evident). for maintaining reasonable complexity, this segment is neglected in this paper. for the sake of economy, the higher segment, the less trainsets should be required. this aim can be achieved by two means: as little number of put lines as reasonable, and as little number of trainsets per put line as reasonable. but, on the other hand, appropriate service interval, and some reserve trainsets should be ensured. the basic service interval for each put line is considered 60 min. the only exception is international put line warsaw – vienna, which is of international more than national significance. the basic service interval of 30 min (of a single put line or an interposition of them) is considered for connection of all regional centres above 90 000 inhabitants with praha, brno or ostrava, if the system travel time to the particular agglomeration is 1 hour or lower. the hs-a segment should end in cities, which are large enough to justify the most expensive and maintenance sensitive rolling stock. for the hs-a segment between praha and brno, a basic interval 15 min is considered. in some studies, even an interval 10 min is discussed, but it would complicate operation of hs-b trains on the same hsl. so, the longest possible trains (400 m), and double-decker trains (such as tgv duplex) are considered as mostly desirable. the number of four basic hs-a put lines (each one with 60 min interval) should not be exceeded. thus, every hs-a train is economically justified because of service between praha and brno. because of ”biggest possible” trains, a 30 min period of hs-a segment between praha and ostrava is likely to be sufficient. it is obvious that vast majority of the demand would be national, mostly between large cities. so, for the sake of economy, a standard hs-a trainset consisting of two half-trains (such as ice 3, but double-decker) is further proposed. this measure would enable eventual disconnection of one trainset in the station, where many passengers leave and only little number of passengers board. such disconnection enables also direct service to two various destinations. as a rule of thumb for the czech republic, middle-sized cities with 30,000 or more inhabitants can be considered as appropriate ends of hs-a put lines. it is, however, important that a runtime from regional centre to such city must not exceed approximately 25 minutes. thus, service for such middle-sized city in 60 min interval would cost only 1 trainset extra (a half-train only). for the hs-b segment, the choice of rolling stock depends on timetable of hsl section used (required maximum speed), and on justification of tilting technology (a long enough conventional line with many curves, and potential time savings related to the population served). the put lines should be composed with respect to equal rolling stock requirements on both sides of a metropolis (for 8 vol. 5/2016 on efficient operational concept the czech republic, this means in practice praha and brno). for the hs-c segment, runtime savings should justify extra costs for ”high-speed-compatible” technical equipment of the rolling stock. thus, such trains should use high-speed line sections both before and after stop in the agglomeration centre. for the feasibility of the proposed operational concept, electrification and upgrading of several mainlines is supposed. further, a new line from třebíč to moravské budějovice is required, to enable direct connection of jihlava, třebíč and znojmo. for the sake of reasonable scope, timetables are not constructed. it is supposed, that in every ipt-node, slower trains leave after faster trains, if they run on the same line. thanks to the symmetry of ipt, arrival sequence is symmetric (slower trains arrive before faster ones). the system travel times are estimated on the basis of kalčík, janoš et al. [4], and lengthened due to additional stops if needed (by qualified estimation). 6. results and discussion the scheme of put lines, ipt-nodes and system travel times between large cities is displayed in figure 2. an interposition into half interval (30 min) is marked by two parallel lines close together. for the hs-a segment, the interpositions into 30 min and 15 min intervals have resulted in the fact that either plzeň or ústí nad labem, but not both cities, can be connected directly with ostrava. considering importance of direct connection of berlin and vienna via praha for the czech republic, ostrava should be connected directly with plzeň rather than ústí. thus, two bundles of hs-a put lines emerged: • berlin – dresden – praha – brno – břeclav – vienna/bratislava – budapest and litvínov/děčín – ústí nad labem – praha – brno – zlín • munich (or nuremberg) – plzeň/plzeň – praha – brno – ostrava – petrovice u karviné – warsaw/opava and plzeň – praha – brno – ostrava – havířov – žilina the sign ”/” stands for coupling and decoupling of half-trains. for international directions, full trains were only considered for berlin (because of national demand between dresden and berlin) and žilina, because of traditional ”czechoslovak” passenger demand (e.g. students, workers or tourists). from plzeň, only a half-train proceeds to bavaria. in břeclav, decoupling enables direct service from praha both to vienna, and bratislava (and budapest). the put line, which ends in ústí nad labem, can proceed both to děčín and teplice, thanks to decoupling. if the line to litvínov would be upgraded, a half-train can end there. so, service of both branches would cost only 1 half-train extra per branch. from ostrava, only a half-train would proceed to warsaw. thus, the second half-train can proceed to opava, and even with present runtime it would cost only 1 half-train extra. hs-b1 segment is proposed mostly in moravia for the connection of central moravia between brno and ostrava. the reason for faster trains is the absence of stops directly on the hsl brno – ostrava. the absence of clear centre resulted in necessity of more put lines. olomouc is connected with brno by a non-stop service every 30 min. every second train proceeds north-westward to connect mohelnice, zábřeh and šumperk directly with brno. due to longer runtime, two extra trains are required. olomouc is also connected with ostrava every 30 min. one put line proceeds as an express segment to pardubice and hradec králové, the second one as a slower inter-regional train to pardubice. from pardubice to praha, the same put line changes to a non-stop segment. between praha and olomouc, an interposition into 30 min interval is proposed. the interposing put line proceeds to vsetín. because the last put line uses hsl only between praha and pardubice, a trainset for 200 km/h could be appropriate. přerov is connected hourly both with brno and ostrava. behind přerov, both put lines proceed as a conventional fast train. hradec králové is connected with praha only hourly. the supplementary connection can be ensured by transfer in pardubice. the put line from hradec králové is proposed to be composed of two emus, because of further decoupling, so that both trutnov and náchod can be connected directly with praha. liberec is connected with praha every 30 min, with only intermediate stop in mladá boleslav. jablonec nad nisou is connected with liberec (and hence with praha) by suburban trains. the same case is kladno with praha (but there are supposed fast regional trains, running directly to praha main station). north-western bohemia is connected with praha every 30 min, with likely stop in louny (for the connection of this peripheral region) between most and praha. one of two put lines proceeds to karlovy vary and cheb, and, because of the terrain, tilting train operation can save considerable amount of runtime. both mentioned put lines proceed from praha to jihlava, but with various stopping. the tilting train as hs-b1 segment runs nonstop, and proceeds to třebíč and znojmo (possible proceeding to vienna is worth consideration), where tilting is supposed to save the runtime. another put line stops in benešov, and on the hsl in vlašim and vysočina (a stop between pelhřimov and humpolec, linked to bus and park+ride). overtaking by hs-a trains in some of these stations is very likely – that is why hs-b2 segment is sufficient. from jihlava, this put line proceeds to havlíčkův brod and žďár nad sázavou. instead of separate link from hsl to havlíčkův brod, a thorough modernization and doubling of the line jihlava – havlíčkův brod is proposed here. jihlava is connected with brno every 30 min, with intermediate stop in velké meziříčí rs, most likely with overtaking by hs-a segment at the same time. thus, hs-b2 segment seems to be sufficient. from jihlava, one put line would proceed to havlíčkův brod, and the second one to české budějovice. modernization of 9 michal drábek acta polytechnica ctu proceedings figure 2. proposed operational concept for hsl network of rs. the line jihlava – veselí nad lužnicí and a new tunnel ševětín – nemanice are supposed to be comlpeted. the last put line of hs-b2 segment is děčín – ústí nad labem – litoměřice – roudnice nad labem rs – praha – tábor – české budějovice. the corridor to české budějovice is supposed to be finished. one of the most important results is a reduction of links from hsls to conventional lines outside large nodes. for long-distance put lines (hs-b1 and hs-b2) there have remained: litoměřice, benešov u prahy (twice), jihlava (twice), olomouc (twice) and přerov (twice) – in total 9 links. it is desirable to try to design links near olomouc and přerov together as well as to design single-track links, if they would be used by only one pair of trains hourly. of course, the proposed operational concept implies plenty of alternatives. for instance, a 30 min interval praha – hradec králové, or another put line layout for the connection of jihlava. if the put line interval is 60 min, the timetable should be constructed so that additional peak trains (which leads to interposition into 30 min interval) can be added without any conflict. the probably biggest disadvantage of the rs concept used by the author is that pardubice cannot be connected with brno within 1 hour system travel time. the author is aware of alternative concepts of hsl praha – brno via pardubice. but, given that system travel time 1 hour between praha and brno is not quite easy to achieve even via jihlava, the longer hsl via pardubice would hardly enable such time, even with a non-stop train running up to 350 km/h. 7. conclusion the presented operational concept is only a brief layout, which served as a test of operational concept economy approach, and a feedback for future making this approach more accurate. the author believes than his layout would also contribute to constructive discussion on future czech rs system, and on the role of hsls in it. the author considers as an important contribution in this paper, that there were shown close economic interdependencies between operational concept, rolling stock and infrastructure, and the operational concept was designed on the basis of such interdependencies, towards economic efficiency, but not at the expense of runtimes between the largest cities. the czech rs network always will be an integral part of both european and national transport system. thus, its layout and construction will be always subject of political decisions. the presented operational concept has clearly demonstrated many possible alternative solutions. although detailed studies will calculate which alternative brings higher benefits for lower costs, the most likely alternative to be constructed will be, in the 10 vol. 5/2016 on efficient operational concept author’s opinion, a result of political compromise or trade-off. but, even by choosing any such sub-optimal alternative the decision makers should keep in mind than it should enable efficient allocation of resources. there is always a high risk not only of construction of excessive infrastructure, but also of inefficient operational concept (too many put lines for too low demand). thus, every alternative, before its detailed economic assessment, has to be designed cautiously to minimize such risk. the compromises are inevitable, but they should not generate disproportionate extra costs. acknowledgements the author would hereby like to propose a vote of thanks to mr. petr šlegr for his long-standing promotion of highspeed railway in the czech republic, which he has crowned by editing and publishing book high speed rail even in the czech republic [5]. the author would hereby like to propose a vote of thanks to dr. vít janoš, a supervisor of his doctoral thesis, for initial layout of an operational concept for rs [4], that the author was glad to follow up. the author would hereby like to propose a vote of thanks to mr. jiří kalčík, a freelance road and railway designer, for searching for efficient high-speed lines, both in official studies (e.g. [4]), and in his spare time [5]. so, he has contributed significantly to the concept mentioned above. all engineers enabled the author to follow their ideas from timetabling viewpoint – for instance, in this paper. the author would hereby also like to propose a vote of thanks to sždc as a former author’s employer, for the occasion to assess five spatial-technical studies of hsls simultaneously from timetabling viewpoint (in summer 2013). this task has made the author to create his own view on efficient operational concept for the future czech rs network. his interest in this field has endured up to now, and has resulted in writing this paper. the author hopes it will not remain his last and the most detailed work in this field. references [1] european commission. directive 2008/57/ec of the european parliament and of the council of 17 june 2008 on the interoperability of the rail system within the community [online], 2011. european union ,brussels, http://eur-lex.europa.eu/legal-content/en/txt/ pdf/?uri=celex:02008l0057-20110322&from=en. [2] european commission. regulation (eu) no 1315/2013 of the european parliament and of the council of 11 december 2013 on union guidelines for the development of the trans-european transport network and repealing decision no 661/2010/eu [online]. 2013. european union ,brussels, http://eur-lex.europa.eu/legal-content/en/all/ ?uri=uriserv:oj.l_.2013.348.01.0001.01.eng. [3] czech statistical office. populations of municipalities [online], 2015. [2016-04-30], https://www.czso.cz/ csu/czso/pocet-obyvatel-v-obcich-k-112015. [4] j. kalčík, v. janoš. operational traffic planning solution for backbone network of high-speed lines, study on behalf of czech ministry of transport. chrást u plzně: projektové středisko kalčík, czech republic, 2010. unpublished. [5] p. šlegr et al. high speed rail even in the czech republic, 2012. editors: p. šlegr, m. robeš, m. drábek, m. stach; isbn 978-80-905005-0-1. [6] j. šulc. actual progress of preparation of rapid services in sždc. in: czech raildays: building of high-speed rail system in the czech republic. separate article [online]. praha: m-presse plus s.r.o., 2014. in czech, http://www.railvolution.net/ czechraildays/2014/buletin_szdc.pdf. [7] uic. high speed lines in the world [online], 2014. paris: uic, http://old.uic.org/img/pdf/20140901_ high_speed_lines_in_the_world.pdf. [8] voev utp: fact and arguments in favour of swiss public transport. p. 46. bern: voev utp, 2010. in german. [9] v. janoš, k. baudyš. railway timetable in czech republic, in systemy transportowe teoria i praktyka, 2009. isbn 978-83-926923-1-7. [10] f. vichta. requirements for public transport system in the czech republic, keynote speech, in future of railway passenger transport in the czech republic, czech raildays [online], 2011. ostrava: railvolution, [2011-06-14], in czech, http://www.railvolution.net/ czechraildays/2011/seminare/1.3_md_vichta.pdf. [11] railhuc project. final results [online], 2014. brno: kordis jmk, isbn 978-80-260-7787-9, http: //www.railhuc.eu/download/category/126-book2. [12] j. kušnír, j. ilík. railway in 2030, keynote speech, in future of railway passenger transport in the czech republic, czech raildays [online], 2013. ostrava: czech ministry of transport, in czech., http://www.railvolution.net/czechraildays/2013/ seminare/konference-kusnir.pdf. [13] m. drábek. periodic freight train paths in network, doctoral thesis, 2014. ctu in prague, http://takt.fd.cvut.cz/cargo/drabek_thesis.pdf. 11 http://eur-lex.europa.eu/legal-content/en/txt/pdf/?uri=celex:02008l0057-20110322&from=en http://eur-lex.europa.eu/legal-content/en/txt/pdf/?uri=celex:02008l0057-20110322&from=en http://eur-lex.europa.eu/legal-content/en/all/?uri=uriserv:oj.l_.2013.348.01.0001.01.eng http://eur-lex.europa.eu/legal-content/en/all/?uri=uriserv:oj.l_.2013.348.01.0001.01.eng https://www.czso.cz/csu/czso/pocet-obyvatel-v-obcich-k-112015 https://www.czso.cz/csu/czso/pocet-obyvatel-v-obcich-k-112015 http://www.railvolution.net/czechraildays/2014/buletin_szdc.pdf http://www.railvolution.net/czechraildays/2014/buletin_szdc.pdf http://old.uic.org/img/pdf/20140901_high_speed_lines_in_the_world.pdf http://old.uic.org/img/pdf/20140901_high_speed_lines_in_the_world.pdf http://www.railvolution.net/czechraildays/2011/seminare/1.3_md_vichta.pdf http://www.railvolution.net/czechraildays/2011/seminare/1.3_md_vichta.pdf http://www.railhuc.eu/download/category/126-book2 http://www.railhuc.eu/download/category/126-book2 http://www.railvolution.net/czechraildays/2013/seminare/konference-kusnir.pdf http://www.railvolution.net/czechraildays/2013/seminare/konference-kusnir.pdf http://takt.fd.cvut.cz/cargo/drabek_thesis.pdf acta polytechnica ctu proceedings 5:4–11, 2016 1 introduction 2 list of largest czech cities 3 ten-t context and recent concepts of hsls for rapid services 4 one hour as a breakthrough in travel time 5 methods 5.1 principle of ipt 5.2 operational concept economy approach 6 results and discussion 7 conclusion acknowledgements references 170 acta polytechnica ctu proceedings 2(1): 170–173, 2015 170 doi: 10.14311/app.2015.02.0170 new insights from inside-out doppler tomography e. j. kotze1,2, s. b. potter1 1south african astronomical observatory, po box 9, observatory 7935, cape town, south africa 2astrophysics, cosmology and gravity centre (acgc), department of astronomy, university of cape town, private bag x3, rondebosch 7701, south africa corresponding author: ejk@saao.ac.za abstract we present preliminary results from our investigation into using an “inside-out” velocity space for creating a doppler tomogram. the aim is to transpose the inverted appearance of the cartesian velocity space used in normal doppler tomography. in a comparison between normal and inside-out doppler tomograms of cataclysmic variables, we show that the inside-out velocity space has the potential to produce new insights into the accretion dynamics in these systems. keywords: accretion accretion discs methods: spectroscopic binaries: close dwarf novae polars cataclysmic variables. 1 introduction cataclysmic variables (cvs) are quintessential stellar objects for the study of mass transfer, accretion flows and accretion discs. the typical interacting system consists of a secondary low-mass, red dwarf star which is filling its roche lobe and is transferring mass via the inner lagrangian point (l1) onto the primary white dwarf star (see warner 1995 for a comprehensive review). doppler tomography, as introduced by marsh & horne (1988), is aimed at rendering the information locked-up in phased-resolved spectra of a cv into a twodimensional map of the binary components in velocity space (doppler tomogram). 2 doppler tomography 2.1 spatial coordinates fig. 1 shows a model cv with an accretion disc in a cartesian spatial coordinate frame that co-rotates with the system. as described by marsh & horne (1988), this two-dimesional frame has its origin at the centre of mass of the system [marked with a plus (+)], the x-axis along the line connecting the centres of mass of the primary and secondary [marked with crosses (×)], and the y-axis parallel to the velocity vector of the secondary. the orbital motion is assumed to be counter-clockwise around the centre of mass of the system. the model cv assumes the following system parameters: inclination i = 87◦; mass of the primary m1 = 0.8; mass ratio q = m2/m1 = 0.2 and orbital period porb = 0.083333 days (120 minutes). the inner disc radius is derived using these parameters and assuming a keplerian velocity of ∼ 2.37×103 km s−1. the 3:1 resonance radius is taken to be the outer disc radius. secondary accretion stream inner edge of disc outer edge of disc roche lobe of primary a(0.02,-0.12) b(-0.62,0.0) x y figure 1: co-rotating cartesian spatial coordinate frame for a model cv. 2.2 velocity coordinates the left and middle panels of fig. 2 show, respectively, the two-dimensional cartesian and polar velocity coordinate frames which correspond to the co-rotating spatial frame shown in fig. 1, with overlays of the velocity profiles of all the main components of the model cv. the polar velocity coordinate frame is obtained by either transforming the cartesian spatial frame to a polar spatial frame which is then projected into a polar velocity frame or by transforming the cartesian velocity frame into a polar velocity frame. since we found that a polar frame allows for easier transformation of the circularly symmetric velocity profile of a doppler tomogram, this is the first step in establishing an inside-out layout. 170 http://dx.doi.org/10.14311/app.2015.02.0170 new insights from inside-out doppler tomography v(r′,θ) [10 3 km s -1 , degrees] secondary accretion stream inner edge of disc outer edge of disc roche lobe of primary a(0.86,55.2°) b(0.73,270°) 0.0 1.0 2.0 r′ θ v(r′,θ) v(r,θ) [10 3 km s -1 , degrees] secondary accretion stream inner edge of disc outer edge of disc roche lobe of primary a(0.86,55.2°) b(0.73,270°) 1.0 2.0r θ v(r,θ) -2.0 -1.0 0.0 1.0 2.0 -2.0 -1.0 0.0 1.0 2.0 v y [ 1 0 3 k m s -1 ] v x [10 3 km s -1 ] secondary accretion stream inner edge of disc outer edge of disc roche lobe of primary a(0.49,0.70) b(0.0,-0.73) figure 2: cartesian (left), polar (middle) and inside-out polar (right) velocity space. 3 inside-out doppler tomography the right panel of fig. 2 shows the same model cv presented in the left and middle panels, but with the zero velocity origin and the maximum velocities transposed, creating an inside-out polar velocity space. the most notable aspects of the inside-out frame are the inner and outer edges of the accretion disc appearing the “right” way around while the secondary and ballistic stream are outside the disc. the secondary appears upside down because it is orbiting as a solid body, i.e., the outside is moving faster than the inside. the ballistic stream also “curves” inwards as it accelerates towards the disc and primary. 4 examples the example doppler tomograms have been created in polar and inside-out polar velocity space using a modified version of the fast maximum entropy doppler mapping code presented by spruit (1998). 4.1 spiral shocks in the accretion disc of the dwarf nova ip peg fig. 3 shows comparative non-axisymmetric normal and inside-out tomograms for the heii 4686å emission line from phase-resolved spectroscopy of ip peg. the model velocity overlays were calculated using porb = 0.158206 days (∼ 228 minutes), q = 0.48, m1 = 1.16 and i = 83.8◦ (copperwheat et al. 2010). the inner and outer edges of the disc (solid lines), the roche lobes of the primary (dashed line) and secondary (solid line) as well as a single particle ballistic trajectory (solid line) from l1 to 20◦ in azimuth around the primary, are shown. in the normal tomogram the secondary appears as a bright spot inside the disc, whereas it becomes a diffuse patch (spread over more pixels) outside the disc in the inside-out tomogram. however, in the inside-out tomogram the disc appears the “right” way around as the two spiral shocks appear to be spiralling “inward” towards higher velocities. 4.2 ballistic and magnetic accretion flow in the polar hu aqr comparative normal and inside-out tomograms for the heii 4686å emission line from phase-resolved spectroscopy of hu aqr are shown in fig. 4. porb = 0.086820 days (∼ 125 minutes), q = 0.4, m1 = 0.875 and i = 84◦ (one of the models from schwope et al. 1997) were used to calculate the model velocity overlays. the roche lobes of the primary (dashed line) and secondary (solid line) as well as a single particle ballistic trajectory (solid line) from l1 to 65◦ in azimuth around the primary, are shown. a dipolar axis azimuth and co-latitude of ∼ 38◦ and ∼ 12◦ (heerlein et al. 1999) respectively, were used to calculate magnetic dipole trajectories (thin dotted lines) at 10◦ intervals from 15◦ to 65◦ in azimuth around the primary. the secondary appears as a bright spot in both the normal and the inside-out tomograms. in the normal tomogram the ballistic part of the accretion flow appears as a prominent ridge with an apparent consistent brightness from l1 to 1.0×103 km s−1, but with almost no discernible detail at higher velocities. in the insideout tomogram the ballistic flow is more exposed and varying in brightness, but retaining discernible detail to at least 1.5× 103 km s−1. low-velocity (0.0− 0.5× 103 km s−1) emission associated with the magnetic coupling region is seen as a diffuse patch in the lower left quadrant of both tomograms. there is no high-velocity (> 1.5 × 103 km s−1) emission discernible in the lower left quadrant of the normal tomogram, whereas in the inside-out tomogram there is a small patch of emission between 1.5 − 2.0 × 103 km s−1 that can be linked to the magnetically confined accretion flow close to the primary. 171 e. j. kotze, s. b. potter 5 conclusions in a normal tomogram the lower-velocity features tend to dominate the brightness scale since they are concentrated over fewer pixels compared to higher-velocity features. in an inside-out tomogram the converse is true with teneous higher-velocity features being enhanced while prominent lower-velocity features are more spread out and exposed. teneous lower-velocity features, however, may be diluted to the point of becoming indiscernible similar to teneous higher-velocity features in a normal tomogram. we have shown that inside-out doppler tomography projects the accretion disc of a cv the “right” way around with the ballistic stream and the secondary outside the disc. furthermore, the accretion flow of a polar appears more intuitive in an inside-out tomogram with the ballistic stream curving “inwards” and the magnetic flows being more exposed. therefore, we conclude that our new technique of inside-out doppler tomography is complementary to the existing technique. acknowledgement the authors would like to thank axel schwope and danny steeghs for sharing their data of hu aqr and ip peg, respectively. references [1] copperwheat c.m., et al.: 2010, mnras, 402, 1824. doi:10.1111/j.1365-2966.2009.16010.x [2] heerlein c., horne k., schwope a.d.: 1999, mnras, 304, 145. doi:10.1046/j.1365-8711.1999.02311.x [3] marsh, t.r., horne, k.: 1988, mnras, 235, 269. doi:10.1093/mnras/235.1.269 [4] schwope a.d., mantel k.-h., horne k.: 1997, a&a, 319, 894. [5] spruit h.c.: 1998, arxiv:astro-ph/9806141. [6] warner b.: 1995, cambridge astrophysics series 28, cataclysmic variable stars. cambridge univ. press, cambridge figure 3: doppler tomography of ip peg. normal (top) and inside-out (bottom) tomograms are shown for comparison. the input and reconstructed trailed spectra are shown in the left and right panels, respectively. 172 http://dx.doi.org/10.1111/j.1365-2966.2009.16010.x http://dx.doi.org/10.1046/j.1365-8711.1999.02311.x http://dx.doi.org/10.1093/mnras/235.1.269 new insights from inside-out doppler tomography figure 4: doppler tomography of hu aqr. normal (top) and inside-out (bottom) tomograms are shown for comparison. the input and reconstructed trailed spectra are shown in the left and right panels, respectively. discussion dmitry kononov: how does your new technique redistributes brightness and are there some physical suppositions behind this redistribution? enrico kotze: as we see in the example of ip peg the upper bright spiral shock in the normal tomogram appears less bright in the inside-out tomogram since it is projected over a larger area of the image. similar to the normal technique the brightness distribution in the new technique is purely a function of the projection of the spectra into the velocity space frame and we have no claims that this is a representation of the physical brightness distribution of the system. linda schmidtobreick: do you encounter problems with the resolution as the low velocities are now spread over a large circle? enrico kotze: yes, there can be a loss of resolution at low velocities. this is the reverse of what happens in the normal tomograms where high velocities are spread over a larger area and we can encounter a loss of resolution in the high-velocity features. that is why we feel the inside-out technique is complementary to the normal technique. where the normal technique tends to enhance low-velocity features with some loss in the resolution of high-velocity features, the inside-out technique tends to enhance high-velocity features with some loss in the resolution of low-velocity features. david buckley: is the magnetic longitude of the accreting pole(s) a parameter in the inside-out maps? enrico kotze: yes, for the model velocity profile overlays in the inside-out tomograms of polars we take both the azimuthal and longitudinal inclination of the assumed magnetic dipole into account. 173 introduction doppler tomography spatial coordinates velocity coordinates inside-out doppler tomography examples spiral shocks in the accretion disc of the dwarf nova ip peg ballistic and magnetic accretion flow in the polar hu aqr conclusions acta polytechnica ctu proceedings doi:10.14311/app.2016.3.0082 acta polytechnica ctu proceedings 3:82–85, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app thermo-viscoelastic characterization of polymer laminate films eliza truszkiewicza,∗, daniel tscharnutera, gerald pilzb a polymer competence center leoben gmbh, rossegerstrasse 12, 8700 leoben, austria b materials science and testing of polymers, montanuniversität leoben, otto glöckel-straße, 8700 leoben, austria ∗ corresponding author: eliza.truszkiewicz@pccl.at abstract. the investigated material laminate is intended as a substrate for small electronic components, electrodes and printed circuits, which are processed onto the laminate prior to thermoforming. the placement of the electronic components and the connecting circuits must be carefully designed to prevent damage during the thermoforming. the thermo-viscoelastic behavior of a polymer laminate film was characterized by mechanical measurements to obtain data for material modeling. the strain was measured using digital image correlation. the film is anisotropic and is able to deform to strains up to 60 %. keywords: thermoviscoelasticity, polycarbonate, polyethylene terephthalate, dynamic mechanical analysis, tensile test, stress relaxation. 1. introduction the material investigated in this study is laminate film composed of a blend of polycarbonate and acrylonitrile butadiene styrene (pc-abs) and polyethylene terephthalate (pet). the thermo-mechanical behavior of neat polycarbonate has been studied extensively, e.g. [1, 2]. they have unique combination of the high processability of abs and very good mechanical properties and heat resistance of pc. blends of pc and abs have also been the subjected of some scientific studies [3–5]. e.g. greco et al. [4] have shown that the impact strength can be improved by adding 20 % to 40 % abs and that tensile strength, young’s modulus and hardness decrease with increasing abs content. due the large variation in properties of different grades of a particular polymer or blend these data are not necessarily applicable for the present material. additionally, the pc-abs and pet films are stretched during manufacture, which introduces anisotropy in the material. the laminate is intended as a substrate for small electronic components, electrodes and printed circuits, which are processed onto the laminate prior to thermoforming. the placement of the electronic components and the connecting circuits must be carefully designed to prevent damage during the thermoforming. the polymer laminate may be stretched substantially, but for e.g. copper, the fracture strain is approx. 10 to 12 % and the ampacity may be compromised already at smaller deformation. the major task is to conduct a thermo-viscoelastic characterization of the laminate to obtain data for a material model that may be used in finite element simulations of the thermoforming process. the parameters will be determined by measurements like uniaxial and biaxial tension testing, dynamic mechanical analysis (dma) and thermomechanical analysis (tma). in this part of the work the first measurements were conducted using digital image correlation on a sample of the thermoformed laminate film (figure 1) to determine the strain field for subsequent uniaxial tensile and relaxation tests. dma was also conducted. 2. the thermoforming process the thermoforming process is a non-isothermal process of converting a sheet into a three-dimensional shape. in the first step the laminate film is heated to the forming temperature, which may be slightly above or much larger than the glass transition temperature depending on the forming pressure. in next step the film is formed using pressurized air or vacuum. the mold temperature is chosen below the glass transition temperature. due to the contact with the mold the film is cooled and the polymer chains are locked in their deformed state. when the desired shape is ready the film is removed from the mold. the thermo-viscoelastic behavior of the film is studied in a non-isothermal tensile test to imitate the heating, deforming and cooling steps of the thermoforming process. 3. experimental the thermo-viscoelastic behavior was characterized by dynamic mechanical analysis, monotonic tensile and relaxation tests for several temperatures and orientations. the dynamic mechanical analysis were carried out using a perkinelmer dma 8000. other mechanical tests were performed using a zwick/roell z250 testing machine equipped with a temperature 82 http://dx.doi.org/10.14311/app.2016.3.0082 http://ojs.cvut.cz/ojs/index.php/app vol. 3/2016 thermo-viscoelastic characterization of polymer laminate films chamber and using digital image correlation (dic; aramis, gom) for strain measurement [6]. a sample of the laminate film has been thermoformed using a generic mold. a millimeter grid has been printed on the film by the supplier. the millimeter grid may be used for strain measurement by dic, however it lacks a unique feature for the tracking of motion in subsequent images. a traceable pattern was therefore created by filling points on the grid using a permanent marker. the same pattern was applied on undeformed grid paper, which was used as a reference sample, and on deformed film to measure the strain field after the thermoforming (figure 1). figure 1. coated laminate film. figure 2. strain field on the thermoformed laminate film. figure 2 shows the major strain field as measured described above. there is almost no strain on the top, where the laminate film comes into contact with the mold first. the slopes lead to tensile strains of around 40 %. on the shoulders, additional shearing leads to major strains of up to 60 %. for the mechanical characterization, testing temperature varied between room temperature and 145°c. specimens were cut at angles of 0°, 45°and 90°and spray-coated with a pattern for dic. the monotonic tensile tests were performed with a nominal strain rate of 1/50 mm/s. the same rate was also used for the initial loading in the relaxation tests. in a non-isothermal tensile test, the film is heated to 145°c without applied stress. in the next stage the specimen is stretched to a nominal strain of 25 % and kept at this strain. the film is quickly cooled using cooling packs. the polymer chain mobility at the low temperature is strongly reduced and deformation of film is therfore locked. when the film is removed from the temperature chamber it retains this stretch. this part of the non-isothermal test is shown in figure 3. the whole process takes about 15 minutes after the removal of the stretched and cooled specimen from the testing machine for the temperature to stabilize at 145°c again. in last step the specimen is placed again in the temperature chamber, but only the upper specimen grip is closed and in this specimen position the continuation of dic strain measurement in again possible. the specimen is heated without external stress, which allows the viscoelastic part of the locked deformation to recover with time. 4. results figure 3 shows the time-dependent recovery from nonisothermal tensile test. the effect of recovery behavior of the two materials is curling up the laminate the pc layer of the film laminate recovers quickly, but it is constrainted because of the pet layer. the rolled-up shape does not permit a dic evaluation. when the laminate unfurls (the stresses have relaxed sufficiently) the strain measurement can configure 3. non-isothermal tensile test with recovery to mimic the thermoforming process. figure 4. dma results. 83 eliza truszkiewicz, daniel tscharnuter, gerald pilz acta polytechnica ctu proceedings figure 5. relation between logarithmic strain and cauchy stress – results for different orientation of specimen. figure 6. relation between the cauchy stress and time depends on temperature for 0°and 90°. tinue (figure 3, starting at stage 381). we observe that 80 % of the deformation is recovered in a short time by reheating the specimen. this test confirms the initial assumption that this thermoforming process creates predominantly viscoelastic deformation. the glass-transition temperature was determined from the dma measurements. the glass-transition of the laminate is defined by the glass-transition of the pc-abs blend and is 122°c (for separte pc amounts around 145°c and 105°c for abs [5]). a small peak at 80°c was observed (figure 4), which is characteristic for the pet film [7]. due to the high crystallinity of the pet film, the effect of this transition is small. the tensile tests showed the expected strong temperature dependence (figure 5), where the stress at a given strain decreases by a factor of 3 to 4 when raising the test temperature from 23°c to 145°c. the effect of orientations is pronounced for strains larger than 10 %. the ultimate stress at 145°c in the transverse direction is for example twice as high as in the extrusion direction, which indicates substantial stretching following the extrusion process. figure 6 shows the stress relaxation in 0°and 90°at approximately 40 % strain for temperatures of 80°c, 120°c and 145°c. for all temperatures, we observe a significant amount of stress relaxation in the first seconds after the initial loading. the relaxation rate then decreases substantially, but the viscoelastic effects are still not negligible after 1000 s of relaxation. 5. conclusions a polymer laminate film was characterized to provide data for thermo-viscoelastic material modeling. the measurements covered temperatures from room temperature to 145°c, which is approximately 20°c above the glass-transition temperature of the laminate. significant anisotropy of the laminate was observed. additional stress relaxation tests were conducted to measure the viscoelastic response of the material. acknowledgements the financial support by the austrian research promotion agency (ffg project no. 843685) is gratefully acknowledged. 84 vol. 3/2016 thermo-viscoelastic characterization of polymer laminate films references [1] s. sarva, m. boyce. mechanics of polycarbonate during high-rate tension. journal of mechanics and structures, mathematical sciences publisher 2(10):1853–1880, 2007. [2] h. azman, w. yeanjwu. mechanical properties of high impact abs/pc blends effect of blend ratio. 2005. [3] r. krache, i. debbah. some mechanical and thermal properties of pc/abs blends. materials sciences and applications 2(5):404–410, 2011. [4] r. greco, m. astarita, l. dong, a.sorrentino. polycarbonate/abs blends: processability, thermal properties and mechanical and impact behavior. polymer engineering and science 27(9):632–639, 1987. [5] w. chiang, d. hwung. properties of polycarbonate/acrylonitrile-butadiene-styrene blends. advances in polymer technology 13(4):259–274, 1994. [6] m. jerabek, z. major, r. lang. strain determination of polymeric materials using digital image correlation. polymer testing 29(3):407–416, 2010. [7] b. demırel, a. yaraş, h. elçıçek. crystallization behavior of pet materials. baü fen bil enst dergisi cilt 13(1):26–35, 2011. 85 acta polytechnica ctu proceedings 3:82–85, 2016 1 introduction 2 the thermoforming process 3 experimental 4 results 5 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2016.5.0001 acta polytechnica ctu proceedings 5:1–3, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app problems of en 50 128:2011 railway standard tomáš brandejský czech technical university in prague, department of applied informatics in transportation, faculty of transportation, praha, czech republic correspondence: brandejsky@fd.cvut.cz abstract. the second version of railway standard en50128:2011 published by cenelec is used for five years and thus the cenelec reasons about preparation of new version of this standard are coming, because the cenelec defined 10-year cycle of its standards innovation. the paper discusses some observations of problems of this standard application from the position of safety assessor which gives us the contact with developers applying this standard into the real railway products. keywords: railway software applications, assessment, safety, reliability, accessibility, maintainability, development. 1. introduction since the origin, the group of cenelec’s railway stands [1] [2] [3] was declared as standard of all safety related railway applications including not only interlocking systems, but rolling stock and related communication too. the standard en50126 defines its applicability to "the specification and demonstration of rams for all railway applications and at all levels of such an application, as appropriate, from complete railway systems to major systems and to individual and combined subsystems and components within these major systems, including those containing software". the standard en50128 defines its application domain as: "this european standard specifies procedures and technical requirements for the development of programmable electronic systems for use in railway control and protection applications. it is aimed at use in any area where there are safety implications. these may range from the very critical, such as safety signalling to the non-critical, such as management information systems. these systems may be implemented using dedicated microprocessors, programmable logic controllers, multiprocessor distributed systems, larger scale central processor systems or other architectures". and the standard en50129 defines its scope as electronic systems related to safety in application to railway interlocking systems. it means that at least standards en50126 and en50128 must be reasoned in any railway system related to safety. on the beginning of application of these standards safety assessors required application of these standards especially in the domain of interlocking systems and the rest was frequently omitted. after the year 2011, when the second generation of these standards has come into the operation the situation changed and the conformity with these standards is required also by assessors of rolling stock and other railway systems. it brings some problems described below due to different requirements on system functions in situation, when the system malfunction is detected. the main aim of the paper is the discussion of problems in nowadays application of the standard en50128 and offering of ways how to improve it. 2. problems of en50128 application the cenelec’s standard en 50128 "railway applications – communications, signalling and processing systems – software for railway control and protection systems" was defined as part of three standards group [1] [2] [3] applying standard iec 61508 "functional safety of electrical/electronic/programmable electronic safety-related systems" into the specific area of railway systems. the main difference is in different safety assessment scheme, where not only developer, validator and assessor are reasoned but also railway safety authority as next independent body. in the next chapter, particular problems will be discussed: (1.) the last version of the standard is less transparent than original one. the change of the standard structure was asked by cenelec due to unification of all cenelec standard structure. whilst the original standard was divided into 17 chapters and 2 annexes, the 2011 version is organized into 9 chapters and 4 annexes (2 are new). this change causes not only that there are no separate chapters e.g. for software validation and assessment, but software assurance chapter describing testing, verification, validation and assessment is before chapter 7 describing development process! furthermore, the chapter 7 is named "generic software development" now not looking that the term "generic software" in computer science doscon mean "common sense software", as this term is used in the standard, but "a class of software that can be used for a number of different purposes without requiring modification", as it is defined e.g. in [4] [5]. what is worse, the 1 http://dx.doi.org/10.14311/app.2016.5.0001 http://ojs.cvut.cz/ojs/index.php/app tomáš brandejský acta polytechnica ctu proceedings chapter 3.14 of 50128:2011 standard defines generic software meaning some way. thus the topic of the chapter 7 does not give any sense. similarly in the chapter v 3.1.4 of original en50128 introduces the term "component" which is defined extremely vague (and in the en50128:2011 even it is not defined), but especially in the area on object oriented programming the meaning of this term if defined precisely and totally different. because the standard en50128 is used especially by programmers, such drifting of frequent term sense might cause many misunderstandings. because en50128:2011 allows to understand term component also as object, module or even function, the meaning of e.g. chapter 7.5 might be understand totally different by particular people in particular situations. (2.) there is not explicitly declared applicability of the standard to railway vehicles and especially differences in requirements to behaviours of vehicle control systems in the case of malfunction, which is opposite to required behaviours of interlocking control systems in the analogical situation. typically, in the case of control system error vehicle must keep moving but interlocking system can signalize stop to all tracks and perform e.g. restart of the control system. (3.) there is not solved defence against targeted attack (terrorism). defence of mission critical systems against targeted attacks e.g. requires ability of the system to isolate attacked parts and thus to reconfigure system. it is a big problem, because dynamic reconfiguration is listed in table a.3 as technique 14 and it is not recommended non respecting fact that this technique is frequently adopted e.g. in military, cosmic or avionics systems. it is not possible to constraint this problem only to subjects of safe communication and physical barriers. on the other hand, standards of the information security like iso 27001 are rather oriented to managing sensitive company information than to control systems located in open space and communicating across it. (4.) the standard does not solve design of programmable hw, where on interface of sw/hw occur many specific problems which solution is not defined in the actual standard. many of these problems were discussed in [6], like specific problems of design, timing and application structure but there also another problems like problem of dedication of safety related functions to development tools which is related to problems discusses herein in chapter (6.) and which is not solved. design tools transforming e.g. vhdl language into configuration bit stream of the chip does not work deterministically and this fact is hard to accept in safe system design. (5.) the standard en50128 contains extensive appendix b "key software roles and responsibilities" on ten pages and small appendix c "documents control summary", which only recapitulate textual part figure 1. the example of lifecycle hierarchy of complex system. of the standard and do not bring any additional information. it is good to delete such chapters because they only decrease clarity of the standard. (6.) chapter 8 "development of application data or algorithms: systems configured by application data or algorithms" should explain better requirements of systems with different level of configurability. it is hard to compare simple system which is configured by one dimensional table of parameters and system where safety-related functions are described in configuration language, which is interpreted in real time and where part on safety checks is dedicated to development tools. the figure 1 draws possible configuration of different life-cycles cooperating on development of final (sometimes also generic) application based on configurable generic kernel where e.g. life cycle of generic system determines requirement on lc of final application and final application development tools life cycle. (7.) in comparison to standard iec 61508-3 this railway standard does not contain equivalent of iec 61508-3 appendix c explaining which sw property is achieved by which technique. such explanation is useful both for designers and assessors because it simplifies, objectivises and formalizes selection of design techniques in atypical, non-standard situations where groups of design techniques predefined in the table a.3 are inapplicable. typical example of this situation is in this moment application of programmable hw, which is not solved in the standards and which requires a little bit different approach than standard hw and sw. (8.) there is not solved problem of design of systems with safety integrity level greater than 4. growing complexity of railway systems, especially of such systems as ertms, tends to requirement of such sil. it is true, that many calls for higher sils are given by misunderstandings of sil meaning. sil is related to tolerable hazard rate, as it is introduced in the standard en 50129, table a.1. tolerable hazard rate is related to one hour and one function, but many designers of railway systems missrelates it to number of invocations of the function and means 2 vol. 5/2016 problems of en 50 128:2011 railway standard that systems working on higher operation frequency must have higher sil. it is mistake. (9.) there is not well defined that sils are determined to top-level functions, not to whole system and not to any sub-functions. the standard en50129 uses formulation single function without precision of the complexity of the function. many top-level functions are performed by groups of lower level functions. this lack of precise definition tends to many useless discussions between manufactures and assessors. (10.) the standard defines five different sil levels but de facto it specifies only three different cases: sil0, sil1 and 2; and sil 3 and 4. in addition, requirements to sil 1 and 2 systems are inappropriate strict as well as there are requirements to documentation complexity of sil0 systems, especially in comparison to cots systems of the equal sil level. but in fact it would be just opposite – e.g. it is need to do precise testing developed by other company, which design process is not well described, where the documentation is missing, than in the case of well documented one. 3. discussion ten year cycle of cenelec standard upgrade is difficult especially to rolling stock manufacturers. locomotives, carriages and other vehicles have extremely long life-cycle taking any tens of years. there is long design phase including real research, own assessment phase sometimes takes about ten years and also operation is reasoned in horizon of thirty years or more. thus the idea that between start of design and start of operation the required standard will be once or even two times changes is not acceptable. because cenelec does not accept this fact, rolling stock making companies provide "diverse activity" in related cenelec work-groups and prevents significant changes of these standards. on the opposite side, above mentioned problems does not represent significant changes of the standards and their acceptance in the new generation of them might increase their applicability. 4. conclusions the above presented paper summarises problems on the today railway standard en50128:2011, which were observed in certification body of czech technical university in prague – cov fd čvut v praze during certifications of many railway systems serving especially (but not only) in czech republic. references [1] en50126 railway applications – the specification and demonstration of reliability, availability, maintainability and safety (rams). [2] en50128 railway applications – communication, signalling and processing systems – software for railway control and protection systems. [3] en50129 railway applications – communication, signalling and processing systems – safety-related electronic systems for signalling. [4] http://www.teach-ict.com/glossary/g/ genericsoftware.htm. [5] http://www.computingstudents.com/dictionary/ ?word=generic%20software. [6] t. musil. návrh metodiky pro vývoj a verifikaci bezpečných algoritmøu implementovaných v dynamicky rekonfigurovatelných fpga, phd. thesis, 2015. 3 http://www.teach-ict.com/glossary/g/genericsoftware.htm http://www.teach-ict.com/glossary/g/genericsoftware.htm http://www.computingstudents.com/dictionary/?word=generic%20software http://www.computingstudents.com/dictionary/?word=generic%20software acta polytechnica ctu proceedings 5:1–3, 2016 1 introduction 2 problems of en50128 application 3 discussion 4 conclusions references 165 acta polytechnica ctu proceedings 2(1): 165–169, 2015 165 doi: 10.14311/app.2015.02.0165 superoutburst of a new sub-period-minimum dwarf nova css130418 in hercules d. chochol1, s. shugarov1,2, n. katysheva2, i. volkov2, a. zharova2, e. pavlenko3, n. pit3, r. zvagelsky3, o. antoniuk3, k. antoniuk3, a. baklanov3, n. borisov4, m. gabdeev4 1astronomical institute of the slovak academy of sciences, 059 60 tatranská lomnica, slovakia 2sternberg astronomical institute of the moscow state university, russia 3crimean astrophysical observatory, nauchny, ukraine 4special astrophysical observatory of the russian academy of sciences, nizhnij arkhyz corresponding author: chochol@ta3.sk abstract multicolour photometry of a new dwarf nova css130418 in hercules, which underwent superoutburst on april 18, 2013, allow to classified it as a wz sge-type dwarf nova. the phase light curves for different stages of superoutburst are presented. the early superhumps were used to determine the orbital period porb = 64.84(1) minutes, which is shorter than the period minimum ∼ 78 minutes for normal hydrogen-rich cataclysmic variables. we found the mean period of ordinary superhumps psh = 65.559(1) minutes. the quiescent spectrum is rich in helium, showing double peaked emission lines of h i and he i from accretion disk, so the dwarf nova is in a late stage of stellar evolution. keywords: cataclysmic variables dwarf novae su uma-type wz sge-type photometry spectroscopy individual: css 130418. 1 introduction cataclysmic variables (cvs) are close binary systems with the white dwarf (wd) accreting matter from a companion which fills its roche lobe. due to non-zero momentum the matter creates accretion disk around the primary component. su uma-type dwarf novae (dne) are subclass of cvs which exhibits outbursts and less frequent brighter superoutbursts. the superhumps are periodic tooth shaped light variations observed during superoutbursts. superhumps periods are a few percent longer than the orbital period. their amplitudes at superoutburst maximum are 0.2−0.7 mag and decrease afterwards. according to the model proposed by whitehurst (1988) and hirose & osaki (1990), superhumps are caused by tidal 3:1 resonance in the outer parts of accretion disk, leading to the formation of an eccentric outer ring undergoing apsidal motion. smak (2009) proposed alternative interpretation of superhumps as being due to modulated mass transfer rate resulting in periodically enhanced dissipation of the kinetic energy of the stream. the wz sge-type objects are the most extreme subgroup of su uma-type dne with the typical orbital periods 80−90 minutes that exhibits only superoutbursts with amplitude 6−8 mag and a long (several years) recurrence time. one of the most remarkable signatures of wz sge-type objects is a presence of early superhumps, observed in the first days of superoutburst. early superhumps have a period very close to a binary period and commonly show a double humped profile. osaki & meyer (2002) suggested, that this phenomenon is manifestation of the tidal 2:1 resonance in accretion disks of binary systems with extremely low mass ratio. resonance forms a two-armed spiral pattern of tidal dissipation, which leads to a double-peaked feature in the orbital light curve. very few cvs have orbital periods below the so called period minimum ∼78 minutes. 2 css130418 2.1 discovery on 2013 april 18.47, the catalina real-time transient survey (crts) detected an outburst of css130418: 174033.5+414756 in hercules (drake et al., 2009). the brightness of the object at the time of discovery was 14.04 mag. according to crts circular, the object had an 7.5 mag outburst in 2007, that lasted two month. prieto et al. (2013) discovered the transient independently with the all sky automated survey for supernovae (asas-sn) on 2013, april 19.53, when it 165 http://dx.doi.org/10.14311/app.2015.02.0165 d. chochol et al. brightness was v = 12.7 mag. they found a precursor with b = 19.2 and r = 18.2 mag in usno-a2 catalog and previous outburst in galex uv source in the galex dr5 catalog with fuv = 13.62 and nuv = 14.17 mag on 2007 may 27. an optical spectrum of the transient, taken by the osmos imagine spectrograph of the mdm 2.4m telescope on 2013, april 21.41, shows a blue continuum (black-body teff = 16 000 k) with balmer and he i lines in absorption and weak he ii in emission. 2.2 light curve of the superoutburst 56410 56420 56430 56440 56450 19 18 17 16 15 14 13 our data dubovsky aavso v jd 2400000+ figure 1: v light curve of superoutburst. 56410 56420 56430 56440 56450 18 16 14 0,2 0,0 -0,2 -0,4 -0,6 v u-b b-v v-r r-i v jd 2400000+ c.i. figure 2: mean v light curve and colour indices curves of superoutburst. our ubv (ri)c ccd observations were carried out with the 0.6m telescope at the stará lesná observatory, 0.4, 1m and 1.25m telescopes of the crimean observatory and 0.6m telescope at the crimean laboratory of the sternberg astronomical institute. we added the ccd observations of p. dubovský taken by 1m telescope at kolonica saddle (slovakia) available at http : //var2.astro.cz/slovakia and aavso v data. the superoutburst v light curve is presented in fig. 1. -0,2 0,0 0,2 0,4 0,6 0,8 0,6 0,4 0,2 0,0 -0,2 -0,4 -0,6 -0,8 u-b b-v f0 g0 b3 a0 12000 10000 8000 6000 5000 2 5 10-15 20 25 k0 figure 3: two colour diagram. the average night magnitudes of v observations from fig. 1 and our colour indices data are shown in fig. 2. the evolution of the nova in a two colour (u−b,b− v ) diagram is displayed in fig. 3. the main and black body sequences are plotted with solid and dashed lines, respectively. the positions of field stars are marked by stars. filled circles correspond to the positions of the dwarf nova at the days after maximum, which occurred at jd=2456403. 2.3 early superhumps early superhumps are periodic modulations of the brightness of wz sge-type dwarf novae seen during superoutburst with a period identical to the orbital period 0,0 0,2 0,4 0,6 0,8 1,0 1,2 1,4 0,06 0,04 0,02 0,00 -0,02 -0,04 phase jd 2456403-406m figure 4: phase light curve of early superhumps. (ishioka et al., 2002). therefore, they are known as orbital humps. after the declining trend removal from v and b light curves of all available data, taken in the first 4 days after maximum, we found the ephemeris 166 superoutburst of a new sub-period-minimum dwarf nova css130418 in hercules for brightness maxima of early superhumps by fourier period analysis as follows: jdmax = 2456402.076 + 0.045026 × e. (1) the phase light curve of early superhumps including the mean light curve is shown in fig. 4. 2.4 ordinary superhumps ordinary superhumps are periodic modulation seen during superoutburst after disappearance of early superhumps. our v observations of superhumps of the object, obtained during the night run 15 days after maximum (am), are presented in fig. 5. 56417,35 56417,40 56417,45 56417,50 56417,55 14,24 14,20 14,16 14,12 v jd 2400000+ figure 5: v light curve of superhumps. after the declining trend removal from v and b light curves of all available data taken on days 5-22 am we found the mean ephemeris for brightness maxima of ordinary superhumps by fourier period analysis as follows: jdmax = 2456402.092 + 0.0455269 × e. (2) the evolution of ordinary superhumps during the superoutburst are presented in figs. 6-10 in different days am. the ephemeris (2) was used for all data in phase light curves. 0,0 0,2 0,4 0,6 0,8 1,0 1,2 1,4 0,06 0,04 0,02 0,00 -0,02 -0,04 phase jd 2456407m figure 6: ordinary superhumps on day 5 am. 0,0 0,2 0,4 0,6 0,8 1,0 1,2 1,4 0,10 0,05 0,00 -0,05 -0,10 phase jd 2456409-410m figure 7: ordinary superhumps on days 7-8 am. 0,0 0,2 0,4 0,6 0,8 1,0 1,2 1,4 0,05 0,00 -0,05 -0,10 phase jd 2456415-416m figure 8: ordinary superhumps on days 13-14 am. 0,0 0,2 0,4 0,6 0,8 1,0 1,2 1,4 0,06 0,04 0,02 0,00 -0,02 -0,04 -0,06 -0,08 phase jd 2456419-420 m figure 9: ordinary superhumps on days 17-18 am. 0,0 0,2 0,4 0,6 0,8 1,0 1,2 1,4 0,08 0,06 0,04 0,02 0,00 -0,02 -0,04 -0,06 -0,08 phase jd 2456423-424 m figure 10: ordinary superhumps on days 21-22 am. 167 d. chochol et al. 3 our spectroscopy our spectra were taken with the scorpio spectrograph of the 6m telescope in sao during the superoutburst and quiescence of the dn in the range 40505100å. they are presented in fig. 11. the spectrum during superoutburst shows h i and he i lines in absorption and he ii in emission. quiescent spectrum is rich in helium, showing double peaked emission lines of h i and he i from accretion disk. the spectrum is similar to the spectrum of the helium-rich cataclysmic variable sbss 1108+574, which has the orbital period 55.3 minutes (carter et al. 2013). figure 11: spectrum of the object in outburst (may 4/5, 2013) and quiescence (august 2/3, 2013). 4 discussion and conclusions we found a new sub-period-minimum cv with the orbital period porb = 64.84(1) minutes and classified it as a wz sge-type dwarf nova. period of ordinary superhumps p = 65.559(1) minutes allowed to determine the fractional superhumps excess ε = [psh/porb 1] = 0.0111(4) and also the mass ratio q = 0.0565(20), applying the relation of patterson et al. (2005): ε = 0.18q + 0.29q2. presented object css130418 enlarged the group of dne under the period minimum and can help to understand its evolutionary status. hydrogen lines in the spectrum exclude the possibility that the object belongs to am cvn stars. the existence of early and ordinary superhumps shows that css130418 is evolved wz sge-type dn. the most probable scenario of evolution is that the mass transfer started near the end of a main-sequence lifetime of the donor star. after the donor transferred its hydrogen envelope, the mass transfer continue from hydrogen deficient interior of the star. the presence of strong he i lines in the spectrum of the object supports this view. acknowledgement we acknowledge with thanks the variable star observations from the aavso international database contributed by observers worldwide and used in this research. this study was supported by the vega grants 2/0094/11, 2/0002/13 and rfbr research projects no. 11-02-01213a, 14-02-00825 and nsh 1675.2014.2. references [1] carter, p.j., steeghs, d., de miguel e., goff, w., et al.: 2013, mnras 431, 372. doi:10.1093/mnras/stt169 [2] drake, a.j., djorgovski, s.g.,mahabal, a., beshore, e., et al.: 2009, apj 696, 870. doi:10.1088/0004-637x/696/1/870 [3] hirose, m., osaki, y. : 1990, publ. astron. soc. japan 42, 135. [4] ishioka, r., uemura, m., matsumoto, k., ohashi, h., et al.: 2002, a&a 381, l41. [5] osaki, y., meyer, f. : 2002, a&a 383, 574. [6] patterson, j., kemp, j., harvey, d.a., fried, r.e., et al.: 2005, pasp 117, 1204. doi:10.1086/447771 [7] prieto, j.l., hainline, k., hickox, r., goulding, a., et al. : 2013, atel 4999. [8] smak, j. : 2009, aca 59, 121. [9] whitehurst, r. : 1988, mnras 232, 35. doi:10.1093/mnras/232.1.35 discussion christian knigge: i think there are 3 possible interpretation for your system: 1) it could move started contact, when the donor was already nuclear evolved (like ei psc). 2) it could be a low metallicity halo object (like j1507 = patterson/uthas). 3) it could be a system in which the secondary was already a substellar object before contact (as had been suggested for j1507 by littlefair et al. (2007). dmitry kononov: how deeply evolved cvs can go beyond the period minimum? drahomír chochol: the shortest orbital period from already known cvs, excluding am cvn stars 168 http://dx.doi.org/10.1093/mnras/stt169 http://dx.doi.org/10.1088/0004-637x/696/1/870 http://dx.doi.org/10.1086/447771 http://dx.doi.org/10.1093/mnras/232.1.35 superoutburst of a new sub-period-minimum dwarf nova css130418 in hercules (orbital periods 5 60 min), has a dwarf nova css102808: 52.1 minutes (woudt et al., 2012). vojtech šimon: a group of cvs with unexpected orbital periods of ≈60 min emerging from the observations. what about the mutual similarities of the spectroscopic properties of these systems? do they show similarities for example in the hydrogen/helium ratio? drahomír chochol: the heiλ6678/hα ratios of css 100603 (p = 65.23 min) and sbss 1108+574 (p = 55.3 min) are 1.49 and 0.81, respectively (breedt et al. 2012; carter et al. 2013), so they are helium rich systems. the ratios in ei psc and v485 cen are higher than those typically seen in su uma systems. spectrum of css130418 is similar to the spectra of previous objects. on the other hand in j1507 heiλ6678/hα ratio is only 0.07. paula szkody: what criteria are used for calling it he-rich? many other cvs show he i strong. unusual short period systems have evolved donors. drahomír chochol: we just simply compare our spectrum with the spectrum of helium rich cv sbss 1108+574 (carter et al. 2013). 169 introduction css130418 discovery light curve of the superoutburst early superhumps ordinary superhumps our spectroscopy discussion and conclusions 139 acta polytechnica ctu proceedings 2(1): 139–142, 2015 139 doi: 10.14311/app.2015.02.0139 high-speed photo-polarimetry of magnetic cataclysmic variables s. b. potter1 1south african astronomical observatory, po box 9, observatory 7935, cape town, south africa corresponding author: sbp@saao.ac.za abstract i review recent highlights of the saao high-speed photo-polarimeter (hippo) on the study of magnetic cataclysmic variables. its high-speed capabilities are demonstrated with example observations made of the intermediate polar ny lup and the polar igrj14536-5522. keywords: cataclysmic variables polars intermediate polars optical polarimetry photometry x-rays individual: ny lup, igrj14536-5522. 1 introduction saaos hippo was designed and built in order to replace its highly successful but aging single channel equivalent, namely the uct (university of cape town) photo-polarimeter (cropper 1985). its purpose is to obtain simultaneous all-stokes parameters, of unresolved astronomical sources. in addition, it is capable of high speed, simultaneous 2 filtered, photo-polarimetry in order to permit investigations of rapidly varying polarized astronomical sources. of particular interest are magnetic cataclysmic variables (mcvs). in the following two sections we demonstrate its capabilities. 2 photo-polarimetry the intermediate polar ny lup figure 1: i-band photo-polarimetric observations of the intermediate polar ny lup. bottom and top panels are the phase-spin-folded photometry and circular polarization respectively. left and right panels were made with the 1.9m of the saao and the vlt respectively. figure reproduced from potter et al. (2012). 139 http://dx.doi.org/10.14311/app.2015.02.0139 s. b. potter fig. 1 shows two sets of i-band observations of the intermediate polar ny lup, phase-folded on its white dwarf spin period of 693s. the data in the left hand panels were made with the 1.9m telescope of the saao (taken from potter et al 2012) and the right hand panels were made with the 27 times larger vlt of the eso (taken from katajainen et al 2010). the saao polarimeter (hippo; potter et al 2010) is equiped with photo-multiplier tubes whereas the vlt polarimeter used a superior, 4 times more quantum efficient, ccd camera. both data sets show a spin modulation in the photometry and agree on the average value of circular polarization of ∼ -1.5 percent. however, contrary to expectations, the hippo observations are by far the superior dataset for the following reasons: the vlt photometry appears to have a residual repeating pattern of about 8 cycles per spin period, probably arising as a result of the different waveplate position angles. the hippo circular polarization shows a clear spin modulation whereas the vlt polarimetry displays a more random scatter about the mean. in addition the hippo also obtained simulatenously b-band observations. these observations (not shown) clearly show the presence of a circularly polarised spin modulation. the vlt b-band were not only not simultaneous, but also did not detect a spin modulation. furthermore the hippo simultaneously measured linear polarization (not shown) albiet a non-detection. the superior performance of the hippo is because it is optimised to measure polarization variability. specifically the exposure readout times of the photomultiplier tubes are very fast (sub-second) thus enabling polarization measurements to be made on a timescale much shorter than the intrinsic variability of the polarization. the ccd readout times on the vlt were too slow leading to the smearing of the polarimetric variability and systematic residuals in the photometry. 3 photo-polarimetry the polar igrj14536-5522 igrj14536-5522 (=swift j453.4-5524) was discovered as a hard x-ray source by integral (kuiper, keek, hermsen, jonker & steeghs 2006) and by swift/bat (mukai et al. 2006). a pointed swift/xrt observation led to the identification with a rosat all-sky survey (rass) source 1 rxs j145341.1-552146, and hence to its optical identification (masetti et al. 2006). based on these observations and the presence of short period optical and x-ray periodic modulations, revnivtsev et al. (2008) classified it as an ip. followup photo-polarimetric observations with the hippo (potter et al. 2010) however clearly shows orbitaly modulated photometry and circularly polarization from ∼ 0 to ∼ 18 per cent, unambiguously identifying igrj14536-5522 as a polar (fig.2, left and right upper panels respectively: from potter et al. 2010). in addition to the orbital modulation, a close inspection of the photometry and polarimetry reveals short period modulations throughout the orbit which, in addition to being a hard integral source, contributed to its initial mis-identification as an ip. the short period modulations are mostly consistent with being due to noise or flickering. however, detailed fourier analysis of all of the data reveals that some of the data sets show significant singularly persistent peaks that are consistent with qpos. the results are shown as a trailed amplitude spectrum in the second row of fig.2. between phases 0.2-1.0 the amplitude spectra do not show any significant peaks which indicates that the variations are mostly flickering or noise. however, there is a significant dominating signal centered on 0.0032(1) hz (5.2 minutes, indicated by the dashed line) between phases 1.0 and 1.3 in both the photometry and the polarimetry. this is clear evidence of a qpo. in the third row of fig. 2 we show the normalised photometry and polarimetry during the phase range that is dominated by the qpo. over plotted are the least squares fit of the qpo frequencies. as one can see, the qpo is very well described by the single dominant frequency as found in the trailed amplitude spectra. the plots in the bottom row of fig. 2 show the corresponding amplitude spectra for the qpo dominated phase range. our polarimetric results unambigously demonstrate that the qpo emissions (photometric and polarimetric) originate from the accretion shock. ultimately, these are caused by variations in the accretion flow. the most natural place to modulate the accretion flow would be at the threading region, perhaps caused by instabilities as a result of the interaction of the accretion flow with the magnetic field. we are now using mhd modelling to investigate this possibility. 140 high-speed photo-polarimetry of magnetic cataclysmic variables figure 2: left plots, a-d: the photometry, the corresponding trailed amplitude spectra, the normalised photometry for the phase range 1.0-1.3 and its corresponding amplitude spectra respectively. the solid curve is the least squares fit using the frequency derived from the trailed spectra (dashed line). right plots: as in the left plots but for the circular polarization. figure reproduced from potter et al. (2010). 4 conclusions we have shown that the saao high-speed photopolarimeter (hippo) is capable of high-speed, multifiltered, simultaneous all-stokes observations. it is therefore ideal for investigating rapidly varying astronomical sources such as magnetic cataclysmic variables. in particular white dwarf spin modulations and quasi-periodic-oscillations (qpos). acknowledgement i thank the organsers for giving me the opportunity to present some of my recent work and for a great conference. references [1] cropper, m. s.: 1985, mnras 212, 709. doi:10.1093/mnras/212.3.709 [2] kuiper, l., et al: 2006, atel 684. [3] katajainen, s., et al.: 2010, apj 724, 165. doi:10.1088/0004-637x/724/1/165 [4] masetti, n. et al: 2006, atel 783. [5] mukai, k. et al: 2006, atel 686. [6] potter, s.b., et al: 2010, mnras 402, 1161. doi:10.1111/j.1365-2966.2009.15944.x [7] potter, s.b., et al: 2012, mnras 420, 2596. doi:10.1111/j.1365-2966.2011.20232.x [8] revnivtsev, m., et al: 2008, a&a 489, 1121. discussion christian knigge: do you have any speculative ideas already for the origin of the ∼ 6 minute qpos? 141 http://dx.doi.org/10.1093/mnras/212.3.709 http://dx.doi.org/10.1088/0004-637x/724/1/165 http://dx.doi.org/10.1111/j.1365-2966.2009.15944.x http://dx.doi.org/10.1111/j.1365-2966.2011.20232.x s. b. potter stephen potter: since the qpo is seen in polarized light then it must be associated with the accretion shock region. so best guess is that the qpo may represent an instability in the threading region causing quasi-modulated accretion onto the white dwarf. pieter meintjes: in one of your slides you showed distinct qpo features with periods of ∼ few seconds. any idea what may have caused that and is that associated with high or low states in accretion? in other words, are they sometimes more prominent than other times (depending on accretion) and is the polarization level also fluctuating depending on accretion? stephen potter: photometric qpos of the order of a few seconds are thought to arise from oscillations in the shock itself. there is not yet a sufficient amount of observational data to see if there is any correlation with e.g. accretion rate and/or magnetic field strengths etc. we detect polarized qpos at ∼ minute timescales but not ∼ second timescales. 142 introduction photo-polarimetry the intermediate polar ny lup photo-polarimetry the polar igrj14536-5522 conclusions 183 acta polytechnica ctu proceedings 2(1): 183–187, 2015 183 doi: 10.14311/app.2015.02.0183 close-in substellar companions and the formation of sdb-type close binary stars l. y. zhu1,2,3, s. b. qian1,2,3, e.-g. zhao1,2, e. fernández lajús4,5, z.-t. han1,2,3 1yunnan observatories, chinese academy of sciences, p.o. box 110, 650011 kunming, p.r. china 2key laboratory for the structure and evolution of celestial bodies, chinese academy of sciences, p.o. box 110, 650011 kunming, p. r. china. 3physical sciences department, graduate university of the chinese academy of sciences, yuquan road 19, sijingshang block, 100049 beijing, china. 4facultad de ciencias astronómicasy geof́ısicas, universidad nacional de la plata, 1900 la plata, buenos aires, argentina. 5instituto de astrofisica de la plata (cct la plata conicet/unlp), argentina. corresponding author: zhuly@ynao.ac.cn abstract the sdb-type close binaries are believed to have experienced a common-envelope phase and may evolve into cataclysmic binaries (cvs). about 10 % of all known sdb binaries are eclipsing binaries consisting of very hot subdwarf primaries and low-mass companions with short orbital periods. the eclipse profiles of these systems are very narrow and deep, which benefits the determination of high precise eclipsing times and makes the detection of small and close-in tertiary bodies possible. since 2006 we have monitored some sdb-type eclipsing binaries to search for the close-in substellar companions by analyzing the light travel time effect. here some progresses of the program are reviewed and the formation of sdb-type binary is discussed. keywords: hot subdwarf binary photometry individual: ny vir, hs 0705+6700, nsvs 07826147. 1 introduction hot subdwarf stars (sdb) lie in the extreme horizontal branch (ehb). they are burning helium in their cores and have very thin hydrogen envelopes. after leaving the main sequence, the progenitors of sdbs would evolve to red giant, ignite helium and settle down on the ehb (heber 2009). they have high temperatures and gravities. to explain these characters, their progenitors must have experienced enhanced mass loss at the tip of red giant branch (castellani and castellani, 1993; d’cruz et al., 1996). however, what causes this extreme mass loss remains an open question. many authors suggested that the mass loss is triggered by the presence of a companion. in 2007, silvotti et al., found a giant planet orbiting around a sdb star, v391 pegasi, at a distance of 1.7 au. after that, an even more extreme case was published by charpinet et al., (2011). they reported the presence of two nearly earth-sized bodies orbiting the sdb star kic 05807616 at distances of 0.0060 au and 0.0076 au, with orbital periods of 5.7625 and 8.2293 hours, respectively. these detections support the way to form single sdb stars that these bodies were originally giant planets immersed in the red-giant envelope and massive enough to survive engulfment and triggered the enhanced mass loss necessary for the formation of an sdb star. so the close-in substellar companions paly an important role to form single sdb stars. actually, about half (or may be more) of the sdbs reside in close binaries (morales-rueda et al., 2006). are there any substellar objects around sdb close binaries just like the substellars founded around the single sdb stars? recently, some circumbinary substellars orbiting around sdb eclipsing binaries were indeed detected, such as hw vir (lee et al., 2009), hs 0705+6700 (qian et al, 2009), ny vir (qian et al., 2012) and sdssj0820+0008 (geier et al, 2012). the sdb close binaries are believed to be formed from binary systems through common envelope(ce) ejection (han et al., 2002, 2003). because the separation of the two components in sdb close binaries is much less than the size of the subdwarf progenitor in its red-giant phase, these systems must have experienced a ce phase. after spiral in and envelope ejection, the present binary system consisting of a sdb star and a low-mass companion star was formed with short periods. the presence of substellar tertiary, especially the close-in objects, orbiting sdb close binaries provides some clues to the inter183 http://dx.doi.org/10.14311/app.2015.02.0183 l. y. zhu et al. active effect between them, and may give evidences of the formation of the planets and the sdb close binaries. 2 targets and method for searching for close-in substellar companions of the sdb close binaries, we chose eclipsing sdb close binaries (i.e. hw vir binaries) as our targets to monitor because their eclipsing profiles provide us with very useful information about their orbital period variations, which may be caused by the presence of third bodies. hw vir binaries have been known for more than four decades. they are detached eclipsing binaries composed of a sdb star and a low-mass companion star. till now, not more than fifteen of such objects were discovered. their well-detached configuration indicates that their eclipses might not be influenced by the accretion-driven radiations from other parts (e.g., the accretion discs and hot spots etc.) observed in cvs. and the compact structures of both components make the eclipses in the light curves very narrow and deep. these characteristics favour a highly precise determination of their times of light minimum, generally with errors less than 0.0001days. thus very small amplitude orbital period variations due to the substellar tertiaries can be detected by analyzing the observed-calculated (o-c) diagrams. therefore they are the most hopeful targets for detecting substellar objects around them with light time effect. using 2.4-m, 1-m and 60-cm telescopes in yunnan observatories, 2.16-m and 85-cm telescopes in xinglong station of national observatories and 2.15-m jorge sahade telescope in argentina, we began to monitor hw vir binaries since 2006. our targets are listed in table 1. table 1: summary of our targets name coordinate period mag. (j2000) h (mag) hw vir 12 44 20.24 -08 40 16.8 2.801 v=11.2 ny vir 13 38 48.14 -02 01 49.2 2.426 v=14.2 hs 0705+6700 07 10 42.09 +66 55 44.0 2.296 b=14.1 hs 2231+2441 22 34 20.89 +24 57 00.4 2.654 v=14.1 nsvs 14256825 20 20 00.51 +04 37 55.6 2.649 v=14.3 bulsc16-335 14 45 20.21 -06 44 03.2 3.001 v=16.3 nsvs 07826147 15 33 49.40 +37 59 28.6 3.883 v=13.6 sdssj 0820+0008 08 20 53.5 +00 08 53.4 2.304 g=14.9 2m1938+4603 19 38 32.61 +46 03 59.1 3.024 g=11.9 ec10246-2707 10 26 56.47 -27 22 57.1 2.844 b=14.2 asas 102322-3737 10 23 21.89 -37 36 59.9 3.343 v=11.6 supposing that there is a third body existing in this system, under the mutual gravitation force, the components of eclipsing pair would rotate around the barycenter of this triple system. seen by a distant observer, the light-travel time of this system will change because of the change in the orbital movement caused by the additional body, which can result in the observed cyclic change in the o-c diagram constructed by the eclipsing timings. this light time effect is very useful to detect tertiaries within au distance level in evolved eclipsing binaries compared with the radial velocity and transit methods, which have been extensively used to search for planets around solar-type main-sequence stars. that is because the high surface gravity of the evolved stars prevents us to achieve the high radial velocity precision required to detect planets, and the small size of the components (for example, r1 = 0.166 and r2 = 0.152 for nsvs 07826147 derived by for et al., 2010.) make the low probability of transits, see silvotti (2009) for more information. 3 new results here we present new results of our three targets (hs 0705+6700, ny vir and nsvs 07826147) from our ongoing search for circumbinary substellars orbiting around sdb eclipsing binaries. for hs 0705+6700 and ny vir, new observations confirmed our previous study (qian et al., 2009, 2012). for nsvs 07826147, preliminary analysis of the o-c diagram constructed by our five years data implied the presence of a close-in planet orbiting around it at a distance about 0.64au. 3.1 hs 0705+6700 hs0705+6700 ( = gsc 4123-265) was listed as a dwarf candidate from the hamburg schmidt survey (hagen et al. 1995 ). the observations indicated that it is an eclipsing binary. a detailed photometric and spectroscopic investigation was carried out by drechsel et al. (2001). absolute parameters of both components were determined suggesting that the primary is an sdb star, while the secondary is a cool stellar object. a cyclic change in the o-c curve of hs 0705+6700 was discovered by qian et al. (2009), which indicated the presence of a possible brown dwarf companion. it was later confirmed by camurdan et al. (2012), beuermann et al. (2012), and qian et al. (2013) who revised the parameters of the brown dwarf. the (o − c)1 diagram of the sdb-type binary hs 0705+6700 with respect to the following linear ephemeris, min.i = bjd 2451822.760549 + 0.09564665×e, (1) was displayed in fig. 1, where dots refer to our new data obtained after qian et al. (2009). it is shown that, apart from the cyclic change reported by previous authors, there is an upward parabolic variation in the (o−c)1 curve. this reveals a period increase at a rate of ṗ = +9.8×10−9 days/year. the angular momentum loss via gravitational radiation or/and magnetic braking should cause a decrease in the orbital period rather than increase. moreover, the period increase cannot be 184 close-in substellar companions and the formation of sdb-type close binary stars 0 10000 20000 30000 40000 50000 -0.003 -0.002 -0.001 0.000 0.001 0.002 0.003 e figure 1: o-c diagram of hs 0705+6700. dots refer to our new data obtained after qian et al. (2009), and open circles to the other data. dashed line refers to the continuous increase in the period, while the solid line to a combination of the period increase and a cyclic change. explained by mass transfer between the components because of the detached configuration of the system. therefore, the observed upward parabolic variation may be only a part of another cyclic change with very longperiod that is caused by the light-travel time effect due to the presence of another substellar object in a wider orbit. 3.2 ny vir ny vir (pg 1336-018) was discovered as a hw vir binary by kilkenny et al., (1998) which is composed of 2.580 2.585 2.590 2.595 2.600 2.605 0.4 0.2 0.0 -0.2 -0.4 6.750 6.755 6.760 6.765 0.4 0.2 0.0 -0.2 -0.4 figure 2: eclipse profiles of ny vir observed in november 2012 and april 2013 with the 2.15-m ”jorge sahade” telescope. dots represent the magnitude differences between the ny vir and the comparison star. a rapid pulsator and an m5-type star. kilkenny et al., (2011) found the orbital period of the binary is decreasing at a rate of ṗ = −11.2 × 10−13 d per orbit. a cyclic change was discovered to be superimposed on the long-term decrease by qian et al. (2012), which was explained by the presence of a circumbinary planet. qian et al. (2012) pointed out that the long-term period decrease can not be explained by angular momentum loss via gravitational radiation or/and magnetic braking and proposed that there is another substellar object in a wider orbit as in the case of hs 0705+6700. new observations of the sdb binary were obtained. the eclipse profiles obtained by using the 2.15-m ”jorge sahade” telescope in argentina were shown in fig. 2. the new determined eclipse times confirm the presence of the circumbinary planet and the parameters will be revised by including more times of light minimum. 3.3 nsvs 07826147 nsvs07826147 (2m 1533+3759) has been suspected as a possible eclipsing sdb binary system by kelley and shaw (2007) using the data from the northern sky variability survey and the two micron all sky survey. they derived the period of this system as 0.16177 days. zhu and qian (2009) improved its period as 0.16177046 days based on all available times of light minimum until that time. the detailed absolute parameters derived by the combination of photometric and spectroscopic observations were published by for et al., (2010). till now, we have monitored this target for more than 5 years. new light curves obtained with the 85-cm telescope and the 2.4m telescope are displayed in fig. 3. the constructed o-c diagram shows the trend of the periodic variation, which implies the presence of a closein circumbinary planet in nsvs 07826147 at a distance about 0.64au. the detailed analysis is in progress. 72.34 72.35 72.36 72.37 0.9 0.0 -0.9 m hjd2455900+ 74.256 74.260 74.264 74.268 74.272 74.276 2 1 0 -1 figure 3: light curves of nsvs07826147. left panel: eclipsing profiles of nsvs07826147 obtained with 85cm telescope on may 26, 2012 in r band. right panel: obtained with 2.4-m telescope on feb. 14, 2012 without filters. dots refer to the magnitude differences between the target and the comparison star, and open circles to the magnitude differences between the comparison and check star. 185 l. y. zhu et al. 4 summary one formation method of sdb-type binaries in theory is through a common envelope (ce) phase after the more massive star in the initially detached system evolves into a red giant. the ejection of the ce results in a large amount of angular momentum loss, and then a shortperiod sdb-type binary is formed. in previous section, new results of the three sdb-type eclipsing binaries are introduced. the presence of substellar companions especially the one orbiting nsvs 07826147 with the closest distance will give some constrains on the formation of this type of objects as well as on the interaction between red giants and their companions. to improve the results, more observations are required in the future. acknowledgement this work is supported by chinese natural science foundation (no.11133007 and 11325315) and yunnan natural science foundation (no. 2013fb084). new ccd photometric observations were obtained with the 2.16m and 85-cm telescope at xinglong station, the 2.4m, 1.0-m, and 60-cm telescopes at yunnan observatories in china, and the 2.15-m ”jorge sahade” telescope in argentina. references [1] beuermann, k., breitenstein, p., debski, b., diese, j., dubovsky, p. a., dreizler, s., et al., 2012, a&a 540, 8 [2] castellani, m., castellani, v., 1993, apj, 407, 649 [3] camurdan, c. m., zengin camurdan, d., ibanoǧlu, c., 2012, newa 17, 325 doi:10.1016/j.newast.2011.08.004 [4] charpinet, s., fontaine, g., brassard, p., et al., 2011, natur, 480, 496 doi:10.1038/nature10631 [5] d’cruz, n. l., dorman, b., rood, robert, t., o’connell, r. w., 1996, apj, 466, 359 doi:10.1086/177515 [6] drechsel, h., heber, u., napiwotzki, r., ostensen, r., solheim, j.-e., johannessen, f., schuh, s. l., deetjen, j., zola, s., 2001, a&a 379, 893 [7] for, b. q., et al., 2010, apj, 708, 253 doi:10.1088/0004-637x/708/1/253 [8] hagen, h-j., groote, d., engels, d., & reimers, d. 1995, a&as, 111, 195 [9] han, z. et al., 2002, mnras, 336, 449 [10] han, z. et al., 2003, mnras, 341, 669 doi:10.1046/j.1365-8711.2003.06451.x [11] heber, u., 2009, ara&a, 47, 211 doi:10.1146/annurev-astro-082708-101836 [12] kelley, n., shaw, j. s., 2007, j. southeast. assoc. res. astron. 1, 13 [13] kilkenny, d., 2011, mnras 412, 487 doi:10.1111/j.1365-2966.2010.17919.x [14] kilkenny, d., o’donoghue, d., koen, c., lynas-gray, a. e., van wyk, f., 1998, mnras 296, 329 doi:10.1046/j.1365-8711.1998.01432.x [15] lee,j. w., kim,s.-l., kim,c.-h., et al. 2009,aj, 137, 3181 [16] geier, s., classen, l., brnner, p., et al., 2012, asp conference series vol. 452, 153 [17] morales-rueda, l., et al., 2006, baltic astronomy, 15, 187 [18] qian, s.-b., dai, z.-b., liao, w.-p., zhu, l.-y., liu, l., zhao, e. g., 2009, apj 706, l96 [19] qian, s.-b., zhu, l.-y., dai, z.-b., fernández lajús, e., xiang, f.-y., and he, j.-j., 2012, apj 745, l23 [20] qian, s.-b., shi, g., zola, s., 2013, mnras, in print [21] silvotti, r., 2009, international journal of astrobiology 8, 241 [22] silvotti, r., schuh, s., janulis, r. et al., 2007, natur, 449, 189 [23] zhu, l. y., qian, s. b., 2010, ap&ss, 329, 107 discussion raymundo baptista: light time travel effect is not the only interpretation for physical period changes in binary stars. an alternative is the magnetic activity cycle of the late-type star modulating the binary period. it is hard to believe a planet at 1 au orbit would survive commom envelope phase of a binary which was at comparable separation before. liying zhu: firstly, the cyclic period change caused by light time effect is strictly periodic change in o-c diagram not only quasi-periodic variation aroused 186 http://dx.doi.org/10.1016/j.newast.2011.08.004 http://dx.doi.org/10.1038/nature10631 http://dx.doi.org/10.1086/177515 http://dx.doi.org/10.1088/0004-637x/708/1/253 http://dx.doi.org/10.1046/j.1365-8711.2003.06451.x http://dx.doi.org/10.1146/annurev-astro-082708-101836 http://dx.doi.org/10.1111/j.1365-2966.2010.17919.x http://dx.doi.org/10.1046/j.1365-8711.1998.01432.x close-in substellar companions and the formation of sdb-type close binary stars by the magnetic activity cycle. secondly, in our fiveyears monitor, no asymmetric light curves caused by the magnetic activity for these hw vir binaries were found. their light curves are very stable. thirdly, one of our target sdss j0820+0008 is composed of an sdb star and a brown dwarf, the cyclic change can not be explained by magnetic activity cycles. the detected planet at 1 au orbit may be protected by the engulfment of the low mass stellar companion during the ce phase. and the other possibility is that the planet is the second-generation one. 187 introduction targets and method new results hs0705+6700 ny vir nsvs07826147 summary 178 acta polytechnica ctu proceedings 2(1): 178–182, 2015 178 doi: 10.14311/app.2015.02.0178 the hidden population of am cvn binaries in the sloan digital sky survey p. j. carter1, t. r. marsh1, d. steeghs1, e. breedt1, c. m. copperwheat2, b. t. gänsicke1, p. j. groot3, g. nelemans3,4 1department of physics, university of warwick, coventry cv4 7al 2astrophysics research institute, liverpool john moores university, ic2, liverpool science park, 146 brownlow hill, liverpool l3 5rf 3department of astrophysics/imapp, radboud university nijmegen, po box 9010, 6500 gl nijmegen, the netherlands 4institute for astronomy, ku leuven, celestijnenlaan 200d, 3001 leuven, belgium corresponding author: philip.carter@warwick.ac.uk abstract we present results from a spectroscopic survey designed to uncover am canum venaticorum (am cvn) binaries hidden in the photometric database of the sloan digital sky survey (sdss). the discovery of only 7 new am cvns in the observed part of our sample suggests a lower space density than previously predicted. based on the complete g ≤ 19 sample, we calculate an observed space density for am cvns of (5 ± 3) × 10−7 pc−3. we also compare the cataclysmic variables (cvs) discovered via this survey to those found in the sdss spectroscopy, and we discuss sbss 1108+574, an unusually helium-rich cv that has a spectroscopically confirmed orbital period of 55 minutes, well below the cv period minimum (∼80 min). sbss 1108+574 may represent an am cvn forming via the ‘evolved cv’ formation channel. keywords: cataclysmic variables dwarf novae binaries: close stars: individual: sbss 1108+574. 1 introduction the am canum venaticorum (am cvn) binaries are a rare group of hydrogen-deficient, ultra-compact, masstransferring white dwarf binaries. they have orbital periods in the range 5 – 65 minutes, well below the observed period minimum of hydrogen accreting cataclysmic variables (∼80 min, gänsicke et al. 10). three formation channels have been proposed for the am cvn binaries, each characterised by the donor. the donor can be (1) a second, lower mass, white dwarf – these systems have the shortest minimum periods, beginning mass-transfer at periods as short as a few minutes [9, 22]; (2) a semi-degenerate helium star [12, 31]; or (3) an evolved main sequence star [23, 32, 34, 36]. the third channel is known as the ‘evolved cv’ channel, and has generally been considered to be unimportant in comparison to the double white dwarf and helium star channels. the evolution of these systems is thought to be governed by gravitational wave radiation [e.g. 22], causing the mass accretion rate to be a steeply decreasing function of orbital separation. this gives rise to a strong dependence of their observational properties on the orbital period. the shortest period systems are expected to undergo direct impact accretion, and no disc forms [19, 28]. for systems with 10 . porb . 20 min, the accretion disc is in a stable high-state, with spectra showing helium absorption from the optically thick disc [e.g. 21]. am cvns with periods greater than ∼40 min, are thought to be in a stable low-state, the spectra of these systems are characterised by emission lines from the accretion disc [e.g. 30]. in the intermediate period systems (20 . porb . 40 min), an instability occurs in the accretion disc, and their appearance varies between that of the high-state and the low-state systems, similarly to the hydrogen-rich dwarf novae [14, 24]. in the past 10 years, the known population of am cvns has quadrupled, largely as a result of dedicated surveys using the sloan digital sky survey (sdss; york et al. 37), and the palomar transient factory [16, 17]. here we discuss estimates of the am cvn space density, and results from our spectroscopic survey designed to uncover new am cvn binaries amongst colour-selected objects from the sdss photometric database [6, 25, 29]. 2 the serendipitous sdss am cvns the first am cvn binaries were discovered in a variety of different ways, and only 10 were known prior to 178 http://dx.doi.org/10.14311/app.2015.02.0178 the hidden population of am cvn binaries in the sloan digital sky survey the burst of discoveries over the last decade. roelofs et al. [26] and anderson et al. [1, 2] discovered a total of six new am cvn systems in the sdss spectroscopic database via their helium emission dominated spectra. this provided the first sufficiently complete and homogeneous sample of am cvn systems that a study of the population became possible. roelofs et al. [27] used these ‘serendipitous sdss am cvns’ to estimate the observed space density of am cvn binaries – a crucial quantity for calibration of predictions from binary evolution theory. they calculate the completeness of the sdss spectroscopy as a function of colour and galactic latitude, and using an assumed magnitude distribution for am cvns, determine the number and distribution of systems that would be expected from nelemans et al. [20]’s population synthesis. these numbers are then compared to the number of systems found in the sdss, giving a value for the am cvn space density of 1–3 × 10−6 pc−3, an order of magnitude lower than the expected value at the time (2 × 10−5 pc−3, nelemans et al. 20). roelofs et al. [27]’s study also indicated that there should be at least 50 am cvns in total in the sdss photometry, most of them ‘hidden’ due to the absence of spectroscopic data. 3 the search for the hidden population since the completeness of the sdss spectroscopy in the area of colour space occupied by the am cvns is low, and this area is sparsely populated (see fig. 1), roelofs et al. [29] began a dedicated spectroscopic survey of objects in this region, intended to uncover the ∼40 am cvns that were expected [27]. fig. 1 shows the low density of sources in the sdss photometry in the colour region occupied by the am cvn binaries. also shown are the ∼2000 candidates selected from the sdss dr7 database by applying the colour cuts given in roelofs et al. [29]. our targeted region of colour space selects those am cvns with emission line spectra – the longer period systems. as am cvns should spend only a few percent of their lifetime as mass-transferring systems at orbital periods below 30 minutes, our selection should include the vast majority of am cvns in the sdss footprint [6]. this region of colour space is also occupied by db white dwarfs, which are the most significant contaminant in our survey. to date we have taken low-resolution, low signal-tonoise ratio spectra of ∼70% of these candidates, uncovering 30 cvs and 7 new am cvns (see carter et al. 6 for more details). −0.5 −0.4 −0.3 −0.2 −0.1 0.0 0.1 0.2 g− r −0.4 −0.2 0.0 0.2 0.4 u − g figure 1: the greyscale represents the density of sources in the sdss photometric database as a function of colour, to a limiting magnitude g = 20.5 (dereddened). the long period sdss am cvn binaries are indicated by star symbols. the solid line marks the blackbody cooling track, the dotted and dot-dashed lines indicate model cooling sequences for da and db white dwarfs. the dashed lines indicate the colour cuts given by roelofs et al. [29], and the dots indicate the candidates selected. 4 the cv population spectra of the cvs discovered in our survey were presented in carter et al. [6]. we compare this sample to the sdss cv population [33, these proceedings] by plotting the equivalent widths (ews) of their hα and he i 5875 emission lines, see fig. 2. the distributions of the two populations appear similar, with the strongest hα emitters falling outside our survey colour box. there are two obvious outliers visible in fig. 2, css 1122-1110 (sdss j1122-1110; breedt et al. 5) from the sloan sample, and sbss 1108+574 (sdss j1111+5712; carter et al. 7) from our sample, both having much stronger helium emission compared to hydrogen than the majority of cvs. the porb = 59 min cv, v485 cen [3] is also shown in fig. 2 for comparison. followup phase-resolved spectroscopy of sbss 1108+574 reveals an orbital period of 55.3± 0.8 minutes [7], consistent with independent photometric and spectroscopically determined periods [13, 18]. this is clear evidence for the evolved nature of the donor, which has been stripped of most of its hydrogen by, or prior to the onset of, mass-transfer. sbss 1108+574 and the similar systems, css 1122179 p. j. carter et al. 1110 [5] and css 1740+4147 (chochol et al., these proceedings), may be evolving along the ‘evolved cv’ evolutionary pathway toward am cvn binaries. 1:1 2:1 3:1 −100 −80 −60 −40 −20 0 ew he i 5875(å) −350 −300 −250 −200 −150 −100 −50 0 e w h α (å ) css1122 sdssj0804 sbss1108 v485cen figure 2: ew of he i 5875 versus hα for our cv sample (triangles), and the cv population from the sdss (crosses). the star symbols represent the am cvns from our sample, which fall on the ew(hα) = 0 line. also plotted are lines showing hα to he i 5875 ew ratios; cvs with unusually low ew ratios are labelled, v485 cen is shown for comparison. the position of the am cvn sdss j0804+1616 is due to strong he ii 6559 emission. 5 the am cvn space density roelofs et al. [27]’s observed space density, 1–3 × 10−6 pc−3, corresponds to ∼40 am cvns in our survey sample. we have found 7 new am cvns in the ∼70% of the sample that has been observed, suggesting that either there is some bias that we have not considered, or the space density is lower than previously estimated. biases in the survey are discussed in detail by roelofs et al. [29] and carter et al. [6]. they show that due to the distribution in colour space of the spectroscopic observations from the sdss, it is unlikely that a large number of am cvns lie outside the selected colour box. there is a slight bias in our survey observations towards the easier to observe brighter objects, but there is no significant colour bias, and the edges of our colour box are well explored. we therefore consider it likely that a lower space density is required to explain our results. since our survey is essentially complete down to a gband magnitude of 19, we use this smaller sample to recalibrate the population synthesis results. following the method described in roelofs et al. [27] we calculate the expected magnitude distribution of am cvn binaries in the sdss photometric database. the roelofs et al. [27] space density corresponds to 11 am cvns with g ≤ 19. in our essentially complete to g = 19 sample there are 4 known am cvns, scaling the space density to match this number, we obtain a value of (5 ± 3) × 10−7 pc−3 [6]. 6 summary the sdss has significantly increased both the numbers of am cvn stars known, and our understanding of the population. our spectroscopic survey of colourselected objects from the sdss photometric database has uncovered a further seven new am cvns. we have also identified a helium-rich cv, sbss 1108+574, follow-up observations of which reveal an orbital period of 55 minutes, well below the cv period minimum. sbss 1108+574 and similar helium-rich systems may be examples of am cvns forming via the ‘evolved cv’ pathway. discovering only seven new am cvns in the observed sample likely indicates a significantly lower space density than previously predicted. we use the essentially complete, brighter part of our sample to estimate the observed space density to be (5 ± 3) × 10−7 pc−3. acknowledgement pjc is grateful to f. giovannelli and the organisers for the invitation to attend this workshop. funding for sdss-iii has been provided by the alfred p. sloan foundation, the participating institutions, the national science foundation, and the u.s. department of energy office of science. the sdssiii web site is http://www.sdss3.org/. fig. 1 makes use of p. bergeron’s synthetic white dwarf colours [4, 11, 15, 35], kindly made available by the authors at http://www.astro.umontreal.ca/∼bergeron/cooling models. references [1] anderson, s. f., et al., 2005, aj, 130, 2230 [2] anderson, s. f., et al., 2008, aj, 135, 2108 [3] augusteijn, t., van kerkwijk, m. h., van paradijs, j., 1993, a&a, 267, l55 [4] bergeron, p., et al., 2011, apj, 737, 28 [5] breedt, e., et al., 2012, mnras, 425, 2548 [6] carter, p. j., et al., 2013, mnras, 429, 2143 180 the hidden population of am cvn binaries in the sloan digital sky survey [7] carter, p. j., et al., 2013, mnras, 431, 372 doi:10.1093/mnras/stt169 [8] espaillat, c., et al., 2005, pasp, 117, 189 doi:10.1086/427959 [9] faulkner, j., flannery, b. p., warner, b., 1972, apj, 175, l79+ [10] gänsicke, b. t., et al., 2009, mnras, 397, 2170 doi:10.1111/j.1365-2966.2009.15126.x [11] holberg, j. b., bergeron, p., 2006, aj, 132, 1221 [12] iben, jr., i., tutukov, a. v., 1987, apj, 313, 727 [13] kato, t., et al., 2013, pasj, 65, 23 [14] kotko, i., et al., 2012, a&a, 544, a13 [15] kowalski, p. m., saumon, d., 2006, apj, 651, l137 doi:10.1086/509723 [16] levitan, d., et al., 2011, apj, 739, 68 doi:10.1088/0004-637x/739/2/68 [17] levitan, d., et al., 2013, mnras, 430, 996 doi:10.1093/mnras/sts672 [18] littlefield, c., et al., 2013, aj, 145, 145 [19] marsh, t. r., steeghs, d., 2002, mnras, 331, l7 doi:10.1046/j.1365-8711.2002.05346.x [20] nelemans, g., et al., 2001, a&a, 368, 939 [21] o’donoghue, d., et al., 1994, mnras, 271, 910 doi:10.1093/mnras/271.4.910 [22] paczyński, b., 1967, acta astron., 17, 287 [23] podsiadlowski, p., han, z., rappaport, s., 2003, mnras, 340, 1214 doi:10.1046/j.1365-8711.2003.06380.x [24] ramsay, g., et al., 2012, mnras, 419, 2836 doi:10.1111/j.1365-2966.2011.19924.x [25] rau, a., et al., 2010, apj, 708, 456 doi:10.1088/0004-637x/708/1/456 [26] roelofs, g. h. a., et al., 2005, mnras, 361, 487 doi:10.1111/j.1365-2966.2005.09186.x [27] roelofs, g. h. a., nelemans, g., groot, p. j., 2007, mnras, 382, 685 doi:10.1111/j.1365-2966.2007.12451.x [28] roelofs, g. h. a., et al., 2010, apj, 711, l138 doi:10.1088/2041-8205/711/2/l138 [29] roelofs, g. h. a., et al., 2009, mnras, 394, 367 doi:10.1111/j.1365-2966.2008.14288.x [30] ruiz, m. t., et al., 2001, apj, 552, 679 doi:10.1086/320578 [31] savonije, g. j., de kool, m., van den heuvel, e. p. j., 1986, a&a, 155, 51 [32] sienkiewicz, r., 1984, acta astron., 34, 325 [33] szkody, p., et al., 2011, aj, 142, 181 [34] thorstensen, j. r., et al., 2002, apj, 567, l49 [35] tremblay, p.-e., bergeron, p., gianninas, a., 2011, apj, 730, 128 [36] tutukov, a. v., et al., 1985, soviet astronomy letters, 11, 52 [37] york, d. g., et al., 2000, aj, 120, 1579 discussion nataly katysheva: do you classify sbss 1108+574 as an am cvn or an su uma star? philip carter: we do not classify sbss 1108+574 as an am cvn because the am cvn classification is classically applied only to objects in which no hydrogen is seen; we decided to refer to it simply as a helium-rich cv. since this system is clearly below the cv period minimum it does not seem entirely appropriate to group it with normal cvs either. whilst it is not certain whether it will become sufficiently hydrogen-depleted to become a ‘true’ am cvn, it is clear that sbss 1108+574 and similar systems lie between the classical definitions of these two classes. koji mukai: is your survey sensitive to am cvn systems with high-state discs, which would have absorption lines, or to direct impact accretors? philip carter: es ceti is a border-line direct impact accretor, showing emission lines [8], and does fall within our colour box. we would have been able to detect systems similar to es cet. those systems showing absorption lines from a high-state disc would appear indistinguishable from db white dwarfs at the low s/n employed in our survey, and so we are not sensitive to them. however, such systems are expected to be a small minority of the total population, and our conclusion about the space density takes this into account. christian knigge: i know the numbers are still small, but have you started to look at the period and magnitude distribution of your systems and checked how they compare to the theoretical predictions? 181 http://dx.doi.org/10.1093/mnras/stt169 http://dx.doi.org/10.1086/427959 http://dx.doi.org/10.1111/j.1365-2966.2009.15126.x http://dx.doi.org/10.1086/509723 http://dx.doi.org/10.1088/0004-637x/739/2/68 http://dx.doi.org/10.1093/mnras/sts672 http://dx.doi.org/10.1046/j.1365-8711.2002.05346.x http://dx.doi.org/10.1093/mnras/271.4.910 http://dx.doi.org/10.1046/j.1365-8711.2003.06380.x http://dx.doi.org/10.1111/j.1365-2966.2011.19924.x http://dx.doi.org/10.1088/0004-637x/708/1/456 http://dx.doi.org/10.1111/j.1365-2966.2005.09186.x http://dx.doi.org/10.1111/j.1365-2966.2007.12451.x http://dx.doi.org/10.1088/2041-8205/711/2/l138 http://dx.doi.org/10.1111/j.1365-2966.2008.14288.x http://dx.doi.org/10.1086/320578 p. j. carter et al. philip carter: we have not yet investigated this in detail, and there are still a few systems for which we do not yet have an orbital period. in a magnitude limited sample, the expected period distribution peaks at ∼50 min, with approximately similar numbers above and below this peak [27]. we have found more systems in the sdss with periods below 50 min, than above, but the numbers are still too small to draw any strong conclusion from this. 182 introduction the serendipitous sdss am cvns the search for the hidden population the cv population the am cvn space density summary acta polytechnica ctu proceedings doi:10.14311/app.2017.13.0043 acta polytechnica ctu proceedings 13:43–48, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app non-invasive inverse problem in civil engineering jan havelka∗, jan sýkora, anna kučerová czech technical university in prague, faculty of civil engineering, thákurova 2077/7, 166 29 prague 6, czech republic ∗ corresponding author: jan.havelka.1@fsv.cvut.cz abstract. in this contribution we focus on recovery of spatial distribution of material parameters utilizing only non-invasive boundary measurements. such methods has gained its importance as imaging techniques in medicine, geophysics or archaeology. we apply similar principles for non-stationary heat transfer in civil engineering. in oppose to standard technique which rely on external loading devices, we assume the natural fluctuation of temperature throughout day and night can provide sufficient information to recover the underlying material parameters. the inverse problem was solved by a modified regularised gauss-newton iterative scheme and the underlying forward problem is solved with a finite element space-time discretisation. we show a successful reconstruction of material parameters on a synthetic example with real measurements. the virtual experiment also reveals the insensitivity to practical precision of sensor measurements. keywords: calderón problem, finite element method, boundary inverse method, neumann-todirichlet map, heat transfer. 1. introduction non-invasive methods are gaining increasing interest in various disciplines spanning from medicine to geophysics. the main advantage of such methods is that they preserve the observed sample intact while getting information about its inner properties. such tasks can therefore play fundamental role in analysis of existing structures, improving future design, minimising the gap between model prediction and real observations etc. moreover today trend is in favour of complex models described by multiple parameters which have to be properly identified from real measurements, often requiring a specially designed set destructive tests with a high precision laboratory equipment. such process often requires a set of samples which do not have to be available and features a rather limited description of the studied material. in this contribution we propose a non-invasive parameter identification technique based merely on boundary observations of some structure. this idea was inspired by a medical imaging technique named electric impedance tomography (eit). the mathematical procedure was first rigorously described by an argentinian mathematician alberto calderón in his foundational paper [1] in 1980, although the idea was studied earlier in 1930 in geophysics [2, 3]. the goal of eit is to recover an electric conductivity field inside some domain using only boundary measurements. basic idea of this method lies in the difference of surface measurements due to variations in the subsurface conductivity distribution. meanwhile a single set of surface measurements for a given loading conditions might result in a number of possible conductivity fields, calderón surpassed this problem by sequentially implying multiple loading conditions each followed by a measurement, which in essence has the potential to contain the complete information about the underlying conductivity distribution. in this contribution we will employ similar techniques of calderón inverse problem paradigm to a parabolic partial differential equation with two independent parameters to describe thermal properties of some structure. our method is designed to be external loading-free, i.e. it completely relies on the environmental factors as a source of changes which are necessary in order to identify the material inside a domain. 2. inverse problem parameters recovery of a given model is often regarded to as ill-posed problem [4, 5]. for such task it is typical that even a small perturbation in the input data can result into a large variation in the solution. this can be due to several reasons e.g. uniqueness issues stemming from information shortage, i.e. data insufficiency or it can be an intrinsic property of the system itself. for this reason needs a stabilization provided by additional assumptions, e.g. some prior information, enforcing smoothness, preferring solution with the smallest norm, provide bounds to the unknown entity, etc. procedures for determining the constrains for solving such problems are generally called regularisation methods and within this contribution we shall employ a deterministic approach. an inverse problem is usually an optimization task solved by minimising some functional which is often stated as follows, with the first term representing the cost function and the second term being the regularisation penalty θ̃ = arg min θ ‖f (θ)− um‖p +g(θ), (1) 43 http://dx.doi.org/10.14311/app.2017.13.0043 http://ojs.cvut.cz/ojs/index.php/app j. havelka, j. sýkora, a. kučerová acta polytechnica ctu proceedings where f (θ) is output of the forward operator, um is the vector of measured quantity, p indicates `p-norm, g(θ) is the regularisation functional introducing the additional constrains to the solution and θ̃ are the parameter fields being reconstructed. a typical choice of the regularisation penalty term in (1) is of following form [4] g(θ) = λ2‖l(θ − θr)‖2`2 , (2) where the hyper-parameter, λ controls the trade-off between solution stability, given constrains and a distance from the actual solution. additional parameters θr represent some a priori known and possibly non-smooth behaviour of the unknown parameters [6]. a straightforward way of explaining the regularisation operator l is such that it draws the solution towards its null space, i.e. ker(l). in our case it takes a form of a discrete approximation to the laplacian. in this contribution, both terms in (1) were chosen to be `2-norm due to the convenience for computational purposes and preference of smooth solutions [7]. in such case, by combining the minimisation scheme (1) for p = 2, penalty term (2) and a gauss-newton approximation of newton-raphson multi-variable method, one can obtain a following iterative formula [6] θk+1 = θk + δθk, (3) δθk = ( jtk jk + λ2r )−1 (jtk δu− λ2r (θk − θr) ) , (4) where jk is the jacobian evaluated at θk, δu is a vector containing the difference between the model output and real measurements, θr is a conductivity field containing its prior assumptions and r = ltl is regularisation operator composed from a pre-calculated laplacian l of a piece-wise constant functions on a finite element mesh. δu = ur − f (θk) , (5) where f (θ) ∈ rvw represents a discrete neumann-todirichlet operator of a forward model with v being the number of measurement points, i.e. a number of nodes of fe mesh on a subset γv of boundary ∂ω that is being observed and w is the number of experiments. the a priori measured quantity is stored in vector ur ∈ rvw. in all cases the reference field θr(x) = θ0(x) = 1 for x ∈ ω. from our experience, the most stable and simple choice of hyper-parameter λk is the one utilized by levenberg-marquardt regularisation (lmr) [8], which is gradually decreasing the parameter during iteration and takes following form λk = max ( max ( jtk jk )) . (6) jacobian jk is updated in each iteration and was calculated numerically in a following way j (jkl) i = ∂ujk ∂θli , (7) where ji is the third-order tensor in i-th iteration, indexes jk are representing measurement nodes in a finite element mesh and individual measurements respectively. index l denotes a conductivity change on l-th fe element. the tensor is calculated numerically and matricised along indexes jk for convenience of calculation purposes. in general θ can represent multiple parameter fields and in such case equations (3) to (7) are evaluated for each parameter individually. additional numerical treatment the iteration scheme (3) does not include any supplementary constrains which provide the solver robustness. therefore one have to adopt further numerical treatment to maintain the assumptions 1 and 2 valid within the iteration. introduction of the following two operators increased the stability and robustness of results substantially. the constrain for strict positivity of conductivity field during the iteration is treated with an ad-hoc algorithm which is not allowing the occurrence of negative numbers in the solution and gives rise to a positivity operator, i.e. tp in a following way tp(θ(x)) = { θ(x) > 0→ x+, θ(x+) = θ(x+), θ(x) < 0→ x−, θ(x−) = min(θ(x+)). (8) since the problem is inherently non-linear and the iteration scheme proceeds with non-restricted linear steps we introduce a cap operator tc limiting the resulting step size to a chosen value k in a following way tc(θ(x)) = { θ(x) > k, θ(x) = sign(θ(x)) · k, θ(x) < k, θ(x) = θ(x). (9) the final modified gn iteration scheme after applying (8) and (9) operators to (3) then takes following form θk+1 = tp (θk + tc (δθk)) . (10) 3. transient model since the numerical model is repeatedly used in each iteration of (10) it plays a fundamental role in the entire inverse procedure. in our case it will to some extent also substitute an actual experiment. numerical solution is obtained using finite element method space-time discretisation [9–12]. the main idea of employing the calderón’s technique is created upon foundational research conducted by k. s. chen [13] in 1989, who proposed and experimentally validated so called complete electrode model (cem) which allows to consider electrodes actual physical size and introduces a contact impedance layer 44 vol. 13/2017 non-invasive inverse problem in civil engineering between the skin and the electrode. further proof for cem solution uniqueness was given by e. somersalo, et al. in 1992 [14]. significant contributions to the theory were papers [15, 16] proving the solution is uniquely determined in dimension n ≥ 3 for complete dirichlet-to-neumann or neumann-to-dirichlet data. unlike in n ≥ 3, in dimension n = 2 the problem is undetermined and the solution was proved to be unique up to a change of coordinates [17, 18]. specific choice of this model is motivated by real application on historical and other structures, where the standard procedure of taking samples is too difficult or the structure should not be weakened or damaged. also in real conditions it is not an easy task to sustain a stable and steady state conditions. not only the surrounding temperature will fluctuate even in a laboratory environment, but for standard building materials like bricks, concrete, wood, etc. the steady state, after changing the loading conditions, can be reached after several hours or days depending on the volumetric capacity, heat conductivity and material thickness. therefore, we intend to apply the identical principles used in a calderón problem for transient models. to capture a time dependent heat transfer, one can adopt following set of equations ρs(x)cp(x)∂u ∂t (x, t)−∇ · (λs(x)∇u(x, t)) = f̃(x, t), n(x) · (λs(x)∇u(x, t)) = f̃n (x, t), α(i)(u(x, t)− u0(x, t)) = f̃t (x, t), u(x, t) = f̃d(x, t), t > 0, ∂ω(i) = ∂ω(i) n ∪ ∂ω(i) t ∪ ∂ω(i) d , i = 1, . . . , i, (11) where ρs is volumetric mass density, cp is specific heat capacity and ∂ω(i) (n,t,d) are disjoint subsets of boundary ∂ω(i) in i-th loading condition with corresponding environmental factors u0, α(i) and f̃n,t,d. in order to maintain neumann-to-dirichlet sensing and uniqueness of the inverse problem, the set of equations in (11) is subjected to following constrain assumption 1. let γm be a subset of boundary ∂ω that is subjected to measurements. then ψ = ( ∂ω(i) n ∪ ∂ω(i) t ) : (ψ ∩ γ) /∈ ∅, ∀i, must hold, i.e. the boundary subjected to measurements must contain at least some neumann conditions. another set of constrains similar to the ones in [14] is represented by following assumptions assumption 2. the material parameters λs, ρs, cp and transfer coefficients α(i) satisfy following (i) λs ∈ l∞(ω;r), inf x∈ω λs(x) = λ+ s > 0, (ii) 0 < ρ−s ≤ ρs ≤ ρ+ s <∞, (iii) 0 < c−p ≤ cp ≤ c+p <∞, (iv) 0 < α (i) − ≤ α(i) ≤ α(i) + <∞, ∀i. in a definition of this model (11), one can notice that there is no mention of electrodes, thermocouples or measurements indicating our intention not to consciously intervene in the system itself, but only to rely on external influences and natural fluctuation of temperature throughout the day and night. for systems where their boundaries ∂ω are not exposed to different external influences, one can adapt a similar techniques to complete electrode model, i.e. to attach a device that can excite a different boundary conditions, or control the ambient temperature in the second or third condition in equation (11). a special feature of this model lies in its independence on excitation device, i.e. stimulation electrodes or thermocouples, and therefore has the least requirements on equipment and the full measurement setup consists of arrays of thermometers and/or thermal cameras. numerical solution of the forward model the forward operator f consists of two independent parameters and solves the system for all time steps nt at once, giving rise to a following formulation f (λs, cv) = um, um ∈ rm ·nt , (12) where the inputs are heat conductivity λs and volumetric capacity cv = ρs · cp. the measurement matrix um ∈ rm ·nt , where m is number of measurements within single time step and nt is number of time steps, is obtained as a subset of complete solution vectors ui, i = 1, . . . nt from a following set of linear equations kcui+1 = ( kc −∆tk̃ ) ui−1 + . . . ∆t ( (1− τ)f̃n,i−1 + τ f̃n,i ) + . . . ∆t ( (1− τ)f̃t,i−1 + τ f̃t,i ) + . . . ∆t ( (1− τ)f̃d,i−1 + τ f̃d,i ) , (13) k̃ = k + kt, (14) kc = c + τ∆tk̃, (15) where ∆t = ti+1− ti is a time step, τ ∈ 〈0; 1〉 is a time integration parameter1 and the system matrices and right hand side vectors are computed in a following way kkl = ∫ ω λs∇φk · ∇φl da k, l = 1 . . . n, (16) 1the foregoing computations were calculated using cranknicolson integration method, i.e. τ = 0.5 45 j. havelka, j. sýkora, a. kučerová acta polytechnica ctu proceedings ckl = ∫ ω ρscpφkφl da k, l = 1 . . . n, (17) kt,kl = ∫ ∂ωt αφkφl ds k, l = 1 . . . n, (18) f̃t,li = ∫ ∂ωt αu0,iφl ds i = 1 . . . nt, l = 1 . . . n, (19) f̃n,li = − ∫ ∂ωn f̃n (ti)φl ds i = 1 . . . nt, l = 1 . . . n, (20) f̃d,i = − (k + kt) f̃d(ti) i = 1 . . . nt. (21) for detailed information and derivation of individual terms, the interested reader is referred to [9–12] and literature therein. 4. results we consider two finite element meshes for each physical domain, i.e. one is used to simulate real measurements and the second is used for the reconstruction algorithm. both finite element meshes are shown on figure 1. further improvements were made by integrating measurement errors in the calculation, specifically we assumed only the direct measured quantity is subjected to errors in a following way ume = um + ε, (22) where ume is some measured quantity with the error included, um is its true value and ε ∼ n ( µ, σ2) is the error. we assume the sensor is calibrated and its deviation is known to fall within 3·σ region, i.e. µ = 0 and deviation dm = 0.25 oc given by manufacturer implies σ = dm/3. all the sensor errors are considered to be mutually independent and identically distributed random variables, although using thermal camera would rather impose spatially correlated random variables forming a random field. figure 1. finite elements meshes: coarse (top) and fine (bottom). observed boundary γm depicted in red colour, where m = 122 nodes of finite element mesh being measured. we assume changes in temperature on the observed boundary over several days can provide sufficient amount of data for the algorithm to recover material fields θ = [λs; cv], i.e thermal conductivity and volumetric capacity respectively. in case the observed structure is located in an environment without sufficient changes in loading conditions, one may use a device that excites a different boundary conditions, e.g. a heater or air conditioning system. the measure of reconstruction algorithm performance is represented by an error on the reconstructed material field in comparison to the original field in a following way εθi = ‖θi,r − θi,o‖2 ‖θi,o‖2 , (23) where θi,r is the i-th recovered material field obtained from (10) and θi,o is the i-th original material field. in order to simulate a natural environment conditions and capture temperature fluctuations in the interior and exterior, we use a realistic measurements shown on figure 2. the environment was in total monitored for eleven consecutive days at minute intervals. for the calculation purposes data were further sparsified to one hour intervals which satisfy both sufficient precision in describing the temperature curve and reasonable computational load. boundary conditions were set accordingly to figure 2 as follows 46 vol. 13/2017 non-invasive inverse problem in civil engineering figure 2. interior and exterior temperatures. preceding temperature in grey, actual observation period in colour. λ ∂u ∂n (x, t)|∂ω1 = 10 · (u(x, t)− t1(t)) , λ ∂u ∂n (x, t)|∂ω2 = 10 · (u(x, t)− t2(t)) . (24) the magnitude of reference fields were set according to regular building materials, i.e. λr = 1 [ w m−1 k−1 ], cv,r = 1× 106 [ j m−3 k−1 ]. (25) in figure 2, the measurement starts from day two and the observation period lasts 9 day. measurement is taken every hour which yields into 216 measurements of boundary γ122 = ⋃2 i=1 ∂ωi. for purpose of this contribution a set of 500 realisations of measured temperatures was given to the reconstruction algorithm. resulting mean and standard deviation of reconstructed fields are displayed on following figures 5. conclusions in oppose to eit where the crucial part of successful material field recovery is a precise placement of measurement electrodes together with boundary shape and knowledge of loading conditions2, in our application the problems might arise from insufficient environmental factors variability leading to imperfections and unwanted artefacts in the reconstructed fields. this can be identified although it can be remedied by a use of an external devices providing different boundary conditions. in a simple case shown on figures 3 and 4 one can observe the possibility of recovering material parameters of such system in the first place. the difference between figures 3a and 4a shows that the variation of temperature in time was not sufficient to fully reconstruct the volumetric capacity field cv resulting into higher reconstruction error of e[εcv ] = 0.2641 in oppose to e[ελs ] = 0.1414. looking closer at deviations of errors std[εcv ] = 0.0014 and std[ελs ] = 0.0017 2especially in eit, where the electrodes are placed on a human body, the boundary shape and electrodes are in continuous motion as the patient breath and move. (a) . e[ελs ] = 0.1414 [-] (b) . std[ελs ] = 0.0017 [-] figure 3. mean (a) and standard deviation (b) of reconstructed conductivity field. in grey: original field, in colour: reconstructed field. one can notice the insensitivity of reconstruction algorithm to induced error on measurements which can be also seen by comparing the magnitudes of plots 47 j. havelka, j. sýkora, a. kučerová acta polytechnica ctu proceedings (a) . e[εcv ] = 0.2641 [-] (b) . std[εcv ] = 0.0014 [-] figure 4. mean (a) and standard deviation (b) of reconstructed capacity field. in grey: original field, in colour: reconstructed field. in figures 3a and 3b or 4a and 4b, i.e. the standard deviation is in both cases approximately two orders of magnitude lower than the mean. our intention is then to extend the existing model with imperfections or errors on all the other levels, i.e. uncertainty in ambient temperature, transfer coefficient or a geometrical level inaccuracies. acknowledgements the financial support of this research by the ga15-07299s and sgs17/042/ohk1/1t/11 is gratefully acknowledged. references [1] a. p. calderón. on an inverse boundary value problem. computational & applied mathematics 25:133 – 138, 2006. [2] l. b. slichter. the interpretation of the resistivity prospecting method for horizontal structures. physics 4(9):307–322, 1933. doi:10.1063/1.1745198. [3] r. e. langer. an inverse problem in differential equations. bulletin of the american mathematical society 39(10):814–820, 1933. [4] m. vauhkonen. electrical impedance tomography and prior information. phd thesis, kuopio university, 1997. [5] a. kirsch. an introduction to the mathematical theory of inverse problems. applied mathematical sciences 120. springer-verlag new york, 2nd edn., 2011. [6] d. s. holder. electrical impedance tomography: methods, history and applications. series in medical physics and biomedical engineering. taylor & francis, 1st edn., 2004. [7] y. mamatjan, a. borsic, d. grsoy, a. adler. experimental/clinical evaluation of eit image reconstruction with `1 data and image norms. journal of physics: conference series 434(1):012078, 2013. [8] h. niu, p. guo, l. ji, et al. improving image quality of diffuse optical tomography with a projection-error-based adaptive regularization method. optics express 16(17):12423–12434, 2008. [9] k. j. bathe. finite element procedures. klaus-jurgen bathe, 2006. [10] t. j. r. hughes. the finite element method: linear static and dynamic finite element analysis. courier corporation, 2012. [11] g. strang, g. j. fix. an analysis of the finite element method, vol. 212. prentice-hall englewood cliffs, nj, 1973. [12] o. c. zienkiewicz, r. l. taylor. the finite element method, vol. 3. mcgraw-hill london, 1977. [13] k. s. cheng, d. isaacson, j. c. newell, d. g. gisser. electrode models for electric current computed tomography. ieee transactions on biomedical engineering 36(9):918–924, 1989. doi:10.1109/10.35300. [14] e. somersalo, m. cheney, d. isaacson. existence and uniqueness for electrode models for electric current computed tomography. siam journal on applied mathematics 52(4):1023–1040, 1992. doi:10.1137/0152060. [15] r. m. brown, g. a. uhlmann. uniqueness in the inverse conductivity problem for nonsmooth conductivities in two dimensions. communications in partial differential equations 22(5-6):1009–1027, 1997. doi:10.1080/03605309708821292. [16] j. sylvester, g. uhlmann. a global uniqueness theorem for an inverse boundary value problem. annals of mathematics 125(1):153–169, 1987. [17] j. sylvester, g. uhlmann. a uniqueness theorem for an inverse boundary value problem in electrical prospection. communications on pure and applied mathematics 39(1):91–112, 1986. doi:10.1002/cpa.3160390106. [18] a. i. nachman. global uniqueness for a two-dimensional inverse boundary value problem. annals of mathematics 143(1):71–96, 1996. 48 http://dx.doi.org/10.1063/1.1745198 http://dx.doi.org/10.1109/10.35300 http://dx.doi.org/10.1137/0152060 http://dx.doi.org/10.1080/03605309708821292 http://dx.doi.org/10.1002/cpa.3160390106 acta polytechnica ctu proceedings 13:44–49, 2017 1 introduction 2 inverse problem 3 transient model 4 results 5 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.8.0014 acta polytechnica ctu proceedings 8:14–16, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app batio3 films deposited onto tinb and ti substrates amount and stability of barium kamila moriováa, zdeněk toldeb, přemysl vaněkc, vladimír starýb, václav nehasila,∗ a faculty of mathematics and physics, charles university, v holešovičkách 2, 180 00 prague 8, czech republic b department of materials engineering, faculty of mechanical engineering, czech technical university in prague, karlovo náměstí 13, 121 35 prague 2, czech republic c institute of physics of the czech academy of sciences, na slovance 1999/2, 182 00 prague 8, czech republic ∗ corresponding author: nehasil@mbox.troja.mff.cuni.cz abstract. batio3 films deposited onto tinb and ti substrates using hydrothermal synthesis method were studied in the presented work. these films are supposed to improve properties of bone implants due to their ferroelectric behaviour, because ferroelectrics induce improved bone formation. a great question is the chemical stability of the used material. it can be crucial for its biocompatibility and possible in vivo application. we studied chemical composition of prepared samples, especially concentration of ba and ti and trends of these concentrations stimulated by a solution saline action. the ba and ti concentrations were determined by xps under ultra high vacuum condition. the batio3 films were investigated as received after the preparation procedure as well as after a long time treatment in solution saline. every sample was introduced to the solution saline at first for 1 and later for 3 weeks. ti concentration almost does not change during our experiments while a meaningful ba decrease is observed. nevertheless, barium release seems to slow down with respect to the time of solution saline action. stability of barium titanate films in a period of several months and an absolute amount of the released barium will be a subject of the next research. keywords: barium titanate, xps, concentration, stability. 1. introduction barium titanate could be a promising material for the development of bone implants. this material exhibits ferroelectric properties. if it is polarised, it can improve the bone adhesion to the implant [1–3]. chemical elements included in barium titanate are biocompatible except for barium which is toxic. we studied chemical composition of thin barium titanate film deposited onto titanium and titanium-niobium alloy substrates using xps method. we have determined the chemical composition of as prepared samples and after their treatment in solution saline. barium release is observed and discussed. 2. experimental barium titanate films deposited onto tinb or ti substrates were prepared by hydrothermal synthesis. samples were in the form of discs of 10-14 mm diameter and thickness 0.5-1.4 mm. using calotest, thickness of deposited films was estimated to be about 1-2 µm . before the preparation of barium titanate films, the substrates were cleaned (ultrasonic cleaning in acetone, etching in 6m hcl) and annealed in oxygen at 500 ◦c for 24 hours. after this procedure, the substrate surface is covered by a tio2 rutile layer. barium titanate films were prepared in an autoclave with a teflon inlet by the hydrothermal reaction of tio2 and ba(oh)2 at 250 ◦c for 6 weeks. using this procedure, two sets of batio3 films deposited onto tinb and one set deposited onto ti substrates were prepared. these sets are marked batio3/tinb 1st and 2nd series and batio3/ti, respectively. because the batio3 films within a given set were prepared in the same run under completely identical conditions, they are identical so only one sample from every set was analysed by xps. before xps measurement, the samples were not specially cleaned except brief rinsing in ethyl alcohol. xps measurements were performed in an ultrahigh vacuum chamber with a base pressure better than 1 × 10−9 torr. system is evacuated by titanium ion getter pump and equipped by a quick sample load lock. working pressure inside of the vacuum system is monitored by a bayard-alpert manometer (varian) and remained about 3 × 10−9 torr during xps measurements. dual anode (al and mg) xray source (vg) and hemispherical electron energy analyser (omicron ea -125) equipped with a 5 channel multiplier detector were used to acquire xp spectra. as a primary radiation, al-kα line of 1486.6 ev energy was used. distance between the x-ray source and the samples was about 1 cm. composition of the barium titanate films was determined using the method of relative sensitivity factors. the obtained data describe the surface film of the depth of about 2 − 4 × 10−9 m, 14 http://dx.doi.org/10.14311/app.2017.8.0014 http://ojs.cvut.cz/ojs/index.php/app vol. 8/2017 batio3 films deposited onto tinb and ti substrates figure 1. photoelectron spectrum batio3 on tinb substrate after preparation of sample. visible peaks (photoelectron as well as auger) are marked, those used to calculation of element concentration are in bold. the relative uncertainty of calculated concentrations should not exceed 20 % of the particular value. the as prepared samples were characterised by means of xps and consequently introduced to the solution saline (0.9 mg of nacl in 100 ml of solution) to check the stability of the batio3 films in a physiological-like environment. the solution saline was temperature-stabilized at 38 ◦c, kept under ambient atmosphere and protected against dust and other impurities. the main goal of this treatment was to observe a potential release of ba. the samples remained in the solution saline for 7 days. after this period, their composition was checked by xps to determine any possible changes. subsequently they were re-introduced to a fresh solution saline for next 3 weeks and measured by xps once more. after every treatment procedure in the solution saline, the samples were rinsed in distilled water. 3. results and discussion typical electron spectrum of batio3 is presented in figure 1. this particular spectrum was obtained for the barium titanate deposited onto tinb within the first series. we can recognise peaks of ba, ti, o, and c. nb peaks are also visible in the spectrum. they originate from the tinb substrate. taking into account the thickness of the barium titanate films, their origin is not clear and is subject of further investigation. a segregation of niobium on the surface or non-completely continuous batio3 films would explain this observation. moreover, different samples contain various amounts of carbon. we assume its quantity is influenced by the transfer time between the preparation of the samples and the xps measurements, by storage conditions etc. it is, however, out of the scope of this contribution to discuss the chemical forms and concentrations of all the involved elements, we will restrict our discussion figure 2. decrease of barium concentration due to an action of solution saline. only to the barium content with respect to titanium and oxygen. oxygen is present in more chemical forms and some of them are obviously included in carbon species. therefore we only used the so-called lattice oxygen for our calculation of the barium content. it is the oxygen chemically bonded within batio3. after fitting o 1s peak, it can be recognised at the binding energy of about 529.5 ev, according to ref. [4], where electron spectra of batio3 powders exhibit similar features as ours. the change in the amount of barium is crucial indicator in this study. in figure 2, relative amount of barium with respect to the total amount of ba, ti, and lattice o is presented. it can be seen that the content of barium on the batio3/tinb sample (2nd series) exhibits much lower values. we are currently not able to explain this effect. the most essential, however, is the general trend of barium content decay with the time of sample treatment in the solution saline, which is clearly observed on all the samples. this decrease is more considerable after the 1st week than after the following three weeks. the slowdown of the barium release into the solution saline is the most obvious on the 1st series of batio3/tinb samples. the barium release was independently confirmed by an xps measurement of nacl obtained from the used solution saline. along with na and cl peaks, we were able to recognise traces of barium in the xp spectra. contrary to barium, the change of titanium concentration is much weaker as can be seen in figure 3. generally, it slightly increases except for the 1st series of batio3/tinb where a decrease is observed after the 1st week. extremely high value of titanium concentration on the batio3/ti sample is probably given by the contribution of the base substrate material. all these results can be identically interpreted as a release of barium to the solution saline. this process could also occur in a human body if barium titanate was used as a material for bone implants. in the follow-up research, we will further investigate if this process fades after some prolonged period of time resulting 15 k. moriová, z. tolde, p. vaněk et al. acta polytechnica ctu proceedings figure 3. titanium concentration due to an action of solution saline. in a stable barium titanate thin film. another topic to be studied on these materials is their ferroelectric properties after the treatment in a solution saline or in a physiological-like environment. 4. conclusion a depletion of barium concentration in batio3 thin films under the impact of solution saline was studied. barium releases into the solution saline, but it can be expected that this effect will become weaker over an extended period of time and the chemical stability of the material will be achieved. such long-time experiment are currently under the progress. acknowledgements this work was supported by grant agency of the czech republic, project number 15-01558s. xps system used to get the experimental results was supported by czech ministry of education (contract number lm2015057). references [1] n. setter, d. damjanovic, l. eng, et al. ferroelectric thin films: review of materials, properties, and applications. journal of applied physics 100(5):051606, 2006. [2] f. r. baxter, c. r. bowen, i. g. turner, a. c. e. dent. electrically active bioceramics: a review of interfacial responses. annals of biomedical engineering 38(6):2079–2092, 2010. doi:10.1007/s10439-010-9977-6. [3] p. vaněk, z. kolská, t. luxbacher, et al. electrical activity of ferroelectric biomaterials and its effects on the adhesion, growth and enzymatic activity of human osteoblast-like cells. journal of physics d: applied physics 49(17):175403, 2016. [4] m. wegmann, l. watson, a. hendry. xps analysis of submicrometer barium titanate powder. journal of the american ceramic society 87(3):371–377, 2004. doi:10.1111/j.1551-2916.2004.00371.x. 16 http://dx.doi.org/10.1007/s10439-010-9977-6 http://dx.doi.org/10.1111/j.1551-2916.2004.00371.x acta polytechnica ctu proceedings 8:14–16, 2017 1 introduction 2 experimental 3 results and discussion 4 conclusion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2016.3.0043 acta polytechnica ctu proceedings 3:43–46, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app surface treatment and examination of grade 2 and grade 5 titanium peter nagya,∗, miklos weszlb, krisztian laszlo tothb, imre kientzla, gyorgy ringa, peter szabaditsa, eszter bognara,c a budapest university of technology and economics, department of materials science and engineering, budapest, hungary b nanoti limited, birmingham, uk c mta–bme research group for composite science and technology, budapest, hungary ∗ corresponding author: npeter@eik.bme.hu abstract. surface characteristics play an important role in the implant-bone integration that is required for the long-term reliability of dental and orthopedic implants. in this paper, we investigate the effect of acid etching on the mass reduction and roughness of grade 2 and grade 5 ti under controlled experimental conditions. three different etching compounds were investigated: 30% hcl, 85% h3po4 and the compound of 30% (cooh)2 × 2h2o and 30% h2o2 in various treatment intervals under controlled temperature. stereo microscopy, scanning electron microscopy, roughness and weight measurements were carried out on the samples. we found that neither 85% h3po4 nor the compound of 30% (cooh)2 × 2h2o and 30% h2o2 were able to remove the machining marks from the surface of ti discs in our experimental setting. on the other hand, etching in 30% hcl yielded even surfaces both on ti grade 2 and 5 discs. we also found that etching at higher temperatures in 30% hcl resulted in significant mass loss. keywords: titanium, chemical etching, mass reduction, roughness. 1. introduction pure titanium and titanium alloys are well-established standard materials of dental and orthopedic implants because of their favorable mechanical strength, chemical stability and biocompatibility [1]. nowadays, the most frequently used pure titanium is identified as “commercially pure” (cp) grade 2 and 4. however, a titanium-vanadium-aluminum alloy, reported as grade 5 or labeled as ti6al4v, is also commonly used. the integration of titanium dental implants with the surrounding bone tissue (osseointegration) is critical to ensure the long-term survival and functionality of the implants [2]. the concept of osseointegration was discovered by brånemark and his co-workers. their research has had a dramatic influence on the design of implants and consequently the clinical outcome of dental implant surgeries [3]. the first generation of successfully applied titanium implants had simple machined surfaces. since then, implant surfaces have long been recognized to play an important role in molecular interactions, cellular response and osseointegration. therefore, tremendous scientific efforts have been focused on the development of implants with surfaces that have the capability of accelerating the osseointegration and improving the long-term survival of the implants. for that purpose, various methods have been developed during the last 20 years, such as sandblasting, acid etching, bioactive coatings, anodization and, more recently, laser modification of surfaces [4–6]. these implants have been extensively investigated in in vivo experiments, including longterm clinical studies and experimental histological and biomechanical evaluation in animal models [7]. titanium and titanium alloys are prone to develop a superficial oxide layer upon contact with oxidants [8]. the quality of the oxide layer may profoundly affect the biological behavior of titanium implants. the mechanical properties of the oxide layer, such as the thickness, texture and roughness are known as the most important parameters that may affect the rate of osseointegration and the biomechanical properties of the devices [9]. several types of surface treatment methods have been proposed in the scientific literature, including mechanical and chemical procedures to improve the osseointegration ability of dental implants. however, usually these publications do not disclose details about the effect of treatment parameters on the mechanical properties of titanium, but rather focus on the optimization of biological properties of the oxide layer [7–10]. 2. aim of experiment in this paper, we focus our attention on the effect of acid etching on the mass reduction, surface texture and roughness of ti grade 2 and ti grade 5 samples under controlled experimental conditions. 3. experiment titanium discs of 2 mm thickness and 14 mm in diameter were cut from grade 2 and grade 5 rods with a turning machine. the weight, roughness and surface texture of the discs were recorded after machining. 43 http://dx.doi.org/10.14311/app.2016.3.0043 http://ojs.cvut.cz/ojs/index.php/app p. nagy, m. weszl, k. l. toth et al. acta polytechnica ctu proceedings figure 1. stereo microscopic images of titanium discs before and after etching in h3po4, in the compound of (cooh)2 × 2h2o and h2o2 and in 30% hcl. 3.1. chemical etching after turning, 54 pieces of ti grade 2 and 54 pieces of ti grade 5 discs were subjected to acid etching. we investigated the effect of three different acids: 30% hydrochloric acid (hcl), 85% phosphoric acid (h3po4), and the compound of 30% oxalic acid ((cooh)2 × 2h2o) and 30% hydrogen peroxide (h2o2). the etching intervals were 10, 600, 1800, 3600, 5400 and 7200 seconds at three temperatures: 20°c, 40°c and 60°c. 3.2. weight measurement the weight of the samples was measured (denver instrument apx-200, new york, united states) after each etching interval. the differences in the weight of the titanium discs measured before and after chemical etching were calculated and plotted. 3.3. microscopy stereo microscopic (olympus szx16, pennsylvania, united states) images were taken of the titanium discs after each etching interval in each experimental group in order to record the surface texture of the samples (figure 1). only those samples were further investigated by scanning electron microscopy (philips xl 30, zagreb, croatia) where the machining marks disappeared from the surface of the discs (see hcl row on figure 1). 3.4. roughness measurement five discs were selected from each experimental group and three measurements were performed on each hcl, 40°c, 1800 s hcl, 60°c, 1800 s 0.00 0.25 0.50 0.75 1.00 ti grade 2 ti grade 5 ti grade 2 ti grade 5 p ro fil e ro ug hn es s (r a) ± 9 5% c i before etching after etching figure 2. mean profile roughness values and their 95% cis for ti grade 2 and ti grade 5 discs before and after etching in 30% hcl at 40°c for 1800 seconds and at 60°c for the same duration. disc. profile roughness (ra) measurements (mitutoyo surftest 211) were performed along 3 radial lines in 120°increments from the outer edge towards the center of each disc. 4. results and discussion the stereo microscopic images showed that machining marks were visible on the surface of titanium discs with width of 15–20 µm (figure 1). after etching either in 85% of h3po4 or in the compound of 30% of (cooh)2 x 2h2o and 30% h2o2 the surface morphology of ti grade 2 and ti grade 5 discs was similar to the untreated surface meaning that the machining marks remained visible even after the 7200 second treatment (top and middle rows of figure 1). on the other hand, the etching in 30% hcl markedly reduced the unevenness of the surfaces both on the ti grade 2 and the ti grade 5 discs (bottom row on figure 1). thus, only hcl etched titanium discs were subjected to further investigations. concerning the treatment parameters, such as time and temperature, the ti grade 2 discs that were treated in hcl at 40°c for 1800 seconds and those that were treated in hcl at 60°c for 1800 seconds showed even surface patterns (figure 3). however, we found a considerable difference in the dissolution profiles of the ti discs treated at 40°c and 60°c. our findings show 44 vol. 3/2016 surface treatment and examination of titanium figure 3. sem images of grade 2 and grade 5 titanium discs before etching and after etching in hcl at 40°c and 60°c for 1800 seconds. ti grade 2 ti grade 5 0 2.5× 10−9 5 × 10−9 7.5× 10−9 1 × 10−8 20°c 40°c 60°c 20°c 40°c 60°c temperature of etching compound m as s di ss ol ve d pe r un it su rf ac e pe r un it tim e [g /m m 2/ s] etching compound hcl cooh h3po4 figure 4. mass dissolution per unit time of ti grade 2 and ti grade 5 in each etching compound. that increasing the temperature has a more pronounced effect on the mass reduction of ti grade 2 than the prolonged treatment time (figure 5). the same treatment parameters were found to be favorable to create even surfaces on ti grade 5 discs as on ti grade 2 discs. the etching of ti grade 5 in hcl at 40°c for 1800 seconds completely removed the machining marks from the surface of the discs (see figure 3). increasing the temperature from 40°c to 60°c resulted in densely pitted surfaces within the same (1800 seconds) treatment period (see figure 3). concerning the dissolution profiles of ti grade 5, increasing the temperature of the 30% hcl etchant resulted in more intense mass reduction of the ti grade 5 than ti grade 2 discs (figure 5). interestingly, higher temperatures increased the dissolution rate of both the ti grade 2 and ti grade 5 samples irrespective to the composition of the etchant at 60°c. ti grade 5 showed higher dissolution rates than ti grade 2 discs and the effect of increased temperature was higher this case than on pure titanium (figure 4). the profile roughness measurements did not unambiguously reflect what was observed visually. the roughness of both ti grade 2 and ti grade 5 showed slight tendencies to decrease when etched in 30% of hcl at 40°c for 1800 seconds and increase when etched in 30% of hcl at 60°c for the same duration, however neither changes were statistically significant. (figure 2) the direction of these changes can be explained by the removal of burr in the case of the lower temperature and by the appearance of pits in case of the higher, however we expected a more distinct effect such as those apparent in the optical tests. 5. conclusion our results show that the optical characterization of an etched titanium surface can be more informative concerning biological performance than the mechanical measurement of the surface roughness. the production of an oxide layer with pitted surface texture on a titanium implant in order to support its osseointegration may be achieved at the cost of considerable material loss depending on the chemical composition of the titanium. ti grade 5 shows higher dissolution rates 45 p. nagy, m. weszl, k. l. toth et al. acta polytechnica ctu proceedings hcl cooh h3po4 ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● 0.0e+00 2.5e−05 5.0e−05 7.5e−05 0.0e+00 2.5e−05 5.0e−05 7.5e−05 t i g rade 2 t i g rade 5 0 2000 4000 6000 0 2000 4000 6000 0 2000 4000 6000 etching time [s] d is so lv ed m as s pe r un it su rf ac e [g /m m 2] temperature ● 20°c 40°c 60°c figure 5. dissolution profiles of ti grade 2 and ti grade 5 discs in 85% h3po4, in the compound of 30% (cooh)2 × 2h2o and 30% h2o2 and 30% hcl at temperatures of 20°c, 40°c and 60°c. than ti grade 2 that might be attributed to the potential difference of its alloying compounds creating an electrochemical cell where the etchant also acts as an electrolyte. from a practical point of view, the uncontrolled etching may adversely affect the fine geometrical structures of dental implants, like the self-tapping part of the thread. blunted threads may cause undue mechanical stress to the bone tissue during insertion that may detrimentally affect osseointegration. our team plans to investigate the optimal combination of etching time and temperature in terms of material loss and surface roughness for various etchants and their effect on the fine geometry of dental implant screws. acknowledgements the present work was funded by the rea under the fp7 grant agreement no. 606624 (nanoti). references [1] m. long, h. rack. titanium alloys in total joint replacement a materials science perspective. biomaterials 19(18):1621 – 1639, 1998. doi:http://dx.doi.org/10.1016/s0142-9612(97)00146-4. [2] r. vayron, e. soffer, f. anagnostou, g. haiat. ultrasonic evaluation of dental implant osseointegration. journal of biomechanics 47(14):3562 – 3568, 2014. doi:http://dx.doi.org/10.1016/j.jbiomech.2014.07.011. [3] r. adell, u. lekholm, b. rockler, p.-i. branemark. a 15-year study of osseointegrated implants in the treatment of the edentulous jaw. international journal of oral surgery 10(6):387 – 416, 1981. doi:http://dx.doi.org/10.1016/s0300-9785(81)80077-4. [4] l. l. guehennec, a. soueidan, p. layrolle, y. amouriq. surface treatments of titanium dental implants for rapid osseointegration. dental materials 23(7):844 – 854, 2007. doi:http://dx.doi.org/10.1016/j.dental.2006.06.025. [5] y. shibata, y. tanimoto. a review of improved fixation methods for dental implants. part i: surface optimization for rapid osseointegration. journal of prosthodontic research 59(1):20 – 33, 2015. doi:http://dx.doi.org/10.1016/j.jpor.2014.11.007. [6] m. kulkarni, a. mazare, e. gongadze, et al. titanium nanostructures for biomedical applications. nanotechnology 26(6):062002, 2015. [7] p. g. coelho, r. jimbo, n. tovar, e. a. bonfante. osseointegration: hierarchical designing encompassing the macrometer, micrometer, and nanometer length scales. dental materials 31(1):37 – 52, 2015. doi:http://dx.doi.org/10.1016/j.dental.2014.10.007. [8] u. diebold. the surface science of titanium dioxide. surface science reports 48(5-8):53 – 229, 2003. doi:http://dx.doi.org/10.1016/s0167-5729(02)00100-0. [9] j. w. choi, s. j. heo, j. y. koak, et al. biological responses of anodized titanium implants under different current voltages. journal of oral rehabilitation 33(12):889–897, 2006. doi:10.1111/j.1365-2842.2006.01669.x. [10] y. iwaya, m. machigashira, k. kanbara, et al. surface properties and biocompatibility of acid-etched titanium. dental materials journal 27(3):415–421, 2008. doi:10.4012/dmj.27.415. 46 http://dx.doi.org/http://dx.doi.org/10.1016/s0142-9612(97)00146-4 http://dx.doi.org/http://dx.doi.org/10.1016/j.jbiomech.2014.07.011 http://dx.doi.org/http://dx.doi.org/10.1016/s0300-9785(81)80077-4 http://dx.doi.org/http://dx.doi.org/10.1016/j.dental.2006.06.025 http://dx.doi.org/http://dx.doi.org/10.1016/j.jpor.2014.11.007 http://dx.doi.org/http://dx.doi.org/10.1016/j.dental.2014.10.007 http://dx.doi.org/http://dx.doi.org/10.1016/s0167-5729(02)00100-0 http://dx.doi.org/10.1111/j.1365-2842.2006.01669.x http://dx.doi.org/10.4012/dmj.27.415 acta polytechnica ctu proceedings 3:43–46, 2016 1 introduction 2 aim of experiment 3 experiment 3.1 chemical etching 3.2 weight measurement 3.3 microscopy 3.4 roughness measurement 4 results and discussion 5 conclusion acknowledgements references 148 acta polytechnica ctu proceedings 2(1): 148–151, 2015 148 doi: 10.14311/app.2015.02.0148 ss cygni revisited r. c. smith1, j. echevarŕıa2, j. v. hernandez2,3, p. szkody4 1astronomy centre, university of sussex, uk 2unam, mexico city, mexico 3physics & astronomy department, university of southampton, uk 4astronomy department, university of washington, usa corresponding author: r.c.smith@sussex.ac.uk abstract new spectroscopic and photometric observations of ss cygni, the brightest dwarf nova system, have been obtained, with the aim of mapping starspots on the surface of the secondary star. four nights of echelle spectroscopy in quiescence have been obtained using the 2.2-m telescope at san pedro martir (mexico) in august 2012 and another two nights at the 3.5-m telescope at apache point observatory, usa, in september 2012, but these data are still being reduced. simultaneous ccd photometry was also obtained at the two sites, and the mexican photometry was extended into the subsequent long outburst. this presentation reveals some interesting photometric behaviour in that outburst, but further data will be necessary before the nature of the behaviour can be determined. keywords: cataclysmic variables dwarf novae optical spectroscopy photometry individual: ss cyg. 1 introduction the canonical model of cataclysmic variable (cv) evolution requires secondaries to be magnetic, to allow magnetic braking to keep the star in contact with its roche lobe. magnetic activity should produce starspots, as shown by observations of rapidly rotating single stars. detection of starspots on cv secondaries provides evidence for magnetic fields, and roche tomography has been used to reveal spots on four systems: ae aqr (watson et al. 2006), bv cen, v426 oph (watson et al. 2007a, 2007b) and ru peg (dunford et al. 2012). the unusual nova-like system ae aqr is the brightest of these, and the others are at least two magnitudes fainter. ss cygni is the brightest dwarf nova, and in quiescence is only half a magnitude fainter than ae aqr. it is therefore an obvious candidate for study and highresolution echelle data were obtained in 2012 august (in mexico) and september (in the usa), with simultaneous photometry. the mexican echelle data were taken with the 2.2-m telescope at the san pedro martir (spm) observatory in baja california; the v photometry was taken with the spm 0.84-m telescope. the us echelle spectra were taken with the 3.5-m telescope at the apache point observatory (apo); simultaneous photometry was also obtained, using the nmsu 1-m telescope at apo (v ) and the uw 0.76-m at manastash ridge observatory (g, r, i). 2 spectra the us spectra were taken on two nights with the apo 3.5-m and have been fully reduced but not yet analysed. in figure 1 we show part of the average spectrum from the first night; the region shortward of 6750 å makes it clear that there are many absorption lines that can be used for roche tomography. four nights of data were taken with the spm 2.2-m; these spectra are still being reduced. figure 1: a portion of the average of 29 spectra of ss cygni taken with the echelle spectrograph on the 3.5-m apo on 20/21 september 2012. in addition to strong emission lines, there are many absorption lines suitable for roche tomography of the secondary. 148 http://dx.doi.org/10.14311/app.2015.02.0148 ss cygni revisited 3 photometry all the photometry has been fully reduced; here we just discuss the analysis of the mexican data. at the san pedro martir (spm) observatory in mexico, simultaneous v photometry with the 0.84-m telescope was taken to enable flux calibration of the echelle spectra being taken with the 2.2-m telescope. by good fortune, ss cygni went into outburst one day after the spectra had been taken, and our mexican colleagues kindly allowed us to continue photometric observing; the complete coverage is shown in figure 2. unfortunately, no useful data were obtained on the fifth night in outburst, which was clouded out; however, the mean level on that night does appear to be higher than on the previous nights, possibly lending support to the prediction of cannizzo (2013; see also cannizzo 2012) that long outbursts should have a precursor outburst at the beginning. subsequent aavso data confirmed that this was a long outburst. figure 2: v photometry of ss cygni in quiescence, rise and outburst, august 2012. we first analysed the quiescent data, looking for the dominant period. as expected, the only significant period to be found was the orbital period; a light curve folded on that period showed the characteristic double hump arising from ellipsoidal variation. there were four nights of useable outburst data. the data were first detrended, by removing linear trends from each individual night and then adding or subtracting suitable constants to bring all the nights to the same average magnitude. the starlink package period was used to search for the dominant period, using five different methods: string-length, minimum chisquared, lomb-scargle, fourier transform and clean. some of these methods produced no very useful results, and the clearest and most consistent results were obtained with the minimum chi-squared and lombscargle methods. the results below quote only the results from those two methods. figure 3: night 3 outburst data folded on a period of 0.35273 days and binned into 400 bins. note that the magnitude scale has brightness increasing downwards. analysing the entire data-set gave a best-fit period that was about 1.5% smaller than the orbital period, but the signal was not strong and this result is not thought to be significant. however, when the different nights were analysed separately a very different pattern emerged: each night had a different dominant period. the clearest result was for the 3rd night in outburst, where the two methods agreed on a period of 0.353 days. this is approaching the length of the data stream on that night (0.384 days), but is significantly shorter, and there is no sign of the data length in the period analysis. this period is also significantly longer than the orbital period of 0.27513 days. figure 3 shows the night 3 data binned and folded on a period of 0.35273 d. the best period on night 2 was close to the orbital period, with minimum chi-squared giving 0.2715 d and lomb-scargle giving 0.2769 d. however, the other two nights both gave significantly shorter best periods: 0.1433 d on night 1 and 0.1963 d on night 4. the lombscargle plots for all the nights are shown in figure 4 – note that the maximum power varies from night to night. thus, apart from night 2, the outburst data are not consistent with the orbital period, with two shorter periods and one longer one. there is a temptation to consider the night 3 data as evidence for a positive superhump – boneva et al. (2009) suggested that in outburst ss cyg has an elliptical disc. if so, ss cyg is not impossibly far off the standard psh, porb relation, and the orbital period of 6.6 h would be the longest on that relation. however, with a well-determined mass ratio q of 0.683 (bitner at al. 2007), it strongly violates the normal resonance criterion of q < 0.33. 149 r. c. smith et al. figure 4: lomb-scargle power plots for the four outburst nights. by far the strongest signal is on night 3, with a maximum power of ∼350. the maximum power on the other nights are: ∼50 (night 1), ∼200 (night 2) and ∼100 (night 4). the dominant periods on nights 1 to 4 are 0.1433 d, 0.27-0.28 d, 0.35273 d and 0.1963 d respectively. the horizontal axis is frequency, in cycles/day. furthermore, the amplitude is low (∼0.08 mag), the superhump excess (28%) is rather large, and two of the other nights suggest negative superhumps (although these have even larger differences from the orbital period, at 48% and 29% smaller, and have similarly small amplitudes). is there a better explanation? one possibility was raised by bisikalo (2013; see also zhilkin & bisikalo 2010), who showed models where fluctuations in the accretion rate onto the white dwarf, caused by variations in the generation of magnetic field in the disc, produced brightness variations on various timescales. perhaps we are seeing evidence in our data for similar brightness variations, which might be stochastic in nature. 4 conclusions the spectral data we have obtained for ss cygni appear to be good enough for us to be able to map starspots on the surface of the secondary component. the photometric data in quiescence appear to show ellipsoidal variations on the orbital period. however, the photometric data in early outburst are generally not consistent with the orbital period. the data from the 1st and 4th nights have shorter periods (negative superhumps?) while the data from the 3rd night show a longer period (a positive superhump in the longest-period system so far?). alternatively, we may have found evidence for variations in the accretion rate onto the white dwarf, caused by magnetic effects in the disc. whatever the explanation, it would be worth monitoring ss cygni intensively during its long outbursts, to see whether this peculiar behaviour is repeated. it turns out that the kind of photometric data we obtained during the long outburst in august 2012 is rare: not many people have carried out time-resolved observations of the long outbursts in dwarf novae and so the nature of the behaviour during these outbursts is still 150 ss cygni revisited quite uncertain (cf. cannizzo 2012, 2013). in order to test whether any changes are periodic or stochastic, it will be necessary in future to monitor as many of these long outbursts as possible, in ss cygni and in similar dwarf novae. it is hoped to do this by organising an international campaign involving both the amateur community and the many robotic telescopes scattered around the world. by the time these data are available, it is hoped that predictions of the magnetic effects in the disc, by bisikalo and others (e.g. bisikalo 2013), will have reached the stage where they may be compared in detail with the data to discover whether the model is compatible with observations. acknowledgement we thank leslie hebb for her painstaking reduction of the apo spectra, our mexican colleagues for allowing us to observe ss cyg in outburst, phil charles for comments on the outburst photometry and tom marsh for help with software. we acknowledge the use of the period program from the starlink package, supported at the joint astronomy centre in hawaii, and of the aavso light curve generator. references [1] bisikalo, d.: 2013, these proceedings. [2] bitner, m.a., robinson, e.l., behr, b.b.: 2007, apj 662, 564. doi:10.1086/517496 [3] boneva, d. et al.: 2009, astronomy reports 53, 1004. doi:10.1134/s1063772909110055 [4] cannizzo, j.k.: 2012, apj 757, 174. doi:10.1088/0004-637x/757/2/174 [5] cannizzo, j.k.: 2013, these proceedings. [6] dunford, a., watson, c.a., smith, r.c.: 2012, mnras 422, 3444. [7] watson, c.a., dhillon, v.s., shahbaz, t.: 2006, mnras 368,637. [8] watson, c.a., et al.: 2007a, an 328, 813. [9] watson, c.a., et al.: 2007b, mnras 382, 1105. doi:10.1111/j.1365-2966.2007.12173.x [10] zhilkin, a.g., bisikalo, d.v.: 2010, astronomy reports 54, 840. doi:10.1134/s1063772910090088 discussion david buckley: i am puzzled by the superhump excess ε for tx col. is there a reference for the superhump period? robert smith: i took the superhump period and excess for tx col from montgomery (2009, apj, 705, 603), who quoted retter et al. (2005, assl, 332, 251). the retter et al. conference paper is suggestive but not definitive. christian knigge: since you typically see only about one cycle of your periods in each epoch, is it not possible that the variability is stochastic rather than periodic? robert smith: in some cases we have two cycles. but more generally, yes, to call them periodic changes is a bit speculative. however, there is a clear single peak in the lomb-scargle power spectrum on each night, and they are certainly at different frequencies on different nights. the night-to-night changes may be stochastic, as you suggest, but there is definitely something interesting happening. 151 http://dx.doi.org/10.1086/517496 http://dx.doi.org/10.1134/s1063772909110055 http://dx.doi.org/10.1088/0004-637x/757/2/174 http://dx.doi.org/10.1111/j.1365-2966.2007.12173.x http://dx.doi.org/10.1134/s1063772910090088 introduction spectra photometry conclusions 326 acta polytechnica ctu proceedings 1(1): 326–328, 2014 326 doi: 10.14311/app.2014.01.0326 some personal conclusions sergio colafrancesco1 1university of the witwatersrand, johannesburg (south africa) corresponding author: sergio colafrancesco. email: sergio.colafrancesco@wits.ac.za abstract i present here some personal considerations on the main theoretical, observational and technological challenges offered to the discussion during the meeting ”multifrequency behaviour of high energy cosmic sources”. 1 the theme this meeting presented a wide collection of excellent results on a wide range of subjects in modern multifrequency astrophysics. i am not able to remember a single talk that did not produce a vibrant discussion in and out of the audience. beyond any attempt to summarize the outcomes of the meeting, it seems more appropriate for me to briefly present here some personal considerations on the main challenges offered to the discussion during this meeting. 2 the challenges one of the main aspects of this meeting is its capacity to induce global discussions on some of the most important challenges in astrophysics and cosmology. these challenges address the nature of fundamental questions in the physics of the universe, the frontier of exa-scale data mining and analysis and the technological challenges related to the construction of the largest astronomical facilities in the next decade. 2.1 theoretical challenges: fundamental questions big theoretical challenges regard two important aspects of the structure and evolution of our universe: the cosmic origins and the cosmic extremes. origins. beyond the successes of the standard cosmological scenario, we are still facing some crucial questions: what happened at the beginning of the universe? inflation and precision cosmology. there’s been incredible progress recently in finding the traces that inflation left behind and upcoming experiments on cmb polarization promise to provide even more evidence of what happened during the universe’s infancy. through its sensitivity to gravitational waves, the study of the cmb provides a glimpse into the state of the universe just ∼ 10−35 seconds after the beginning and of physics on grand-unification-theory (gut) energy scales around ∼ 1016 gev, some ≈ 13 orders of magnitude above the energies achievable by current terrestrial particle accelerators. a gravitational-wave background in the early universe would leave a unique, oddparity pattern of polarization in the cmb (b-modes), the magnitude of which is characterized by the tensorto-scalar ratio r. a gwb is generically predicted to exist by inflationary theories, and the current generation of cmb polarization experiments will probe the interesting parameter space of r ∼< 0.05 corresponding to single-field inflationary models at gut scales. the challenges here seem to be a statistically confident measurements of b-modes and the imperative study of the systematics that are present in such a difficult measurement. a multi-frequency study of b-modes with extremely high sensitivity, over a wide range of frequencies and large sky areas would likely be able to measure in the not-so-distant future the value of r with a ∼ 10% precision and will open the field to a deep theoretical exploration of inflationary cosmologies. what is the dark matter? this is a particularly exciting time for dark matter study because there are some intriguing clues pointing to where dark matter particles might be hiding. these clues are helping researchers develop a variety of searches. the three major strategies are direct detection, collider production and indirect detection. while there is a mounting scientific frustration in the non conclusive evidence for the detection of dm particles with direct and collider detection techniques, the sensitivity and the specific strategy of the next coming astronomical observatories (mainly the cta and the ska) will probably allow in the next decade to shed a conclusive word on the nature of dm, or close a large fraction of the dm parameter space and thus open the way to a more detailed exploration of realistic alternatives of the theory of gravity. 326 http://dx.doi.org/10.14311/app.2014.01.0326 some personal conclusions what makes up the rest of the universe? dark energy. in the past 15 years or so, scientists have realized that the ”stuff” making up all the atoms in all the galaxies, stars, planets, and humans we have ever observed only constitutes about 5% of the universe. while we might be close to pinning down the nature of part (≈ 27%) of the missing stuff (e.g., dark matter), what we know about the dominant (≈ 68%) component of the universe, (named historically dark energy for a vague analogy with dm) is still almost nothing. observational efforts are planned (e.g., euclid, ska, des, lsst, etc.) and theoretical exercises to narrow down the available de parameter space are the subject of a restless activity, but a detailed physical characterization of the ”dark energy” is still missing and probably this theoretical activity will be very relevant in pointing at the true nature of the physical mechanism providing the late-stage cosmic acceleration. extremes. where did that come from? cosmic rays and intergalactic particle accelerators. after a century of study, researchers still struggle to understand the origin of cosmic rays, and especially those of ultra high energy. we believe these extreme high-energy oddities play a key role influencing the physics and chemistry that form stars and planets, and even influence life on earth by occasionally causing mutations in dna. and yet, the exact ways in which cosmic rays are accelerated remains a major open question. we’ve discovered where many come from within our galaxy, but the most extreme cosmic rays continue to confound us. the need of a very large collecting area experiment for the extremely rare uhecr events poses several observational challenges, but its delivery will probably open the way to a physical clarification of their origin and of the production sites. challenges to particle acceleration theories in cosmic structures are stronger and stronger and the scientific qualification of the possible product sites is reducing more and more towards regions of compact objects with extremely strong gravitational fields and magnetic fields. what can compact objects teach us? black holes and neutron stars, extreme physics in small packages. enormously powerful gravitational fields that warp the local fabric of space and time. incomparably strong magnetic fields that can stretch atoms themselves into long spindles. materials so dense a teaspoonful would weigh billions of tons. these are just some of the exotic properties of compact objects, a catch-all term for several types of unbelievably dense and remarkable objects, like white dwarfs, neutron stars and black holes. compact objects are known to possess some of the most extreme physical properties ever observed. scattered throughout our galaxy and agns, these objects serve as astrophysical laboratories that test the very limits of physics as we know it. 2.2 observational: big data science it is now becoming clear that the answers to big questions in astrophysics and cosmology requires to address the challenge of dealing with big data quantities, analysis and transport. how will we make sense of it all? astronomically big data. astrophysics and cosmology deal with big everything: big datasets, big simulations and big collaborations. we have information on billions of astronomical objects, and expect to make measurements of many billions more in the next decade. yet the challenge with such a large dataset is not so much in handling its size, but in its complexity. the struggle in trying to find a single rare star in a haystack of billions of nearidentical stars, or understanding the relationships between every single galaxy in the universe, goes beyond simply the enormous number of gigabytes. as more and more data piles up, the teams who are most innovative about analyzing and combining those datasets will be the ones who will likely make the biggest discoveries. instruments like the ska will fully live into the era of big data complexity and will have to address not just the complex techniques of data reduction and analysis, but also the challenges of data distribution and transport over inter-continental distances and yet with high computing capacity on our everyday desktop computer. the next generation of astronomical surveys (and even single observations) will contain information that spans multiple frequencies, and many epochs in time. however there is not yet a next generation of catalog than can describe these surveys. a more meaningful description of catalog data will ultimately lead to better comparisons of astronomical surveys and more robust scientific output. it is not unreasonable that a stratification of various computational -tasks and a possible -re-definition -of -the -data -analysis -objectives and -techniques -will -be -(re-)considered in the light of the experimental and theoretical challenges of the next decade big astronomy science. in this context, small or mid-size multifrequency data centers will probably play a major role in developing innovative applications for (astronomical) data science and producing cutting edge scientific exploitation of the data achieved by large astronomical facilities. 2.3 experimental: big facilities the future large astronomical projects will live inherently in the era of multifrequency astronomy. examples of this synergy are provided by the ska, the cta, the lsst, and the largest future space missions like e.g. 327 sergio colafrancesco euclid, millimetron. the wealth of planed astronomy projects is such that it seems that the future of astronomy can only be limited by the financial constraints of international funding available. both ground-based and space-borne experiments are facing challenges specific to their different nature. some of these are technical and will give rise to extensive technological developments and innovations. some other are programmatic and are related to the complex and ambitious nature of future projects. it is not unlikely that the complementarity between large-scale projects and pathfinders will provide the scientific community the clarity on the technological routes to be followed for the construction of the most successful and challenging astronomical facilities of the next decade, as well as the directions in the optimal integration of these facilities in the most successful multifrequency strategy. this seems to be mandatory in order to answer the remaining big questions on the nature and the evolution of our universe. 3 predictions based on the decennial successes of this meeting, as also testified by this specific one, it is not difficult to predict that the next meeting of this series will provide an even more extended discussion on the major challenges of multifrequency astrophysics, cosmology and astro-particle physics in the next future. acknowledgments s.c. acknowledges support by the south african research chairs initiative of the department of science and technology and national research foundation and by the square kilometre array (ska). 328 the theme the challenges theoretical challenges: fundamental questions observational: big data science experimental: big facilities predictions acta polytechnica ctu proceedings doi:10.14311/app.2017.10.0016 acta polytechnica ctu proceedings 10:16–33, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app testing methods for mechanically treated soils: reliability and validity ana petkovšek∗, matej maček, jasna smolar university of ljubljana, faculty of civil and geodetic engineering, jamova 2, ljubljana, slovenia ∗ corresponding author: ana.petkovsek@fgg.uni-lj.si abstract. a possibility of in-situ mechanical improvement for reducing the liquefaction potential of silty sands was investigated by using three different techniques: vibratory roller compaction, rapid impact compaction (ric) and soil mixing. material properties at all test sites were investigated before and after improvement with the laboratory and the in situ tests (cpt, sdmt, dpsh b, static and dynamic load plate test, geohydraulic tests). correlation between the results obtained by different test methods gave inconclusive answers. keywords: liquefaction, experimental site, rapid impact compaction, soil mixing. 1. introduction the term ground improvement refers to any technique or process that improves the engineering properties of the treated soil mass in order to fulfil the purpose intended. usually, the modified properties are strength, stiffness, permeability, workability (willingness for compaction), resistance to frost, etc. [1–4]. the type of ground improvement/soil treatment depends on the demands of the structure to be built, the soil type, the available materials and tools, and the local tradition and experience. the efficiency of a specific improvement technique may be measured by using different testings and instrumentation. whenever a laboratory or field test/measuring device is used as part of the data collection process, the validity and the reliability of the test/device is important. just as we would not use a test for the determination of particle size distribution to assess the activity of clay, we would not want to use any measuring device not capable of measuring properties which are of the design or qa – qc interest. this paper focuses on the validity and sensitivity of the laboratory and field tests used to assess the efficiency of the mechanical improvement of siltysandy soils. special attention is given to the use of kozeny-carman equation for the estimation of the soil permeability. analysis presented in the paper refers to the investigation performed at the location of hydropower plant (hpp) brežice, se slovenia, where the top layer of the foundation ground indicates properties of liquefiable soil. the main goal of the ground improvement is to increase the soil liquefaction resistance and to assure the required permeability of the fill material to be used for app. 14 km long dikes along the hpp reservoir. 2. background 2.1. site description the reservoir of the hpp brežice requires the construction of app. 7 km long and up to 10 m high dikes on both sides of the river sava. the top layer of the foundation ground consists of loose silty sands, prone to liquefaction. hpp brežice is the 5th in the chain of the lower sava river hpps (figure 1) and is situated in the influential area of nucler power plant krško (npp). tectonically, the wider area belongs to the tectonic unit named “krško basin”, which is considered a potentially active structure [5]. a well-documented earthquake with a magnitude of 5.7 and intensity of viii ems occurred in january 1917 [6]. the so called “zagreb earthquake” in 1880 triggered liquefaction along the river bank between brežice and zagreb (croatia) [7, 8]. the design ground accelerations in the krško basin for different earthquake return periods are presented in table 1. 2.2. geological profile the geological profile is quite uniform over the entire area of the hpp (figure 2). the top layer is up to 5 m thick, made of very loose sandy silts and sands (ml, sm, sp), deposited by recent floods. the top soil layer contains fine coal particles that origin from the flotation processes from the area around 60 km upstream where the coal mines have operated for the last 300 years. coal particles confirm the very young origin of the sediments. poplar tree roots appear up to 4 m deep and also prove the development of the “paleo” ground between the larger flood events. beneath the top layer the medium dense to dense quaternary gravels are deposited. the gravel is classified as silty sandy gravel (gm) to poorly graded gravel (gp) and consists mainly of limestone grains. 16 http://dx.doi.org/10.14311/app.2017.10.0016 http://ojs.cvut.cz/ojs/index.php/app vol. 10/2017 testing methods for mechanically treated soils table 1. design ground accelerations for different earthquake return periods [9–11] figure 1. location of the hpp brežice. the thickness of gravel deposits varies between 8 and 12 m. the pre-quaternary bedrock below the gravel consist of miocene sediments, represented by overconsolidated, not cemented silts and marls, with some inclusions of the weak, soft limestones. the ground water (gw) level is controlled by the sava river. during most of the year, the gw level appears app. 4 – 6 m below the ground surface, inside the gravel layer. during the floods, the gw may rise up to 2 m above the ground and may stay there for days. when the hpp brežice is put into operation, the existing ground surface and silty/sandy layers will be permanently flooded in the area between the dikes on the left and the right river bank. the permanent rise of the gw level is forecast also at the influential area from brežice to krško, on the dry sides of the dikes. 2.3. soil properties 2.3.1. index properties the grain size distribution of the quaternary soils is not uniform. in the top layer they may vary from sandy silt to poorly graded sand (figure 3). according to empirical data [12, 13], the top layer soils belong to the groups of most liquefiable and potentially liquefiable soils. index properties of typical soils from the top layer are given in table 2. laboratory proctor compaction tests show that due to the presence of coal particles, unfavourable grading and uneven water content distribution, the top layer soils willingness to compaction is poor. different compaction curves (figure 4) confirm heterogeneity of different strata, deposited inside the top layer. 2.3.2. liquefaction potential the spt testsperformed in top soil layer shown the modified blow count (n1)60 between 2 and 8. seed and idriss [14] proposed an empirical method for assessing 17 a. petkovšek, m. maček, j. smolar acta polytechnica ctu proceedings figure 2. schematic geological profile (left) and schematic cross section of the valley after the hpp construction (right). not in scale. figure 3. relationship between grading and liquefaction potential [13], with the boundaries of the grading of top layer and quaternary gravel at the hpp brežice. grading curves *nova loza and *moj dvor, reported by veinović et al. [7] belong to the area, where liquefaction appeared in 1880. figure 4. proctor curves for three typical groups of soils from the top layer. 18 vol. 10/2017 testing methods for mechanically treated soils table 2. properties of three typical groups of soils from the top layer. the likelihood of liquefaction of level sites (figure 5, left). the cyclic stress ratio (csr) is calculated from eq.1 [9]. (csr)m=7,5 = csr msf = β ( σv0 · amax σ′v0 ) · rd msf (1) msf = 6.9 exp (−m 4 ) − 0.058 msf ≤ 1.8 (2) where β is a ratio between real maximum and equivalent seismic stresses (0.65) [15], amax is the maximum ground surface acceleration on the foundation ground, rd is stress reduction factor that drops from 1 at the surface to about 0.9 at 10 m depth. msf is a factor to account for the varying number of cycles associated with different magnitude events and has values shown in table 1. the seismic dilatometer tests (sdmt) in top layers gave the shear wave velocities (vs) of 160-300 m/s, while the seismic refraction test indicates the vs of 90-110 m/s. seed and idris [14], youd et al. [16] and andrus [17] proposed an empirical relation for assessing the likelihood of liquefaction of level sites, based on relationship between the csr and vs (figure 5, right). the cyclic simple shear test (csst) was used to study the influence of the density on the liquefaction potential (figures 6,7). the tests were carried out on soil samples with properties given in table 2. specimens were prepared at different initial void ratios, saturated, consolidated at 75 kpa of effective stress and then loaded with horizontal sinusoidal load at desired stress ratio in undrained condition. the beginning of liquefaction was defined when the increase of pore water pressure was equal to 95 % of effective vertical stress before cyclic loading. the reference number of cycles was defined after kramer [18], for an earthquake of magnitude 7.5. results of the laboratory tests are given in figure 7 and confirm that the top layer soil are prone to liquefaction. the compacted soil samples at 95 % of maximum proctor density (dpr) will very probably resist the 475 year return period earthquakes and will very probably liquefy at stronger earthquakes. 2.4. preliminary conclusions the grain size distribution, the spt, the seismic refraction as well as csst indicate the same ranges of liquefaction potential and can be estimated as valid and reliable. the test results can also be confirmed by the historical data from the 1880’ zagreb earthquake. the sdmt test gave the shear wave velocities (vs) in a range of 160 – 300 m/s. comparing the sdmt test results with other tests as well as with calculation, using the empirical equation 3 and 4, explained in chapter 4, we may conclude, that the sdmt test values are too high for the top soil layer probably affected by field site heterogeneity or by the influence of other men activities. based on other tests the conclusions are clear: the top layer represents a very unfavourable foundation ground and must be improved or removed from the influential area of the dikes. 3. discussion on improvement technique several options were discussed to improve the liquefaction resistance of the foundation ground, as follows: • loose material from the top layer shall be removed and replaced with compacted gravel material. the idea was recognized as the most promising and reliable choice as large quantities of good quality gravel material are available at the location. however, due to the large volumes of top soil to be replaced (length of app. 14 km, depth up to 5 m, width that locally exceeded 50 m) the decision was made to investigate other options too. 19 a. petkovšek, m. maček, j. smolar acta polytechnica ctu proceedings figure 5. relationship between cyclic stress ratios causing liquefaction and (n1)60 (after seed and idriss [14]) and the position of the top soil in it (left). relationship between cyclic stress ratios causing liquefaction and shear wave velocity values (after seed and idris [14], youd et al. [16] and andrus [17]) and the position of the top soil in it (right). bc – before compaction, fc – fines content, ts – top soil layer. figure 6. the seiken cyclic simple shear apparatus, used for the laboratory tests (left) and the cell (right). figure 7. the relationship between the number of cycles needed for liquefaction and the cyclic stress ratio (csr) for top soils at different void ratios. 20 vol. 10/2017 testing methods for mechanically treated soils • option 1 (es 1): static and vibratory roller compaction. the main attention was paid to the following questions: (a) is the 95 % of max. proctor density attained on site, (b) what is the effective depth of the roller compaction and (c) what are the potentially harmful effects of coal particles and roots to the soil compaction behaviour? the four test fields were made to study the compaction efficiency of the foundation ground and up to 2.5 m high test embankment was constructed to study the roller compaction efficiency above the soft subgrade, the vertical and horizontal movements, the internal erosion and to analyse the sensitivity of different test methods, like cone penetration test (cpt), flat dilatometer test (dmt, sdmt), dynamic probing super heavy (dpsh b), etc. the test field was made in september and october 2009. • option 2 (es 2): rapid impact compaction (ric). to avoid the shortcomings of the shallow effects of roller compaction, the ric technique was proposed. two test sites were made in february 2011. a comprehensive investigation was made on site before and after compaction [19, 20]. • option 3 (es 3): soil mixing on site to achieve liquefaction resistance, low permeability and better willingness to compaction. the idea was to excavate top soil and mix it with quaternary gravel in such proportion that it would fulfil three criteria: (a) resistance against liquefaction, (b) the designed permeability to eliminate the need for additional sealing of the dike and (c) improved willingness to compaction with reduced influence of seasonal water content changes on stiffness. the trial tests were made in april and may 2014, and the roller with the roller integrated continuous compaction control (ccc) was used for compaction. as the trial fields showed promising results, the temporary, app. 1.2 km long dike was constructed in order to protect the deep excavation for the powerhouse against the floods, as well as to get more data about the homogeneity, permeability and the resistance against liquefaction of the dike. figure 8 shows the locations of the field trial tests es 1 to es 3 and the temporary dike. 4. results from the experimental sites 4.1. experimental site es 1: roller compaction trial field 4.1.1. site description the soil profile and the soil properties were the same as presented in figure 2 and table 2. the thickness of the top layer was 4 m, the roots appeared in dense network to the depth up to 3.5 m. figure 9 shows the depth of the roots (left) and the size of the first of four test fields prepared to study the roller compaction efficiency of the foundation ground – subgrade (right). figure figure 8. location of the field trial tests: es 1: roller compaction; es 2: ric; es 3 and temporary dike: soil mixing. 10 shows the test embankment (left), constructed by using the silty sands from the top layer and the amount of coal particles (right) that floated up after the layer wetting. during compaction different modes of roller operation, layer thickness, drying and wetting of compacted layers were studied. the efficiency of the roller compaction was measured by using the nuclear gauge and by the calibrated cylinders to measure the water content and the density. stiffness of compacted layers was measured by static and dynamic plate load test. undisturbed samples were taken to check the liquefaction potential in the csst. the spt, cpt and the sdmt tests, planned to be realised at the test sites, were not possible, as the flood destroyed the trial sites soon after construction. 4.1.2. results and discussion at the foundation ground, the roller compaction was found not effective due to the influence of soft sublayers, coal particles and roots. the average achieved dp r, expressed as ratio ρd/ρd,max, was 88 % and the average stiffness, measured by the dynamic load plate test (zorn) was evd < 7 mpa. the efficiency of compaction on embankment layers strongly depended on the layer position above the ground level, as the influence of the soft subgrade decreases with the embankment height. at the level of 2 m above the subgrade, the average compaction of dp r = 94 % was achieved (figure 11), while the average stiffness of the embankment layers remained at the same average ranges as measured on the subgrade, evd = 5 − 10 mpa. figure 12 compares the results of dry densities (left) and water content (right), achieved by using the nuclear gauge and the calibrated cylinders. the nuclear gauge gives significantly higher values of water content, which can be explained by the presence of coal particles and the nuclear gauge water content mea21 a. petkovšek, m. maček, j. smolar acta polytechnica ctu proceedings figure 9. depth of the roots (left) and the size of the first of four test fields prepared to study the roller compaction efficiency (right). figure 10. finished test embankment (left) and the amount of coal particles (right). suring principles. figure 7 (red diamonds) shows the csst results on the undisturbed samples from the test field. the data conform well to the preliminary forecast. 4.1.3. experimental site es 1 conclusions with the use of roller compaction, it is not possible to improve the top soil layer in order to reduce its liquefaction potential. the dynamic and static load plate test results strongly depend on saturation/water content and therefore do not measure parameters, which are decisive for the intended purpose. 4.2. experimental site es 2: rapid impact compaction (ric) test fields 4.2.1. background the hpp brežice test sites represented the first attempt to introduce the ric in slovenia. the detailed description of the ric test site is given in vukadin [20]. to highlight the importance of the test method validity and reliability, we will focus our discussion on the results of the dmt and sdmt tests, not reported in vukadin [20], as well as on the results of the cpt and dpsh b test, interpreted from a standpoint differing from that of vukadin [20]. 4.2.2. ric test site description the locations of the test sites are shown in figure 8, while a view to the ric during operation and the test site layout is given on figure 13. rough dimensions of each test field were 18 × 25 m. before the ric was put in operation, the vegetation layer of app. 1 m had been removed from the test site. the thickness of the top layer was from 3.8 to 4.0 m, with the fines content between 21 and 66 %, water content between 16 and 21 % and the dry densities of 1.2 – 1.6 t/m3 [20]. the gw table was in the quaternary gravel. at each test field, a comprehensive program of field tests (cpt, dmt, sdmt, dpsh b and dynamic cone penetrometer (dcp) panda) was performed before and after compaction. the filed measurements were complemented by samplings from trial pits and laboratory tests. each test field was divided in 4 sections (p1 to p4, figure 13) in order to study the influence of different compaction modes on the compaction efficiency. the compaction point raster density increased from section p1 to section p4 and the compaction was executed in one, two or three passes. after each compaction pass the ground was levelled by filling the holes created during compaction with the locally available sand. the decision about the end of the compaction at each point was made considering two criteria: (a) the accumulated total settlement per pas of 800 mm, or (b) the minimal depth of settlement per blow less than 10 mm. the average energy per unit cell area was 800 (p1), 1160 (p2), 1000 (p3), and 1230 kj/m2 (p4). 22 vol. 10/2017 testing methods for mechanically treated soils figure 11. comparison of standard proctor test curve (spp) and dry density achieved during trial embankment compaction. figure 12. comparison between nuclear gauge and laboratory measurements of water content and dry density. 4.2.3. results and discussion the efficiency of ric was controlled by using different field test methods. this paper will focus primarily on the interpretation of the cpt, sdmt and dpsh b results. cpt test figure 14 shows the soil behaviour type (sbtn), the normalized cone resistance (qtn) and the sleeve friction resistance (fs) evaluated from the cpt test. the qtn is a non-dimensional parameter taking into account the in-situ vertical effective stress and the soil type and is not depth dependent. the fs depends on friction between soil and metal sleeve and horizontal effective stress. the horizontal stress increases with vertical effective stress (σ′v) and could be calculated by multiplying σ′v with horizontal stress coefficient during the cpt testing. the influence of compaction on the fs is given in two diagrams, as the relationship fs – depth and fs/σ′v depth. the fs/σ′v diagram presents the increase of horizontal stress coefficient during the cpt testing due to compaction. due to the impact of levelling of ground surface, the uppermost 1 m of the test field is excluded from the evaluation of the results. figure 14 shows that classification based on sbtn was not changed due to compaction (5: sand mixtures – silty sand to sandy silt and 6: sands – clean sand to silty sand). the qtn increases from the initial 40 to 60-160 after the ric. in natural ground the fs is increasing with the depth. after compaction the fs increases slightly to the depth of 1.5 m. at the depth of 1.5 m the sharp increase of fs is detected towards the value of 100 kpa. the fs/σ′v is constant with the depth before ric, thus indicating homogeneous ground conditions. after the ric the highest increase of fs/σ′v is observed at the depth of 1.6 m and then decreases with the depth towards the initial value at the depth of 4 m. the cpt test did not recognize effects of different compaction energies on the increase of qtn and the fs. figure 15 compares the qtn and the fs before and after ric. after compaction the qtn is 2 to 4 times higher and the fs is 2 to 6 times higher than before compaction. below the depth of 3 m the effect of ric is decreased. no influence of different compaction energies used for the compaction can be recognized. (s)dmt test the results of the dmt test are presented as intermediate parameters: material index (id), horizontal 23 a. petkovšek, m. maček, j. smolar acta polytechnica ctu proceedings figure 13. ric during compaction (left) and the test site es 2 layout (right – adapted from vukadin, [20]). figure 14. results of cpt tests. cpt 1 and cpt 2 before ric, cpt p1 to cpt p4 after ric performed on sub-fields p1 to p4 (tests performed by irgo, [19]). figure 15. results of cpt after ric compared to those before ric (tests performed by irgo, [19]). 24 vol. 10/2017 testing methods for mechanically treated soils stress index (kd), and dilatometer modulus (ed) (figure 16). the id and kd are effective vertical stress independent. the value of ed is presented also in relationship with the vertical effective stress (ed/σ′v) [21]. results show that the classification based on id changed a little due to compaction (mostly sandy silt and silty sand). the general soil behaviour type remains the same. below the depth of 1 m, thekd was around 5 before compaction. this value was higher than expected for normally consolidated soils [22]. after compaction the kd first increases and then, below the depth of 2 m, decreases; however, it remains slightly higher than recorded before compaction. the kd is related to fs [23], as the first one gives a ratio between horizontal and vertical effective stress during the driving of dmt, and the second one reflects the friction between soil and metal sleeve induced by horizontal effective stress during the driving of the cpt probe. therefore, the development trend of the kd with the depth should be of the same range as the developing of fs/σ′v. the ed increases with the depth before compaction, as expected, and results in higher values after compaction. the ed/σ′v exhibits nearly constant values with the depth before compaction and clearly increases after compaction. to estimate the ric efficiency with the depth, the values of kd and ed before and after compaction are compared (figure 17). the kd increases by 2 to 3 times and the ed increases by 2 to 4 times. the dmt tests after compaction exhibit almost no increase of kd and ed at the depth of 2 to 2.5 m. at the depth of 3 m both parameters start to decrease towards the values measured before compaction; however, the decrease is not as clear as in case of cpt. contrary to the cpt results, the dmt shows clear influence of compaction energy on the increase of the measured values. the sdmt enables measurements of shear wave velocity (vs). shear wave velocity depends on void ratio, effective vertical stress, stress history, cementation and over-consolidation (ocr) ratio [24]. the increase of all parameters with the exception of void ratio increases the vs. during compaction the void ratio decreases and the ocr increases. thus, the increase of vs is expected. figure 18 compares the constrained moduli (mv /cpt and md/dmt ) and the vs before and after ric. the right graph gives also the lines of vs, calculated by using the empirical equation (3) given by hardin and drnevich [25]. gmax = 1230 · (2.973 − e)2 (1 + e) · (ocr)k · p′ 1 2 (3) gmax = ρ · v2 s (4) where gmax is shear modulus at small deformations, ρ is density, e is void ratio, ocr overconsolidation ratio, k is empirical material factor (depends on plasticity index) and p′ is mean effective stress. figure 18 shows that before compaction, the vs, calculated after hardin and drnevich [25], is lower than measured and after compaction the calculated vs is close to the measured. when comparing the measured values of vs before and after compaction, no improvement and no influence of the compaction energy can be detected. cpt and dmt show the increase of constrained modulus (mv and md) after compaction. the range of measured values after compaction is similar. this is not in accordance with the findings reported by schmertmann [26], lee et al. [27], among others, who found the increase of dmt constrained modulus (md) higher than that of cpt (mv ). dynamic probing super heavy (dpsh b) dpsh b raw results are presented in figure 19 (upper line). before compaction the number of blows (n20sb) increases slightly with the depth. the n20sb values are lower than minimum required (5) according to en iso 22476-2. after compaction the n20sb values are higher and nearly constant with the depth, but the scatter of the result is high. from the n20sb the equivalent spt blow-count (n1)60 was calculated using the empirical equation (5) adapted after macrobert et al. [28] and using corrections given by ec 7.2. equivalent nsp t = n20sb 0.02 ·n20sb + 0.53 (5) dpsh b clearly indicates the efficiency of ric and the influence of compaction energy on the increase of the measured values. from this point of view, the sensitivity of the dpsh b test could be estimated as more indicative for the intended purpose than the sensitivity of cpt, dmt and sdmt methods. contrary to cpt and sdmt, the dpsh b confirms the compaction efficiency along the whole depth of the top layer, which was not observed by using the cpt and sdmt. the question for the discussion is: which method could be estimated as decisive? can we estimate the efficiency of the improvement by preferring optimistic test results (dpsh b) and neglecting less optimistic (cpt, sdmt) results? experimental site es 2, conclusions the analysis of the test results confirm that the ric technique is an effective tool for improving the geotechnical properties of silty and sandy soils, as it was already reported by adam and paulmichl [29]. however, the decision about the use of the ric technique to reduce the liquefaction potential must rely on the test results which are consistent and confirm without any doubts the efficiency of the improvement. as it was shown in the graphs, the scattering of the collected data raises serious questions about the validity, sensitivity and reliability of the test methods used to confirm the ric efficiency as well as questions about the homogeneity of the improvement. analysis of the results shows: 25 a. petkovšek, m. maček, j. smolar acta polytechnica ctu proceedings figure 16. intermediate dmt results. dmt 1 before ric, dmt p1 and dmt p4 after ric performed on sub-fields p1 and p4. figure 17. results of sdmt after ric compared to those before ric. figure 18. constrained modulus (mv-cpt and md-dmt)and measured/calculated vs (sdmt) 26 vol. 10/2017 testing methods for mechanically treated soils figure 19. comparison of n20sb and calculated (n1)60 values before and after compaction (tests performed by irgo, [19]). • the cpt and the dmt do not confirm the compaction efficiency along the whole depth of the top layer, while the dpsh b does • the cpt does not recognize the effect of compaction energy on the interpreted values, while the dmt and the dpsh b do • the sdmt (vs) does not recognize any improvement after compaction • the cpt and the dmt clearly recognize the less effective compaction at the depth of 2 m, while the dpsh b does not. although the dpsh b tests clearly show the efficiency of ric, the achieved improvement does not satisfy the criteria needed to reduce the liquefaction potential (figure 19). due to lack of previous experiences with the ric technique in slovenia and inconsistency of the test results, the ric technique was not recognized as a promising method for reducing the liquefaction potential. however, the authors of the paper believe that by preparing more test fields and by using slightly modified execution of ric and field testing, the results would be different and very probably more promising, too. 4.3. experimental site es 3: soil mixing 4.3.1. background the idea of soil mixing arose by joining three demands: (a) to reduce the liquefaction potential of silty-sandy soils, (b) to assure low enough permeability to avoid any additional sealing of the dikes, and (c) to improve the mixture willingness to compaction. 4.3.2. soil mixing test site description figure 8 shows the location of the test site and figure 20 gives a view to one of the test sites during test compaction and calibration of roller with ccc. as the results from the test fields were promising, an app. 1.2 km long temporary dike was constructed to protect the up to 70 m deep excavation and to gain additional data necessary to support the decision for the construction of 14 km long dikes (figure 21). 4.3.3. soil mixture demands before the soil mixing tests started, the designer prepared the requirement for the soil mixture, as follows: 27 a. petkovšek, m. maček, j. smolar acta polytechnica ctu proceedings • hydraulic conductivity lower than 1 × 10−6 m/s • shear strength must assure stable slopes at 1:1.75 (β = 30°) • homogeneity and good willingness to compaction • resistance to liquefaction, as already explained in previous chapters. 4.3.4. test program the test program was divided in five steps, i.e.: • mixture design, using the kozeny-carman equation • laboratory mixture preparation and testing • test fields on site to define the mixing and compaction procedures and to correct the laboratory mixture design, if necessary • construction of temporary dike with the qa-qc control tests during construction, using the ccc and conventional field test methods: the nuclear gauge, the dynamic and static load plate test and the double ring infiltrometer test • field testing on the temporary dike by using the sdmt, dpsh b and geohydraulic tests in boreholes. 4.3.5. the laboratory mixture design the mixture was proposed by using the kozeny–carman semi-empirical equation [30] [31] [32]. the equation relates the hydraulic conductivity to specific surface area, porosity and tortuosity. the main obstacle to wider use of the kozeny–carman equation is the specific surface area (ssa) of soil particles [33]. carrier [34], among others, proposed the estimation of ssa based on grain size distribution. the derived hydraulic conductivity based on the kozeny–carman equation and estimation of the ssa area based on grain size distribution is: k = 1.99×104  100 %∑ fi d0.404 i−1 ·d0.595 i  · ( 1 sf )2 · ( e3 1 + e ) (6) where k is hydraulic conductivity at 20 ◦c (cm/s), sf shape factor (6 for rounded grains), di particle size at sieve size i (cm), fi fraction between sieve i and i-1, e void ratio (%). the problem of the above equation is the determination of the finest fraction. based on chapuis in legare [35], 1/3 of the smallest measured grain size could be used for the estimation of an equivalent grain size of this fraction. fi d0.404 i−1 ·d0.595 i = fi 1 3di−1 (7) there are some limitations to the use of the kozeny–carman equation: • not valid for clays • valid for laminar flow of water (darcy law) and therefore not valid for clean, coarse gravel with pore size greater than 3 mm and large hydraulic gradients • the grains should be rounded or cubic (blocky) • soils with a long tail of small fractions (soils which are subject to internal erosion and segregation) can make problems. particles from the tail of small fractions are not in soil matrix but rather on larger grains. in this case the grain size distribution could be corrected by using 20 % of the increase of passing by 10 times of the increase of the grain size [33]. • anisotropy of hydraulic conductivity. it is assumed that the calculated value relates to the vertical hydraulic conductivity. the grading ranges of the available soils are given in figure 3. based on the kozeny–carman equation the mixture of sandy and gravely soil was proposed in mass ratio of 20:80 to 25:75 (figure 22). 4.3.6. laboratory testing the hydraulic conductivity of sands was measured in the triaxial cell and in variable head permeameters, while gravel and mixtures were tested in a large constant head permeameter. the diameter (d) of the large constant head permeameter was 304 mm and its height (h) was approximately 600 mm (figure 23). there were 9 piezometers on 3 levels to measure the local hydraulic head (total potential). the disadvantage of large constant head permeameter is poor compaction due to thin plastic walls. the smaller constant head permeameter (d = 150 mm h = 125 mm) enabled proper compaction of soils with maximum grain size of 31.5 mm. during the gravel tests in large permeameter a non-linear decline of hydraulic head in piezometers was observed. three hydraulic conductivities were calculated (average, maximum and minimum). this problem indicates possible segregation and anisotropy of compacted gravels. the results of the tests are presented in figure 24. the calculated hydraulic conductivity using the kozeny-carman equation are in agreement with the laboratory test results. the measured value on different mixtures was up to 10 times different than calculated. the reason for this is very probably in material segregation and imperfect saturation. in general, the laboratory tests confirmed predictions of the kozeny-carman equation and the suitability of proposed mixture. 4.3.7. test fields the dimension of the test field was app. 50 m × 10 m. each test field was made of two 55 cm thick layers of mixture. at the beginning, due to the rainy weather, it was difficult to assure the homogeneity due to the high 28 vol. 10/2017 testing methods for mechanically treated soils figure 20. vibratory roller during compaction on one of the test fields (left) and a view to the control pit in one of the test layers (right). figure 21. a view to the temporary dike, constructed from soil mixture and used as part of the large scale test embankment. figure 22. calculated ranges of soil mixture to achieve the required hydraulic conductivity (k < 10−6m/s) and stiffness. water content of the silty sandy soils. the achieved dry density and stiffness of the mixture were in direct relationship with the water content and the fines content, detected at each controlling point (figure 25). on mixtures with higher content of fines the achieved layer stiffness after compaction was lower. the difference in stiffness on different test tracks was clearly observed by ccc (figure 26). later on, the weather improved and the mixing processes and the compaction ran according to expectations. the decision was accepted to construct a temporary dike by using the soil mixture. 4.3.8. temporary dike construction control during the construction of the temporary dike, a comprehensive program of control test was realised, including the 61 sieve analyses and water content tests, 13 double ring infiltrometer tests, 325 spot tests – nuclear gauge. the ccc was used to control the stiffness and homogeneity. 53 gradation curves were inside the required area and 8 samples contained app. 1% lower content of fines than required. results of all hydraulic conductivity tests were inside the design requirements (figure 27). the average achieved density was 98 % of the modified proctor (mpt) maximum dry density. 4.3.9. temporary dike post construction control two years after the construction control tests were made from the dike crown. in three bore holes field water permeability (variable head) tests were performed at different depths. two tests (at depths of 2-4 m and 4-6 m) were performed in the dike and one test (at a depth of 6-8 m) in the foundation ground (figure 27). four tests in the dike met the design requirements (1 × 10−6 m/s) and two tests indicated k higher than required. results from four dpsh b probing are presented in figure 28. as the crown has been used as a temporary unsealed road for the needs of construction site for 2 years, higher n20sb values were observed at the depths up to 2 m below the crown. at greater depths 29 a. petkovšek, m. maček, j. smolar acta polytechnica ctu proceedings figure 23. a view to the permeameter cell (left) and a view to the surface of gravel and mixture (right). figure 24. comparison of calculated (kc) and measured hydraulic conductivity (k). the n20sb values were higher than recorded at the ric test sites. three sdmt probings were performed. before the test started, the boreholes were filled with dry uniform sand. therefore, a greater variation in result can be expected due to the effects of backfill. the third probe (sdmt3b) was repeated to check the repeatability of the results due to the difficulties during the test in probe sdmt3. the vs results in all probes at the dike were around 200 to 450 m/s and were significantly higher than those measured in the top layer before compaction and after the ric compaction. the measured shear wave velocities are close to the values calculated by using hardin and drnevich equation [25] (figure 28). 4.3.10. experimental site es 3 conclusions the kozeny-carman equation was found to be an effective tool for the design of the mixture with the given hydraulic conductivity considering the equation limitations. the laboratory test and the field double ring infiltrometer test results were in good agreement with the calculation. however, two of six tests in the borehole using open systems gave by a decade higher value of k. the ccc test results show that the compaction behaviour and layer stiffness of sandy gravel mixtures containing app. 10 20 % of fines are mainly controlled by the water content of fines. this means that even though the mixture is classified as silty gravel, its compaction behaviour is typical for less permeable soil mixtures. the achieved dry density after compaction, the sdmt (vs) and the dpsh b tests show that the mixture has properties of gravel. figure 29 shows that for a given csr the mixing of locally available soil is a promising method to reduce the liquefaction potential. however, the decision was made not to use the soil mixing for the construction of the dikes. all the soils from the top layer were removed and replaced by clean gravel. gravel was also used as fill material for all dikes and the sealing of the dikes was achieved by the geosynthetic bentonite barriers. 30 vol. 10/2017 testing methods for mechanically treated soils figure 25. results from the first test section. high water content in silty part of the mixture control the achieved stiffness and density. evd – dynamic deformation modulus measured by dynamic load plate test; evib – dynamic elasticity modulus of soil beneath drum (terrameter ccc system). figure 26. ccc record from one of the first test sections showing heterogeneity of the compaction. figure 27. comparison of hydraulic conductivity predicted after kozeny-carman equation (upper limit, lower limit) and measured values in laboratory and on site. 5. conclusion mechanical stabilisation for ground improvement has become a widely accepted system to support foundations for a wide variety of structures as well as for the construction of embankments and embankment dams. the use of mechanically stabilized locally available soils is also one of the top priorities of the philosophy generally understood as “sustainable development” [36]. the paper focuses on the interpretation of the results of the tests used for the control of the efficiency of some of the stabilisation techniques. the analysis of the tests shows inconclusive results. in foundation ground, where the requirements are different than those given for regular earthworks and the safety demands are higher, the use of different test methods is necessary. due to the lack of experiences, the use of different methods may lead to inconsistent results and often raises more questions than gives answers. understanding the local conditions and mechanisms that may influence the test results in different soil types/stabilisation techniques is important for engineering judgement and leads to the ability to make tough decision. however, past experiences are also important and sometimes a lot of time and energy are needed before a new method/ technique becomes widely accepted. 6. acknowledgement this work was funded by the hess and realised in close cooperation with irgo ljubljana. authors would like to express special thanks to mr. b.sc. andrej unetič (hse invest) for his help at realising the investigation program and to many engineers and technicians for their essential field work and data collection. the advice of prof. dietmar adam from tu vienna is highly appreciated. 31 a. petkovšek, m. maček, j. smolar acta polytechnica ctu proceedings figure 28. temporary dike. shear wave velocity, hydraulic conductivity, and results of dpsh b (from left to right). figure 29. diagrams for evaluation of liquefaction potential based on (n1)60 (upper) and vs1 (lower). bc – before compaction, fc – fines content, mix – soil mixture, ric – rapid impact compaction, ts – top soil layer. references [1] w. f. v. impe. soil improvement techniques and their evolution. aa balkema, rotterdam, netherlands., 1989. 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[8] ž. veinović, p. kvasnička, v. jurak. geohazard characteristics of the sava river plain near zagreb. konferencija razvitak zagreba 2008. acessed 15.9.2016. [9] i. idriss, r. boulanger. semi-empirical procedures for evaluating liquefaction potential during earthquakes. soil dynamics and earthquake engineering 26(2):115– 130, 2006. 11th international conference on soil dynamics and earthquake engineering (icsdee): part ii, doi:https://doi.org/10.1016/j.soildyn.2004.11.023. [10] d. aleksovski, g. mirakovski, d. dojčinovski, et al. he brežice geofizikalne raziskave in seizmična mikrorajonizacija,. geofizikalne raziskave in seizmična mikrorajonizacija, iziis univerze sv. kiril i metodij, skopje., 2008. [11] arso, slovenian environment agency. agencija republike slovenie za okolje. 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[16] t. l. youd, s. k. noble. liquefaction criteria based on statistical and probabilistic analyses p. 201–215, 1997. [17] r. d. andrus, k. h. stokoe. liquefaction resistance of soils from shear-wave velocity. journal of geotechnical and geoenvironmental engineering 126(11):1015–1025, 2000. doi:10.1061/(asce)1090-0241(2000)126:11(1015). [18] s. l. kramer. geotechnical earthquake engineering. prentice-hall international series in civil engineering and engineering mechanics. upper saddle river, new jersey., 1996. [19] irgo. he brežice, poročilo o impulznem globinskem zgoščevanju na testnih poljih. faza: pgd. report nr. ic161/11. ljubljana, slovenia., 2011. [20] v. vukadin. the improvement of the loosely deposited sands and silts with the rapid impact compaction technique on brežice test sites. engineering geology 160(supplement c):69–80, 2013. doi:https://doi.org/10.1016/j.enggeo.2013.03.025. [21] p. k. robertson. cpt-dmt correlations. journal of geotechnical and geoenvironmental engineering 135(11):1762–1771, 2009. doi:10.1061/(asce)gt.1943-5606.0000119. [22] s. marchetti. in situ tests by flat dilatometer. journal of the geotechnical engineering division 106(3):299–321, 1980. [23] j. m. o. hughes, p. k. robertson. full-displacement pressuremeter testing in sand. canadian geotechnical journal 22(3):298–307, 1985. doi:10.1139/t85-043. [24] r. dobry, m. vucetic. state of the art report: dynamic properties and seismic response of soft clay deposits. in proceedings of the intl. symposium on geotechnical eng. of soft soils, vol. 2, pp. 51–87. mexico city, 1987. [25] b. hardin, v. p. drnevich. shear modulus and damping in soils: design equations and curves 98:667–692, 1972. [26] j. h. schmertmann. comparing dmt with cpt in nc/oc sand bucket test. dmt digest (4), 1984. [27] m. lee, s. choi, m. kim, w. lee. effect of stress history on cpt and dmt results in sand. engineering geology 117(3-4):259–265, 2011. doi:10.1016/j.enggeo.2010.11.005. [28] c. macrobert, d. kalumba, p. beales. correlating standard penetration test and dynamic probe super heavy penetration resistance values in sandy soils. journal of the south african institution of civil engineering 53(1):46–54, 2011. [29] d. adam, i. paulmichl. rapid impact compactor an innovative dynamic compacttion device for soil improvement. in proc. 8th international geotechnical conference, pp. 183–192. slovak university of technology, bratislava, 2007. [30] j. kozeny. über kapillare leitung des wassers im boden, 136 (2a). hölder-pichler-tempsky, a.-g. akad. d. wiss., wien., 1927. [31] p. c. carman. the determination of the specific surface of powders. journal of the society of chemical industry 57:225–238, 1938. [32] p. c. carman. flow of gases through porous media. new york: academic press, 1956. [33] r. chapuis, m. aubertin. predicting the coefficient of permeability of soils using the kozeny-carman equation. école polytechnique de montréal 2003. [34] w. d. carrier. goodbye, hazen; hello, kozeny-carman. journal of geotechnical and geoenvironmental engineering 129(11):1054–1056, 2003. doi:10.1061/(asce)1090-0241(2003)129:11(1054). [35] r. chapuis, p. p. légaré. a simple method for determining the surface area of fine aggregates and fillers in bituminous mixtures. effects of aggregates and mineral fillers on asphalt mixture performance pp. 177–177–10, 1992. doi:10.1520/stp24217s. [36] i. vaníček. sustainable construction. ed. 1st. czech technical university in prague, prague, 2011. 33 http://dx.doi.org/10.3208/sandf1972.20.4_127 http://dx.doi.org/10.1061/(asce)1090-0241(2000)126:11(1015) http://dx.doi.org/https://doi.org/10.1016/j.enggeo.2013.03.025 http://dx.doi.org/10.1061/(asce)gt.1943-5606.0000119 http://dx.doi.org/10.1139/t85-043 http://dx.doi.org/10.1016/j.enggeo.2010.11.005 http://dx.doi.org/10.1061/(asce)1090-0241(2003)129:11(1054) http://dx.doi.org/10.1520/stp24217s acta polytechnica ctu proceedings 10:16–33, 2017 1 introduction 2 background 2.1 site description 2.2 geological profile 2.3 soil properties 2.3.1 index properties 2.3.2 liquefaction potential 2.4 preliminary conclusions 3 discussion on improvement technique 4 results from the experimental sites 4.1 experimental site es 1: roller compaction trial field 4.1.1 site description 4.1.2 results and discussion 4.1.3 experimental site es 1 conclusions 4.2 experimental site es 2: rapid impact compaction (ric) test fields 4.2.1 background 4.2.2 ric test site description 4.2.3 results and discussion 4.3 experimental site es 3: soil mixing 4.3.1 background 4.3.2 soil mixing test site description 4.3.3 soil mixture demands 4.3.4 test program 4.3.5 the laboratory mixture design 4.3.6 laboratory testing 4.3.7 test fields 4.3.8 temporary dike construction control 4.3.9 temporary dike post construction control 4.3.10 experimental site es 3 conclusions 5 conclusion 6 acknowledgement references acta polytechnica ctu proceedings doi:10.14311/app.2017.11.0053 acta polytechnica ctu proceedings 11:53–62, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app domains of railway traffic in the czech republic, which need the safety improvement dana procházková∗, jan procházka, tomáš kertis czech technical university in prague, faculty of transportation sciences, praha, czech republic ∗ corresponding author: prochdana7@seznam.cz abstract. the paper analyses the railway accidents sources in the czech republic on the basis of knowledge on complex system behaviour. it derives seven categories of sources of railway accidents. the individual categories include the accident sources from the same field domain. these domains are: technical related to rail traffic vehicles; technical related to rail infrastructure and railway station; railway operation control – organizational causes; railway operation control – cyber causes; control of rail traffic vehicles; attack on the train; domain legislative and other. the results show that for railway traffic safety improvement, it is necessary to pay attention to all categories, and especially to these that lead to organizational accidents origination. keywords: railway, railway accident, safety, security, criticality, railway accident causes. 1. introduction humans need infrastructures for their life quality and development. especially, at critical conditions the infrastructures’ operations support the human survival. the traffic infrastructure in present dynamic age has three basic tasks at critical conditions caused by disasters occurrences, namely to ensure: the human evacuation from afflicted region; the transposition of response units to afflicted region; and interconnections between afflicted region and its vicinity. therefore, its safety (the set of anthropogenic measures and activities that improve the system security) is the goal of human management and behaviour. from the general view the railway system plays very important role in terms of transportation in the european area. the transportation mode is widely used not only for middle and long-distances, but it has also very important role in short distances between small agglomerations and for the public transport in cities. therefore, the safety of railway system has long-term tradition as well as railway operating itself since twenties 19th century. it is very followed in the czech republic that has very dense railway network with 9458 km of rail track, including 1329 km of rail track for the international transportation within the european railway system. although the railway safety has the long tradition, the number of requirements on safety and their depths are increasing because the increase of population density and vulnerability of environ, in which the railway system operates. especially, in the european railway system the requirements on interoperability are very important [1]. because the social phenomena based on human intent were found as the significant threat, the security requirements have been step by step introduced into practice. from the system viewpoint there are other influencing aspects which affect the railway safety, e.g. the interconnection of cyber and physical systems, the human-machine interfaces and overall perceiving and handling with such complex systems, i.e. sociotechnological (technical) systems [2]. the practice shows that their violation is often the cause of serious railway accidents, and therefore, we need to protect the railway system against them. the monitoring of railway system and the critical assessment of previous railway accidents are necessary for understanding the complicated nature of railway system safety, for which reach there are necessary to implement the protective, mitigating, response and renovation measures. owing to complex structure of problem, it is also needed to understand the railway system in terms of integral safety that deals with systems of systems (sos) safety, because we also need to reduce losses caused by the cascades effects or by phenomena that are the consequences of interfaces between systems of completely different nature, i.e. technological, cyber, social, environmental etc. the results of research described in [3] show the causes of traffic accidents on railway and road that belong to the technical domain and the human factor domain, which is connected with drivers error. the present work is only directed to railway system. its goal is to obtain the detail findings that can help to improve the safety in the railway traffic, which is the important part of critical infrastructure. the next given results are based on the concept of integral safety of complex system with type "system of systems (sos)" [2]. the main target is to reveal real causes of railway accidents. the authors’ effort is especially focused on the recognition of risks that are connected with interdependences in the railway traffic system. they are mainly concentrated to those interdependences that are originators of organizing accidents, i.e. accidents caused due to bad human 53 http://dx.doi.org/10.14311/app.2017.11.0053 http://ojs.cvut.cz/ojs/index.php/app d. procházková, j. procházka, t. kertis acta polytechnica ctu proceedings decision or due to bad human management. 2. risk and safety if we want to ensure the safety of any system, we need to determine the sources of losses and damages (generally denoted by term "disasters") and to determine the sizes of their destructive potentials. it means that incident, accident and other similar phenomena are the subcategories of category "disaster" [4]. in the risk engineering we work with three fundamental terms: • danger marks the conditions of human system at which the origin of harms on protected assets has the high probability; it is almost sure that the harm will origin [5], i.e. the term marks the rate of conditions. it means that it goes on mark of possibility of origin of harm, loss or damage of one or more assets. the danger is predetermined by substance properties that are in facility, object or territory and by properties of processes that are running in facility, object or territory. it is immediate, if the course uncontrollably goes to the disaster origin that causes the emergency situation; and it is creeping, if the course goes to disaster origin inconspicuously and without clear-cut precursors [5]. the danger for human means both, the big phenomena (e.g. natural disasters, industrial accidents, environmental or social disasters) and the seemingly small phenomena from daily life as slump of snow, icicle or roofing from roof, rough pavement etc. [5]. • hazard marks the disaster potential to cause the harms, losses and damages on protected assets in a given site that is prescriptively determined. it goes on prescriptive measure of danger that is connected with the given disaster. for the strategic planning needs, the centennial disaster is often considered, i.e. the hazard is size of disaster that occurs once in hundred years, or professionally exactly, the disaster size that has return period 100 years; at special buildings and facilities it is considered from safety reasons the hazard determined by connected with thousand years’ disaster or ten thousand years’ disaster [5]. • risk connected with a given disaster is the probable size of damages, harms or losses on protected assets that originate in given place at origin of disaster with size of normatively determined hazard, which is normalized to the certain territory unit or number of individuals and the time unit [5]. the difference between risk and danger is the following: the danger is specific (it denotes the topical conditions) and the risk is only expected opportunity. the humans ensure the protection of human society and populated territory against risks by the way that for each disaster they determine the certain size (so called design disaster). they only perform the preventive measures so the possible risk size may be acceptable. the problem arises if disasters with size greater than design disaster occur, because great damages, harms and losses origin as the consequence of failure of man-made technological systems [2, 5–7]. from the practical reasons it is necessary to consider that the entity risk connected with the given disaster does not represent only the direct losses on assets but also the indirect ones; the indirect losses are caused by: delays or errors in response, cascades of failures caused by synergic and cumulative effects, which are caused by linkages and couplings among the assets; and by domino effects. due to the entity structure its risk is the integral risk that is expressed by following formula r(h) = [ ∑n i=1 ai(h)zi(h) +∑n i=1 ∫ t 0 ∫ f (h,ai, pi, o, t)dsdt ] ∗ τ−1 where: h is the hazard connected with the considered disaster; ai are the values of assets, i = 1, 2, ..., n that are considered in connection with complex technological facility safety, where n is the number of monitored assets; zi are the vulnerabilities of assets taken under account, i = 1, 2, ..., n; f is the loss function; pi is the occurrence probability of i-th asset damage – conditional probability; o is the vulnerability of safeguard measures; s is the size of followed territory/facility; t is the time that is measured from the origin of harmful phenomenon in facility; t is the time for which losses arise; and τ is the return period for the given disaster [2]. because the loss function f form is not known, we use for determination of total risk (i.e. the integral risk) the scheme given in figure 1 [2]. the problem is complicated by reality that the world is in dynamic development, i.e. both, the entity conditions and the risk sources are changing in time. moreover, there is necessary to respect that the risk and safety are not complementary quantities – it holds that the risk reduction leads to safety increase but at the same risk value the safety can increase if humans perform special measures or at their behaviour use special manners following from correct safety culture [2]. therefore, at solution of practical tasks connected with both, the entity safety and the entity risk, it is necessary to consider that risks are normal and for the entity safety it is necessary to apply not only the risk prevention measures and activities determined on the basis of correct intent and correct data and methods, but also: the safety culture by which the human behaviour in the entity and its vicinity is targeted to safety; and the tools that reduced losses and damages if some important disasters occur. therefore, it is necessary to prepare the qualified response for important risks realizations, such as: the risk management plans for both, the entity and the entity vicinity for all relevant risks; the continuity 54 vol. 11/2017 domains of railway traffic in the czech republic figure 1. flowchart for determining the risks for the strategic management of safety; a – assets and z losses, damages and harms to the assets; description: 1 – the human lives and health, 2 – human security, 3 – property, 4 – the public welfare, 5 – the environment, 6 – infrastructures and technologies, p – private. plans for survive of important complex technological objects and facilities; and the operational crisis plans for both, the complex technological objects and facilities and their vicinities. according to knowledge concentrated in [2], the risk engineering uses the following principles: • the risk is followed and considered during the given system whole life cycle, i.e. at sitting, designing, building, operation and putting out of operation, and eventually at territory bringing in original condition, • the risk determination is directed to user’s demands and to the level of provided services, • the risk is determined according to the criticality of impacts on facility processes, provided services and on assets that are determined by public interest, • the unacceptable risks are mitigated by tools according to technical and organisational proposals, by standardisation of operating procedures or by automatable check-up. the advanced risk engineering directed to human system safety respects the co-existence of systems with different nature (sos), and so fulfils present demands of humans [6]. to prepare groundwork it is necessary to combine analytical methods with expert judgement by which we remove vagueness in data. the problems that we need to solve in this consequence consist in acquisition of knowledge and in assignment "who is expert"; the last mentioned problem was broadly discussed in world conference esrel2011 [8]. for the first problem solution we need systematically to monitor the human system and obtained data to process by qualified methods [9]. the process model for work with risks is shown in figure 2 [5]. the criterions determine the condifigure 2. process model of work with risks targeted to safe entity. tions at which the risk is acceptable, conditionally acceptable or unacceptable. the aims in real case are selected from further given possibilities: to reduce risk to certain level; to secure the system, i.e. to ensure its security; to ensure safe system, i.e. to ensure security for system and its vicinity. the feedbacks are used in case if the monitoring shows that the risk is unacceptable; firstly, it is used the cheapest feedback 1; in case of its failure the feedback 2 etc.; at huge harms immediately it is used the feedback 4 that means the change of concept of work with risks. 3. criticality and safety management in followed context the criticality is directed to failures and hazards [10]. the infrastructure criticality needs to be determined on the basis of analysis of relevant and dangerous incidents and failures, losses and damages caused by functionality loss, outer disasters, mitigation measures, reactions and substances in a given facility, releases, leakages or discharges of substances (products’ pipelines) etc. the criticality determines the condition at which the system does not ensure expected functions in a required time, a site and in a required quality. to criticality of each partial infrastructure we can approach from two viewpoints, teleological and systemic [8]. from the teleological viewpoint it follows that the criticality is a result of role and function of partial infrastructure in the society. this concept enables to work with non-network and non-technical objects and processes. partial infrastructure criticality from the systemic viewpoint is a result of its position in the system or of its link to another partial infrastructure. from both approaches it follows that the partial infrastructure criticality also influences the system that is a social partial infrastructure created by public administration, business subjects, educational and research institutions and civic clubs. 55 d. procházková, j. procházka, t. kertis acta polytechnica ctu proceedings adopting the findings from the systems system safety management [10] the set of partial infrastructures in a region is critical one, if it is only capable to ensure activities at which there is only ensured human surviving in a given region. for this purpose, there have been in the world performed the analyses of sectors to which individual partial infrastructure belong and they have been followed the dependences among sectors, and the safety management then respect both, the conditions for functionality of individual partial infrastructures and the conditions for functionality of set of infrastructures; aggregated (critical) infrastructure. the term "criticality" was firstly used in a connection with the nuclear reaction where it denoted the threshold after which the spontaneous chain reaction followed. in connection with partial infrastructures and with critical infrastructure (set of infrastructures), the criticality is the most competently expressed by phrases: (1.) criticality is a relative measure of impacts of frequently occurred defects and failures. (2.) criticality is expressed by conditions that describe a transition between quality differ conditions. (3.) criticality is a condition of extensive urgency. from the given criticality definitions, it is possible to derive that the criticality is a threshold value that may be designed and that can relate to event, process/function parameter, type of defects and resistance. the determination of criticality is consistently related to a size of impacts caused by loss of functionality of each infrastructure on the society [10]. from this reason, at the criticality determination, it is necessary to consider: (1.) concentration of humans and assets (especially protected ones). (2.) sectors of economy (sector analysis). (3.) types of mutual dependences among the partial infrastructures/sectors: (a) on which item the assets of given sector are dependent? (b) what is the mutual dependence of assets among sectors? (4.) types of services for public: (a) how long has been taken the renovation of services furnishing? (b) which compensations/substitutes can be accessible and available? (5.) public confidence in the public administration institutions: (a) can defect of assets/public services result in a fall of moral of citizens, a loss of national prestige, panic, rebellion or civic disorders? (b) can defect of assets induce some impacts/changes in the environment? the determination of criticality in service of territory goes from the hazard assessment for disasters possible in a given region, considering the vulnerability of partial infrastructures in a given region, the mutual interconnections of partial infrastructures in a given region, i.e. theoretically the same principle as in analysis and assessment of risks in a region, at which several protected interests is considered. therefore, the criticality determination process is the following: (1.) characteristics of assets (there are considered physical, cyber and human assets). (2.) determination of criticality (hazard analysis and consideration of assets vulnerabilities in a given site). (3.) assessment of impacts on assets (concentration of humans and assets, economic impacts, mutual dependences, reliability). (4.) assessment of consequences of losses, victims, damages and harms of assets. (5.) determination of priorities according to the given rules. (6.) the criticality is mostly determined by scoring, i.e. by decision making matrix. the criticality matrix of infrastructure shows scaling the infrastructure vulnerability vs. infrastructure importance (i.e. its damage causes the infrastructure failure). for safe infrastructure operation there are used the tools: for middle criticality assets the continual monitoring and risk management plans for important risks; and for high criticality assets the operational crisis plans and continuity plans [2]. it is true that above described procedure shows that assessment of infrastructure/technology/set of infrastructures according to two criteria, namely measure of vulnerability and measure of importance of service in a region is not a result of objective computation of process analysis but rather result of subjective estimations, that is only tolerable in case of determination of basic frame. more complex it is the determination of criticality for some process. at scoring the vulnerability and importance of service it is necessary according to [2] to consider following items: duration of renovation of infrastructures and technologies; impact of failure of infrastructures and technologies on human lives and security; caused detriment, harms and loses; impacts on environment; and induced adverse situation. in the frame of ensuring the human system security and sustainable development it is necessary permanently to perform the measures that reduce an infrastructure criticality in a region. by building the new infrastructure it is necessary to ensure suitable number and regional distribution of objects of important infrastructure that are sufficiently resistant to expected disasters in a given region, and by that systematically to reduce infrastructure criticality. 56 vol. 11/2017 domains of railway traffic in the czech republic expenses for critical infrastructure are not only costs for its design and building but they also include costs for its operation, maintenance, repair and modernisation. therefore, the risks connected with each infrastructure must also include the risks from just given domains and the region management must know how to deal with them. it is necessary to assess the risks from disasters that can be denoted as financial market failure because with them it is connected failure of finances for maintenance, operation, repair and modernisation of objects of critical infrastructure. it is caused by the fact that infrastructure criticality increases if not good maintenance and good repair are performed (which cause the vulnerability increases). because nothing is out of defects, it must be prepared the plan for renovation of each infrastructure, namely critical one. this plan needs to be proactive, properly assessed; it needs to contain transparently managed risks and answers to questions as: (1.) what to do? (2.) how to do? (3.) in which time interval? (4.) do not risks for other protected interests in crease? etc. risk reduction in the context of safety management covers several topics: safety of processes; the protection of workers’ health and safety (safety of work); and reducing the impacts on the environment. therefore, in practice, it was introduced that the analysis of the impacts of management on the safety of the facility shall be carried out according to the reason model of organizational accident [11]. the causes of organizational accidents are in three basic aspects: organizational processes; the conditions which cause the origin of errors or infringements of rules; and no solved problems, which permit the errors and/or violation of regulations. safety management is increasingly focused on resilience due to increasing complexities and connectivity of real technological facilities. this is based on the concept that it is increasingly difficult to identify all the hazards and unwanted accidents, and therefore, to avert and reduce the consequences of various disorders it is important the resilience. investigation of failures and accidents of complex technological systems indicate that these are often caused by a combination of several improbable accidents and the capability of their predictions means to avoid combinations that have the potential to cause accidents, accompanied by large losses, which should enhance the safety. the procedures and tools are described in [2]. 4. data on railway system criticality and accidents the railway system including the trans-european transport network corridors and also the local specific rails creates the complex transportation infrastructure. in many cases it goes on the critical infrastructure, because the railway system ensures the state basic functions for human survival in the territory, state and may be also on the continent level at critical conditions. the elements of critical infrastructure, therefore, need the special attention, study and approaches for increasing their resilience, i.e. it is necessary to ensure their robustness, durability and adaptability with regard to the origin of non-acceptable events. in other words, it means to secure the systems under consideration in which the individual elements are located. individual elements shall also to have inherent safety so that they and their surrounding (i.e. public assets in their vicinity) might not be endangered by their imperfection and failure. certain level of safety shall be also provided the less important local elements of systems with less importance, the location and nature of which can cause at their failure the significant problems to the whole system, and at huge failures they could cause the losses on public assets (including the human lives and health) in immediate or far off surrounding [9]. by introducing the new technologies which are not well verified in practice, and by increasing the system interdependences caused by interface of cyber, material, energetic, economic, social etc. technologies, the systems are becoming more complex. it is the fact that the complexity influences the system safety, because it leads to increasing number of possible systems’ conditions, and also to the origin of non-assessable emergent phenomena, i.e. phenomena which occur at certain conditions suddenly and unpredictably [2]. in work [12] the criticality rates for individual types of transportation infrastructure in the czech republic were judged by experts from the areas: transportation; transportation management in the territory; supply chains; public administration; and the integrated rescue system. the experts assessed 14 factors and the result was determined by using the multi-attribute utility theory. the result showed that the rail transport has very high criticality rate. regarding to just describe research results, it is necessary to trade-off with risks very carefully and to use the advanced tools of risk engineering. for investigation of railway accidents, two databases were compiled [13]. the first one was created for the whole world by help of internet [14] with using the passwords "rail disasters", "railway disasters", "rail accidents" and "railway accidents", especially from the sources [15–18]. the second one was created on the basis of national data that are given in the database of the rail safety inspection from the period 2006 up to 2015 [19]; it contains 204 special reports on railway accidents in the czech republic and in some reports the description of similar accidents that happen in another sites since 2006 and were not often the object of investigation of inspection. 57 d. procházková, j. procházka, t. kertis acta polytechnica ctu proceedings 5. methods used at data processing the data on railway traffic accidents in database [13] are judged in the context of integral safety of railway system, i.e. not only from the viewpoint of railway system, but from the human security and development. the data are processed by current statistic methods and by special risk engineering procedures as the cba, separation of accidents into seven accident sources’ categories, determination of logic interconnections among the accident sources and their expression by fish-bone diagram [20]. 6. items important for safety improvement of railway traffic in the czech republic data summarizes in [13] show that the railway accidents have been reported since 1650. the first described accident originated in whickham, county durham, uk two boys die when they are run down by a wagon on a wooden coal tramway. the continuous reports are after the accident in philadelphia, county durham, uk on july 15, 1815 that was described by words thirteen or sixteen people, mainly spectators, are killed and 40 are injured by the boiler explosion of the experimental locomotive. comparison of data in [13] shows that the worst train disaster in the rail history was caused by tsunami on sri lanka at december 26, 2004 – the death of over 1700 people. from the same source it follows that the railway accidents often occur in india; the biggest accident was in the state of bihar in june 6, 1981, it died more than 800 people when passenger train derailed when it had crossing the bridge over the bagmati river. the huge consequences have the railway accidents of freight trains shipping the hazardous substances. the huge railway accidents with presence of hazardous substances was on the january 6, 2005 in the us, graniteville, south carolina at which 9 people died, more than 250 people were injured when the freight train collided head-on with a parked local freight train near the avondale mills plant in graniteville. 16 wagons (including a tank car that ruptured 90 tons of chlorine gas into the air) derailed in the accident. the us ntsb determined that the cause of the accident was the failure of the local freight’s crew members to realign the switch for mainline operations. very great accident of freight train was on the july 6, 2013 in lac-mãľganic, quebec, canada (figure 3). the freight train containing 72 tank cars of crude oil runs away unattended and derails. several wagons explode, destroying over 30 buildings in the town’s centre, roughly half of the downtown area, and requiring the demolition of all but three of the remainder of the buildings in the downtown area due to contamination by petroleum from the train; these combine to require the evacuation of 2,000 people, a third of figure 3. consequences of freight train accident in lac-méganic, quebec, canada on july 6, 2013 [19]. the town’s population. 42 are confirmed killed, along with 5 missing and presumed dead, making this the fourth-deadliest rail accident in canadian history. the results of detail study of railway accidents with presence of hazardous substances are in [3]. the analysis of consequences of railway accidents in the czech republic given in [13] shows that there is only considered the direct loses on humans and rail traffic components. to the accidents’ costs there are not included the costs on responses performed by the integrated response system, the costs on renovation and the costs for alternative traffic serviceability. the sites of rail accidents in the czech republic in the period 2006 up to 2015 are shown in figure 4. from this figure it follows that rail accidents occur on all railways; mostly on the railways with high frequency shipping. the main causes of accidents and near-misses in the czech republic supplemented by the accident causes from the world that are possible in our country due to present situation (e.g. cyberattacks) were revealed in domains [21]: • technical – related to rail traffic vehicles, • technical – related to rail infrastructure and railway station, • railway operation control – organizational causes, • railway operation control – cyber causes, • control of rail traffic vehicles, • attack on the train, • legislative and other. founded technical causes related to rail vehicles (as locomotive, coach, car, wagon, freight car) are the following: • errors in design or at construction of traffic vehicle (wrong wagon or locomotive construction from the stability viewpoint, inappropriate location of fuel tank or power conductor at a terminal block in the locomotive – possibility of short circuit etc.), • wrong maintenance of locomotive or wagons, 58 vol. 11/2017 domains of railway traffic in the czech republic figure 4. places of railway incidents in the czech republic. • wrongly performed technical overhaul of traffic vehicle, • wrongly performed the repair of rail traffic vehicle (e.g. brake systems, mechanical parts of brake systems, mainly in the case of car hand brake), • wrongly loaded wagons, • wrongly closed wagon doors, • sudden technical fault of locomotive or some of wagons (damage of axle bearing, engine broken, traction interruption, direction controller out of operation, or failure of another crucial device, outage of air-conditioning etc.), • fuel shortages or power outage, • failure of technical equipment of locomotive control system (broking the speedometer, outage of radio connection with control centre (dispatching) etc.), • malfunction of redundant system when it is needed. founded technical causes related to rail infrastructure and railway station are the following: • siting the railroad in the territory (steeper gradient, insufficient load capacity of rail track foundation, sharp rail swerve, a lot of unprotected crossings with roads or field roads, tall and lush vegetation caused the decrease of visibility etc.), • construction errors at the railway station design and building (too short operating space, sitting the rails in the direction in which the tall buildings are, which decreases the view of engine-driver and switchmen (shunter operator) in the case of change of position of rail vehicle, headwind etc.), • rail track condition (error in construction, disorder in the railway station area, wrong maintenance – ruggedness, ice, snow, rail track drift, cracked rail switch, unanchored rail track to sleepers etc.), • missing the periodic overhauls of rail tracks, • wrongly performed technical overhaul of rail tracks (no detection of cracked rail switch), • failure of early repair execution of identified relevant faults on the rail track or on signalling equipment, • missing the signalling equipment or it has insufficient power, • sudden technical failure of operation control devices (insufficient maintenance, fault or failure of technical equipment of control system in operation control centre, etc.), • equipment layout for service of rail vehicles (refuelling, loading and unloading of goods, entrance and exit of passengers etc.), • physical damaging the railway station or rail tracks (war, robbery attack, terrorist attack, vandalisms etc.), • siting the train to the wrong rail, • obstacles on the rail tracks, • insufficient radio equipment of railway station, • deficit of knowledge and experience of railway station service (e.g. worker who operates the movement of rail vehicles on rail tracks in railway area etc.), • out of function of warning system at railway station signalling the minimal safe distance between two trains that are on one rail track. founded causes related to railway operation control the – organizational causes are the following: • wrong setting up the train route, • failure of start-up of operation of crossbars, lights or sound signals before train arrival to crossing the rail tracks with road or field road, • keeping the obstacles on the rail tracks, • insufficient identification of rail track, • insufficient identification of crossing the rail track with road or field road, • guiding the train approaching to railway station on the incorrect rail track (train collisions, derailment etc.), • bad decision of train dispatcher (wrong evaluation of report from police and stopping the train operation at another rail track than at this on which the obstacles were occurred, • non-passing the information on fire to the enginedrivers of relevant trains, • wrong consideration of meteorological conditions (wrong information to engine-driver), • dispatching the wrong instructions to trains owing to the control system failure in dispatcher workplace (e.g. as a consequence of electricity outage, the pc outage etc.), • dispatching the wrong instructions to trains owing to the dispatcher (controller) error or ignorance, • chaos at operation control/dispatcher workplace/room (wrong information to engine-drivers, information delay etc.), 59 d. procházková, j. procházka, t. kertis acta polytechnica ctu proceedings • deficiency in railway station staff (train collisions etc.), • wrong maintenance or wrong platform lighting, • wrong communication between train dispatchers at setting up the train routes, • insecurity of movement of shunted vehicle, • shunters are not furnished by a red signal lighting, • insufficient training the shunters, • insecurity of control at crossing the rail track with road or field road at train shunting, • error of railway station staff (at train guidance, cleaning the railway station and rail tracks, rail station and rail tracks maintenance etc.), • wrong communication between the operation control centre and companies which repair the rail tracks, • wrongly distributed responsibilities at the operation control centre, • insufficient communication among the enginedrivers in service area, • insufficient knowledge and experiences of staff in the operation control centre, • absence of instructions for support to engine-drivers who occur in unexpected emergency up to critical conditions. founded causes related to railway operation control – cyber causes are the following: • distortion of data from monitoring – the operation data acquisition system (false information to the engine-drivers and from engine-drivers, chaos at operation control centre etc.), • false software (it does not consider all possible variants of possible operational conditions, from which it follows the false instructions to engine-drivers and other staff), • insufficient hardware (wrong data processing and evaluation, dispatching the false instruction to engine-drivers in operation owing to pc failure, delay of reports etc.), • hacking attack to control centre of dispatch workplace. founded causes related to control of rail traffic vehicles are the following: • error of engine-driver at train control – e.g. forbiddance of train drive behind the semaphore with signal forbidding the train drive (e.g. signal at danger), non-keeping the view conditions at bad visibility (owing to health conditions, tiredness, stress, wrong information from the rail operation control centre, failure of critical equipment of locomotive or other vehicle due to wrong maintenance, incorrect evaluation of situation as reduced speed signalling owing to effort to correct the disharmony with the time table, bump to obstacle on the rail track, turn off the functional device instead of faulty one – exit and entrance to the station, derailment, non-use of wedge at train stop at train shunting etc.), • engine-driver fault at assessment of meteorological conditions (hoar, snow drifts, obstacles on the rail track etc.), • engine-river fault at unexpected conditions occurrence (owing to insufficient preparation for coping with emergency conditions – storm, reduced visibility etc.), • engine-drive fault at locomotive preparation for drive (bad instruction studying before the drive – e. g. regarding to freight, wrong setting the speedometer, false adjusted input data for the drive, e. g. at expensive goods shipping etc.), • engine-driver fault at radio control, • wrong co-operation of engine-driver, conductor and other train staff, • fault of engine-driver at reporting (using the false train code – short distance between trains), • fire or smoke in locomotive, passenger cars, in cargo wagons, or the engine fire, • bad intent of engine-driver (change of speed, nonresponding to instructions from the control – dispatcher – centre or from surrounding trains, etc.), • engine-driver ignorance of procedures of train control (at unexpected emergency up to critical situations – e.g. obstacle on the rail track etc.). founded attacks on the train are the following: • rocket/missile from another train or buildings lying outside the track (throwing the stones and other heavy objects from the bridge above the rail track on the train etc.) • intent damage of rail track or track foundation, • illegal act in the train, • bad dispatcher intent, • bad intent of railway station service staff (worker guiding the movement of train at the railway station), • train collision with aircraft or another flying object. founded legislative and other causes are the following: • lack of regulations which prevent the wrong track setting at railway station, • missing the precise instructions for performance of maintenance of train body, rail tracks, track foundation and rail track vicinity, • missing the texts of intelligible and precise instructions for communication between engine-driver and control operation centre, • the absence of a uniform system of marking the railway crossings with roads and field roads serving 60 vol. 11/2017 domains of railway traffic in the czech republic figure 5. causes of railway accidents in the czech republic. to their identification from the viewpoint of rail and road topologies, enabling the direct designation and informing, • inappropriate behaviour of passengers at boarding, train drive or exit from train (non-observing the instructions, indiscipline, poor care on children behaviour at the train), • soggy or else damaged rail track foundation, • behaviour of road vehicle drivers on the road and rail level crossing (non-respecting the traffic symbols, sound signals or obstructions). the fish-bone diagram showing the main categories of railway accident causes is shown in figure 5. it only contains six main categories of causes. the diagram helps the specialists and the paper readers to in-depth insight into the problem of railway accidents. we see the causes arranged according to affinity, which enables to look up the possible actions, i.e. the measures for railway system safety improvement, for the whole groups of accident causes. because some accident causes repeat, it is necessary to prepare quality technical and organisational measures. sometimes, the relative simple measures can avert the accidents; the examples belonging to this category are for example the following: • the many railway accidents are on the crossing the rail track with road or field road where safety is only ensured by the symbol on the road "cautionary cross", • the huge material losses are at accidents of freight trains with expensive goods or with hazardous substances, • all rail track crossings with field routes are not denoted by warning symbols, • rail track crossings with routes are not clearly identified, • many works do not respect simple rule "the responsible person for order is the person who gives it, and the responsible person for order implementation is the person, who has to carry out it". therefore, it is necessary to pay attention to freight trains, the check-up from the side of rail workers at train loading seems very necessary – for this purpose the special check lists are necessary to prepare. for communication at critical situations it is necessary to prepare the texts of reports that are clear, concise and comprehensible. there are necessary rules for maintenance, regular technical overhauls of rail tracks etc. generally, it is necessary to take into account that accidents can occur and for these cases to prepare both, the train personnel, especially the engine-drivers and the railway stations personal, especially those who set up the train rotes. because each train accident means the reduction of traffic service and also costs for responses that are performed by the integrated rescue system that is paid from the public sources, the state administration needs to prepare legislative for improvement the safety in rail sector. 7. conclusion the railway accidents in the czech republic were divided into seven categories according to the accident sources. individual categories have the same domain of accident sources – technical – related to rail traffic vehicles; technical – related to rail infrastructure and railway station; railway operation control – organizational causes; railway operation control – cyber causes; control of rail traffic vehicles; attack on the train; legislative and other. for railway traffic safety improvement, it is necessary to pay attention to all categories and especially to this that lead to organizational accidents. the critical analysis of railway accidents revealed that some of accident causes often repeat, e.g. the insufficient maintenance, low-class overhauls and renovation. they have immediate cause that is not the root cause of such accident type; the root cause is in poor safety culture in the sector and in deficits in training. our research will continue in preparation of real tools for individual sectors of followed domain such as check lists, risk management plans and operational crisis plans for great railway stations, especially those in which the hazardous substances in great amount are present. acknowledgements authors thanks to czech technical university in prague for support (grant sgs2015-17). references [1] eu. directive 2004/49/ec of the european parliament and of the council of 29 april 2004 on safety on the community’s railways and amending council directive 95/18/ec on the licensing of railway undertakings and directive 2001/14/ec on the allocation of railway infrastructure capacity and the 61 d. procházková, j. procházka, t. kertis acta polytechnica ctu proceedings levying of charges for the use of railway infrastructure and safety certification (railway safety directive). [2] d.procházková. safety of complex technological facilities. saarbruecken: lambert academic publishing, 2015. isbn: 978-3-659-74632-1. [3] d. procházková, j.procházka, h.patáková, et al. kritické vyhodnocení přepravy nebezpečných látek po pozemních komunikacích v čr. čvut v praze, 2014. isbn 978-80-01-05599-1. [4] g.giannopoulos, r.filippini, m. schimmer. risk assessment methodologies for critical infrastructure protection. part i: a state of the art. european commission, joint research centre, institute for the protection and security of the citizen, eur 25286 en. luxembourg: publications office of the european union, 2012. isbn:978-92-79-23839-0. [5] d.procházková. analýza a řízení rizik. čvut v praze, 2011. isbn 978-80-01-04841-2. [6] d.procházková. strategie řízení bezpečnosti a udržitelného rozvoje území. čvut v praze, 2011. isbn 978-80-7251-243-0. [7] d.procházková. rizika spojená s pohromami a inženýrské postupy pro jejich zvládání. čvut v praze, 2014. isbn 978-80-01-05479-6. [8] ch.bérenguer, a. grall, c. g. s. (eds). advances in safety, reliability and risk management. london: taylor & francis group, 2012. isbn 978-0-415-68379-1. [9] d.procházková. základy řízení bezpečnosti kritické infrastruktury. čvut v praze, 2013. isbn 978-80-01-05245-7. [10] d.procházková. challenges connected with critical infrastructure safety. saarbruecken: lambert academic publishing, 2014. isbn: 978-3-659-54930-4. [11] j.reason. human error. cambridge: cambridge university press, 1990. [12] j. procházka, d.procházková. criticality of transportation infrastructure in czech republic, iricon 2016. acta polytechnica ctu proceedings, 2016. isbn: 978-80-01-06022-3, issn 2336-5382. 5. [13] archiv poznatků o pohromách a haváriích. čvut v praze, fakulta dopravní. [14] google. "www.google.com". [15] railway-technology. "www.railway-technology.com". [16] revolvy. "www.revolvy.com". [17] isdo. "www.isdo.org". [18] u. dot. railway accident reports. "http://specialcollection.dot.library.dot.gov/home". [19] d. inspekce. archiv. "http://www.dicr.cz". [20] d.procházková. metody, nástroje a techniky pro rizikové iženýrství. čvut v praze, 2011. isbn 978-80-01-04842-9. [21] t.kertis, d.procházková, j.procházka. railway accidents in the czech republic, causes of risks and their mitigation, in: esrel 2017 proceedings. london: crc pres / balkema. in print. 62 acta polytechnica ctu proceedings 11:53–62, 2017 1 introduction 2 risk and safety 3 criticality and safety management 4 data on railway system criticality and accidents 5 methods used at data processing 6 items important for safety improvement of railway traffic in the czech republic 7 conclusion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.11.0063 acta polytechnica ctu proceedings 11:63–69, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app possible ways of improving railway operation and infrastructure in area between děčín and rumburk pavel purkarta,∗, david vodáka, tomáš hořeníb, tomáš javoříka a department of transportation systems, ctu in prague faculty of transportation sciences, prague, czech republic b metroprojekt praha a.s., prague, czech republic, graduate of ctu in prague faculty of transportation sciences, prague, czech republic ∗ corresponding author: purkapav@fd.cvut.cz abstract. this paper is dealing with improving the railway transport on axis děčín – rumburk. this journey can be undertaken in two possible ways (as an interstate one or an international one through germany), however the connections between trains are limited (especially problematic is the rumburk junction, where the connection would be desired). the aim of this paper is to improve the connections in the whole area, in order to reach the maximal effectiveness of a railway passenger transport. keywords: rumburk, děčín, ústecký region, railway transport, periodic timetable, node, service conception, travel times reduction. 1. introduction and goals 1.1. researched area the researched area is located in ústecký region near borders with federal republic of germany, particularly in the area between towns děčín and rumburk (mainly north and south from děčín). the most significant towns in the area are děčín, česká kamenice, rumburk, varndorf and šluknov. whole area is also very attractive for tourists – some railway lines are located very close to the borders of national park české švýcarsko. following railway lines can be included into the researched area (numbers according to the timetable 2016/2017 [1], see fig. 1): • railway line 080 in the section česká lípa – jedlová, • railway line 081 děčín – benešov nad ploučnicí – jedlová – rumburk • railway line 083 děčín – bad schandau – dolní poustevna – šluknov – rumburk, • railway line 084 rumburk – panský – mikulášovice with bypass panský – krásná lípa (– rumburk), • railway line 086 in the section benešov nad ploučnicí – česká lípa, • railway line 089 liberec – zittau – rybniště, • railway line rumburk – jiříkov – ebersbach without regular passenger transport. 1.2. reasons behind selecting the researched area main reason for selection of this area was restoration of operation on border crossing dolní pustevna sebnitz in the year 2014. this brought certain changes in service conception in the area. unfortunately, those changes also caused some connection between trains in the station rumburk to disconnect. despite the fact, that some conceptual changes were made after the year 2014, current situation is still not optimal and that is why the problem is still topical. after the opening of border crossing dolní pustevna – sebnitz, most of the trains in rumburk were concentrated to the time period around minute x.30 [1], but it did not created periodic timetable node, because many trains remained without mutual connection due to infrastructural issues. it is also hardly possible to consider it partial periodic timetable node, because connections were actually interrupted, rather than made functional. change in passenger service conception came with the activation of railway station markvartice, where regular crossing of the passenger trains was moved. paradoxically, this made the creation of connections in the railway station rumburk even more matter of distant future. this step creates really close sequence of trains děčín – jedlová – rumburk and děčcín – česká lípa in the section děčín hl.n. – benešov nad ploučnicí that disrupts periodic sequence of trains in this section. therefore, effect of implemented conceptual changes is questionable. if the goal was to disconnect links to ec trains in the station děčín hl. n. (due to their limited reliability – more frequent and higher delays, compared with average values), it is possible to understand those changes. on the other hand, it is also possible to see those actions as a form of resignation to solve problems where they appear. formulation of those reasons made the team of authors to reflect on this issue and they attempted to find a solution. this solution should solve all the problems and also offer attractive pass through the railway 63 http://dx.doi.org/10.14311/app.2017.11.0063 http://ojs.cvut.cz/ojs/index.php/app p. purkart, d. vodák, t. hoření, t. javořík acta polytechnica ctu proceedings figure 1. diagram of railway network in the researched area. junction rumburk for the passengers. importance of this pass through is regional, but still important. 2. understanding and solving the issue solving of the issue was performed in several steps, as it is usual in transport planning: • detailed analysis of the commuting in the researched area in the relation to the railway transport and its possibilities, • specifying the principles of new service conception and important construction points of the periodic timetable • detailed design of service conception, • specifying necessary infrastructural changes to reach service conception 3. solution of the issue 3.1. summary of facts about commuting in the researched area to asses meaningfulness of transit through the railway junction rumburk it is necessary to evaluate regular commuting in the researched area first. to do so, data from the national counting of inhabitants, houses and flats 2011 [2], has been used. the evaluation of data shows following: • from the regional point of view, both commuting to děčín and rumburk are important. the closer to děčín or rumburk a populated area is, the more people are commuting, • part of inhabitants also commutes to smaller cities such as česká kamenice, benešov nad ploučnicí, šluknov and etc. • very significant is commuting to the regional capital ústí nad labem, but commuting to another regional capital – liberec, has also been found in a part of the area (railway line 038), • many inhabitants from the rumburk area are commuting to varnsdorf and we also cannot omit the influence of česká lípa, • it is appropriate to ensure availability of prague for whole area, • breaking branches of railway lines 081, 083 in rumburk does not influence major numbers of passengers (breaking somewhere else can have worse consequences), but their connection may bring significant improvement of transport in the whole area (direction to/from varnsdorf) of transport to larger cities – that makes this idea meaningful. it is crucial to identify transport relations, which would pass through this junction, to defend creation of connections in rumburk. as it has been already 64 vol. 11/2017 possible ways of improving railway operation and infrastructure mentioned – good connections and fast pass through station rumburk may attract many local inhabitants. significant interactions in relations šluknov – varnsdorf, velký šenov – varnsdorf, mikulášovice – varnsdorf, were identified in regular commuting. another relations, which can be considered as long distance commuting, were also identified. improving of pass through rumburk could have positive effect also on these relations. there is a potential of 250 – 300 regular commuters in villages located only near railway lines (with acceptable walking distance from village to railway line), this number is sufficient enough to take this into consideration. however it is necessary to prefer more important transport relations in order to not create a negative impact on them. 3.2. design of the new service conception design of the new service conception was made according to all the periodical timetable rules. the most important passenger line, which should eliminate all problems in the station rumburk, is new passenger line děčín – benešov nad ploučnicí – jedlová – rumburk – dolní poustevna – sebnitz – bad schandau – děčín. it is proposed to connect branches of both lines děčín – rumburk (an interstate one and an international one through germany) and create pass through model in the station rumburk. basic interval is 120 minutes. interval is shortened to 60 minutes in the section děčín – česká kamenice (– jedlová). another section with interval 60 minutes is děčín – schöna. combination of the new line and long-distance trains in the section jedlová – rumburk – šluknov – dolní poustevna also creates interval of 60 minutes (long-distance trains in the section šluknov – dolní poustevna are operated only on work days). it is crucial to establish important line construction points for periodical timetable. key connection in the station děčín is connection to ec trains from/to prague (node in the minute x.00). extra trains should be extended to/from ústí nad labem in the time of afternoon rush hours, as a fast connection to the regional capital (ec trains are operated only in 120 minutes interval). these trains should be operated with minimum stoppings (in the section děčín – ústí nad labem). other important construction point is in the station jedlová in minute x.00 and in the station rumburk in minute x.30 (because of important connections). second line branch from děčín, in direction bad schandau, arrives to děčín in the minute x.00. there are important connections to long-distance trains děčín – ústí nad labem – lovosice – praha and regional trains děčín – most. both railway line branches, which are entering the junction have the connection to/from prague ensured. in one case the new connection is faster than the one in current timetable. there are 4 vehicles necessary to provide base interval of 120 minutes (without reserve). those trains are also capable of ensuring extra trains děčín – schöna. another two vehicles are necessary for extra rush hour trains ústí nad labem – děčín – česká kamenice – jedlová (without reserve). together with designing new circular line, service conception of the lines in the area was also modified. this includes long-distance trains ústí nad labem – liberec and kolín – rumburk – šluknov and regional trains děčín – česká lípa, jedlová – česká lípa or rybniště – varnsdorf – liberec. also new routes of mikulášovice dolní nádraží – panský – rumburk – ebersbach trains were designed, in case of shortening intervals (mikulášovice dolní nádraží – panský – rumburk) or restoring the regular passenger operation (rumburk – ebersbach). and finally routes for a pair of seasonal tourist trains děčín – jedlová – krásná lípa – panský – mikulášovice dolní nádraží has also been found. complex design of whole system is summarized in the network diagram (fig. 2). 3.3. infrastructural changes necessary for the new service conception following infrastructure modifications are necessary for the application of designed timetable: • reconstruction of the railway station rumburk, so it can handle the operation of periodic timetable node at minute x.30, • reducing the travel times at the benešov nad ploučnicí – rumburk branch (reducing time by 2 or 3 minutes, in some parts of the branch reduction could be reached by using modern vehicles) • reducing the travel times at the rumburk – panský – mikulášovice dolní nádraží and rumburk – šluknov – mikulášovice dolní nádraží branches (reducing time by 5 minutes), • reducing the travel times in the section jedlová – česká lípa to the systematical travel time 30 minutes, • reducing the travel times of long distance trains in the section bakov nad jizerou – česká lípa by 10 minutes, • consider necessary modifications of the stations on railway lines 081 and 083, • in case of implementing a pair of seasonal tourist trains, it is necessary to divide section panský – mikulášovice into two blocks. 3.4. reconstruction of the railway station rumburk new timetable brings higher requirements for continuity and stability of train operations in the station rumburk. 65 p. purkart, d. vodák, t. hoření, t. javořík acta polytechnica ctu proceedings figure 2. network diagram summarizing proposal of service conception in the researched area. 66 vol. 11/2017 possible ways of improving railway operation and infrastructure railway station rumburk is junction for four railway lines from four directions with four neighboring railway stations: • krásná lípa (railway line 081), • šluknov (railway line 083), • panský (railway line 084 – currently with regular passenger transport only on weekends), • jiříkov (currently without regular passenger transport – not numbered). designed timetable assumes regular passenger transport on all four railway lines. new timetable is periodical with base intervals 60 or 120 minutes. in addition, full periodical timetable node in the minute x.30 is established in the station rumburk. first 3 railway lines above are connected to the western part of the station. railway line from jiříkov is connected to the eastern part of the station. operation on station head in the western part of the station, where three railway lines are meeting, must be organized very strictly. main reason is implementing periodical timetable, which causes all arrivals and departures to take place in 10 minutes (6 train routes in 10 minutes). due to pass through model many routes are colliding in the area of station head. to ensure the stability of new timetable arrivals of trains from šluknov, krásná lípa a panský must be performed without collision of routes. based on all mentioned conditions reconstruction of the railway station rumburk seems to be the best solution. reconstruction should include at least tracks configuration, platforms and interlocking [3, 4]. fig. 3 shows ideal variant of reconstruction. western station head allows simultaneous arrival from all three directions at the same time. longer platform edges are primary located by tracks, where trains to krásná lípa and šluknov are expected to stop. these trains have potential to be longer than trains on other branches. signal should be placed to the longer edge of platform 3, in order to coupling train sets. platform 1 is extra. this configuration of the railway station is crucial for implementation of new service conception. 3.5. infrastructure modifications for reducing the travel times and possible new stops from infrastructural point of view, this paper offers solution for benešov nad ploučnicí – jedlová – rumburk – šluknov – mikulášovice dolní nádraží section. upgrading this section is crucial for possible new circular line operation. all modifications are mainly undertaken in the sections between railway stations, railway stations are skipped as a kind of "black box" – cutting the travel times is considered, but modifications were not proposed in detail. main infrastructure modifications are changes in geometrical alignment and establishing speed profile for cant deficiency 130 mm. the longest section with new geometrical alignment has length of 9 km. steel sleepers with shape of "y" are used when there is a new geometrical alignment in a vertical curve, in order to avoid extending subgrade. limit values of the parameters of geometrical alignment are usually reached while increasing the maximal speed. maximal/minimal values are reached on exceptionally [4, 5]. also the reconstruction of signalling and control systems is designed in order to establish device with the third safety level. safety level is increased on some level crossing as well. section rumburk – šluknov is not considered in interlocking reconstructions, because current interlocking has already been ungraded to the third safety level. section šluknov – mikulášovice d.n. (– dolní poustevna) is also skipped, because all railway operation is currently organized according to rule sždc d3. table 1 shows reached travel times reduction on sections. travel times has been calculated in software "dynamika 1.7.1.", with railcar 843 as a reference vehicle. some proposed infrastructure modifications are not necessary, because travel times has already been reached in timetable 2016/17, but their introduction may increase the timetable stability. in order to improve railway transport availability some new stops are proposed – some are designed to replace inappropriate ones and some as completely new. for example: village horní habartice is located really close to the railway, so the new stop could be made there. new stop can replace current stop in veselá pod rabštejnem, which is located too far away from inhabited area. establishing new stop rumburkdolní křečany (fig. 4) on the railway line 083 could be also interesting, because this stop would be located in the center of inhabited area. stop rumburk-dolní křečany already exists on the 084 railway line, but second stop could attract more passengers. 4. conclusion during the problem solving process was managed to prove that the attractive connections between trains in the station rumburk can be reached without major infrastructure changes and without disconnecting any other important connections. this allowed formation of service conception not only for děčín and rumburk areas, but also for parts of česká lípa and liberec areas with overlap to germany. the result is the paper, which presents a possible way how to increase the effectiveness of a railway passenger transport in researched area. acknowledgements all the facts presented in the article are based on the results of work on project 12x2zs railway network of the czech republic and europe, which is undertaken on ctu faculty of transportation sciences, department of transport systems. 67 p. purkart, d. vodák, t. hoření, t. javořík acta polytechnica ctu proceedings figure 3. optimal variant of modifications of the railway station rumburk. section length travel time reduction [min] os r section benešov nad ploučnicí – jedlová benešov n. pl. – markvartice 5,4 -0,5 – markvartice – česká kamenice 7,9 -1 – česká kamenice – jedlová 15,4 -2 – section jedlová – rumburk jedlová – rybniště 9,3 -1,5 -1,5 rybniště – krásná lípa 4,8 -0,5 -0,5 krásná lípa – rumburk 6 -0,5 -0,5 section rumburk – mikulášovice dolní nádraží rumburk – šluknov 10 -2,75 -3 šluknov – mikulášovice d.n. 10,6 -1,75 – table 1. travel time reduction on individual sections. figure 4. proposed location of the new stop rumburk-dolní křečany. 68 vol. 11/2017 possible ways of improving railway operation and infrastructure references [1] sždc. aids of theoretical graph of train running. (for researched area between years 2014 – 2016). [2] commuting to work and school according to summation of inhabitants, houses and flats 2011 – ústecký region [online], 2013. [cit. 2015-02-20], https://www.czso.cz/csu/czso/dojizdka-do-zamestnania-skol-podle-scitani-lidu-domu-a-bytu-2011-usteckykraj-2011-b9vyzff32a. [3] čsn 73 4959. platforms and roofs of platforms of state, regional and industrial railways. únmz praha, 2009. [4] čsn 73 6360-1. geometrical characteristics of railway tracks – part 1: layout. únmz praha, 2008. [5] sždc s.o. drawing tables of superstructure. (for researched area). 69 acta polytechnica ctu proceedings 11:63–69, 2017 1 introduction and goals 1.1 researched area 1.2 reasons behind selecting the researched area 2 understanding and solving the issue 3 solution of the issue 3.1 summary of facts about commuting in the researched area 3.2 design of the new service conception 3.3 infrastructural changes necessary for the new service conception 3.4 reconstruction of the railway station rumburk 3.5 infrastructure modifications for reducing the travel times and possible new stops 4 conclusion acknowledgements references 3 acta polytechnica ctu proceedings 2(1): 3–20, 2015 3 doi: 10.14311/app.2015.02.0003 the golden age of cataclysmic variables and related objects (old and news) f. giovannelli1, l. sabau-graziati2 1inaf istituto di astrofisica e planetologia spaziali, area di ricerca di tor vergata, via fosso del cavaliere, 100 i00177 roma, italy 2intadpt. cargas utiles y ciencias del espacio, c/ra de ajalvir, km 4 e28850 torrejón de ardoz, madrid, spain corresponding author: franco.giovannelli@iaps.inaf.it abstract in this paper we review cataclysmic variables (cvs) discussing several hot points about the renewing interest of today astrophysics about these sources. we will briefly discuss also about classical and recurrent novae, as well as the intriguing problem of progenitors of the type ia supernovae. this paper is an extended and updated version of the review by giovannelli (2008). because of limited length of the paper and our knowledge, this review does not pretend to be complete. however, we would like to demonstrate that the improvement on knowledge of the physics of our universe is strictly related also with the multifrequency behaviour of cvs, which apparently in the recent past lost to have a leading position in modern astrophysics. keywords: cataclysmic variables dwarf novae intermediate polars polars novae optical spectroscopy photometry sub-mm ir radio uv x-rays multifrequency astrophysics x-ray binary systems high energy astrophysics. 1 introduction in the 1950s it was recognized that the various phenomena displayed by the cvs are all the consequence of accretion of matter onto a white dwarf (wd) from a low mass donor star (e.g., warner, 1976; 1995a). cvs are binary systems in which the primary component is a wd (mwd ∼ 1 m�) and the secondary is a late type main sequence star (ms ≤ 1 m�) (e.g., smak, 1985a). mass transfer is strongly depending, besides the orbital parameter of the system, on the magnetic field intensity at the surface of the primary. such process produces a large fan of behaviour that are detectable in different energy ranges: from radio to x-rays, and even in γ-rays. the orbital periods of cvs are ranging from ∼ 80 m to ∼ 12 h with a distribution showing a gap between 2 and 3 hours, in which few systems have been detected. in the past this gap was empty and this was the reason because was nicknamed ’period gap’. more than 600 cvs are known, most of them discovered through optical observations, and some, especially those in which the magnetic field of the wd is strong, discovered through x-ray observations, but with the detectors of the second and further generations, since cvs are in general not very bright in x-ray energy range. those with known or suspected orbital period are listed by ritter & kolb (1998). the first cv detected in the x-ray range, with rocket experiments, was the dwarf nova ss cyg (rappaport et al., 1974; heise et al., 1978). the uhuru satellite detected two cvs, which were not recognized as such. warner (1976) proposed the identification of 4u 1249-28 with ex hya, and the variable am her, which on further optical studies was recognized as a cv (forman et al., 1978). the magnetic field in these two systems is strong (≈ 107–108 g). a few dozen cvs were detected in x-rays with heao-1 satellite, with exosat, and with the einstein satellite (e.g., reviews of cordova & mason, 1983; cordova, 1995). later verbunt et al. (1997) recognized 91 cvs from a sample of 162 systems with known or suspected binary periods by using data of the rosat xrt-pspc all sky survey. historically, because cvs were observed photometrically and without seeming to follow any regular pattern, they were named with the term cataclysmic (from the greek word kataklysmos = flood, storm; hack & la dous, 1993). as collecting of observational data progressed it became apparent that these objects were regular binary systems which for some reason changed in brightness; some of them also regularly (recurrent novae and dwarf novae) while some others only once (classical novae). therefore the classification of cvs was based on the optical outburst properties, by which one may distinguish four groups of cvs: (i) classical novae; (ii) recurrent novae; (iii) dwarf novae; (iv) nova3 http://dx.doi.org/10.14311/app.2015.02.0003 f. giovannelli, l. sabau-graziati like objects (e.g., giovannelli & martinez-pais, 1991 and references therein; ritter, 1992; giovannelli, 2008). this classification, however, is neither self-consistent nor adequate and it is much better to consider primarily the observed accretion behaviour (smak 1985b). one obvious advantage of such an approach is connected with the time scales of various accretion phenomena, which are sufficiently short to avoid any major observational bias: the mass accretion rates in cvs usually range from 10−11 to 10−8 m� yr−1 (patterson, 1984); the time scales are from tens of seconds (oscillations in dwarf novae at outbursts) to years (super-outbursts of su uma stars or long term variations in vy scl stars). however, in the class of nova-like objects there are two sub-classes: the dq her stars and the am her stars. in these sub-classes of cvs the wds possess magnetic fields with intensity enough high for dominating the accretion disk and all the phenomena related to it. these classes of magnetic cvs, whose names are coming from the prototypes dq her and am her took later the names of intermediate polars and polars, respectively. a short history of their discovery has been discussed by warner (1995b). fundamental papers about these subclasses are those by patterson (1994), warner (1996). the class of ips has been split into two subclasses with relatively large and relatively weak magnetic field (norton et al., 1999). one example of a system belonging to the latter subclass is do dra (previously registered as yy dra) (andronov et al., 2008). there is another class of cvs, the rare am canum venaticorum (am cvn) star systems. they have extremely short orbital periods between ∼ 10 − 65 minutes. their spectra do not show evidence for hydrogen. they appear to be helium–rich versions of cvs (e.g. warner, 1995c; nelemans, 2005). there is an old suggestion, that in these systems the mass transfer is driven by gravitational wave radiation losses, proposed by paczyński (1967), after the discovery of the prototype with an orbital period of ∼ 17 minutes (smak, 1967). depending on the magnetic field intensity at the wd, the accretion of matter from the secondary star onto the primary can occur either via an accretion disc (in the so-called non-magnetic cvs: nmcvs) or a channelling through the magnetic poles (in the case of polars: pcvs) or in an intermediate way (in the case of intermediate polars: ipcvs). cvs in a time scale of order between weeks and years flare up almost periodically, about few magnitudes in optical wavelengths; the duration of the outbursts is much shorter than the recurrence time. typical light curves for classical novae and dwarf novae of the u gem, z cam, and su uma types can be seen in ritter (1992) and e.g. in giovannelli (2008). the recurrence time-scale of outbursts in dwarf novae is correlated with their amplitude and the outburst duration is depending on the orbital period (warner, 1987). in pcvs the wd magnetic field is strong enough to make the alfvén radius greater than the circularization radius, so no accretion disc is formed and the accretion structure is fully governed by the magnetic field, which canalize the accreting matter across the field lines. owing to the intense magnetic field (∼ 10–200 mg), the wd rotation is synchronized with the binary orbital period (a few hours). however, there are few systems (v1432 aql, by cam, v1500 cyg, v4633 sgr, and cd ind) in which pspin and porb differ by around 2% or less. these are assumed to be polars that have been disturbed from synchronism by a recent nova explosion (norton, sommerscales & wynn, 2004, and the references therein). ipcv wds have moderate magnetic fields (order of a few mg); the alfvén radius is smaller than the circularization radius but it is greater than the wd radius. therefore an accretion disc is formed in these systems but being disrupted at its inner region. in ipcvs matter follows again the magnetic field lines but just inside the alfvén radius. the rotating wd is asynchronous with the binary orbital period (pspin � porb). however, there are few systems that may be best described as nearly synchronous intermediate polars (v381 vel, rxj0524+42, hs0922+1333, and v697 sco) (norton, sommerscales & wynn, 2004, and the references therein). two of these systems lie in the ‘period gap‘. probably all four systems are ips in the process of attaining synchronism and evolving into polars. the last group defined by the accretion structure criterion, nmcvs, includes those systems whose wd magnetic fields are not relevant in governing the accretion structure. in these systems the accretion disc extends down to the wd surface and a boundary layer is formed. this family shows a great diversity of observational behaviour; for this reason the historical criterion of classification is, in this case, more appropriate for distinguishing their sub-classes. however, it is simply an attempt of classification for lack of a more general physical classification (e.g., giovannelli, 1991 and references therein). indeed, in general, we can consider the wd of a cv as a gravimagnetic rotator, characterized by a mass m — accreting matter at a rate ṁ from the optical companion (the secondary star) — rotating with a velocity ~ω and having a magnetic moment ~µ, not necessarily coaxial with the rotational axis (lipunov, 1987; 1991). then the accreting system is completely characterized by the following physical parameters: mass m, accretion rate ṁ, rotational velocity ~ω, and magnetic moment ~µ. in the plane spin period of the wd (and in general of the compact object) – gravimagnetic param4 the golden age of cataclysmic variables and related objects (old and news) eter y = ṁ/µ2 it is possible to find any sort of physical conditions of gravimagnetic rotators, as discussed by e.g. giovannelli (1991). figure 1 shows the positions of few cvs in the diagram spin period of the wd – gravimagnetic parameter (in unit -42): am her (terada et al., 2010 and references therein), ae aqr (patterson, 1979; de jager et al., 1994; wynn, king & horne, 1997), dq her (patterson, 1994; zhang et al., 1995), ei uma (reimer et al., 2008), ss cyg (giovannelli & sabau-graziati 2012a). it appears evident the power of this diagram obtained by lipunov (1987) using 1 m� white dwarf. the polars am her and ae aqr lie in the zone of propeller, how they must stay, while the ipcv dq her (the prototype of this class), ei uma (a very well known ipcv), and ss cyg (whose nature as ipcv is claimed by giovannelli’s group on the base of many circumstantial proofs and also because of a cogent similarity with ei uma, e.g. giovannelli & sabau-graziati 2012a,c) lie just in the zone predicted by lipunov for such objects. figure 1: the positions of several cvs in lipunov’s diagram calculated for 1 m� white dwarf (after lipunov, 1987). as recalled by giovannelli & sabau-graziati (1999), it is evident that the properties of an outburst in cvs depend crucially on the accretion rate, the mass of the wd, and the chemical composition of its hydrogen rich envelope in which the thermonuclear runaway occurs. and the accretion process onto the wd is strongly influenced by its magnetic field intensity. indeed, the three kind of cvs (non-magnetic, polars, and intermediate polars) obey to relationships between the orbital period of the system and the spin period of the wd (warner & wickramasinghe, 1991), where the magnetic field intensity plays a fundamental role. the orbital evolution of cvs, and hence the mass-transfer rate (ṁ) from the secondary to the white dwarf is driven by magnetic braking of the secondary for long-period systems (porb > 3 hr) and gravitational radiation for shortperiod systems (porb < 2 hr). however, such a gap — which was believed true for long time — is now partially filled by the sw sex systems (e.g. rodriguez-gil, 2003; rodriguez-gil et al., 2007). the apparent ’period gap’ was due to a smaller number of systems having orbital periods in such an interval, which were escaping from the observations. therefore the investigation on the magnetic field intensities in wds is crucial in understanding the evolution of cvs systems. the fundamental parameters to be searched are the magnetic moment, the mass accretion rate and the orbital parameters of the systems. in this way it will be possible to fulfill the plane log pspin– log porb, where a priori there are not restricted ranges of magnetic moment | ~µ |, or special correlations between pspin and porb and | ~µ |. the distribution of objects in that diagram is owed to the interaction of braking torques and accretion torques, with the superposition of the observed or implied variations of the accretion rate on long time scale (> 102 yr), acting on a continuum of magnetic moments. in this way each system is completely described by those physical parameters. davis et al. (2008) applied population synthesis techniques to calculate the present day number of two types of wd-main sequence star (wdms) binaries within the ’period gap’. the first are post-common envelope binaries with secondary stars that have masses 0.17 ≤ ms/m� ≤ 0.36 (gpcebs), such that they will commence mass transfer within the period gap. the second type are systems that were cvs at some point in their past, but detached once they evolved down in orbital period to ≈ 3 h as a consequence of disrupted magnetic braking, and are crossing the ’period gap’ via gravitational radiation (dcvs). they predicted an excess of dcvs over gpcebs within the ’period gap’ of ∼ 4 to∼ 13. this excess is revealed as a prominent peak at the location of the ’period gap’ in the orbital period distribution of the combined gpceb and dcv population. they suggest that if such a feature is observed in the orbital period distribution of an observed sample of short orbital period wdms binaries, this would strongly corroborate the disruption of magnetic braking. willems et al. (2005) and willems et al. (2007) by using population synthesis tools studied the population of nmcvs with orbital periods 1) < 2.75 h, and 2) > 2.75 h, respectively. 1) a grid of detailed binary evolutionary sequences was calculated and included in the simulations to take account of additional angular momentum losses beyond that associated with gravitational radiation and mass loss, due to nova outbursts, from the system. as a specific example, willems et al. (2005) considered the 5 f. giovannelli, l. sabau-graziati effect of a circumbinary disc to gain insight into the ingredients necessary to reproduce the observed orbital period distribution. the resulting distributions showed that the period minimum lies at about 80 minutes, with the number of systems monotonically increasing with increasing orbital period to a maximum near 90 minutes. there is no evidence for an accumulation of systems at the period minimum, which is a common feature of simulations in which only gravitational radiation losses are considered. the shift of the peak to about 90 minutes is a direct result of the inclusion of systems formed within the period gap. 2) the population of nmcvs with unevolved main– sequence–like donors at orbital periods greater than 2.75 h was investigated. in addition to the angular momentum losses associated with gravitational radiation, magnetic braking, and mass loss from the system, willems et al. (2007) also included the effects of circumbinary discs on the evolution. for a fractional mass input rate into the disc, corresponding to 3×10−4 of the mass transfer rate, the model systems exhibit a bounce at orbital periods greater than 2.75 hr. the simulations revealed that: i) some systems can exist as dwarf novae throughout their lifetime, ii) dwarf novae can evolve into novalike systems, and iii) novalike systems can evolve back into dwarf novae during their postbounce evolution to longer orbital periods. among these subclasses, novalike cataclysmic variables would be the best candidates to search for circumbinary discs at wavelengths ≥ 10 µm. the theoretical orbital period distribution is in reasonable accord with the combined population of dwarf novae and novalike systems above the period gap, suggesting the possibility that systems with unevolved donors need not detach and evolve below the period gap as in the disrupted magnetic braking model. experimental data are necessary for checking the validity of theoretical predictions. the field strength distribution of mcvs differs from that of single wds, although both cluster around 30 mg. the distribution of isolated wds extend on a wide range of magnetic field strength (∼ 105–109 g), whilst in accreting wds of cvs, as far as is presently known, there is a lack of systems at both high and low field strengths. however, the apparent absence of low field mcvs might be explained by the ips, which generally have unknown field strengths, and the lack of high field systems is still not understood (e.g., beuermann, 1998). wynn (2000) discussed the problem of accretion flows in mcvs. on the base of the ratio pspin/porb he divided the mcvs in three classes: class 1, class 2 and class 3 if such a ratio is � 0.1, ∼ 0.1, and � 0.1, respectively. for the systems in class 1 the disc equilibrium condition is clearly satisfied. those in class 2 are very unlikely to possess accretion discs. the systems in class 3 are ex hya-like systems which lie below the ’period gap’ and cannot possibly contain accretion discs. these are ex hya, ht cam, rxj1039.7-0507, and v1025 cen. these all have pspin/porb > 0.1 and porb < 2 hr. dd cir and v795 her lie within the ’period gap’ with pspin/porb ∼ 0.1 and may be included in the class 2 (norton, somerscales & wynn, 2004, and the references therein). wynn (2000) crudely classified the mcvs according to the magnetic moment and orbital period. ex hya systems have magnetic moment similar to ips above the ’period gap’ and comparable to the weakest field am her-like systems. this indicates that mcvs above the ’period gap’ will evolve to long spin periods below it. norton, wynn & somerscales (2004) investigate the rotational equilibria of mcvs. they predict that ipcvs with µ ≥ 5× 1033 g cm3 and porb > 3 hr will evolve into pcvs, whilst those with µ ≤ 5 × 1033 g cm3 and porb > 3 hr will either evolve into low field strength polars that are presumably unobservable, and possibly euv emitters, or into pcvs when their fields, buried by high accretion rate, revive when the mass accretion rate reduces. warner (1996) deeply discussed torques and instabilities in ips on the base of measured spin periods of the primaries and found several important relationships between fundamental parameters of these systems, such as log ṁ vs log porb, log µ33 vs log ṁ17, log lx vs log ṁ, as shown in fig. 2 in the left, central, and right panels, respectively. there is a range of magnetic moments µ and mass transfer rates in which synchronized rotation of the primary can occur even though it possesses an accretion disc. ak et al. (2010), using available astrometric and radial velocity data, computed the space velocities of cvs with respect to the sun and investigated kinematical properties of various sub-groups of cvs. the orbital period distribution of cvs in the refined sample of 159 systems resembles that of the whole sample of cvs (e.g. connon smith, 2007). ak et al. (2010) found that the mean kinematical age (mka) of the 159 systems is mka159 = 5 ± 1 gyr. in the sample, 134 of 159 systems are non magnetic (nmcv) having mkanmcv = 4.0± 1.0 gyr. in the sub–sample of nmcvs, 53 of 134 have porb < 2.62 h and their mka is 5.0±1.5 gyr, whilst 81 of 134 systems have porb > 2.62 h and their mka is 3.6±1.3 gyr. this means that cvs below the ’period gap’ are older than systems above the gap. this result in agreement with the standard evolution theory of cvs. the selection of 2.62 h as the border between the two groups of systems lies roughly in the middle of the ’period gap’, where systems have been detected. this means that the ’period gap’ does not exist anymore and the systems inside this ’gap’ are just frontier objects between systems experiencing gravitational radiation and those experiencing magnetic braking. the reason because they are not so numerous as 6 the golden age of cataclysmic variables and related objects (old and news) figure 2: left panel: intermediate polars in the plane ṁ-porb. the two lines are lines of disc stability: stable above and dwarf nova outburst below. they were computed for f=0.2 and 0.3, with rout = f × a, being a the separation of the two stars in the system (by courtesy of warner, 1996). central panel: magnetic moment in units of 1033 g cm3 versus mass accretion rate in units of 1017 g s−1. boundaries for white dwarf mass m1 = 1 m� and m1 = 0.6 m� have been computed for porb = 4 h (by courtesy of warner, 1996). right panel: mass transfer rate onto white dwarf versus (2-10 kev) x-ray luminosity (by courtesy of warner, 1996). those placed at sides could be the relative shorter time of permanence in the ’gap’, and then difficult to be detected. our opinion is that a more appropriate investigation of the class of the so-called ipcvs is necessary. indeed, such systems could show surprises if deeply studied, as for instance occurred for ss cyg. this system, usually considered a nmcv because of a classification once made by bath & van paradijs (1983), whilst since 1984 it has been claimed as an ipcv by giovannelli et al. (1985) and later confirmed several times (e.g., giovannelli & martinez-pais, 1991; giovannelli, 1996; giovannelli & sabau-graziati, 1999, gaudenzi et al., 2002). giovannelli & sabau-graziati (2012a) discussed all the circumstantial proofs in favor of the magnetic nature of ss cyg, as well as those adverse, concluding with reasonable certainty that its nature is magnetic, being the magnetic field intensity b = 1.7 ± 0.8 mg, in agreement with the value (b ≤ 1.9 mg) derived by fabbiano et al. (1981) by using x-ray, uv and optical coordinated measurements. this would teach a lesson: it is mandatory to observe cvs for long time in order to follow at least a whole period of the binary system between two successive outbursts. this is, of course, possible only for systems like dwarf novae where the almost periodical outbursts occur in time scales of weeks-months. networks of robotic telescopes can help in this matter (giovannelli & sabau-graziati, 2012b) however, we can say that cvs form a broad stellar family of highly variable and dynamical members. when it comes to explaining particulars about, e.g., the detailed interaction between the transferred matter and the wd’s atmosphere; irregularities within regular photometric behaviour; turbulent transport in the disc; or the final fate of these objects, more is missing than what is known, rendering their study ever more challenging. at least, cvs are natural multi–wavelength laboratories offering us the possibility of studying in detail the behaviour of plasma and radiation under extreme physical conditions. the understanding of stellar evolution, electromagnetism and polarization, mass and radiation transfer or 3-d geometrical effects, in a broad spectral range from hard x-rays to radio, is mandatory for improving the knowledge of the nature of cvs. variability, from milliseconds to hundreds of years, follows from different physical processes taking place in these systems and can be studied by means of several astronomical techniques. as our skills in developing further these techniques grow our understanding of the cvs insights also grows; and the more we learn about cvs the further techniques and theory develop. on the other hand, it is well known that conclusions obtained in the field of cvs have been extrapolated, upwards or downwards in scale, to other fields such as agns or lmxrbs, and vice versa. from such exchanges of information and results astrophysical research in general always benefits. rapid oscillations in cvs are particularly interesting. as reviewed by warner (2004), the rich phenomenology of dwarf nova oscillations (dnos) and quasi–periodic oscillations (qpos) observed in cvs favour the interpretation that these rapid brightness modulations (3 to 11,000 s timescales) are magnetic in nature — magnetically channelled accretion from the inner accretion disc for dnos and possible magnetically excited traveling waves in the disc for qpos. there is increasing evidence for the magnetic aspects, which extend to lower fields the well–known properties of strong field (pcvs) and intermediate strength field (ipcvs) cvs. the result is that almost all cvs show the presence of magnetic fields on their wd primaries, although for many the intrinsic field may be locally enhanced by the accretion process itself. there are many behaviour that parallel the qpos seen in x-ray binaries, with 7 f. giovannelli, l. sabau-graziati high– and low–frequency x–ray qpos resembling, respectively, the dnos and qpos in cvs. other papers about rapid oscillations in cvs are those by warner & woudt (2005) and pretorius, warner & woudt (2006). the current estimate of the space density of cvs is of ∼ 3 × 10−6 pc−3 (warner, 2001). this may be a significant underestimate of cvs space density, as discussed by patterson (1984). although densities from the most comprehensive optical palomar–green survey raises the estimate at (3−6)×10−6 pc−3, x-ray all-sky surveys give densities of ∼ 1 × 10−5 pc−3 for detected systems of low ṁ in hard x-rays (patterson, 1998). then from observational point of view, it is necessary an intensive search for the faint cvs predicted by population synthesis with orbital periods at ∼ 80 − 100 min that have passed through the orbital period minimum at ∼ 78 min and have increasing orbital periods. this research must be done among the low ṁ systems detected by x-ray surveys. thanks to its high sensitivity, integral is very useful for this purpose. up to now, it discovered several new faint cvs, with porb > 3 hr, and only one with porb < 3 hr (e.g. šimon et al., 2006; hudec et al., 2008). high speed photometry of faint cvs have shown that: i) 1 of 10, tv crv has porb = 1.509 hr (woudt & warner, 2003); ii) 5 of 13 have porb < 2 hr (woudt, warner & pretorius, 2004); iii) 1 (cal 86) of 12 has porb = 1.587 hr (woudt, warner & spark, 2005); iv) 3 of 11 have porb > 3 hr (witham et al., 2007). for reviews about cvs see the fundamental papers by robinson (1976), patterson (1984, 1994), hack & la dous (1993), and the books of warner (1995a) and hellier (2001). more recent reviews are those by connon smith (2007), and giovannelli (2008). the long review the impact of space experiments on our knowledge of the physics of the universe by giovannelli & sabaugraziati (2004) contains also a part devoted to cvs. 2 multifrequency emissions in cvs there are several components that are responsible for the total emission. deep discussions about these components can be found in the literature, but there is a recent review by giovannelli (2008, and the references therein) that exhaustively summarize their contributions to the total multifrequency emission of cvs. briefly, such components are: a) the secondary stars are cool main sequence stars with spectral type ranging from g8 to m6, corresponding to temperatures from 5,000 to 3,000 k. their contribution is mainly in red and ir regions of the electromagnetic spectrum. b) the primary stars. the temperatures of wds are known only in few cases: when they belong to high inclination systems, or when they accrete matter with a very low mass transfer rate. however, the wd temperatures range between 10,000 and 50,000 k (sion, 1986; 1991). urban & sion (2006) found that the wds in cvs above the period gap are hotter and more accretion heated (teff = 25, 793 k) than those below the gap (teff = 18, 368 k). therefore wds are expected to radiate essentially in the uv, but they can be visible also in the optical range if they are not too hot. c) the accretion disc: it does not have a homogeneous temperature, but spans a large range. since the temperature distribution in discs is poorly known, in order to obtain a rough evaluation of their contribution to the total emission it is necessary to evaluate the contributions at different frequencies of a synthetic disc constituted of black bodies at different temperatures, the temperature distribution being that of a stationary accretion disc (e.g., la dous, 1994). it then appears evident that the contribution of such an accretion disc is important in the whole range between euv and ir, depending on the choice of the disc parameters. furthermore, the uv radiation can be supplied from a zone in the vicinity of the wd (some ten stellar radii), which could contain any optically thick material left there. however, the argument of accretion discs deserves an important comment. it appeared evident that the viscosity of matter inside the accretion discs plays a fundamental role in the description of physical processes occurring there. in spite of numerous attempts in determining such a viscosity, the physical nature of that still remains largely indeterminate. the best training for study the viscosity is the subclass of dwarf novae, showing quasi-periodic outbursts which occur on a time scale from weeks to months (or even years) and are due to non-stationary accretion. meyer & meyer-hofmeister (1981, 1982, 1983) firstly discussed the physical mechanism responsible for dwarf nova outbursts which is connected with the thermal instability of the disc which occurs in the temperature range corresponding to the ionization of hydrogen. soon after smak (1984a,b) extended the study of such a mechanism. the details are summarized by smak (2002). it is important to point out that the shapes of dwarf nova light curves, which depend on a number of relevant parameters, depend also on viscosity. in particular, the characteristic time-scales observed during outbursts depend on the viscous time-scale. this provides an important and almost unique opportunity of obtaining some constraints on viscosity or – within the α disc approach (shakura & sunyaev, 1973) – of an empirical determination of α. for a more complete and detailed discussion of dwarf novae and models of their outbursts – see reviews by cannizzo (1993), osaki (1996), and lasota (2001). 8 the golden age of cataclysmic variables and related objects (old and news) d) the boundary layer: a very important zone for the emission is that of the transition between the accretion disc and the wd surface, namely the boundary layer. it is possible that all, or at least a significant fraction, of the kinetic energy of the material contained in the accretion disc must be radiated away within the geometrically very small boundary layer in order to have the possibility of the material accreting onto the wd’s surface. then, whatever the situation, one can assume the presence of a strong x-ray source at the boundary layer, which will be visible also in the euv and shortwavelength uv according to the choice of disposable theoretical parameters. most of the radiation then comes from the accretion disc and boundary layer, which contribute roughly 50% each. from the accretion disc the radiation is essentially emitted in the optical and uv, whilst from the boundary layer — optically thick (which occurs at high accretion rates) — the radiation is emitted in the soft x-ray range; when the accretion is at low rates the boundary layer is optically thin and appears as a hard thermal bremsstrahlung source. these predictions have been tested experimentally, comparing the observations of cvs in optical, uv and soft x-ray ranges (e.g. wood et al., 1989; horne et al., 1994). e) the gas stream: it is definitively optically thin and cool and contains rather little material; so, probably, its contribution to the total emission of cvs is negligible at all frequencies as source of continuum, whilst it could contribute to the formation of lines in the red and ir regions. f) the hot line: the energy excess zone in the place where the stream comes to the disc is a shock wave. this zone was previously known as ‘the hot spot‘. its structure and radiation characteristics are still an open problem; it is visible in many systems in optical photometry (less in the ir and never in the uv) as a periodically recurring hump in the orbital light curve. its temperature must be ≤ 10, 000 k. g) hot corona or chromosphere: is a shell of optically thin and rather hot gas, below and above the accretion disc. x-ray and uv line radiation are tentatively attributed to it, whilst it probably does not contribute to the uv, optical or ir continuum emission. usually no radio emission from cvs has been measured. only upper limits for individual systems of order of a few mjy are available (e.g ≤ 10 mjy in ss cyg — cordova, mason & hjellming 1983). however, recently, körding et al. (2008) detected a radio flare from ss cyg peaked at 1.1 mjy with a duration of order 20 days, above the upper limit of 0.08 mjy. this radio flare was simultaneous with the optical long outburst peaked at about 1 jy. pringle & wade (1985) computed the contribution functions of the most important components of a cataclysmic system, previously discussed. the plot can be found also in fig. 6 of giovannelli’s paper (2008). during quiescence dwarf novae emit essentially hard x-rays (∼ 0.1–4.5 kev) and the flux distribution is rather well approximated by a thermal bremsstrahlung with ktbrems ≈ 10 kev (cordova & mason, 1983). a direct correlation between the hard x-ray/optical fluxes ratio and hβ equivalent width has been found by patterson & raymond (1985). during outburst dwarf novae emit soft x-rays (0.18– 0.5 kev) with an increase of the flux of the order of 100 or more, although most of the radiation is hidden in the euv range (cordova & mason, 1984). the soft x-ray spectra can be fitted either with black bodies at ktbb ≈ 25–30 ev or, alternatively, with bremsstrahlung spectra at ktbrems ≈ 30–40 ev. the most important features are the anti-correlation between the hard and soft x-ray emissions during the outburst cycle and the correlation between soft x-ray and optical emissions, as measured for ss cyg (watson, king & heise, 1985), or — what is the same — anti– correlation between the hard x-ray and optical emission (ricketts, king & raine, 1979). during an outburst of ss cyg there is also the correlation of optical and euv emissions, that are anti–correlated with the hard x-ray emission detected by rxte (wheatley et al., 2003). what does that mean? the uv flux and the bulk of optical flux in dwarf novae and nova-like stars originate in the accretion disc. the ir flux observed during quiescence and possibly some of the optical flux come from the secondary late-type star. the rise to an outburst either occurs simultaneously at all wavelengths when it is slow, or progressively starts later with decreasing wavelengths when it is fast, since ever more central hotter parts of the disc become involved. indeed, several dwarf novae have been observed in the uv and optical during the rise to maximum outburst brightness and their behaviour are quite similar: the uv rise lags the optical rise by up to a day (e.g., vw hyi: hassall et al. (1983); cn ori and rx and: cordova, ladd & mason (1986); wx hyi: hassall, pringle & verbunt (1985). with respect to the optical band, this lag is similar also in the euv region covered by the voyager (50–1200 å) for ss cyg (polidan & holberg, 1984) and vw hyi (polidan & holberg, 1987). this fact strongly supports the origin of the outburst being in the cooler outer part of the disc rather than in the hotter parts near the wd; therefore mininova models for the outbursts are probably excluded (cordova & howarth, 1987). the two models for triggering the outbursts, compatible with the lag observations, are then: 9 f. giovannelli, l. sabau-graziati • an instability in the secondary star which allows the transfer of more mass to the disc; • a thermal instability in the outer disc, which results in material stored there being suddenly transported through the disc. during the decline, the whole disc cools simultaneously. the contribution to the total emission from the boundary layer between the disc and the wd surface is in uv and x-ray ranges: the boundary layer is optically thin during quiescence and then emits hard x-rays, but it is optically thick during outburst and then emits soft x-rays since the radiation is thermalized before escape (la dous, 1993). from the euve (extreme ultraviolet explorer) craig et al. (1997) have shown the euv spectra of three npcvs in outburst, namely vw hyi, u gem and ss cyg. vw hyi shows the softest euv spectrum peaked at ∼ 250 å. however, its boundary layer/disc luminosity ratio — lbl/ldisc ∼ 0.2 (mauche et al., 1991) — is in contrast with the boundary layer models. in u gem the total size of the euv emitting region is comparable to that of the wd itself, which indicates that the outburst in mainly confined to the inner disc/boundary layer region (long et al., 1996). its lbl/ldisc ∼ 1. ss cyg is the hardest of the three euv nmcvs. its euv spectrum is rather complex and changed by a factor 100 during the outburst with an almost constant spectral energy distribution. quasi-coherent oscillations (∼ 7−9 s) have been detected in the euv emission (mauche, 1996). ss cyg shows no euv emission longward ∼ 130 å. mauche, raymond & mattei (1995) found that for ss cyg the relation lbl/ldisc ∼ 1, valid for the boundary layer models is strongly violated, being this ratio lbl/ldisc ∼ 0.07. and this is one more proof that ss cyg is not a nmcv — as already remarked — as claimed by giovannelli’s group. iue satellite deserves special comments since it was fundamental in improving the knowledge of cvs. a detailed review can be found in giovannelli (2008). briefly, the iue gave significant contributions on: i) knowledge of disc accreting and magnetic cvs, as extensively discussed by cordova (1995), and references therein. ii) nature of the high velocity winds. during outburst of ss cyg the spectral emission features disappear or go into absorption, some of them showing p cygni profile (e.g. civ), which clearly indicate the presence of high velocity wind from the system. the emission features appear again when the system is going into quiescence (giovannelli et al., 1990). iii) boundary layer emission. multifrequency observations show that x-ray luminosity at all outburst phases is much lower (about at least a factor 10) than the uv/optical luminosity from the disc, as expected from the models (e.g., mauche, 1998). this simply means that the boundary layer models are not correct. iv) underlying wd and its photosphere. iue provided the first evidence that the wd is heated by the dwarf nova outburst and subsequently cooled. a list of nine such systems has been reported by szkody (1998). these measurements are very difficult because of the long quiescence–outburst–quiescence cycles (from weeks to years). the short outburst period dwarf nova vw hyi cooled to 18,000 k (from 20,500 k) in the 14 days before the next outburst began (verbunt et al., 1987). v) magnetic field of the wd. indirect evaluations of magnetic field intensities in cv wds have been obtained through multifrequency observations (e.g., fabbiano et al., 1981). our feeling is that the problem of magnetic fields in wds has been underestimated in the studies of cvs. too many simplified models of disc accreting and magnetic cvs have been developed under the hypothesis that cvs can be sharply divided into three classes: polar, ip, non-magnetic. magnetic fields are smoothly varying in their intensities from one class to another. the discovery in some ips of a circularly polarized optical emission suggests that these intermediate polars will evolve into polar systems (e.g., mouchet, bonnetbidaud & de martino et al., 1998). some evidence of the continuity between the ipcvs and pcvs is coming from the detection of the sw sex systems. they have orbital periods just inside the so-called ’period gap’, which separates the two classes of ipcvs and pcvs (e.g. rodriguez-gil, 2003 and references therein; rodriguez-gil et al., 2007). looking at the homogeneous set of data coming from the iue for pcvs and ipcvs, it has been possible to obtain important information on common properties and peculiarities of these binaries (de martino, 1999 and references therein), which render the two classes rather similar in some of their uv behaviour. mouchet, bonnet-bidaud & de martino (1998), and de martino (1998) made the hypothesis that the two classes are evolutionary related. the far uv vs near uv colour–colour diagram for mcvs was constructed by de martino (1999). such a diagram was constructed measuring broad band continua in the iue short wavelength range (1420–1520 å and 1730–1830 å) and in the long wavelength range (2500–2600 å and 2850–2900 å). clearly the uv continua cannot be simply described by a single component but possess different contributions, as discussed by de martino (1999) and already noted in the past, since 1984, by giovannelli et al. (1985). araujo-betancor et al. (2005) obtained hubble space telescope (hst) stis data for a total of 11 pcvs 10 the golden age of cataclysmic variables and related objects (old and news) as part of a program aimed at compiling a homogeneous database of high–quality fuv spectra for a large number of cvs. comparing the wd temperatures of pcvs with those of nmcvs, they find that at any given orbital period the wds in pcvs are colder than those in nmcvs. the temperatures of wds in pcvs below the period gap are consistent with gravitational radiation as the only active angular momentum loss mechanism. the differences in wd effective temperatures between pcvs and nmcvs are significantly larger above the period gap, suggesting that magnetic braking in pcvs might be reduced by the strong field of the primary. araujo-betancor et al. (2005) derive a lower limit on the space density of pcvs of 1.3× 10−6 pc−3. 3 renewed interest for cataclysmic variables before the advent of rosat x-ray satellite, mcvs were relegated to a subsection of conferences about cvs that were mainly concentrated on nmcvs. the rosat satellite discovered many mcvs that even menaced to overthrow our understanding of the secular evolution of ‘normal‘ cvs by appearing – apparently inexplicable – in the so–called ‘period gap‘ in the orbital–distribution of cvs (e.g. vrielmann & cropper, 2004). but in spite of this, cvs were not considered, in general, for many years as principal targets of high energy x-ray experiments. at the beginning of the nineties of the last century, acceleration of particles by the rotating magnetic field of the wd in intermediate polars in the propeller regime — ae aqr -– detected by ground-based cherenkov telescopes in the tev passband (e.g. meintjes et al. 1992), and tev emission from the polar am her detected by ground-based cherenkov telescopes (bhat et al. 1991) — measurements never confirmed — were the main reasons of renewed interest for cvs in the high energy astrophysicists community. the integral observatory, until the beginning of 2007, had observed over 70 percent of the sky, with a total exposure time of 40 million seconds. bird et al. (2007) published the third integral catalogue of gamma-ray sources. it contains a total of 421 gammaray objects. most have been identified as either binary stars in our galaxy containing exotic objects such as black holes and neutron stars, or active galaxies, far away in space. but a puzzling quarter of sources remain unidentified so far. they could be either star systems enshrouded in dust and gas, or cvs. integral observes in the gamma-ray band so it can see through the intervening material. it has demonstrated that it can discover sources obscured at other wavelengths. one surprise has been the efficiency with which integral has detected just one minor subclass cvs, the socalled ipcvs. initially astronomers were not sure that cvs would emit gamma rays. indeed, integral has already shown that only about one percent of them do. this fact overbearingly renewed the interest for cvs, apparently fallen into disgrace in favour of binary systems containing either neutron stars or black holes. the fourth ibis/isgri catalog reports 331 additional sources when compared to the third catalog. of these, 120 are associated with extragalactic sources, while only 25 are associated with known galactic sources, and the remainder are so far unidentied (bird et al. 2010). cvs constitute ∼ 5% of the total sources. moreover, since the cvs measured by the integral observatory are magnetic in nature, the interest for such class of objects has been addressed to evolutionary problems. the long–standing fundamental predictions of evolution theory are finally being tested observationally. all facets of the accretion process in cvs, including variability, disc winds and jets, are universal with accreting wds, neutron stars, and black holes (knigge, 2010, 2011). knigge, baraffe & patterson (2011) extensively discussed the reconstruction of the complete evolutionary path followed by cvs, based on the observed mass–radius relationship of their donor stars, following knigge (2006) that discussed the observational and theoretical constraints on the global properties of secondary stars in cvs using the semi–empirical cv donor sequence, and concluded that most cvs follow a unique evolutionary track. in the standard model of cv evolution, angular– momentum–loss (aml) below the period gap are assumed to be driven solely by gravitational radiation (gr), while amls above the gap are usually described by a magnetic bracking (mb) (rappaport, verbunt & joss (1983). knigge, baraffe & patterson (2011) with their revised model, found the optimal scale factors fgr = 2.47 below the gap and fmb = 0.66 above, whilst the standard model gives fgr = fmb = 1. this revised model describes the mass–radius data much better than the standard model. the sub-class of cvs, named classical novae (cne), which are the third more powerful stellar explosions in a galaxy, have been observed as close as a kpc and as far as galaxies in fornax cluster. the time to report on the recent renaissance in studies on cne thanks to observations with 8-10m class telescopes, high resolution spectroscopy, in synergy with observations from space carried out with swift, xmm, chandra, hst, and spitzer, coupled with recent advances in the theory of the outburst, seems now in order. moreover, the possible connection among some cv-types and sne-ia will definitively justify the renewed interest about cvs. 11 f. giovannelli, l. sabau-graziati 4 classical and recurrent novae classical novae are expected to recur on timescales from 100,000 years to just a few decades. the most important physical parameters controlling this recurrence timescale are the wd mass, and the mass accretion rate from the secondary (e.g. yaron et al. 2005). once classical nova (cn) is recorded more than once, it can be designated as “recurrent” (rn). since the wd and the binary system remain intact after an outburst, it is possible that classical novae may actually be the same as recurrent novae if observed over a long enough time period. while the interval between outbursts of recurrent novae range from 10 to 100 years, it has been estimated that the time interval for classical novae would range from about 30,000 years for a 1.3 m� wd to 100,000 years for a 0.6 m� wd. given long enough it is expected that all classical novae will be observed as recurrent novae. the long term behaviour of classical old novae, and the optical behaviour of cne in outburst were discussed by bianchini (1990), and seitter (1990), respectively. the books by cassatella & viotti (1990) and by bode & evans (2008) are very useful for studying the physics of classical novae. recurrent novae are a rare sub-class of cataclysmic variable stars; wds accreting material from a binary companion in which more than one classical nova-type outburst has been observed (see the book of hellier, 2001 for a comprehensive review of cvs). nova outbursts are suspected to be due to a thermonuclear runaway on the surface of the wd, which releases huge amounts of thermal energy once a critical pressure is reached at the base of the shell of accreted material. one of the most interesting rne is rs ophiuchi (rs oph). it is an amazingly prolific recurrent nova, with recorded outbursts in 1898, 1907, 1933, 1945, 1958, 1967, 1985 and 2006 (schaefer 2010). the short time between outbursts (∼ 20 yrs) suggests that rs oph hosts a massive wd accreting material at a significantly high rate. in the latter paper schaefer discussed not only rs oph, but also the photometric histories of all known galactic rne. classical and recurrent nova outbursts have been recently discussed by bode (2011a,b) and evans (2011). the proceedings of a conference about rs oph and recurrent phenomenon can be very useful for details (evans et al., 2008). general properties of quiescent novae have been discussed by warner (2002). the very useful book of bode & evans (2008) about classical novae examines thermonuclear processes, the evolution of nova systems, nova atmospheres and winds, the evolution of dust and molecules in novae, nova remnants, and observations of novae in other galaxies. it includes observations across the electromagnetic spectrum, from radio to gamma rays, and discusses some of the most important outstanding problems in classical nova research. of the ∼ 400 known galactic classical novae, only 10 of them are recurrent. eight of them harbour evolved secondary stars, contrary to classical novae that contain main sequence stars (darnley et al., 2011). they propose a new nova classification based on the evolutionary state of the secondary star, contrary the current schemes based on the properties of outbursts. such classification contains three groups of novae: i) main sequence nova (ms–nova); ii) sub–giant nova (sg– nova); and iii) red giant branch nova (rg–nova). rne play an important role in the studies of sn ia progenitors (surina et al., 2011). rne are likely progenitors of type–ia supernovae. in order to brave this important problem the use of archival data is the only way to answer the big question. now, huge and comprehensive set of archival rn data go back to 1890. 5 progenitors of sn ia it is well accepted by the community that type–ia sne are the result of the explosion of a carbon–oxygen wd that grows to near chandrasekhar’s limit in a close binary system (hoyle & fowler, 1960). but the debate is focussed around the different kinds of progenitors. indeed, in the past, two families of progenitor models have been proposed. they differ in the mode of wd mass increase. the first family is the so–called single degenerate (sd) model (whelan & iben, 1973), in which the wd accretes and burns hydrogen–rich material from the companion. the second family is the so–called double degenerate (dd) model, in which the merging of two wds in a close binary triggers the explosion (webbing, 1984; iben & tutukov, 1984). the two scenarios produce different delay times for the birth of the binary system to explosion. thus it is hopefully possible to discover the progenitors of type–ia sne by studying their delay time distribution (ddt). the ddt can be determined empirically from the lag between the cosmic star formation rate and type–ia sn birthrate. the energy released through runaway thermonuclear process ejects the majority of the unburnt hydrogen from the surface of the star in a shell of material moving at speeds of up to 1.5 ×103 km s−1. this produces a bright but short-lived burst of light the nova. although type–ia supernova appear to have similar origin to classical novae, there are key differences. the most important is that in a classical nova, the thermonuclear runaway occurs only on the surface of the star, allowing the wd and the binary system to remain intact (e.g. townsley & bildsten, 2005). in a type–ia 12 the golden age of cataclysmic variables and related objects (old and news) supernova, the thermonuclear runaway occurs within wd itself, completely disrupting the progenitor. this is reflected in the amount of energy released in the explosions, with classical novae releasing ∼ 1044 erg, and type–ia supernovae ∼ 1051 erg. the possible progenitors of sn ia are: i) recurrent novae; ii) symbiotic stars; iii) super-soft sources; iv) double wd binaries; and v) wds accreting material from red–giant companions. i) recurrent novae are just a subset of ordinary novae that happen to go off more than once per century. as such, they are binary systems with matter flowing off a companion star onto a wd, accumulating on its surface until the pressure gets high enough to trigger a thermonuclear runaway that is the nova. only 10 rne are known in our milky way galaxy, including: u sco (1863, 1907, 1917, 1936, 1945, 1969, 1979, 1987, 1999); t pyx (1890, 1902, 1920, 1944, 1967); t crb (1866, 1946); rs oph (1898, 1907, 1933, 1945, 1958, 1967, 1985, 2006). to recur with τrec < 100 years, rne must have: high wd mass (1.2m� < mwd < mchandra), and high accretion rate (ṁ ∼ 10−7 m� yr−1). sn ia occurs if: i) the mass ejected for each eruption is less than the mass accreted onto the wd (mejected < ṁ τrec); ii) the rate of death rne must be enough to produce the sn ia rate (rrndeath = rsnia), being rrndeath = nrn ×(0.2m�ṁ). in order to solve the problems we need to know τrec (recurrence time scale) from archive plates, nrn (number of rne in the milky way) from archive plates and aavso, ṁ (mass accretion rate onto wd) from the average in the last century, mejected (mass ejected in eruption) from pre–eruption eclipse timing. some results have been obtained for becoming optimists in solving the problem of sn ia production. indeed schaefer (2011) obtained for ci aql and u sco mejected << ṁ τrec). thus, wds are gaining mass and the latter rne will collapse as sn ia. moreover, for the milky way, m31, and lmc rrndeath ∼ nrn. then there are enough rne to supply the type–ia sn events. ii) symbiotic stars contain wds efficiently accreting material from the secondary star. in most cases they steadily burn h–rich material allowing them to grow in mass. some of these systems can produce high mass wds. in symbiotic rne (syrne) the wd mass is already very close to chandrasekhar’s limit. for instance in v 407 cyg a very massive wd is accreting material at a rate of ∼ 10−7 m� yr−1 from a mira– type companion (miko lajewska, 2011). iii) super–soft sources are probably wds that accrete material and burn hydrogen. voss & nielemans (2008) discovered an object at the position of the type– ia sn2007on in the elliptical galaxy ngc1404 on pre– supernova archival x–ray images. this result favours the accretion model (sd) for this supernova, although the host galaxy is older than the age at which the explosions are predicted in sd models. however, the dd model cannot be ruled out by this event because a hot accretion disc is probably the intermediate configuration of the system, between first wd–wd roche–lobe contact and explosion (yoon, podsiadlowski & rosswog, 2007). greggio, renzini & daddi (2008) starting from the fact that type–ia sn events occur over an extended period of time, following a distribution of delay times (ddt), discussed theoretical ddt functions that accommodate both ‘prompt‘ and ‘tardy‘ sn events derived by empirically–based ddt functions. moreover such theoretical ddt functions can account for all available observational constraints. the result is that sd/dd mix of snia’s is predicted to vary in a systematic fashion as function of cosmic time (redshift). iv) double wds binaries are systems containing two wds that can merge and giving rise to sn explosion. yoon, podsiadlowski & rosswog (2007) explored the evolution of the merger of two carbon–oxygen (co) wds. their results imply that at least some products of double co wds merger may be considered good candidates for the progenitors of type–ia sne. brown et al. (2011) and kilic et al. (2011) studied a complete colour–selected sample of double–degenerate binary systems containing extremely low mass (elm) (≤ 0.25 m�) wds. milky way disc elm wds have a merger rate of ≈ 4 × 10−5 yr−1 due to gravitational wave radiation. the elm wd systems that undergo stable mass transfer can account for about 3% of am cvn stars. the most important fact is that the elm wd systems that may detonate merge at a rate comparable to the estimate rate of underluminous sne. these sne are rare explosions estimated to produce only ∼ 0.2 m� worth of ejecta. at least 25% of elm wd sample belong to the old tick disc and halo components of our galaxy. thus, if merging elm wd systems are the progenitors of underluminous sne, transient surveys must find them in both elliptical and spiral galaxies. v) wds accreting material from red–giant companions. observations carried out by patat et al. (2008) with vlt–uves allowed to detect circumstellar material in a normal type–ia sn. the expansion velocities, densities and dimensions of the circumstellar envelope indicate that this material was ejected from the system prior to the explosion. the relatively low expansion velocities favour a progenitor system where a wd accretes material from a companion star, which is in the red–giant phase at the time of explosion. bianco et al. (2011) searched for a signature of a non–degenerate companion in three years of supernova 13 f. giovannelli, l. sabau-graziati legacy survey data. they found that a contribution from wd/red–giant binary system to type–ia sn explosions greater than 10% at 2σ, and than 20% at 3σ level is ruled out. type–ia sne are used as primary distance indicators in cosmology (e.g. phillips, 2005). phillips (2011) reviewed the near–infrared (nir) of type–ia sne concluding that such sne are essentially perfect standard candles in the nir, displaying only a slight dependence of peak luminosity on decline rate and colour. lira (1995) first noted that b–v evolution during the period from 30 to 90 days after v maximum is remarkably similar for all sn ia events, regardless of light–curve shape. this fact was used by phillips et al. (1999) to calibrate the dependence of the bmax–vmax and vmax– imax colours on the light curve parameter ∆m15 (b) which can, in turn, be used to separately evaluate the host galaxy extinction. using these methods for eliminating the effect of the reddening, they reanalyzed the functional form of the decline rate versus luminosity relationship and gave a value of the hubble constant of h0 = 63.3± 2.2± 3.3 km s−1 mpc−1. the use of type–ia sne is also fundamental for determining some cosmological constraints, such as ωm and ωλ that fit a λcdm models with values of 0.211±0.034 (stat) ±0.069 (sys) using a set of 252 high– redshift sne (guy et al., 2010) and 0.713+0.027 −0.029 (stat) +0.036 −0.039 (sys) using a set of low–redshift nearby–hubble– flow sne (kowalski et al., 2008), respectively. in order to explore the difficult topic of the expansion of the universe it is necessary to know the evolution of metallicity in old universe that changes the hubble diagram shape. the proposed space observatory super nova acceleration probe (snap) is designed to measure the expansion of the universe and to determine the nature of the mysterious dark energy that is accelerating this expansion. snap is being proposed as part of the joint dark energy mission (jdem) (stril et al., 2010), which is a cooperative venture between nasa and the u.s. department of energy. if selected it will be launched before 2020. snap cannot achieve its main goal without progenitor/evolution solution. for comments and prospects about type–ia sn science in the decade 2010–2020 see the paper by howell et al. (2009). 6 some open questions several fundamental questions concerning cvs still remain waiting for a proper answer. we will present briefly only some of them here. one of them is the lack of a coherent classification, especially for nls. on the other hand, in gross features and in most respects, dn and nls, as well as quiescent novae, are almost indistinguishable, although, in addition to their different outbursts’ behaviour, there appear to be some further minor differences which are not yet understood (see hack & la dous 1993). the question arises of whether the outburst behaviour, the current basis of almost all classification is really a suitable criterion for sorting cvs in physically related groups. there are also too many exceptions, either systems that do not fit in any particular group or that can be included in several of them, to be able to render the observational behaviour, at least as it is used at the present, suitable. could cvs be considered simply gravimagnetic rotators? this should be the most suitable approach for studying them from a physical point of view. studies of rotational equilibria of mcvs predict that ipcvs will evolve either into pcvs or into low field strength polars — presumably unobservable, and possibly euv emitters — depending on their magnetic moments and orbital periods. indeed, there are systems, like ex hya-type, having magnetic moment similar to ipcvs above the ’period gap’ and comparable to the weakest field am her-like systems. moreover, the detection of several sw sex systems having orbital periods inside the so-called ’period gap’ opens a new interesting problem about the continuity in the evolution of cvs. the rare am canum venaticorum (am cvn) stars have extremely short orbital periods, between 10 and 65 minutes, and their spectra show no evidence for hydrogen. they appear to be helium-rich versions of cvs. they are still waiting for a general model. they are probably binary systems of two white dwarfs, but even this is still controversial. despite all the work developed during the last decades, the problem of modeling accretion discs in cvs is by no means closed, especially in quiescence. closely related is the problem of the cause of outbursts. we really do not know which of the present two families of models (disc instability models or secondary instability models) is responsible for the cvs outburst phenomenon, or in which system is each model valid, although martinez-pais et al. (1996) gave a contribution in solving this problem at least in the case of ss cygni; they found some evidence for an increase of the mass transfer rate from the secondary star as the mechanism responsible for symmetric outbursts. something similar can be said about the super-outburst phenomenon in su uma systems. gaudenzi et al. (1990), analyzing iue spectra of ss cygni, discussed about the outburst production as due to the destruction of the accretion disc. the matter, passing through the boundary layer, slowly accretes onto the wd. long and short outbursts correspond to 14 the golden age of cataclysmic variables and related objects (old and news) total or partial destruction of the disc, respectively. alternatively, could nuclear burning be responsible of the production of outbursts in cvs? indeed, nuclear burning onto white dwarf’ surface was proposed by mitrofanov (1978, 1980) as a mechanism suitable to generate x-rays in cvs. in spite of this shrewd suggestion, the community of theoreticians did not consider such a mechanism — certainly possible — worthy of taking up a part of their time. however, we believe that this alternative solution in explaining the generation of outbursts in cvs would deserve theoretician community’s care. for instance, the white dwarf surface interested in the accretion in the system ss cygni has been evaluated as 24% of the total (gaudenzi et al., 2002). there, nuclear burning could occur. accretional heating by periodic dn events increases substantially the surface temperature of the wd in cvs (godon & sion, 2002). then, the envelope thermal structure resulting from compression and irradiation should be a crucial component in understanding the envelope structure of a pre–nova wd. another problem still open is connected with the classification of cvs in three kinds, namely nmcvs, pcvs and ipcvs. this is, in our opinion, another convenient classification, although artificial, probably not necessary if cvs are studied as gravimagnetic rotators. in this way a smooth evolution of the systems could be responsible of the variations of the gravimagnetic parameters. are the ipcvs and pcvs smoothly connected via the sw sex-like systems placed just in between? sw sex systems have indeed orbital periods belong to the so-called ’period gap’, and then their presence there sure cancel that gap. could some systems behave in different ways depending on their instantaneous physical conditions? for this reason they could apparently behave sometimes as pcvs and sometimes as npcvs. an example very clear is that of ss cygni, usually classified as a non-magnetic dwarf nova. it has been detected by the integral observatory in a region of the spectrum (up to ∼ 100 kev). this emission is very hard to be explained without the presence of polar caps in the wd of the system. several proofs have been shown and discussed many times by giovannelli’s group in order to demonstrate the intermediate polar nature of it (e.g., giovannelli, 1996, and references therein; giovannelli & sabau-graziati, 1998; 2012a); indeed, ss cygni shows characteristics of a nmcv, as well as those of ip and sometimes even those of polars, although its position in the log pspin–log porb plane is very close to the line where ips lie. important results are coming from the spitzer space telescope with the detection of an excess (3-8) µm emission from magnetic cvs, due to dust (howell et al., 2006; brinkworth et al., 2007). gaudenzi et al. (2011) discussed about the reasons of the variable reddening in ss cyg and demonstrated that this reddening is formed by two components: the first is interstellar in origin, and the second (intrinsic to the system itself) is variable and changes during the evolution of a quiescent phase. moreover, an orbital modulation also exists. the physical and chemical parameters of the system are consistent with the possibility of formation of fullerenes. the spitzer space telescope detected the presence of fullerenes in a young planetary nebula (cami et al., 2010). fullerenes are the first bricks for the emergence of the life. therefore, the possible presence of fullerenes in cvs opens a new line of investigation, foreboding of new interesting surprises. 7 conclusions at the end of this review it appears evident that the most suitable approach for studying cvs from a physical point of view is to consider them as gravimagnetic rotators. the detection of several sw sex systems having orbital periods inside the so-called ’period gap’ opens a new interesting problem about the continuity in the evolution of cvs. are the ipcvs and pcvs smoothly connected via the sw sex-like systems placed just in between? in order to fully understand the emission properties and evolution of cvs, the mass–transfer process needs to be clearly understood, especially magnetic mass transfer, as well as the properties of magnetic viscosity in the accretion discs around compact objects. consequently, the investigation on the magnetic field intensities in wds appears crucial in understanding the evolution of cvs systems, by which it is possible to generate classical novae (e.g., isern et al., 1997) and type-ia supernovae (e.g., isern et al., 1993). in those catastrophic processes the production of light and heavy elements, and then the knowledge of their abundances provides strong direct inputs for cosmological models and cosmic ray generation problems. acknowledgments this research has made use of nasa’s astrophysics data system. references [1] andronov, i.l., chinarova, l.l., han, w., kim, y., yoon, j.-n.: 2008, a&a, 486, 855. 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properties of ae aquarii will be reviewed and explained in context of its evolution from a high mass transfer phase, during which period it could have been a supersoft x-ray source (sss). keywords: cataclysmic variable: ae aquarii radiation mechanisms: non-thermal line: identification techniques: spectroscopic. 1 introduction since its discovery on photographic plates in optical wavelengths (zinner 1938), the rapid variable star ae aquarii has been a source of continuous observational and theoretical study involving a wide range of frequencies from radio to tev gamma-rays. optical photometric studies showed that the system is highly variable, with ∆mv ≤ 2 magnitude outbursts occurring nearly continuously (e.g. henize 1949, patterson 1979, van paradijs, kraakman & van amerongen 1989). distance estimates place the source at ∼ 100 pc (welsh, horne & oke 1993). 2 optical and x-ray pulsations the first photometric pulse-timing study of ae aquarii in the optical band (patterson 1979) revealed steady coherent pulsations in the power spectra at p◦ ≈ 33 s and p1 ≈ 16 s, which were interpreted as the spin period of an obliquely rotating white dwarf and its associated first harmonic, caused by the second pole reflecting from the inner edge of the accretion disc (patterson 1979). this led to its initial classification as a dq herculis type system (patterson 1979). fast optical spectroscopy performed later with the mount wilson 2.5 m coudé spectrograph in the wavelength band 636 682 nm, combined with simultaneous photometry in the same wavelength band (welsh, horne & gomer 1993), revealed that the pulsations originate from the white dwarf. however, it has been pointed out (patterson 1979) that the low pulsed fraction (≤ 1%) of the 33 s oscillation of ae aquarii is peculiarly low for a disc accreting white dwarf. in order to place ae aquarii with its rapidly rotating white dwarf in the dq herculis sub-class of the cataclysmic variables, accreting in the slow rotator limit from a well developed accretion disc, a magnetic surface field of b∗ ≤ 100 kg is required (e.g. patterson 1994). this is significantly lower than the inferred surface field of a disc accreting dq herculistype system, which is b∗ ∼ 106 − 107 gauss (patterson 1979). optical polarimetry (cropper 1986, stockman et al. 1992; beskrovnaya et al. 1995) revealed circular polarization ∼ 0.05− 0.1 % in optical light, which confirmed that the dwarf surface magnetic field is at least of the order b∗ ≥ 106 g (e.g. chanmugam & frank 1987). x-ray observations made by einstein (0.1 4 kev) showed the 33 s oscillation, with no indication of the associated 16 s first harmonic (patterson et al. 1980). this is confirmed by recent chandra x-ray observations (e.g oruru & meintjes 2012), which shows a single coherent pulse at 33 s. in optical wavelengths the 33 s period often disappears during outbursts (e.g patterson 1979; meintjes et al. 1992;1994), while the x-ray pulsed fraction determined with the einstein data seems to show some correlation with increasing count rate according to the relation pf(%) = 45(%/s−1)cr(s−1) in the observed count rate range 0.15-0.5 s−1 (e.g. meintjes & de jager 2000). no noticeable changes in the hardness ratio of the x-ray data has been observed during periods of enhanced activity (e.g. meintjes & de jager 2000; oruru & meintjes 2012). the weak correlation between the optical pulsed fraction of the coherent 33 s period and outbursts, together with the radial velocity measurements of uv lines observed during time-resolved spectroscopic observations made with the hubble space telescope hst, suggest a very effective propeller driven mass outflow in ae aquarii (e.g. patterson 1994; eracleous & horne 1996). 86 http://dx.doi.org/10.14311/app.2015.02.0086 ae aquarii: a short review 3 the propeller phase doppler tomography profiles of the ae aquarii system (e.g. wynn, king & horne 1997; ikhsanov, neustroev & beskrovnaya 2004) show tell-tale signatures of a propeller driven mass outflow from the system. the magnetospheric propeller process in ae aquarii was first explained within the framework of large diamagnetic blobs being propelled by a magnetospheric drag (wynn & king 1995; wynn, king & horne 1997). roche tomography of the secondary star (dunford & smith 2005; watson et al. 2006; smith, dunford & watson 2012) shows that ∼ 20% of the surface of the secondary star is covered with starspots, which may suggest a magnetically active secondary star. the effect of secondary star magnetic fields on the mass transfer process has been investigated (meintjes 2004). it has been shown that magnetic prominences can fragment the mass transfer flow into a blob-like stream, which upon interacting with the fast rotating white dwarf field, can be propelled from the system on time-scales that are short compared to the keplerian periods at the distance of closest approach of the stream (meintjes & venter 2005). recent spectroscopy performed with the 1.9 m telescope at sutherland revealed broad emission lines, which is most probably an indicator of high velocity gas in the system. the full-width half maximum width of these lines all implies velocities in excess of vesc ≥ 1000 km s−1 (meintjes, oruru & odendaal 2012), which is of the order of the escape velocity from the radius of closest approach of the stream. it has been shown (venter & meintjes 2006) that the interaction between the fast rotating magnetosphere and the stream of material from the secondary star may result in the development of kelvin-helmholtz instabilities, resulting in effective turbulence driven mixing of magnetic field with plasma. this results in a very effective transfer of angular momentum to the stream, propelling it from the system (venter & meintjes 2006). this has been confirmed by numerical simulations of the interaction between the fast rotating magnetic field of the white dwarf in ae aquarii and the mass flow from the secondary star (bisikalo & zhilkin 2012). the low accretion rate of the white dwarf in ae aquarii (ṁ∗ ∼ 1014 g s−1) compared to the mass transfer rate deduced from the uv emission line spectra (ṁ2 ∼ 1017 g s−1) implies that the white dwarf in ae aquarii is in a super-propeller (ejector) state (bisikalo & zhilkin 2012; ikhsanov & beskrovnaya 2012). the brightening of the source observed in optical on a regular basis, can therefore not readily be explained in terms of enhanced mass accretion onto the white dwarf. it has been shown (beardmore & osborne 1997) that the flaring activity in ae aquarii can be explained satisfactorily within the framework of colliding blobs propelled form the system by the magnetospheric propeller. these authors showed that collisions between faster and slower blobs will result in heating and resultant radiative cooling which can account for the outbursts in ae aquarii. 4 spin-down and particle acceleration the dissipated mhd power due to the magnetospheric propeller process in ae aquarii (e.g. meintjes & de jager 2000; meintjes & venter 2005) is of the order of pmag ∼ 1034 erg s−1, and comes at the expense of the rotational kinetic energy of the rapidly rotating white dwarf. a detailed pulse timing study of the white dwarf spin period, using a 14 year baseline (de jager et al. 1994) revealed that the white dwarf is spinning down at a rate of ṗ∗ ∼ 5.64 × 10−14 s s−1. this translates to a spin-down luminosity of the order of ls−d = iωω̇ ∼ 1034 erg s−1. a more recent study (mauche 2006) revealed that the spin-down rate of the white dwarf has sped-up. this can possibly be explained within the framework of mass transfer variations from the secondary star. the low accretion in comparison to the mass transfer α = ṁ∗/ṁ2 ∼ 0.1% may indicate that the white dwarf in ae aquarii is currently in a super-propeller (bisikalo & zhilkin 2012) or ejector phase (ikhsanov & beskrovnaya 2012) and that the white dwarf in ae aquarii may exhibit the same properties as a spun-up radio pulsar (e.g ikhsanov & bierman 2006). this implies that the low mass accretion and rapid rotation of the highly magnetized white dwarf may provide a mechanism for pulsar-like particle acceleration and nonthermal emission. recent results from suzaku x-ray satellite (terada et al. 2008) showed a non-thermal spectrum at energies εx ≥ 10 kev. it has been showed recently (e.g. oruru & meintjes 2012) that particles can be accelerated in the magnetosphere of the white dwarf to energies in excess of ε ≥ 100 gev, which may radiate synchrotron radiation at energies of the order of εx ∼ 10 kev in the weak magnetic field outside the corotation radius. 5 non-thermal emission radio observations performed in the late 1980’s showed that ae aquarii is a non-thermal emitter (bookbinder & lamb 1987, bastian, dulk & chanmugam 1988), showing continuous radio outbursts with maximum flux smjy ≤ 15 at frequencies ν ≤ 22.5 ghz. the high brightness temperature measured tb ≥ 1010 k definitely implies non-thermal emission, with the spectral slope smjy ∝ να, with α ∼ 0.3 − 0.5 (bastian, dulk & chanmugam 1988). the spectral properties of the radio emission in ae aquarii can be explained in 87 p. j. meintjes, a. odendaal, h. van heerden terms of a superposition of synchrotron emitting plasmoids, which expand and cool radiatively through synchrotron radiation (van der laan 1963; 1966). subsequent studies in infrared with iso (abada-simon et al. 2005) and spitzer (dubus et al. 2007) showed that the smjy ∝ να (α ∼ 0.5) non-thermal spectrum extends to a frequency ν ∼ 2000 ghz (dubus et al. 2007). the non-thermal radio-ir spectrum has been modeled successfully (meintjes & venter 2003; venter & meintjes 2006) in terms of synchrotron emission from relativistic electrons in expanding magnetized plasmoids in the propeller outflow. it has been shown that the frequency where the spectrum turns optically thin to radio emission is of the order of νt ≤ 3000 ghz. reports of pulsed burst-like vhe and tev gammaray emission in the 1990’s (bowden et al. 1992; meintjes et al. 1992;1994) sparked interest in ae aquarii as a non-thermal source of high energy emission. subsequent studies with various modern cerenkov detectors could unfortunately not confirm the earlier reports, leaving the vhe-tev status of ae aquarii still in doubt (e.g. lang et al. 1998; sidro et al. 2008; mauche et al. 2012). 6 the evolution the current properties of ae aquarii is consistent with a high mass accretion history (meintjes 2002; schenker et al. 2002). if one consider initial parameters porb,i ∼ 15h, m1,i ∼ 0.6m�, m2,i ∼ 1.6m� (i.e. qi ∼ 2.7) and r2,i ∼ 1.6r�, it can be shown that the initial thermal time-scale (τth ∼ 6.3 × 106(m2/1.6m�)−1 yr) mass transfer could have been of the order ṁ2,i ∼ 2×1019(m2,i/1.6m�)(τ/τth)−1 g s−1, still below the eddington value of ṁedd ≤ 7 × 1020(m1,i/0.6m�)−0.8 g s −1. it has been shown that this could have lasted until a critical q-ratio was reached, i.e. qcrit = 0.73 (meintjes 2002) during which time accretion disc torques could have spun-up the white dwarf to periods around ∼ 30 s over a time scale τsu ∼ 3 × 106 yr, which is similar to the thermal mass transfer time scale, i.e. τṁ ∼ few × 106 yr (meintjes 2002). the high mass accretion in this initial phase could have resulted in ae aquarii being a supersoft xray source (sss) (meintjes 2002; schenker et al. 2002). 7 conclusions the multi-frequency properties of ae aquarii have been summarized. the current asynchronicity of the spin and orbital period of ae aquarri can be explained in terms of a high mass accretion history during which period the white dwarf could have been spun-up by accretion disc torques to a short period. in this phase the high accretion rate could have resulted in the system being a sss. a subsequent decrease in the mass transfer rate from the secondary drove the system into the propeller state, which may be the driving mechanism behind the multi-frequency emission from the system. acknowledgement the authors thank the organisers for the invitation to present this work at this conference. references [1] abada-simon, m. et al.: 2005, a&a, 433, 1063 [2] bastian, t.s., dulk, g.a. & chanmugam, g.: 1988, apj, 324, 431 doi:10.1086/165906 [3] beardmore, a.p. & osborne, j.p.: 1997, mnras, 290, 145 doi:10.1093/mnras/290.1.145 [4] bisikalo, d.v. & zhilkin, a.g.: 2012 in golden age of cataclysmic variables and related objects, palermo (september 12-17, 2011), memorie s.a.it, vol 83 (2), p. 562 (eds. f. giovanelli & l. sabau-graziati) [5] beskrovnaya, n.g., ikhsanov, n.r., bruch, a. & shakovskoy, n.m.: 1995, in proc. of the cape workshop on magnetic cataclysmic variables, cape town (1995), asp conf. ser. vol. 85, p. 364, astron. soc. pacific, san francisco (eds. d.a.h. buckley & b. warner) [6] bookbinder j.a. & lamb, d.q.: 1987, apj, 323, l131 doi:10.1086/185072 [7] bowden, c.c.g. et al.: 1992, astropart. phys., 1, 47 doi:10.1016/0927-6505(92)90008-n [8] chanmugam, g. & frank, j.: 1987, apj, 320, 746 doi:10.1086/165592 [9] cropper, m.: 1986, mnras, 222, 225 doi:10.1093/mnras/222.2.225 [10] de jager, o.c., meintjes, p.j., o’donoghue, d. & robinson, e.l.: 1994, mnras, 267, 577 doi:10.1093/mnras/267.3.577 [11] dubus, g., taam, r.e., hull, c., watson, d.m. & mauerhan, j.c.: 2007, apj, 663, 516 doi:10.1086/518407 [12] dunford a. & smith r.c.: 2005, proc. of the astrophysics of cataclysmic variables and related objects workshop, strasbourg (france), asp conference series, vol. 330, p. 399, astron. soc. pacific, san francisco (eds. j.-m hameury & j.-p lasota) 88 http://dx.doi.org/10.1086/165906 http://dx.doi.org/10.1093/mnras/290.1.145 http://dx.doi.org/10.1086/185072 http://dx.doi.org/10.1016/0927-6505(92)90008-n http://dx.doi.org/10.1086/165592 http://dx.doi.org/10.1093/mnras/222.2.225 http://dx.doi.org/10.1093/mnras/267.3.577 http://dx.doi.org/10.1086/518407 ae aquarii: a short review [13] eracleous, m, & horne, k.: 1996, apj, 471, 427 doi:10.1086/177979 [14] henize, k.g.: 1949, aj, 54, 89 [15] ikhsanov, n.r., neustroev, v.v. & beskrovnaya, n.g.: 2004, a&a, 421, 1131 [16] ikhsanov, n.r. & biermann, p.l.: 2006, a&a, 445, 305 [17] ikhsanov, n.r. & beskrovnaya, n.g.: 2012, arxiv: 1205.4330v1 [astro-ph.he] (19 may 2012) [18] lang, m.j. et al.: 1998, astropart. phys., 9, 203 doi:10.1016/s0927-6505(98)00020-6 [19] mauche, c.w.: 2006, mnras, 369, 1983 doi:10.1111/j.1365-2966.2006.10447.x [20] mauche, c.w. et al.: 2012, in golden age of cataclysmic variables and related objects, palermo (september 12-17, 2011), memorie s.a.it, vol 83 (2), p. 651 (eds. f. giovanelli & l. sabau-graziati) [21] meintjes, p.j. et al.: 1992, apj, 401, 325 [22] meintjes, p.j. et al.:1994, apj, 434, 292 [23] meintjes, p.j., oruru, b. & odendaal, a.: 2012, in golden age of cataclysmic variables and related objects, palermo (september 12-17, 2011), memorie s.a.it, vol 83 (2), p. 643 (eds. f. giovanelli & l. sabau-graziati) [24] meintjes, p.j. & de jager, o.c.: 2000, mnras, 311, 611 [25] meintjes, p.j.: 2002, mnras, 336, 265 [26] meintjes, p.j.: 2004, mnras, 352, 416 [27] meintjes, p.j. & venter l.a.: 2003, mnras, 341, 891 [28] meintjes p.j. & venter, l.a.: 2005, mnras, 360, 573 [29] oruru, b. & meintjes p.j.: 2012, mnras, 421, 1557 doi:10.1111/j.1365-2966.2012.20410.x [30] patterson, j.: 1979, apj, 234, 978 doi:10.1086/157582 [31] patterson, j., branch, d., chincarini, g. & robinson e.l.: 1980, apj, 240, l133 doi:10.1086/183339 [32] patterson, j.: 1994, pasp, 106, 209 doi:10.1086/133375 [33] schenker, k. et al.: 2002, mnras, 337, 1105 doi:10.1046/j.1365-8711.2002.05999.x [34] sidro, n. et al.: 2008, international cosmic ray conference (icrc), 2, 715 [35] smith, r.c., dunford, a. & watson, c.a.: 2012, in golden age of cataclysmic variables and related objects, palermo (september 12-17, 2011), memorie s.a.it, vol 83 (2), p. 708 (eds. f. giovanelli & l. sabau-graziati) [36] stockman, h.s., schmidt, g.d., berriman g., liebert, j., moore, r.l. & wickramasinghe, d.t.: 1992, apj, 401, 628 [37] terada, y. et al.: 2008, publ. astron. soc. japan, 60, 387 [38] van der laan, h.: 1963, mnras, 126, 535 [39] van der laan, h.: 1966, nature, 211, 1131 [40] van paradijs, j., kraakman, h. & van amerongen, s.: 1989, a&a, 79, 205 [41] venter, l.a. & meintjes, p.j.: 2006, mnras. 366, 557 [42] watson, c.a., dhillon, v.s. & shahbaz, t.: 2006, mnras, 368, 637 [43] welsh, w.f., horne, k., & oke,j.b.: 1993, apj, 406, 229 [44] welsh, w.f., horne, k., & gomer, r.: 1993, apj, 410, l39 [45] wynn, g.a. & king, a.r. 1995:, mnras, 275, 9 [46] wynn, g.a., king, a.r. & horne, k. 1997: mnras, 286, 436 [47] zinner, e.: 1938, astron. nach., 265, 345 discussion dimitri bisikalo: is there any observational evidence of mass flow surrounding the white dwarf? pieter meintjes: there is observational evidence of mass being ejected from the system. the propeller is extremely effective, only ∼ 0.1% of the mass transfer flow gets accreted onto the surface. the rest is ejected from the system. optical and uv spectroscopy indicate high velocity flows. there may be a circumbinary ring of ejected matter present surrounding the system. 89 http://dx.doi.org/10.1086/177979 http://dx.doi.org/10.1016/s0927-6505(98)00020-6 http://dx.doi.org/10.1111/j.1365-2966.2006.10447.x http://dx.doi.org/10.1111/j.1365-2966.2012.20410.x http://dx.doi.org/10.1086/157582 http://dx.doi.org/10.1086/183339 http://dx.doi.org/10.1086/133375 http://dx.doi.org/10.1046/j.1365-8711.2002.05999.x introduction optical and x-ray pulsations the propeller phase spin-down and particle acceleration non-thermal emission the evolution conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.9.0008 acta polytechnica ctu proceedings 9:8–12, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app phase analysis of niti wire based on synchrotron 2d x-ray diffraction pattern in matlab martin dudra,∗, daniel šimekb, jan drahokoupila,b a department of solid state engineerign faculty of nuclear sciences and physical engineering czech technical university in prague, trojanova 13 120 00 prague 2, czech republic b institute of physics , na slovance 2 182 21 prague, czech republic ∗ corresponding author: dudrmart@fjfi.cvut.cz abstract. this paper deals with simplified phase analysis of 2d diffraction patterns obtained using microfocused x-ray at various places of superelastic niti wire under combined load. for this purpose, matlab routines and functions were created, which carry out integration of the patterns in various sectors of debye ring, fitting of the patterns by a mixture of austenite and martensite (having neglected the r-phase) and successive evaluation of the quantitative phase content. the most crucial simplificating assumptions were: the neglection of the r-phase and the assumption of a) fibre texture or b) no texture. keywords: nitinol spring, combined load, x-ray diffraction, phase analysis, synchrotron. 1. introduction a superelastic nitinol wire under combined load was subjected to xrd measurements using microfocused beam at european synchrotron radiation facility (esrf) in grenoble. quantitative phase analysis at different points on the wire was expected to be carried out. as the number of outcoming images was large (12 000), there was need of their automated processing. moreover the sample was strongly textured and therefore the integration of debye rings was preferred to be done "per partes", that means separately in various sectors ("pieces of cake") in order to implement some texture corrections later. some matlab routines were created that fulfilled these specific demands. this paper briefly explains basic principles of the approach in use and presents results obtained from the routines. 2. material and methods 2.1. nitinol nitinol is a well-known shape memory alloy of a near equiatomic stoichiometric composition ni-ti. the shape memory in niti is based on so called martensitic transformation (mt) between cubic austenite (high-temperature phase) and monoclinic twinning martensite (low-temperature phase). mt can be induced by lowering the temperature below transition point or by applying sufficient mechanical stress onto austenite. there is a third phase called r-phase, which under certain conditions stands in between the former two. it is unstable and hardly preparable solely. [1] r-phase is trigonal. [2] 2.2. quantitative phase analysis quantitative phase analysis (qpa) responds to both questions "what?" and "how much?" when talking about a mixture of phases. the diffraction pattern outcoming from measurement on a polycrystalline sample in transmission geometry recorded on 2d detector looks like a set of concentric circles. each of the circles corresponds to one set of equivalent crystallographical planes of the sample. when the pattern is integrated in tangential direction 1d patterns are obtained for the integrated interval. position of the peak in 1d pattern (i.e. the radius of the corresponding circle) is important for qualitative phase analysis (i.e. "what?"), the integrated intensity of the peak determines the amount of phase in a mixture ("how much?"), hence it is used by quantitative phase analysis. there are many factors determining the real value of integrated intensity. let ihkl be an integrated intensity of crystallographical planes (hkl), then we can write [3] ihkl = k ·phkl ·lθ ·pθ ·aθ ·thkl ·ehkl · |fhkl|2 . (1) k is a scale factor, which is proportional to diffracting volume of the phase and therefore it is of great importance in qpa. other factors are multiplicity of planes phkl, lorentz factor lθ, polarization factor pθ, absorption factor aθ , texture correction thkl which will be discussed further on, extinction factor ehkl and important structure factor squared |fhkl|2. the principle of qpa is very simple: to isolate the scale factors k for the phases in mixture from the equation 1. nevertheless, some of the other factors and corrections need not to be easily determinable. especially texture correction may be troublesome as texture (also called preferred orientation) description usually requires specific measurement and nontrivial data analysis. in this paper the authors tried to approximate the real texture by two simplificating cases separately: 8 http://dx.doi.org/10.14311/app.2017.9.0008 http://ojs.cvut.cz/ojs/index.php/app vol. 9/2017 phase analysis of niti wire based on synchrotron 2d xrd pattern mm 0 1 2 3 4 5 6 7 8 9 10 m m 0 0.5 1 figure 1. visualization of gridpoints showing diffraction on the sample. one pixel corresponds to one image, axes have equal scale. a) radially symmetric fibre texture and b) no texture at all. 2.3. experimental the sample was a coiled round wire of 0.2 mm diameter from superelastic alloy niti#1 [4]. this helical spring was elongated in uniaxial tension, which induced a complex stress state consisting of torsion and tension/compression due to bending of the spring. the tensile load was of 1.6 n. measurements were carried out at esrf, grenoble, at beamline 15a [5]. the wavelength of used radiation was λ = 0.0268128 nm. microfocused x-ray beam of rectangular cross-section 20 µm× 5 µm was used to scan in a rectangular grid of 12 000 points of which approximately 2 200 covered the sample. more precisely speaking it was a grid of 100× 120 points and of measures 10 mm× 1.1 mm. so the step was 100 µm in the x direction and cca 9.1 µm in the y direction. in figure 1 the scanned area is to be seen. each pixel corresponds to one gridpoint (one measurement, one image). blue pixels represent measurements where only background was captured (low average intensity in the image) and the yellow pixels correspond to images capturing the sample diffraction pattern (average intensity was larger). the wire profile is clearly visible. 2.4. data processing before the data processing itself the wavelength and sample-detector distance were determined using two calibration images taken on calibrant ceo2 in different sample-detector distances. then the integration in polar angle was carried out. due to strong texture of the sample and as a macrodeformation is expected, the integration was carried out in nine sectors separately, as indicated in figure 2. as the structure of austenite and martensite is known [6] it is possible to estimate the positions of diffraction lines of these phases. there was designed such an algorithm, that tries to fit an analytical function pearson vii to place where we expect austenitic or martensitic line. the whole pattern is then superposition of these pearsons which are all fitted at once, hence it is a whole profile fitting approach, more specifically le bail fitting the latter means that the intensities of lines are fitted parameters (see parameter a1 below). it is possible to write pearson vii in figure 2. indication of nine sectors in which the integration was carried out. each sector has angular width of 20°. a following form [7] pvii(x) = a1 1 [1 + (x−a2)2a3]a4 . (2) parameters a1, a2, a3 and a4 define the height of the function, its position in x, width and shape respectively. in the work other form was used, but the above mentioned one is more clear. the parameter a2 was a function of lattice parameters and macrodeformation (voigt model of strain distribution was assumed). the parameter a3 was a function of crystallite size and microdeformation (accordingly to williamson-hall equation for width of a diffraction line). parameters a1 (for all lines) and a4 (for each phase austenite and martensite) were fitted directly. the area under pearson vii function is possible to express analytically from the parameters a1, a2, a3 and a4. this area represents the integral intensity of a given line. the fitting was performed using nonlinear least squares, by so called levenberg-marquardt method. the fitting was carried out in all the sectors at once. some parameters were related only to a specific sector (e.g. a height a1 of a particular line in a sector), others were fitted on basis of all sectors (e.g. 3 macrodeformation-describing parameters per phase). there were 60 linear parameters in each sector (height a1 of 50 lines of martensite and 7 lines of austenite plus 3 parameters describing background) and cca 10 other nonlinear parameters which was possible to exclude from fitting (these were related to a2, a3 and a4). altogether it makes cca 550 parameters to be fitted in one image. once the integral intensity of all lines (of austenite as well as martensite) is assumed to be known from fitted parameters, the left side of equation 1 is known and thus it is possible to start isolating scale factors k of both phases from the equation (if we know all other terms). in order to finish, the texture evaluation (in this case approximation) has to be carried out. the main difference between the fibre-texture approximation and no-texture approximation was especially in the weights, which were given to integral intensities 9 martin dudr, daniel šimek, jan drahokoupil acta polytechnica ctu proceedings mm 0 2 4 6 8 10 m m 0 0.2 0.4 0.6 0.8 1 aust mart mm 0 2 4 6 8 10 m m 0 0.2 0.4 0.6 0.8 1 aust mart figure 3. relative volume fractions of austenite and martensite with respect to the whole diffracting volume. in the left-hand figure the fibre-texture correction was applied, while on the right it was the no-texture approximation. the martensite is being represented by red channel, the austenite by the blue one. sin3/6 [angst-1] 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 in te ns ity [c ts ] #104 0.5 1 1.5 2 2.5 3 3.5 4 4.5 data fit figure 4. demonstration of fit in one sector. of lines from different sectors and in the number of lines which were taken into account. it is important to notice here that the r-phase was not taken into account in fitting. 3. results and discussion an example showing fit in one sector of image is in figure 4. each of the images taken on the sample (yellow pixels in figure 1) was processed individually and the ratios a/(a+m) and m/(a+m) were determined, where a resp. m stand for the volumes of austenite resp. martensite which contribute to diffraction, i.e. the volume fractions of the phases. the resulting volume fractions of both phases are in the figure 3. the strong prevalence of martensite is easily to be seen. four scans across the wire were chosen to demonstrate the results in detail, concretely scans 11, 36, 66 and 96 with no-texture correction. they have cca a quarter of spring coil period spacing in between, as mm 0 1 2 3 4 5 6 7 8 9 10 m m 0 0.2 0.4 0.6 0.8 1.1 11 966636 figure 5. indication of four scans which are presented in more detail. there were 100 scans in total, each of the indicated scans has its number denoted nearby. indicated in figure 5. each scan consists of cca 22 images. for the results themselves see figure 6. besides the diffracting volume of austenite and martensite there are two more informations in each graph. firstly a sum of austenite and martensite, which should follow an ellipse-like arch (the wire has more mass in the center than at the borders) and secondly illustrative semi-ellipse chosen so that its maximum value is slightly higher than maximum point of the sum of the phases. this is because the absorption correction was applied only partly during image integration, but it is still expected that the resulting intensity will be affected by absorption. the illustrative wire profile (semi-ellipse) serves only to easier comparison of the sum of volumes and the expectations. scans 36 and 96 mutually seem to be a mirror image of the other (with the mirror being placed vertically in the middle of each figure) in both we can see a decrease of sum of diffracting volumes close to the middle of the wire but shifted more to the right in scan 36 and to the left in scan 96. below this effect is explained by presence of r-phase. in figure 7 there is to be seen a central group of lines in the measured angle interval, where one line of austenite (110) and four lines of martensite are expected. obviously, there are two other lines which lay in between the austenitic line (110) and martensitic lines (1-11) and (002). the positions of austenitic and 10 vol. 9/2017 phase analysis of niti wire based on synchrotron 2d xrd pattern pattern no. 5 10 15 20 di ffr ac in g vo lu m e [a .u .] 0 0.05 0.1 0.15 scan no. 11 pattern no. 5 10 15 20 di ffr ac in g vo lu m e [a .u .] 0 0.05 0.1 0.15 scan no. 36 pattern no. 5 10 15 20 di ffr ac in g vo lu m e [a .u .] 0 0.05 0.1 0.15 scan no. 66 pattern no. 5 10 15 20 di ffr ac in g vo lu m e [a .u .] 0 0.05 0.1 0.15 scan no. 96 aust mart sum aust+mart wire profile figure 6. results of phase analysis for four scans (no-texture approximation). the y axis shows diffracting volumes, x shows the order number of the images in the given scan. blue color stands for the diffracting volume of austenite, the red one for the diffracting volume of martensite and the green one is a summation of the two. the black line indicates the theoretical wire mass profile. martensitic lines in the group are well defined the pattern was fitted at once, hence all the well-isolated lines in the pattern fix positions of lines in the group. they are all bound together by the lattice parameters. but then the two excessive lines must belong to other phase. it is concluded that this phase is r-phase. as the algorithm could not move the lines, it could minimize the sum of squares only using height, width and shapes of lines. the height is most significant factor then, and its adjustment subsequently influences the resulting austenite or martensite volume fraction. but this compensation is not perfect, which implies the loss of overall sum of the fractions. r-phase is usually found somewhere in between the austenite and martensite. if the interface is more or less of a planar aspect then from some angle the microfocused beam could be passing through the r-phase region rather perpendicularly (scans 11 and 66 in figure 6) and so the irradiated r-phase volume would be low. on the other hand it would be significantly higher if the beam was passing along the r-phase region (scans 36 and 96). in that case the sum of diffracting volumes evaluated from the presented fit would be most deficient (as explained above). when the overall sum of diffracting volumes was subtracted from virtual wire profile, pictures in figsin( 3)/6 [nm -1 ] 0.42 0.44 0.46 0.48 0.5 0.52 in te ns ity a .u . #10 4 0.5 1 1.5 2 2.5 3 3.5 4 4.5 data fit aust+mart fit aust fit mart lines mart lines aust (1-11) (110) (021)(111) (002) figure 7. central group of peaks proving the presence of r-phase. positions of austenitic, resp. martensitic lines are denoted by crosses of the same color as the fit of the given phase (austenite is denoted by blue, martensite by red color). green line stands for the sum of the former two fits, black dots are measured values. ure 8 were obtained. these pictures depict this difference relative to the virtual wire profile, i.e. (vvirt − vcalc)/vvirt. because the absorption correc11 martin dudr, daniel šimek, jan drahokoupil acta polytechnica ctu proceedings mm 0 2 4 6 8 10 m m 0 0.2 0.4 0.6 0.8 1 -1 -0.8 -0.6 -0.4 -0.2 0 0.2 0.4 0.6 0.8 1 mm 0 2 4 6 8 10 m m 0 0.2 0.4 0.6 0.8 1 -1 -0.8 -0.6 -0.4 -0.2 0 0.2 0.4 0.6 0.8 1 figure 8. relative difference of calculated diffracting volume from virtual wire profile with respect to wire profile (symbolically (vvirt −vcalc)/vvirt). on the left with fibre-texture correction, on the right with no-texture correction. tion was not carried out thoroughly, some excess of calculated diffracting volume was observed on the borders and a systematic decrease in the central part. still, some deviation from this behavior is well noticeable. notice that extreme values (±1) are nearly only on the wire border. notice also that the virtual wire profile is only illustrative and serves for visualization of "shape" of the sum of diffracting volumes. it is also possible to see that the regions of greatest decline (orange-red regions in figure 8, where r-phase is expected, especially in the figure on the left) are the same as the regions where the most austenite was observed (compare with figure 3). from this we conclude that in this case we are unable to distinguish between austenite and r-phase. 4. conclusion a simplified quantitative analysis of 2d diffraction patterns was carried out from transmission diffraction measurements of niti spring at european synchrotron radiation facility (esrf), grenoble. routines were created, which enabled automatic integration of 2d diffraction patterns and successive fitting of 1d patterns regarded as a two-phase mixture (whole-profile fitting based on analytical approach and levenbergmarquardt method of nonlinear least squares). with simplifying assumptions about texture it was possible to roughly estimate the ratio of the phases (austenite and martensite). martensite appears to be strongly prevalent in the sample. as the r-phase (which was present) was not taken into account the fit had troubles with convergence in those images where the r-phase occured significantly. these images show a loss of calculated overall diffracting volume. regions of higher austenite amount seem to be correlated with regions showing this loss, i.e. with regions where r-phase is expected too. on basis of presented results these two are not distinguishable. acknowledgements this work was supported by the grant agency of the czech technical university in prague, grant no. sgs16/245/ohk4/3t/14. references [1] šittner, landa, lukáš, novák. r-phase transformation phenomena in thermomechanically loaded niti polycrystals. mechanics of materials 38:475–492, 2006. [2] t. goryczka, h. morawiec. structure studies of the r-phase using x-ray diffraction methods. journal of alloys and compounds 367:137–141, 2004. [3] v.k. pecharsky, p.y. zavalij. fundamentals of powder diffraction and structural characterization of materials, 2nd edition, springer, usa, e-isbn: 978-0-387-09579-0, 2009. [4] fort wayne metals specification of nitinol#1 alloy http://www.fwmetals.com/services/ resource-library/nitinol-1/ [5] esrf official web page: id15a materials chemistry and materials engineering. [2016-10-14] , http://www.esrf.eu/usersandscience/experiments/ structmaterials/id15a. [6] h. p. stuwe,y. shimomura. gitterkonstanten der kubisch raumzentrierten phasen feti, coti, niti. zeitschrift fur metallkunde 51:180-181, 1960. [7] r. kužel. informace v práškovém difraktogramu a jeho zpracování. materials structure 10(1a): 18-19, 2003. 12 http://www.fwmetals.com/services/resource-library/nitinol-1/ http://www.fwmetals.com/services/resource-library/nitinol-1/ http://www.esrf.eu/usersandscience/experiments/structmaterials/id15a http://www.esrf.eu/usersandscience/experiments/structmaterials/id15a acta polytechnica ctu proceedings 9:1–5, 2017 1 introduction 2 material and methods 2.1 nitinol 2.2 quantitative phase analysis 2.3 experimental 2.4 data processing 3 results and discussion 4 conclusion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2016.3.0075 acta polytechnica ctu proceedings 3:75–77, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app preliminary assessment of the change in the mechanical behavior of synthetic yarns submitted to consecutive stiffness tests felipe tempel stumpf∗, carlos eduardo marcos guilherme, fulvio enrico giacomo chimisso policab stress analysis laboratory, av. itália km.8 , rio grande, brazil ∗ corresponding author: felipe.stumpf@furg.br abstract. anchoring systems of offshore platforms are designed to work uninterruptedly for 20 to 30 years, and despite the increasing number of studies concerning these systems’ mechanical behavior in working conditions, most of them are conducted in speeding environments, due to the necessity of results in the short term. there are standardized stiffness tests, such as iso 18692, based on quantities like dynamic stiffness and quasi-static stiffness, through which one can compare, quantitatively, two different ropes. however, there is a lack of research aiming to assess the change in the mechanical behavior of these ropes after certain number of consecutive loading cycles (or stiffness tests). this study aims to assess, at the yarn level, the change in the quasi-static and dynamic stiffness parameters of two materials when submitted to repeated stiffness tests. results in terms of qualitative assessment of the mechanical behavior, as well as quantitative changes in the parameters are presented. keywords: synthetic mooring ropes, ultra-deepwater, experimental mechanics. 1. introduction mooring lines used as anchoring systems of oil platforms must be designed to work uninterruptedly over more than 20 years, which means that, from a mechanical design point of view, their material’s mechanical behaviour must be well known (or, at least, accurately predictable) at each moment over the system’s life span. in the case of steel wire cables, for quite a long time that was not a major concern of engineers, since the mechanical behaviour of such metallic materials tends not to suffer considering changes in that amount of time. however, over the course of the last couple of decades, new oil fields have been discovered in ultradeepwater (5000 m to 7000 m water depth), what has led the oil companies to use light-weight materials as mooring lines of their platforms’ anchoring system [1]. initially, polyester (pet) was considered the most suitable material for such applications [1], especially due to its low cost and its reliability in terms of small changes in the mechanical behaviour over time (very low creep rate, for instance). one of the main disadvantages of pet, however, is that it tends to show considerable elongation (aprox. 20 % in rupture) in tension, what might present a problem for long mooring lines in terms of station-keeping [1, 2]. aiming to find a more suitable option for these systems, the oil companies are testing several other synthetic materials, such as aramid, polyamide, high modulus polyethylene (hmpe), liquid crystal polyethylene, etc. all of those show a considerable lower elongation in comparison to pet [3, 4], but sometimes the price to be paid is a significant increase of their creep rate, or even higher production costs [5, 6]. high modulus polyethylene, for example, has the advantage to have a lower-than-water density [2], which means that it does not add weight to the platform when installed. there are some standardized stiffness tests, such as iso 18692:2013 [7], based on quantities such as static stiffness, dynamic stiffness (ds) and quasistatic stiffness (qss), through which one can compare, quantitatively, the mechanical behavior of two different ropes after some pre-defined tension/creep loads. however, there is a lack of research aiming to assess the change in the mechanical behavior of these materials after a certain number of consecutive loading cycles (or stiffness tests). the present study aims to promote a preliminary assessment, at the yarn level, of the change in the quasi-static and dynamic stiffness parameters of these materials when submitted to repeated stiffness tests. yarns of two different hmpe were submitted to a series of four consecutive stiffness experiments, with a period of ten hours between tests to promote possible relaxation of the samples in controlled environment. 2. quasi-static stiffness and dynamic stiffness the industry, both oil companies and rope makers, make use of [7] to measure qss and ds of their products in order to compare the stiffness of different materials or different rope configurations. 2.1. quasi-static stiffness according to the standard, the qss consists in "the static stiffness, which is reduced to account for the 75 http://dx.doi.org/10.14311/app.2016.3.0075 http://ojs.cvut.cz/ojs/index.php/app stumpf, guilherme, chimisso acta polytechnica ctu proceedings figure 1. test routine according to iso 18692:2013 [7]. rope creep under an environmental event". during its life in service, a mooring rope is submitted not only to dynamic loadings, but also to constant loads at moderate to high intensity. therefore, one must consider the creep behavior of these systems when designing an anchoring system, as well as the influence that this kind of loading has over the mechanical behavior of the rope. the quasi-static stiffness attempts to evaluate the loss in stiffness of the rope due to these creep regimes to which it is submitted during its lifetime. 2.2. dynamic stiffness the definition of ds follows as "the ratio of change in load to change in strain in a rope under cyclic loading". it is a quite straighforward definition, since instead of the classic stiffness which is measured during quasistatic tension tests, it is obtained at the hundredth load cycle, as depicted in figure 1. 3. materials and methods for a specific rope, subrope, strand, or yarn, the test routine depicted in figure 1 together with equation 1 are used to calculate qss and ds. qss, ds = fy − fx y bl ly − lx l0 + ly (1) the test routine (tr) showed in figure 1 was performed four consecutive times (tr#1, tr#2, tr#3 and tr#4) for each sample and for each type of hmpe (hmpe#1 and hmpe#2), with an interval of 10 hours between experiments. at the end of each routine, the quasi-static (qss#1, qss#2, qss#3, total qss) and the dynamic stiffness (ds#1, ds#2, ds#3) were calculated. the yarn samples were 500 mm long and were attached to the clamps of the machine using sandwich type endings. figure 2 shows one of the samples. all the tests have been run at room temperature of 20 ± 2 °c and 65 ± 4 % of air relative humidity. the tests were performed on an instron 8801 servohydraullic fatigue testing machine using a 10kn dynacell load cell. figure 2. typical yarns sample with sandwich type endings. 4. results figures 3–6 and tables 1–4 resume the results obtained for the evolution of qss and ds of the two types of hmpe over each test routine. figure 3. evolution of qss over each tr for hmpe#1. qss#1 qss#2 qss#3 total qss tr#1 18,9 33,2 32,4 15,7 tr#2 19,8 30,1 34,0 17,1 tr#3 18,7 33,9 34,6 17,3 tr#4 17,8 30,0 31,7 15,6 table 1. results for qss: hmpe#1. 5. conlcusions it can be seen that both quasi-static and dynamic stiffness of both materials show, in general, a stabilizing tendency along calculations #1, #2 and #3. the first stiffness (qss#1 and ds#1) is always the lowest one, followed by a considerable increase at moment #2 (qss#2 and ds#2) and, finally, a smaller increase 76 vol. 3/2016 mechanical behavior of synthetic yarns figure 4. evolution of ds over each tr for hmpe#1. ds#1 ds#2 ds#3 tr#1 58,1 59,5 60,3 tr#2 57,3 58,4 59,0 tr#3 57,4 60,0 59,2 tr#4 57,1 60,1 59,6 table 2. results for ds: hmpe#1. figure 5. evolution of qss over each tr for hmpe#2. qss#1 qss#2 qss#3 total qss tr#1 18,4 30,9 32,4 16,4 tr#2 19,4 31,7 34,7 20,0 tr#3 19,9 31,3 32,2 18,1 tr#4 19,2 32,2 33,3 19,0 table 3. results for qss: hmpe#2. figure 6. evolution of ds over each tr for hmpe#2. up to calculation #3 (qss#3 and ds#3). in other words, the more you cycle these materials, the more stiff they get, until they reach what appears to be a limiting stiffness. ds#1 ds#2 ds#3 tr#1 54,4 57,4 57,5 tr#2 54,0 55,5 56,9 tr#3 52,6 57,1 57,0 tr#4 54,3 57,1 57,7 table 4. results for ds: hmpe#2. in terms of the quasi-static stiffness, the total qss (dashed lines in figures 3–6) tends to be similar to qss#1, leading to the conclusion that both can be used for a conservative approach. comparing results between tr#1, tr#2, tr#3 and tr#4, there is no evidence, so far, that the consecutive loading of the same specimen leads to a trending change of these stiffness properties for hmpe. perhaps, if the routines were repeated a few more times, we could see a drop in qss and ds, what would mean that the material is becoming less stiff with time, what could be a problem in terms of designing a mooring line. list of symbols f force [n] y bl yarn break load [n] l elongation [m] acknowledgements policab team would like to thank petrobras brazilian petroleum for sponsoring this work. references [1] c. j. m. d. vecchio. light weight materials for deep water moorings. phd thesis. university of reading, 1992. [2] p. davies, y. reaud, l. dussud, p. woerther. mechanical behaviour of hmpe and aramid fibre ropes for deep sea handling operations. ocean engineering 38:2208–2214, 2011. doi:10.1016/j.oceaneng.2011.10.010. [3] p. davies, s. d. weller, l. johanning, s. j. banfield. a review of synthetic fiber moorings for marine energy applications. 5th international conference on ocean energy (icoe 2014) 2014. [4] s. leite, j. boesten. hmpe mooring lines for deepwater modus. offshore technology conference (otc) 2011. [5] w. huang, h. liu, y. lian, l. li. modeling nonlinear creep and recovery behaviors of synthetic fiber ropes for deepwater moorings. applied ocean research 39:113–120, 2012. doi:10.1016/j.apor.2012.10.004. [6] h. s. d. c. mattos, f. e. g. chimisso. modelling creep tests in hmpe fibres used in ultra-deep-sea mooring ropes. int j sol struct 48:144–152, 2011. doi:10.1016/j.ijsolstr.2010.09.015. [7] international organization for standardization. iso 18692:2013: fibre ropes for offshore stationkeeping — polyester, 2013. 77 http://dx.doi.org/10.1016/j.oceaneng.2011.10.010 http://dx.doi.org/10.1016/j.apor.2012.10.004 http://dx.doi.org/10.1016/j.ijsolstr.2010.09.015 acta polytechnica ctu proceedings 3:75–77, 2016 1 introduction 2 quasi-static stiffness and dynamic stiffness 2.1 quasi-static stiffness 2.2 dynamic stiffness 3 materials and methods 4 results 5 conlcusions list of symbols acknowledgements references 34 acta polytechnica ctu proceedings 1(1): 34–37, 2014 34 doi: 10.14311/app.2014.01.0034 a novel approach in the wimp quest: cross-correlation of gamma-ray anisotropies and cosmic shear marco regis1 1dipartimento di fisica, università di torino and infn, torino, italy corresponding author: regis@to.infn.it abstract we present the cross-correlation angular power spectrum of cosmic shear and gamma-rays produced by the annihilation/decay of weakly interacting massive particle (wimp) dark matter (dm), and by astrophysical sources. we show that this observable can provide novel information on the composition of the extra-galactic gamma-ray background (egb), since the amplitude and shape of the cross-correlation signal depend on which class of sources is responsible for the gamma-ray emission. if the dm contribution to the egb is significant (at least in a definite energy range), although compatible with current observational bounds, its strong correlation with the cosmic shear (since both signals peak at large halo masses) makes such signature potentially detectable by combining fermi-lat data with forthcoming galaxy surveys, like dark energy survey and euclid. keywords: dark matter extragalactic gamma rays background weak gravitational lensing. 1 introduction the presence of gravitational anomalies at different scales (galactic, cluster, large scale structure, and cosmological scales) is observationally well-established. however, it is not fully understood yet whether such anomalies are due to a new form of matter (i.e., dark matter (dm)) or to a new form of interaction (e.g., a modification of the laws of gravity). currently, the dm solution represents the mainstream, mainly because there is no theory of gravity which can account for all the anomalies at different scales simultaneously. for example, mond (modified newtonian dynamics) is a theory stating that acceleration is not linearly proportional to gravitational force at small accelerations, and seems to be quite successful in explaining galactic rotation curves. however, it cannot explain cluster dynamics without the addition of some dm components. on the other hand, it is possible that we just haven’t been good enough to build the proper extension to newtonian and einstein gravity. moreover, if dm interacts only gravitationally with ordinary matter, the two classes of solution are hardly distinguishable. one of the best ways to settle the issue would be to detect a non-gravitational signal of dm coming from the regions with gravitational anomalies. in this talk, we will present a novel strategy in this direction. in particular, if dm is made by weakly interacting massive particles (wimps), they have weak but non-negligible interactions with ordinary matter, and one of the predictions of the model is sizable fluxes of γ-rays from dm halos. both cosmic shear and cosmological gamma-ray emission stem from the presence of dm in the universe: dm structures are responsible for the bending of light in the weak lensing regime and while γ-rays can be produced by astrophysical sources hosted by dm halos (i.e. star-forming galaxies (sfg) or active galactic nuclei (agn)), dm itself may be a source of γ-rays, through its self annihilation or decay, depending on the properties of the dm particle. those γ-rays emitted by dm should therefore have the potential to exhibit strong correlation with the gravitational lensing signal. the most recent measurement of the egb was performed by the fermi-lat telescope in abdo et al. (2010)a, covering a range between 200 mev and 100 gev: the emission is obtained by subtracting the contribution of resolved sources (both point-like and extended) and the galactic foreground (due to cosmic rays interaction with the interstellar medium) from the whole fermi-lat data. unresolved astrophysical sources like blazars or radio galaxies contribute to the egb but the exact amount of their contribution is still unknown. the γ-rays produced by dm annihilation or decay can also contribute to egb (e.g., ullio et al. (2002)). however, the fact that the egb energy spectrum is compatible with a power-law, without any evident spectral feature, suggests that dm cannot play a leading role in the whole energy range, see abdo et al. (2010)b. 34 http://dx.doi.org/10.14311/app.2014.01.0034 a novel approach in the wimp quest: cross-correlation of gamma-ray anisotropies and cosmic shear in the angular anisotropies of the egb emission, the dm also plays a subdominant role: indeed, a detection of a significant auto-correlation angular ps has been recently reported in ackermann et al. (2012) (for multipoles ` > 100, which is the range of interest for our analysis, since there the contamination of the galactic foreground can be neglected), but the features of such a signal (in particular its independence on multipole and energy) seem to indicate an interpretation in terms of blazars, harding & abazajian (2012). both cosmic shear and γ-ray emission depend on the large scale structure of the universe: because this is what generates the lensing effect and because those same structures can produce γ-rays. here we will show how to use the lensing signal in order to possibly disentangle a dm signal in the egb. a detection of such cross-correlation would demonstrate that the weak lensing observables are indeed due to particle dm matter and not to possible modifications of general relativity. this presentation is based on camera et al. (2012). figure 1: left: egb emission as a function of observed energy for the four extragalactic components described in the text. data are from abdo et al. (2010)a. right: γ-ray angular ps at e > 1 gev for the same models of the left panel. the observed angular ps is summarized by the black band from ackermann et al. (2012). this figure is taken from camera et al. (2012). figure 2: left: window functions vs. redshift. for γ-ray sources we consider the flux above 1 gev normalized to the total egb intensity measured by fermilat. right: three-dimensional ps of cross-correlation shear/γ-rays at z = 0. this figure is taken from camera et al. (2012). 2 theoretical modeling the source intensity along a given direction ~n can be written as: ig(~n) = ∫ dχ g(χ,~n) w̃ (χ) , (1) where χ(z) is the radial comoving distance, g is the density field of the source, and w̃ is the window function (which does not depend on ~n). we then define a normalized versionw = 〈g〉 w̃ , so 〈ig〉 = ∫ dχ w (χ). expanding the intensity fluctuations of two source populations i and j in spherical harmonics, one can compute the cross-correlation angular ps (here in the dimensionless form): c (ij) ` = 1 〈ii〉〈ij〉 ∫ dχ χ2 wi(χ)wj(χ)pij(k = `/χ, χ) . (2) the definition of the 3-dimensional ps pij is 〈f̂gi(χ,~k)f̂∗gj (χ′,~k′)〉 = (2π)3δ3(~k − ~k′)pij(k, χ, χ ′) , (3) where fg ≡ [g(~x|m, z)/ḡ(z) − 1] (f̂g is its fourier transform) and the limber approximation (k = `/χ) is assumed to hold. we consider the sources to be characterized by a parameter m (typically the mass), and g(~x|m) is the density field of an object associated to m, while ḡ(z) = 〈g(~n, z)〉. pij can be computed following the so-called halo-model approach. the two-point correlation is given by the sum of two components, the 1-halo and 2-halo terms, i.e. pij = p 1h ij +p 2h ij , (scherrer & bertschinger (1991), ando & komatsu (2006)): p 1h ij (k) = ∫ dm dn dm f̂∗i (k|m) f̂j(k|m) (4) p 2h ij (k) = [∫ dm1 dn dm1 bi(m1)f̂∗i (k|m1) ] × [∫ dm2 dn dm2 bj(m2)f̂j(k|m2) ] p lin(k) ,(5) where dn/dm is the number density distribution of sources, p lin is the linear matter ps, and bi(m) is the linear bias between the object i and matter. note that the average of 〈g〉 is given by: ḡ(z) = 〈g(~n, z)〉 = ∫ dm dn dm ∫ d3~x g(~x|m, z) , (6) which implies that at small k (where f̂ ∼∫ d3~x g(~x|m)/ḡ) the terms in the square-brackets in eq. (5) are ∼ 1 (except in the case of a significant bias). 35 marco regis the 2-halo term is thus normalized to the standard linear matter ps at small k, which motivates the normalization of the window function introduced above. we aim at cross-correlating the shear signal (source i in eqs. (2–5)) with γ-rays emitted by dm, sfgs, and blazars (source j in eqs. (2–5)). 3 results the above formalism can be applied to all the mentioned components, by considering the specific g, w , and dn/dm of each case. for the sake of clearness we will focus on a benchmark model for each component. they are described in camera et al. (2012). in particular, we note that, although we take dm to provide a significant contribution of the egb at e ≥ 1 gev in fig. 1a, it is basically impossible to obtain an evidence for dm from the angular ps of γ-rays alone because the latter is dominated by the blazar contribution. the contributions to the egb and to the γ-ray autocorrelation aps of each components are shown in fig. 1. in fig. 2 we show the ingredients of eq. (2) for the computation of the shear/γ-ray cross-correlation angular ps: the window functions and 3d power spectra. the window function for the cosmic shear signal nicely overlaps with the dm window function, both for annihilating and decaying dm, while this happens only at intermediate redshifts for the sfg window function and only at high redshifts for the case of blazars. this suggests that a tomographic approach could be a powerful strategy to further disentangle different contributions in the angular ps (this will be explored in a forthcoming work, camera et al. (in preparation)). the shear signal is stronger for larger dm masses. the same is true also for the γ-ray signal from dm and this fact gives a large 1-halo contribution which dominates in the range k = 1−10h/mpc in fig. 2b. those wavenumbers correspond to ` ' 100 − 1000. galaxies have masses ≤ 1014m�, thus they correlate with the shear signal of lower-mass halos and the 1-halo contribution becomes important at smaller scale k � 1h/mpc. thus, an important result is that, since both the shear and dm-induced γ-ray signals are stronger for larger halos, their cross-correlation is more effective with respect to the case of astrophysical sources at intermediate wavenumbers. this, together with the sizable overlapping of the dm γ-ray and shear window functions at low redshift, leads to the expectation of a sizable dm signal in the angular ps, which is indeed what we find in fig. 3. the observational forecasts for the cross-correlation between dark energy survey (des), abbott et al. (2005), or euclid, laureijs et al. (2011), and fermilat are shown for the benchmark models considered in this work (for error estimates, we take observational performances from atwood et al. (2009), laureijs et al. (2011), and abbott et al. (2005). fig. 3 shows that a dm signal can be disentangled in the angular ps at ` ≤ 103. the same conclusion can be derived for dm models with different mass and annihilation/decay channels, provided the dm is a significant component of the total γ-ray egb (at least in one energy bin) as in our assumptions. figure 3: left: cross-correlation between cosmic shear and γ-ray emission, for the different classes of γray emitters described in the text (with a γ-ray threshold expected for fermi-lat after 5 years of exposure). each contribution is normalized by multiplying eq. (2) by 〈ij〉/〈iegb〉 to make them additive. des is taken as the reference galaxy survey. error bars are estimated for the total signal (in black). right: same as in the left panel but for annihilating dm, with euclid as the reference galaxy survey. this figure is taken from camera et al. (2012). 4 conclusions in this talk, we discussed the cross-correlation angular power spectrum of weak lensing cosmic shear and γrays produced by wimp annihilations/decays and astrophysical sources. we showed that this method can provide novel information on the composition of the egb. since the shear signal is stronger for structures of larger masses and most of the γ-ray emission from decaying and annihilating dm is also produced in large mass halos, their cross-correlation is typically stronger than the case of astrophysical sources (which are associated to galactic-mass halos) for ` ' 100 − 1000. the combination of fermi-lat with forthcoming surveys like des and euclid can thus potentially provide evidence for wimps. acknowledgement we would like to thank the organizers for the invitation to the workshop and the participants for interesting discussions. we acknowledge infn grant fa51. 36 a novel approach in the wimp quest: cross-correlation of gamma-ray anisotropies and cosmic shear references [1] t. abbott et al. [des collab.], astro-ph/0510346. [2] a. abdo et al. [fermi-lat collab.], phys. rev. lett. 104 (2010) 101101. doi:10.1103/physrevlett.104.101101 [3] a. abdo et al. [fermi-lat collab.], jcap 1004 (2010) 014. [4] m. ackermann et al. [fermi lat collab.], phys. rev. d 85 (2012) 083007. doi:10.1103/physrevd.85.083007 [5] s.’i. ando, e. komatsu, phys. rev. d73 (2006) 023521. [6] w. atwood et al. [lat collab.], ap. j. 697 (2009) 1071. doi:10.1088/0004-637x/697/2/1071 [7] s. camera, m. fornasa, n. fornengo and m. regis, astrophys. j. 771 (2013) l5 [arxiv:1212.5018 [astro-ph.co]]. [8] s. camera, m. fornasa, n. fornengo and m. regis, in preparation. [9] j. harding and k abazajian, jcap 1211 (2012) 026. [10] r. laureijs et al., arxiv:1110.3193; l. amendola et al. [euclid theory working group collab.], arxiv:1206.1225; http://www.euclid-ec.org. [11] r. scherrer and e. bertschinger, ap. j. 381, 349 (1991). [12] p. ullio et al. phys. rev. d 66 (2002) 123502. doi:10.1103/physrevd.66.123502 discussion sergio colafrancesco: what are the effects of dm-density profiles and of the cross-correlation of dm halos with gamma-ray emitting galaxies on the results you have shown? marco regis: dm density profiles in the inner part are model dependent; however this affects the cross-correlation angular power spectrum only at multipoles ` > 103−104, so above the range of our interest. since the bulk of anisotropies from dm comes from very large halos, the galactic mass halos are not crucial in the estimate of the total dm signal. jim beall: how much of an improvement in the error bars do you need to better delimit the model? marco regis: this changes with the overall normalization of the wimp cross-correlation signal which depends on the (unknown) interaction rate. however, the bottom-line is that, provided the dm is one of the most relevant components of the egb in at least a energy band, current and next future experiments, like fermi-lat and des, would suffice. 37 http://dx.doi.org/10.1103/physrevlett.104.101101 http://dx.doi.org/10.1103/physrevd.85.083007 http://dx.doi.org/10.1088/0004-637x/697/2/1071 http://dx.doi.org/10.1103/physrevd.66.123502 introduction theoretical modeling results conclusions 103 acta polytechnica ctu proceedings 2(1): 103–106, 2015 103 doi: 10.14311/app.2015.02.0103 why a new code for novae evolution and mass transfer in binaries? g. shaviv1, i. idan1, n. j. shaviv2 1department of physics, israel institute of technology, haifa, israel 2racah institute of physics, the hebrew university, jerusalem, israel corresponding author: gioras@physics.technion.ac.il abstract one of the most interesting problems in cataclysmic variables is the long time scale evolution. this problem appears in long time evolution, which is also very important in the search for the progenitor of sn ia. the classical approach to overcome this problem in the simulation of novae evolution is to assume: (1) a constant in time, rate of mass transfer. (2) the mass transfer rate that does not vary throughout the life time of the nova, even when many eruptions are considered. here we show that these assumptions are valid only for a single thermonuclear flash and such a calculation cannot be the basis for extrapolation of the behavior over many flashes. in particular, such calculation cannot be used to predict under what conditions an accreting wd may reach the chandrasekhar mass and collapse. we report on a new code to attack this problem. the basic idea is to create two parallel processes, one calculating the mass losing star and the other the accreting white dwarf. the two processes communicate continuously with each other and follow the time depended mass loss. keywords: nova modeling thermonuclear runaways. 1 introduction the classical prediction or identification of a sn ia progenitor as a wd in a compact binary system is usually based on the calculation of a single thermonuclear flash or at most few and how much mass the wd gains or loses in such a flash. extrapolations of the behavior of binary systems based on single or few thermonuclear flashes are not expected to be reliable. prialnik and kovetz (1995) were the first to simulate numerically a rather long series of thermonuclear runaway, up to a 1000. these authors solved in this way the question of the initial conditions assuming that after so many flashes, the wd converges to periodic behavior. idan et all (2013) carried a similar calculation for a high accretion rate and the results were not similar, nor were they strictly periodic. in both calculations the rate of accretion was constant in time and many flashes were calculated. however, the behavior of the mass losing star and its response to mass loss are not uniform in time so that the assumption of constant mass loss (and accretion at a constant rate on the wd) is not justified. for a star of radius r undergoing mass loss dr dt = ( ∂r ∂t ) ev + ∂r ∂m ṁ. (1) the index ev means change of r due to normal secular stelar evolution. one usually assumes that ( ∂r ∂t ) ev � ∂r ∂m ṁ. (2) but then r − rroche 6= constant and clearly, the expression for mass loss due to roche lobe overflow yields a non constant rate of mass loss, as this expression depends on r(t). note that if we assume that dr/dt = 0, namely an equilibrium or a steady state and we neglect the time variability of rroche, then ṁ = − ( ∂r ∂t ) ev / ∂r ∂m � 1, (3) in units of solar radius per solar mass. hence this expression does not yield observable values and does not imply that ṁ(t) = const. hence, this assumption is unacceptable. webbink (1977) evaluated the mass derivative of the roche radius and obtained:( ∂ lnrroche ∂ lnm ) m̄,j = f(q) (4) where q = ln(m+0.005m∗)−0.5 lnp − ln(p +1016) has to do with the mass shell division of the calculation. webbink also assumed that a = ( d lnr d lnm ) t ≈ d lnr d lnm � d lnrroche d lnm (5) 103 http://dx.doi.org/10.14311/app.2015.02.0103 g. shaviv, i. idan, n. j. shaviv where a is the adiabatic constant and the inequality holds for all ṁ. 2 mass loss rate there are several empirical expressions for the mass loss. webbink (1977) for example, assumed that ṁ = −λ ( r−rroche r )2 with λ = const (6) provided r − rroche > 0, while ritter (1988) wrote that ṁ = ṁ0 exp (r−rroche) hp for r−rroche > 0. (7) here m0 is a constant to be evaluated from the geometry of the roche lobe while hp is the pressure scale height near the l3 point. it is clear that if these expressions are valid, then a change caused by a change in the radius of the star affects the accretion rate (and the nova long time evolution). 3 time scale involved the reaction of the donor star depends on three time scales. (a) the kelvin-helmholtz-ritter time scale given by: τkhr = gm2 donor rldonor ( ∆m mdonor ) , (8) where ∆m is the mass affected by the mass loss perturbation. (b) the accretion time scale τacc = ∆mflash ṁ (9) where ∆mflash is the accreted mass at which the thermonuclear runaway takes place (of the order of 10−5m�) and (c) the dynamic time scale is given by: τdyn = √ 3 4πgρ̄ . (10) here ρ̄ is the mean density of the star. only mflash, the mass at which the nuclear flash occurs, depends (slightly) on the mass of the wd. the dynamic time depends on the entire star and τkhr depends on the outermost mass-shell involved. the interplay between these three time scales controls the phenomenon and it varies with the rate of mass loss. consequently, we calculated the hydrodynamic and thermodynamic evolution of the star under the condition that the accretion rate is given (by the parameters of the binary system). as the present calculation is carried out irrespective of the mass of the accretor, we cannot evaluate the accretion rate but have to impose it as given. 4 the dynamic behavior of the donor our goal is to investigate the dynamic response of the donor star to mass loss. we assume spherical symmetry and solve the full hydrodynamic equations of the donor and evaluated the requested derivatives. in figure 1 we see how dr/dm behaves in the case of low accretion rate (10−10m�/yr). the donor is a main sequence star of 1.25m�. 0 2000 4000 6000 time(years) 2x105 4x105 6x105 8x105 106 0 – 2 – where index ev means change of radius due to stellar evolution and @r/@m means change of radius due to change in the total mass due to mass loss from the surface. this equation does not expose the full processes taking place in the star and assumes that @r/@m) does not depends on ṁ. moreover. the derivative @r/@m) is usually calculated assuming the star is in thermal equilibrium and in strict hydrostatic equilibrium, namely the effect of ṁ on the process is ignored. if we do neglect these effect then we may ask what happens when dr/dt were to vanish. in this case we could write that ṁ = � � @r @t � ev @r @m . (2) this however, yields extremely small ṁ and implies that the assumption of ’steady state’, namely dr/dt = 0, is untenable. the thermal relaxation of the donor star in response to the mass loss of mass �m is given by ⌧khr = gm2 d rld ✓ �m md ◆ (3) where ld is the luminosity of the donor and md its mass. the accretion time scale is given by ⌧acc = mflash ṁ (4) where mflash is the accreted mass which leads to a thermonuclear runaway and ṁ is the accretion rate generated by the donor envelope. we assume that of the mass lost by the donor a fraction 1 � ⌘ is lost and does not reach the accreting star. we first ask when the thermal time scale of the donor is of the same order and the accretion time, namely gm2 rld �m md = ⌘�mmwd ṁ (5) or: ṁ mwd = rld gm2 d (6) and hence the critical accretion rate is: (7) 2. references 10�6m�/yr 10�7m�/yr 10�9m�/yr 10�10m�/yr @r @m ⇣ r� m� ⌘ – 2 – where index ev means change of radius due to stellar evolution and @r/@m means change of radius due to change in the total mass due to mass loss from the surface. this equation does not expose the full processes taking place in the star and assumes that @r/@m) does not depends on ṁ. moreover. the derivative @r/@m) is usually calculated assuming the star is in thermal equilibrium and in strict hydrostatic equilibrium, namely the effect of ṁ on the process is ignored. if we do neglect these effect then we may ask what happens when dr/dt were to vanish. in this case we could write that ṁ = � � @r @t � ev @r @m . (2) this however, yields extremely small ṁ and implies that the assumption of ’steady state’, namely dr/dt = 0, is untenable. the thermal relaxation of the donor star in response to the mass loss of mass �m is given by ⌧khr = gm2 d rld ✓ �m md ◆ (3) where ld is the luminosity of the donor and md its mass. the accretion time scale is given by ⌧acc = mflash ṁ (4) where mflash is the accreted mass which leads to a thermonuclear runaway and ṁ is the accretion rate generated by the donor envelope. we assume that of the mass lost by the donor a fraction 1 � ⌘ is lost and does not reach the accreting star. we first ask when the thermal time scale of the donor is of the same order and the accretion time, namely gm2 rld �m md = ⌘�mmwd ṁ (5) or: ṁ mwd = rld gm2 d (6) and hence the critical accretion rate is: (7) 2. references 10�6m�/yr 10�7m�/yr 10�9m�/yr 10�10m�/yr @r @m ⇣ r� m� ⌘ figure 1: the derivative dr dm in units of m�/τkhr for an imposed mass loss of 10−10m�/yr. in this case τflash ≈ 105yr. we realize that neither dr/dt nor (∂r/∂m)ṁ are constant and one should not expect the accretion rate to be constant (in time) either. even during the period of mass building for a single flash, the accretion rate is not constant. – 2 – where index ev means change of radius due to stellar evolution and @r/@m means change of radius due to change in the total mass due to mass loss from the surface. this equation does not expose the full processes taking place in the star and assumes that @r/@m) does not depends on ṁ. moreover. the derivative @r/@m) is usually calculated assuming the star is in thermal equilibrium and in strict hydrostatic equilibrium, namely the effect of ṁ on the process is ignored. if we do neglect these effect then we may ask what happens when dr/dt were to vanish. in this case we could write that ṁ = � � @r @t � ev @r @m . (2) this however, yields extremely small ṁ and implies that the assumption of ’steady state’, namely dr/dt = 0, is untenable. the thermal relaxation of the donor star in response to the mass loss of mass �m is given by ⌧khr = gm2 d rld ✓ �m md ◆ (3) where ld is the luminosity of the donor and md its mass. the accretion time scale is given by ⌧acc = mflash ṁ (4) where mflash is the accreted mass which leads to a thermonuclear runaway and ṁ is the accretion rate generated by the donor envelope. we assume that of the mass lost by the donor a fraction 1 � ⌘ is lost and does not reach the accreting star. we first ask when the thermal time scale of the donor is of the same order and the accretion time, namely gm2 rld �m md = ⌘�mmwd ṁ (5) or: ṁ mwd = rld gm2 d (6) and hence the critical accretion rate is: (7) 2. references 10�6m�/yr 10�7m�/yr 10�9m�/yr 10�10m�/yr @r @m ⇣ r� m� ⌘ – 2 – where index ev means change of radius due to stellar evolution and @r/@m means change of radius due to change in the total mass due to mass loss from the surface. this equation does not expose the full processes taking place in the star and assumes that @r/@m) does not depends on ṁ. moreover. the derivative @r/@m) is usually calculated assuming the star is in thermal equilibrium and in strict hydrostatic equilibrium, namely the effect of ṁ on the process is ignored. if we do neglect these effect then we may ask what happens when dr/dt were to vanish. in this case we could write that ṁ = � � @r @t � ev @r @m . (2) this however, yields extremely small ṁ and implies that the assumption of ’steady state’, namely dr/dt = 0, is untenable. the thermal relaxation of the donor star in response to the mass loss of mass �m is given by ⌧khr = gm2 d rld ✓ �m md ◆ (3) where ld is the luminosity of the donor and md its mass. the accretion time scale is given by ⌧acc = mflash ṁ (4) where mflash is the accreted mass which leads to a thermonuclear runaway and ṁ is the accretion rate generated by the donor envelope. we assume that of the mass lost by the donor a fraction 1 � ⌘ is lost and does not reach the accreting star. we first ask when the thermal time scale of the donor is of the same order and the accretion time, namely gm2 rld �m md = ⌘�mmwd ṁ (5) or: ṁ mwd = rld gm2 d (6) and hence the critical accretion rate is: (7) 2. references 10�6m�/yr 10�7m�/yr 10�9m�/yr 10�10m�/yr @r @m ⇣ r� m� ⌘ 0 0.5 1 1.5 2 2.5 3 1013 1012 1011 1010 109 108 time(years) figure 2: the derivative dr/dm in units of m�/τkhr for an imposed mass loss of 10−6m�/yr. in this case τflash ≈ 10yr. the results for all accretion rates are collected and summarized in figure 3. we see that in all cases, irrespective of the accretion rate, the time dependence of the derivative is given by: dr dm = 14.07 t2.35 + ε(ṁ) for all ṁ, (11) where ε(ṁ) is a constant in time which depends on ṁ. 104 why a new code for novae evolution and mass transfer in binaries? 10-6 10-5 10-4 10-3 10-2 10-1 100 101 102 103 1014 1013 1012 1011 1010 109 108 107 106 105 104 103 102 – 2 – where index ev means change of radius due to stellar evolution and @r/@m means change of radius due to change in the total mass due to mass loss from the surface. this equation does not expose the full processes taking place in the star and assumes that @r/@m) does not depends on ṁ. moreover. the derivative @r/@m) is usually calculated assuming the star is in thermal equilibrium and in strict hydrostatic equilibrium, namely the effect of ṁ on the process is ignored. if we do neglect these effect then we may ask what happens when dr/dt were to vanish. in this case we could write that ṁ = � � @r @t � ev @r @m . (2) this however, yields extremely small ṁ and implies that the assumption of ’steady state’, namely dr/dt = 0, is untenable. the thermal relaxation of the donor star in response to the mass loss of mass �m is given by ⌧khr = gm2 d rld ✓ �m md ◆ (3) where ld is the luminosity of the donor and md its mass. the accretion time scale is given by ⌧acc = mflash ṁ (4) where mflash is the accreted mass which leads to a thermonuclear runaway and ṁ is the accretion rate generated by the donor envelope. we assume that of the mass lost by the donor a fraction 1 � ⌘ is lost and does not reach the accreting star. we first ask when the thermal time scale of the donor is of the same order and the accretion time, namely gm2 rld �m md = ⌘�mmwd ṁ (5) or: ṁ mwd = rld gm2 d (6) and hence the critical accretion rate is: (7) 2. references 10�6m�/yr 10�7m�/yr 10�9m�/yr 10�10m�/yr @r @m ⇣ r� m� ⌘ – 2 – where index ev means change of radius due to stellar evolution and @r/@m means change of radius due to change in the total mass due to mass loss from the surface. this equation does not expose the full processes taking place in the star and assumes that @r/@m) does not depends on ṁ. moreover. the derivative @r/@m) is usually calculated assuming the star is in thermal equilibrium and in strict hydrostatic equilibrium, namely the effect of ṁ on the process is ignored. if we do neglect these effect then we may ask what happens when dr/dt were to vanish. in this case we could write that ṁ = � � @r @t � ev @r @m . (2) this however, yields extremely small ṁ and implies that the assumption of ’steady state’, namely dr/dt = 0, is untenable. the thermal relaxation of the donor star in response to the mass loss of mass �m is given by ⌧khr = gm2 d rld ✓ �m md ◆ (3) where ld is the luminosity of the donor and md its mass. the accretion time scale is given by ⌧acc = mflash ṁ (4) where mflash is the accreted mass which leads to a thermonuclear runaway and ṁ is the accretion rate generated by the donor envelope. we assume that of the mass lost by the donor a fraction 1 � ⌘ is lost and does not reach the accreting star. we first ask when the thermal time scale of the donor is of the same order and the accretion time, namely gm2 rld �m md = ⌘�mmwd ṁ (5) or: ṁ mwd = rld gm2 d (6) and hence the critical accretion rate is: (7) 2. references 10�6m�/yr 10�7m�/yr 10�9m�/yr 10�10m�/yr @r @m ⇣ r� m� ⌘ – 2 – where index ev means change of radius due to stellar evolution and @r/@m means change of radius due to change in the total mass due to mass loss from the surface. this equation does not expose the full processes taking place in the star and assumes that @r/@m) does not depends on ṁ. moreover. the derivative @r/@m) is usually calculated assuming the star is in thermal equilibrium and in strict hydrostatic equilibrium, namely the effect of ṁ on the process is ignored. if we do neglect these effect then we may ask what happens when dr/dt were to vanish. in this case we could write that ṁ = � � @r @t � ev @r @m . (2) this however, yields extremely small ṁ and implies that the assumption of ’steady state’, namely dr/dt = 0, is untenable. the thermal relaxation of the donor star in response to the mass loss of mass �m is given by ⌧khr = gm2 d rld ✓ �m md ◆ (3) where ld is the luminosity of the donor and md its mass. the accretion time scale is given by ⌧acc = mflash ṁ (4) where mflash is the accreted mass which leads to a thermonuclear runaway and ṁ is the accretion rate generated by the donor envelope. we assume that of the mass lost by the donor a fraction 1 � ⌘ is lost and does not reach the accreting star. we first ask when the thermal time scale of the donor is of the same order and the accretion time, namely gm2 rld �m md = ⌘�mmwd ṁ (5) or: ṁ mwd = rld gm2 d (6) and hence the critical accretion rate is: (7) 2. references 10�6m�/yr 10�7m�/yr 10�9m�/yr 10�10m�/yr @r @m ⇣ r� m� ⌘ – 2 – where index ev means change of radius due to stellar evolution and @r/@m means change of radius due to change in the total mass due to mass loss from the surface. this equation does not expose the full processes taking place in the star and assumes that @r/@m) does not depends on ṁ. moreover. the derivative @r/@m) is usually calculated assuming the star is in thermal equilibrium and in strict hydrostatic equilibrium, namely the effect of ṁ on the process is ignored. if we do neglect these effect then we may ask what happens when dr/dt were to vanish. in this case we could write that ṁ = � � @r @t � ev @r @m . (2) this however, yields extremely small ṁ and implies that the assumption of ’steady state’, namely dr/dt = 0, is untenable. the thermal relaxation of the donor star in response to the mass loss of mass �m is given by ⌧khr = gm2 d rld ✓ �m md ◆ (3) where ld is the luminosity of the donor and md its mass. the accretion time scale is given by ⌧acc = mflash ṁ (4) where mflash is the accreted mass which leads to a thermonuclear runaway and ṁ is the accretion rate generated by the donor envelope. we assume that of the mass lost by the donor a fraction 1 � ⌘ is lost and does not reach the accreting star. we first ask when the thermal time scale of the donor is of the same order and the accretion time, namely gm2 rld �m md = ⌘�mmwd ṁ (5) or: ṁ mwd = rld gm2 d (6) and hence the critical accretion rate is: (7) 2. references 10�6m�/yr 10�7m�/yr 10�9m�/yr 10�10m�/yr @r @m ⇣ r� m� ⌘ – 2 – where index ev means change of radius due to stellar evolution and @r/@m means change of radius due to change in the total mass due to mass loss from the surface. this equation does not expose the full processes taking place in the star and assumes that @r/@m) does not depends on ṁ. moreover. the derivative @r/@m) is usually calculated assuming the star is in thermal equilibrium and in strict hydrostatic equilibrium, namely the effect of ṁ on the process is ignored. if we do neglect these effect then we may ask what happens when dr/dt were to vanish. in this case we could write that ṁ = � � @r @t � ev @r @m . (2) this however, yields extremely small ṁ and implies that the assumption of ’steady state’, namely dr/dt = 0, is untenable. the thermal relaxation of the donor star in response to the mass loss of mass �m is given by ⌧khr = gm2 d rld ✓ �m md ◆ (3) where ld is the luminosity of the donor and md its mass. the accretion time scale is given by ⌧acc = mflash ṁ (4) where mflash is the accreted mass which leads to a thermonuclear runaway and ṁ is the accretion rate generated by the donor envelope. we assume that of the mass lost by the donor a fraction 1 � ⌘ is lost and does not reach the accreting star. we first ask when the thermal time scale of the donor is of the same order and the accretion time, namely gm2 rld �m md = ⌘�mmwd ṁ (5) or: ṁ mwd = rld gm2 d (6) and hence the critical accretion rate is: (7) 2. references 10�6m�/yr 10�7m�/yr 10�9m�/yr 10�10m�/yr @r @m ⇣ r� m� ⌘ time (years) m*=1.25msun figure 3: the derivative dr/dm in units of m�/τkhr for all accretion rates calculated here (for a ms star of mass 1m�). moreover, time dependence of the derivatives tend for sufficiently long times, to an asymptote. we find that: for t� ε(ṁ) dr dm → 14.07 t2.35 , (12) namely, all results (for a given mass of the donor) converge for long times to an asymptote. we do not know at the moment how this asymptote changes with the mass of the donor. at the same time we can write for the roche lobe radius (eggelton, 1984) that: rroche ≈ 0.49q2/3 0.6q2/3 + ln(1 + q1/3) where q = mwd + ṁt md − ṁt (13) assuming conservative mass loss. hence for sufficiently small t (at the beginning) we have that: ∣∣∣∣ drroche dm ∣∣∣∣� ∣∣∣∣ drdonor dm ∣∣∣∣ (14) the thermodynamic state is shown in figure 4 time(years) – 2 – where index ev means change of radius due to stellar evolution and @r/@m means change of radius due to change in the total mass due to mass loss from the surface. this equation does not expose the full processes taking place in the star and assumes that @r/@m) does not depends on ṁ. moreover. the derivative @r/@m) is usually calculated assuming the star is in thermal equilibrium and in strict hydrostatic equilibrium, namely the effect of ṁ on the process is ignored. if we do neglect these effect then we may ask what happens when dr/dt were to vanish. in this case we could write that ṁ = � � @r @t � ev @r @m . (2) this however, yields extremely small ṁ and implies that the assumption of ’steady state’, namely dr/dt = 0, is untenable. the thermal relaxation of the donor star in response to the mass loss of mass �m is given by ⌧khr = gm2 d rld ✓ �m md ◆ (3) where ld is the luminosity of the donor and md its mass. the accretion time scale is given by ⌧acc = mflash ṁ (4) where mflash is the accreted mass which leads to a thermonuclear runaway and ṁ is the accretion rate generated by the donor envelope. we assume that of the mass lost by the donor a fraction 1 � ⌘ is lost and does not reach the accreting star. we first ask when the thermal time scale of the donor is of the same order and the accretion time, namely gm2 rld �m md = ⌘�mmwd ṁ (5) or: ṁ mwd = rld gm2 d (6) and hence the critical accretion rate is: (7) 2. references 10�6m�/yr 10�7m�/yr 10�9m�/yr 10�10m�/yr @r @m ⇣ r� m� ⌘ – 2 – where index ev means change of radius due to stellar evolution and @r/@m means change of radius due to change in the total mass due to mass loss from the surface. this equation does not expose the full processes taking place in the star and assumes that @r/@m) does not depends on ṁ. moreover. the derivative @r/@m) is usually calculated assuming the star is in thermal equilibrium and in strict hydrostatic equilibrium, namely the effect of ṁ on the process is ignored. if we do neglect these effect then we may ask what happens when dr/dt were to vanish. in this case we could write that ṁ = � � @r @t � ev @r @m . (2) this however, yields extremely small ṁ and implies that the assumption of ’steady state’, namely dr/dt = 0, is untenable. the thermal relaxation of the donor star in response to the mass loss of mass �m is given by ⌧khr = gm2 d rld ✓ �m md ◆ (3) where ld is the luminosity of the donor and md its mass. the accretion time scale is given by ⌧acc = mflash ṁ (4) where mflash is the accreted mass which leads to a thermonuclear runaway and ṁ is the accretion rate generated by the donor envelope. we assume that of the mass lost by the donor a fraction 1 � ⌘ is lost and does not reach the accreting star. we first ask when the thermal time scale of the donor is of the same order and the accretion time, namely gm2 rld �m md = ⌘�mmwd ṁ (5) or: ṁ mwd = rld gm2 d (6) and hence the critical accretion rate is: (7) 2. references 10�6m�/yr 10�7m�/yr 10�9m�/yr 10�10m�/yr @r @m ⇣ r� m� ⌘ – 2 – where index ev means change of radius due to stellar evolution and @r/@m means change of radius due to change in the total mass due to mass loss from the surface. this equation does not expose the full processes taking place in the star and assumes that @r/@m) does not depends on ṁ. moreover. the derivative @r/@m) is usually calculated assuming the star is in thermal equilibrium and in strict hydrostatic equilibrium, namely the effect of ṁ on the process is ignored. if we do neglect these effect then we may ask what happens when dr/dt were to vanish. in this case we could write that ṁ = � � @r @t � ev @r @m . (2) this however, yields extremely small ṁ and implies that the assumption of ’steady state’, namely dr/dt = 0, is untenable. the thermal relaxation of the donor star in response to the mass loss of mass �m is given by ⌧khr = gm2 d rld ✓ �m md ◆ (3) where ld is the luminosity of the donor and md its mass. the accretion time scale is given by ⌧acc = mflash ṁ (4) where mflash is the accreted mass which leads to a thermonuclear runaway and ṁ is the accretion rate generated by the donor envelope. we assume that of the mass lost by the donor a fraction 1 � ⌘ is lost and does not reach the accreting star. we first ask when the thermal time scale of the donor is of the same order and the accretion time, namely gm2 rld �m md = ⌘�mmwd ṁ (5) or: ṁ mwd = rld gm2 d (6) and hence the critical accretion rate is: (7) 2. references 10�6m�/yr 10�7m�/yr 10�9m�/yr 10�10m�/yr @r @m ⇣ r� m� ⌘ – 2 – where index ev means change of radius due to stellar evolution and @r/@m means change of radius due to change in the total mass due to mass loss from the surface. this equation does not expose the full processes taking place in the star and assumes that @r/@m) does not depends on ṁ. moreover. the derivative @r/@m) is usually calculated assuming the star is in thermal equilibrium and in strict hydrostatic equilibrium, namely the effect of ṁ on the process is ignored. if we do neglect these effect then we may ask what happens when dr/dt were to vanish. in this case we could write that ṁ = � � @r @t � ev @r @m . (2) this however, yields extremely small ṁ and implies that the assumption of ’steady state’, namely dr/dt = 0, is untenable. the thermal relaxation of the donor star in response to the mass loss of mass �m is given by ⌧khr = gm2 d rld ✓ �m md ◆ (3) where ld is the luminosity of the donor and md its mass. the accretion time scale is given by ⌧acc = mflash ṁ (4) where mflash is the accreted mass which leads to a thermonuclear runaway and ṁ is the accretion rate generated by the donor envelope. we assume that of the mass lost by the donor a fraction 1 � ⌘ is lost and does not reach the accreting star. we first ask when the thermal time scale of the donor is of the same order and the accretion time, namely gm2 rld �m md = ⌘�mmwd ṁ (5) or: ṁ mwd = rld gm2 d (6) and hence the critical accretion rate is: (7) 2. references 10�6m�/yr 10�7m�/yr 10�9m�/yr 10�10m�/yr @r @m ⇣ r� m� ⌘ – 3 – 10�11m�/yr (lph�lnuc) lnuc @r @m ⇣ r� m� ⌘ – 2 – where index ev means change of radius due to stellar evolution and @r/@m means change of radius due to change in the total mass due to mass loss from the surface. this equation does not expose the full processes taking place in the star and assumes that @r/@m) does not depends on ṁ. moreover. the derivative @r/@m) is usually calculated assuming the star is in thermal equilibrium and in strict hydrostatic equilibrium, namely the effect of ṁ on the process is ignored. if we do neglect these effect then we may ask what happens when dr/dt were to vanish. in this case we could write that ṁ = � � @r @t � ev @r @m . (2) this however, yields extremely small ṁ and implies that the assumption of ’steady state’, namely dr/dt = 0, is untenable. the thermal relaxation of the donor star in response to the mass loss of mass �m is given by ⌧khr = gm2 d rld ✓ �m md ◆ (3) where ld is the luminosity of the donor and md its mass. the accretion time scale is given by ⌧acc = mflash ṁ (4) where mflash is the accreted mass which leads to a thermonuclear runaway and ṁ is the accretion rate generated by the donor envelope. we assume that of the mass lost by the donor a fraction 1 � ⌘ is lost and does not reach the accreting star. we first ask when the thermal time scale of the donor is of the same order and the accretion time, namely gm2 rld �m md = ⌘�mmwd ṁ (5) or: ṁ mwd = rld gm2 d (6) and hence the critical accretion rate is: (7) 2. references 10�6m�/yr 10�7m�/yr 10�8m�/yr 10�9m�/yr 10�10m�/yr 102 101 100 10-1 10-2 10-3 10-4 10-7 10-6 10-5 10-4 10-3 10-2 10-1 100 101 102 103 – 3 – 10�11m�/yr (lph�lnuc) lnuc @r @m ⇣ r� m� ⌘ figure 4: the time to reach thermodynamic equilibrium. we see that stars with mass loss rate smaller than 10−9m� tend to thermal equilibrium. the timescales to reach the thermal equilibrium vary. accretion rates higher than 10−9m� diverge, namely they become unstable and runaway. the rate of accretion drives the star out of thermal equilibrium to be never restored. this fact should be taken into account in evaluating the mass loss rate from the donor. 5 conclusions first conclusion: it is not justified to assume that τkhr is negligible. second, polytropic estimates are nice and simple, but wrong (motl et al.2002) the mass loss is not constant in time. the mass loss does not start suddenly and reaches the assumed value gradually. there is no fixed period between eruptions. the system can have n eruptions with an almost constant time interval and then pause and let the donor recover on a kelvin-helmholtz-ritter time scale of its envelope. during this time the wd may relax to a new state. the accretion rate changes in time and affects the evolution of the nova. a nova calculation must include the evolution of the donor and the accretion rate. an important element in the evolution of nova is the time variability of the accretion rate. 0 2x1013 4x1013 6x1013 8x1013 1x1014 -0.0014 -0.0012 -0.001 -0.0008 -0.0006 -0.0004 -0.0002 0 time (seconds) m as s l os t f ro m d on or (s ol ar m as se s) figure 5: the time depended mass loss from the donor. 6 discussion and conclusions a significant part of present day interest in nova includes the cases that may become progenitors of sn ia. in this case the behavior of the binary system is followed through a single or few thermonuclear runaways and then the result is extrapolated over 6-7 orders of magnitudes. the mass accreted or lost is of the order of 10−7m�. the initial mass of the wd is of the order of 1m� and if a conservative mass transfer is assumed this means a huge extrapolation in the behavior of the accretor and the the donor. we conclude that the evolution of the two stars must be followed simultaneously. we developed a code which 105 g. shaviv, i. idan, n. j. shaviv does just that. two processors are created, each devoted to a star. thus the donor star is calculated on one cpu and the accretor on a second cpu. the two processes, which may run on different computers or on a computer with more than one cpu, communicate with one another via an open gate. the communication can take place at fixed time intervals or whenever the conditions on one star deviate significantly and an update is due. 0 2x1013 4x1013 6x1013 8x1013 1x1014 0 5x107 1x108 1.5x108 2x108 2.5x108 time (seconds) ln uc / ls un ln uc /l su n figure 6: the flashes of nuclear energy as a function of time. the code is in the debugging phase but the results seem to justify the claims present here. we find that the accretion rate is not constant in time and it stops when the radius of the donor shrinks below the roche lobe radius. in figure 5 we show one such example. the periods of no accretion appear as horizontal section (no change in mass lost). the period of mass loss appear as decreasing lines. note that these parts of the curve are straight lines at the beginning but not later. hence the rate of mass loss changes even during accretion. the recovery time depends on the mass loss rate and the τkhr of the donor. the resulting nuclear flushes are shown in figure 6. we see that the picture of flashes at a constant rate is correct only of a couple of flashes and the flashes come in groups. the time between the groups, the relaxation time of the donor increases gradually. acknowledgement this research has been supported by the israel science foundation, grant 1589/10. shaviv giora is delighted to thank dr. ilan shaviv in setting the code. references [1] eggleton,p.p.1983,apj.,268,368. doi:10.1086/160960 [2] idan, i., shaviv, n.j. & shaviv, g. , 2013, mnras, 433, 2884 doi:10.1093/mnras/stt908 [3] kolb, u. & ritter, h. 1990. a&a, 236, 385. [4] motl, p.m., tohline, j.e. & frank, j., 2002, apjs, 138,121. doi:10.1086/324159 [5] prialnik, d. & kovetz, a., 1995, apj, 445, 789. [6] ritter, h. 1988, a&a, 202,93. [7] webbink, r. f. , 1977, apj, 211, 881. 106 http://dx.doi.org/10.1086/160960 http://dx.doi.org/10.1093/mnras/stt908 http://dx.doi.org/10.1086/324159 introduction mass loss rate time scale involved the dynamic behavior of the donor conclusions discussion and conclusions 27 acta polytechnica ctu proceedings 1(1): 27–33, 2014 27 doi: 10.14311/app.2014.01.0027 astrophysics without black holes, and without extragalactic gamma-ray bursts wolfgang kundt1 1argelander-institut für astronomie der universität bonn, auf dem hügel 71, d-53121 bonn corresponding author: wkundt@astro.uni-bonn.de abstract contrary to common belief, it is argued that our universe contains neither black holes, nor extracalactic gamma-ray bursts. keywords: black holes, gamma-ray bursts galactic center burning disks magnetars. 1 introduction modern cosmology makes confident statements about processes which have happened throughout the universe, all the way back to its beginnings, even though no convincing cosmological initial data have ever been reliably proposed [hoyle et al 2000]. such confidence is somehow based on the undoubted successes of einstein’s general theory of relativity in our immediate cosmic surroundings – the inner solar system – with or without a λ-term which has been termed ”dark energy” (by mike turner) when it has the sign opposite to that of energy, whose necessity is still debated. in these years, almost generally accepted as cosmic building blocks are (i) supermassive black holes (smbhs) in the centers of (almost all?) galaxies, without any physical justification, (ii) sources of almost all the gammaray bursts (grbs) at cosmic distances, viz. of the bursts with line redshifts z & 1, and (iii) non-baryonic dark matter, even though we cannot even reliably measure the amount of ionised hydrogen between us and the (neighbouring) andromeda galaxy [braun 2013].. in this presentation, i will restrict myself to the first two listed source classes, and start with the smbhs. not only have all the well-observed galactic central engines (ces) defied a plausible bh interpretation, by their (large) luminosities, (high) temperatures, (strong) outflows, (relativistic) twin-jets, nonpointlike central potential, and halo-scale high-energy (.102gev) plumes, but even their theoretical existence is no longer justified because rigorous calculations have (recently) shown that the expectations of the 1970s have been hasty, that roger penrose’s hypothesis of ‘cosmic censorship’ has been premature. we now know that complete gravitational collapse leads to naked singularities – not to bhs – except for a highest-symmetry subset of initial data, of measure zero. on top of not having been verified throughout more than 35 years, therefore, bhs are now no longer expected by theorists [joshi 2009, quevedo 2011, joshi & malafarina 2013]. in particular, our galactic center (sgr a*) deviates from containing a smbh for at least 15 reasons [kundt 2012], the 15th being the happy survival, so far, of cloudlet g2 during its ongoing approach of sgr a*. the second goal of this presentation is to refine my earlier considerations – dating back to the 1980s, when galactic grbs used to be common wisdom – that all detected grbs come from local-galactic neutron stars, rather than from ill-understood supersources at cosmic distances. not only have there five quantitative distance estimates been published in the past which must not be forgotten, based on well-measured properties, which place their sources nearer than a few kpc from us, but meanwhile, a number of bursters have even been directly identified, and their tentative distances lowered, with the convergent result that we deal with the spectacular class of nearby magnetars in our galaxy [kundt 2008, 2010-2013, ghisellini 2010, archibald et al 2013, rea et al 2013, ho 2013]. the grbs are a local-galactic phenomenon, is my iterated message. 2 bh physics reconsidered black holes have been baptised in princeton, in 1971, by john wheeler and remo ruffini. their name stuck immediately, because years of hard international research had been invested, mainly in the united states and in europe, until the complete family o f spinning bh spacetimes was finally published by roy kerr in 1963, and until the holes’ hairlessness had been (essentially) proven, during the decade to follow, with brandon carter among the cheerleaders. mass, spin, and 27 http://dx.doi.org/10.14311/app.2014.01.0027 wolfgang kundt electric charge are a bh’s (three) only free parameters [heusler 1996]. but how to detect bhs in the universe? could we ever hope to identify a bh in the sky? wouldn’t they hide forever, on grounds of their expected dimness, their not being able to radiate? to my knowledge, this question was first asked seriously in 1972, during international meetings between theorists and observers, with a distinct emphasis on candidates of stellar mass. a first, promising suggestion was the x-ray emitting stellar binary system cyg x-1 – the brightest stellar x-ray source in the cygnus region – whose optically invisible component had to be more massive than a neutron star: bingo! slowly, please: cannot the dark component be a neutron star surrounded by a self-gravitating disk [kundt 1979]? aren’t self-gravitating disks stable? disks are thought to form stars, their planets, and probably likewise all their moons; from what other instabilities could a disk suffer? probably none. and how to blow the jets seen to spring forth from the dark component of the cyg x-1-system? binary neutron stars are observed to blow jets, whereas bhs cannot do that because they lack an inclined, co-rotating magnetosphere, for generating the jets’ pair plasma [kundt 2011]. in 1989, daniel fischer and i could not find a single bh in the whole class of (stellar-mass) bhcandidates [kundt & fischer 1989]. in order to still detect a bh in the sky, should we perhaps search the hole in a higher weight class, as a supermassive bh, at the center of some galaxy, perhaps even our own? but how should it form there in the first place, or how else should it get to a galaxy’s center? are not self-gravitating disks stabilised radially by centrifugal forces, and vertically by pressure forces, if necessary via nuclear burning, like stars? i received “honorable mention” for this idea in 1978, by grg, and described its structure more in detail at bad honnef in 1995 [kundt 1996], in vital contact with peter scheuer, (see his contribution to that same book). from suzy collinsouffrin i had learned that mass spiral-in rates through galactic disks – determined indirectly by the central disk’s luminosity – tend to balance mass-ejection rates through the broad line region (blr), determined by its emission-line intensities, whereby the ejection energy is supplied by nuclear burning, like in stellar explosions. instead of like a bh, the stable galactic disk would act like a burning disk, a ”bd”. mass would spiral in through the disk, at a rate of .m�/yr for a galaxy like ours, and would subsequently be ejected explosively through its blr, nlr, elr out to the eer beyond the galaxy’s halo, in the form of a galactic-scale fountain [kundt 1987, 1990, 1996, 2005], cf. fig. 1, and [kormendy 2011]. the case of our milky-way galaxy was my topic last year at vulcano [kundt 2012]; it will not be repeated here. no bh is needed for this fountain to function; on the contrary, a bh near the center would have prevented its formation, via irreversible accretion. it would have swallowed the incoming nuclear fuel, and thereby grown in mass. instead, the sdss plot of galacticcenter masses has shown a (statistical) monotonic decrease of ce masses from some initial 109.3m� down to the present-day rather low values, of order 10−3 that much, in the redshift range from z = 4.5 down to (the present) z = 0. galactic ces have monotonicly lost mass during cosmic evolution, defying a bh interpretation, see fig. 2. figure 1: most impressive evidence against a bh at our galactic center: the fermi bubbles (or plumes), at photon energies .102gev, probably emitted by buoyantly rising relativistic pair plasma from the near vicinity of sgr a*, throughout the milky-way halo, to heights well above 20 kpc, taken from [su et al 2010, 2011]. these same halo structures had already been detected and mapped decades earlier by [sofue 2000], from radio and x-ray data. at this point, my reasoning departs drastically from that of most of my colleagues, who use words like ”downsizing” and ”co-evolution” to describe the average monotonic shrinkage of ce masses plotted in fig. 2. they speak of a high bh ‘efficiency’, without indicating how a bh should do that, because as already stated in the introduction, galactic centers are often observed to be quite luminous, stormy, jet-blowing, and pluming (at .102gev), from their center all the way out into their halo. how is this central activity powered? my answer reads: by nuclear burning of the central disk, combined with magnetic reconnections in its (very) fast and differentially rotating corona [kundt 1996]. a bd avails of abundant rotational, infall, and nuclear energy, for both non-thermal and thermal ejections: of radiation, jets, winds, and plumes. a smbh would suppress all this. instead, a few of my decades-long friends call a smbh the ‘only thinkable’ central engine (ce) of galactic centers without telling the reader how such a smbh could have formed and grown, how it could e.g. emit the observed hard spectra [aharonian et al 2004], and 28 astrophysics without black holes, and without extragalactic gamma-ray bursts how it could perform the multiple hard ejections [su et al 2010]. i think in particular of max camenzind, of harald lesch, and of andreas müller. they have published books, or contributed to books in which they claim, already on the book’s cover, that mankind would not have formed without bhs [müller 2010]. these publications have appeared fairly recently so that i have not gotten a chance to sort myself out with their authors, in friendly, animated discussions. how did my friends reach their present opinions? have they found flaws in my 1996 model? why did they never tell me? figure 2: the sdss plot of the ce masses m(z) of all the (&104) sampled galaxies by the sloan digital sky survey. as functions of cosmicredshift z (≥ 0.2), [vestergaard et al, 2008]. small squares denote (vertical) averages at fixed redshift bin. the plot shows that m(z) decreases monotonicly, from 109.3m� at z = 4.5 down to .108m� at the smallest plotted redshift, z = 0.2. the scientific situation is, in fact, more inconsistent than described so far. exact analytical calculations have meanwhile shown that mass concentrations collapsing under their own weight will no longer form bhs, rather naked singularities, except for configurations of highest symmetry which are, however, of measure zero among all initial data [joshi 2009, quevedo 2011, joshi & malafarina 2013]. penrose’s hypothesis of “cosmic censorship” ought to be strengthened into the hypothesis of an “avoidance of unhalted gravitational collapse”, auc, unless we do not mind contenting ourselves with a piecewise singular theory, or unless we are ready to search for a replacement of gr by some new, nonsingular spacetime theory. my own preference is for auc, as i have never failed to find hurdles to any proposed unhalted gravitational collapse. 3 gamma-ray bursts from galactic magnetars now to item (ii) of this pamphlet: what are the sources of the grbs? isn’t it clear since some 20 years that those sources ‘must be’ at cosmological distances? to my mind, it has never been: true: the bursts reach us from all directions, three per day on average from outer space, in an almost isotropic fashion, but small anisotropies of well-defined subclasses of bursts have repeatedly been published; the isotropy is not perfect, and a nearby population of sources (.0.3 kpc) can certainly not be excluded, in particular when individual bursters have anisotropic radiation patterns, oriented with respect to their (low-mass) accretion disks whose normals prefer to lie in the galactic plane. (such a preference is expected for disks assembled by neutron stars during their oscillatory motion through the galactic disk). next think of the redshifts z of the bursts’ afterglows, and host galaxies, z lying between 0 and 9, corresponding to lorentz-factors γ between 1 and 5, according to the kinematic law z + 1 = γ(1 + β). such redshifts may well be kinematic redshifts of matter ejected centrifugally from near the speed-of-light cylinder of a sufficiently magnetised, slowly spinning neutron star, hence need not mean a (cosmologically) large distance. note that a few bursts have even had z = 0, including those from the sgrs, so that a distal interpretation of z would deal with a range of distances through a factor of order 108, corresponding to a range of powers through a factor of 1016, for essentially the same type of sources, viz. accreting neutron stars. this reason alone has never encouraged me to take a cosmic interpretation of the grbs seriously: the distant sources would have to radiate almost infinitely times brighter than their cousins in the milky way, even if you try to save a factor of γ2 .106 by postulated beaming (of both the prompt and the afterglow emission!). to me, the redshifts mean velocities, not distances (of the sources). note that there is no problem with missing blueshifts from spherical explosions: only the first flash from a distant, spherical explosion is blueshifted, all later radiation (from a small angular neighbourhood of the explosion site, due to scattering) is received redshifted, mainly from the receding polar cap of the expanding sphere of ejecta. and what about host galaxies, at the same redshift? only a quarter of all bursts have had reliable-looking hosts, whereby no host galaxy has ever been intrinsicly brighter than the lmc! fancy the gigantic intrinsic energy (&1053erg) of a grb interpreted cosmologically, illuminating the csm of its host galaxy: the host would have to flare, rather than be just about detectable. no ‘ordinary’ galaxy (like ours) has ever hosted a grb! .my preferred explanation: what observers call ‘host’ are the flaring ejecta plus dragged-along csm of the (nearby) bursting magnetar, before the hadronic ejecta start losing a significant fraction of their kinetic energy received at launch. we receive cooling radiation from 29 wolfgang kundt thermalised (kinetic) burst energy, around the magnetar, part of which is still moving transrelativistically away from us, with the same redshift as the early ejecta. all bursts come from inside our milky way; the published ‘hosts’ are all fake. now let us look again at the five published distance estimates for grbs, all of which imply source distances of less than a few kpc, depending on the strength s of the recorded burst [kundt 2010]. the first three of them take similar shapes: d / kpc < {1/ √ s−4, γ √ l38, 1/ √ s−11} , (1) in which s stands respectively for the peak incoming energy-flux density of the {prompt at & mev, early optical afterglow} emission in the {first, third} entry, where s−4 := s/10−4erg/cm2s is evaluated in cgs units (as always), and γ stands for the (assumed) bulk lorentz factor of the neutron-star system w.r.t. which the power l is emitted. more in detail, the first estimate in (1) uses photon crowding at the source, which would soften a grb’s spectrum above the pair-formation threshold (of ≈mev) [schmidt 1978, baring 1992] unless it were emitted in a highly beamed way. it rules out a distance of 50 kpc (of lmc) for the sgr 0526-66 – which flared on 5 march 1979 – and it likewise rules out a distance of 8.7 kpc for sgr 1806-20; in the main table of mcgill sgr/axp online catalog. in the meantime, the fermi mission has measured energetic hard tails to many grbs reaching up in energy towards &10 gev, which begin to reach us right after the prompt emission, see [ghisellini 2010], and eleonora troja’s contribution to this workshop. even so, their roof-like spectral peak (near 1 mev), at the top of the band spectrum, did not look grossly distorted in the new spectra. for all of them, therefore, distances larger than one kpc are inconsistent with their (hard) spectra unless their power was emitted in a highly beamed fashion, whose detailed mechanism has never been explained convincingly at conferences, or anywhere in the literature. required would be hadronic jets formed on the timescale of seconds, but lasting long enough (months) in order to allow likewise for beamed afterglows. such postulated jets would have to function very differently from the hundreds of well-studied quasi-stationary pair-plasma jets observed to spring forth from the various well-known jet sources, all powered by heavy rotating magnets [kundt 2011]. the second inequality in (1) holds under the assumption that the source of the grb is a neutron star, whose small surface area restricts its maximal possible luminosity l, via the eddington constraint. it was always satisfied during the 1980s, when scientists trusted the galactic-neutron-star model for the grbs. finally, the third estimate in (1) assumes that the afterglows are emitted incoherently, from the near surroundings of the burst sites which are hit by the explosion. bright afterglows tend to have poynting fluxes .10−10erg/cm2s, for which (1) yields distances d . 0.3 kpc., in accord with the estimated magnetar densities in the milky way. again, this third estimate would not hold for jetlike emission; but how, or why would such be expected? two even much smaller distance estimates d have been derived for the nearest among all grbs, for which we even see their much more frequent but much fainter repetitions, for the soft gamma-ray repeaters (sgrs), of which 13 are presently listed in the mcgill catalog. (only 8 sgrs were listed in [kundt 2010]). so far, none of them has flared more than once at their large, original intensity, but their intense flares were much brighter than all those of the non-repeaters. for this reason, i feel encouraged to use again the second estimate of (1), but this time not with the classical eddington luminosity l = 1038erg/s of a steadily accreting neutron star, but instead with the maximal possible luminosity expected for an isolated, clumpy impact onto a neutron star, of order l = 1042erg/s. another, independent estimate involves the typical galactic peculiar velocity cβ of a magnetar (blowing radio bubbles, with measured angular velocities), of order β .10−3. the two estimates read [kundt 2010]: d / 30pc . { √ l41.9, β−2.9} , (2) in agreement with the nearest expected magnetar distances, and also with our additional knowledge about the sgrs. all these distance estimates are some 108 times smaller than their cosmological counterparts, given by d ≈ z c / h0. so where have we arrived? in the first three paragraphs of this section, we have argued that neither quasi-isotropic arrivals, nor relativistic redshifts (z . 9), nor frequent (seeming) host galaxies needed imply cosmological source distances for plausible source properties. then, in the following five paragraphs, we have repeated earlier inequalities, all of which rule out extragalactic distances for magnetar models. in the future, it will certainly help to get more reliable distance estimates for the small subset of already identified burst sources. but let us look once more at the evidences: to begin with, all the soft repeaters have been directly identified, as grbers, during their first, large bursts, with measured spin rates during their early afterglow oscillations. unfortunately, their distances are highly controversial, with grb 050379 as their worst case, projecting onto n49 in the lmc, though having been some 106-times too bright during outburst for that (large) distance, in30 astrophysics without black holes, and without extragalactic gamma-ray bursts consistent with its band spectrum [schmidt 1978, baring 1992]. next the axps: they share the (long) spin periods of the sgrs, qualifying them as dead pulsars, after 106.4yr of active pulsar spindown [kundt 2008]. their ‘anomaly’ as permanent x-ray emitters can be understood as their being surrounded by low-mass fallback disks, from the collapsed cavity blown into their csm during their past pulsar activity. their (comparatively large) number agrees with that of the dying pulsars, and with their expected small distances from us, inconsistent with certain estimates in the literature. figure 3: schematic drawing of the expected ejection geometry of a grb by a magnetar: an ultramassive clump from the inner edge of its (low-mass) accretion disk hits the surface of the central neutron star, heats up, expands, and gets seized and centrifugally re-ejected by the magnetar’s strong, corotating magnetosphere, near its speed-of-light distance, with lorentz factors γ . 5. as a result, a hard electromagnetic flash is emitted (mostly peaking near 1 mev, but ranging from radio frequencies up through ir, optical, x-ray, and γ-ray frequencies all the way towards and beyond 102gev photon energies), closely followed by a centrifugally ejected transrelativistic hadronic shell. this couple of two more or less radially emitted and/or boosted transrelativistic shells of ejecta impact on the grb’s csm, they both heat up, and give rise to the burst’s prompt and afterglow emissions, as well as to the evolving appearance of a ‘host galaxy’. this model can be shown to be flexible enough to account for all the observed grbs, including their intrinsic differences, and occasional anomalies, such as short and long bursts (due to repeated accretions), pre-cursors and post-cursors (for the same reason), redshifts, early afterglow oscillations (by the output of the spinning central neutron stars), strong flaring of the x-ray afterglows (during collisions with the csm), linear polarisations (for scattered radiation), and so on and so forth. independently of the distance problem, the hard spectra of the grbs – reaching up to and beyond 102gev – tell me that their sources involve neutron stars. these neutron stars must not be isolated, or else they would be radio pulsars. which means that we deal with strongly magnetised neutron stars, though not in excess of 1014g surface strength, a neutron star’s extreme field [kundt 2008]. the bursters’ occasional strong magnetic torques can be achieved via confinement by a surrounding low-mass accretion disk, which explains their name ‘magnetars’. their (invisible) disk was first indicated by glitches of the sgrs 1900+14 and 1806-20, during which their spindown rates increased, i.e. required a stronger torque after the glitch, and has been recently fostered by the anti-glitch of the axp 1e 2259+586 [archibald et al 2013], whose sudden spindown cannot be understood (to my mind) without a strong centrifugal mass ejection [kundt 2010]. and how do the magnetars emit their bright, hard bursts? fig. 3 sketches my understanding of how they are thought to do it. every now and then, at large temporal separations (of &50 yr), a supermassive clump (&1016g) accretes onto a magnetar’s surface, from the inner edge of its surrounding accretion disk, via rayleigh-taylor instabilities. preand post-cursors occur when even several successive such clumps fall down. the freefall potential of a heavy clump, crashing onto a neutron star’s surface, creates transient temperatures near 1012k on impact, so that matter gets ionised, and raised to scale heights kt / mg & 106cm.. this lifted, ionised matter is seized by the n*’s corotating magnetosphere, and centrifugally ejected at speed-of-light lever arms, with lorentz factors γ . 5. this hot re-ejected matter emits a bright photonic flash, closely followed by an intense, transrelativistic hadronic flash. when these two successive outgoing flashes hit the burster’s csm, they cause its afterglow emission, from radio frequencies up to 102gev energies, and eventually also the burst’s seeming ‘host galaxy’. 4 summary old and new arguments have been compiled that bhs are no longer even plausible, and that all grbs are emitted by the galactic magnetars. acknowledgement my warm thanks go to ole marggraf for help with the proceedings, and to thomas tauris for acquainting me with up-to-date literature on magnetars. references [1] aharonian, f., et al (100 authors): astron. astrophys. 425, l13-l17, 2004. [2] archibald, r.f., kaspi. v.m., et al (9 authors): an anti-glitch in a magnetar, nature 497, 591-593, 2013. doi:10.1038/nature12159 31 http://dx.doi.org/10.1038/nature12159 wolfgang kundt [3] baring, m.g.: spectral breaks for theorists, nature 358, 624, 1992. [4] braun, r.: the cosmic web in focus, nature 497, 191-192, 2013. doi:10.1038/497191a [5] ghisellini, g., ghirlanda, g., nava, l., celotti, a.: gev emission from grbs: a radiative fireball?, mnras 403, 926-937, 2010. doi:10.1111/j.1365-2966.2009.16171.x [6] heusler, m.: black hole uniqueness theorems, cambridge lecture notes in physics 6, 1-249,1996. [7] ho, wynn c.g.: more than meets the eye: magnetars in disguise, mnras 429, 113-118, 2013. [8] hoyle, f., burbidge, g., narlikar, j.: a different approach to cosmology, cambridge univ. press, 2000. [9] joshi, p.s.: sci. am., february, 26-33, 2009. [10] joshi, p.s., malafarina, d., instability of bh formation under small pressure perturbations, in: gen. rel. grav. 45, 305-317, 2013. [11] kormendy, j., bender, r. : nature 469, 374-379, 2011. [12] kundt, w.: cygnus x-1 – a neutron star surrounded by a massive disk? astron. astrophys. 80, l7-l10, 1979. [13] kundt, w.: our galaxy a former seyfert?, astrophys. & space sci. 129, 195-201, 1987. [14] kundt, w.: in: jets from stars and galactic nuclei, lecture notes in physics 471, 265-270, 1996. doi:10.1007/bfb0102617 [15] kundt, w.: astrophysics, a new approach, springer, 147-152, 2005. [16] kundt, w.: pulsar physics without magnetars, chin. j. astron. astrophys. vol. 8, supplement, 213-218 (2008). [17] kundt, w.: the local-galactic interpretation of the gamma-ray bursts, in: multifrequency behaviour of high-energy cosmic sources, memsait vol. 81, n.1, 449-459, 2010. [18] kundt, w.: black holes cannot blow jets, in: xivth brazilian school of cosmology and gravitation, mangaratiba 2010, eds. novello & bergliaffa, cambridge sci. pub., pp.109-119, 2011. [19] kundt, w.: our galactic center the nearest burning disk, frascati workshop 2012, overdue. [20] kundt, w.: the inorganic machines of the universe, in: xvth brazilian school of cosmology and gravitation, mangaratiba 2010, eds. novello & bergliaffa, cambridge sci. pub., ≥2013. [21] kundt, w., fischer, d.: is there a black hole among the bhcs?, j. astrophys. astron. 10, 119138, 1989. [22] müller, a., schwarze löcher, die dunklen fallen der raumzeit, spektrum akademischer verlag heidelberg, 1-206, 2010. [23] quevedo, h., multipolar solutions, in: xivth brazilian school of cosmology and gravitation, eds. novello & bergliaffa, cambridge sci. pub., 83.97, 2011. [24] rea, n., pons, j., torres, d., turolla, r.: the fundamental plane for radio magnetars, apj. 748, l12 (6pp.), 2012. [25] schmidt; w.: distance limit for a class of model grb sources, nature 271, 525-527, 1978. [26] sofue, y.: bipolar hpershell galactic center starburst model: further evidence from rosat data and x-ray simulations, apj 540, 224-235, 2000. [27] su, m., slatyer, t.r., finkbeiner, d.p.: giant gamma-ray bubbles from fermi-lat: agn activity or bipolar galactic wind?, apj 724, 10441082, 2010. [28] su, m., slatyer, t.r., finkbeiner, d.p.: fermi bubbles: a 10 kpc shock from the galactic center, aas 43, 2011. [29] vestergaard, m., et al (5 authors): mass functions of the active bhs in distant quasars from the sloan digital sky survey data release 3, apj 674, l1l4, 2008. discussion pieter meintjes: you propose an extended burning disc, instead of a supermassive bh in the center of the mw galaxy. what is the size of that disc in relation to the orbits of the innermost stars that orbit that region? also, what influence will such an extended disc have on the orbits of these stars compared to a bh, for example? wolfgang kundt: thank you, pieter, for asking me these constructive questions. in my approximation, the bd inside sgr a* – the ce of the mw galaxy – has a radius of ≈1014cm, whilst the peri-astron distance of the innermost monitored star, 32 http://dx.doi.org/10.1038/497191a http://dx.doi.org/10.1111/j.1365-2966.2009.16171.x http://dx.doi.org/10.1007/bfb0102617 astrophysics without black holes, and without extragalactic gamma-ray bursts s2, measures &1015cm. as already mentioned in my talk of last year [kundt 2012], the orbit of s2 showed a peri-astron advance of 3 deg after its first revolution, consistent with a maclaurin mass distribution (instead of pointlike potential), and six successive measured positions near peri-astron were offset by .10 marcsec towards ne, which i interpret as a fata morgana in the infrared (caused by the high plasma density in the inner disk). at this same time, the star s2 flared by half a magnitude, plausibly due to friction on the disk. 33 introduction bh physics reconsidered gamma-ray bursts from galactic magnetars summary acta polytechnica ctu proceedings doi:10.14311/app.2017.13.0049 acta polytechnica ctu proceedings 13:49–54, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app plasma treatment impact on physical and chemical properties of polymeric fibers radim hlůžeka,∗, zdeněk prošeka,b, jan trejbala, josef fládra, štěpán potockýc a czech technical university in prague, faculty of civil engineering, thákurova 7, 166 29 prague 6, czech republic b university centre for energy efficient buildings of technical university in prague, třinecká 1024, 273 43 buštěhrad, czech republic c czech academy of science, institute of physics, na slovance 1999/2, 182 21 prague 8, czech republic ∗ corresponding author: radim.hluzek@fsv.cvut.cz abstract. presented work focuses on chemical and physical properties of plasma modified polymeric macro-fibers. polyethylene terephthalate (pet) and polypropylene (pp) fibers having approx. 300 µm in diameter were modified using cold oxygen plasma in order to achieve their surface changes needed for durable bond and adhesion with cement matrixes. a duration of plasma modification differed between 5 to 480 seconds, where an effect of the treatment was examined. fiber surfaces chemical changes were researched via wettability measurement with demineralized water (the measurement was repeated immediately and after 1, 7 and 30 days to find out the changes stability). physical changes were studied by means of weight balance (determination of weight loss) and tensile strength tests. it was found that wettability was enhanced significantly – up to two times, while mechanical properties of treated fibers decreased only slightly. keywords: polymer macro-fibers, plasma treatment, wettability, tensile strength. 1. introduction usage of man-made macro fibers as reinforcement of any composites become a commonality in majority of industry fields, civil engineering including. in the final consequence, a small bulk property improvement has strong impact in civil engineering due to mass production [1]. fiber-reinforced materials exhibit good mechanical properties, e.g. high mechanical resistance (abrasion, impact resistance), ductility, water resistance etc. [2, 3]. the main task of the macro fiber addition is the distribution of shrinkage into several small cracks in the case of materials based on shrinking binders (mainly lime and cement), and to prevent the single crack openings after linear elastic response in the case of loaded samples [1]. in the civil engineering, the macro fiber reinforcement is the most often used for a) production of watertight concretes and concretes exposed to risk of steel reinforcement corrosion (absence of cracks disallows water penetration), and b) for production of large-scale construction exposed to temperature or moisture changes, dynamic loads, point loads (the fiber reinforcement provides a compactness – hence usability – of materials after the crossing the material loading capacity) [4, 5]. the fiber reinforcement can be classified by fibers material, diameter, tensile strength and their modulus of elasticity. as material, polymeric fibers can be used. both polymeric (in particular pet and pp) fibers have high tensile strength equal to about hundred or even thousands mpa. their diameter is equal to tens or hundreds micrometers. other characteristic property is low ratio of diameter to length (and related high specific surface enabling better stress transferring from matrix to fibers) and favorable cost [6, 7]. polymeric fibers reveal low surface wettability (hydrophobicity). on the other hand, fiber reinforcement requires good adhesion between the fiber surface and matrix. to improve the mechanical strength of reinforced materials, adhesion between the fiber surfaces and matrix must be unambiguously ensured [5, 8]. the required adhesion can be modified by fiber surface treatment by chemical and physical methods [7, 9– 13]. currently, the newly introduced plasma treatment becomes popular as a progressive physico-chemical method. the low-pressure plasma treatment represents a universal, efficient and eco-friendly alternative for surface modifications. plasma can be defined as ionized gas (composed of electrons, ions, and neutral species). the mechanism for plasma surface modification relays on surface atoms replacement by oxygen atoms and formation of polar groups. the presence of polar or functional chemical groups enhances the reactivity with the matrix based on cement or lime binder (both contain water) [5]. in the present work, we report on the modification of polyethylene terephthalate (pet) and polypropylene (pp) fibers by oxygen plasma treatment. the influence of the plasma treatment on the contact angle, the weight and the tensile strength of the fibers is studied. 49 http://dx.doi.org/10.14311/app.2017.13.0049 http://ojs.cvut.cz/ojs/index.php/app r. hlůžek, z. prošek, j. trejbal et al. acta polytechnica ctu proceedings figure 1. digital camera photo of pet (left), pp fibers (right). 2. materials 2.1. polymer macro-fibers two different types of fibers were used: pet and pp. both of them were made by spokar manufacturer (czech republic). they were primary made for the production of most types of brushes (tooth, paint etc.) and brooms [14]. the fibers had diameter equal to approx. 300 µm (measured using mechanical micrometer), original length was 1200 mm (subsequently chopped according to need). an industrial water flushable sizing is standardly applied onto fiber surfaces as an integral part of their production. fibers are shown in figure 1. 3. experimental methods 3.1. plasma treatment to improve the wettability and related adhesion between fiber surfaces and surrounded matrix, oxygen treatment in inductively coupled plasma was realized using device tesla vt 214 (13.56 mhz). parameters of the whole process differing only in exposition time from 5 to 480 seconds, the others were constant; total power of rf source 100 w, total gas pressure 20 pa, oxygen flow 50 sccm. 3.2. contact angle measurement according to reference [15], using horizontal direct optical method, contact angles were measured between meniscus of distilled water (adhering on fiber surfaces) and fiber perpendicularly submerged into the water. thus obtained results were averaged from 6 independent measurements. 3.3. weight ratio analysis due to ion bombardments and polymer oxidation and surface structuring (etching) during the plasma treatment, the fibers can be damaged. weight ratio observation carried out before and after treatment enables to assess the fiber weight loss, which is connected to tensile strength capacity loss. in order to quantify the fiber weight loss, fibers were weighed before and immediately after plasma treatment on weighing-machine kern alj 120-4 (d = 0.1 mg). 3.4. tensile strength tests physical and chemical processes mentioned earlier can influence the fibers tensile strength. to determine the extent of fibers mechanical properties damage, tensile strength test was carried out using loading frame web tiv ravestein fp100. the test was displacement controlled at a constant rate equal to 6 mm/min in the case of pet and 3 mm/min in the case of pp fibers, respectively. the results were averaged from 6 independents experiments for each plasma treatment time of both fiber types. 4. results and discussions 4.1. contact angle measurement contact angle measurement revealed 84.7±2.2◦ on untreated pet fibers and 88.3±0.6◦ on untreated pp fibers. the results provided on the treated fibers showed the unexceptionable positive plasma impact of the fibers wettability. all treated fibers independently on plasma exposition time showed significant decrease of contact angle. the angle measured immediately after plasma treatment on both types of fibers was moving between approx. 25–30◦. after 1, 7 and 30 days from the treatment, contact angle increased up to 65–70◦ for pet fibers and for the pp fibers up to 55–70◦. besides, the results showed that it is not effective to do any treatment longer duration than several seconds. another finding is the fact that storage of fibers, even for one day, is very inefficient, and the contact angle increase rapidly towards the reference values. dependence between contact angle, duration of plasma treatment and time of storage in atmospheric conditions is shown in figure 2 and figure 3. based on these finding, it was decided that plasma treatment duration realized within other experiments throughout the study were shortened to 120 seconds only. demonstration of the fibers wettability captured during contact angle measurement is shown in figure 4. 4.2. weight ratio analysis weight ratio observation performed on fibers before and after plasma treatment showed that the weight 50 vol. 13/2017 physical and chemical properties of polymeric macro-fibers figure 2. pet fibers – dependence between contact angle, duration of plasma treatment and time of exposure to atmospheric conditions. figure 3. pp fibers – dependence between contact angle, duration of plasma treatment and time of exposure to atmospheric conditions loss is negligible. fibers treated by 120 seconds exhibited practically no weight loss, just less than 0.25 %. comparing both types of fibers, it can be said that the weight loss is the same until 30 seconds of plasma treatment. after 30 seconds of treatment, there are some small difference between pet and pp fibers. after the longest time of treatment (120 seconds), the maximum averaged weight loss was 0.06 % and 0.21 % for pet and pp fibers, respectively. based on these findings, it can be assumed that mechanical properties of treated fiber were not affected by plasma treatment, which is a positive result. graphic relation between weight loss and duration of plasma treatment is shown in figure 5. 51 r. hlůžek, z. prošek, j. trejbal et al. acta polytechnica ctu proceedings figure 4. contact angles captured during the wettability measurement figure 5. relation between fibers weight loss and duration of plasma treatment obtained before and after plasma treatment. figure 6. dependence between fibers tensile strength and duration of plasma treatment. 52 vol. 13/2017 physical and chemical properties of polymeric macro-fibers 4.3. tensile strength tests tensile strength (more precisely load carrying capacity) of reference and plasma treated fibers was approximately constant for all plasma treatment times (measured on reference, 10, 60 and 120 seconds treated fibers). pet fibers reached on approx. 20 n, while pp fibers on approx. 32 n. as it was already shown by weight loss ratio mentioned earlier, fiber tensile strength test confirmed that the plasma treatment had no significant effect on fiber mechanical performance. the relation between fibers tensile strength and duration of plasma treatment is shown in figure 6. 5. conclusions polypropylene (pp) and polyethylene terephthalate (pet) commercial macro fibers spokar having approx. 300 µm in diameter were surface treated by mean of low-pressure cool oxygen plasma treatment in order to achieve their chemical and physical surface changes. the aim of the executed treatment was to improve fiber surface wettability (from hydrophobic to hydrophilic) and morphology (from smooth to roughened), both standardly required for strong interphase interaction with cement matrix, when fibers used as reinforcement. the plasma modification differed in duration (from 5 to 480 seconds). an effect on physico-chemical changes on fiber surfaces was examined by wettability measurement, wight loss ratio (fibers were weighed before and after plasma treatment) and finally by fiber tensile strength tests, when the main focus of the research was targeted to impact of plasma treatment on fiber mechanical performance. besides, time-stability of chemical changes on modified fibers was researched – wettability between fiber surfaces and distilled water was examined using direct optical set for contact angle measurement immediately, 1, 7 and 30 days after plasma modifications. it was found out that: • the wettability of plasma treated (regardless to duration of treatment time) both pp and pet fibers increased almost three times, if compared to reference samples. • the modified wettaility was very short-term. it was degraded almost to reference values already after one day, when fibers exposed to standard atmospheric conditions. • impact of realized treatment did not have no obvious effect on fiber mechanical performance, as demonstrated by no weight loss and no tensile strength changes for much as treated fibers. acknowledgements this work was financially supported by czech technical university in prague – sgs project sgs16/201/ohk1/3t/11, by the czech science foundation research project 15-12420s and by the ministry of education, youth and sports within national sustainability programme i, project no. lo1605. the work occurred in frame of the lnsm infrastructure (no. lm2015087). references [1] p. k. mallick. materials. in fiber-reinforced composites, materials, manufacturing and design, chap. 2. crc press, 2007. 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[15] j. trejbal, l. kopecký, s. potocký, z. remeš. direct optical method for contact angle measurement on micro fibers. in nanomaterials and nanotechnology in civil engineering 2015 – conference proceedings, pp. 89–90. czech technical university in prague, 2015. 54 http://www.spokar.com/cz/technologie/vyroba-vlaken http://www.spokar.com/cz/technologie/vyroba-vlaken acta polytechnica ctu proceedings 13:50–55, 2017 1 introduction 2 materials 2.1 polymer macro-fibers 3 experimental methods 3.1 plasma treatment 3.2 contact angle measurement 3.3 weight ratio analysis 3.4 tensile strength tests 4 results and discussions 4.1 contact angle measurement 4.2 weight ratio analysis 4.3 tensile strength tests 5 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0043 acta polytechnica ctu proceedings 7:43–47, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app numerical predictions and mechanical testing of braided composite structures utilising digital image correlation emil pitz∗, matei-constantin miron, imre kállai, zoltán major institute of polymer product engineering, johannes kepler universität linz, altenberger straße 69, linz, austria, 4040 ∗ corresponding author: emil.pitz@jku.at abstract. the current paper is describing the implementation of a multiscale numerical model for prediction of stiffness and strength in braided composites. the model is validated by experimental testing of single-layer braided tubes under torsional loading utilising digital image correlation (dic). for the numerical model the entire braided structure is modelled at yarn detail level, taking into account the yarn behaviour as well as individual yarn-to-yarn interactions by using cohesive contact definitions. by means of hashin’s failure criteria and cohesive contact damage, failure of the yarns and failure of the yarn-to-yarn interface is being accounted for. thereby the material failure behaviour can be predicted. for validation of the model, torsion tests of biaxially braided single-layer composite tubes were performed. the strain distribution at the specimen surface was studied using the dic system aramis in 3d mode. keywords: braided composites, finite element analysis, failure prediction, torsion testing, digital image correlation. 1. introduction aim of this research is the implementation and validation of a numerical tool providing reliable predictions of the mechanical properties of braided composite materials. modelling the structure at yarn detail level (meso-level), the undulation of the yarns is taken into account as well as individual yarn-to-yarn interactions, utilising cohesive contact interactions in the finite element software abaqus. by implementation of failure models, the approach can predict occurring failure mechanisms, distinguishing damage at the yarn level (intra-yarn) and yarn-interface level (inter-yarn). material properties required as input parameters are obtained by mean-field homogenization (mfh) from the individual constituents behaviour (matrix and fibres). for validation of the model, single layer braided tubes are tested under torsional loading utilising dic for full-field strain measurement on the surface of the specimen. the global loading response predicted by the numerical model as well as the local strain distribution and occurring instability behaviour is compared to the experimentally obtained results. 2. numerical model generally three structural levels can be distinguished in textile composites: the macro-level, defining the overall 3d geometry of the composite structure, the meso-level, defining the internal structure of the reinforcement, consisting of the impregnated undulating yarns and resin pockets corresponding to the empty space between the yarns, and the micro-level, defining the arrangement of the fibre filaments in the impregnated yarn [1]. a schematic representation of the multiscale problem can be seen in figure 1. to describe this structure in the numerical model, a multiscale modelling approach was utilised, describing the entire structure at yarn-detail level and distinguishing between intra-yarn (fibre-dominated) and inter-yarn (matrix-dominated) behaviour [3, 4]. 2.1. 3d-model of the braided composite in order to achieve the mentioned degree of accuracy, a 3d-model of the braiding geometry was developed, modelling both the yarn undulation path and the yarn cross section. the path of each undulating yarn was analytically approximated by a tapered cosine function: r (x) = r0 − t 2 sin (π 2 cos (x− δ) ) . (1) the phase shift δ is changing periodically for each yarn path, depending on the modelled weave pattern (plan or twill), leading to interwoven and repeating undulation paths (see figure 2). the yarn cross section shape is linked to the shape of the yarn path. in this approach, it is taken from projection of the undulation path onto a plane orthogonal to the braiding direction. for simulation, mid-plane shell bodies are extracted from the solid geometry and the local thickness is mapped on the shell mesh. 43 http://dx.doi.org/10.14311/app.2017.7.0043 http://ojs.cvut.cz/ojs/index.php/app e. pitz, m. miron, i. kállai, z. major acta polytechnica ctu proceedings figure 1. structural levels of a textile composite. (adapted from [2]) figure 2. undulation paths of the braided yarns modelled with a tapered cosine function following an arbitrary spline. it should be noted that, due to the analytical modelling of the yarn undulation paths and cross sections, the numerical model assumes perfect in phase arrangement of the yarns. hence there is total absence of any nesting or imperfections in the alignment of the yarns in the model. 2.2. material model to take into account the meso-structure of the composite in the presented modelling approach it is distinguished between yarn behaviour (intra-yarn behaviour) and yarn-to-yarn interactions (inter-yarn behaviour). the yarns (intra-yarn behaviour) are modelled utilising a transversely isotropic elastic material, taking into account the change of orientation along the yarn due to the yarn undulation. the material properties are determined from the constituents behaviour (matrix and fibres) using the mfh approach by mori and tanaka [5]. furthermore, for modelling failure of the yarns (intra-yarn failure) hashin’s composite failure criteria [6] are implemented. the determined yarn stiffness and strength properties can be found in table 1. inter-yarn behaviour (yarn-to-yarn interactions) is being modelled using cohesive contact behaviour to prevent the yarns from separating during loading. by implementing a quadratic traction damage initiation e‖ (gpa) 183 xt (mpa) 1810 e⊥ (gpa) 20 xc (mpa) 669 ν‖⊥ (-) 0.21 y t (mpa) 64 ν⊥⊥ (-) 0.46 y c (mpa) 174 g‖⊥ (gpa) 8.1 sl (mpa) 105 g⊥⊥ (gpa) 6.9 st (mpa) 105 α (-) 1 table 1. yarn stiffness and strength properties. criterion and energy based damage evolution, failure of the yarn-to-yarn interface is being accounted for. the used cohesive properties are specified in table 2. normal stiffness (gpa) 20 tangential stiffness (gpa) 6.9 damage initiation (mpa) 3 damage evolution (mj/mm2) 3 · 10−3 table 2. cohesive contact surface properties. 3. experimental torsion tests were performed on thin walled single layer carbon fibre braided tubes using an instron 8850 (250 kn / 2400nm) testing machine. the specimens had a total length of 300mm, an inner diameter of 70mm and a wall thickness of 0.4mm. for gripping, glass fibre tabs with a thickness of 5mm were glued to the specimens giving them an active length of 150mm. fibre volume ratio (fvr) of the specimens was determined by burnt residue analysis to be approximately 53%. an overview of the specimen geometry can be seen in table 3. the torsion tests were conducted in rotation controlled mode with axial displacement restricted. full-field strain measurement was conducted using the dic system aramis 6.3 in 3d mode. to provide the necessary contrast for the aramis measurement a speckle pattern was sprayed onto the specimens. during testing initial failure was caused by torsional buckling of the structure (see figure 3) followed by failure of the matrix. upon further loading, buckling 44 vol. 7/2017 braid fvr (%) 53 yarn thickness (mm) 0.2 yarn width (mm) 4 yarn count (yarns/cm) 2.15 layer thickness (mm) 0.4 braiding angle (◦) 45 table 3. yarn and braiding geometry of the test specimens. of the structure developed but failure of the yarns was not observed. a more detailed overview of the experimental results will be given in the following section. figure 3. torsion test of a tubular specimen with applied speckle pattern for full-field strain measurement and visible torsional buckling of the specimen. 4. results and comparison the presented numerical model accurately predicts stiffness and strength of the braided tubular structure under torsional loading (a comparison is given in table 4) and correlates well with the experimentally obtained data (see figure 4). experiment simulation torsional stiffness (nm/◦) 137 140 maximum torque (nm) 48 48 table 4. comparison of experimental results and predicted values. 4.1. instability behaviour in the numerical model, damage is initiated, during loading, at the yarn-to-yarn interface (inter-yarn level), leading to torsional buckling of the structure upon 0 0.1 0.2 0.3 0.4 0.50 10 20 30 40 50 60 rotation (◦) to rq ue (n m ) specimen 1 specimen 2 specimen 3 simulation figure 4. comparison of the simulated and tested torque-rotation response. further loading (see figure 5(a)). failure at the intrayarn level does not develop in the simulated rotation range. similar instability and failure behaviour was observed during the experimental torsion tests (see figure 5(b)). comparing the displacement magnitude of the simulated structure and determined by dic (figure 5), the computed displacement generally follows the qualitative trend of the measured values while the maximum displacement of the buckles varies. variations of the maximum displacement magnitude were also observed between the tested specimens though. as buckling under torsional load is generally prone to imperfections, this leads to the assumption that the differences originate mainly from imperfections in the specimens that were not taken into account in the numerical model. (a) (b) figure 5. buckling of the simulated structure (a) and of the tested specimen with an overlay of the dic results (b), at a rotation angle of 0.65◦. 45 e. pitz, m. miron, i. kállai, z. major acta polytechnica ctu proceedings 4.2. strain distribution as the strains obtained by digital image correlation are measured on the surface of the specimen while the simulated strains are received at the yarn level, with the orientation following the undulation paths of the yarns, numerically and experimentally determined strains cannot be directly compared. therefore a thin, low stiffness, and isotropic membrane layer was tied to the yarn surfaces at the outside of the tubular specimen in the numerical model. this does not influence the overall behaviour of the model but the strain distribution of the membrane layer now correlates to the surface strains of the specimen and hence it enables comparison with the digital image correlation results. the strain in circumferential direction (εx) on the surface of the sample examined for the numerical model and the dic measurements (see figure 6), shows a pattern of periodically repeating tensile and compressive strains as a consequence of the periodically crossing yarns. the measured strain generally follows the trend of the numerically predicted strain, with the simulation showing a more repetitive distribution. x y (a) x y (b) figure 6. strain distribution in the simulated structure (a) and experimentally obtained strain distribution (b) at a rotation angle of 0.25◦, with εx being the strain in circumferential direction of the cylinder. to further compare the distribution, the measured and simulated strain profiles were traced along a circumferential line on the surface of the specimen, as can be seen in figure 7. the period length of the computed strain oscillations is approximately 13.7mm, which corresponds to the circumferential distance between two recurring yarn crossings. compared to the calculated strain profile, amplitude and period length of the measured strain profile show variations along the path. it is again assumed that these variations arise from irregular spacing of the yarn crossings in the specimen, which causes variations of the local specimen wall thickness and the local stiffness. such irregularities are not taken into account in the numerical model and hence cause the more repetitive strain profile of the numerical model. 0 5 10 15 20 25 30 −1 −0.5 0 0.5 1 ·10−3 circumferential distance between two recurrent yarn crossings. x y line length (mm) ε x () digital image correlation simulation figure 7. comparison of the circumferential strain distribution (εx) along a circumferential path (y-axis being parallel to the braiding direction). 5. conclusions the proposed modelling approach accurately reproduces the macroscopic response to loading and exhibits similar instability behaviour compared to experimental torsion tests and accurately predicts overall stiffness and strength of the component. further validation of the model was accomplished by utilising dic, enabling full-field strain measurement on the surface of tubular braided samples. comparing the numerically and experimentally obtained local displacement and strain profiles, generally similar trends can be observed. arising differences are assumed to be caused by imperfections in the tested samples that were not regarded in the numerical model. this states the necessity to further develop the numerical model to realistically represent imperfections in the structure and predict their influence on the performance of the component. list of symbols fv r fibre volume ratio [%] e‖ longitudinal elasticity modulus [gpa] e⊥ transversal elasticity modulus [gpa] g‖⊥ longitudinal shear modulus [gpa] g⊥⊥ transversal shear modulus [gpa] ν‖⊥ longitudinal poisson’s ratio [–] ν⊥⊥ transversal poisson’s ratio [–] xt longitudinal tensile strength [mpa] xc longitudinal compressive strength [mpa] y t transversal tensile strength [mpa] y c transversal compressive strength [mpa] sl longitudinal shear strength [mpa] st transversal shear strength [mpa] 46 vol. 7/2017 α contribution of shear stress to fibre failure [–] r current radius of the braiding layer [mm] r0 mean radius of the braiding layer [mm] t braiding layer thickness [mm] δ phase shift [mm] εx circumferential strain [–] acknowledgements the current research is performed within the project number 5320343 / 849425 (andisia) supported by the austrian research promotion agency, in cooperation with teufelberger gmbh austria and the university of applied sciences upper austria. references [1] s. v. lomov, d. s. ivanov, i. verpoest, et al. full-field strain measurements for validation of meso-fe analysis of textile composites. composites part a: applied science and manufacturing 39(8):1218 – 1231, 2008. full-field measurements in composites testing and analysis, doi:http://dx.doi.org/10.1016/j.compositesa.2007.09.011. [2] s. neudorfer. modelling and simulation of braided and filament-wound composite torsion-shaft, 2015. master’s thesis, johannes kepler universität. [3] m.-c. miron, h. katzinger, s. neudorfer, et al. mechanical testing and numerical predictions of the behavior of braided carbon fiber components. procedia structural integrity 2:3593 – 3600, 2016. 21st european conference on fracture, ecf21, 20-24 june 2016, catania, italy, doi:http://dx.doi.org/10.1016/j.prostr.2016.06.448. [4] e. pitz, m.-c. miron, z. major. failure analyis of braided composite structures in torsional loading. submitted for publication. [5] t. mori, k. tanaka. average stress in matrix and average elastic energy of materials with misfitting inclusions. acta metallurgica 21(5):571 – 574, 1973. doi:http://dx.doi.org/10.1016/0001-6160(73)90064-3. [6] z. hashin. failure criteria for unidirectional fiber composites. journal of applied mechanics 47(2):329– 334, 1980. doi:http://dx.doi.org/10.1115/1.3153664. 47 http://dx.doi.org/http://dx.doi.org/10.1016/j.compositesa.2007.09.011 http://dx.doi.org/http://dx.doi.org/10.1016/j.prostr.2016.06.448 http://dx.doi.org/http://dx.doi.org/10.1016/0001-6160(73)90064-3 http://dx.doi.org/http://dx.doi.org/10.1115/1.3153664 acta polytechnica ctu proceedings 7:43–47, 2017 1 introduction 2 numerical model 2.1 3d-model of the braided composite 2.2 material model 3 experimental 4 results and comparison 4.1 instability behaviour 4.2 strain distribution 5 conclusions list of symbols acknowledgements references acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0068 acta polytechnica ctu proceedings 4:68–72, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app measurement of neutron spatial distribution of the bnct epithermal beam at the reactor lvr-15 michaela rabochováa,∗, miroslav vinšb, jaroslav šoltésb, božena michalcovác a faculty of electrical engineering, czech technical university in prague, czech republic b department of neutron physics, research centre řež, husinec-řež, czech republic c department of neutronography processing, nuclear physics institute of the cas, husinec-řež, czech republic ∗ corresponding author: michaela.rabochova@seznam.cz abstract. in this study, a measurements of neutron field using a special positioning device with a 6li + si detector and image plate is described. the measurements were provided for boron neutron capture therapy (bnct) channel of the lvr-15 reactor in the research centre rez ltd., czech republic. mapping of neutron field represents an essential and crucial part of planning bnct treatment (especially for patients suffering from brain tumor glioblastoma multiforme). keywords: bnct, map of neutron field, 6li + si detector, positioning device. 1. introduction glioblastoma multiforme [1–4] is the most common malignant radio-resistant and chemoresistant tumor of the central nervous system which has been incurable for decades and even today, unfortunately, the prognosis is not favorable [5]. this type of tumor is characterized by very fast growth and aggressive invasion to the surrounding normal brain tissue. it is very difficult to remove all of the affected tumor cells without serious damage of the brain. despite the advanced diagnostics (especially in neuroimaging), and various multimodal therapies that include surgical resection followed by radiation therapy (and alternatively chemotherapy) still remains a considerable problem with finding efficient and gentle treatment of the sensitive area of brain tissue. in this regard, boron neutron capture therapy (bnct) is unique selective radiotherapy based on capture of non-radioactive nuclide 10b by cancer cells and the subsequent capture of thermal neutrons resulting in the nuclear reaction 10b(n, α)7li. these products of reaction selectively damage cancer cells while healthy tissue is spared of radiation load. an absolutely essential part of the treatment planning is determination of parameters and proper setting of correct compensation of neutron beam. the purpose of this project was to measure the spatial distribution of neutrons inside the epithermal horizontal channel of the research reactor lvr-15 (the research centre rez ltd., czech republic) [6], which is used for the method of boron neutron capture therapy. 2. research background 2.1. the special positioning device the mapping of neutron beam was done by using a special positioning device which fixed a si semiconductor detector with 6li converter. the positioning device can moves the detector in three axis and it basically consists of a specially modified support frame with three engines. the special positioning device is shown in fig. 1. figure 1. the special positioning device. 2.2. 6li + si detector for the spatial mapping of neutron beam was used a detector which was consisted of 6li converter and si semiconductor detector [7]. the 6li converter provided a production of 3h (after its insertion into neutron flux) via 6li(n, α)3h reaction. the total energy of the reaction is 4.78 mev (2.73 mev for 3h and 2.05 mev for α particle). the tritium 3h is then detected in a si detector. the active diameter of 6li 68 http://dx.doi.org/10.14311/ap.2016.4.0068 http://ojs.cvut.cz/ojs/index.php/app vol. 4/2016 measurement of neutron spatial distribution of the bnct beam converter is 3 mm; the case of si detector has diameter 25 mm. the distance between converter and detector is approximately 8 mm [8]. the scheme of the detector is shown in fig. 2. figure 2. the scheme of 6li + si detector [8]. 2.3. the image plate another method that has been performed is the experimental determination of the intensity distribution excitations caused by neutron beam by means of the image plates (fig. 3). displaying the neutron flux through the imaging plate is mainly used for neutron radiography method. the principle is based on passing the neutron beam through an object and its subsequent detection on the imagine plate. the result is a 2d (or 3d) image of the different intensities of the neutron flux which is determined by the absorption properties of the object material. in the case of the experiment mentioned in this work was used this method by the same way, but not for displaying a particular subject, but purely for displaying the parameters of the neutron beam intensities. figure 3. the image plate. 3. method of measurement 3.1. the mesaurement with the positioning device the measurement was carried out from march 31 to april 1, 2016 in front of the horizontal channel bnct of the research nuclear reactor lvr-15 in the research centre rez ltd. the acquisition of the data was based on communication between genie-2000 program (detector) and special positioning device utility program. the getting device to work was accomplished by sequential modifications of batch codes. the codes control position of the positioning device and also provide a record of the data of measurements. the main aim of this measurement was to determine the spatial distribution of neutron beam, which is important to verify its homogeneity for subsequent applications of bnct. the map of the route of detector was created and loaded into the control position program of positioning device. the movement of positioning device with 6li + si detector was determined with fixed increments of 1 cm along the horizontal axis y and along the vertical axis z. the time of measurement was ∼ 4 minutes for every position of detector. the scheme of route of the detector is shown in fig. 4. figure 4. the scheme of the route of 6li + si detector. the entire measurement lasted 9 and 1 2 hours (240 second for one position) and data from detector were analyzed with the software genie-2000 by canberra company [9]. the resulting peak areas of 3h have to be corrected for the change in reactor power as the power was not stable during whole measurement. the power of reactor was higher at the beginning of measurement. for the time of the correction was used the data from ionization chambers which monitoring the bnct channel (see fig. 5). figure 5. the development of reactor power. 69 m. rabochová, m. vinš, j. šoltés, b. michalcová acta polytechnica ctu proceedings the resulting peak areas after correction were calculated based on the following relationship spk = m xi sp, where spk denotes the peak area after correction, m is a median of the numbers of pulses during irradiation, xi is an arithmetic average of the numbers of pulses during the i-th interval of irradiation in a given position and sp is the peak area. 3.2. the measurement with image plate the second experiment of mapping neutron field was performed on april 21, 2016. the main aim was to take a radiography image of thermal neutron beam and its evaluation using neutron imaging plate. the plate was placed under the outlet of the neutron beam. all manipulation were done by hand, the image plate was moved to the beam exit after the beam was opened. this system was provided for pulling the plate upward for start measuring so that the enter of the channel was subsequently overlapped and after the end of irradiation the plate was pull down to the start position. this principle was chosen in order to avoid an unwanted exposure during opening and closing the bnct horizontal channel. start experimental position of image plate is shown in fig. 6. overall exposure time was 2 minutes. figure 6. the neutron image plate (in the red frame) located in the default position below the enter of the bnct horizontal channel (green frame). after the irradiation, the plate was evaluated at the institute of nuclear physics institute of the cas in rez. subsequently, the measured data was processed by the device fujifilm bas-1800 (bas – bioimaging analyzer system), which evaluated the measured intensity. 4. result of measurement 4.1. the mesaurement with the positioning device based on neutron beam radiation of 6li + si detector the map of thermal neutron flux distribution was obtained (fig. 7). values within each field represents the value of the peak area. figure 7. the map of neutron flux distribution. the graphical representation of the measured data is on the fig. 8. the axis x represents the values of the peak areas of 3h and the axes y and z are the positions. the measurement uncertainty was around 1 %. figure 8. 3d graph of neutron flux distribution. 4.2. the measurement with image plate the measured neutrogram of the neutron beam of reactor lvr-15 was then rendered fig. 9. 70 vol. 4/2016 measurement of neutron spatial distribution of the bnct beam figure 9. the neutrongram of neutron beam. the neutron beam is seen here as a red-edge circle. the dark blue color represents the lowest level of excitation (the largest decline), while the white color represents the high intensity. on the neutrongram are partially visible muffled two horizontal bars in the upper and lower half, which are dependent on the properties of a neutron plate and therefore do not reflect the actual intensity values at those locations. unfortunately it is not possible to suppress this phenomenon. small local changes in intensity are the result of small surface scratch of the plate. on the picture is evident symmetrical circular beam (red-purple-white colored intensity) with the lowest attenuation values in the centre, as one might expect. however, the upper half of the image shows a higher level of exposure than the lower half. possible in this case, this could be the influence of gamma radiation to which the neutron plate can be also sensitive. this impact would be affected by the opening bnct channel. another additional measurements intended to clarify these results are planned. it is possible to plot a 3d graph (fig. 10). figure 10. 3d neutrogram of neutron beam. the values on the axes x, y represent the pixel, resp. one unit corresponds to one pixel, which is equivalent to 50 micrometers. thus e.g. 500 px = 2.5 cm, 1000 px = 5 cm, 2000 px = 10 cm etc. the z axis is then plotted excitation intensities in individual pixels. the values are relative and they do not represent actual neutron flux density. the point [x, y] = [0, 0] represents the upper-left corner of the neutron plate placed looking towards the enter of the horizontal channel. again, this graph shows the slope, which is probably caused again by the opening of the channel. 5. conclusions the measurement results show that the profile of the beam is quite homogeneous in its whole crosssection without any significant peaks. in the future, other measurements with other types of converter are planned. also properly functionality of special positioning system which fixed the 6li + si detector was confirmed. the measurement using neutron image plates showed that the neutron beam is symmetrical with the highest intensity in the centre of the beam. it was detected intensity changes in the upper half of the image compared to the lower half of the image. this situation may be caused by the influence of unwanted exposure during opening horizontal channel or by unwanted exposure of gamma radiation at the opening horizontal channel. both methods were sensitive to thermal neutrons (i.e. 6li converter and gd layer of neutron image plate). both experiments confirmed the symmetry of the neutron beam of bnct horizontal channel of lvr-15 reactor. acknowledgements the presented work was financially supported by the ministry of education, youth and sport czech republic project lq1603 (research for susen). references [1] k. urbánek. nádory mozku: gliomy – astrocytom, glioblastoma, příznaky, léčba, diagnostika, 2008. http://www.zbynekmlcoch.cz/informace/medicina/ neurologie-nemoci-vysetreni/nadory-mozkugliomy-astrocytom-glioblastom-priznaky-lecbadiagnostika-prognoza. 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[5] s. s. stylli, a. h. kaye, l. macgregor, et al. photodynamic therapy of high grade glioma – long term survival. j clin neurosci 12(4):389–398, 2005. doi:10.1016/j.jocn.2005.01.006. [6] j. burian. lvr-15 reactor – applications of neutron beam in medicine, biology, dosimetry. iaea technical meeting lecture, vienna, austria, 2011. [7] l. viererbl, j. šoltés, m. vinš, et al. measurement of thermal neutron beam parameters in the lvr-15 research reactor. in transaction of igorr 2013 conference. 2013. http://www.igorr.com/home/ liblocal/docs/igorr2013/07_1001.pdf. [8] l. viererbl, j. burian, s. hladky, et al. si diode with converter used for measurement of epithermal neutron beam of lvr-15 reactor. nuclear instruments and methods in physics research section a: accelerators, spectrometers, detectors and associated equipment 580(1):366–368, 2007. doi:10.1016/j.nima.2007.05.180. [9] canberra industries, inc. genie 2000 basic spectroscopy software, 2016. http://www.canberra. com/products/radiochemistry_lab/pdf/g2kbasicspect-ss-c40220.pdf. 72 http://www.abta.org/resources/spanish-language-publications/glioblastoma-y-astrocitoma-maligno.pdf http://www.abta.org/resources/spanish-language-publications/glioblastoma-y-astrocitoma-maligno.pdf http://www.abta.org/resources/spanish-language-publications/glioblastoma-y-astrocitoma-maligno.pdf http://dx.doi.org/10.1016/j.jocn.2005.01.006 http://www.igorr.com/home/liblocal/docs/igorr2013/07_1001.pdf http://www.igorr.com/home/liblocal/docs/igorr2013/07_1001.pdf http://dx.doi.org/10.1016/j.nima.2007.05.180 http://www.canberra.com/products/radiochemistry_lab/pdf/g2k-basicspect-ss-c40220.pdf http://www.canberra.com/products/radiochemistry_lab/pdf/g2k-basicspect-ss-c40220.pdf http://www.canberra.com/products/radiochemistry_lab/pdf/g2k-basicspect-ss-c40220.pdf acta polytechnica ctu proceedings 4:68–72, 2016 1 introduction 2 research background 2.1 the special positioning device 2.2 6li + si detector 2.3 the image plate 3 method of measurement 3.1 the mesaurement with the positioning device 3.2 the measurement with image plate 4 result of measurement 4.1 the mesaurement with the positioning device 4.2 the measurement with image plate 5 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.10.0034 acta polytechnica ctu proceedings 10:34–37, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app fiber reinforced sand backfill for underground pedestrian crossing andrey b. ponomarev∗, v.i. kleveko, o.v. moiseeva, k.r. kashapova perm national research polytechnic university, kuibysheva street 109, perm, russia ∗ corresponding author: spstf@pstu.ru abstract. crosswalk is an essential element of the transport system of any city. a priority assignment in any such crossing is to ensure the safety of pedestrians. underground pedestrian crossings are much safer than crossings at another level, but they lose in attraction when it comes to cost. the cost of the construction of an underground pedestrian crossing often leads to project abandonment. the cost of construction can be reduced through the use of flexible corrugated metal structures instead of ordinary concrete structures. the stress-strain state of the structural shells need to be known to facilitate their rational design. the stress-strain state of flexible corrugated metal shells largely depends on the strength and deformation characteristics of the surrounding soil. therefore, improving the characteristics of backfill soil is an urgent task in reducing the cost of construction for such tunnels. one way to improve the strength and deformation characteristics of soils is the use of reinforcement. currently, there are a large number of reinforcement schemes and also associated reinforcing materials. one of the most prospective methods of soil reinforcement is the use of fibre filaments. fibre reinforced soils have significantly higher strength and deformation characteristics in comparison with unreinforced soils. numerical modelling of a tunnel shell made out of a corrugated metal structure was undertaken to evaluate the effectiveness of using fibre reinforced sand. ordinary sand and sand reinforced with polypropylene fibres have been used as soil backfill. the calculation results for a pedestrian tunnel structure involving different strength and deformation characteristics of the backfill soil are presented in this article. keywords: fibre reinforced soil, fem, tunnel lining. 1. introduction crosswalk is an integral element of the transportation system of any city. the first and foremost function of a pedestrian crossing is user safety. annually, in russia, a large number of people travelling on foot are killed, which indicates some lack of effectiveness in the transfer and transport system as a whole [1, 2]. the most commonly used and the most projected type is a pedestrian crossing with a light regulation of type “zebra”. this type of transit actually maximises the probability of pedestrian-car contact. underground pedestrian crossings offer a significantly safer transit to light regulation, but lose on the cost criterion. this cost of construction often leads to abandonment of the concept. however, the cost of construction can be reduced through the use of corrugated metal structures instead of the standard concrete shell [3–6]. to reduce the earthworks and consequently the cost of construction, the pedestrian tunnel is laid at the ground-level for traffic vehicles and in this case is carried out using the device of the mound (fig. 1). earlier studies showed that the optimal cross section is a round pipe [6]. the stress-strain state of flexible metal corrugated shells largely depends on the strength and deformation characteristics of the surrounding soil [7, 8]. therefore, the characteristics of the soil backfill gives an actual opportunity to reduce the cost of construction of pedestrian tunnels. one way to improve the strength and deformation characteristics of soils is the use of reinforcement. currently, there are a large number of schemes for reinforcement and their related reinforcing materials. 2. fibre reinforced sandy backfill one of the most promising ways of reinforcement of soils is using fibre. fibre reinforced soils have a significantly higher strength characteristics compared to unreinforced soils [9–12]. fig. 1 shows the structure of the pedestrian crossing at ground level. this design of pedestrian crossing does not need light regulation, and thus saves time for drivers and pedestrians, requires less effort compared to aboveground and underground pedestrian crossings and generally serves to enhance the safety of all road users. 34 http://dx.doi.org/10.14311/app.2017.10.0034 http://ojs.cvut.cz/ojs/index.php/app vol. 10/2017 fiber reinforced sand backfill figure 1. the construction of a pedestrian crossing at ground level figure 2. a round pipe figure 3. specifications of corrugated sheet gl 55 to identify the optimal soil backfill there was calculation by the finite element method, implemented in the software package plaxis 2d. the construction of a pedestrian crossing at ground level was made for specific geological conditions. at the construction site there were identified the following primers: • loam, layer thickness h = 7.2 m, intercept cohesion c = 20.5 kpa, angle of internal friction ϕ = 18°, modulus of deformation e = 11 mpa; • sand, h = 1.0 m, c = 2 kpa, ϕ = 18°, e = 11 mpa; • gravel, h = 1.8 m, c = 1 kpa, ϕ = 40°, e = 30 mpa; • mudstone, h = 2.1 m, e = 20 mpa. fig. 2 shows the geometrical dimensions of a metal corrugated pipe. in the pipe there was used corrugated sheet gl55 (fig. 3), which had the following characteristics: • thickness 4 mm; • the moment of inertia of the cross section i 181.92 cm4/m; figure 4. design scheme • the moment of resistance of section w 61.67 cm3/m; • the plasticity moment of resistance of section wp 79.72 cm3/m. the most common soil backfill for underground structures is sand. therefore, to evaluate the influence of soil characteristics on the stress-strain state of the shirred casing, two calculations were done. the first calculation was derived from a filling with sand with the following characteristics: e = 30 mpa; ϕ = 40°; c = 1 kpa. the second calculation was made for the filling out of fibrocartilagenous sand with the following characteristics: e = 30 mpa; ϕ = 45°; c = 67.0 kpa. the characteristics of sand reinforced with polypropylene fibres to an amount of 0.5 % is taken from test results given in [9–12]. according to the current design standard sp 35.13330.2011 “bridges and pipes”, the cargo load was a four-axle truck n14 with an axle load of 252 (kn), and the distance between the axles 1.2 m. the design scheme is shown in fig. 4. the results of calculating the stress-stain state of the tunnel lining with soil backfill are in figs. 5, 6, 7 and 8. analysis of the graphs showed that in the tunnel lining there occurs compressive strength with a maximum value of nmax = 147.87 kn and a considerable alternating bending moment with a maximum value 35 a. b. ponomarev, v.i. kleveko, o.v. moiseeva, k.r. kashapova acta polytechnica ctu proceedings figure 5. deformed scheme figure 6. the diagram of shell displacements for sand backfill (umax = 29.32 mm) of mmax = 6.5 knm. the maximum displacement of the tunnel lining was observed in the upper zone and amounted to 29.32 mm. the results from calculating the stress-strain state of the tunnel lining and soil backfill from fibroareolar sand is shown in figs. 9, 10 and 11. based on the calculation results the following data was obtained: • max. travel: imax = 20.71 mm; • max axial force nmax = 164.28 kn; • max bending moment mmax = 3.78 knm. the analysis of the above plots shows that using fibre reinforced soil instead of unreinforced soil leads to a decrease of the deformations of the tunnel shell by 8.6 %, a bending moment at 42 % and to an increase in longitudinal force of 9.7 %. based on the obtained calculation results there were calculated the normal stresses in the metal corrugated shell. the calculation results are presented in figs. 12 and 13. the analysis of these plots shows that the normal stresses in a metal enclosure when using the filling out fibre reinforced soil is much less than for soil that is unreinforced. figure 7. the diagram of axial force for sand backfill (nmax = 147.87 kn) figure 8. the diagram of bending moment for sand backfill (mmax = 6.5 knm) figure 9. the diagram of shell displacements for fibre reinforced sand backfill (umax = 20.71 mm) figure 10. the diagram of axial force for fibre reinforced sand backfill (nmax = 164.28 kn) 36 vol. 10/2017 fiber reinforced sand backfill figure 11. bending moment diagram for fibre reinforced sand backfill (mmax = 3.78 knm) figure 12. stress diagram for sand backfill (σmax = 105.39 mpa) 3. conclusions (1.) using fibre reinforced soil can improve the strength and deformation characteristics of the soil backfill corrugated metal tunnel lining, which leads to a significant reduction of stresses and strains in it. stress was reduced by 42 %, and the deformation by 8.6 %. (2.) the results of the calculations showed that improvement of the mechanical characteristics of the soil backfill for the tunnel allows the use of thinner corrugated sheets, which reduces the cost of construction. references [1] o. moiseeva, v. kleveko. analysis of accident cases involving pedestrians in perm. pnrpu construction and architecture bulletin (4):134–143, 2015. [2] p. a. tretyakova, v. kleveko. modern methods of increasing the efficiency of urban transport systems. pnrpu construction and architecture bulletin (1):101–108, 2012. figure 13. stress diagram for fibre reinforced sand backfill (σmax = 61.19 mpa) [3] o. v. moiseeva, v. i. kleveko. choice of a rational type of pedestrian crossing with safety for pedestrians and construction costs. world science and innovation 8(2):90–93, 2015. [4] a. e. polovnikova, v. i. kleveko. choice of a rational type of pedestrian crossings with regard to the safety of pedestrian traffic. modernization and research in the transport sector 2:356–361, 2015. [5] o. v. moiseeva, v. i. kleveko. choice of rational type of crosswalk with regard to the safety for pedestrians and the cost of construction. sworldjournal j21504.(2(9)):3–5, 2015. [6] o. v. moiseeva, v. i. kleveko. using prefabricated corrugated metal structures for the construction of a pedestrian tunnel. modern scientific researches and innovations 12(56):409–411, 2015. [7] v. v. kovalchuk. the effect of corrugated elements thickness on the deflected mode of corrugated metal structures. nauka ta progres transportu 3(57):199–207, 2015. [8] a. l. novodzinsky, v. i. kleveko. the account influence of a thickness of the goffered element on durability and stability of a metal water throughput pipe. pnrpu construction and architecture bulletin (1):81–94, 2012. [9] v. i. kleveko, y. m. shangina. the impact of the use of fibre reinforced sand as backfilling on the value of act. sworldjournal 04(116 (10)):16–21, 2016. [10] a. b. ponomarev, a. s. kuznetsova, v. g. ofrikhter. application of fibroreinforced sand as the foundation of buildings and constructions. bulletin of volgograd state university of architecture and civil engineering series: construction and architecture (30):101–107, 2013. [11] a. s. kuznetsova, v. g. ofrikhter, a. ponomarev. strength research of sand reinforced by discrete polypropylene fibres. pnrpu construction and architecture bulletin (1):44–55, 2012. [12] a. b. ponomarev, a. s. kuznetsova. laboratory testing of the strength characteristics of fibre reinforced sand with various water. bulletin of civil engineers 6(47):127–132, 2014. 37 acta polytechnica ctu proceedings 10:34–37, 2017 1 introduction 2 fibre reinforced sandy backfill 3 conclusions references 322 acta polytechnica ctu proceedings 1(1): 322–325, 2014 322 doi: 10.14311/app.2014.01.0322 final remarks giulio auriemma1,2 1universiẗı¿œ degli studi della basilicata, potenza,italy 2infn sezione di roma, rome, italy corresponding author: giulio.auriemma@cern.ch this year we have to celebrate the 50th anniversary of the book “the structure of the scientific revolutions” by thomas kuhn that has been published in 1963.. in this book, the more influential science philosopher of the last century, changed the old view of the development of the natural sciences as a linear process accumulation of knowledge into a substantially discontinuous passage from one paradigm to a new one. two drastic changes of paradigm occurred near the beginning of last centuries with the shift from newton’s absolute time to relativistic space-time and from laplace determinism to quantum mechanics. around the middle of the same century another crucial shift of paradigm was the introduction of gauge symmetries, that led to the formulation of the standard model of electromagnetic, weak and strong interactions (sm for brief) [1], whose complete experimental verification has been given recently by lhc [2, 3]. the carriers of those three forces are spin-1 particles, namely the photon for the electromagnetic, the gluon for the strong and the w±,z for the weak one. it is well known that the first two particles are massless, while the others, that were discovered at lep. have large masses (∼ 80− 90 times the mass of the proton), which can explain the weakness of the corresponding interactions. since the sm does not include gravity, there is no hint in it for the mass of the particles, that are put “by hand” in the lagrangian. what is now usually called the “higgs mechanism” [4, 5] is the possibility that the mass of particles, in particular that of the weak bosons, could be originated by the coupling with a universal scalar field, which carriers would be a weakly interacting spin-0 particles very similar to the one recently observed at lhc. nevertheless even a confirmed discovery of the higgs would not be the end of the story, because thanks to astronomy and cosmology, we have strong observational evidences for phenomena like inflation dark matter dark energy baryon asymmetry that are not understood in the framework of the minimal sm. this justify the diffuse opinion (hope?) that a lot of new physics remains to be discovered in the sky and laboratory. 1 cosmological parameters the results presented by rubiño-martin [6] on behalf of the planck collaboration is one of the highlights of this conference. the new measurement of the hubble constant from the fit of the cmbr obtained from the planck satellite 2013 data is h0 = (67.3± 1.2) km s−1 mpc−1 is fully compatible with the previous value of 70 ± 2.2 published by wmap collaboration. however the central value of h0 is changed by non-negligible factor (-4%) that indicates that the age of the universe is effectively t0 = (13.82± 0.12) gy, about 100 million longer then the previous estimate from wmap. incidentally that caused a funny “communication” problem with the media, because it was public ally announced on being the “universe older then the big bang”. figure 1: reproduced from ref. [6] the tension of the h0 value between hst key project (cepheid+sne ia) and the cmbr anisotropy fit, shown in fig. 1, that was marginal (−1.2σ) with 322 http://dx.doi.org/10.14311/app.2014.01.0322 final remarks wmap, is now at a level of −2.5σ with the new planck data. not a suspicious level yet, but close to become interesting. table 1: universe composition from cmbr before planck after planck dark energy 72.8% 68.3%(−4.5% ⇓) dark matter 22.7% 26.8%(+4.1% ⇑) ordinary matter 4.5% 4.9%(+0.4% ') total 100% 100% a similar situation is observed in the determination of the λcdm composition breakdown as shown in table 1. the uncertainty on the fractions is estimated by the planck collaboration to be about ±3% [7]. but it should be also stressed that this fraction are obtained with a multivariate fit over a constrained domain, in which correlations play an essential role. therefore the fit error given independently for each of the variables could be strongly underestimated. generally speaking a reliable error on the determination of each parameter should be obtained using the full covariance matrix of the fit, if definite positive. 2 dark energy nino panagia [8], presenting the most recent results of the hubble supernovae cosmology project (scp), strongly stressed that the λcdm model with ωλ = 0.729 ± 0.014 indicating a present universe dominated by the mysterious dark energy, are all based on the assumption that the explosive properties of the sne ia do not depend from redshift, up to z ' 1.4. both the scp and ground based telescope surveys of light curves and spectroscopic distributions of hundreds of supernovae, consistently found that the supernovae around z ≈ 0.5 appear to be ≈ 0.3 mag dimmer then expected from a flat universe with ωλ = 0. what if a cosmical conspiracy made the sne at redshift ≈ 0.5 intrinsically dimmer? as predictable this pebble thrown in the placid pool (near stockholm) started a heated discussion. many in the audience supported the argument that the good fit of distance modulus vs. redshift curve [9] and of the tt spectrum of cmb fluctuations. in the discussion following the presentation of his paper, nino questioned from a philosophical point of view that a successful fit is not to be taken as a definitive proof of validity for a theory. his point is absolutely correct, but popper would object that a scientific theory can be falsified, not affirmed. therefore we can exclude theories that do not fit the data, but not viceversa. on the same ground i think that would be very hard to fit the planck data with ωλ = 0. harmes [10] has presented an interesting paper on a possible identification of the dark energy with solitonic primordial gravitational waves in the framework of quantum gravity with one warped extradimension, similar to the russel saunders one. beside the specific model presented in that talk, that may explain both strength and time evolution observed by planck [11], it has been speculated that dark energy could be the present manifestation of long lasting relics, with lifetime much larger then the hubble time, produced in the planck era (tu . 5 × 10−44 s) by quantum gravity effects. 3 dark matter astrophysical evidence for dark matter is now overwhelming. in a recent paper bahcall and kuilier [12] tracing the mass-to-light ratio with dynamical and lensing methods, show that this ratio m/l � 1 is nearly constant for scales from 350h.1 kpc up to 22h−1 mpc, while the fraction of the stellar mass over the total mass remains of the order of few percent over all scales and environments. it worth noticing that quantitatively the observed mass-to-light ratio on large scales gives an estimate of the mass density of the universe ωm = 0.26 ± 0.02, slightly smaller (≈ 1.5σ) then the planck value [6]. after the discovery of the higgs particle, dark matter is considered to be the most compelling evidence for new physics [13, 14]. particle theory offers several type of objects that could play the role of observed dark matter, as for example axions and majorana neutrinos, but excellent theoretical candidates are the supersymmetric neutral partners of the sm particles. lhc has definitively the possibility of discovering these particles if their mass is in the tev range. however, as i said in my talk, there is a fruitful confrontation among astronomical observatories and accelerators but not a competition, because astronomy cannot demonstrate that wimp’s are supersymmetrical particles and accelerators cannot prove that a certain kind of particle really is the dark matter. several talks have described the status of the search for wimp annihilation signal in γ-rays survey. in particular morselli [15] presented on behalf of the fermilat collaboration several interesting results both on the diffuse component and of the gc region. at present we have some indications that the allowed mass scale for wimp as well as the one of the susy neutralino at accelerators is to be found above several hundreds of gevs. 4 uhe neutrinos (?) the detection of neutral particles in the km3 detector icecube [16] in antarctica with an energy release ≥ 50 323 giulio auriemma tev is something waited since a long time. the study of a deep underwater muon and neutrino detector (dumand) in the pacific ocean, off the shore of the island of hawaii, usa, started in the late ’70s [17]. but unfortunately after many years of r&d the project was interrupted in 1996, after the decision of the doe science committee of not funding its deployment. in the meanwhile many other projects were initiated in many parts of the world, and often the collaborations have presented progress reports to the vulcano conferences. the icecube collaboration has announced last april the detection of two contained showers with an energy estimated from the total number of photo-electrons & 1 pev. it is worth noticing that this energy estimate is based upon the assumption that all the light is emitted in the electromagnetic cascade. the total number of events (28) detected until now by the detector [18] seems to give the first clear indication of nongeophysical and extra-solar origin neutrinos. 1. fargion[19] has proposed in his talk some intriguing possible mechanism originating these events, that could be tested in the future, when a larger number of events will be hopefully detected. it is however to be stressed that these events are really exceptional under many aspects. if they are true neutrinos the c.m.s energy of their interaction: √ s = √ 2mneν = 316− 1400 gev�mz is order of magnitudes larger than any neutrino-nucleon interaction observed in laboratory until now. it has been proposed in the past [20, 21, 22] that different kind of new physics could enhance substantially in this energy range. moreover the detected showers could have been originated not by neutrinos but by new physics messenger, such as for example susy particles. acknowledgments i am sure to interpret the feelings of all the participants to this very successful meeting thanking the scientific committee for having assembled such an interesting program; all the speakers for their efforts in communicating results and ideas; daniela and francesco for the precious help given to run smoothly the meeting; valentina, lisa, flavia and alessandro for the good music and readings, that gave us a moment of true ... “felicitas” the weather in mondello not making us to regret of being segregated inside the lecture room; and finally franco ... everybody knows why! references [1] g. altarelli, standard model of particle physics, in: j.-p. francoise, g. l. naber, , t. s. tsun (eds.), encyclopedia of mathematical physics, academic press, oxford, 2006, pp. 32-38. arxiv:hep-ph/ 0510281. [2] g. aad, et al., observation of a new particle in the search for the standard model higgs boson with the atlas detector at the lhc, phys.lett. b716 (2012) 1-29. arxiv:1207.7214 doi:10.1016/j.physletb.2012.08.020 [3] s. chatrchyan, et al., observation of a new boson at a mass of 125 gev with the cms experiment at the lhc, phys.lett. b716 (2012) 30–61. arxiv:1207.7235. doi:10.1016/j.physletb.2012.08.021 [4] p. w. higgs, broken symmetries, massless particles and gauge fields, phys. lett. 12 (1964) 132– 133. doi:10.1016/0031-9163(64)91136-9 [5] f. englert, r. brout, broken symmetry and the mass of gauge vector mesons, phys. rev. lett. 13 (9) (1964) 321–323. doi:10.1103/physrevlett.13.321 [6] j. rubiño-martin, planck results : a review, in: these proceedings, 2013. [7] p. ade, et al., planck 2013 results. xvi. cosmological parameters, arxiv:1303.5076. [8] n. panagia, the hubble space telescope cluster supernova survey, in: these proceedings, 2013. [9] n. suzuki, et al., the hubble space telescope cluster supernova survey. v., astroph. j. 746 (2012) 85. arxiv:1105.3470, [10] b. harmes, gravitational waves and dark energy, in: theese proceedings, 2013. [11] p. l. biermann, b. c. harms, can dark energy be gravitational waves? arxiv:1305.0498. [12] n. a. bahcall, a. kulier, tracing mass and light in the universe: where is the dark matter?, mon. note r. astron. soc. in press. arxiv:1310.0022. [13] g. altarelli, the higgs: so simple yet so unnatural, in: talk given at the nobel symposium on lhc results, krusenberg, sweden, 3-17 may,, 2013. arxiv:1308.0545. 324 http://arxiv.org/abs/hep-ph/0510281 http://arxiv.org/abs/hep-ph/0510281 http://arxiv.org/abs/1207.7214 http://dx.doi.org/10.1016/j.physletb.2012.08.020 http://arxiv.org/abs/1207.7235 http://dx.doi.org/10.1016/j.physletb.2012.08.021 http://dx.doi.org/10.1016/0031-9163(64)91136-9 http://dx.doi.org/10.1103/physrevlett.13.321 http://arxiv.org/abs/1303.5076 http://arxiv.org/abs/1105.3470 http://arxiv.org/abs/1305.0498 http://arxiv.org/abs/1310.0022 http://arxiv.org/abs/1308.0545 final remarks [14] l. bergstrom, cosmology and the dark matter frontier, in: invited talk at the nobel symposium on lhc physics, krusenberg, sweden, may 13-17,, 2013. arxiv:1309.7267. [15] a. morselli, last results from the fermi-lat gamma-ray telescope, in: these proceedings, 2013. [16] m. aartsen, et al., first observation of pev-energy neutrinos with icecube, physical review letters 111 (2) (2013) 021103. doi:10.1103/physrevlett.111.021103 [17] a. roberts, r. donaldson (eds.), 1976 dumand summer workshop, 1977. [18] m. spurio, photonic, neutrino and particle astronomy as messenger of the universe, in: these proceedings, 2013. [19] d. fargion, uhecr correlated tev anisotropy connection with pev neutrino shower events, in: this proceedings, 2013. [20] m. s. carena, d. choudhury, s. lola, c. quigg, manifestations of r-parity violation in ultrahighenergy neutrino interactions, phys.rev. d58 (1998) 095003. arxiv:hep-ph/9804380, doi:10.1103/physrevd.58.095003 [21] m. kachelriess, m. plumacher, ultrahighenergy neutrino interactions and weak scale string theories, phys.rev. d62 (2000) 103006. arxiv:astro-ph/0005309. doi:10.1103/physrevd.62.103006 [22] r. gandhi, ultrahigh-energy neutrinos: a review of theoretical and phenomenological issues, nucl.phys.proc.suppl. 91 (2001) 453–461. arxiv:hep-ph/0011176. doi:10.1016/s0920-5632(00)00975-0 hope to meet you all at the next frascati workshop 325 http://arxiv.org/abs/1309.7267 http://dx.doi.org/10.1103/physrevlett.111.021103 http://arxiv.org/abs/hep-ph/9804380 http://dx.doi.org/10.1103/physrevd.58.095003 http://arxiv.org/abs/astro-ph/0005309 http://dx.doi.org/10.1103/physrevd.62.103006 http://arxiv.org/abs/hep-ph/0011176 http://dx.doi.org/10.1016/s0920-5632(00)00975-0 cosmological parameters dark energy dark matter uhe neutrinos (?) 320 acta polytechnica ctu proceedings 1(1): 320–321, 2014 320 doi: 10.14311/app.2014.01.0320 concluding remarks gennady s. bisnovatyi-kogan1 1space research institute, profsoyuznaya str. 84/32, moscow 117997, russia, and national research nuclear university ”mephi”, kashirskoye shosse, 31, moscow 115409, russia corresponding author: gkogan@iki.rssi.ru abstract short comments to the conference talks. keywords: cosmology x-ray sources sne star formation agn jets grb. 1 cosmology sz effect (s. colafrancesco, m. arnaud): does it help investigation of cmb fluctuation? sz influence on the cmb spectrum in clusters interferes with primordial cmb perturbations. so we have: *contamination with cluster scale cmb perturbations *clumpiness of a gas inside cluster does not permit to extract cosmological parameters from the comparison of radio and x ray observations. b. harms: gravitational waves as a dark energy strong gravity branes support gw density constant (seems like vacuum eos), but gw produce gravity, not antigravity, like de. n. panagia: sn1a, wmap, planck are the cosmological parameters coincide inside error bars (hubble constant and de density) ? 1 2 magnetic field in astrophysics *core-collapse sn explosions *cr acceleration in snr *accretion disk structure and coronae formation *jet formation and collimation *magnetic accretion and cyclotron lines *magnetars 2.1 x-ray sources heating of accretion disk corona by magnetic reconnection (s. orlando). about 35 years ago this problem was considered in papers of g. s. bisnovatyi-kogan and s. i. blinnikov ”a hot corona around a black-hole accretion disk as a model for cygnus x-1.” sov.astron.lett. 2, 191-193 (sep.oct. 1976) and a.a. galeev, r. rosner, g.s. vaiana ”structured coronae of accretion disks”. apj, 229, 318-326 (april 1979). in the first paper a convective instability of the radiation dominated region in accretion disks was established, and its connection with formation of a hot corona was considered. ”heat transfer in the region of maximum energy release of an accretion disk will take place mainly by convection, serving to enhance the turbulence and to generate a powerful acoustic flux. the hard x-rays emitted by cyg x-1 (e ≤ 200 kev ) might result from comptonization of soft photons in a corona formed around the disk through this heating.” in the second paper the magnetic mechanism of the corona heating over the convective region of the accretion disk was studied. ”a model for the fluctuating hard component of intense cosmic x-ray sources (such as cyg x-i) is developed, based upon the amplification of magnetic fields by convective motions and differential rotation within a hot (t > 106 k) accretion disk. field reconnection within the inner portion of the disk is shown to be ineffective in limiting field amplification; magnetic fields may therefore attain strengths comparable to the equipartition value, leading to their emergence via buoyancy in the form of looplike structures and resulting in a very hot (t > 108k) magnetically confined, structured corona analogous to the observed structure of the solar corona. the energy balance of these loop structures is examined, and it is shown that the disk soft x-ray luminosity determines the predominant energy loss mechanism in loops: at low disk luminosities, thermal bremsstrahlung from these loops domi1resent discovery (arxiv:1312.3313) of an error in the planck detector at 217 ghz make the differences even less convincing. 320 http://dx.doi.org/10.14311/app.2014.01.0320 concluding remarks nates and contributes a steady, shot-noise-like hard xray component. at high disk luminosities the emerging loops are compton-cooled; the soft x-ray flux from the disk is comptonized by the emerged loops, forming a transient, flarelike hard x-ray component.” schematic drawing of the inner accretion disc corona, heated by magnetic reconnection in the emergent magnetic loops, (from the second paper) is given in fig.1. v. simon: analogy between lmxb ks1731-260 (ms pulsar), and her x-1 (p ≈ 1.24 sec) does not seems to be realistic. in particular, these objects have very different magnetic fields, with 2-4 orders of magnitude difference in strength 2.2 jets, grbs and sgrs a long time before the magnetar concept for sgrs came out, a related object called magnetoid was considered by l.m. ozernoi in the paper ”a theory for the formation and structure of quasistellar radio sources quasar model as supermassive star.” astron. zh. 43, 300-312 (1966). ”a ”magnetoid” is a quasistationary configuration whose equilibrium is governed by a magnetic field, provides an idealized representation of many effects occurring in galactic nuclei and especially in the central parts of quasars. the gravitational energy released through secular contraction of the nucleus is the ultimate source of the intense quasar radiation. the magnetic field is an important intermediary. ... local jets and streams of matter connected with active regions may occur when quasar nuclei reach global quasiequilibrium. although the magnetoid approach furnishes a unified explanation for the basic property of quasistellar radio sources an intense and variable flux emitted over a fairly long period many aspects necessarily remain speculative.” now there is a general opinion that quasars and agn are connected with an accretion into supemassive black holes, may be, besides a minority, represented by w. kundt, who gave a talk ”astrophysics without black holes and extragalactic grbs”. there are some observational evidences which do not support a magnetar model for sgrs, so later it could join its magnetoid predecessor. j. beall: numerical simulations, jets of different scale. heating of the surrounding matter by jet propagation. m. della valle: grb and sne connection questions remain. 2.3 sn 1987a b ashenbach: x ray development of sn 1987a 3 fundamental problems of physics chemistry in astrophysics. susana iglesias groth the talk ”the impact of fullerenos, pahs and amino acides in high energy astrophysics”. thermodynamics and gravity. marco merafina & daniele vitantoni the talk ”data analysis of globular cluster harris catalog in view of the king’s models and evolution” gravitational theory. mariafelicia de laurentis the talk ”testing f(r) theories using the first time derivative of the orbital period of the binary pulsars” leopoldo milano the talk ”eccentric eclipsing detached binaries: a toll for testing gravitational theories” 4 conclusion many topics, covering almost all sides of the modern astrophysics were presented. number of participants and number of reports is increasing. duration of talks is decreasing proportionally from 35 min maximal duration talk (1999), to 25 min (2013) in the conference of japan astronomical society (1978) the duration of each talk was 5 minutes, and some participants managed to show more than 50 transparances during this time (competition). let us hope, that franco giovannelli will find a better solution! thank you franco, and collaborators! 321 cosmology magnetic field in astrophysics x-ray sources jets, grbs and sgrs sn 1987a fundamental problems of physics conclusion 278 acta polytechnica ctu proceedings 1(1): 278–282, 2014 278 doi: 10.14311/app.2014.01.0278 havms: highly available virtual machine computer system fault tolerant with automatic failback and close to zero downtime memmo federici1, carlo gaibisso2, bruno l. martino3 1istituto di astrofisica e planetologia spaziali, inaf iaps via fosso del cavaliere 100, 00133 roma, italy 2istituto di analisi dei sistemi ed informatica ”antonio ruberti”, iasi-cnr viale manzoni 30, 00185 roma , italy 3associated inaf iaps corresponding author: memmo.federici@iaps.inaf.it abstract in scientific computing, systems often manage computations that require continuous acquisition of of satellite data and the management of large databases, as well as the execution of analysis software and simulation models (e.g. monte carlo or molecular dynamics cell simulations) which may require several weeks of continuous run. these systems, consequently, should ensure the continuity of operation even in case of serious faults. havms (high availability virtual machine system) is a highly available, ”fault tolerant” system with zero downtime in case of fault. it is based on the use of virtual machines and implemented by two servers with similar characteristics. havms, thanks to the developed software solutions, is unique in its kind since it automatically failbacks once faults have been fixed. the system has been designed to be used both with professional or inexpensive hardware and supports the simultaneous execution of multiple services such as: web, mail, computing and administrative services, uninterrupted computing, data base management. finally the system is cost effective adopting exclusively open source solutions, is easily manageable and for general use. keywords: havms high availability fault tolerant open source multitask. 1 introduction havms effectively solves the problems related to the ”robustness” of computer systems wholly embracing the concept of high availability. a system in high availability, ha in what follows, must ensure the continuity over time of the provided services, which, in case of fault, must be restored in the shortest possible time. havms, through an accurate design of the hw and sw, significantly reduces the faults and their negative effects on the provide services. havms has been designed mainly keeping in mind the following requirements: cost effectiveness, ease of management and, above all, the ability to automatically implement restoring strategies of the provided services without any interruption. all the above requirements have been met by an accurate choice of the available open source solutions meeting our targets and their integration with the sw specifically conceived by the authors. in particular, the last of them makes the system unique in its kind and competitive with analogous commercial solutions. havms is made by two servers, one active and the other dormant, but from the point of view of users, as well as from that of applications, the system is seen as a single server. the fault tolerance of the system is ensured by a continuous synchronization of the two servers. this synchronization keep the data and the states of all the virtual machines, vms in what follows, perfectly aligned. every service runs on a different vm each of which has its own ram, storage and some computing resources. each vm is independent of the others. when a fault occurs, the sleeper server is awakened and automatically takes the place of the broken server. once the fault is fixed, it will be enough to reconnect the repaired server and automatically the failback procedure restores the proper functioning of the system including its ha capabilities. 1.1 the context havms is a general purpose system, this is one of its strengths. among the potential areas in which the system proved its effectiveness, there is the acquisition and processing of data from space missions. the main abilities required to havms by this particular context are: • managing of processes that require uninterrupted data analysis and data acquisition; 278 http://dx.doi.org/10.14311/app.2014.01.0278 havms: highly available virtual machine computer system fault... • storing the results of the analysis for long periods of time; • making these results available to the scientific community, in an effective, continuos and reliable way. in fact, scientists in this area are interested in performing their analysis and tests on spatial observations as soon and on as much data as possible. furthermore, missions such as integral (international gamma-ray astrophysics laboratory) winkler, et al. (2003), have to maintain for a long period of time the results of the scientific analysis performed on the whole data set and usually released, as surveys, about every year. finally a further important requirement that has been met is making the management of the whole system, as far as possible, easy and automatic, thus minimizing the costs related to human resources devoted to the management itself. 1.2 the alternatives in designing, havms we deeply analyze and consider as points of reference the more widespread alternatives currently implementing the concept of ha. all these alternatives, in general, suffers from the problem of the adoption of often expensive sw and hw architectures. more in details these are, from our point of view and with respect to the particular operation context we are considering, the main drawbacks of the considered solutions: • windows server failover clustering (wsfc): requires the purchase of a quite expensive sw license (when this paper is written, about 900 euros per processor). all servers in the cluster must be absolutely identical. ha is guaranteed by a mirroring system, replicating the status of the severs every 5-10 minutes: if there is a fault during a replica, the replica itself may fail and the running jobs are aborted with a high probability. • vmware vsphere: requires the purchase of a quite expensive enterprise license (when this paper is written, about 4000 $). requires professional hw and an additional server to handle the nodes in the system. the setup is not simple. • red hat cluster manager (red hat enterprise linux server): requires the purchase of an annual license (when this paper is written, about 500 $). in case of fault the system must be restarted, as a consequence all runs in progress are stopped. does not support an automatic failback mechanism. 2 our solution figure 1: havms block diagram fig.1 shows the general architecture of havms. continuity of service is provided through an automatic failover (activates the dormant server in case of fault of the active one) and failback (restores the initial system configuration and operation) mechanisms. the software components implementing these mechanisms are: • xen vms manager, a manager of virtual machines; • drbd (protocol d), a synchronizer of block devices; • remus, provides transparent, comprehensive high availability to ordinary vms running on xen; • some components, designed and developed by the authors especially conceived, among the others, to implement the automatic failback and system startup. the system is based on the services provided by xen vms manager. each vm has its own ip address by which it is accessible from the outside. as previously stated, one server is active, the other one is dormant. the two servers are connected through a lan at 1 gb/sec. remus (in green) and drbd (in red) seamlessly (once every 40 msec) replicates the state of the active server on the dormant one. in particular, remus replicates the states of vms and simultaneously sends a trigger to drbd, which, in turns, synchronizes 279 memmo federici, carlo gaibisso, bruno l. martino the block devices (hard disks) of the two servers. as a consequence the two servers are aligned once every 40 msec. users connect to the vms through their unique ip address. vms makes it possible to install different operating systems, on which different softwares and services can be run, such as: matlab, idl and web servers, compilers and so on. 3 servers software and hardware architecture both servers have the same software architecture, already introduced in the previous section. the whole architecture leans on linux ubuntu server 10.04 64 (with a kernel customized to support xen). in what follows the single components of the architecture are briefly described. 3.1 xen xen hypervisor is a virtualization platform licensed under the gpl developed at the computer laboratory of the university of cambridge. xen is included in all major linux distributions and increasingly adopted by commercial solutions. one of the its most interesting feature is the ability to effectively control the requests of access to physical resources coming from vms through a paravirtualization mechanism. this mechanism guarantees a minimum decay of performance due to virtualization, since requests of access coming from vms are mainly executed on the physical computing resources. paravirtualization requires a customized version of the ubuntu kernel. 3.2 drbd drbd (distributed replicated block device) is a distributed storage system for the gnu/linux platform, usually adopted by ha clusters. drbd is responsible for the synchronization of data between the servers: one of them is identified as primary, the other one as secondary. when the primary server fails, a management process promotes the secondary one to the role of primary. when the fault is fixed, the system may reestablish the roles initially assigned to the servers, after a resynchronization of the data storage devices. this synchronization is particularly effective since only those blocks that were changed during the outage are resynchronized. 3.3 remus remus is part of xen and implements the ha concept by replicating on the dormant server the state of all the vms machine running on the active server. this snapshot occurs once every 40 msec (this value can be changed at setup time); at the same time remus sends a trigger to drbd for the synchronization of the hard disks. in this way the active server is constantly aligned, both for what concerns data and computational aspects, with the dormant server. in case of fault of the active server, the dormant one is awakened and becomes immediately active, thus avoiding any interruption in the provisioning of services. moreover, the tcp/ip protocol guarantees the correct transmission of data packets, even when the connectivity is temporary interrupted. the architecture required to effectively support our ha solution, does not expect the use of professional hw. in fact, as will be evident from the following description of our experiences in the field, an entry level solution with the following characteristics turns out to be absolutely appropriate to the achievement of our goals: • i7 8 cores intel processor • 8/16 gb ram ddr3 • 2 tb hard disk • 2 network interfaces 3.4 failover the typical faults of a operating environment such as the one here considered here, can be attributed mainly to two categories: lack of connection, malfunctioning of some vms. in case of a fault, the failover process is automatically triggered, which: 1. stops the drbd synchronization between servers; 2. if running, stops the execution of remus on the active server; 3. awakens the dormant server. the execution of vms is consequently resumed from the last committed checkpoint (at most 40 msec before). 3.5 failback unfortunately, remus does not support any kind of automatic failback. the sw developed for havms compensates for this deficiency and gives it its unicity. this process, which is automatically triggered and implemented, restores the initial configuration and operational capabilities of the system once the fault has been fixed, included its ha functionality. 280 havms: highly available virtual machine computer system fault... 4 practical applications the development of havms was determined by some practical needs. below we briefly describe the two applications that currently rely on the services offered by the system. 4.1 the ha data storage system of integral the laboratory of distributed computing at iaps (inaf) is in charge of aves federici et al. (2012), the cluster devoted to the analysis of data collected by integral. aves is connected to data storage subsystem (dss) a dedicated storage system martino and federici (2011) adopting havms. dss automatically downloads from integral science data center (isdc) courvoisier et al. (2003) the data collected by the satellite, backups this data and makes them available to aves (16 tb to rise). as a consequence of a fault of dss the download is interrupted and aves as no longer access to the shared data. this might have severe consequences on the ongoing activities since, in turn, may cause a data misalignment and a crash of the running analysis. havms avoid these risks and their unwanted consequences. 4.2 continuity of service at iasi havms guarantees the continuity of the service provided by iasi it division, among them: attendance control, centralized computing, storage and backup, printing services management. a different vm is allocated to each service. 5 further potential applications in the following we describe two potential fields of application of havms we are investigating. these fields differ substantially from one another. each of them is representative of a significant and large family of applications. 5.1 high end solution large structures, such as hospitals or national administrative offices should provide a relevant number of services that are usually hosted on individual servers. these servers, to ensure an acceptable level of reliability, should be equipped by systems for the backup of the status of the provided services and the data they deal with. this is therefore a privileged context within which to exploit the characteristics of havms. a quick market survey has shown that our solution can meet the above mentioned reliability requirements with not negligible costs but still low if compared with those of similar commercial solutions. in fact, one of the adoptable hw solutions could be the following: motherboard supermicro xeon mp series x9qxxx, equipped with 4-socket xeon processors (32 cores), 120 gb of ram, 4 ethernet interfaces etc. this configuration may provide up to 30 services, each with its own vms and ip address, with a cost of approximately 5000 euros per server. 5.2 a little gem in this section we describe a solution adopting havms that fundamentally, both in terms of computing power and cost, differs from the high end solution, which is a good example of the great versatility of our ha solution. this solution has been designed to deal with the monitoring of atmospherical and geological events by the use of sensors in hard to reach sites. the resulting system, which has a cost of about 300$ when this paper is written, is composed by three raspberry pi collecting analog and digital signals from sensors and transferring them by a radio link to a remote control station. thanks to the low power consumption, the system can be powered by a small photovoltaic panels. two of the three raspberry’s are allocated to havms; the third one, which is initially turned off, is switched on in case of failure of any one of the first two. this is obtained by a hw signal sent through lan (wakeup on lan). the awakened raspberry takes the place of the broken one thus guaranteeing the continuity of service, included those offered by havms. this solution substantially limits the number of maintenance interventions, thereby reducing the relative costs. figure 2: the raspberry pi three node havms 6 further work we plan to improve the ha capabilities of havms by adding to the current configuration a third server in 281 memmo federici, carlo gaibisso, bruno l. martino wake on lan. in case of fault this third server is automatically awakened by an hw signal sent through the lan and takes the place of the broken one. this automatic mechanism should not require any intervention by the system manager. with this solution, the system maintains its characteristics of ha also in case of fault of one server. to improve the effectiveness of havms in relation to the use of network resources, multiple network connections can be combined in parallel (bonding) to increase throughput beyond what a single connection could sustain, and to provide redundancy in case one of the links fails. 7 conclusions and discussion havms is a highly available fault tolerant general purpose, recyclable system based on the use of vms, assuring continuity of operation and no interruption in services providing in case of fault. havms is cost effective since it only adopts open source solutions. it is also extremely versatile, providing all operating systems supported by xen. paravirtualization dramatically reduces the negative impact of virtualization on the performance of the whole system. the system supports automatic failover and failback within times close to zero. automatic failback is an exclusive feature of havms. acknowledgement the authors thanks to: giuliano sabatino, fabio guglietta. references [1] winkler, c., et al.: the integral mission. astron. astrophys. 411, l1l6 (2003) [2] m. federici, et al. 2012, aves: a high performance computer cluster array. exp astron (2012) 34:105121 [3] b.l. martino and m. federici ”an high availability data storage subsystem for the integral data analysis”, mem. s.a.it. vol. 83, 377 2011 [4] courvoisier, t.j.-l., et al.: the integral science data centre (isdc) for the integral satellite scientific data analysis. astron. astrophys. 411, l53l57 (2003) doi:10.1051/0004-6361:20031172 discussion beall james’s question: do you plan to use the raspberry pi machine for computation? memmo federici’s answer: not in the traditional sense because rb is equipped with small amount of ram (only 256 mb) and little computing power. there are some applications that see this hw used in small clusters with low consumption. we plan to use rb to make some services such as web servers and print servers. this small device is very versatile and lends itself also to the process control. – 282 http://dx.doi.org/10.1051/0004-6361:20031172 introduction the context the alternatives our solution servers software and hardware architecture xen drbd remus failover failback practical applications the ha data storage system of integral continuity of service at iasi further potential applications high end solution a little gem further work conclusions and discussion 269 acta polytechnica ctu proceedings 1(1): 269–273, 2014 269 doi: 10.14311/app.2014.01.0269 active galactic nuclei: jets as the source of hadrons and neutrinos athina meli1,2,3, paolo ciarcelluti3 1department of physics and astronomy, university of gent, belgium 2ifpa, department of astrophysics, geophysics and oceanography, university of liege, belgium 3web institute of physics, www.wiph.org corresponding author: athina.meli@ugent.be abstract active galactic nuclei are extragalactic sources, and their relativistic hot-plasma jets are believed to be the main candidates of the cosmic-ray origin, above the so-called knee region of the cosmic-ray spectrum. relativistic shocks, either single or multiple, have been observed or been theorized to be forming within relativistic jet channels in almost all active galactic nuclei sources. the acceleration of non-thermal particles (e.g. electrons, protons) via the shock fermi acceleration mechanism, is believed to be mainly responsible for the power-law energy distribution of the observed cosmic-rays, which in very high energies can consequently radiate high energy gamma-rays and neutrinos, through related radiation channels. here, we will focus on the primary particle (hadronic) shock acceleration mechanism, and we will present a comparative simulation study of the properties of single and multiple relativistic shocks, which occur in agn jets. we will show that the role of relativistic (quasi-parallel either quasi-perpendicular) shocks, is quite important since it can dramatically alter the primary cr spectral indices and acceleration efficiencies. these properties being carried onto gamma-ray and neutrino radiation characteristics, makes the combination of them a quite appealing theme for relativistic plasma and shock acceleration physics, as well as observational cosmic-ray, gamma-ray and neutrino astronomy. keywords: active galactic nuclei jets relativistic shocks cosmic rays acceleration gamma-rays neutrinos. 1 introduction cosmic rays (crs) are subatomic particles (e.g. protons) and radiation of extra-terrestrial origin. their energies range between a few ev to hundreds of pev. these particles register a power-law spectrum, and the low-energy ones are believed to originate from galactic, while the crs with higher energies originate from extra-galactic sources. specifically, crs above energies of ∼ 1017ev, almost certainly originate from extragalactic sources such as active galactic nuclei (agn) and their relativistic jets. it is the particle shock acceleration in the superalfvenic jet plasmas, which is believed to be the main mechanism responsible for the production of the nonthermal crs (e.g. krymskii, 1977). especially, the importance of the very high energy cr acceleration is a favourable theme of study, as it is also the tev photons and neutrinos theme, which are produced either by the primary proton-photon or primary proton-nucleon interactions, offering further insights about the environment of a considered astrophysical source. agn sources are actually a compact region at the centre of a galaxy, which is believed to be a supermassive black hole. the radiation from an agn is believed to be mainly a result by the accretion of mass around the black hole. the accretion of matter around the spinning core of an agn produces twin, highly collimated fast outflows of hot gas, called jets, extending to distances of a few parsecs to thousands of parsecs. it is of importance to mention that the physics of jet mechanism and the jet composition on very small scales, are not perfectly understood at present. we know thought, that the agn black holes and their jets radiate in all wavebands, from the radio up to the gamma-ray regime via mostly the synchrotron and the inverse-compton scattering processes. moreover with a typical agn luminosity of l ∼ 1042 − 1047 erg/s, it is possible to explain the origin of the very high energy cr flux, under the assumption that these objects follow the star-formation-rate. for example, moran et al. (2001) find an average luminosity from an estimated 95 x-ray active agn within 60 mpc of 4.8 × 1044 erg/s, this distance being the cr absorption horizon at about 2×1020 ev. within the regions of local space accessible to cr diffusion, the energy supply over a hubble time is 6.6× 10−16 erg/cm3. by comparison, the gamma ray bursts supply is 6.7×10−20 erg/cm3. thus, agn as the most luminous permanent sources in the sky can stand as the most likely candidate for the acceleration of very 269 http://dx.doi.org/10.14311/app.2014.01.0269 athina meli, paolo ciarcelluti high energy crs. interpretation of data on the electron synchrotron radiation observed in the radio regime, suggests the presence of mildly-relativistic shocks with mean boost factors of γ = 10 − 30 in the jets of agn, see biermann and strittmatter (1987). moreover, assuming that hadrons (as we do in this work) are also accelerated along with the electrons in the jet, justify agn to be as good candidates as to provide at least a significant fraction of the extragalactic component of the hadronic cr flux observed. here we will discuss the primary particle shock acceleration mechanism in agn jets, in the context of comparative test-particle simulation studies, for relativistic single and multiple quasi-parallel and quasiperpendicular shocks. we will also briefly highlight the possible consequent tev-photon and neutrino emission. 2 single-relativistic shocks here we will review shock acceleration simulations, based on the relativistic single-shock, test-particle monte carlo code of meli and quenby (2003a,b), as a comparative tool to the multiple-shock acceleration study of the following section. in our simulations we inject a large number of particles n = 104 upstream towards a single planar shock, with an initial particle energy γ = γsh + 5. we use shock lorentz factors of γ = 10 and 30, and we numerically let the particles’ guiding-centers to scatter with the assumed background magnetic field irregularities, around a shock region of a length d = 2 pc. for details on the code see meli and quenby (2003a,b) and meli et al. (2008). briefly, our exemplary simulations show that : the relativistic quasi-parallel (e.g. ψ = 25o) and quasiperpendicular (e.g. ψ = 75o) single-shock acceleration mechanism manifests into a clear deviation of the cr spectral index (compared to standard, unaffected non-relativistic spectral index of ∼ 2.0) with an absent ’universal’ power-law spectrum, which depends on three parameters: i) speed of the shock, ii) shock inclination, and iii) different scattering modes, see table 1. we clearly see a high acceleration efficiency (in terms of emax) for the cases of quasi-parallel shocks. albeit, quasi-perpendicular shocks result into more ’conservative’ acceleration efficiencies and lower attained energies. it is important to note that it is been reported that the lower the turbulence, in terms of the mean-free-path η = λ/rg, the steeper the particle spectrum (meli et al. 2008). near-perpendicular shocks strongly appear to give the steepest spectra compared to quasi-parallel shock cases, and are the less efficient accelerators, see also e.g. niemec and ostrowski (2004), stecker et al. (2007), etc. summarizing, it is widely accepted that (with a few exceptions) as soon as an astrophysical shock speed becomes comparable to the speed of light, the power-law index of the accelerated cr spectra, depends strongly not only on the speed of the shock but also on the shock obliquity (scattering mode is also important, see meli, 2011), identifying clearly flatter spectra for small shock inclinations, with greater acceleration efficiencies. table 1: examples of simulations for single shocks with different shock lorentz factors (γ) and shock inclination angles (ψ), and the attained spectral indices (σ), and maximal particle energies e, respectively. γ ψ = 25o ψ = 75o 10 σ = 2.0, e = 109.3gev σ = 2.4, e = 105.6gev 30 σ = 1.9, e = 109.8gev σ = 2.3, e = 106.0gev 3 multiple-relativistic shocks after the brief insights on the relativistic single-shock acceleration above, we will now discuss a case study of particle acceleration in multiple-shocks, based on the fully relativistic multiple-shock, test-particle monte carlo code by meli and biermann (2013). in the past it was shown that for an infinite number of subsequent non-relativistic shocks with injection at each shock, the flattening of the spectrum (compared to a single shock) extends even to the highest energy particles with a momentum dependence of f(p) ∝ p−3 (e.g. white 1985). here we will investigate the acceleration mechanism in relativistic, multiple, quasi-parallel and quasiperpendicular shocks. we can envisage blobs of hot plasma ejected by the black hole of an agn that can travel along the jet and pass through a sequence of shocks, as it has been also observed in blac pks 1510089 (marscher et al. 2010) and other sources. here we numerically calculate the scattering of the particles’ guiding-center with pre-determined background magnetic field irregularities, around multipleshock regions and within a distance d = 5 pc. at the beginning of the acceleration we allow a single initial injection of particles of a fixed number n = 104, with an initial γ = γsh + 5, and shock lorentz factor γ = 30 (for the first two shocks) and γ = 10 (for the second pair), justified by the decompression-compression conditions of the downstream plasma (melrose and pope 1993) of the precedent shock pattern (i.e., a velocity compression ratio r=3). that is, during the acceleration we allow a probability of escape pesc = 0.1 between shocks due to decompression effects. the escape probability gives the fraction of particles of the downstream distribution of each shock, that will not be accelerated 270 active galactic nuclei: jets as the source of hadrons and neutrinos more. these particles remain in the system and contribute directly to the downstream distribution of the 4-th shock. this factor would naturally result in steeper spectral slopes comparing to a single shock acceleration spectrum as the relativistic conditions render the spectra flatter. assuming also a field compression ratio rbc equal to , and an assumed magnetic field strength of the order of a few mgauss, the distance between each shock is safely set as d = 1pc. we study two cases of shock patterns: i) a set four quasi-parallel shocks (with the same apex to the assumed jet axis), and inclination angles ψ1, ψ2, ψ3, ψ4 = 25o, and ii) a set of four quasi-perpendicular shocks and inclination angles ψ1, ψ2, ψ3, ψ4 = 75o. table 2: aaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaa γ ψ σ e[gev ] 30 25o 2.6 105.9 30 25o 2.2 106.9 10 25o 2.1 108.6 10 25o 1.5 109.5 table 3: in the tables above we see indicative simulation numbers for two sets of four-shocks, their maximal attained energies e at each shock downstream, and their spectral indices σ. shock inclination angles are denoted as ψ, and γ is the shock lorentz factor. γ ψ σ e[gev] 30 75o 2.7 104.6 30 75o 2.4 105.2 10 75o 2.3 105.9 10 75o 2.2 106.4 briefly, from the tables above, one notices that (i) the spectra by each shock in every shock-set become gradually flatter, following on one hand the findings of single relativistic shocks discussed in the previous section, and on the other hand the trends reported in e.g. melrose and pope (1993) and gieseler and jones (2000) for multiple shocks. (ii) the flatness of the spectra is more evident for the consecutive quasi-parallel shocks than for the quasi-perpendicular ones, following, as expected, the individual shock effects we discussed in the previous paragraph. (iii) the acceleration in the case of quasi-parallel shocks seems very efficient and comparable to single shock acceleration. 4 neutrino and gamma-ray astronomy over the years many models have been created (e.g. stecker, 2005), assuming protons are accelerated at the shocks of agn jets and interact with different photon fields to produce high energy gamma-rays and neutrinos. the cr acceleration cases shown here, have implications for neutrino and gamma-ray astronomy, and especially for the tev sources. we know that only from e.g. the p−γ interaction (where the optical depth must be equal or larger than 1), the consequent decay of the π0 results into a high energy photon (in 0.33 of the cases). also π± particles produce neutrinos. specifically, the probability for π+ production is 0.66. around 0.20 of the proton energy goes into pion, and the products carry equal energy, so that a fraction of 0.25 (0.50) is transferred to each neutrino (photon) and furthermore, one must also consider that neutrinos oscillate. therefore the high-energy photon and neutrino spectra can be connected as dnν deν = 1 8 · dnγ deγ . additionally it can be assumed that the neutrino carries about 1/20th of the proton’s energy (see halzen, 2008). all these can be very helpful in understanding crs and related consequent emissions. nevertheless, in many agn the photon signal at tev energies is not unique, since leptonic processes like inverse compton scattering could also contribute at the same energies. but there is a way of identifying hadronic interactions in astrophysical shocks by estimating the flux of neutrinos. not to let unmentioned, one can also assume that the spectral indices for the tev photon and neutrino emission at a break threshold energy, generally at around 102gev, can be considered to be about the same. it is accepted that not all agn sources can be seen or inferred emitting crs, and this due to either the high galactic background absorptions, or particle’s random diffusion in magnetic fields, or even insufficient power to accelerate very high crs. nevertheless, neutrino signals, could reveal the possible hadronic nature of a tev source. we saw in this work that relativistic quasiperpendicular shocks in agn, single or multiple, cannot accelerate crs to very high energies. we know also that a photon field in the jet of an agn can range from low energies to many tev. we also know (e.g. becker et al. 2011) that the proton energy necessary to produce a delta resonance in the observer’s frame, can be given as, ep ≥ γ2 (1+z)2 m2 ∆−m2 p 4 · e−1 γ , where m∆ is the mass of the delta resonance, mp is the proton-mass, eγ is the characteristic photon energy and z is the redshift of the source (e.g. cen a, z = 0.001). therefore, simplistically, one can assume a photon field (i.e. but dense enough for photo-hadronic interactions) to make 271 athina meli, paolo ciarcelluti an estimation of the maximal energy of the proton (as shown in this work) necessary to produce tev-photons and gev-tev neutrinos, or vice-versa, and make further estimations on the correlations of different wavelengths from the same source. as an example here for the case of the favourable tev emitter, cen a, with z = 0.001 and an assumed shock(s) lorentz factor of γ = 30, the proton energy sufficient to produce a delta resonance and with these, tev-photos and neutrinos, can be given as ep ≥ 105 · (1 + z)−2 · ( γ 30 )2 · ( eγ 1 mev )−1 gev . thus, for quasi-perpendicular shocks, the proton spectra found in our simulations reach low energies ep ∼ 106 gev, which could not be directly observed. in order though to achieve tev photons and along with them neutrinos, one would require photon field energies at the jet of equal or greater than eγ ≥ 10 mev. of course these energies can be produced via the inverse compton scattering of synchrotron or external photons with the accelerated electrons certainly present at the jet. therefore one would expect a high energy signal of neutrinos, if the source is of a hadronic nature. what one can in generally conclude from the above brief discussion, is that the extragalactic tev sources, which can not be observed as candidates of ultra-high energy crs, may nevertheless emit high energy neutrinos implying the hadronic nature of the cosmic rays. this fact can be used as a supplementary tool to filterout neutrino source candidates. calculations on flux and further details on radiative consequences are under away. 5 conclusions the relativistic shocks in the jets of agn are a favourable accelerator of high-energy as well as lowenergy crs, via the shock acceleration mechanism. here, we performed comparative monte-carlo simulation studies for single and multiple relativistic shocks, assuming protons as the primary accelerated particle and we showed that relativistic (quasi-parallel either quasi-perpendicular) shocks are very important since they can alter dramatically the cr spectral indices and acceleration efficiency. these properties are carried onto gamma-ray and neutrino emission from the same sources. thus, assuming a hadronic primary accelerated scenario, one could have an additional understanding regarding expected neutrino fluxes from tev sources. specifically, agn with tev gamma-ray emission, and non-observable or low-energy crs, could have the potential to carry an additional high energy neutrino flux signal, mimicking accordingly the primary accelerated particle spectra in the jet, separating it from the inverse compton leptonic or other related processes. accurate flux expectancies of gamma-rays and mostly neutrinos within earth neutrino-observatory potentials (e.g. icecube, km3net), is the next step for deeper understanding of agn jets. acknowledgement a.m. would like to thank the organisers for the invitation to give an advanced talk on the topic of shock acceleration and cosmic rays. she also likes to thank p. l. biermann, j. j. quenby and j. k. becker for contributing their valuable expertise to the cited studies above; she acknowledges fruitful discussions with antares and icecube/icetop collaborations; and she is constantly indebted to a. mastichiadis, s. dimitrakoudis, r. protheroe, a. donea, t. kneiske, m. dieckmann, a. reimer, m. ostrowski, i. brancus, j. wentz, m. giller, a. wolfendale, t. stanev, k.nishikawa for offering, in different occasions over the last years, valuable advice and insights on related studies. references [1] becker, j., meli, a. & biermann p. l., 2011 nucl. ist. meth., 630 269 doi:10.1016/j.nima.2010.06.082 [2] biermann, p. l. & strittmatter, p. a., 1987 apj, 322, 643 [3] gieseler, j. & jones, t. w., 2000, aa 357, 1133 [4] halzen, f., j., 2008 phys. conf. ser., 120 (6) 062004 doi:10.1088/1742-6596/120/6/062004 [5] krymskii, g. f., 1977 akademiia nauk sssr, 234, 1306 [6] marscher, a. p., jorstad, s. g., larionov, v. m., et al., 2010 apj, 710l, 126 doi:10.1088/2041-8205/710/2/l126 [7] meli, a. & quenby, j. j., 2003b aph 19, 649 [8] meli, a., becker, j. k., j., quenby, j. j., 2008 a&a 492, 323 [9] meli, a., 2011, astrspsc 7, 287 [10] meli, a & p. . biermann, 2013 a&a in press [11] melrose, d. b. & pope, m. h., 1993 pasau, 10, 222 [12] moran, e. c., kay, l. e., davis. m., filippenko, a. v., barth., 2001 ast.j., 566, l75 [13] niemiec, j. & ostrowski, m., 2004, apj 610, 851 doi:10.1086/421730 [14] stecker f. w., 2005 phrvd, 72j 7301 [15] stecker f. w., baring j., summerlin e. j., 2007 apj, 667l, 29 doi:10.1086/522005 [16] white r. l., 1985 apj 289, 698 discussion pieter meintjes: you mentioned that strong relativistic shocks will be accompanied by turbulence. can you comment on the role that mhd can possibly play in the 272 http://dx.doi.org/10.1016/j.nima.2010.06.082 http://dx.doi.org/10.1088/1742-6596/120/6/062004 http://dx.doi.org/10.1088/2041-8205/710/2/l126 http://dx.doi.org/10.1086/421730 http://dx.doi.org/10.1086/522005 active galactic nuclei: jets as the source of hadrons and neutrinos acceleration process? is it possible that strong mhd turbulence can distort a power-law spectrum into a kind of relativistic maxwellian as a result of acceleration through mhd waves? if this happens, under what conditions? athina meli: the numerical approach of the model presented here is that of the test-particle approach, investigating a collision-less plasma (kinetic theory) and not a collisional plasma (fluid theory). i note that shocks do exist in collisionless media, i.e. without collisional dissipation (resistivity/viscosity). let me also add though that an mhd description of a collisionless plasma it is not entirely wrong to be assumed, because all fluid equations (except closure) are exact conservation laws (and closure is not too sensitive to microphysics at large scales), but there are many other exceptions mainly when large scales are not independent of the small ones with critical limits. for the present case, the mhd turbulence effect connection can be attained at the context of assuming the strength of scattering modes directly in the code (i.e. strong or weak scattering, as large angle diffusion or pitch angle scattering), by relating it to the diffusion coefficient (κ) which is dependent on the level of media turbulence, denoted by the ratio λ/rg. please see detailed descriptions of the particle kinematics in meli and quenby (2003b), meli et al.(2008) and meli (2011). as i discussed here, the type of scattering hence the level of mhd turbulence in the media can alter the produced spectra in the relativistic shock acceleration cases. jim beall: does the spectra you get from these shocks depend on the specific shock structure? athina meli: the shock structure can alter the steepness of the shock, and i deal with this matter in another recent work (meli, 2013) (not presented here, planar shocks only). maurizion spurlo: cosmic rays with energies above 1019 ev, following the auger measurements, seem to be mainly heavy nuclei. can the acceleration model from agn jets you presented, accelerate heavy nuclei instead protons maintaining the same features? athina meli: the relativistic shocks presented here produce spectra mainly below 1019ev , favoured for protons. nevertheless, in some ideal cases one can obtain easily spectra that reach energies of 1020−21ev, as i showed in a related work. this acceleration model can treat the acceleration of heavy nuclei, but the consideration of added losses must be taken into account in the code, which will mostly steepen the spectrum by an order of magnitude or more, as some of my preliminary test-runs have shown. i note here though an important point: the spectra even above energies of 1019ev seem to be a (unknown) mix of protons and heavy nuclei, since pure heavy nuclei population seems highly improbable. 273 introduction single-relativistic shocks multiple-relativistic shocks neutrino and gamma-ray astronomy conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.9.0026 acta polytechnica ctu proceedings 9:26–31, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app removal of diquaternary ammonium cations from as-synthesized ssz-16 zeolite tatana supinkovaa,c,∗, ivan jirkaa, jan drahokoupilb,d, jan langmaiera, vlastimil filac, libor brabeca, milan kocirika a j. heyrovsky institute of physical chemistry,czech academy of sciences, dolejskova 2155/3, prague 8, czech republic b faculty of nuclear sciences and physical engineering, czech technical university, trojanova 13, prague 2, czech republic c faculty of inorganic technologies, university of chemistry and technology in prague, technicka 5, prague 6, czech republic d institute of physics, czech academy of sciences, na slovance 1999/2, prague 8, czech republic ∗ corresponding author: tatana.supinkova@jh-inst.cas.cz abstract. zeolites are stable microporous aluminosilicates with numerous applications in chemical technology such as separation of species and catalytic transformations. our study is focused on a weakly explored zeolite ssz-16 with pore constrictions defined by 8-membered oxygen rings. key results are the preparation of et6-diquat-5 dication used as a structure directing agent (sda) and finding the optimum synthesis conditions with respect to zeolite phase purity. stability of sda was examined in conditions similar to those of autoclave synthesis (concentration, ph, temperature). moreover, the content and location of sda species in zeolite phase and conditions of sda decomposition were investigated. keywords: zeolite, hydrothermal synthesis, ssz-16, afx, et6-diquat-52+. 1. introduction zeolites and zeolite-like materials consist of tetraedral building units to4 where t are central atoms most frequently si and al+. tetraedra are linked to each other through oxygen atoms. the spaceous arrangement of tetrahedra form as a rule microporous structure where micropores take the shape of regular voids (channels and/or cavities) which are repeated through the crystals with the regularity of the crystalline structure. in zeolites, t-atoms can be replaced by isomorphous substitution, for example ge, ti, p, fe, ga, b and thus form zeolite analogues. zeolites and their analogues are crystalline materials with regular microporous structure (with pore width < 2 nm). the intracrystalline pores are thus of molecular dimensions. the surface of intracrystalline pores is formed by oxygen atoms. the critical pore width is for atoms and molecules as a rule determined by oxygen rings containing 8, 10 or 12 oxygen atoms. small cations can pass even through 6-membered oxygen rings. micropores can accommodate spherical molecules typically with the diameter of 0.3-1.0 nm or cylindrical molecules with cylinder diameter in the above range. zeolites are also called molecular sieves due to possible exclusion of molecules with size exceeding some critical value. zeolites are perspective materials for industrial applications due to their molecular sieve effect, high adsorption capacity, and frequently to the presence of catalytic sites or to their ion exchange capability. a relatively novel zeolite ssz-16 belongs to the class of small pore zeolites characterized by 8membered oxygen rings which may exhibit molecular sieve effect for gases with small molecules. the main field of its application is believed to be in gas separation of various hydrocarbons and mixtures containing molecules such as co2, h2, ch2 and other gases [1–3]. furthermore, zeolite ssz-16 can be used as microporous layers and particles to develop composite and mixed matrix materials [4–6]. zeolite ssz-16 was also tested as a catalyst. for example, cu-ssz-16 [7, 8] seems to be promising as a selective catalytic reduction catalyst for the direct conversion of no into n2 and o2. zeolite h-ssz-16 was found to be highly selective to dimethylamine in the catalytic reaction of ammonia and methanol [9]. the principal aim of this work is to optimize zeolite ssz-16 hydrothermal synthesis and contribute to answering questions concerning limits to phase purity, yield and posibility to control morphology and size of crystals. moreover, the research could clarify the role of diquaternary ammonium species in the synthesis. the principal aim of this work is to contribute to the knowledge of structure-directing agent (diquaternary ammonium dications) chemistry in relation to its (i) synthesis and purity, (ii) role in the synthesis of ssz-16 zeolite, (iii) stability in synthesis batches and (iv) its thermal removal from the zeolite framework. 26 http://dx.doi.org/10.14311/app.2017.9.0026 http://ojs.cvut.cz/ojs/index.php/app vol. 9/2017 removal of diquaternary ammonium cations from as-synthesized ssz-16 zeolite figure 1. left afx framework type representation using cbu and their arrangement (adapted from www.iza-online.org), right afx framework type representation using 6-6 sbu (adapted from ilyushin et al. 2015). figure 2. view of the afx structure along the caxis; yellow spheres t-atoms, red spheres oxygen atoms, blue patterns visualization of electron density distribution. 2. theory 2.1. zeolite ssz-16 and its structure zeolite ssz-16 is isotypic with its zeolite analogue sapo-56 [7, 10, 11]. both these microporous materials exhibit the afx framework type. this framework shows the hexagonal symmetry, the corresponding space group of symmetry is p63/mmc and the unit cell idealized parameters are a = b = 13.7 å, c = 19.7 å. fundamental articles on ssz-16 present the afx framework type in the terms of composite building units (cbu): gmelinite (gme) and aft cavities and d6r (double six-ring) cages [10, 12, 13], see figure 1 (left). this method of afx framework type representation is widely used to visualize spaces capable of accommodating sorbing species. however, this method is less suitable for the analysis of various zeolite framework topology features due to the existence of common t-atoms for the neighbouring cbu. an alternative way of afx framework representation is by secondary building units (sbu) using either an array of 6-membered rings (6 code) or double 6-membered rings (6-6 code), see figure 1 (right). figure 2 represents the view of the afx structure along the c-axis using the visualization of electron density distribution (computed by dft calculation implemented in castep program). zeolites ssz-16 and sapo-56 belong to small-pore zeolites with 3d pore system. the narrowest passages through these pores (also called bottlenecks or configure 3. 8-membered oxygen ring in sapo-56 viewed normal to [001], red spheres oxygen atoms, yellow spheres t-atoms figure 4. structure of sda hexaethylpentane diammonium dication (blue spheres nitrogen n+, grey carbon, white hydrogen). strictions) are formed by 8-membered oxygen rings. dimensions of these rings were published for sapo56 [11], see figure 3. 2.2. role of sda species in synthesis of ssz-16 essential components for zeolite synthesis are silica, alumina, source of alkali, sda and water. theoretical approaches offer a great number of hypothetical zeolite structures. however, only a small fraction of them can be synthesized. besides, a considerable number of zeolite phases can be formed only in the presence of particular organic species termed as structure-directing agents (sda). a mechanism of sda action in synthesis mixtures is still an open question. attempts were made to explain sda effect on the basis of sda species size and shape, its rigidity, hydrophobicity/hydrophilicity and sda species interactions with solution components. diquaternary ammonium species were proposed in the nineties as a novel group of sda species for the synthesis of zeolites. the research in our laboratory showed that hexaethylpentane diammonium dication (c2h5)3n+(ch2)5n+(c2h5)3 (also called as et6-diquat-52+), appears to be, among diquaternary ammonium species, the most efficient sda for the synthesis of zeolite ssz-16 [14]. the model of this sda dication is shown in figure 4. 27 t. supinkova, i. jirka, j. drahokoupil et al. acta polytechnica ctu proceedings figure 5. computer simulated location of sda molecules in uc of ssz-16 a theoretical picture of sda species in ssz-16 structure was derived using the following assumptions: • a non-decomposed sda dication can be accommodated only in the aft cavity and thus oriented with its maximum dimension along the c-axis (see figure 5). • any aft cavity accomodates just a single sda dication. • there are two aft cavities per uc. therefore, the uc contains two sda dications non-decomposed during the synthesis procedure. • in principle, the gme cavities can accomodate only some products of sda decomposition; this phenomenon is not considered in the theoretical estimate of sda content. based on these assumptions, the following formula for sda dication mass fraction (gsda)th in molar mass of uc for non-calcined zeolite ssz-16 can be formulated as (gsda)th = nsda msda (muc)0 +nsda msda , where nsda stands for the number of sda per uc and is equal to 2, msda denotes the molar mass of sda and equals to 272.32 gmol−1. (muc)0 represents the molar mass of zeolite ssz-16 free of sda and can be expressed depending on the atomic ratio si/al = z as (muc)0 = 48 mna 1 + z + 48 msi z 1 + z + 48 mal 1 + z + 96 mo, for z = 6 and (muc)0 = 3029.23 gmol−1. based on these equations, the sda dication mass fraction (gsda)th can be calculated and it equals to 0.152. the experimentally measured sda content (gsda)th in the zeolite synthesis product will be compared to this value. 3. experimental 3.1. synthesis of sda in view of the fact that the price of species containing et6-diquat-52+ dication appeared to be prohibitive, a protocol for its synthesis was developed. the reactants used for this purpose were 1,5-dibromopentane and triethylamine. the reaction proceeded in ethanol solvent. the crystallization was performed in diethyl ether solvent. because the synthesis proceeds in twostages, the purity of the synthesis product were examined by x-ray diffraction and by thermogravimetry. the heating program for sda thermogravimetry was the same as for zeolite samples calcination and zeolite thermogravimetry, see below. sda with significant content of the first stage synthesis product can thus be rejected or recycled. 3.2. synthesis of ssz-16 particles the research was directed to the development of a static in-situ hydrothermal crystallization procedure of ssz-16 zeolite [14, 15]. the synthesis was performed in three steps: preparation of starting synthesis mixture, ageing of synthesis mixture (formation of viable nuclei), and crystallization of aged mixture. the most suitable silica source appeared to be colloidal silica. the starting synthesis mixture was composed of colloidal silica ludox as 30 (30% sigma-aldrich), aluminum nitrate nonahydrate, sodium hydroxide, organic template et6-diquat-5 br2 and deionized water [14, 16]. the synthesis process was adapted by changing the synthesis solution composition, ageing period, temperature and duration of crystallization [15, 16]. the composition of synthesis solution was varied and optimized to obtain pure phase of ssz-16 particles. the ageing period was performed for seven days to promote nucleation of precursor particles (formation of viable nuclei). the ageing process of ssz-16 was performed at elevated temperature with the synthesis solutions heated up to 80 °c inside an oil bath, continuous stirring was ensured by a magnetic stirrer inside teflon vessels. the crystallization process was performed for seven days, temperature adjusted to 160 °c. the hydrothermal in-situ synthesis of ssz-16 crystalline particles performed inside teflon-lined stainless steel stationary autoclaves from the pre-aged solutions under autogenous pressure. the crystalline ssz-16 products were purified inside an ultrasonic bath, washed and dried in a pre-heated oven overnight. after the synthesis, the sda was removed by the two-cycle thermal calcination process under nitrogen/air atmosphere to open pores inside the aft cage. the temperature program for both the cycles was as follows: heating with the rate 0.5 °c/min to 120 °c, keeping at 120 °c for two hours, heating to the temperature 550 °c with the rate 0.5 °c/min, then keeping at 550 °c for 8 hours and cooling to the room temperature with the rate 0.5 °c/min. 28 vol. 9/2017 removal of diquaternary ammonium cations from as-synthesized ssz-16 zeolite 3.3. characterization zeolite ssz-16 particles were characterized by scanning electron microscopy (sem) technique using jeol jsm 5500lv to examine crystal morphology and particle size. powder x-ray diffraction (xrd) technique was used to determine crystallinity and phase purity of zeolite ssz-16 particles. x-ray diffraction was performed on panalytical x’pert pro diffractometer with co anode (wavelength λ = 0.1789 nm) in bragg-brentano geometry. the fixed divergent slits in primary beam and 1d detector x’celerator in diffracted beam were used. the spectra were collected in the 2θ range of 5-30°. the measurements and analyses of collected spectra were performed in the institute of physics, cas. the micropore volume of calcined zeolite ssz-16 particles was evaluated from nitrogen adsorption-desorption isotherms. the isotherms were measured on asap 2020 (micromeritics, usa) volumetric instrument at -196 °c. the sample was degassed under a vacuum at 350 °c for 8 h prior to the analysis. the micropore volume was evaluated by the t-plot method. particular attention was paid to sda. it concerned sda purity (xrd analysis), thermal stability and its decomposition both in synthesis solutions and products. thermal stability of sda in alkaline solutions were analyzed after the heat treatment in an autoclave. sda concentration was measured using cyclic voltammetry (cv) [17] with the home-made apparatus in j. heyrovsky institute of physical chemistry, cas. sda content in zeolite samples and sda residua after their calcination were measured using elemental analysis performed on elementar vario el iii in chns operation mode, and further on with x-ray photoelectron spectroscopy xps using esca 3 mk ii spectrometer (vg) in fixed transmission mode. the kinetics of sda removal/decomposition and related heat effects were investigated with thermogravimetry and differential scanning calorimetry using setsys evolution tga, setaram. 4. results and discussion among silica sources for synthesis mixtures, ludoxbased synthesis mixtures had the best properties both from the point of view of hydrogel density and capacity of crystallization. optimum synthesis batch composition to eliminate unwanted phases in product was determined as 3 sda: 15 na2o: 0.5 al2o3: 30 sio2: 1200 h2o. deviation from this composition causes considerable changes in phase composition and formation of different zeolitic phases. the introduction of ludox as 30 as silica source had two consequences: (i) reducing the size of amorphous core of zeolite particles which was observed in the early stages of synthesis procedure development (see figure 6a) and (ii) dramatic reducing the size of particles. the size of particles decreased to approximately 2 µm and well-developed polycrystalline particles formed (see figure 6b). this favourable development of product quality manifests itself also (i) in x-ray spectra (see figure 6. a amorphous core and crystalline shell of a particle (2 000×), b well developed polycrystalline particles (10 000×). figure 7. xrd spectra of selected samples and theoretical spectrum of ssz-16 figure 7) and (ii) in sda content measured gravimetrically from mass difference between non-calcined and calcined samples, showing on selected zeolite samples the development of (gsda)exp. in contrast to earlier preparations where amorphous cores were visible on disrupted particles and the values of (gsda)exp ranged between 0.160 and 0.180, in more recent experiments the amorphous cores were not observed and (gsda)exp ranged between between 0.140 and 0.150 approximately. it is suspected that amorphous cores exhibited a higher content of sda as compared with zeolite phase. figure 7 represents an example of the x-ray diffraction spectra of selected calcined samples compared to the theoretical diffraction spectrum for the zeolite ssz-16. the samples were confirmed to be crystalline and pure phase ssz-16 particles. regarding the content of organic species in the synthesized zeolite, a question arises whether some decomposition products of sda cannot be located in gme cavities. the evaluation of sda thermal stability in alkaline solutions performed by cyclic voltammetry showed a relatively rapid sda decomposition. the time dependence of sda concetration during its thermal treatment in alkaline solution at temperature, ph, and sda concentration close to those in synthesis mixtures is shown in figure 8. it is obvious that during the reaction time 6 to 8 hours the sda concentration decreases to a value lower than 50 % of its initial value. this may generate a considerable number of sda fragments and enhance the mass of organics incorporated in ssz-16 crystals. nevertheless, for optimized synthesis procedure the values of (gsda)exp remain in the range 0.140 to 0.150 which cast doubt on additional places of organics accommodation in ssz-16 crystals. accessibility of microporous crystal cavities after 29 t. supinkova, i. jirka, j. drahokoupil et al. acta polytechnica ctu proceedings figure 8. kinetics of et6-diquat-52+ decomposition at 160 °c. initial concentration of et6diquat-5 br2 c0 sda = 0.168mol dm−3, initial concentration of naoh c0 sda = 1.66mol dm−3, solvent deionized water. figure 9. n2 adsorption-desorption isotherm. full circles adsorption, empty circles desorption. template removal was confirmed by measurements of adsorption and desorption isotherms of n2 at -196 °c. this result is exemplified by isotherms measured on calcined sample (figure 9). the isotherm shows a sharp rise in n2 adsorption at low relative pressure and negligible hysteresis loop. its shape shows that the material is microporous with negligible effect of mesopores. the sample showed the micropore volume of 0.24 cm3 g−1. at the same time, the elemental analysis excluded presence of organic residua in crystal bulk after ssz-16 calcination. this is a contrast to the situation in crystal subsurface region where carbonaceous deposits were detected after zeolite calcination by xps. the thermogravimetric curves monitored during sda removal from zeolite samples using the above temperature program are exemplified on figure 10. temperature calibration was performed using cuso4.5h2o and sn. on the picture is the comparfigure 10. examples of tg curves percentage of the sample mass based on initial mass vs. temperature; red silicalite-1 templated with tpa+; blue ssz-16 templated with et6-diquat-52+. ison of sda removal from silicalite-1 (tpa+) with that from ssz-16 (et6-diquat-52+). there is bigger amount of organics in ssz-16 and steeper decay in the first portion of the tg curve. we suspect that it may be related to more rapid thermal decomposition of et6-diquat-52+ in synthesis batch as compared with tpa+ in silicalite-1 which is considerably more stable. we also suspect that sda fragments may be incorporated into gme cavities. 5. conclusions the principal contribution of this work is the feasibility of zeolite ssz-16 synthesis. the selected sda hexaethylpentane diammonium cation turned out to be appropriate and the synthesis route to this species was elaborated. by variation of synthesis parameters of aging and crystallization, the particle size was reduced from cca 50 µm to approximately 2 µm. moreover, the conditions to attain purity of ssz-16 higher than 98 % were found and polycrystalline samples with well developed morphology were obtained. using n2 adsorption and desorption at -196 °c, volume of micropores vmicro = 0.24 cm3 g−1 was evaluated. an insight into the chemistry of sda was presented. in particular, in its synthesis and conditions of its purity. further on, a novel technique was introduced to measure concentration variation of cationic sdas under conditions close to those at synthesis conditions. particular attention was also paid to the investigation of template removal kinetics. acknowledgements the financial support by czech science foundation via grant ga16-02681s is gratefully acknowledged. references [1] m. pera-titus et al. porous inorganic membranes for co2 capture: present and prospects. chem rev 114(2):1413–1492, 2014. doi:10.1021/cr400237k. 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[17] j. langmaier et al. extreme basicity of biguanide drugs in aqueous solutions: ion transfer voltammetry and dft calculations. j phys chem a 120:7334–7350, 2016. doi:10.1021/acs.jpca.6b04786. 31 http://dx.doi.org/10.1021/cm4015095 http://dx.doi.org/10.1016/j.seppur.2007.09.008 http://dx.doi.org/10.1039/c4ta02744b http://dx.doi.org/10.1016/j.apcatb.2010.12.022 http://dx.doi.org/10.1039/c4cc09645b http://dx.doi.org/10.1016/j.apcata.2006.02.044 http://dx.doi.org/10.1021/cm960289c http://dx.doi.org/10.1016/s1387-1811(98)00293-5 http://dx.doi.org/10.1021/cs300558x http://dx.doi.org/10.1016/s1387-1811(01)00441-3 http://dx.doi.org/10.1016/s1387-1811(03)00381-0 http://dx.doi.org/10.1016/j.micromeso.2016.03.033 http://dx.doi.org/10.1016/j.micromeso.2013.03.007 http://dx.doi.org/10.1021/acs.jpca.6b04786 acta polytechnica ctu proceedings 9:26–31, 2017 1 introduction 2 theory 2.1 zeolite ssz-16 and its structure 2.2 role of sda species in synthesis of ssz-16 3 experimental 3.1 synthesis of sda 3.2 synthesis of ssz-16 particles 3.3 characterization 4 results and discussion 5 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2015.1.0008 acta polytechnica ctu proceedings 2:8–14, 2015 © czech technical university in prague, 2015 available online at http://ojs.cvut.cz/ojs/index.php/app on fpga based acceleration of image processing in mobile robotics petr čížek∗, jan faigl department of computer science, faculty of electrical engineering, ctu in prague, technická 2, 166 27 prague, czech republic ∗ corresponding author: petr.cizek@fel.cvut.cz abstract. in visual navigation tasks, a lack of the computational resources is one of the main limitations of micro robotic platforms to be deployed in autonomous missions. it is because the most of nowadays techniques of visual navigation relies on a detection of salient points that is computationally very demanding. in this paper, an fpga assisted acceleration of image processing is considered to overcome limitations of computational resources available on-board and to enable high processing speeds while it may lower the power consumption of the system. the paper reports on performance evaluation of the cpu–based and fpga–based implementations of a visual teach-and-repeat navigation system based on detection and tracking of the fast image salient points. the results indicate that even a computationally efficient fast algorithm can benefit from a parallel (low–cost) fpga–based implementation that has a competitive processing time but more importantly it is a more power efficient. keywords: fpga, system–on–chip, image processing, fast feature detector, visual navigation. 1. introduction one of the key indicators of the intelligent behaviour of a mobile robot is its ability to react promptly in complex situations and make fast and correct decisions regarding the robot goals. on micro-robotic platforms, this is a very comprehensive task due to limited computational resources. a typical example of micro-robotic platforms are micro aerial vehicles (mavs) [1], small legged robots [2] or robots used to study swarm intelligence [3]. they can be characterized by constrained dimensions and payload, which is directly related to the limited battery capacity. altogether, these parameters determine an available computational power on-board of the mobile robot. a direct trade-off between the computational capabilities and power consumption can be identified, characterizing the maximum time for which the robot can perform its mission. this trade-off between computationally demanding and power efficient decision-making techniques is especially recognizable in navigation algorithms that rely on computer vision methods based on processing of a large amount of visual data. salient point extractors are popular techniques of machine perception in the mobile robot navigation tasks; however, not all available approaches are currently suitable for micro-robotic platforms due to the limited on-board computational resources. moreover, a practical deployment of a mobile robot always demands a real-time performance of decision-making algorithms, which imposes further restrictions on the applicable approaches regarding the available resources. two fundamental approaches how to deal with limited computational resources on micro-robotic platforms can be considered. the first approach is a simplification of the computationally demanding processing, e.g., by introducing approximations of the demanding method and simplifying the whole principle, which can be a daunting task as it may not be always possible. the second approach is a utilization of the optimized implementations for newly available features of the modern processors, e.g., a dedicated optimization for special (typically simd– single instruction multiple data) instructions of the new cpus. besides, dedicated co-processors can be utilized to speedup the computationally demanding calculations by massively parallel processing that is available using conventional graphics cards, e.g., using cuda or opencl. although modern graphics cards are able to provide superior peak performance, they also have high power consumption requirements (in order of hundreds of watts) and thus they are not suitable for micro-robotic platforms. therefore, as an alternative solution for parallel based and power-efficient computations, it is a more suitable to consider field-programmable gate array (fpga) technology to develop a custom architecture specifically designed for the particular computational task, which, in the end, can be very power and computationally efficient while also small in dimensions and cheap in development. however, fpga-based solutions need a significantly different approach for an efficient implementation of the particular algorithms than a conventional cpu. thus, the deployment time can be high compared to a gain from the implementation of a custom design computational architecture for the fpga. in this paper, we report our results on a comparison 8 http://dx.doi.org/10.14311/app.2015.1.0008 http://ojs.cvut.cz/ojs/index.php/app vol. 2/2015 on fpga based acceleration of image processing in mobile robotics of the selected image processing techniques suitable for embedded computation of the visual navigation task implemented on a conventional on-board platform and a dedicated solution based on fpga processing of the image data. in particular, we consider a detection of the salient points in the image. the salient points are image patterns which differs from their local neighbourhood and are expected to be reliably and repeatably detectable, preferably invariant to camera viewpoint changes. such features provide a mobile robot with a limited set of environmental anchor points which are then utilized for a vision-based navigation. feature based methods consist of three stages. the first stage is a detection of features to identify salient points in the image. then, for each detected feature its descriptor is calculated to describe the local image surrounding of the feature in order to distinguish individual features. the third stage is a process of establishing feature correspondences which is called feature matching. the matching is based on a comparison of the feature descriptors to determine whether the features correspond to the same salient object already detected in the environment. regarding the computational complexity of the feature detection, we can classify the features to artificial, like blobs or patterns, and naturally occurring in the environment. for the field robotics, natural landmarks are more important; however, artificial landmarks are much easier to detect. one of the foundational feature detectors is the scale-invariant feature transform (sift) algorithm [4], which is unfortunately computationally very demanding, and therefore, a speeded-up robust features (surf) algorithm has been proposed [5] to provide salient points with less computational requirements. although surf is less demanding than sift, it can be still computationally restrictive on small platforms. that is why researchers investigate other methods how to detect and describe salient objects in the environment by a computationally efficient algorithm such as the fast feature detector [6]. fast is widely adopted by robotic community for its low computational complexity. it has been deployed in several visual navigation methods, e.g., [7, 8], and it also provides a base for different feature extractors [9, 10]. following our intention to have a power and computationally efficient image processing available on a mobile robot, we consider fast as a suitable algorithm for visual navigation task computed on-board. therefore, we compare a performance of the fast feature extraction implemented on a conventional embedded platform with a cpu based on an arm architecture and a custom implementation of the fast detector on an fpga-based dedicated co-processor. the comparison indicates that even a computationally efficient feature extraction based on the fast algorithm can benefit from parallel fpga-based implementation that has a competitive processing time figure 1. hexapod walking robot platform and it is a more power efficient. the paper is organized as follows. an overview of the most related reports on enhanced computationally and power efficient vision-based navigation approaches based on fpga co-processor is presented in section 2. the proposed evaluation of the fpga-based image processing is considered in the context of a monocular vision-based teach-and-repeat autonomous navigation [11] that is briefly described in section 4 together with the main idea of the fast feature detection and the selected brief feature descriptor [12]. results on the evaluation of the computational burden reduction using an embedded platform of the hexapod walking robot (see figure 1) and fpga–based solution are presented in section 5. concluding remarks and future work is dedicated to conclusion in section 6. 2. related work this paper is focused on fpga-based implementations of computer vision techniques that are utilized in mobile robot navigation tasks. several approaches have been published and their authors reported improvements of the computational and power efficiency in vision-based navigation tasks by a dedicated implementation on fpga. probably one of the first fpga based implementation of the surf feature extraction has been introduced in [13], where an embedded module capable of image processing suitable for mobile robotics is presented. the module implements a surf feature extraction [14] from images with the resolution of 1024×768 pixels. the reported frame rate is 15 fps, which can be considered low in a comparison to the 24 fps gpu-based implementation of surf; however, the power consumption is only 6 watts. notice, the fpga implementation outperforms a pure cpu implementation running on an intel atom dual-core processor, which is able to process only a single frame per second. another fpga-based module for stereo image processing has been recently introduced by the eth 9 petr čížek, jan faigl acta polytechnica ctu proceedings computer vision and geometry group [15]. it is based on the fpga and arm cortex a9 quad-core cpu and calculates dense disparity images with the resolution of 752×480 pixels at the 60 frames per second. the disparity estimation relies on the semi global matching approach, which is computationally a very intensive task. the reported power consumption of the module is 5 watts. in [16], the same authors extend their module by implementing a reactive based collision avoidance method for mavs and tested it in an outdoor environment. authors of [17] presented a miniature module with a low-cost fpga and mcu for visual navigation of mavs. they utilize a reduced version of the ptam algorithm [8] (mapping maximum of 200 features due to memory limitations) for an estimation of the visual odometry. their approach is based on the fpga implementation of the fast features detection and brief [12] feature description. the mcu is utilized for visual odometry calculation and the whole system operates at 30 frames per second on images with the resolution of 160×120 pixels. in [18], authors consider the fpga to synchronize data from the imu and fast feature extraction from a camera stereo pair for a robust inertial assisted realtime visual slam. the reported update rate is about 20 frames per second for images with the resolution of 752×480 pixels. similar results with a slightly different approach are presented in [19]. an embedded fpga–based computer vision module has been presented in [20]. the proposed fpga architecture uses an efficient pipelining for the fast feature detection in a video stream with the resolution of 752×480 pixels at the frame rate of 60 frames per second, which is utilized in the visual teach–and– repeat navigation method. regarding the physical dimensions of the aforementioned modules, they are all based on system–on–chip (soc) solutions on fpga development boards which (in all cases) do not exceed 12 cm × 8 cm. the power consumption of these modules is less than 10 watts while all of them exhibit a real-time performance in the particular robotic navigation task. the soc architecture combines the advantages of the fpga with a regular cpu in order to reduce deployment costs and improve performance of the system. its main aspects are described in section 3. all of the discussed approaches seem to be a suitable choice for deployment on a micro-robotic platform. however, the most promising are the approaches ([17– 20]) based on the fast feature detector [6] because this detector is widely adopted by the robotic community due to its low computational complexity. hence, it represents a base for further methods. for example, it is a source of the parallel tracking and mapping (ptam) method [8] that can be considered as a visual monocular odometry (or slam – simultaneous localization and mapping) technique, also suitable for mavs, albeit the original ptam method was designed to be used in small augmented reality workspaces. the method relies on tracking and mapping of fast features for the 6dof position estimation in the environment. fast has been recently utilized in the semi-direct monocular visual odometry [7] in which fast features are tracked and used to build a map that is further used for a visual odometry estimation. the algorithm was tested on mav equipped with the odroid-u2 arm quad-core computer achieving computational speed of 50 frames per second. despite of the cpu implementation, the reported power consumption of the system is 10 watts, which is a competitive to the one of the first fpga module for the surf detection introduced in [13]. therefore, we consider the fast features detection on the arm–based computer and fpga–based implementation [20] in this evaluation study of the potential benefits of the parallel (fpga–based) implementation of the image processing for visual navigation. 3. processor centric design a combination of the fpga and cpu allows to accelerate a computer vision application and also allows to carry out more complex tasks by an improved system. the main idea of combining these two types of computational architectures is the processor centric system–on–chip co-design, which allows to exploit benefits of both architectures. generally, a cpu is a more suitable for general purpose computations and it is also a more easily programmable. however, a parallel nature of the fpga fabric makes it well suitable for accelerating demanding or repetitive computational operations performed by the cpu. besides, it is also suitable for online signal processing and sensory interfacing [21]. there are two principal ways how to incorporate both the fpga and cpu in a single embedded design. it is possible to have both of them soldered on the printed circuit board and utilize a communication channel like spi for a fast data transmission between them. however, much more efficient is to utilize the system-on-chip (soc) solution, where the cpu is a part of the fpga chip. the cpu can be either softcore or hardcore. the fpga fabric is extremely versatile, and therefore, it can implement even a cpu in its fabric, which is called a softcore cpu. on the other hand, manufacturers started to incorporate the cpu in the design of the chip to further exploit the fpga–cpu co-design possibilities. in that case, the cpu is etched into the silicon of the chip together with the fpga fabric and such a solution is then referenced as the hardcore cpu. nowadays hardcore processors are usually based on multi-core arm architecture and they are running at the units of ghz. in the case of the softcore processors, their speed is limited to around 200 mhz due to the fpga fabric limitations. the main advantage of the both hardcore and softcore processors is that they 10 vol. 2/2015 on fpga based acceleration of image processing in mobile robotics can be directly programmed in the c programming language. in addition, they can host a real-time operating system, which makes their programming for time critical applications even simpler. from the processor point of view, the fpga fabric can act either as a memory mapped slave device or it can be directly connected to the cpu core and accelerates the processor instructions. in that case, the instruction set of the cpu is extended by custom designed instructions. the main advantage of fpga–based soc systems is their versatility and reconfigurability which may be of a particular use in the field of mobile robotics. the programmer can choose components which assemble the system according to the needs of the particular application. the fpga resources allow to build both internal computational units and io communication interfaces, which can be directly connected to the main cpu. moreover, fpga always posses a lot of general purpose io pins which can be used for any communication not exceeding maximum frequency of the given fpga chip (usually about 300∼350 mhz) regardless the communication, which can be serial like spi and i2c or parallel. in addition, specialized hardcore bus endpoints for a high-speed communication are common integral parts of nowadays fpgas, e.g., gigahertz serial endpoints like pcie, sata or parallel dram interfaces. 4. bearing-only visual navigation the navigation algorithm used for the evaluation of implementations of the fast feature detector on the cpu and fpga is based on the teach-and-repeat navigation algorithm proposed in [11]. the navigation is based on tracking previously mapped visual features that are used for a bearing-only navigation. the approach relies on the relative localization provided by the odometry, which would eventually integrate unbounded position error over time. however, the approach considers the odometry only locally for traversing a short straight line segment along which detected visual landmarks are utilized to correct the robot heading and thus suppresses the odometric error. the corrections of the heading are based on a modus of the horizontal displacements of the tentative correspondences between previously mapped and the currently perceived visual features. the modus is found by a histogram voting as it is visualized in figure 2. the tentative correspondences are established using the fast feature detector and the brief feature descriptor [12] which are briefly described in the following subsections. 4.1. features from accelerated segment test the fast feature detector [6] belongs to the family of the so called appearance based detectors because it figure 2. surfnav navigation algorithm. matched features from the current and previously learned image. the corresponding navigation histogram is depicted at the bottom. searches the image for corner-like structures. the detector is optimized with respect to the computational complexity. the algorithm uses a set of comparisons between the center pixel p and pixels defined on the 7×7 neighbourhood using the circle in the image determined by bresenham’s circle algorithm, which is shown in figure 3. figure 3. fast feature detection. courtesy of [6]. at first, the pixels on the circle are labelled dark or bright depending on their relative brightness to the central pixel. the candidate pixel is considered as a feature if there are n contiguous bright or dark pixels in the circle. for n ≥ 12 it is possible to use a rapid rejection method for a faster outlier rejection which leads to a common setting of n = 12. however, the original paper [6] approved that the best repeatability is exhibited for the setting of n = 9. the corner score, which is necessary for the non-maxima suppression, is calculated as the sum of the absolute differences between the pixels in the contiguous arc and the central pixel. the fpga architecture presented in [20] uses efficient pipelining for the fast feature detection acceleration. the image data are processed as an online stream and the architecture performs all the steps of the algorithm, i.e., the corner detection, corner score calculation, and non-maxima suppression, in parallel as data are transmitted from the image sensor. the architecture also allows to use different values of n without an impact on the computational speed or used 11 petr čížek, jan faigl acta polytechnica ctu proceedings resources. 4.2. binary robust independent elementary features once features are detected, individual salient points are characterized by descriptors. the purpose of the descriptor is to describe the image neighbourhood of the point and thus characterize the salient object of the environment. in the proposed evaluation, the selected descriptor is the brief descriptor which stands to the binary feature descriptor [12]. it is based on pairwise intensity comparisons of pixels inside an image patch surrounding the located feature. these comparisons form a set of unique binary tests which are subsequently stored into a q-dimensional bit vector. the pairwise comparisons can be chosen either randomly or evolutionary, e.g., they can be trained by methods of reinforcement learning [22], which optimize the descriptor for the particular environment. typically used values of q are 64, 128, and 256 bits that correspond to the brief8, brief16, and brief32 variants of the feature descriptor, respectively. the descriptor similarity is evaluated using the hamming distance that computes how many bits of two given feature vectors are different. 5. evaluation the main motivation behind the utilisation of fpga– based systems in visual navigation tasks is a latency reduction in the robotic navigation system which is especially recognizable in experiments performed in dynamic or confined environments, which impose imminent threats to the mobile robotic platform [1, 23] and the reduction of the computational load thus power consumption of the mobile robot platforms. this section presents the results of the experimental evaluation of the impact of the fpga–based coprocessor utilization on the reduction of the computational burden of the feature extraction process in the monocular vision–based teach–and–repeat autonomous navigation. the particular parts of the whole navigation system under the evaluation are the feature extraction chain and the computationally most demanding parts of the navigation algorithm: the feature detection and description; features matching to the map previously created in the teach mode; construction of the navigational histogram; and determination of the robot heading correction based on the maximum peak in the histogram voting method. for the feature extraction the fast feature detector [6] is used with the setting of n = 12, while 256 bit long brief [12] (brief32) is utilized as the feature descriptor. the number of features is set to approx. 200 features per image and the pre-learned map in the navigation pipeline evaluation contains 200 features. the pure cpu based implementation running on the odroid u3 board [24] was compared to the (a) . outdoor urban env. (b) . indoor lab env. figure 4. testing environments. fpga–based soc implementation on terasic de0nano board [25]. in particular, the hardware and software used in the evaluation are as follows: odroid u3 – a small embedded micro-computer suitable for robotic applications. it features 1.7 ghz arm cortex a9 quad-core microprocessor (samsung exynos4412 prime) running the ubuntu 12.04 linux operating system. the attached camera is the mobius actioncam with the resolution of 640×480 with 60 fps. the implementation of the navigation algorithm was based on the open computer vision library [26] (opencv 2.4.9) implementations of the fast feature detector and brief32 descriptor. de0-nano board – an embedded module with the altera cyclone iv ep4ce22 fpga equipped with the aptina mt9v034 grayscale camera sensor with the global shutter and the resolution of 752×480 providing images with 60 fps. the implementation of the navigation algorithm follows the approach described in [20]. it utilizes the bare-metal programmed nios iie softcore processor clocked at 150 mhz for the feature description, matching, and histogram voting and a dedicated fpga–based parallel co-processor for the fast feature detection. the proposed evaluation consists of the focused examination of the feature detector and descriptor and examination of the performance of the whole navigation system. the tests were performed in field conditions both in outdoor urban (fig. 4a) and indoor lab (fig. 4b) environments. first, we evaluated the performance of the fpga– based and cpu–based implementations of the fast feature detector and computation of the brief descriptor. two criteria are considered in this evaluation: correctness of the fpga–based implementation and computational requirements. regarding the correctness of the fpga–based implementation, it provides identical results to the cpu– based counterpart for the detected features and also the same descriptors. this test was performed on artificially generated data in order to ensure the correctness of the results. the data consists of a checkerboard pattern with grayscale gradient which allows to detect various number of corners depending on the predefined threshold. concerning the computational requirements of the 12 vol. 2/2015 on fpga based acceleration of image processing in mobile robotics feature extractor, the odroid implementation needs (in average) 17.07 ms for approximately 200 fast feature detections with brief32 descriptors in an image with the resolution of 640×480 pixels. the de0nano implementation exhibits similar performance with the processing time of 16.91 ms for 200 feature detections and descriptions. the navigation stack performance benchmarking consists of the feature extraction, feature matching against the pre-learned map, and the histogram voting method to establish the heading correction of the robot. the achieved results are summarized in table 1. platform odroid u3 de0-nano cpu cores 4 1 cpu clock 1.7 ghz 150 mhz fpga 22320∗∗ fpga usage 28% feature extraction 17.07 ms 16.91 ms navigation pipeline 35.89 ms 24.38 ms power consumption 8.13 w 1.82 w ∗∗ the number of available logic elements. table 1. navigation pipeline processing results of odroid u3 and de0-nano soc platforms 5.1. discussion the results presented in table 1 indicate that the fpga–based soc approach does not significantly reduce the required time for feature extraction; however, the power consumption is reduced by 4.5 times magnitude in comparison to the purely cpu–based implementation. regarding the update rate of individual methods the fpga–based implementation is capable to process each other image in the 60 fps camera stream, which gives about 30 processed images per second while the cpu–based implementation can process 20 frames per second if we consider a uniform image retrieval; otherwise the update rate of the cpu–based implementation is 27 fps but images are dropped at non-deterministic way which leads to uneven distribution of information in time. the fast feature detector of the de0-nano implementation performs feature detection online on the stream of camera data, which implies that the image coordinates of all salient points in the image are known during the readout of a single image from the camera sensor. the feature description and matching to the pre-learned map is performed in an instant when the feature is detected in the camera stream. however, 256 bit long brief32 descriptor calculation together with matching to approx. 200 features from pre-learned map on the 150 mhz single core cpu makes it impossible to finish all the computations during the readout of one single image. therefore, each other frame in a 60 hz camera stream is skipped, which allows the algorithm to finish all the calculations in less than 32 ms during the readout of the next image. 6. conclusion in this paper, we consider a problem of decreasing the computational load of the embedded computational resources utilized in the vision-based navigation tasks. the presented results show that although the processing times of both the fpga–based and cpu– based implementations are almost similar most-likely due to the overall low complexity of the used feature extraction, the fpga–based system–on–chip design can significantly reduce the power consumption of the embedded processor in comparison to a purely cpu–based solution. in order to further verify and quantify the results, we plan to thoroughly benchmark each part of the visual navigation algorithm stack and incorporate the fpga-based image processing in a more complex navigation task of a visual slam, where the computational power of the fpga platform can be of potential benefit. acknowledgements the presented work has been supported by the czech science foundation (gačr) under research project no. 13-18316p. references [1] n. michael, d. mellinger, q. lindsey, v. kumar. the grasp multiple micro-uav testbed. robotics automation magazine, ieee 17(3):56–65, 2010. doi:10.1109/mra.2010.937855. 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[26] bradski, g. and kaebler, a. computer vision with the opencv library. o’reilly media, 2008. 14 http://dx.doi.org/10.1109/ismar.2007.4538852 http://dx.doi.org/10.1109/iccv.2011.6126542 http://dx.doi.org/10.1109/iccv.2011.6126544 http://dx.doi.org/10.1002/rob.20354 http://dx.doi.org/10.1007/978-3-642-15561-1_56 http://dx.doi.org/10.1007/s00138-014-0599-0 http://dx.doi.org/10.1016/j.cviu.2007.09.014 http://dx.doi.org/10.1109/iros.2014.6943263 http://dx.doi.org/10.1109/icra.2015.7138979 http://dx.doi.org/10.1109/icra.2014.6907625 http://dx.doi.org/10.1109/icra.2014.6906892 http://dx.doi.org/10.1109/icra.2014.6907232 http://dx.doi.org/10.3390/s140406247 http://dx.doi.org/10.1016/j.mechatronics.2013.11.006 http://www.hardkernel.com http://www.terasic.com.tw acta polytechnica ctu proceedings 2:8–14, 2015 1 introduction 2 related work 3 processor centric design 4 bearing-only visual navigation 4.1 features from accelerated segment test 4.2 binary robust independent elementary features 5 evaluation 5.1 discussion 6 conclusion acknowledgements references frascati workshop 2013 the tenth international workshop on multifrequency behaviour of high energy cosmic sources palermo, sicily, italy, may 27 – june 1, 2013 edited by franco giovannelli & lola sabau-graziati workshop on multifrequency behaviour of high energy cosmic sources palermo, sicily, italy may 27 june 1, 2013 organizing institutions istituto di astrofisica e planetologia spaziali iaps-inaf, roma, italy dpt de cargas utiles y ciencias del espacio, dcuce-inta madrid, spain e.o. hulburt center for space research, hca-nrl, washington d.c., usa max-planck institut fr extraterrestrische physik, mpe, garching, germany st. john’s college, sjc, annapolis md, usa institute für astronomie und astrophysik, karls eberhard, universität sand 1, tübingen, germany ascr astronomical institute, ondřejov, czech republic ctu czech technical university, prague, czech republic scientific organizing committee james howarth beall, hca-nrl & sjc franco giovannelli, inaf-iaps (chairperson) thomas boller, mpe lola sabau-graziati, inta-dcuce andrea santangelo, iaa, universitt tübingen rené hudec, ascr & ctu, prague, czech republic local organizing committee franco giovannelli, inaf-iaps (istituto di astrofisica e planetologia spaziali) (chairperson) daniela giovannini, cnr-ibcn (istituto di biologia cellulare e neurobiologia) paolo persi, inaf-iaps (istituto di astrofisica e planetologia spaziali) francesco reale, cnrisc (istituto dei sistemi complessi) ii foreword the workshop on multifrequency behaviour of high energy cosmic sources is a classical biennial meeting held in the same historical place for our workshops: the beautiful and wild island of vulcano. unfortunately, because of the eolian hotel is closed for repairs, this tenth edition of our workshop has been developed in palermo at the splendid hotel la torre. we are completely convinced that a deep discussion on the multifrequency behaviour of high energy cosmic sources, defined mostly by the physical processes rather than the types of objects, is the most powerful way for a better and faster development of our knowledge of the physics governing our universe. for this purpose, we invited distinguished colleagues representative the most important space– and ground–based experiments of the present generation. they painted the whole panorama on the experimental results and on their interpretation by using current models and/or developing new ideas for a better comprehension of the detected phenomena. during the discussion of a lot of new results, obtained along most of the electromagnetic spectrum, we have learned that the astrophysics of galactic sources is still extremely interesting and unavoidable. indeed it provides crucial information on the same physical processes occurring also in the extra– galactic sources, with obvious different scale factors. moreover, new results coming from very high energy γ-ray experiments have shown the richness — and its potential increase — of the sky at those energies having detected hundreds cosmic sources until few years ago completely unknown, but hopefully to be detected since the cosmic ray spectrum extends up to energies as high as ≥ 1020 ev. the fluxes of very high energy γ-rays are attenuated because of their interactions with the cosmic radio, microwave, infrared and optical radiation fields. measurements of the flux attenuation can then provide important information on the distribution of such fields. then, very high energy γ-ray astronomy is the most powerful tool for solving the problem about the origin of cosmic rays. many thanks to the authors, that accepted our reminders recalled at the beginning of the workshop, for keeping to schedule. however, in spite of the accurate respect of the dead line of a number of authors, we still suffer a delay in publishing these proceedings because of the laziness of a considerable part of other authors. in spite of this, these proceedings will appear roughly within one year from the workshop date. this is the tenth edition of the workshop (tenth if we consider the first historical one, held in vulcano in 1984), whose proceedings are published in the international czech journal ‘acta polytechnica’. we would like to thank all participants and especially the speakers for their active contributions in rendering this workshop updated with their talks, alive with their discussions, and friendly with their attitudes. particular thanks to mr francesco reale for his excellent assistance for informatics in roma, during the preparation of the workshop, and for his faultless assistance in palermo. a special thank to daniela giovannini for her help during the critical moments of the registration of participants. we are grateful to the pianist maèstra valentina usai, to the violinist maèstro alessandro perpich and to the actresses lisa colosimo and flavia giovannelli for their wonderful performance ”hic habitat felicitas: mozarterie from the kingdom behind”. iii many thanks to: the director of the istituto di astrofisica e planetologia spaziali of the istituto nazionale di astrofisica (iaps-inaf) (dr pietro ubertini); the caen s.p.a. (viareggio) who partially supported the organization of this workshop. particular thanks to the plan nacional de i+d+i of spain for partially supporting the publication of this book. finally, we would like to thank mr daniele inzerillo, the chef of the splendid hotel la torre, who delighted us with his creations during our stay and to the whole staff of the hotel for their professionalism and kindness. the editors franco giovannelli & lola sabau-graziati iv list of participants amati lorenzo , inaf–iasf, bologna, italy amati@iasfbo.inaf.it ambrosino filippo , la sapeinza university, roma, italy filippo.ambrosino@roma1.infn.it anderson gemma , university of southampton, uk gemma.anderson@hotmail.com arnaud monique , cea service d’astrophysique, gif sur yvette, saclay, france monique.arnaud@cea.fr aschenbach bernd , prv vaterstetten, germany bernd.aschenbach@t-online.de auriemma giulio , universit degli studi della basilicata, italy giulio.auriemma@cern.ch barret didier , irap, toulouse, france didier.barret@irap.omp.eu barrière nicolas , space sciences lab uc berkeley, ca, usa barriere@ssl.berkeley.edu beall james h. , ssd-nrl, washington dc, usa beall@sjca.edu behar ehud , technion. haifa, israel behar@physics.technion.ac.il beilicke matthias , washington university in st.louis, la, usa beilicke@physics.wustl.edu bisnovatyi-kogan gennady , space research institute, iki, moscow, russia gkogan@iki.rssi.ru v blay pere , gace–lpi–universidad de valencia, spain pere.blay@uv.es boller thomas , mpe, garching, germany bol@mpe.mpg.de bordas pol , iaat & isdc, tübingen, germany pol.bordas@uni-tuebingen.de buckley david , southern african large telescope, cape town, south africa dibnob@saao.ac.za castellina antonella , inaf–oato and infn, torino, italy castelli@to.infn.it castro cerón josé maŕıa , villanueva de la cañada, madrid, spain josemari@alumni.nd.edu colafrancesco sergio , school of physics wits university, johannesburg, south africa sergio.colafrancesco@wits.ac.za costamante luigi , dipartimento di fisica, università di perugia, italy luigic2011@gmail.com dar arnon , technion, israel institute of technology, haifa, israel arnon@physics.technion.ac.il de laurentis mariafelicia , dpt scienze fisiche, università ”federico ii”, napoli, italy felicia@na.infn.it de ugarte postigo antonio , iaa–csic, granada, spain adeugarte@gmai.com della valle massimo , inaf–osservatorio astronomico di capodimonte, napoli, italy dellavalle@na.astro.it di sciascio giuseppe , infn–sezione di roma tor vergata, italy disciascio@roma2.infn.it vi ebisawa ken , jaxa/isas, sagamihara, japan ebisawa@isas.jaxa.jp moshe elitzur , university of kentucky, ky, usa moshe@pa.uky.edu fargion daniele , dipartimento di fisica, università ”la sapienza” di roma, italy daniele.fargion@roma1.infn,it federici memmo , inaf–iaps, roma, italy memmo.federici@iaps.inaf.it georganopoulos markos , university of maryland, baltimore county, nasa–gsfc, baltimore, md, usa georgano@umbc.edu giovannelli franco , inaf–iaps, roma, italy franco.giovannelli@iaps.inaf.it gómez de castro ana inés , universidad complutense de madrid, spain aig@mat.ucm.es guainazzi matteo , european space agency, villanueva de la cañada, spain matteo.guainazzi@sciops.esa.int harms benjamin , university of alabama, al, usa bharms@bama.ua.edu hudec rené , astronomical institute academy of science, ondřejov & ctu prague, czech republic rene.hudec@gmail.com iglesias-groth susana , instituto de astrof́ısica de canarias, la laguna, spain sigroth@iac.es katsuda satoru , riken, wako, saitama, japan satoru.katsuda@riken.jp vii kreykenbohm ingo , dr karl remeis observatory & ecap, bamberg, germany ingo.kreykenbohm@sternwarte.uni-erlangen.de krumpe mirko , eso, garching, germany mkrumpe@ucsd.edu kundt wolfgang , argelander institute of bonn university, germany wkundt@astro.uni-bonn.de lott benoit , cenbg, gradignan, france lott@cenbg.in2p3.fr maeda keiichi , kavli ipmu, university of tokyo, japan keiichi.maeda@ipmu.jp marshall herman , mit, cambridge, ma, usa hermanm@space.mit.edu martino bruno luigi , cnr–iasi (istituto analisi dei sistemi ed informatica), roma, italy brunolmartino@gmail.com meintjes pieter , university of the free state, bloemfontein, south africa meintjpj@ufs.ac.za meli athina , university of gent, dept. of physics and astronomy, gent, belgium ameli@phys.uoa.gr merafina marco , dipartimento di fisica università ”la sapienza” di roma, italy marco.merafina@roma1.infn.it milano leopoldo , dipartimento di scienze fisiche, università ”federico ii”, napoli, italy milano@na.infn.it morihana kumiko , institute of physical and chemical reserch (riken), wako, saitama, japan morihana@crab.riken.jp viii morselli aldo , infn roma tor vergata, roma, italy aldo.morselli@roma2.infn.it motch christian , cnrs–observatoire astronomique de strasbourg, france christian.motch@unistra.fr muñoz-tuñon casiana , instituto de astrof́ısica de canarias, la laguna, spain cmt@iac.es nebot ada , observatoire astronomique de strasbourg, france ada.nebot@astro.unistra.fr nozawa takaya , kavli ipmu, university of tokyo, kashiwa, japan takaya.nozawa@ipmu.jp orlando salvatore , inaf–osservatorio astronomico di palermo, italy orlando@astropa.inaf.it panagia nino , space telescope science institute, baltimore, maryland, usa panagia@stsci.edu parisi pietro , inaf–iaps, roma, italy pietro.parisi@iaps.inaf.it persi paolo , inaf–iaps, roma, italy paolo.persi@iaps.inaf.it perucho manel , dpt d’astronomı́a i astrof́ısica, universitat de valència, spain manel.perucho@uv.es piro luigi , inaf–iaps, roma, italy luigi.piro@iaps.inaf.it pittori carlotta , inaf–oar and asdc, frascati, italy pittori@asdc.asi.it reale francesco , cnr–isc, roma, italy francesco.reale@sic.rm.cnr.it ix rebolo rafael , instituto de astrof́ısica de canarias, la laguna, spain rrl@iac.es regis marco , università di torino and infn–torino, italy regis.mrc@gmail.com reimer anita , universität innsbruck, austria anita.reimer@uibk.ac.at ribó marc , universitat de barcelona, spain mribo@am.ub.es rodŕıguez fŕıas , space and astroparticle group, uah–madrid, alcal de henares, spain dolores.frias@gmail.com rosinska dorota , kepler institute of astronomy, university of zielona gora, poland dorota@astro.ia.uz.zgora.pl rubino-martin josé alberto , instituto de astrof́ısica de canarias, la laguna, spain jalberto@iac.es sabau-graziati maŕıa dolores , inta–división de cargas utiles y ciencias del espacio, torrejón de ardoz, madrid, spain sabaumd@inta.es sanchez-portal miguel , herschel science centre, esac/european space agency, villanueva de la cañada, spain miguel.sanchez@sciops.esa.int sani eleonora , inaf-oa arcetri, firenze, italy sani@arcetri.astro.it santangelo andrea , institute of astronomy and astrophysics, kepler center, university of tübingen, germany andrea.santangelo@uni-tuebingen.de sasaki manami , institute of astronomy and astrophysics, kepler center, university of tübingen, germany sasaki@astro.uni-tuebingen.de x schartel norbert , esa/xmm–newton soc, villanueva de la cañada, madrid, spain norbert.schartel@sciops.esa.int sikora marek , pan–nicolaus copernicus astronomical center, warszawa, poland sikora@camk.edu.pl šimon vojtěch , astronomical institute academy of science, ondřejov, czech republic vojtech.simon@gmail.com van soelen brian , university of the free state, bloemfontein, south africa vansoelenb@ufs.ac.za spurio maurizio , university of bologna and infn–bologna, italy spurio@bo.infn.it stanev todor , university of delaware, newark, de, usa stanev@bartol.udel.edu tluczykont martin , university of hamburg, germany tluczykont@gmail.com tornambé amedeo , inaf–roma observatory, monteprozio catone, italy tornambe@oa-teramo.inaf.it troja eleonora , nasa–gsfc/cresst, greenbelt, md, usa eleonora.troja@nasa.gov tsuru takeshi , physics dpt, university of kyoto, japan tsuru@cr.scphys.kyoto-u.ac.jp ubertini pietro , inaf–iaps, roma, italy pietro.ubertini@iaps.inaf.it vitantoni daniele , dipartimento di fisica università ”la sapienza” di roma, italy daniele.vitantoni@roma1.infn.it walter roland , isdc, university of geneva, versoix, switzerland roland.walter@unige.ch xi yoon sung-chul , university of bonn, germany astroyoon@gmail.com zió lkowski janusz , pan–nicolaus copernicus astronomical center, warszawa, poland jz@camk.edu.pl xii acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0058 acta polytechnica ctu proceedings 7:58–63, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app experimental, numerical and analytical investigations of wind-induced net pressures for industrial buildings with envelope porosities vanessa saubke∗, rüdiger höffer ruhr-universität bochum, universitätsstraße 150, 44801 bochum, germany ∗ corresponding author: vanessa.saubke@rub.de abstract. the magnitude and the spatial distribution of wind-induced net pressures (external and internal) on buildings are frequently discussed among research communities and construction industries. this paper deals with this topic based on a case study about an industrial building in denmark, which was damaged due to the wind impact during a storm when a large part of the roof covering was blown off. in order to detect the reason for the damage the wind-induced loads were studied by i) wind tunnel experiments on the external pressures due to different wind directions, ii) analytical investigations of internal pressure due to envelope porosities and planned openings and iii) numerical analyses for the internal and the external pressure. the reynolds averaged navier-stokes (rans) method is employed to build a numerical model. the experimental, analytical and numerical results are compared with the indicated characteristic loads from the eurocode [1]. keywords: net pressure, internal pressure, industrial building, eurocode. 1. introduction the storm "christian" caused a lot of significant damages in northern europe in october 2013, including also failure of supporting structures of buildings. especially in denmark high wind velocities were measured. according to the danish meteorological service local wind peaks of 53.5 m/s were listed, which were the highest values ever measured in denmark. the wind velocity distribution for the maximum values for this day is given in figure 1 (b). the diagram in figure 1 (c) shows the data of the two measurement stations nearby the building which is considered here. the peaks of the wind velocity at 1 p.m. and at 3 p.m. are clearly visible. figure 1. (a) cardinal points (google earth [2], modified), (b) distribution of the peak wind velocity in denmark during hurricane "christian" in october 2013 (danmark meteorologiske institut [3], modified) and (c) measurements of the wind velocities at stations near to the building. at 3.15 p.m. the industrial building was damaged due to the wind impact. a large part of the roof structure breaks off and leads to an extended hole in the roof construction (see fig. 3 (a)). the debris were blown over the building and damaged also the leeward building (see fig. 2). the wind direction was west-southwest (for the cardinal points see fig. 1 (a)). figure 2. pictures from a security camera taken during the storm in 2013, the roof failure is visible. the damage started at the edge of the roof where the foil peeled off. this led to a deformation of the parapet wall (see fig. 3 (d)). approximately 7.5 % of the roof construction was completely blown off, additional 6 % of the roof foil was torn off and the trapezoidal sheets were folded and buckled (see fig. 3 (b)). in total more than 10 % of the roof construction was destroyed. futhermore this caused a damage at the sprinkler system and the leaking water destroyed a big part of the stored goods. the impact of the wind load was huge so that also the girders of the supporting roof construction were deformed (see fig. 3 (c)). 58 http://dx.doi.org/10.14311/app.2017.7.0058 http://ojs.cvut.cz/ojs/index.php/app vol. 7/2017 exp., num. and anal. investigations of wind-induced net pressures figure 3. qualitative description of typical damages: (a) partically opened roof, (b) buckled sheets, (c) bent girder and (d) deformed parapet. the considered building is located in the east part of denmark. it is situated at the west of a complex of three storage buildings of the same type. each building is about 135 m long, 55 m wide and 38 m tall. the shelfs for the stored goods are part of the supporting steel construction which consists of a regular framework of stiffening frames (see fig. 4). this main structure is covered by a sandwich-element facade. figure 4. example of a warehouse building under construction (google maps [2]). the roof consists of supporting girders, trapezoidal sheets, mineral insulating panels and a roof foil. the sheets are connected to the supporting girders by screws and the foil is fixed by spikes. for the sandwichelement facade a connection type with unsealed joints was used. after lange and rädel [4] this specific joint construction can lead to a leakage of the building walls. for the consideration of this leakage an effective joint was estimated as 3.5 mm (for investigations on the leakage of joint see kuhnhenne [5]). with this information the general porosity φ, the relation of the area of the openings to the area of the surfaces, was calculated: φ = ∑ a′∑ a = 0.0026 = 0.26%. (1) at the southern facade the gates for the delivery of the goods are located behind an antecedent flat hall. if the gates are not closed the total area of openings is 61.43 m2. 2. materials and methods 2.1. wind loads after 1991-1-4 after the eurocode external and internal pressures due to wind impact are taken into account [1]. a superposition of both leads to the net pressure. the definition of the signs of this values are given in figure 5. figure 5. three typical cases for the internal pressure (cook [6], modified). the code defines the wind load we,i as multiplication of the peak velocity pressure and a pressure coefficient: we = qp · cpe and wi = qp · cpi. (2) the peak velocity pressure qp is influenced by different factors like the terrain category, the building height and the wind zone. the external pressure coefficient cpe is influenced by the shape of a building and the internal pressure coefficient cpi by the distribution of the openings over the four faces of the building. in the following investigations pressure coefficients are considered and compared. for this purpose the external pressure coefficients for the roof of this building are determined in table 2. figure 6. distribution of the pressure coefficients for a flat roof with (a) wind direction on the short side and (b) wind direction on the long side. regarding the flow around a rectangular cube of a certain height (see hucho [7]) the code estimation of 59 vanessa saubke, rüdiger höffer acta polytechnica ctu proceedings the distribution of the pressure coefficients is given in figure 6. the distribution depends on the dimensions of the building and has to be estimated for every building and every wind direction individually due to the regulations. the cpe,1 values should be used for loaded areas of less than 1 m2 and the cpe,10 values for loaded areas of more than 10 m2 with the possibility of a logarithmic interpolatin for intermediate values. the internal pressure can be calculated according to two different regulations: (1.) for homogeneously distributed openings the pressure coefficient can be determined from a diagram by calculating the opening ratio µ, which is the relation from the area of the openings in the suction region divided by the area of all openings: µ = ∑ area of openings with cpe ≤ 0∑ area of all openings (3) (2.) a face with an area of openings that is more than twice the area of the sum of the openings in the remaining faces is considerd as a dominant face. • the internal pressure coefficient can be calculated with the following equation: cpi = 0.75 · cpe. (4) • if the area is more than three times the remaining openings then it is calculated with the following equation: cpi = 0.9 · cpe. (5) the considered building has firstly a general porosity because of the leakage due to the facade-elements. secondly it has large openings for the delivery of the stored goods at the short face where the open flat building is located. it is not known yet if openings were open or closed during the storm. therefore, three different situations for two wind directions are considered. these different cases are explained in table 1. the results for the internal pressure coefficients for these six cases are listed in the table 3. case windward face porosity delivery gates 1 x 2 short x x 3 x 4 x 5 long x x 6 x table 1. description of the six load cases. 2.2. experimental tests wind tunnel tests were performed at the boundary layer wind tunnel at ruhr-universität bochum to build up a reference data-base of wind-induced loads on the structure for specifically chosen spots of the building envelope, especially on the parts damaged during the storm event. the focus of the measurements was set on the roof construction which failed (see fig. 7 (a)). the effect of the parapet wall was neglected due to the small size in relation to the building. this leads to results on the safe side. figure 7. (a) positions of the pressure measurement points and (b) the principal set-up of the model. the tests were performed in a geometrical scale of 1:300 for different wind directions from southwest to northwest. the building was investigated as a (i) single standing, isolated building and (ii) in a group arrangement with the neighboring buildings (see fig. 7 (b) for the set-up). the evaluated cpe values represent the 78 % fractiles of the analyzed measurement data. the pressures are measured over a point-like averaging area which represents an area smaller than 1 m2 in full scale. the minimum values from the flow direction on the long face and of all measured directions for every zone are listed in table 2. figure 8. (a) the minimal cpe values of the flow direction west (on long face) and (b) of all measured flow directions. 2.3. numerical simulations for the numerical investigations a cfd method applying finite volumes and the rans method with the standard k-ε-model is used. the applied inlet velocity profile was introduced by richards and hoxey [8] in 1993 and is commonly used for this method. effects of building interferences were neglected by running all simulations with a single building. figure 9. (a) idealization of the joints and (b) idealization of the openings. 60 vol. 7/2017 exp., num. and anal. investigations of wind-induced net pressures because a simulation of all explicit openings and joints would lead to an extremely high number of volume elements the openings were idealized. the general porosity of the joints was considered with four explicit idealized joints distributed over the height (see fig. 9, left). the openings of the delivery gates were also idealized as one large opening with the same area which is located in the center of gravity of all gates (see fig. 9, right). figure 10. numerical results for the internal pressure coefficients cpi: (a) case 1, (b) case 2, (c) case 3, (d) case 4, (e) case 5 and (f) case 6. figure 11. numerical results of the external pressure coefficients of the roof for (a) flow on the short side and (b) flow on the long side. geometrical models and meshes were generated for all six cases (see table 1) with approximately three million volume elements per case. the distribution of the external pressure coefficients is pictured in figure 11. the maximum values for every zone are listed in table 2. the internal pressure coefficients for the six different cases are plotted in figure 10 and numbered in table 3. 2.4. analytical calculations an analytical investigation is performed for the estimation of the internal pressure. as cook [6] 1990 already described, the internal pressure pi depends on the external pressure pe at the openings a′. it is defined as the balance between the inflow and outflow of the building (see also fig. 5 (c)): inflow∑ ( a′ (pe − pi) 1 2 ) = outflow∑ ( a′ (pi − pe) 1 2 ) . (6) the equation cannot be solved directly but iteratively with an estimated value for the internal pressure. the left-hand and right-hand side of equation 6 are not fixed during the iteration process, because an outflow can become an inflow and vice versa. figure 12. distribution of the external pressure coefficients from a wind tunnel test for (a) the wind direction on the short face and (b) the wind direction on the long face (tpu aerodynamic database [9], modified). to calculate the internal pressure analytically a distribution of the external pressure is needed. because the performed wind tunnel tests are putting the focus on the damaged area of the roof construction, complete roof and wall distributions of external pressures have not been measured and are missing for analytical calculations of internal pressures. therefore mean values of external pressure coefficients from wind tunnel tests of a building with similar proportional dimensions from the tpu aerodynamic database [9] were used (see fig. 12). because the building from the database was smaller than the original one, the area of the openings was scaled down whereas the opening ratio µ stayed unchanged. in this scale the distributions of the pressure coefficients were evaluated and the area of the different pressure coefficients calculated. in order to maintain the comparability the same idealized opening of the delivery gates like those for the numerical investigations in section 2.3 were used. for the joints a general porosity of 0.26 % was considered. the internal pressure was calculated for all six cases as given in table 1 after cook’s method, [6]. the results are listed in table 3. 61 vanessa saubke, rüdiger höffer acta polytechnica ctu proceedings 3. results the results of the wind tunnel investigations correspond relatively good to the required values of the eurocode, for example the eurocode requires a value of cpe = 2.2 for the zone f and the wind tunnel results leads to the highest value of cpe = 2.14 considering all investigated directions. the results are compared to the cpe,1 values although the area of the measurement points in the experiments correspond to an area of smaller 1 m2 in full scale. the normative values of zone f and g suit to the minimum values of the testing results for all directions while the normative value of zone h fits better to the averaged value. but as one can see in figure 8 the values of this zone have a certain variation, they decrease in direction to the leeward side of the building. therefore, it is obvious that a design for the maximum value would not be economic, but one should be aware of the possibility that higher values can occur. zone f g h eurocode1) -2.2 -1.8 -1.2 windtunnel test (long face) -1.64 -1.34 -1.43 (-1.192)) windtunnel test (all directions) -2.14 -1.84 -1.63 (-1.292)) numerical simulation (case 1-3) -1.19 -1.11 -1.01 numercial simulation (case 4-6) -1.18 -1.13 -1.03 table 2. comparison of the external pressure coefficients cpe for the roof construction. 1)cpe,1 values in order to maintain comparability 2)averaged value of zone h the cpe values of the wind tunnel tests for the wind on the long face can be compared to the numerical results of cases 4 to 6. it should also be taken into account that the rans method does not lead to peak values and deliver average value only. the distribution of the external pressure coefficient shows a satisfactory similarity to the experimentally determined distribution from the windtunnel tests. but rans underestimates the external pressure in the separation area because the turbulence is modelled mathematically and local instationary vortices are neglected. the values of the numerical results are between 72 % to 84 % of the values of the wind tunnel test. the investigations of the internal pressure coefficients lead to different results for the six cases. the magnitude of the values are similar, in most of the cases, like case 1, 3 and 6, the eurocode overestimates the values and is on the safe side, but in case 5 it underestimates the internal pressure in comparison to the analytical solution. case 1 2 3 4 5 6 windward face short long porosity x x x x delivery gates x x x x eurocode -0.30 0.34 0.64 -0.03 -0.33 -0.83 numerical simulation -0.21 -0.12 0.52 -0.24 -0.31 -0.63 analytical calculation -0.20 0.34 0.59 -0.23 -0.48 -0.62 table 3. comparison of the internal pressure coefficients cpi for the six considered load cases. in case 2 the numerical analysis lead to a complete different value than the results of the analytical solution, which seems to fit perfectly to the value of the eurocode. in a further investigation, e.g. with the les-method, the numerical results should be checked, but it is sure, that this is connected to the position of the opening. if the position of the opening in the analytical calculation is changed to a higher position in the middle of the face (see fig. 13), the value increases from cpi = 34 to cpi = 0.45. figure 13. changed position of the opening at the windward face (tpu aerodynamic database [9], modified). also in some additional numerical investigations on a 1m x 1m x 1m cube, where the position of the openings over the height was changed, the same behaviour was determined (see fig. 14). this shows that the internal pressure reacts quite sensitive to the position of the openings, especially for openings in the windward side. figure 14. investigation on a 1m x 1m x 1m cube due to the position of the opening: (a) opening at the bottom, (b) opening in the middle and (c) opening at the top. in case 4 the eurocode diagram leads to a value of nearly zero (with µ = 0.63 in fig. 15) in contrast to the numerical and analytical solution, which leads to good corresponding results of -0.24 and -0.23. in 62 vol. 7/2017 exp., num. and anal. investigations of wind-induced net pressures the old german code near to zero values were avoided. in the range of the diagram where the value leads to zero one has to consider two values (0.2 and -0.3) on the safe side (see the red square in fig. 15 (b)). figure 15. diagram for the cpi values: (a) eurocode [1] and (b) the previous code din 1055 [10]. 4. conclusions the results show, that the regulation of the internal pressure for a dominant face is conservative for dimensioning a building (see regulation (2.) in section 2.1). the regulation for homogeneously distributed openings however seems to falsify the internal pressure (see regulation (1.) in section 2.1). as well for very homogeneously distributed openings, like a general porosity, the regulation (1.) does not work properly, like in case 4. also in case 5 the value is underestimated in comparison to the analytical value. the normative din en 1991-1-4 [1] offers the opportunity to use the fixed values of +0.2 and -0.3, if it is not possible or not justifiable to estimate a µ. these values seems to represent an underestimation of the effects of the internal pressures as one can understand from the results of the investigations for cpi ranging from +0.59 to -0.63. this apparent load underestimation through the quoted simplified code regulation does not necessarily lead to damages of the structure as it can be assumed to be based on experiences and sound practice requirements which are included into code regulations. however, such configuration can be insecure in connection with a certain systematical underestimation of external pressures after specific design regulation for trapezoidal sheets. for example, the german din 18807-3 [11] considers the higher pressures at the edge of the roof (zone f and g) just for the design of the screw connections; for the design of the sheets the high suction in these zones is neglected, which leads to an underestimation of the external pressure at the edge of the roof. together with the simplified eurocode regulation as described above this can result into a safety relevant lack of net design pressures. the research on the topic of the internal pressure should be continued to validate the results. to perform some additional wind tunnel tests on buildings with different proportions in combination with numerical simulations would be useful. for the numerical simulations some further methods should be used to improve the results. the aim would be to find a stable model that leads to good results for the different proportions so that it can be used as a tool to check and improve the regulation of the code. list of symbols a area of the faces [m2] a′ area of the openings [m2] cpe external pressure coefficient cpi internal pressure coefficient pe external pressure [n/mm2] pi internal pressure [n/mm2] we external pressure (eurocode) [n/mm2] wi internal pressure (eurocode) [n/mm2] µ opening ratio φ general porosity references [1] e. c. for standardization. en 1991-1-4 eurocode 1: actions on structures part 1-4: general actions wind actions. 2010. [2] google maps. panoramio, 2007. [3] danmark meteorologiske institut (dmi). orkan satte danmarksrekord i vind se kortene, 2013. [4] j. lange, f. rädel. die fugendichtigkeit von sandwichelementkonstruktionen wasserund luftdichtigkeit in längsfugen und fensteranschlussfugen. in festschrift zum 60. geburtstag von gerhard hanswille, heft 20. institut für konstruktiven ingenieurbau, bergische universität wuppertal, 2011. [5] m. kuhnhenne. energetische qualität von gebäudehüllen in stahl-sandwichbauweise. dissertation, rheinisch-westfälische technische hochschule aachen, fakultät für bauingenieurwesen, 2009. [6] n. j. cook. the designer’s guide to wind loading of building structures part 2: static structures. butterworths, 1990. [7] w.-h. hucho. aerodynamik der stumpfen körper. vieweg+teubner, 2nd edn., 2011. [8] p. richards, r. hoxey. appropriate boundary conditions for computational wind engineering models using the k-ε turbulence model. journal of wind engineering and industrial aerodynamics 46-47:145–153, 1993. [9] t. p. u. aerodynamic database. database of isolated low-rise building without eaves. http://www.wind.arch.t-kougei.ac.jp/info_ center/windpressure/lowrise/mainpage.html. [10] din 1055-4 action on structures part 4: wind loads. din deutsches institut für normung e.v., 2005. [11] din 18807-3 trapezoidal sheeting in buildings; steel trapezoidal sheeting; strength analysis, structural design. din deutsches institut für normung e.v., 1987. 63 http://www.wind.arch.t-kougei.ac.jp/info_center/windpressure/lowrise/mainpage.html http://www.wind.arch.t-kougei.ac.jp/info_center/windpressure/lowrise/mainpage.html acta polytechnica ctu proceedings 7:58–63, 2017 1 introduction 2 materials and methods 2.1 wind loads after 1991-1-4 2.2 experimental tests 2.3 numerical simulations 2.4 analytical calculations 3 results 4 conclusions list of symbols references acta polytechnica ctu proceedings doi:10.14311/app.2016.6.0011 acta polytechnica ctu proceedings 6:11–17, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app using robot operating system for autonomous control of robots in eurobot, erc and robotour competitions grzegorz granosik∗, kacper andrzejczak, mateusz kujawinski, rafal bonecki, lukasz chlebowicz, błażej krysztofiak, konrad mirecki, marek gawryszewski lodz university of technology, stefanowskiego 18/22, lodz, poland ∗ corresponding author: granosik@p.lodz.pl abstract. this paper presents application of the navigation stack available in robot operating system as a basis for the autonomous control of the mobile robots developed for a few different robot competitions. we present three case studies. keywords: ros, navigation, robot, erc, eurobot. 1. introduction students from the scientific association for robotic research skaner [1] at the lodz university of technology (tul) have been competing in various international robotic contests (e.g. eurobot, robot challenge, robotour, sumo challenge, european rover challenge) for several years. they have been working in separate teams focused on robot construction, electronics and control specific for the contest. this year we have decided to join forces and use robot operating system (ros) as a common software platform to build autonomous mobile robots for various competitions. ros has been introduced in automatic control and robotics curricula at tul a few years ago in a very smooth way [2]: (1) by modeling various robots in our web-based application mymodelrobot in order to learn xml syntax and robot structure used in gazebo and ros, and (2) by utilizing rosserial and rosserial_arduino to gather sensory data and control small mobile robots. that way the interest in ros started to grow and we have learned how to use all advantages of this system effectively, and specifically: • a multitude of tools and libraries that were created around ros to rapidly prototype the high and middle level of control system for mobile robots. • its modern software architecture to easily connect different applications and devices. we could build systems where most of processes work in parallel and on different machines without building multithreading or networking procedures by ourselves. • its “thin“ ideology — in some cases programs did not need to be highly integrated with ros. • we could reuse many tools created outside this system by adding only small parts bridging them to the ros. documentation and support provided by books [3], [4], tutorials online, and ros forum [5]. • ease of debugging, visualization and logging by using several tools: rxgraph to see system‘s state graph, rxplot to plot different variables online, rviz to visualize the whole robot and its sensors readings, or to archive and replay all data. • free and open access based on straightforward licenses [6]. we could use many libraries, adapt them to our needs and compile by ourselves. the most complex problem all skaner teams have been facing is an autonomous navigation of a robot. in the further part of this paper we will present our approach to use ros to solve this problem in the case of three robots built for different contests: eurobot (robot husarz), european rover challenge (raptors rover) and robotour (quadron and raptors rover). these robots have different constructions, different kinematics and control systems. further description starts with application of navigation stack at the husarz robot then the specific adaptations to other robots are presented. 2. ros navigation stack the husarz system (composed of two robots, shown in figure 1) was developed by our skaner team for eurobot competitions. each edition of eurobot. has different main topic, in year 2016 it was beachbot and the tasks symbolized enjoying time on the beach. • the flags — robots must close doors of a shed to rise the flag. • the sea fishing — robots must catch plastic fishes from a aquarium with water and put them in a net. • the sand castle — robots must build a sand castle from several elements (cubes, cylinders, cones). • the sea shell — shells are symbolized by round discs, and they are in five configurations on the playing area. robot must take shells to the starting place. 11 http://dx.doi.org/10.14311/app.2016.6.0011 http://ojs.cvut.cz/ojs/index.php/app g. granosik, k. andrzejczak, m. kujawinski et al. acta polytechnica ctu proceedings figure 1. husarz robots at the eurobot competitions • hide in the shade — this is the funny action, after 90 seconds (the end of a match) robot must rise a beach umbrella to get extra points. each team is allowed to have up to two robots on the playing area. robots must be fully autonomous during a match (no interference with human operator) and avoid crashes with opponents (referee could give negative points for a crash). we have built two differential drive robots, the bigger one has wheels while the smaller uses tracks. they share the control system schematically shown in figure 2. we can clearly see that this control system is organized according to the ros navigation stack presented in figure 3 and in [7]. we used this approach to take advantage of the provided programs (or nodes in ros nomenclature, see figure 3): planner/navigator (move_base) and the adaptive monte carlo localization (amcl). on the other hand we had to provide exact structure of the control system and format of all topics (messages being sent between nodes). the high-level controller knows all tasks (required by competitions) and can choose which robot will perform the specific one. these tasks are provided in the script (in the form of sentences). every sentence is composed of several stages. the first one always uses the move_base node to set the robot in an appropriate position to run the task. next steps depend on the type of the task (for example: sending order with a linear velocity directly to the robot to move something on the playing area, or sending order to the manipulators to pick up something, or some combination of such orders). in the application prepared for eurobot 2016 contest we have specified four global tasks: move pads (1), close doors (2), pick up and bring the sand castle to point area (3) and catch the fish (4). tasks 1 and 2 could be performed by either robot, while 3 and 4 could be made only by the bigger one. at the beginning of a match, the big robot has got three tasks to do, the small one has one regular task and an extra task to be performed after the end of the match (opening an umbrella after 90 seconds). figure 2. control sytem of the husarz robot let‘s look closer on the sea fishing task. always in a first step robot uses move_base planner to get to the point nearby the task execution (close to the aquarium in this case). after the robot gets to the right place (with the right orientation) the main controller sends order to the low-level controller to deploy a manipulator (fishing boom). in the next step the main controller sends the value of linear velocity directly to the low-level controller (which control drivers). the main controller continuously analyzes position read from /odom topic. when the robot reaches the other end of aquarium the main controller sends order to stop, then to return (sends negative value of linear velocity). after that, the controller repeats the above operation one more to go along the wall. on the next run robot goes further to reach a net and leave fishes (appropriate order sent to the manipulator) to score points. each step has got a time limit. after reaching a time limit before completing a step, the program has to choose either to repeat the step one more time or tag this task failed and proceed to the next task. the main controller counts how many times it sent specific orders. if this value reaches the limit, the program will move to another task. the high-level controller node publishes the /move_base_simple/goal topic containing information about position and orientation of the target point in the standard format of geometry_msgs/posestamped message. this is one of the inputs of the planner — which do all hard work of finding safe path on the playing area and avoiding obstacles — and further publishes /cmd_vel topic containing reference linear and angular velocities for the mobile robot in the format: geometry_msgs/twist. this topic is subscribed by the node which realizes the low level controller and which is located on the arduino board controlling motor drivers. the low-level controller also publishes an odometry information. planer and navigator hidden in the move_base node has to be configured before use, we have to set robot‘s size, maximum and minimum angular and linear velocities, and accelerations, planner‘s frequency, map 12 vol. 6/2016 using robot operating system for autonomous control of robots figure 3. standard ros navigation stack [7]. figure 4. building the navigation map (middle) based on the geometry of playing board (up) of eurobot competitions, or based on several scans taken on the real board (down) parameters etc. if the robot has different kinematics one can use another ros planer leaving the operating principles of the navigation stack unchanged. the most important parameters in case of eurobot contest were pdist/_scale and gdist_scale: pdist_scale — the relative importance of sticking to the global path as opposed to getting to the goal. gdist_scale — the relative importance of getting to the goal rather than sticking to the global path. by trying different values we have tuned these values pdist_scale = 0.75, and gdist_scale = 1. our robot do not stick to global path but tries to get to goals in a smooth way. when pdist_scale is larger than gdist_scale the robot drives only trough global path (often stops and sets up orientation) and wastes more time (match lasts only 90 seconds). the other important information is the map which can be created directly using external sensors (e.g. laser scanner) or prepared in any graphics software. the format of /map topic is also standardized by map.pgm (portable greymap) file. in case of the eurobot competitions we had to prepare the map based on geometric data describing playing area and a few criterions. the elements on the playing board are divided into three groups: • fixed (walls), • movable untouchable (opponent robots), • movable touchable (playing elements). only fixed elements are included in the initial map, as shown in figure 4 (middle). this map is further used by simultaneous localization and mapping (slam) method. robot localizes itself and creates cost maps in every step of the control. necessary sensor data are delivered by hokuyo laser scanner in message sensor_msgs/laserscan — visible as white dots in figure 4 (down). these scans together with a laser-based map and transform messages are used by amcl node to produce pose estimates alternative to dead reckoning. laser scans are also used for obstacle avoidance in the navigator — /local_costmap. based on the map, current scans and the next target point (provided by the high-level controller), the planner is generating reference path for the robot, as shown in figure 5. the high-level controller takes care of the husarz behavior, it tracks the time of match, monitors communication between nodes and the status of the task. 13 g. granosik, k. andrzejczak, m. kujawinski et al. acta polytechnica ctu proceedings figure 5. rviz screens presenting two consecutive steps of planning robot‘s movements (red line), red arrow shows orientation of the robot required in the step we have assumed that robot can have four attempts to fulfil each task. these attempts are limited in time, because the match lasts only 90 seconds. after 4 unsuccessful tries the status of the task is switched to “fail“ and the robot moves to the next task. program selects the next task on the basis of distance to move and the remaining time. if one of the robots cannot finish the task it can be sent to the other robot if that robot would be able to run the task. in case of problems with communication the controller will wait until communication is reestablished. the main controller monitors condition of connections between ros and robots. we are using a part of standard ros messages called header. header includes sequence id (uint32 format), time stamp (time format) and frame_id (string format). for connection monitoring the most important is time stamp indicating ros time at the moment when the message was sent. the monitor compares time stamps of incoming messages. when the time stamp does not increase with real time the main controller knows that the connection with robot it lost. in this case main controller goes to stop mode. while the controller is in the stop mode it will not send messages to lower level to avoid situation when the robot loses some orders. in the stop mode the controller continue to check time stamps of incoming messages in order to detect recovery of communication. 2.1. bridging ros with labview another mobile robot requiring mobility planning and autonomous control is raptors rover (see figure 6) figure 6. the raptors rover and its control system being prepared for european rover challenge (erc). one of the tasks in this contest is navigation — intended to demonstrate rovers and teams ability of approaching locations on the field with limited or without supervision. we have to develop a system which will allow operator to navigate rover without access to visual data such as video streaming, photos and other sensor sources placed on the rover that are presenting visual information. the raptors rover was built entirely in house — it is a six wheels platform with well-known rockerbogie suspension system, wireless communication and several cameras. the robot is also equipped with exchangeable tools: 5dof manipulator with gripper and drilling sampler. the control system is organized into 4 levels (see figure 6): the operator‘s console working on a pc computer and developed in labview, the onboard main controller based on sbrio embedded system and developed also in labview, low-level controllers based on arm processors with our own software written in c++, and motor drivers. the communication system employs mainly wifi and can networks with local connections based on rs232 and spi. application of the navigation stack in this case requires the following modifications the original control system: • providing coordinates of goal points based on the 14 vol. 6/2016 using robot operating system for autonomous control of robots figure 7. raptors rover navigation system (up) nodes and topics of the ros structure (down) topological 3d map of erc field, • extending slam to 3d or providing alternative source of pose estimation insensitive to traveling on the rough terrain, • connecting ros nodes to labview based control system to seamlessly exchange control and feedback data. the first requirement can be fulfilled by changing script inside the high-level controller described in the previous chapter. to address the second requirement we have built an independent navigation system based on ros, as shown in figure 7. our system runs on multiple machines with different hardware architectures, file systems and oss but it is not a problem for ros. inertial data is provided by high quality imu with six degrees of freedom, containing gyroscope and accelerometer. the sensor‘s output is three axis angular velocity and linear acceleration. using specialized filters system computes very accurate orientation. gps module outputs position data with one meter accuracy. these data pass through the raspberry pi3 (rpi3) microcontroller and ethernet to the computer in base station that is ros master and process the most demanding calculations (this computer can be finally placed on the robot for full autonomy). wheel odometry is read from the sbrio board via wifi connection. to address the third modification correctly we need to understand that ros requires all nodes to be created in certain way and in specific programming language (usually python or c++). however, there are appliances which requires specific programming language or hardware platform, and this leads to problem with incompatibility of such ros and non — ros system. this problem is common for various robotics projects, and two bridging methods between ros and external applications were proposed: • rosserial — simple wrapper for ros messages, defigure 8. ros bridge functionality signed to allow communication between microcontrollers and ros nodes, • ros_bridge — dedicated node, which translate ros messages into standard json format, and route them to the right node. non-ros application is required to provide support for websockets and serialization of json messages, as shown in figure 7. in our application, sbrio board runs the labview application, which is not able to talk with ros nodes. however, labview includes functions allowing serialization and deserialization of messages in json format and is capable to communicate over the network. ros_bridge package was chosen as a method of communication, because of its flexibility and full support of ros message format. additionally, format of the control data in the raptors rover is different than required by navigation stack. robot has 6 independently driven wheels, the steer maneuver is obtained by differential control of the wheel speeds of the left and right side of the robot and these speeds are scaled in per cents. linear velocity is in the range 0-255 (0-100%), the angular velocity is also 0-255 (0-100%), but we do not steer directly the angle, instead we use a difference of control between the left and right side drives of the robot. due to the further coding of these control signals on the can bus (in order to send them to stm modules), we have used the following ranges of values of a linear speed: 127-128 (50%) means stop, 0-127 is reverse, and 128-255 is forward. similarly, the angular velocity of the robot or the difference between the left and the right side is zero for values of 127-128 (50%), the range 0-127 means turning left, and 128-255 means turning right. to obtain a uniform data format for input to the ros module, before sending data through the ros bridge we have to scale it in an additional vi (section of main program in labview) which produces a reference linear velocity and angular velocity — see figure 8 during tests we were using crossbow imu800ca which was directly publishing raw data over rs232. in this case we were forced to use a specialized filter, 15 g. granosik, k. andrzejczak, m. kujawinski et al. acta polytechnica ctu proceedings as mentioned, to parse the data from the raw digital sensor outputs to proper quaternion based format. we have tried two filters from the navigation stack: madgwick‘s algorithm and complementary filter. they can be found in imu_tools package. these filters are responsible for inertial data fusion and noise reduction. we have also tested the new imu unit that is xsens mti 1. it has both accelerometer and gyroscope and additional magnetometer on board. usually we would have used our node that reads data from serial port but more often ros comes with packages supporting particular hardware eq. xsens. the package we use is called xsens_driver and contains nodes for gathering data and launch file that even automatically searches for a right serial port and baudrate. for getting gps data from our omnistar 3200lr12 we use the excellent nmea_navsat_driver that plugs to the serial port directly and parses nmea sentences from gps unit into gps location form on-the-fly. the final data in a form of digital latitude and longtitude is being sent in sensor_msgs/ navsatfix via /fix topic. the only thing we had to do here was to create the launch file that indicates which sub-nodes to launch and which serial port and baudrate to choose. wheel odometry data has longer way to go. it is published from wheel encoders via can bus to the sbrio computer and then using rosbridge and json format to ros. in a specialized node it is used to calculate position in respect of rover‘s kinematics. having these three data lines, we could use it all over the distributed ros system eq. plug it to a kalman filter available in robot_localization node and connect the output topic of estimated odometry to planning structure made by our colleagues from eurobot team. 2.2. quadron robot we have built quadron robot (shown in figure 9) to compete in robotour contest. it has a carlike kinematic configuration, the base of this vehicle is an electric quad. we have introduced a number of electrical and mechanical modifications, especially in the supporting frame, the drive systems and steering mechanisms, that now can be done with electric motors. for the main drive we have used 500w dc motor, while for the steering the smaller dc gear motor and a coupler system developed in house. each engine is equipped with a driver, encoders and security features the same as used in raptors rover. the robot is further equipped with a number of sensors and modules responsible for security, localization and navigation in the field: navigation module with gps and imu (described earlier), sick lms291 lidar and ultrasonic sensors facing forward. the concept of a multilayer control required the use of computers at different levels: arm microcontroller (stm32 nucleo) at the lower, and mini size pc at the higher layer, as shown schematically in figure 10. entire system is based on ros. the low level node with the software written in c++ is interfacing motors, figure 9. quadron robot for robotour contest encoders, sensors and gamepad. it also receives a higher level commands from the pc, sends appropriate signals to the motors and data from sensors to pc. the board and the pc communicate using rosserial. basically, nucleo is connected to the computer using a serial connection and data is transmitted using usb port. the rosserial protocol can convert the standard ros messages to embedded device equivalent data types, it also implements multi-topic support. a package which enables us to run a ros node at the embedded devices such as nucleo is called the rosserial_client. on the pc side, we need some other packages to decode the serial message and convert to exact topics from the rosserial_client libraries. the recommended pc side node for handling serial data from a device is rosserial_python. for high-level layer is realized by mini pc located on the robot. it is connected to nucleo, laser scaner, imu and gps to receive sensor values which are essential for map building process using slam, obstacle avoidance and also the odometry as mandatory input to the navigational stack. we use standard ros messages inside i.e. sensor_msgs/laserscan, sensor_msgs/range, nav_msgs/odometry. we have applied the same navigation stack (as in husarz robot) and used teb_local_planner node. it supports car-like kinematics, minimizes the trajectory execution time (time-optimal objective), provides separation from obstacles and compliance with kinodynamic constraints (i.e. maximum velocities and accelerations). the base control system of quadron robot is very similar to husarz, and is shown in figure 11. most of the components are the same, the main differences are described below. we have added a node called base_controller which communicates directly with the electronics of the robot. this node finally generates the motor speed 16 vol. 6/2016 using robot operating system for autonomous control of robots figure 10. controller of the quadron robot commands for each motor (pwm). base_controller node subscribes to a topic cmd_vel, which is being published by the local planner and it converts standard message type geometry_msgs/twist (which publishes linear v and angular omega velocities) to the other type called ackermann_msgs/ackermanndrive according to the kinematic structure of the robot (see figure 12) and using classic equations for ackerman steering robots. the base_controller node incudes also an implementation of pid controller, that is why it subscribes odomerty. what is more, in the quadron robot we used additional odometry sources i.e. imu and gps to obtain precise localization, and ultrasonic sensors in order to improve obstacle avoidance. in case of any problems with high-level controller we are still able to control robot manually through gamepad which is connected directly to nucleo board over spi interface. 3. conclusions the great advantage of ros is that we can supervise and visualize our data in real time. however, plotting is available only on x86 or x64 architecture because arm processors (raspberry pi 3) do not support ros graphic libraries. in our system the external computer is just a client that has an access to topics and can run its own nodes. the only requirement is to share the same network and configure the /.bashrc file to define the master‘s and client‘s ip addresses. basically, it is the vital that we use appropriate forms of messages — specific message types and topic names to meet the nodes requirements. it is possible to remap topic names in launch files but it is somehow against ros‘s philosophy that assumes focusing on preestablished design rules. this design concept makes ros systems extremely extendable. easy and logical file figure 11. navigation structure of the quadron robot figure 12. kinematics of the quadron robot structure gives the opportunity to modify source code and add new nodes quickly. the growing ros society is still supplying the repositories with a new software that can be used immediately after committing it to github. acknowledgements research and participation in robotic contests supported by the polish ministry of science and higher education under grant no. mnisw/2016/dir/199/nn references [1] an official webpage of skaner. http://skaner.p.lodz.pl. [2] i. zubrycki, g. granosik. introducing modern robotics with ros and arduino, including case studies. journal of automation, mobile robotics & intelligent systems jamris 8(1):69–75, 2014. doi:10.14313/jamris_1-2014/9. [3] p. goebel. ros by example. lulu, 2013. [4] a. martinez, e. fernaandez. learning ros for robotics programming. packt publishing, 2013. [5] ros answers forum. http://answers.ros.org. [6] ros developers guide. http://wiki.ros.org/developersguide. [7] setup and configuration of the navigation stack on a robot. http: //wiki.ros.org/navigation/tutorials/robotsetup. 17 http://skaner.p.lodz.pl http://dx.doi.org/10.14313/jamris_1-2014/9 http://answers.ros.org http://wiki.ros.org/developersguide http://wiki.ros.org/navigation/tutorials/robotsetup http://wiki.ros.org/navigation/tutorials/robotsetup acta polytechnica ctu proceedings 6:11–17, 2016 1 introduction 2 ros navigation stack 2.1 bridging ros with labview 2.2 quadron robot 3 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0043 acta polytechnica ctu proceedings 4:43–49, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app assessment of burnable absorber fuel design by uwb1 depletion code martin loveckýa,∗, jana jiřičkováa, radek škodaa,b a regional innovation centre for electrical engineering, university of west bohemia, univerzitní 8, 306 14 plzeň, czech republic b faculty of mechanical engineering, czech technical university, technická 4, 160 07 praha 6, czech republic ∗ corresponding author: lovecky@rice.zcu.cz abstract. uwb1 depletion code is being developed as a fast computational tool for the study of burnable absorbers in university of west bohemia in pilsen, czech republic. the research of fuel depletion aims at a development and introduction of advanced types of burnable absorbers in nuclear fuel. burnable absorbers compensate for the initial excess reactivity and consequently allow for lower power peaking factors and longer fuel cycles with higher fuel enrichments. the paper describes the depletion calculations of candu, pwr and sfr nuclear fuel doped with rare earth oxides as burnable absorber. uniform distribution of burnable absorber in the fuel is assumed. based on performed depletion calculations, rare earth oxides are divided into two groups, suitable burnable absorbers and poisoning absorbers. moreover, basic economic comparison is performed based on actual stock prices. keywords: burnable absorber, fuel depletion, monte carlo. 1. introduction uwb1 nuclear fuel depletion code [1, 4] is being developed as a fast fuel depletion code to conduct burnable absorber research. the goal of the research is to optimize new materials as burnable absorbers (ba) in nuclear fuel. bas compensate for the initial excess reactivity and consequently allow for lower power peaking factors and longer fuel cycles with higher fuel enrichments. research of advanced types of burnable absorbers (ba) in nuclear fuel requires fast depletion code that would be able to calculate broad range of elements, nuclides or their combination. state-of-art depletion codes require large amount of computational time, therefore, decision to develop fast depletion code was made. currently developed uwb1 depletion code comprises of transport and burnup solver that works in 2spc depletion scheme in order to perform fast calculation of nuclear fuel depletion. in order to achieve high precision in uwb1 code, monte carlo solver for lattice cell calculations is used to solve transport equation. bateman equations are solved in special depletion scheme that relies on nuclide-based predictorcorrector method in both transport and burnup part of fuel depletion. the paper describes the depletion calculations of candu, pwr and sfr nuclear fuel doped with rare earth oxides as burnable absorber. uniform distribution of burnable absorber in the fuel is assumed. based on performed depletion calculations, rare earth oxides are divided into two groups, suitable burnable absorbers and poisoning absorbers. moreover, basic economic comparison is performed based on current stock prices. 2. uwb1 depletion code first version of the newly developed uwb1 fast nuclear fuel depletion code [1] significantly reduced calculation time by omitting the solution step for the boltzmann transport equation. however, estimation of multiplication factor during depletion was not sufficiently calculated [2]. moreover, 1-group effective cross sections for strong absorber models like gadolinium showed disagreement between the uwb1 tested code and the serpent reference code [3]. monte carlo transport solver for uwb1 code was introduced [4] in order to improve code accuracy and remove pre-calculated case-dependent data libraries, therefore, eliminate constant effective cross section assumption. nuclear data from endf/b-vii.1 library is used for uwb1 monte carlo solver. standard raytracing algorithm for neutron random walk is a part of the solver. two-dimensional fuel pin models geometry, where fuel lattice model is assumed. the speed of the solver is higher than for the mcnp6 reference code. for light water reactor models, uwb1 monte carlo solver is on average 10 times faster. two-step predictor-corrector method (2spc) was developed for uwb1 code. the idea is to change the coupling of transport and burnup solvers by omitting major fraction of transport solver callings, because transport solver is, by orders of magnitude, slower than burnup solver. both transport and burnup variables are calculated for predicted states and corrected with more precise values as the two parts of fuel depletion are coupled. only three transport solver solutions are used, the initial fuel state and predicted and corrected states for final burnup state. effective cross sections are evaluated during fuel depletion by 43 http://dx.doi.org/10.14311/ap.2016.4.0043 http://ojs.cvut.cz/ojs/index.php/app m. lovecký, j. jiřičková, r. škoda acta polytechnica ctu proceedings assuming nuclide-based non-linear dependency. multiplication factors in the depletion steps other than the first and the last one are estimated by neutron production to absorption ratio that is calculated without the need to call the transport solver. employing 2spc depletion scheme leads to a significant reduction of calculation time by a factor of 10. with the monte carlo speed-up against the reference code, fuel depletion with uwb1 code is around 100 times faster than with mcnp6 reference code. 3. burnable absorbers in order to mark a material as a good burnable absorber, two properties are desired. these are a high neutron absorption cross section with low daughter nuclide’s neutron absorption cross section. high neutron capture cross section causes neutrons to be absorbed, therefore, multiplication factor of the fuel is decreased and initial excess of reactivity is compensated. the absorber is burnable if the nuclide resulting from neutron absorption has a lower neutron absorption cross section, therefore, reactivity worth of inserting burnable absorber is decreasing during fuel depletion. the higher the differences between cross sections, the faster the burnable absorber will be burned. typical absorption reaction for burnable absorbers is (n,γ), although another reactions are possible, e.g. (n,α) for light elements like boron. present nuclear fuels use mainly gadolinium, europium and erbium oxides. gadolinium oxide is burned faster than the two others and because of the very high absorption cross section of gd-157 nuclide, initial reactivity compensation for gadolinium higher than for other materials. gadolinium nuclides with interesting burnable properties are gd-155 and gd-157 with natural abundances 14.80 at% and 15.65 at%. europium has natural abundance of 47.81 at% eu-151 and 52.19 at% eu-153. both europium nuclides behaves as a good burnable absorber nuclide, both nuclides have have high neutron capture cross sections with end-product nuclide characterized by low capture cross section. erbium nuclides with interesting burnable properties are er-166 and er-167 with natural abundances 33.50 at% and 22.87 at%. total cross section for thermal energy 0.0253 ev are: 60 801 barns for gd-155, 253 929 barns for gd-157, 9190 barns for eu-151, 367 barns for eu153, 31 barns for er-166 and 652 barns for er-167. 4. rare earth oxides burnable absorber research will be conducted in two phases. the first phase will be represented by parametric study of various types of ba materials. the uwb1 depletion code will be used in order to calculate a large number of cases, employing its fast calculation scheme. promising materials will be used in the second phase for a deeper neutronic analysis with state-of-art codes, possible discrepancies or inaccuracies of the uwb1 code will be removed. the output of the research is to sort materials by their suitability as ba from neutronics point of view. after that, another types of analyses, like chemical compatibility, thermal conductivity, economic evaluation and other relevant areas will be performed. the paper focuses only on rare earth oxides as burnable absorbers. these are often used or planned to use as ba in pwr nuclear fuel. the most common is gadolinium oxide, followed by europium and erbium oxides. rare earth oxides were briefly analyzed in [5] for vver nuclear fuel, in this paper, pwr, candu and sfr nuclear fuels are compared. rare earth elements are available as metals or oxides. thermal reactors and some of proposed fast reactors use uranium oxide fuel, therefore, rare earth oxides were evaluated. seventeen rare earth elements are abundant in nature (scandium, yttrium and 15 lanthanides from lanthanum to lutetium). most of them are available in oxides with x2o3 stechiometry, in order to introduce the same normalization for all elements, masses of all other rare earth cases were recalculated to have x2o3 stechiometry. 5. calculation cases candu, pwr and sfr nuclear fuel depletion was calculated. of seventeen available rare earth oxides, 16 were calculated. promethium, having only radioactive nuclides, was excluded from the study. it the first part of the study, criticality calculations with uwb1 code were performed in order to determine rare earth oxides content in the fuel (wt% x2o3). the target multiplication factor was selected to be around 0.05 lower than for the fresh fuel without ba, namely 1.10 for candu fuel, 1.25 for pwr fuel and 1.15 for sfr fuel (fresh fuel multiplication factors are 1.15, 1.32, 1.20). in the second part, fuel depletion with uwb1 code were calculated and multiplication factor dependency on fuel burnup was analyzed. finally, economic comparison was performed. uwb1 code requires simple fuel cell geometry. recently, the option to include arbitrary number of concentric cylinders with either square or triangular lattice was included. candu fuel was homogenized and modeled as 18 concentric cylinders that represents four fuel rings of the total number of 37 pins. natural uranium oxide fuel with final burnup 10 000mwd/mtu was assumed. fuel depletion was divided into 31 steps with constant power 32.4364mw/mtu. standard candu materials were used in the model – zircaloy-4 for fuel cladding, zr2.5nb alloy for pressure tube that is divided by co2 gap from zircaloy-2 calandria tube, heavy water with density 0.8179 g/cm3 and purity 99.11 wt% as coolant in the pressure tube and heavy water with density 1.086 99 g/cm3 and purity 99.97 wt% as moderator between calandria tube. pwr nuclear fuel was modeled as 5.0 wt% u-235 enriched uranium oxide with zircaloy-4 cladding and light water moderator with 600 ppm boric acid. fuel radius 0.4025 cm and cladding radius 0.4750 cm was 44 vol. 4/2016 assessment of burnable absorber fuel design by uwb1 depletion code used, lattice half pitch 0.6295 cm was assumed as typical pwr dimensions. the fuel was depleted with power 40.0mw/mtu in 34 steps up to final burnup 50 000mwd/mtu. sfr nuclear fuel was modeled as 15.0 wt% u-235 enriched uranium oxide with 7.9 g/cm3 iron cladding and 0.88 g/cm3 sodium coolant. fuel radius 0.28 cm and cladding radius 0.33 cm was used, lattice half pitch 0.42 cm were used as typical sfr dimensions (bn-800 reactor was assumed as typical sfr reactor). the fuel was depleted with power 130.0mw/mtu in 74 steps up to final burnup 150 000mwd/mtu, three times higher than of pwr fuel. 6. criticality results candu, pwr and sfr nuclear fuel criticality calculation results from uwb1 code are presented in fig. 1 to fig. 3. the figures show dependency of multiplication factor for fresh fuel with various ba content (mass fraction) on logarithm scale. 1 e 0 5 1 e 0 4 1 e 0 3 1 e 0 2 1 e 0 1 1 e + 0 0 0 . 0 0 . 2 0 . 4 0 . 6 0 . 8 1 . 0 1 . 2 mu ltip lica tio n f ac tor (-) b a w e i g h t c o n t e n t ( ) 2 1 s c 3 9 y 5 7 l a 5 8 c e 5 9 p r 6 0 n d 6 2 s m 6 3 e u 6 4 g d 6 5 t b 6 6 d y 6 7 h o 6 8 e r 6 9 t m 7 0 y b 7 1 l u c a n d u : m u l t i p l i c a t i o n f a c t o r v s b a c o n t e n t figure 1. candu multiplication factor vs ba content. 1 e 0 5 1 e 0 4 1 e 0 3 1 e 0 2 1 e 0 1 1 e + 0 0 0 . 0 0 . 2 0 . 4 0 . 6 0 . 8 1 . 0 1 . 2 1 . 4 mu ltip lica tio n f ac tor (-) b a w e i g h t c o n t e n t ( ) 2 1 s c 3 9 y 5 7 l a 5 8 c e 5 9 p r 6 0 n d 6 2 s m 6 3 e u 6 4 g d 6 5 t b 6 6 d y 6 7 h o 6 8 e r 6 9 t m 7 0 y b 7 1 l u p w r : m u l t i p l i c a t i o n f a c t o r v s b a c o n t e n t figure 2. pwr multiplication factor vs ba content. multiplication factor reduction from ba insertion into the fuel is higher for candu fuel that needs only a small ba content to achieve target multiplication 1 e 0 5 1 e 0 4 1 e 0 3 1 e 0 2 1 e 0 1 1 e + 0 0 0 . 2 0 . 4 0 . 6 0 . 8 1 . 0 1 . 2 mu ltip lica tio n f ac tor (-) b a w e i g h t c o n t e n t ( ) 2 1 s c 3 9 y 5 7 l a 5 8 c e 5 9 p r 6 0 n d 6 2 s m 6 3 e u 6 4 g d 6 5 t b 6 6 d y 6 7 h o 6 8 e r 6 9 t m 7 0 y b 7 1 l u s f r : m u l t i p l i c a t i o n f a c t o r v s b a c o n t e n t figure 3. sfr multiplication factor vs ba content. factor. pwr fuel is similar to candu, however, due to higher fuel enrichment, more ba content is needed. lastly, sfr with fast neutron spectra and high fuel enrichment requires considerably higher ba content than previous fuel types in order to achieve desirable initial reactivity compensation. based on performed criticality calculations and selected target multiplication factor values 1.10 for candu fuel, 1.25 for pwr fuel and 1.15 for sfr fuel, ba weight fraction was calculated. linear interpolation between selected ba contents (3 values for each logarithm order) was used. calculated ba content is shown in fig. 4 to fig. 6. 2 1 s c 3 9 y 5 7 l a 5 8 c e 5 9 p r 6 0 n d 6 2 s m 6 3 e u 6 4 g d 6 5 t b 6 6 d y 6 7 h o 6 8 e r 6 9 t m 7 0 y b 7 1 l u 1 e 0 6 1 e 0 5 1 e 0 4 1 e 0 3 1 e 0 2 1 e 0 1 1 e + 0 0 ba ox ide we igh t fr ac tio n ( -) b u r n a b l e a b s o r b e r t y p e ( ) c a n d u : b u r n a b l e a b s o r b e r w e i g h t f r a c t i o n figure 4. candu burnable absorber weight fraction. in the case of both candu and pwr fuel, even maximum considered ba content (50 wt% x2o3) was not enough for dropping the multiplication factor to the target one. for pwr fuel, 58-ce content was also too high. for sfr fuel, it was possible to achieve desired target multiplication factor for all rare earth oxides ba. 45 m. lovecký, j. jiřičková, r. škoda acta polytechnica ctu proceedings 2 1 s c 3 9 y 5 7 l a 5 8 c e 5 9 p r 6 0 n d 6 2 s m 6 3 e u 6 4 g d 6 5 t b 6 6 d y 6 7 h o 6 8 e r 6 9 t m 7 0 y b 7 1 l u 1 e 0 5 1 e 0 4 1 e 0 3 1 e 0 2 1 e 0 1 1 e + 0 0 ba ox ide we igh t fr ac tio n ( -) b u r n a b l e a b s o r b e r t y p e ( ) p w r : b u r n a b l e a b s o r b e r w e i g h t f r a c t i o n figure 5. pwr burnable absorber weight fraction. 2 1 s c 3 9 y 5 7 l a 5 8 c e 5 9 p r 6 0 n d 6 2 s m 6 3 e u 6 4 g d 6 5 t b 6 6 d y 6 7 h o 6 8 e r 6 9 t m 7 0 y b 7 1 l u 1 e 0 3 1 e 0 2 1 e 0 1 1 e + 0 0 ba ox ide we igh t fr ac tio n ( -) b u r n a b l e a b s o r b e r t y p e ( ) s f r : b u r n a b l e a b s o r b e r w e i g h t f r a c t i o n figure 6. sfr burnable absorber weight fraction. minimum ba content was calculated for gadolinium oxide for candu and pwr fuel (7.52 × 10−6 and 1.02 × 10−4 weight fraction) and for europium oxide for sfr fuel (8.67 × 10−3 weight fraction). for most of rare earth oxides, candu and pwr fuel requires ba content from 0.1 wt% x2o3 to 1.0 wt% x2o3. for sfr fuel, required ba content mostly varies from 1.0 wt% x2o3 to 10.0 wt% x2o3, i.e. 10 times higher than of thermal spectra fuels. maximum ba content was calculated for 58-ce. for candu fuel, 26.8 wt% ce2o3 was determined. slightly lower conten of 20.4 wt% ce2o3 was calculated for sfr fuel. pwr fuel required more than 50.0 wt% ce2o3 and cerium oxide was excluded, making 39-y the case of maximum ba content for pwr fuel (40.5 wt% y2o3). 7. depletion results candu, pwr and sfr nuclear fuel criticality calculation results from uwb1 code are presented in fig. 7 to fig. 9. 0 2 0 0 0 4 0 0 0 6 0 0 0 8 0 0 0 1 0 0 0 0 0 . 9 0 0 . 9 5 1 . 0 0 1 . 0 5 1 . 1 0 1 . 1 5 mu ltip lica tio n f ac tor (-) b u r n u p ( m w d / m t u ) n o _ b a 6 0 n d 6 7 h o 2 1 s c 6 2 s m 6 8 e r 3 9 y 6 3 e u 6 9 t m 5 7 l a 6 4 g d 7 0 y b 5 8 c e 6 5 t b 7 1 l u 5 9 p r 6 6 d y c a n d u : f u e l d e p l e t i o n w i t h b a figure 7. candu multiplication factor during fuel depletion. candu figure shows that from macroscopic view, only 63-eu and 64-gd compensate initial reactivity in the way that initial reactivity transient due to fission product build-up almost disappears. for other ba, initial reactivity is compensated, however, initial reactivity transient is still presented. for good burnable absorbers, residual poisoning (decrease of multiplication factor compared to no ba case) is negligible, other ba have residual poisoning that, for some cases, is even higher than initial reactivity compensation. 0 1 0 0 0 0 2 0 0 0 0 3 0 0 0 0 4 0 0 0 0 5 0 0 0 0 0 . 8 5 0 . 9 0 0 . 9 5 1 . 0 0 1 . 0 5 1 . 1 0 1 . 1 5 1 . 2 0 1 . 2 5 1 . 3 0 1 . 3 5 mu ltip lica tio n f ac tor (-) b u r n u p ( m w d / m t u ) n o _ b a 6 0 n d 6 7 h o 2 1 s c 6 2 s m 6 8 e r 3 9 y 6 3 e u 6 9 t m 5 7 l a 6 4 g d 7 0 y b 5 8 c e 6 5 t b 7 1 l u 5 9 p r 6 6 d y p w r : f u e l d e p l e t i o n w i t h b a figure 8. pwr multiplication factor during fuel depletion. for pwr fuel, similar conclusions as for candu fuel can be deduced. only 63-eu and 64-gd oxides are able to change the shape of multiplication factor dependency on burnup, i.e. remove initial reactivity transient. however, for pwr fuel, initial reactivity transient is not only removed, but the effect is reversed, 46 vol. 4/2016 assessment of burnable absorber fuel design by uwb1 depletion code multiplication factor increases in the first days of fuel operation. for sfr fuel, all rare earth oxides show similar behavior, burning of the oxides is very slow and reactivity compensation remains relatively constant, therefore, rare earth oxides behaves mostly as non-burnable absorbers. 0 2 5 0 0 0 5 0 0 0 0 7 5 0 0 0 1 0 0 0 0 0 1 2 5 0 0 0 1 5 0 0 0 0 0 . 9 0 0 . 9 5 1 . 0 0 1 . 0 5 1 . 1 0 1 . 1 5 1 . 2 0 mu ltip lica tio n f ac tor (-) b u r n u p ( m w d / m t u ) n o _ b a 6 0 n d 6 7 h o 2 1 s c 6 2 s m 6 8 e r 3 9 y 6 3 e u 6 9 t m 5 7 l a 6 4 g d 7 0 y b 5 8 c e 6 5 t b 7 1 l u 5 9 p r 6 6 d y s f r : f u e l d e p l e t i o n w i t h b a figure 9. sfr multiplication factor during fuel depletion. based on performed depletion calculations and multiplication factor progress during fuel depletion, ba worth was calculated. ba worth is defined as reactivity differences between two cases, the one with ba in the fuel and the one without ba. results are depicted in fig. 10 to fig. 12. 0 2 0 0 0 4 0 0 0 6 0 0 0 8 0 0 0 1 0 0 0 0 8 0 0 0 6 0 0 0 4 0 0 0 2 0 0 0 0 ba wo rth (p cm ) b u r n u p ( m w d / m t u ) n o _ b a 6 0 n d 6 7 h o 2 1 s c 6 2 s m 6 8 e r 3 9 y 6 3 e u 6 9 t m 5 7 l a 6 4 g d 7 0 y b 5 8 c e 6 5 t b 7 1 l u 5 9 p r 6 6 d y c a n d u : b a w o r t h figure 10. candu burnable absorber worth during fuel depletion. from ba worth curve variation during fuel depletion, it can be stated which rare earth oxides behaves like more or less suitable burnable absorbers and which behaves like poisoning absorbers. the latter group can be divided into constant poisoning absorbers (ba worth is constant function of burnup) and increasingly poisoning absorbers (ba worth is decrasing function of decrasing function of burnupburnup, i.e. diverges 0 1 0 0 0 0 2 0 0 0 0 3 0 0 0 0 4 0 0 0 0 5 0 0 0 0 1 2 0 0 0 1 0 0 0 0 8 0 0 0 6 0 0 0 4 0 0 0 2 0 0 0 0 ba wo rth (p cm ) b u r n u p ( m w d / m t u ) n o _ b a 6 0 n d 6 7 h o 2 1 s c 6 2 s m 6 8 e r 3 9 y 6 3 e u 6 9 t m 5 7 l a 6 4 g d 7 0 y b 5 8 c e 6 5 t b 7 1 l u 5 9 p r 6 6 d y p w r : b a w o r t h figure 11. pwr burnable absorber worth during fuel depletion. 0 1 0 0 0 0 2 0 0 0 0 3 0 0 0 0 4 0 0 0 0 5 0 0 0 0 5 0 0 0 4 0 0 0 3 0 0 0 2 0 0 0 1 0 0 0 0 ba wo rth (p cm ) b u r n u p ( m w d / m t u ) n o _ b a 6 0 n d 6 7 h o 2 1 s c 6 2 s m 6 8 e r 3 9 y 6 3 e u 6 9 t m 5 7 l a 6 4 g d 7 0 y b 5 8 c e 6 5 t b 7 1 l u 5 9 p r 6 6 d y s f r : b a w o r t h figure 12. sfr burnable absorber worth during fuel depletion. from zero reactivity worth, rather than converging behaviour of burnable absorbers). because of the fact that ba worth curve does not change its derivation sign (constant, increasing or decreasing function), it is possible to define ratio of eoc to boc reactivity worth and compare it to unity, see final results in fig. 13. candu and pwr fuel behaves similarly, burnable absorbers are more depleted for final burnup in the case of candu fuel, therefore, residual poisoning is lower for candu and burnable absorbers are more suited for candu fuel. total number of 9 out of 16 rare earth oxides are marked as burnable absorbers for both candu and pwr fuels, namely 21-sc, 60-nd, 62-sm, 63-eu, 64gd, 66-dy, 67-ho, 68-er and 69-tm. total number of 4 out of 16 rare earth oxides are marked as burnable absorbers only for candu fuel, but behaves as poisoning absorbers for pwr fuel. these are 39-y, 57-la, 59-pr and 71-lu. the rest 3 out of 16 rare earth oxides, 65-tb, 58-ce and 70-yb, are poisoning absorbers for both candu and pwr fuel. 47 m. lovecký, j. jiřičková, r. škoda acta polytechnica ctu proceedings 2 1 s c 3 9 y 5 7 l a 5 9 p r 6 0 n d 6 2 s m 6 3 e u 6 4 g d 6 5 t b 6 6 d y 6 7 h o 6 8 e r 6 9 t m 7 1 l u 0 . 0 0 . 5 1 . 0 1 . 5 2 . 0 ba wo rth eo c / ba wo rth bo c ( -) b a e l e m e n t ( ) c a n d u p w r s f r b a w o r t h r a t i o b e t w e e n e o c a n d b o c figure 13. rare earth oxides as ba eoc/boc worth ratio. situation for sfr fuel is simpler than for both thermal spectra fuels. only 2 out of 16 rare earth oxides, 66-dy and 69-tm, are suitable as burnable absorbers. thulium oxide is a far better ba for sfr than dysprosium oxide that burns very slowly. however, significant fraction of thulium oxide remains in the fuel at eoc. 8. economic comparison economic comparison of rare earth oxides as burnable absorbers is based on prices from early 2016 [6], however, rare earth oxides are mined mainly in one country and prices are volatile. table 1 (or fig. 14) summarizes the results. input oxides prices (rmb/mt) were converted to match x2o3 stechiometry and multiplied by target ba content (weight fraction) to evaluate oxides prices for unit uranium mass (rmb/mtu). total fuel price comprises of ba price, uranium price and other factors, only ba price is compared in this study. element price (rmb/mt) 39-y 34 000 57-la 13 250 58-ce 13 900 59-pr 429 000 60-nd 322 500 62-sm 17 000 63-eu 1900 64-gd 87 500 65-tb 4300 66-dy 1915 68-er 265 000 table 1. rare earth oxides as ba – economic comparison. 3 9 y 5 7 l a 5 9 p r 6 0 n d 6 2 s m 6 3 e u 6 4 g d 6 5 t b 6 6 d y 6 8 e r 1 e 0 1 1 e + 0 0 1 e + 0 1 1 e + 0 2 1 e + 0 3 1 e + 0 4 1 e + 0 5 ba pr ice (r mb /m tu ) b a e l e m e n t ( ) c a n d u p w r s f r r a r e e a r t h o x i d e p r i c e s a s b u r n a b l e a b s o r b e r s figure 14. rare earth oxides as ba – economic comparison. for the best burnable absorbers, the economic comparison showed the price of rare earth oxide in mtu vary from 1rmb to 1000rmb for candu and pwr fuels and approximately 100 times higher prices for sfr fuels. 9. conclusions uwb1 depletion code was used to assess burnable absorber design in the nuclear fuel. candu, pwr and sfr fuel lattice criticality and depletion calculations were performed for rare earth oxides as burnable absorbers uniformly distributed in the fuel. rare earth oxides content needed to achieve target initial reactivity compensation was evaluated. based on multiplication factor behavior during fuel depletion and ba reactivity worth ratio for final burnup and inital state, rare earth oxides were divided into two groups, burnable absorbers and poisoning absorbers. candu and pwr fuel behaves similarly. total number of 9 out of 16 rare earth oxides are marked as burnable absorbers for both candu and pwr fuels, namely 21-sc, 60-nd, 62-sm, 63-eu, 64-gd, 66-dy, 67ho, 68-er and 69-tm. total number of 4 out of 16 rare earth oxides are marked as burnable absorbers only for candu fuel, but behaves as poisoning absorbers for pwr fuel. these are 39-y, 57-la, 59-pr and 71-lu. the rest 3 out of 16 rare earth oxides, 65-tb, 58-ce and 70-yb, are poisoning absorbers for both candu and pwr fuel. situation for sfr fuel is simpler than for both thermal spectra fuels. only 2 out of 16 rare earth oxides, 66-dy and 69-tm, are suitable as burnable absorbers. thulium oxide is a far better ba for sfr than dysprosium oxide that burns very slowly. for the best burnable absorbers, the economic comparison showed the price of rare earth oxide in mtu 48 vol. 4/2016 assessment of burnable absorber fuel design by uwb1 depletion code vary from 1rmb to 1000rmb for candu and pwr fuels and approximately 100 times higher prices for sfr fuels. further analysis of possible burnable absorbers with broad range of elements, nuclides or their combination is in progress. the research aims to a quantitative comparison of materials that could be used as burnable absorbers. the resulting data are planned to be utilized in subsequent fuel design analyses including thermal conductivity, chemical compatibility, irradiation stability, economic evaluation etc. list of symbols boc beginning of cycle (irradiation) eoc end of cycle (irradiation) mt metric ton mtu metric tons of uranium rmb renminbi (chinese currency system) acknowledgements research and development has been funded by tacr, project no. te01020455 – centre for advanced nuclear technologies (canut). references [1] m. lovecky, l. piterka, j. prehradny, r. skoda. uwb1 – fast nuclear fuel depletion code. annals of nuclear energy 71:333–339, 2014. doi:10.1016/j.anucene.2014.04.021. [2] j. prehradny, m. lovecky, r. skoda. burnable absorber comparison between vver, pwr and sfr with uwb1 and serpent codes. in proceedings of the 2014 22nd international conference on nuclear engineering. 2014. doi:10.1115/icone22-30894. [3] j. leppanen. development of a new monte carlo reactor physics bode. ph.d. thesis, helsinki university of technology, 2007. [4] m. lovecky, j. jirickova, r. skoda. monte carlo solver for uwb1 nuclear fuel depletion code. annals of nuclear energy 85:778–7879, 2015. doi:10.1016/j.anucene.2015.06.035. [5] j. prehradny, m. lovecky, r. skoda. rare earth oxides as burnable absorber for vver nuclear fuel. in proceedings of the 2015 23rd international conference on nuclear engineering. 2015. [6] shanghai metals market, prices of rare earth oxide, http://www.metal.com/metals/rare-earth/prices. 49 http://dx.doi.org/10.1016/j.anucene.2014.04.021 http://dx.doi.org/10.1115/icone22-30894 http://dx.doi.org/10.1016/j.anucene.2015.06.035 http://www.metal.com/metals/rare-earth/prices acta polytechnica ctu proceedings 4:43–49, 2016 1 introduction 2 uwb1 depletion code 3 burnable absorbers 4 rare earth oxides 5 calculation cases 6 criticality results 7 depletion results 8 economic comparison 9 conclusions list of symbols acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2016.6.0006 acta polytechnica ctu proceedings 6:6–10, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app on evaluation of motion gaits energy efficiency with a hexapod crawling robot lukáš černý∗, petr čížek, jan faigl czech technical university, faculty of electrical engineering, technicka 2, prague, czech republic ∗ corresponding author: cernylu6@fel.cvut.cz abstract. in this work, we are concerning the problem of energy efficient locomotion of a hexapod crawling robot. we are emphasizing a practical verification and deployment on a real walking robot to evaluate relations between the energy consumption, motion speed, and terrain type with a particular motion gait. the tripod, tetrapod, and pentapod motion gaits are considered in the presented evaluation report. keywords: rgb-d slam, localization, ground-truth construction, legged robot, rough terrain traversal, adaptive motion gait. 1. introduction energy efficient and fast locomotion is a key ability for the mobile robot to extent its operation capabilities. as legged robots offer the potential to traverse various types of terrains, it is desirable to adjust their locomotion to be as energy efficient as possible. in general, there are two principal ways of locomotion control for legged robots operating in rough terrains. either deliberative control where individual foot-tip positions of each leg are planned in advance (e.g., [1]) or reactive control based on a repetitive motion gait with prescribed leg trajectories with a certain amount of adaptability such as [2]. the later approach builds on the fact that legged robots often utilize collections of gait patterns to locomote over a variety of surfaces with each gait tuned for a specific surface and set of operational conditions. several commonly used gait patterns such as tripod, tetrapod, and pentapod motion gaits have been developed for hexapod crawling robots. during traversing a rough terrain, it is possible to select a particular gait pattern and stick with it for the whole process of the navigation; however, it may be beneficial to utilize knowledge of the terrain currently being traversed to select the most appropriate gait to optimize a particular criterion, e.g., speed, stability, or energy consumption. the gait selection can be based on both exteroceptive and proprioceptive sensing. in this paper, we consider proprioceptive sensory data only, specifically the current sensory data to evaluate the energy efficiency of individual gaits on different terrain types. we use the information about the overall current drawn from the robot energy source (the used battery pack) to compute instantaneous power and consequently the consumed energy during the robot operation. we performed a series of experiments to collate information about the energy efficiency of different gaits on different terrain types to establish a gait selection strategy that would let us alter gaits according to the terrain that is being traversed. for this purpose, we expect the terrain to be foreknown, i.e., classified in advance. we distinguish following terrain types: office floor, grass, inclined plane, and wooden blocks, see figure 1. online terrain classification can be done using exteroceptive data; however, this topic is out of the scope of this paper, therefore in the herein presented evaluation of the energy consumption, we rather assume the current terrain type is available. an evaluation of the energy efficiency applied for the hexapod crawling robot has been shown in [3]. the authors propose a method of energetic cost evaluation and they applied it in a gait transition algorithm that alters between two different gaits according to the power consumption and thus, according to the particular terrain type. several methods of traversability cost evaluation based on proprioceptive sensors are proposed in [4]. the authors also consider a hexapod walking robot and utilize information about the current torque at the leg joints to estimate the power consumption. contrary to this approach, we consider a direct current measurement in this paper, which provides a more precise estimation of the overall power consumption during crawling. this paper is organized as follows. section 2 describes the utilized hexapod robot platform, the considered motion gait patterns, and used evaluation methodology for measuring the energy efficiency of the individual motion gaits. section 3 is dedicated to the experimental results. finally, in section 4, we discuss the experimental results and propose further research directions. 2. problem statement 2.1. hexapod platform the idea of optimizing the energy consumption by altering gaits according to the terrain type can be applied to any legged robot. in this work, we utilize a robot based on an off-the-shelf phantom x mark 6 http://dx.doi.org/10.14311/app.2016.6.0006 http://ojs.cvut.cz/ojs/index.php/app vol. 6/2016 on evaluation of motion gaits energy efficiency (a) . office floor (b) . grass (c) . inclined plane (d) . wooden blocks figure 1. terrain types. ii platform with six legs. each leg consists of three actuated joints driven by the dynamixel ax-12 intelligent servos. this makes the robot easy to use and relatively cheap with surprisingly large locomotion capabilities in rough environments. 2.2. motion gaits a straightforward approach to a hexapod robot locomotion is to predefine and fix a particular motion gait pattern and simply repeat such a pattern over and over. based on the number of legs moving simultaneously and on the order in which the legs are altering between the support phase and the swing phase, different motion gaits can be recognized. this include regular tripod, tetrapod, pentapod, and ripple gaits. further details on these regular gaits can be found in [5]. a basic locomotion controller assume crawling on a flat terrain by default; however, it is necessary to negotiate the landscape using the robot sensory feedback to surpass a rough terrain. in this report, we consider the default tripod, tetrapod, pentapod, and ripple gaits which assume crawling on a flat terrain and their adaptive variants for tripod, tetrapod, and pentapod gaits [2]. the adaptive gaits exploit the sensory feedback from the intelligent servo drives to detect the contact point of the leg with the supporting surface [6]. in particular, a position error of the servo joint, which is proportional to the applied torque, is utilized to stop the motion of the leg during the swing phase, and thus to detect the contact point of the leg with the ground. 2.3. energetics the fundamental sensory input for the proposed evaluation of the energy efficiency of the individual gaits is based on measuring of the current i drawn from the robot main battery. from the measured current i we can compute the instantaneous power as pin = v i, (1) where i is the instantaneous current (in units of amperes), v is voltage of the battery (in units of volts), and pin is the instantaneous power (in units of watts). as shown in [3], pin is the total power consumed by the robot that consists of the power generating mechanical forces and the power representing the energy loss. however, we consider the total power only because we aim to minimize the overall energy consumed. from the gathered information about the instantaneous power (1), we can estimate the energy consumed during traversing a particular terrain. based on the relationship between the consumed energy e and the instantaneous power pin(t) = de(t) dt (2) we can write e(t) = ∫ t 0 pin(τ) dτ , (3) where e(t) is the energy consumed (in units of joules) from the beginning of the experiment up until the specified time t. from (3) we can estimate the overall energy consumption by integrating the instantaneous power numerically, e.g., using the trapezoidal rule. 3. evaluation 3.1. experimental set-up the following experimental setup has been designed to evaluate and compare particular abilities of each considered gait to traverse a particular terrain type. the robot has been requested to walk a fixed distance of one meter straight ahead and traverse a particular terrain type. considered terrain types are the office floor, artificial grass, inclined plane, and wooden blocks of irregular heights (see figure 1). the office floor and artificial grass represent terrain types with different adhesion, and thus with a different slippage. the inclined plane and wooden blocks represent an environment with elevated demands on the power consumption. the locomotion of the robot on the wooden blocks is also often subjected to slippage and abrupt motions which apply further load on the servo drives, leading to a higher energy consumption. the experiment has been repeated three times for each gait on each terrain type except the default gaits and wooden blocks because the default gaits are not capable of traversing such a rough terrain. the distance traveled by the robot has been estimated based on the legged odometry only. 7 l. černý, p. čížek, j. faigl acta polytechnica ctu proceedings time [s] 0 5 10 15 20 25 c o n su m ed en er g y [j ] 0 50 100 150 200 250 300 energy consumption of default gaits on o/ce .oor default tripod gait default tetrapod gait default pentapod gait default ripple gait (a) . default gaits on office floor time [s] 0 5 10 15 20 25 c o n su m ed en er g y [j ] 0 50 100 150 200 250 300 350 energy consumption of default gaits on grass default tripod gait default tetrapod gait default pentapod gait default ripple gait (b) . default gaits on grass time [s] 0 5 10 15 20 25 c o n su m ed en er g y [j ] 0 50 100 150 200 250 300 350 400 450 energy consumption of default gaits on slope default tripod gait default tetrapod gait default pentapod gait default ripple gait (c) . default gaits on inclined plane time [s] 0 20 40 60 80 100 120 c o n su m ed en er g y [j ] 0 200 400 600 800 1000 1200 energy consumption of adaptive gaits on o/ce .oor adaptive tripod gait adaptive tetrapod gait adaptive pentapod gait (d) . adaptive gaits on office floor time [s] 0 20 40 60 80 100 120 c o n su m ed en er g y [j ] 0 200 400 600 800 1000 1200 1400 energy consumption of adaptive gaits on grass adaptive tripod gait adaptive tetrapod gait adaptive pentapod gait (e) . adaptive gaits on grass time [s] 0 20 40 60 80 100 120 c o n su m ed en er g y [j ] 0 200 400 600 800 1000 1200 1400 1600 energy consumption of adaptive gaits on slope adaptive tripod gait adaptive tetrapod gait adaptive pentapod gait (f) . adaptive gaits on inclined plane time [s] 0 20 40 60 80 100 120 c o n su m ed en er g y [j ] 0 500 1000 1500 energy consumption of adaptive gaits on wooden blocks adaptive tripod gait adaptive tetrapod gait adaptive pentapod gait (g) . adaptive gaits on wooden blocks figure 2. energy consumption over time. the overall current drawn from the battery has been measured using the acs712 hall effect-based linear current sensor with the measuring range of ±5 a. each current data sample was provided with a timestamp. the reading frequency was not completely invariant due to the time consumed by the motion control and other factors. in spite of that the reading frequency was approximately 100 hz. before each experiment, we measured the battery voltage and we assumed it is constant during the robot movement because the drop of the voltage was insignificant during the experiment. thereby, we have acquired all the information needed to estimate the energy consumed by the robot motion. 3.2. results having done all the experiments described above, the instantaneous power for each current sample using (1) has been computed. consequently, the power has been numerically integrated according to (3). the plotted energy consumption over time is presented in figure 2, where the particular plots are as follows. figure 2a and figure 2d show the results of the experiments performed on the office floor. figure 2e and 2e show the results for the artificial grass. experimental results performed on the inclined plane are shown in figure 2c and figure 2f. finally, the results from traversing the wooden blocks are presented in figure 2g. the experiments have been run three times for each terrain type and gait. therefore, results from the particular trials have been grouped and marked by a specific color in the plots. each color represents one gait pattern, and thus each color group consists of three lines that correspond to the three experiments performed for every gait and terrain type. 3.3. discussion in figure 2, we can clearly see that a gait selection can significantly influence the energy efficiency of the robot motion. tables 1 and 2 and figure 3 together with figure 4 summarize the overall energy consumption and the time needed for traversing the terrain (a distance of 1 m) by each motion gait. the results were computed as the mean values of the data resulting from each triplet of the performed experiments. according to table 1, we can establish a strategy for gait selection to prefer the default tripod gait whenever the particular terrain type can be traversed by it. in rough terrains, the adaptive tripod gait is preferred. considering the time in table 1, the switching strategy that minimizes the time consumption (the speed of the robot) yields the same result. however, such a gait selection rule optimizes only the energy and time consumption. different optimization criteria might be induced by the application scenario, e.g., the tripod gait is the least safe gait in terms of the robot stability, and thus it is not capable of traversing such challenging terrains as the pentapod gait, which is the most stable gait. the results presented above indicate the influence of the energy consumption is proportional to the time by a multiplication factor. the factor can be utilized as a single parameter describing the energy efficiency of the gait pattern on a particular terrain type. the multiplication factor actually coincides with the average power consumed by the robot. moreover, the average power might be used as a characteristic for the terrain classification. however, to get relevant information about an average power, we need to collect data over a longer time interval because the instantaneous power changes signif8 vol. 6/2016 on evaluation of motion gaits energy efficiency gait consumed energy [j] floor grass plane blocks def. tripod 130.9 144.0 148.3 — def. tetrapod 168.7 183.0 200.9 — def. pentapod 289.7 327.9 403.2 — def. ripple 171.9 183.7 218.4 — ad. tripod 386.6 482.5 485.6 507.6 ad. tetrapod 543.1 617.0 699.0 700.0 ad. pentapod 1019.1 1248.7 1543.4 1270.3 table 1. energy consumption. office floor artificial grass inclined plane wooden blocks 0 200 400 600 800 1000 1200 1400 1600 c on su m ed e ne rg y [j ] consumed energy adaptive pentapod adaptive tetrapod adaptive tripod regular pentapod regular tetrapod regular tripod figure 3. energy consumption on different terrain types. icantly during a single gait cycle. this can be observed for the terrain of wooden blocks as fluctuations of otherwise relatively straight lines in figure 2. based on the presented results, we can deduce that the time interval of few seconds (or few gait cycles) should be sufficient to provide the relevant data. notice, the wooden blocks are not, unlike the other terrain types, uniform, and therefore, fluctuations in the estimated energy consumption may be observed in the presented results. the energetic cost together with the traversability of the terrain vary from place to place and they both depend on exact location of the robot in the environment. this observation motivate us that a terrain classification might divide the area into smaller parts and evaluate traversability in these local areas. notice that all the gait parameters such as speed, stride length, etc. were fixed for each gait individually for all experiments reported in this paper. however, the energy efficiency can be used in the optimization of the gait and it can be also improved by a mechanical construction of the robot. a further experimental evaluation can also be enhanced by a precise measurement of the distance traveled by the robot. in this manner, factors such as traction and leg slippages can be taken into account, which may provide additional information about suitability of particular gaits for specific terrain types. gait time [s] floor grass plane blocks def. tripod 8.1 8.1 8.1 — def. tetrapod 12.2 12.2 12.2 — def. pentapod 24.4 24.4 24.3 — def. ripple 12.3 12.2 12.2 — ad. tripod 32.6 35.8 35.7 35.7 ad. tetrapod 56.5 56.6 57.3 56.1 ad. pentapod 110.6 112.5 114.6 95.8 table 2. traversing time. office floor artificial grass inclined plane wooden blocks 0 20 40 60 80 100 120 140 c on su m ed ti m e [s ] consumed time adaptive pentapod adaptive tetrapod adaptive tripod regular pentapod regular tetrapod regular tripod figure 4. traversing time on different terrain types. 4. conclusion in this work, we study the problem of energetic characteristics of the hexapod legged robot locomotion. we have evaluated the consumed energy for the most common motion gait types and different terrain types. from the presented experimental results, we can observe that the default tripod gait is the fastest and the most energy efficient gait for flat terrains. this observation yields the main strategy for the gait switching rule that minimizes the overall energy consumption. the gait switching rule can be formulated such as whenever the default gait is not capable of traverse a terrain due to the terrain roughness, its adaptive version should be preferred. the results indicate the proportional relation between the operational time and the energy consumption, which, in fact, is not a surprising result. however, the multiplication factor can be used as a characteristic for the terrain classification. all the proposed applications and implications of presented results are intended as a motivation for further research. a deployment of the gait switching decision rule and further investigation of the gait optimal parametrization using the energy characteristics evaluation is of our particular interest. acknowledgements the presented work was supported by the czech science foundation (gačr) under research project no. 15-09600y. the support of grant no. sgs16/235/ohk3/3t/13 to petr čížek is also gratefully acknowledged. 9 l. černý, p. čížek, j. faigl acta polytechnica ctu proceedings references [1] d. belter, p. skrzypczynski. rough terrain mapping and classification for foothold selection in a walking robot. journal of field robotics 28(4):497–528, 2011. doi:10.1002/rob.20397. [2] j. mrva, j. faigl. tactile sensing with servo drives feedback only for blind hexapod walking robot. in robot motion and control (romoco), 2015 10th international workshop on, pp. 240–245. 2015. doi:10.1109/romoco.2015.7219742. [3] n. kottege, c. parkinson, p. moghadam, et al. energetics-informed hexapod gait transitions across terrains. in ieee international conference on robotics and automation (icra), pp. 5140–5147. 2015. doi:10.1109/icra.2015.7139915. [4] j. mrva, m. stejskal, j. faigl. on traversability cost evaluation from proprioceptive sensing for a crawling robot. in acta polytechnica ctu proceedings, pp. 34–39. 2015. doi:10.14311/app.2015.1.0034. [5] g. dudek, m. jenkin. computational principles of mobile robotics. cambridge university press, new york, ny, usa, 2000. [6] j. mrva, j. faigl. tactile sensing with servo drives feedback only for blind hexapod walking robot. in 10th international workshop on robot motion and control, romoco, pp. 240–245. 2015. doi:10.1109/romoco.2015.7219742. 10 http://dx.doi.org/10.1002/rob.20397 http://dx.doi.org/10.1109/romoco.2015.7219742 http://dx.doi.org/10.1109/icra.2015.7139915 http://dx.doi.org/10.14311/app.2015.1.0034 http://dx.doi.org/10.1109/romoco.2015.7219742 acta polytechnica ctu proceedings 6:6–10, 2016 1 introduction 2 problem statement 2.1 hexapod platform 2.2 motion gaits 2.3 energetics 3 evaluation 3.1 experimental set-up 3.2 results 3.3 discussion 4 conclusion acknowledgements references 238 acta polytechnica ctu proceedings 2(1): 238–241, 2015 238 doi: 10.14311/app.2015.02.0238 spectroscopic monitoring observations of nova v1724 aql in 2012 t. kajikawa1, m. nagashima1, h. kawakita1, a. arai1,2, y. ikeda1,3, m. isogai1,4, m. fujii5, k. ayani6 1kyoto sangyo univearsity / koyama astronomical observatory 2university of hyogo / nishi-harima astronomical observatory 3photocoding 4national astronomical observatory of japan 5fujii-kurosaki observatory 6bisei astronomical observatory corresponding author: kawakthd@cc.kyoto-su.ac.jp abstract spectroscopic and photometric monitoring observations of nova apl 2012 (v1724 apl) were conducted at koyama astronomical observatory, fujii-kurosaki observatory and bisei astronomical observatory. the nova was initially considered as an outbursting pre-main-sequence young stellar object. our monitoring observations have revealed the nova to be a fe ii type classical nova. the temporal evolution of spectra and light curves of the nova were similar to those of a slow nova (e.g., v1280 sco and v5558 sgr). we observed no evidence of molecule formation in v1724 aql in contrast with v2676 oph in which dust formation occurred after the molecular formation in the nova outflow. keywords: cataclysmic variables classical novae optical spectroscopy photometry individual: v1724 aql. 1 introduction nova aql 2012 (later named as v1724 aql) was discovered on 2012 october 20.4 ut (nishiyama & kabashima 2012). the brightness of the nova during the discovery was reported as 12.6 mag. just after the discovery, we conducted our spectroscopic monitoring observations at the koyama astronomical observatory (kao), fujii-kurosaki observatory (fko) and bisei astronomical observatory (bao) in japan. the first optical spectrum taken on october 21.4 ut was reported by fujii (2012) at fko. the object showed a sharp hα emission ( probably with a p cygni profile) on a very red continuum. this object was considered a classical nova affected by a severe interstellar extinction (strong absorption of the na d line was observed). munari (2012) also reported that the spectrum of this object on october 21.8 ut showed a weak and sharp hα emission on a very red continuum, with strong na i and ba ii absorption lines. this spectrum was basically consistent with that reported by fujii (2012). however, it was considered that the spectrum is more similar to that of an outbursting premain-sequence young stellar object than that of a nova before maximum brightness. on 2012 october 23.5 ut, ayani (2012) also reported the optical spectrum of this object taken at bao, with fe ii emission and o i emission with a p cygni profile. this object was finally identified as a fe ii type classical nova according to the classification by williams (1992). here we report the spectroscopic and photometric observations of v1724 aql performed in a collaboration among three observatories (kao, fko and bao) in japan. 2 spectroscopic and photometric observations the observations conducted in our collaboration were follows. spectroscopic observations were performed at three sites: 1. a 0.4-m telescope with a low-dispersion spectrograph (λ = 4500 — 9000 å with r ∼ 500) at fujii-kurosaki observatory, 2. a 1.01-m telescope with a lowand moderatedispersion spectrograph (λ = 3600 — 9000 å with r ∼ 1500 for a low-resolution mode) at bisei astronomical observatory, and 3. a 1.3-m araki telescope with a low-dispersion 238 http://dx.doi.org/10.14311/app.2015.02.0238 spectroscopic monitoring observations of nova v1724 aql in 2012 spectrograph losa/f2 (λ = 3800 — 8000 å with r ∼ 600; shinnaka et al. 2013) at koyama astronomical observatory. in addition to the spectroscopic observations, photometric observations were performed at kao by the imaging camera adler (araki dual-band imager; nakagawa et al. 2013) with intermediate and broadband filters (y-, i′-, and z′-band filters). figure 1 shows the spectral evolution of v1724 aql. figure 2 shows the light curves (with the multi-band light curves taken from aavso database). we also show the close-up views for hα and o i emission lines to make clear the evolution of their line shapes. clearly, the line widths increased for later epochs in the case of hα while the temporal change in the p cygni profile of o i emission indicated faster expansion velocities at later dates. 0 5 10 15 20 25 4000 5000 6000 7000 8000 9000 wavelength [a] +35d:k +26d:k +25d:f +24d:f +22d:f +22d:k +17d:k +16d:f +16d:k +10d:k +8d:k +5d:f +4d:k +4d:b +4d:f +3d:f +2d:f +2d:b +1d:k +0d:f h β f e ii (7 4) f e ii (7 4) f e ii (7 4) o i ( 77 74 ) n a i( 58 89 ) m gi i+ o i o i( 84 46 ) f e ii (4 2) h α[o i] (6 30 0) c a ii k: kao f: fko b: bao lo g ( f lu x) + c on st . 10 figure 1: low-dispersion spectra of v1724 aql obtained at three sites from 2012 oct 21 to nov 25 ut. all spectra are shifted by different offsets for readability. emission lines were on the highly red continuum. the line width of hα emission became broader and stronger compared with the nearby continuum, and the ca ii triplet emission lines bacame stronger later. note that the bluish continuum might overlap with the spectra of the nova in the shorter wavelength region (λ < 4500 å ), probably due to a forground (or background) star. 239 t. kajikawa et al. 3 discussion and conclusion from the viewpoint of the spectral evolution, the spectra of v1724 aql slowly changed during the period of our observations. emission lines (hα, hβ, fe ii, na i, o i and ca ii) were on the reddened continuum. we estimated e(b − v ) based on the measurements of balmer decrement by the method described in helton et al. (2010), e(b − v )∼3.1, which indicated severe interstellar extinction for the nova. this value is slightly higher than that reported by rudy et al. (2012) but both values indicate severe interstellar reddening. note that the spectra of the nova showed enhancement in a shorter wavelength region (λ < 4500å ) that appeared similar to a bluish continuum component but was noisier. the nova may be overlapped with another foreground (or background) stellar object that had a high temperature. although one may consider that we should estimate e(b − v ) based on the (b − v ) of the nova around the optical brightness maximum, we had to be careful of the contamination with the b-band brightness of the nova. 8 9 10 11 12 13 14 15 16 17 18 19 0 5 10 15 20 25 30 35 40 45 m ag ni tu de s days from 2012 oct 20 ut v r i b y i’ z’ figure 2: optical light curves of v1724 aql obtained at kao with the multi-band light curves of the nova taken from aavso database. the vertical tick-marks at the top of panel indicate the dates of our spectroscopic observations. the line width of hα emission had clearly increased and became stronger compared with the nearby continuum, and o i and ca ii triplet emission lines grew at later dates. the ejection velocity was ∼400 km/s based on the p cygni profile of hα at t=1d after the outburst (figure 3). it then increased; 630 km/s (t=2d), 640 and 750 km/s (t=5d), and 1150 km/s (t=9d) based on the p cygni profiles of o i as shown in figure 4. finally, the ejection velocity reached ∼2000 km/s based on the fwzi of hα (figure 3) after the brightness maximum at t=17d. the ejection velocities were slower during the earlier phase, and faster during later phase. such temporal changes in ejection velocity in v1724 aql was similar to those of slow novae, e.g., v1280 sco (naito et al. 2012) and v5558 sgr (tanaka et al. 2011). v1724 aql was similar to a slow nova from the viewpoint of spectral evolution. 0 0.2 0.4 0.6 0.8 1 -4000 -2000 0 2000 4000 r el at iv e flu x velocity [km/s] +10d:k +8d:k +5d:f +4d:k +3d:f +2d:f +1d:k 0d:f 0 0.2 0.4 0.6 0.8 1.0 -4000 -2000 0 2000 4000 r el at iv e flu x velocity [km/s] +35d:k +26d:k +25d:f +24d:f +22d:k +17d:k +16d:k +10d:k figure 3: temporal change of hα emission line before and after the brightness maximum at t=17d after the outburst (upper and lower panels, respectively). the line widths became broader at later dates. the black arrow in the lower panel shows the change in blue-shift component that could have been caused by the change in the velocity structure of the ejected materials. based on the light curves shown in figure 2, nova v1724 aql showed very slow evolution in brightness after the outburst until its brightness maximum in the v band (t=17d, v=13.6±0.2 mag). the visual brightness was almost unchanged (but oscillating with small amplitude) until the brightness maximum since the outburst (14.4±0.4 mag in v -band). the evolution in brightness was slow for v1724 aql in earlier phase. however, after the brightness maximum (t=17d), its brightness in v -band become fainter with a decline rate of +0.14 mag/day (t2 was 14.3 days). although this decline rate was indicative of a fast nova rather than a slow nova (payne-gaposchkin 1957), the light curves after the brightness maximum might be affected by dust formation as suggested by the molecular formation observed by rudy et al. (2012). 240 spectroscopic monitoring observations of nova v1724 aql in 2012 -1 -0.5 0 0.5 1 -4000 -3000 -2000 -1000 0 1000 2000 3000 4000 r el at iv e flu x velocity [km/s] +10d:k +8d:k +4d:k +1d:k figure 4: temporal change of the p cygni profile for o i (7774 å at rest) emission line before the brightness maximum. the measured ejection velocites based on the p cygni profiles were 630 km/s (at t=2d), 640 and 750 km/s (at t=5d), and 1150 km/s (at t=9d). rudy et al. (2012) reported the detection of co molecular emission in the near-infrared spectra taken on 2012 oct 27 and 28 ut (before the brightness maximum), indicating that molecule formation was ongoing, with dust formation likely to follow. nova v1724 aql was probably a slow nova that showed co emission during the pre-maximum halt (at least, before the maximum). however, there were no hints for c2 and cn absorption bands in optical spectra of the nova (c.f. v2676 oph, nagashima et al. 2014). those molecular absorption bands were expected to appear during several days (as in the cases of v2676 oph and dq her). our spectroscopic observations were performed frequently enough to detect them if a considerable amount of molecules formed in the outflow of the nova. we propose the hypothesis that the ejecta of v1724 aql was oxygen-rich and the atomic carbon might not be over-abundant with respect to the atomic oxygen (c < o) in the ejecta. as demonstrated by the model calculations (pontefract & rawlings 2004), formation of c2 (and also cn) is more difficult than co in an oxygen-rich atmosphere. v1724 aql might have oxygen-rich ejecta. the spectroscopic observations of v1724 aql in the nebular phase (if reported in the future) will be helpful to test this hypothesis. references [1] ayani, k. 2012, electronic telegram no. 3273, central bureau for astronomical telegrams, international astronomical union (ed., green, d.). [2] fujii, m. 2012, electronic telegram no. 3273, central bureau for astronomical telegrams, international astronomical union (ed., green, d.). [3] helton, l.a., woodward, c.e., walter, f.m., vanlandingham, k., schwarz, g.j., evans, a., ness, j.-u., geballe, t.r., gehrz, r.d., greenhouse, m., krautter, j., liller, w., lynch, d.k., rudy, r.j., shore, s.n., starrfield, s., & truran, j. 2010, aj, 140, 1347. [4] munari, u. 2012, electronic telegram no. 3273, central bureau for astronomical telegrams, international astronomical union (ed., green, d.). [5] nagashima, m., arai, a., kajikawa, t., kawakita, h., ktao, e., arasaki, t., taguchi, g., & ikeda, y. 2014, apjl, 780, l26. doi:10.1088/2041-8205/780/2/l26 [6] naito, h., mizoguchi, s., arai, a., tajitsu, a., narusawa, s., yamanaka, m., fujii, m., iijima, t., kinugasa, k., kurita, m., nagayama, t., yamaoka, h., & sadakane, k. 2012, a&a, 543, 86. [7] nakagawa, s., noguchi, r., iino, e., ogura, k., matsumoto, k., arai, a., isogai, m., & uemura, m. 2013, publ. of astron. soc. japan, 65, 7. doi:10.1093/pasj/65.3.70 [8] nishiyama & kabashima 2012, electronic telegram no. 3273, central bureau for astronomical telegrams, international astronomical union (ed., green, d.). [9] payne-gaposchkin, c. 1957, the galactic novae. amsterdam:north-holland. [10] pontefract, m., & rawlings, j.m.c. 2004, mnras , 347, 1294. doi:10.1111/j.1365-2966.2004.07330.x [11] rudy, r.j., laag, e.a., crawford, k.b., russell, r.w., puetter, r.c., & perry, r.b. 2012, electronic telegram no. 3287, central bureau for astronomical telegrams, international astronomical union (ed., green, d.). [12] shinnaka, y., kawakita, h., kobayashi, h., naka, c., arai, a., arasaki, t, kitao, e., taguchi, g., & ikeda, y. 2013, icarus, 222, 734. doi:10.1016/j.icarus.2012.08.001 [13] tanaka, j., nogami, d., fujii, m., ayani, k., kato, t., maehara, h., kiyota, s., & nakajima, k. 2011, publ. of astron. soc. of japan, 63, 911. [14] williams, r. e. 1992, aj, 104, 725. 241 http://dx.doi.org/10.1088/2041-8205/780/2/l26 http://dx.doi.org/10.1093/pasj/65.3.70 http://dx.doi.org/10.1111/j.1365-2966.2004.07330.x http://dx.doi.org/10.1016/j.icarus.2012.08.001 introduction spectroscopic and photometric observations discussion and conclusion acta polytechnica ctu proceedings doi:10.14311/app.2017.9.0039 acta polytechnica ctu proceedings 9:39–42, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app surface characterization of titanium alloys for nitrogen ion implantation petr vertata,∗, jan drahokoupilb, petr vlcakc a department of solid state engineering, fnspe ctu in prague, trojanova 13, 120 00, prague 2, czech republic b department of advanced structural materials, institute of physics as cr, na slovance 2, 182 21, prague 8, czech republic c department of physics, fme ctu in prague, technicka 4, 166 07, prague 6, czech republic ∗ corresponding author: vertatp@gmail.com abstract. ion implantation is one of the modern methods of the surface modification of various materials. industrially used ti–6al–4v titanium alloy and commercially pure ti grade 2 were characterized using the x–ray diffraction methods. texture of the material and dependence of the microstructural properties on the method of the surface modification were examined in order to determine suitable conditions for application of the process in the industry. the structure of ti–6al–4v alloy before and after the nitrogen ion implantation process is discussed and observed surface hardening is explained. keywords: ti–6al–4v, ti grade 2, ion implantation, x–ray diffraction. 1. introduction ti–6al–4v titanium alloy (also called ti grade 5) and commercially pure ti grade 2 are materials widely used in the industry and the biomedicine for their low density, high tensile strength, biocompatibility and resistance to corrosion in some common environments. disadvantages of the titanium alloys for their applications are their poor performance in sliding, insufficient surface hardness and insufficient resistance to some chemical environments. for these reasons is the surface of common titanium alloys often modified. nowadays, one of the most suitable surface modification methods seems to be the ion implantation of nitrogen ions into the surface of the sample. it has been shown that mechanical qualities and wear and corrosion resistance of many materials can be improved using this method. concerning the titanium and its alloys, creation of hard tinx phases [1] or stabilization of the α–ti phase [2] leading to the increase of the surface hardness is expected. compared to the other commonly used surface modification methods, the advantages of the nitrogen ion implantation are the ability to control the process precisely (esp. the fluence of the implanted ions, their energy and thus the depth distribution) and so the ability of automating the process and the possibility to implant at the low temperatures. 2. experimental details for purpose of characterizing the sample preparation method and the surface modification using the nitrogen ion implantation the ti–6al–4v (ti grade 5) alloy with a microstructure consisting of the α + β ti phases with a chemical composition of (wt% 0.1% c, 5.50–6.75% al, 3.50–4.50% v, 0.2% o, 0.05% n, 0.0125% h, 0.3% fe and ti balance) and the ti grade 2 consisting mainly of the α-ti phase, chemical composition of (max. wt% 0.08% c, 0.25% o, 0.03% n, 0.015% h, 0.3% fe and ti balance), were examined. the disc samples were cut from commercially available bars, ground and polished with a diamond paste in order to obtain a flat smooth surface suitable for the ion implantation. phase composition of the polycrystalline samples, microstrain and texture were determined using the x–ray diffraction. data were measured on the panalytical x’pert pro horizontal powder diffractometer with a cobalt anode (λkα1= 0.1789 nm) using the divergent bragg-brentano geometry and parallel beam geometry. for pole figures measurements the atc–3 texture cradle was used allowing rotation of the sample in the φ angle, change of the inclination angle χ and horizontal movement of the sample. for temperature dependences the htk 2000 heating chamber was used. measured data were processed by rietveld analysis using the topas 3 software. in this method the measured diffraction pattern is compared with the calculated one and the input parameters are varied on the basis of differences between them. for the calculation of diffraction pattern, this program uses so called "fundamental parameter approach" [3], i.e. that the calculated diffraction profile is based on convolution of particular contributions to the total profile. three components of diffraction peak broadening are taken into account: an instrumental broadening, an average crystallite size and microstrains. thus 39 http://dx.doi.org/10.14311/app.2017.9.0039 http://ojs.cvut.cz/ojs/index.php/app p. vertat, j. drahokoupil, p. vlcak acta polytechnica ctu proceedings figure 1. measured diffraction patterns of the ti–6al–4v and ti grade 2 samples. figure 2. detailed diffraction diagram of the ti– 6al–4v sample. both present titanium phases: α–ti and β–ti are marked using different colors and their reflections are indexed. rietveld fit of the measured data is marked with red color. precise determination of average crystallite sizes and microstrains is possible. the pole figures for reflections 100, 002, 110 and 101 were measured using the reflection geometry. the inability of this method to measure the whole pole figures was solved by calculation of the odf function followed by recalculation of desired pole figures. the background and defocusing corrections were applied using the homemade software. calculation of the odf and recalculation of the pole figures were made in the x’pert texture program. in order to verify the effect of the nitrogen ion implantation on the surface properties of the ti– 6al–4v alloy and in order to explain such possible effect, samples were implanted using the ion implanter tecvac 221 in conventional setup the fluency of figure 3. detailed diffraction diagram of the ti grade 2 sample, only the α–ti phase (blue line, corresponding miller indices are shown) is present. rietveld fit of the measured data is marked with red color. 6·1017 cm−2 and the 90 kev accelerating voltage at the temperatures lower than 80 ◦c. 3. results and discussion 3.1. samples characterization before the nitrogen ion implantation ti–6al–4v and ti grade 2 samples were examined using the methods of the x-ray diffraction analysis, measured diffraction patterns are shown in figure 1. differences in the peak positions are caused by the different chemical compositions of the alloys. measurements of the ti–6al–4v sample (detailed view in figure 2) showed the presence of two titanium structures: hexagonal α–ti (76%) phase and cubic β–ti (24%). in the ti grade 2 sample only α–ti phase 40 vol. 9/2017 surface characterization of ti alloys for ni ion implantation figure 4. recalculated direct pole figures of the 002, 010, 011 and 110 reflections of the ti grade 2 sample. figure 5. detail of the diffraction profile of the ti grade 2 sample (reflection 211 of the α–ti phase) after different preparation treatment. was present. diffraction diagram of ti grade 2 sample after the electro-polishing might be seen in figure 3. the texture analysis shows the samples are textured (figure 4). the crystallographic direction 001 has low rate in the direction that is normal to the surface of the sample. although the samples physicaly have the rotational symmetry, the pole figures reveal only the mirror symmetry of the inner microstructure. this has to be taken into account when doing other xrd measurements, namely measurements with the inclined sample or with fixed incident angle. influence of the sample preparation on the microstructure of ti grade 2 has also been studied. detailed look on the diffraction profiles of the sample treated only by grinding and polishing using the diamond paste reveals broadening of the diffraction lines indicating lower crystallite size and higher microstrain in the structure. considerable asymmetry indicates the depth gradient of the macroscopic residual stress (figure 5). in an effort to eliminate such effects that have arisen due to the preparation of the sample, influence of the electrolytic polishing and annealing on the microstructure was examined. figure 6. time dependence of the microstrain during the annealing of the ti grade 2 sample. annealing temperatures are distinguished using different colors. initial value at the room temperature obtained after grinding and polishing the sample using a diamond paste is also shown. absolute error < 0.003 %. diffraction profiles measured after the mentioned procedures are shown in figure 5. measured influence of the annealing at different temperatures (300 ◦c, 400 ◦c and 500 ◦c) on the microstrain is shown in figure 6 representing the time dependence of this quantity. the dominant effect of removing the residual microstresses is reached during the first minutes after reaching particular temperature. for the temperature of 300 ◦c there is no visible progress after several minutes at all. for higher temperatures there is a jump followed by a continuous decreasing of microstrains. the results show sufficient decrease of the microstrain value when compared with the initial state of the sample after its necessary treatment by grinding and polishing using the diamond paste. however, the influence of the sample preparation is not eliminated completely. state closest to the initial microstructure of the bulk sample is revealed (according to figure 5) by the electro-polishing. under the common circumstances 41 p. vertat, j. drahokoupil, p. vlcak acta polytechnica ctu proceedings figure 7. depth profile of the indentation hardness measured on ti–6al–4v sample before and after the nitrogen ion implantation. [4] values influenced by the relative error originating from the calibration ∼ 10 %. this method of the surface treatment can be considered as the most suitable one. regarding the ti–6al–4v alloy, analogous behavior can be expected. 3.2. samples characterization after the nitrogen ion implantation after the nitrogen ion implantation into ti–6al–4v samples using the suitable implantation parameters, desired surface hardening is observed as proven by the typical depth profile of the nanoindentation hardness (figure 7) [4]. phase composition of the ti–6al–4v samples after the implantation with parameters described in section 2 was characterized. in addition to hexagonal α–ti and cubic β–ti phases observed before the implantation, two new phases were detected: smaller amount of the solid solution α–ti(+n) and majority of the tin solid phase. formation of these two phases describes the mechanism of observed surface hardening in our alloy. dependences of different implantation parameters on concrete phase composition and mechanical properties of mentioned titanium alloys are now the object of further research. 4. conclusions samples of ti–6al–4v (ti grade 5) and ti grade 2 alloys were characterized by the x–ray diffraction methods. texture in the samples of such commonly available materials and improvement of their microstructural properties by annealing at different temperatures and by electro-polishing were discussed. best results were obtained using the last method. presented results create the precondition for a further research in the field of functionalizing the surface of ti–6al–4v and ti grade 2 alloys aiming mainly at characterizing the influence of various ion implantation parameters on the phase composition and physical properties of these materials for their future application in the industry and biomedicine. acknowledgements authors thank dr. j. sepitka for the nanoindentation measurements. this work was supported by the grant agency of the czech technical university in prague, grant no. sgs16/245/ohk4/3t/14, and czech science foundation, grant no. 16-22276s. references [1] y. z. liu, x. t. zu, s. y. qiu, j. cao, c. x. li, x. q. huang, c. f. wei: phase formation and modification of corrosion property of nitrogen implanted tialv alloy. vacuum 81 (1):71–76, 2006. doi: 10.1016/j.vacuum.2006.02.013 [2] h. schmidt., a. schminke, m. schmiedgen, b. baretzky: compound formation and abrasion resistance of ionimplanted ti6al4v. acta mater. 49 (3):487–495, 2001. doi: 10.1016/s1359-6454(00)00326-8 [3] r. w. cheary, a. a. coelho, j. p. cline: fundamental parameters line profile fitting in laboratory diffractometers. j. res. natl. inst. stand. technol. 109:1–25, 2004. doi: 10.6028/jres.109.002 [4] p. vlcak, f. cerny, j. drahokoupil, j. sepitka, z. tolde: the microstructure and surface hardness of ti6al4v alloy implanted with nitrogen ions at an elevated temperature. j. alloys compd. 620:48–54, 2015. doi: 10.1016/j.jallcom.2014.09.125 42 acta polytechnica ctu proceedings 9:39–42, 2017 1 introduction 2 experimental details 3 results and discussion 3.1 samples characterization before the nitrogen ion implantation 3.2 samples characterization after the nitrogen ion implantation 4 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2016.6.0001 acta polytechnica ctu proceedings 6:1–5, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app on construction of a reliable ground truth for evaluation of visual slam algorithms jan bayer∗, petr čížek, jan faigl czech technical university, faculty of electrical engineering, technicka 2, prague, czech republic ∗ corresponding author: bayerja1@fel.cvut.cz abstract. in this work we are concerning the problem of localization accuracy evaluation of visual-based simultaneous localization and mapping (slam) techniques. quantitative evaluation of the slam algorithm performance is usually done using the established metrics of relative pose error and absolute trajectory error which require a precise and reliable ground truth. such a ground truth is usually hard to obtain, while it requires an expensive external localization system. in this work we are proposing to use the slam algorithm itself to construct a reliable ground truth by offline frame-by-frame processing. the generated ground truth is suitable for evaluation of different slam systems, as well as for tuning the parametrization of the on-line slam. the presented practical experimental results indicate the feasibility of the proposed approach. keywords: rgb-d slam, localization, ground truth construction, legged robot, rough terrain traversal, adaptive motion gait. 1. introduction reliable localization is an essential prerequisite in many practical robotic scenarios, thus its accuracy is the most important parameter in the evaluation of newly developed localization techniques. there are numerous methods based on various principles that can localize the robot in its operational environment. however, when benchmarking such localization methods it is necessary to use a reliable ground truth together with some established metrics (e.g. [1, 2]). in this work, we address the problem of localization accuracy assessment in a visual simultaneous localization and mapping (slam) task [3]. in principle, it is possible to use publicly available datasets, e.g., the freiburg uni dataset [1], the rgb-d slam dataset [2], or the kitty dataset [4], to evaluate the accuracy of slam method. however, our particular environment, setup, and sensory equipment might not exhibit similar properties as the ones used in these standardized datasets. therefore we need to construct our own dataset and acquire a ground truth to assess the localization accuracy. all the above-mentioned datasets are supplied with a centimeter-level precision ground truth provided by an external localization system like a differential gps [4], which is based on a standard gps enhanced with ground reference stations with known geospatial positions. other types of external localization systems used in publicly available datasets are motion capture system [2] or a total station [5]. the former utilizes the data captured by camera sensors to localize the robot marked with special patterns well-distinguishable in the environment. the later measures distance between the observed object and the static ground station using time of flight principle. a 3-dof position of the robot in a global reference frame is obtained from figure 1. experimental environment the distance and the angles measured by the total station. however, acquisition of a reliable ground truth using any of the mentioned localization techniques might be a considerable problem while all of the aforementioned principles are very expensive. thus we are proposing to use the dataset itself for the ground truth construction by offline frame-by-frame processing of the dataset using the slam algorithm. in such a case, we are not interested in an on-line performance of the algorithm rather than the reliability and accuracy of the constructed trajectory estimate to be used as a ground truth. such a processing is assumed to provide the best trajectory estimate for the given dataset and localization technique. moreover, by taking into account certain factors in the dataset construction., which are discussed further in this paper, it is possible to improve the reliability of the generated ground truth. 1 http://dx.doi.org/10.14311/app.2016.6.0001 http://ojs.cvut.cz/ojs/index.php/app j. bayer, p. čížek, j. faigl acta polytechnica ctu proceedings to verify our hypothesis, we are reporting on the results of such a ground truth construction evaluation based on the rgb-d slam method [6] compared to the ground truth provided by the whycon motion capture system [7]. we evaluated the proposed approach on a challenging dataset obtained with the rgb-d camera mounted on a hexapod walking robot crawling in rough terrain (see fig. 1). such a scenario requires full 6-dof position estimation, while the camera is subjected to unpredictable motion and the resulting dataset is very different in comparison to all the standardized datasets obtained mainly by wheel platforms. the presented approach to ground truth construction is somehow similar to the task of structure-frommotion studied in computer vision community. in [8], the authors use color images from the rgb-d microsoft kinect camera to recover its pose, but for the scene and object recognition purposes. however, in our work we are focusing solely on the localization accuracy rather than the quality of the model (map) of the environment. the paper is structured as follows. section 2 explains our method of getting the ground truth for the evaluation and the used evaluation metrics. the set-up of a practical experiment together with the evaluation results are described in section 3. conclusion and remarks for future work are dedicated to section 4. 2. proposed solution the main motivation of our work is to provide a reliable ground truth estimate whenever a precise external localization is not available to be used as the ground truth. for this reason, we are proposing to use the captured dataset and process it with a slam system offline frame-by-frame with special settings of parameters to minimize the trajectory error. afterward, the resulting trajectory estimate can be used as a ground truth to compare to the online generated trajectories, while in deployment scenarios we are interested in the online performance of slam methods. such an estimated ground truth can be used to compare different slam methods or to find the best parametrization for the online slam trajectory estimation. 2.1. evaluation metrics the slam algorithms can be compared either by the quality of the generated map or the accuracy of the estimated trajectory. as the evaluation metrics, we use the established metrics of ate (absolute trajectory error) and rpe (relative pose error) presented in [2]. ate is given as: fi = q−1 i spi, (1) where q−1 i is transformation matrix, which maps (i + 1)th point of ground truth to ith point of ground truth. pi is a similar matrix, which maps ith point of the estimated trajectory to the (i + 1)th point of the trajectory. s is a transformation matrix, which aligns the estimated trajectory to the ground truth. ate measures the absolute error of all estimated 6-dof positions, which means that ate can be represented by atet and ateφ, where atet are euclidean distances between estimated poses and corresponding ground truth positions and ateφ is the absolute error of the estimated orientations. rpe measures the drift of the estimated trajectory (error in shape of the trajectory estimate) and it is given by the equation: ei = (q−1 i qi+∆)−1(p−1 i pi+∆), (2) where ∆ defines a fixed frame interval. we used ∆ = 1 for the evaluation, which means that rpe measures a drift of visual odometry. rpe can be also represented by rpet (the relative translational error) and rpeφ (the relative rotational error). 3. evaluation to test our hypothesis and prove its feasibility we designed a practical experiment where we evaluated the localization accuracy provided by an offline frame-byframe processing of a visual slam dataset captured by a hexapod robot traversing rough terrain with a ground truth provided by an external localization system. in particular, we focused on evaluation with the structured light camera and rgb-d slam algorithm based on [6]. we choose to use the structured light sensor because it is inexpensive and provide the slam method with a metric information unlike the stereo and monocular slam methods which can estimate the trajectory up to scale. for the establishment of a reliable ground truth, we used motion capture system whycon [7] which tracks the circular markers attached to the robot using two logitech hd pro webcam c920 cameras. used external localization provided centimeter-level precision ground truth. we used the rgb-d camera asus xtion pro for the visual slam, which acquires a color image and also depth measurements. the experimental dataset captured using the rgb-d camera mounted on a hexapod walking platform contains sequences of rgb and depth images in full asus xtion pro resolution 640 × 480 px at 10 frames per second. the whole dataset for the evaluation was captured using the ros framework [9]. 3.1. rgb-d slam the considered rgb-d slam system is based on [6] and it operates as follows. first positions of the salient image features are extracted from the rgb image supplemented by their depth provided by the rgb-d sensor. then, a rigid transformation is found 2 vol. 6/2016 on construction of a reliable ground truth frame-by-frame processing online processing trial atet ateφ rpet rpeφ end dist. atet ateφ rpet rpeφ end dist. [cm] [rad] [cm] [rad] [cm] [cm] [rad] [cm] [rad] [cm] no. 1 4.00 – 0.92 – 7.11 9.60 – 1.13 – 3.5 no. 2 4.32 – 0.54 – 12.54 8.13 – 0.56 – 8.93 no. 3 3.68 – 0.40 – 5.21 22.02 – 0.87 – 33.15 no. 4 9.97 0.08 1.21 0.01 9.13 12.50 0.09 1.31 0.01 7.12 no. 5 11.44 0.06 0.80 0.01 15.96 15.64 0.06 0.94 0.02 27.55 table 1. trajectory estimation results y [m] ground-truth and rgb-d slam trajectories 1 0.5 0 -0.5 -12 x [m] 1 0 1.5 -1 -0.5 0 0.5 1 z [ m ] ground-truth rgb-d slam (a) . no.3 y [m] ground-truth and rgb-d slam trajectories 1 0.5 0 -0.5 -12 x [m] 1 0 0.5 -0.5 0 1 z [ m ] ground-truth rgb-d slam (b) . no.4 y [m] ground-truth and rgb-d slam trajectories 1 0 -1 2 x [m] 1 0 1.5 1 -1 0.5 0 -0.5 z [ m ] ground-truth rgb-d slam (c) . no.5 figure 2. trajectory estimation results. using the ransac [10] algorithm between the currently processed frame and a subset of already mapped frames. this subset consists of np directly preceding frames, ng graph neighboring frames and nr random frames from the whole map which serves to detect large loop closures. the estimated pose is then added to the map (pose graph) and refined using the g2o graph optimizing algorithm [11]. the optimization is especially beneficial in case of large loop closures when the whole trajectory estimate is improved. 3.2. experimental setup experimental environment (see fig. 1) that has been used for capturing of the dataset consists of a plane, low stairs, ramp, and square filled with wooden blocks of different heights. the dataset has been captured by a hexapod walking robot equipped with adaptive motion gait [12] which enables the robot to traverse difficult obstacles. the robot was guided by an operator along the squared path of approx. 9 m length. our experimental environment has been designed to represent some basic problems, which can slam method face. these include high speed of rotation at the corners of the trajectory, which affects the precision of rotation estimation. the stairs and wooden blocks parts of the trajectory force angular rotations along the geometrical axis and the descending ramp force the slam method to deal with the limited number of image features. moreover, the locomotion of the hexapod robot induces unpredictable and abrupt camera motions during the whole trajectory. 3.3. results altogether 5 trajectories were captured and analyzed in order to test our hypothesis. ground truth for the first three trajectories; however, does not contain information about the heading of the robot, and thus only translational component of the ate and rpe can be verified. the considered rgb-d slam parametrization for the frame-by-frame dataset processing has been the surf [13] feature extractor detecting 600 features and keeping 400 best matches with a very long comparison horizon of np = 16, ng = 4 and nr = 1. ransac stopping criteria have been set to 85% of inliers and 1000 iterations considering point an inlier if it is not outside the range of 3 pixels. optimization precision has been set to the best values optimizing each individual frame. such a processing took more than 4 hours per one trajectory on intel core i5 machine. to show the feasibility of our approach we processed the dataset online as well. the parametrization for the online processing has been the surf feature extractor detecting 400 features and keeping 250 of them, np = 3, ng = 3 and nr = 1 with 500 ransac iterations and optimization after every 10 frames. such a processing achieves an online performance of average 5.2 frames per second on the same evaluation hardware. the results are summarized in table 1. resulting trajectories for trials no. 3, no. 4 and no. 5 are depicted in figure 2. 3 j. bayer, p. čížek, j. faigl acta polytechnica ctu proceedings 3.4. discussion table 1 indicates that an average atet, when using frame-by-frame processing, is about 1% of the trajectory length and the average rpet is under 1 cm. notice the atet and rpet values are always higher for the online processing results. on the other hand, differences in the ateφ and rpeφ are neglectable although the slight imperfections in the orientation estimation are the most influencing factor in the accuracy of the localization [14]. the results also indicate that the frame-by-frame processing provides the best result obtainable by a given slam method. thus, it is possible to use the estimated ground truth for the evaluation of the online versions of the same algorithm to find the best parametrization which is deployable online onboard of the mobile robot. note, the resulting localization accuracy is also greatly influenced by the loop closure in case the robot visits previously mapped location. if there is no loop closure, then the trajectory estimate is given as the visual odometry only, which error is asymptotically unbound. in case the loop closure is detected, the optimization process corrects the pose estimates along the whole trajectory. the phenomenon is illustrated in figure 2c, where the loop did not close; thus, the trajectory estimate exhibits higher error in the end part of the trajectory, and figure 3 which presents the results of the frame-by-frame processing of the same trajectory with open-loop enabled and disabled. the results for the closed-loop trajectory are atet = 4.19 cm, rpet = 0.94 rad·10−2 and end dist = 7.33 cm, while for the open-loop trajectory are atet = 8.72 cm, rpet = 0.96 rad·10−2 and end dist = 13.73 cm. although the drift of the visual odometry represented by the rpet is similar in both cases, the resulting end distance and absolute trajectory error are higher when the open-loop scenario is considered. thus, we recommend designing the experimental trajectory to exploit the loop closures to obtain a better ground truth estimate. note the prerequisite of our method is that there are no systematic errors, which can significantly decrease the precision of ground truth estimate. to avoid systematic errors we recommend to use a special shape of the robot’s path, e.g., square. 4. conclusion in this paper, we have studied the problem of the localization accuracy assessment in a slam task whenever a reliable ground truth provided by an external localization system is not available. we have proposed to use frame-by-frame processing of the captured dataset to obtain a sufficiently reliable ground truth for the quantitative evaluation of the online slam systems. the estimated ground truth is then suitable for the comparison of different slam methods or determination of the best parametrization of the online slam. note, the important thing for the dataset creation is ground-truth and rgb-d slam trajectories -2 -1.5 x [m] -1 -0.5 0 1.5 1 0.5 y [m] 0 -0.5 0 0.6 0.4 0.2 z [ m ] ground-truth closed-loop open-loop figure 3. comparison of closed-loop and open-loop frame-by-frame processed trajectories the loop closing, which can significantly improve the robot localization and it is also important to design the shape of the path in order to avoid systematic errors. we tested the presented method with a hexapod crawling robot and rgb-d slam system, but we suppose that the proposed method is applicable to different slam methods and different platforms too. presented results support the feasibility of the proposed approach and can be utilized in cases when expensive and hard to setup external localization systems are not available or suitable. acknowledgements the presented work was supported by the czech science foundation (gačr) under research project no. 15-09600y. the support of grant no. sgs16/235/ohk3/3t/13 to petr čížek is also gratefully acknowledged. references [1] r. kümmerle, b. steder, c. dornhege, et al. on measuring the accuracy of slam algorithms. autonomous robots 27(4):387–407, 2009. doi:10.1007/s10514-009-9155-6. [2] j. sturm, n. engelhard, f. endres, et al. a benchmark for the evaluation of rgb-d slam systems. in ieee international conference on intelligent robots and systems, pp. 573–580. 2012. doi:10.1109/iros.2012.6385773. [3] s. thrun, w. burgard, d. fox. probabilistic robotics. mit press, 2005. doi:10.1162/artl.2008.14.2.227. [4] m. menze, a. geiger. object scene flow for autonomous vehicles. in conference on computer vision and pattern recognition, pp. 3061–3070. 2015. doi:10.1109/cvpr.2015.7298925. [5] n. sünderhauf, k. konolige, s. lacroix, p. protzel. visual odometry using sparse bundle adjustment on an autonomous outdoor vehicle, pp. 157–163. springer berlin heidelberg, 2006. doi:10.1007/3-540-30292-1_20. [6] f. endres, j. hess, n. engelhard, et al. an evaluation of the rgb-d slam system. in ieee international conference on robotics and automation, pp. 1691–1696. 2012. doi:10.1109/icra.2012.6225199. 4 http://dx.doi.org/10.1007/s10514-009-9155-6 http://dx.doi.org/10.1109/iros.2012.6385773 http://dx.doi.org/10.1162/artl.2008.14.2.227 http://dx.doi.org/10.1109/cvpr.2015.7298925 http://dx.doi.org/10.1007/3-540-30292-1_20 http://dx.doi.org/10.1109/icra.2012.6225199 vol. 6/2016 on construction of a reliable ground truth [7] t. krajník, m. nitsche, j. faigl, et al. a practical multirobot localization system. journal of intelligent & robotic systems 76(3-4), 2014. doi:10.1007/s10846-014-0041-x. [8] s. bao. semantic structure from motion. in intl. conf. on computer vision and pattern recognition (cvpr), pp. 2025–2032. 2011. doi:10.1109/cvpr.2011.5995462. [9] m. quigley, k. conley, b. p. gerkey, et al. ros: an open-source robot operating system. in ieee international conference on robotics and automation (icra) – workshop on open source robotics. 2009. [10] m. a. fischler, r. c. bolles. random sample consensus: a paradigm for model fitting with applications to image analysis and automated cartography. communications of the acm 24(6):381–395, 1981. [11] r. kümmerle, g. grisetti, h. strasdat, et al. g2o: a general framework for graph optimization. in ieee international conference on robotics and automation, pp. 3607–3613. 2011. doi:10.1109/icra.2011.5979949. [12] j. mrva, j. faigl. tactile sensing with servo drives feedback only for blind hexapod walking robot. in 10th international workshop on robot motion and control, romoco, pp. 240–245. 2015. doi:10.1109/romoco.2015.7219742. [13] h. bay, a. ess, t. tuytelaars, l. van gool. speeded-up robust features (surf). computer vision and image understanding 110(3):346–359, 2008. doi:10.1016/j.cviu.2007.09.014. [14] p. čížek, j. faigl. on localization and mapping with rgb-d sensor and hexapod walking robot in rough terrains. in ieee international conference on systems, man, and cybernetics, pp. 2273–2278. 2016. 5 http://dx.doi.org/10.1007/s10846-014-0041-x http://dx.doi.org/10.1109/cvpr.2011.5995462 http://dx.doi.org/10.1109/icra.2011.5979949 http://dx.doi.org/10.1109/romoco.2015.7219742 http://dx.doi.org/10.1016/j.cviu.2007.09.014 acta polytechnica ctu proceedings 6:1–5, 2016 1 introduction 2 proposed solution 2.1 evaluation metrics 3 evaluation 3.1 rgb-d slam 3.2 experimental setup 3.3 results 3.4 discussion 4 conclusion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2015.1.0015 acta polytechnica ctu proceedings 2:15–21, 2015 © czech technical university in prague, 2015 available online at http://ojs.cvut.cz/ojs/index.php/app reconnaissance micro uav system petr gabrlika,∗, vlastimil kriza, ludek zaludb a ceitec central european institute of technology, brno university of technology, technicka 3082/12, 616 00 brno, czech republic b faculty of electrical engineering and communication, brno university of technology, technicka 3082/12, 616 00 brno, czech republic ∗ corresponding author: petr.gabrlik@ceitec.vutbr.cz abstract. this paper describes the design and implementation of the uranus uav. this quad-rotor flying robot was created to extend the abilities of the hitherto developed with airborne missions. the first part deals with the mathematical model of the robot. next, the control system is designed, and the proposed hardware as well as the implemented software solution are presented. for integration into the robotic system, a new communication protocol was created and is described here too. keywords: uav, multirotor, robotics, mathematical model, state-space controller. 1. introduction in the research laboratories of ceitec and but, the cassandra robotic system has been developed [1]. this is a heterogeneous group of robots controlled mainly by telepresence from the operator base station. within the described concept, each robot is assigned a specific task, such as reconnaissance, terrain mapping or contamination measurement. the intended purpose of the entire group is to perform these tasks in locations which are dangerous or inaccessible for humans. until recently, this group included only ground robots. in order to enable the group to pursue the assigned tasks from the air or to reach locations unapproachable for ground robots, it was decided to extend the group with a flying robot. to facilitate operation in a closed environment where airplanes can manoeuvre only with difficulty, an aircraft with the ability to hover was required. because airships provide a poor payload/dimensions ratio, helicopters were taken into consideration; the first attempts were carried out with classical machines. however, such helicopters were not robust enough for the intended use in a difficult environment, mainly due to the fact that they contain lot of small moving parts which get easily damaged. quadrotors (and multi-rotor copters in general) have proved to be the best platform for our purposes. the only moving parts on these devices are their rotors rigidly connected to the engines. everything is controlled just by changing their rotor speeds. yet this solution also exhibits a disadvantage, namely internal instability; thus, a control system needs to be implemented to provide the necessary operational ability [2]. currently, quadrotors are being developed within a large number of projects, from hobby to professional ones. after investigating some of these projects, we considered the given status and decided to create our own solution. this approach offers a significant advantage: as the applied software is not license-restricted, figure 1. uranus uav during a flight. we will have full control over the solution and will be able to modify our device if necessary. in this context, a specific airframe and control system were created. to design the control system, the behavior of the designed airframe with rotors was described and mathematical model assembled. 2. quadrotor model the mathematical model of the uranus uav comprises two parts. the first part handles the relation between the speed of the rotors and the forces and torques affecting the quadrotor rigid body. the second portion defines the dynamics of the rigid body, including transformation between frames and effect of gravity force. this separation allows us to design a controller with better dynamics, because the first part of the model can be easily linearized in the controller. the forces and torques caused by propellers of the rotors and affecting the quadrotor rigid body are denoted as u1 to u4. the meaning is as follows: u1 torque around the x axis caused by different thrust of rotors 2 and 4; u2 torque around the y axis caused by 15 http://dx.doi.org/10.14311/app.2015.1.0015 http://ojs.cvut.cz/ojs/index.php/app p. gabrlik, v. kriz, l. zalud acta polytechnica ctu proceedings different thrust of rotors 1 and 3; u3 torque around the z axis caused by different reaction torques from rotors rotating in opposite directions; u4 force in the z axis caused by common thrust of all the rotors. the relation between the thrust and propeller speed of a rotor is ft = kt · n2, (1) and the relation between the reaction torque and propeller speed of a rotor is mr = km · n2. (2) here, kt and km are constants determined by the measurement. the first part of the model then could be described as u1 = (−n2 2 + n2 4)kt l u2 = (n2 1 − n2 3)kt l u3 = (−n2 1 + n2 2 − n2 3 + n2 4)km u4 = (n2 1 + n2 2 + n2 3 + n2 4)kt (3) l denotes the distance between the rotors and the center of gravity of a quadrotor. the second part of the model can be further divided into four parts: equations that describe rotational movement; equations of linear movement; equations describing transformation between frames; and equations expressing the effect of gravity force. all variables are defined in 2 frames: robot frame and ground frame. the robot frame is bound to the uav while the x axis faces forward, y faces right, and z faces down. the ground frame is bound with the ground and oriented north-east-down. rotational movement (robot frame): ω̇x = (iyy − izz)ωyωz + u1 ixx ω̇y = (izz − ixx)ωxωz + u2 iyy ω̇z = (ixx − iyy)ωzωy + u3 izz (4) ixx, iyy and izz represent moments of inertia around a given axis. translation movement (robot frame): v̇x = mωyvz +mωzvy +gx m v̇y = mωxvz +mωzvx +gy m v̇z = mωxvy +mωyvx +gz − u4 m (5) gx, gy and gz are the gravity forces component in a given axis: gx = −mg sin θ gy = mg cos θ sinφ gz = mg cos θ cosφ (6) transformation between the robot frame and ground frame [3]: φ̇ = ωx + ωy sinφ tan θ + ωz cos θ tan θ θ̇ = ωy cos θ − ωz sinφ ψ̇ = ωy sinφ cos θ + ωz cosφ cos θ ẋ = vz(sinφ sinψ + cosφ cosψ sin θ) − −vy(cosφ sinψ − cosψ sinφ sin θ) + +vx cos θ cosψ ẏ = vy(cosφ cosψ + sinφ sin θ sinψ) − −vz(cosψ sinφ− cosφ sin θ sinψ) + +vx cos θ cosψ ż = vz cosφ cos θ − vx sin θ + vy cos θ sinφ (7) the parameters m, l, kt , km of the models was measured and ixx, iyy, izz were computed. the values are as follows: m = 1.05 kg l = 0.35 m kt = 0.14 · 10−6 n ·rpm−2 km = 4.6 · 10−9 nm ·rpm−2 ixx = 8.6 · 10−3 kg ·m2 iyy = 8.6 · 10−3 kg ·m2 izz = 12.0 · 10−3 kg ·m2 (8) 3. controller design to stabilize the uranus uav, a controller based on state space representation of the quadrotor was designed. as shown in sect. 2, the model of the quadrotor comprised 2 parts. the first part handles the non-linear relation between the rotation speed of the propellers and the introduced variables u1 u4 denoting the forces and torques affecting the rigid body. because this part of the model does not contain any dynamics, this relation can be expressed by purely static equations (3). to handle this, a mathematical block with 16 vol. 2/2015 reconnaissance micro uav system inverse function (9) is implemented in the controller. n1 = √ 2kmu2 − kt lu3 + km lu4 4kmkt l n2 = √ −2kmu1 + kt lu3 + km lu4 4kmkt l n3 = √ −2kmu2 − kt lu3 + km lu4 4kmkt l n4 = √ 2kmu1 + kt lu3 + km lu4 4kmkt l (9) this block, together with the first part of the model, will act as a linear section with unitary transfer function (while operating in the working range of the rotor drivers). this allows direct use of the variables u1 u4 as inputs to the system and enables us to treat these parts of the system as linear. the schema of the system with the controller is shown in fig. 2; here, a classical state space controller is extended by few enhancements. the first one is a bias (u4−0) added to the input u4, whose function is to ensure the thrust needed to keep the quadrotor in hover flight. the next one consists in adding a new state iz , which is an integral of the altitude error, z. the purpose of this is to achieve zero steady-state error while hovering, because it is almost impossible to set up a thrust that exactly compensates the gravity force. the design of the state space controller is based on a linearized model of the rigid part of the quadrotor. equations (6) and (7) are linearized around the working point, which is hovering. for the equilibrium point, we have φ = θ = ωx = ωy = 0. (10) to reach this state, the thrust of the rotors must compensate the gravity force acting in z axis at horizontal flight. thus u4−0 = mg. (11) the system matrices a and b required for the controller design are derived from linearized equations (4), (5), (6) and (7). the matrix c is an identity matrix, and the matrix d is a zero matrix. the matrix k, which determines the control law, was obtained experimentally by the pole placement method. matrix k: ωx ωy ωz vx vy vz φ θ ψ x y z iz u1 1.05 0 0 0 0.29 0 2.66 0 0 0 0.12 0 0 u2 0 1.05 0 −0.29 0 0 0 2.66 0 −0.12 0 0 0 u3 0 0 0.66 0 0 0 0 0 0.44 0 0 0 0 u4 0 0 0 0 0 −4.08 0 0 0 0 0 −6.32−3.06 it can be observed from this matrix that the linearized state space description decoupled the system into independent subsystems for each axis.; the controller therefore handles it in this manner. in fact, from the perspective of attitude control, the state space controller can be understood as a set of separated pi or pd controllers. the results then prove that the approach involving a space controller and the approach employing pid controllers provide comparable results in this mode of flight. first, the real behavior of the designed controller was tested in a laboratory. figs. 3 and 4 show the step responses for the angular rotations pitch and yaw, which were both measured independently on a special tool. 4. implementation 4.1. construction the uranus uav has a well-known, four-rotor structure often referred to as quadrotor or quadrocopter. the construction consists of two orthogonal aluminum beams, which form a symmetric cross. all the electronic devices and printed circuit boards (pcb) are situated in the middle of the cross to ensure that the center of gravity is also in the middle. at the end of each beam there is one brushless dc (bldc) axi 2212/34 electromotor equipped with a graupner 11"x 5" carbon propeller. to suppress the mechanical vibrations, the motors are mounted on the rigid quadrotor frame through rubber pads. the uav overall dimensions are 701x701x188 mm, and the weight is 1.05 kg. the maximal combined motor thrust is about 24 n, so it is possible to carry a 150 g payload without reducing the maneuverability. the construction is mechanically simple and also allows additional modifications. 4.2. hardware the uav is equipped with several pcbs. the central one is the control board, which contains a control microcontroller (mcu), a power supply, and various sensors. the other boards are the communication module, bldc controllers, and ultrasound sensor. the sensor unit and gps receiver are encased in their own packages, and they are connected to the control board. the block scheme of the uranus uav system is shown in fig. 5. all the electronic devices on the uav are powered by a li-pol accumulator. in this construction, a 3-cell accumulator with the nominal voltage of 11.1 v, and the capacity of 2200 mah is used. this voltage is fed to all the engines, while the remaining electronics are supplied with 3.3 v and 5 v. the voltage level reduction is performed by switching and ldo (lowdropout regulator) stabilizers. the control board was designed specifically for this application. the main part of the board consists in an mcu lm3s8962, which is based on the 32-bit arm cortex m3 architecture and is able to operate at frequencies up to 50 mhz. it provides sufficient 17 p. gabrlik, v. kriz, l. zalud acta polytechnica ctu proceedings figure 2. designed controller. 0 5 10 15 −5 0 5 10 15 time [sec] θ [° ] figure 3. pitch angle step response. 0 5 10 15 0 20 40 60 80 100 time [sec] ψ [° ] figure 4. yaw angle step response. computing power [4], all the required communication buses (spi, uart, i2c), and internal a/d converters. an xsens mti-g is applied as the main sensor unit; this component is an inertial measurement unit (imu) and an attitude and heading reference system (ahrs). firstly, instead of this imu, a vectornav vn-100 was used. with this imu, however, we obtained worse results in stabilization, since the linear movement also cause a change in the measured angles. thus, it was replaced with the xsens mti-g, a component widely used in other uav projects, e.g. [5], [6]. the unit contains triaxial digital devices, namely an accelerometer, a gyroscope, and a magnetometer; further, the unit also comprises a gps receiver in one package with an external gps antenna. an internal kalman filter provides precise orientation estimation with 1 deg rms roll/pitch and 2 deg rms heading dynamic accuracy and the accuracy of 2.5 meters cep in position. the control board is also equipped with a bmp085 barometric sensor for the purpose of altitude measurement. an ultrasound sensor, which is used at low altitudes (during take-off and landing), is situated on the special pcb. the battery level is determined on the basis of the voltage and current measurement. regularly available bldc controllers bl-ctrl v2.0 provide the continuous current of 35 a for each motor and a very compact design. the controllers communicate with the control board via an i2c bus. it is also possible to mount an ip wireless camera on the construction and broadcast the image to the base station. 4.3. microcontroller software the software for the mcu was written in the embedded c language due to high requirements for the real-time behavior and reliability. the software does not use a commercial rtos but a simple and nonpreemptive os written specifically for this application. to achieve the real-time behavior, a system timer with the period of 100 ns was used; this is the shortest possible period to handle any application task. the application also uses mcu hardware interrupts to handle various asynchronous events. the interval for the computing of the main quadrotor stabilization (angular rotations stabilization) is 10 ms. at the same period, the data from the imu/ahrs are read and the actuator speeds updated. the sample period in altitude measurement depends on the used sensor; for example, we thus have the period of 25 ms for the ultrasonic sensor. the implemented control structures for the stabilization are constant, but their parameters can be tuned according to the current uav configuration. the application operates in several modes: the configuration/stop mode, applied when the uav is switched on but the actuators are disabled; the flight remote mode, used for standard remotely controlled operation; the signal lost mode, activated in the flight mode when the signal is lost and the uav is landing automatically; and the flight auto mode, which is ready for future autonomous flying using gps. 18 vol. 2/2015 reconnaissance micro uav system mcu arm cortex m3 ultrasound board 3-axis accelerometer xsens mti-g 3-axis gyroscope 3-axis magnetometer gps receiver 4x bldc electromotor 4x bldc controller zigbee wireless module zigbee wireless module notebook + cassandra hid / gamepad uranus uav base station uart1 uart2 i c 2 usb uart usb pressure sensor i c 2 figure 5. the block scheme of uranus uav system. figure 6. uav control board and the other electronics. 4.4. communication the communication between the robot and the base station is wireless. it is provided by two paired xbee pro s2b rf modules transmitting within the band of 2.4 ghz; the modules use the zigbee protocol and operate in a transparent mode. in this mode, the 2 devices work as a virtual uart wire. thus, every uart frame send to the input of one module appears on the output of the other (if the rf channel is established). the baud rate of this line is 57.6 kbps. above this layer of communication, the uranuslink protocol was created. it was designed as a packetoriented, non-reliable protocol. this protocol defines the packet structure as well as the transmitted data representation. as shown in table 1, every packet in uranuslink consists of 6 fields: the preamble (pre); the sequence number (sqn); the message identification (mid); the data length (len); the data as such; and the checksum (cs). all the data are in the big endian format. the preamble has the constant value of 0xfd. it is used to determine the beginning of the packet. the sqn is intended for the numbering of the packets; while every sent packet increases this number by 2, the sqn can only take even values. this property is utilized in one of the packet validation mechanisms. another important application of the sqn is in packet loss detecting. the mid determines the interpretation of bytes in the data part of the message, while the len specifies the length of this part. there are 24 different packet types distinguished by the mid. the most important ones are: compounded joystick command, robot mode, and acknowledge in the direction towards the robot; and all data stream, battery voltage, and acknowledge in the direction towards the base station. the computed joystick command holds the required roll, pitch, yaw, and thrust. the robot mode is used to switch between the robot modes, as described in sect. 4.3. this packet is specific, because it must be confirmed by the acknowledge packet from the robot. the acknowledge packet carries, in its data section, the sqn number of the packet which is confirmed by it. towards the base station, the all data stream carries important telemetric data such as the robot attitude and altitude, gps position, and status (e.g., if the gps data are valid or the inertial measurement unit was initialized successfully). while these data are sent every 10 ms, the battery voltage, for example, is sent once per second. in the direction towards the robot, the compounded joystick command is sent approximately every 100 ms and the robot mode only when it is required to switch the mode. as stated above, this packet must be confirmed by the acknowledge packet. if it is not, the station begins retransmitting it and continues until confirmation is obtained. this is carried out to ensure that the robot mode will be switched even when the packet is lost. the other packets remain unconfirmed, because the system overheads will be more significant than the advantage of ensuring that all flight data will be transmitted ok. if there is a packet outage lasting longer than 0.5 s, the robot will handle this as signal loss and take an action. it will set the required roll, pitch and yaw to zero; also, the system performs slow descent and can proceed to eventual landing. 4.5. base station one of the requirements for the uranus was its integration in the cassandra system. this system has been developed at ceitec and the but for several 19 p. gabrlik, v. kriz, l. zalud acta polytechnica ctu proceedings pre sqn mid len data ... cs 1b 2b 1b 1b 1-252 b 1b table 1. uranuslink packet format. years. this system comprises a heterogeneous group of robots and a base station. the core of the base station consists of software written in c#, communication hw, and human-device interface. this interface includes a joypad and a virtual reality helmet, or, in the simpler version, a monitor screen and an optional keyboard. the base station software can be run on a classical pc, a laptop, or an embedded pc; thus, the base station can be a mobile or even wearable system. a new communication hw was built to operate the uranus uav. this portable device consists of x-bee modules (as described in section 4.4), a high-gain antenna, and an uart-over-usb converter, all placed in box attached to a foldable tripod stand to ensure a higher position of the communication system above the ground (and, thus, better coverage). from the base station, the operator can control all the powered robots by switching among them. the display provides the operator with a first person view from the robot. the robot movements are controlled via the joypad. if the camera on a given robot is capable of rotating, its motion can by controlled via movement of the operator’s head (in case that the virtual reality helmet is used) or by means of the joypad. the cassandra base station display provides, besides a view from the onboard camera, important telemetric and other mission-related data, as shown in fig. 8. the bottom part of the display presents attitude information, namely the actual roll and pitch angle in the artificial horizon in the left circular indicator, and the yaw angle in the compass in the right one. the upper left corner includes the robot status indicator. this contains the name of the active robot, its battery voltage, signal outage indicator, actuator state, robot mode, and other information if required. the lower part of this indicator can show important text information and warnings. all the indicators can be hidden, plus there are a couple of indicators not opened by default. such indicators display, for example, the status of the other robots, the actual position of the robot on the map, or the actual camera orientation. 5. operation for flying with the uranus uav, we use the following configuration: a laptop with the cassandra system installed; a joypad; and a designed communication device. the uranus is controlled by a joypad with 2 joysticks, of which the left one regulates the pitch and roll and the right one modifies the thrust and yaw. before the flight, the following steps need to be carried out: after switching the power on, the uranus figure 7. base station and uranus uav. figure 8. the user interface of the cassandra system. uav is in the configuration/stop mode. this mode has to be switched to the run mode from the joypad. subsequently, all the rotors start and operate at a very low speed. after that, the right joystick, which controls the thrust, needs to be pushed all the way down. then the rotors will gradually achieve the speed corresponding to the actual joystick position. this solution was implemented to prevent the rotors from starting at very high rpms if the mode is switched with the joystick in default position. from this moment on, the uranus uav is ready to flight. if the thrust joystick is released, the robot will take off and hover at about 1 meter above ground. to precisely suppress the gravity force by the thrust, the output levels sent to the motors from the controller are modified according to the battery voltage. this occurs because the thrust of the motors varies in accordance with the battery voltage. the battery voltage level is also reported to the base station to warn the pilot if the voltage drops too low. a warning is also produced by signal loss. if this happens, the uranus uav will automatically land. during the test flights, it was proven that uranus is stable, and while the control joysticks are released, the quadrotor hovers in position. but because no position stabilization has been implemented to date, the uranus could slowly drift from the given position. this feedback will be integrated only in the next versions. controlling the uranus with the joypad was easy, and the operator was able to operate the uav 20 vol. 2/2015 reconnaissance micro uav system effectively after a short while. 6. conclusion regarding the successful test flights, it can be concluded that the assembled mathematical model clearly expresses the quadrotor behavior; thus, the designed control system was able to stabilize the robot suitably. although the controller was designed as a state-space device, it was proven that the resulting controller can be interpreted as a set of separate pi or pd controllers in each axis. this is due to the model linearization around the working point, namely hovering. for intended use, the described approach provides good results: the quadrotor was able to hover and to maneuver. to facilitate integration in the cassandra system, a new communication protocol was designed, and the cassandra system was modified to be capable of handling the flying robots. as the purpose of the developed uranus uav was to enable the cassandra robotic system to perform air missions, it can be stated that the given goal was achieved. for the future, we plan to navigate the uranus uav by the gps, to design our own imu, and to create a bigger airframe with a higher payload capacity. list of symbols θ angle of rotation around the lateral axis [◦] φ angle of rotation around the longitudinal axis [◦] ψ angle of rotation around the vertical axis [◦] ω angular speed [◦ s−1] ft thrust [n] g gravitational acceleration [m s−2] g gravity force [n] i mass of inertia [kg m2] km rotational speed to reaction torque ratio constant [nm rpm−2] kt rotational speed to thrust ratio constant [n rpm−2] l length [m] m weight [kg] mr reaction torque [nm] n rotations per minute [rpm] u1 torque in the longitudinal axis caused by motors [nm] u2 torque in the lateral axis caused by motors [nm] u3 torque in the vertical axis caused by motors [nm] u4 force in the vertical axis caused by motors [n] u4−0 force in the vertical axis required to compensate gravity force [n] v linear speed [m s−1] x longitudinal axis; position in this axis [–; m] y lateral axis; position in this axis [–; m] z vertical axis; position in this axis [–; m] acknowledgements this work was supported by the project ceitec central european institute of technology (cz.1.05/1.1.00/02.0068) financed from european regional development fund and by the project fekt-s-142429 “the research of new control methods, measurement procedures and intelligent instruments in automation” financed from internal grant system but. references [1] l. zalud, l. kopecny, f. burian, t. florian. cassandra heterogeneous reconnaissance robotic system for dangerous environments. in 2011 ieee/sice international symposium on system integration (sii), pp. 1275–1280. 2011. doi:10.1109/sii.2011.6147632. [2] s. bouabdallah. design and control of quadrotors with application to autonomous flying. ph.d. thesis, ãľcole polytechnique fãľdãľrale de lausanne, 2007. doi:10.5075/epfl-thesis-3727. [3] f. solc. modelling and control of a quadrocopter. advances in military technology 5(2):29–38, 2010. [4] h. lim, j. park, d. lee, h. kim. build your own quadrotor: open-source projects on unmanned aerial vehicles. ieee robotics automation magazine 19(3):33–45, 2012. doi:10.1109/mra.2012.2205629. [5] s. grzonka, g. grisetti, w. burgard. a fully autonomous indoor quadrotor. ieee transactions on robotics 28(1):90–100, 2012. doi:10.1109/tro.2011.2162999. [6] k. alexis, c. papachristos, g. nikolakopoulos, a. tzes. model predictive quadrotor indoor position control. in 2011 19th mediterranean conference on control automation (med), pp. 1247–1252. 2011. doi:10.1109/med.2011.5983144. 21 http://dx.doi.org/10.1109/sii.2011.6147632 http://dx.doi.org/10.5075/epfl-thesis-3727 http://dx.doi.org/10.1109/mra.2012.2205629 http://dx.doi.org/10.1109/tro.2011.2162999 http://dx.doi.org/10.1109/med.2011.5983144 acta polytechnica ctu proceedings 2:15–21, 2015 1 introduction 2 quadrotor model 3 controller design 4 implementation 4.1 construction 4.2 hardware 4.3 microcontroller software 4.4 communication 4.5 base station 5 operation 6 conclusion list of symbols acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.12.0112 acta polytechnica ctu proceedings 12:112–115, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app dangerous driver’s behavior libor topol∗, ivo drahotský univerzita pardubice, dopravní fakulta jana pernera, studentská 95, 532 10 pardubice ∗ corresponding author: libortopol@seznam.cz abstract. different types of dangerous driver’s behavior are discussed in this paper. case study analysis of young drivers’ hazardous behavior is also provided from authors’ practices. the practical research is collaborated with the statistical data that aggressive driving induces the number of fatalities on the roads in the czech republic by 25%. the improvement to driver’s training and other countermeasures is then suggested. keywords: dangerous driving behavior, driver training, road safety. year number of accidents number of fatalities number of serve injuries number of light injuries 2010 75522 753 2823 21610 2011 75137 707 3092 22519 2012 81404 681 2986 22590 2013 84398 583 2782 22577 2014 85859 571 2409 18074 2015 93067 660 2540 24426 table 1. evolution of basic indicators of accidents in 2010-2015. 1. introduction road transport occupies a significant segment in transportation in general and due to its high accident rates and hence economical losses, considering the affecting factors is rather crucial for safety improvement. road traffic safety may be characterized by direct and indirect safety indicators. direct indicators are the number of road accidents, their consequences and economical losses. indirect indicators are phenomena or circumstances that project safety assessment into experimental plane of relations between human behavior and transportation safety (following the speed limits, application of safety systems, maintaining safe distances between vehicles, estimation and anticipation of errors in real traffic). high traffic intensity on roads is a reason of high workload for car drivers. this overload is related to the number of accidents in the czech republic, which, despite various measures for its reduction in comparison with other european countries, is still very high. traffic accidents are a major social issue. the table tracks a noticeable increase of fatalities in traffic accidents. number of light and heavy injuries increases as well. one may notice a constant increase in total number of accidents. in 2015 total of 93,067 accidents was figure 1. total number of recorded accidents in the czech republic from 2011-2015. reported and investigated. for example, compared to 2014, there were about 7,208 more accidents in 2015. every day the czech police has conduct around 255 accident investigations on average. this is equal to approximately 14.901.712,00 czk of property losses every day[1]. 2. dangerous driver’s behavior among other factors, aggressive driving contributes to traffic accidents to a high extent. per úamk, 91% of drivers have been exposed to aggressive driving to a certain extent. under the term of dangerous driver’s behavior, we may assume the one that is in contradiction to official and so-called unofficial or nonwritten rules, an unexpected, aggressive or unusual and non-customary behavior on the road[2]. human behavior is diverse. driver’s behavior differs from every person. it is possible to categorize dangerous behavior from different perspectives. inattentive driving can be related to dangerous behavior as it is, besides speeding, the most common cause of traffic accidents. another category is driving while being involved in some secondary activities that are not related to vehicle control. these are smoking, talking 112 http://dx.doi.org/10.14311/app.2017.12.0112 http://ojs.cvut.cz/ojs/index.php/app vol. 12/2017 dangerous driver’s behavior accident #1 accident #2 time of accident: 5:15 am time of accident: 6:54 road class: ii road class: ii road section type: roundabout road section type: two-way road weather conditions 8°c, clear weather conditions 12°c, clear driver’s age: 25 y.o. driver’s age: 28 y.o. vehicle vehicle car make: audi a6 car make: suzuki swift year of issue: 2001 year of issue: 2004 outcomes outcomes # of fatalities: 3 – immediate (including driver), 1 – in hospital # of fatalities: 3 – immediate (including driver) # of severely injured: 2 # of severely injured: 3 description: driver approached and entered the roundabout without any or with low speed reduction and thus couldn’t manage the turning but ran across the safety island in the middle of roundabout and broke through the roundabout fence ended up on a roof in retention tank. accident sketch can be seen in the image bellow. description: driver exit the lane and with right vehicle side hit front of vehicle in an opposing traffic. accident sketch can be seen in the image bellow. table 2. figure 2. damaged vehicles from accident 1 (left) and accident 2 (right). 113 libor topol, ivo drahotský acta polytechnica ctu proceedings on the phone while driving, eating, drinking, involving into conversations with other passengers and so on. a driver’s personality, psychological and medical condition, lack of knowledge of traffic rules can be the risk itself[3]. these and many features of driver’s behavior that can be gathered under one term of aggressive driving. committing traffic violations can occur both because of negligence, and unintentionally[4]. driver’s age is also one of the factors that influences road safety. lack of experience of novice drivers can cause a potential danger in traffic situations as well as deteriorating physical state of senior drivers[5]. hence, we can categorize dangerous behavior by age or driving experience. young drivers (age group under 24 years old) are said to be the highest risk group of drivers in agewise[6]. they lack the capacity to adequately evaluate dangerous situations, they tend to overestimate their own abilities, have little driving experience and, therefore, fewer skills in vehicle control. beginner drivers are often subject to influence of opinions of other car occupants, they often drive vehicles in poor technical condition and tend to drive high-speed powerful vehicles and thus are exposed to a false feeling of safety. statistical research confirms that young drivers are referred as the most dangerous group. they, more often than others, exceed the speed limit, overtake in sections with low visibility road sections or when not allowed and tend to hit the red traffic light signal. in this group there are also individuals who tend to drive more often under the influence of alcohol and other drugs. young male drivers tend to take more risky maneuvers, rather than young women who tend to avoid dangerous situations, by extent and frequency. young males are also less attentive than females of the same age category. it is, of course, worth noticing that percentage of female drivers in general is still lower than that of male, women drive less in general (kilometers-wise)[7, 8]. driving school instructors in many european countries believe that nowadays, young drivers behave more hazardously on the road, not realizing the potential threat of accidents and their consequences. speeding is associated with masculinity. nowadays, young drivers’ attention, compared to the one in the past, is affected by many disturbing factors such as advertising and bill-boards, loud car acoustic systems, mobile phones etc. driving instructors believe that it may be necessary to reconsider approach to young driver training in terms of study program duration and extension of training programs on driving simulators[9]. 3. traffic accidents with participation of young drivers – case study information for the following study is based on authors’ personal practice of forensic expertise. the expert evaluation of vehicles has been performed, the technical information is given in table 2. the two accidents have some typical features in common. both drivers were from the dangerous group – young drivers. in each case, the accident took place at early morning hours, which makes experts relate to so called "after party" accidents. both were older cars, which may have affected the severity of consequences. the number of passengers at the time of the accident was higher than allowed (6 car occupants in both cases). 4. conclusion dangerous behavior of younger drivers is a reason of many fatal accidents on the roads. one of the important reasons is lack of training for new drivers, which should include both psychological preparation of novice drivers and extensive practical training. also lack of experience is one of the reasons younger drivers overestimate their ability to handle vehicle at high speeds or while turning, neglect the car technical state (old cars) or its power (new cars). this aspect shall be addressed along with other valid methods of accidents rate reduction[10]. references [1] directorate of traffic police 2016. statistics of traffic accidents. online: policie.cz/clanek/statistika-nehodovosti. [2] m. šucha. dopravní psychologie pro praxi: výběr, výcvik a rehabilitace řidičů. praha: grada publishing, 2013. isbn 978-80-247-4113-0. [3] m. šucha. agresivita na cestách. 1. vyd. olomouc: univerzita palackého v olomouci, 2009. isbn 9788024423753. [4] p. bouchner, m. novák, s. novotný, et al. human behavior while driving the road vehicle. prague: faculty of transportation sciences, ctu in prague, department of vehicle technology, 2015. 1st electronic. isbn 978-80-01-05872-5. [5] m. novák, p. bouchner, j. faber, et al. senioři za volantem. praha: department of informatics academy of sciences in czech republic, v.v.i., 2008. isbn 978-80-87136-02-7. [6] s. novotný, p. bouchner, m. novák. agresivní a nebezpečné chování řidičů motorových vozidel v čr – analýza dat z plovoucích vozidel. in: dopravní nehodovost a rizikové chování řidičů motorových vozidel. praha: vyšší policejní škola mv v praze, 2013, pp. 49-59. isbn 978-80-260-5466-5. [7] z. šejdová. riskantní jednání mladých řidičů v české republice. master thesis. palacký university olomouc, 2015. [8] mladí řidiči a dopravní nehodovost. 2007. source: czrso.cz. available on 8.5.2017. [9] goodyear europe, middle east and africa. a report by goodyear europe, middle east and africa (emea). november 2013. 114 policie.cz/clanek/statistika-nehodovosti czrso.cz vol. 12/2017 dangerous driver’s behavior [10] p. bouchner, j. faber, p. hrubeš, et al. road accident reduction. roma: aracne editrice s.r.i., 2010. isbn 978-88-548-3550-4. 115 acta polytechnica ctu proceedings 12:112–115, 2017 1 introduction 2 dangerous driver's behavior 3 traffic accidents with participation of young drivers – case study 4 conclusion references 311 acta polytechnica ctu proceedings 2(1): 311–320, 2015 311 doi: 10.14311/app.2015.02.0311 who discovered the hoyle level? g. shaviv1 1department of physics, israel institute of technology, haifa, israel 32,000 corresponding author: gioras@physics.technion.ac.il abstract the prediction of hoyle that the nucleus of 12c must have a resonance at 7.62mev was the trigger to the anthropic principle. we review the history of the discovery of this level and investigate to what extent this was a genuine prediction. keywords: anthropic principle nuclear physics stellar evolution. 1 who is who three dominant personalities were involved in the present story: sir fred hoyle frs (1915-2001), who was one of the greatest astrophysicists in the second half of the twentieth century with major contributions to stellar structure (nuclear astrophysics synthesis of the elements) and to cosmology (steady state theory dubbed the name big bang) as well as planetary formation. william a. fowler (1911-1995), who can be considered as the father of nuclear astrophysics and edwin salpeter (1924-2008) top theoretical astrophysicist, who has numerous seminal contributions in many astrophysical fields as well as in physics. fred hoylewilly fowlered salpeter edwin e, salpeter william a. fowler fred hoyle figure 1: the dominant personalities involved in this story: the discovery of the triple α process. 2 what is the hoyle level the synthesis of helium into carbon in stars proceeds via resonant reaction, namely the three α particles fuse into an excited energy level in the 12c nucleus. the rate of the reaction was calculated before the existence of this level was known and was found to be very low compared to the rate of destruction of 12c by collisions with α particles. as a consequence, it was impossible to predict the evolution off the main sequence towards the red-giant branch and the calculation implied that all the 12c is converted into 16o. but stars do evolve and we know that somehow carbon is synthesized. in view of the impass, hoyle predicted therefore, that 12c has an energy level just at the right place and the reaction of carbon synthesis proceeds via this resonance level. the level was then discovered in the laboratory. this chain of events: prediction the existence of a nuclear level from astrophysical constraints, wa s considered as a big victory for astrophysics and the level was named the hoyle level. 3 what is the anthropic principle the anthropic principle is a philosophical hypothesis that measures of the physical universe must be compatible with the existence of conscious life that observes it. the phrase ”anthropic principle” appeared first in brandon carter’s contribution to the 1973 krakow symposium honoring copernicus’s 500th birthday. carter argued as well, that humans do not occupy a privileged position in the universe. the trigger to the idea that life as we know it, and the cosmos around us, ”are tuned”, emerged from hoyle’s prediction of the existence of a special energy level in the nucleus of 12c. if such a level did not exist, argued hoyle, life could not have develop in the cosmos, more accurately, 12c based life could not emerge. was it really so amazing? was it a full prediction? the basic astrophysical problem emerged when hoyle and schwarzschild calculated, in the early nineteen-fifties, the evolution of stars off the main sequence into the red-giant using reaction rates known at the beginning of the nineteen fifties and got that as soon as 12c is synthesized from helium, it absorbs another α particle and becomes 16o leaving no carbon. the reaction forming 12c was much slower than the reaction that destroys it. if so, argued hoyle, life should not exist! alternatively, as 12c does exist in our uni311 http://dx.doi.org/10.14311/app.2015.02.0311 g. shaviv verse, there must be a resonance in this nucleus that accelerates the formation of carbon by many orders of magnitude. this was ’reverse engineering’ at its best. you know what should happen and find out how can it be. could 12c be synthesized elsewhere? the only known alternative was the big-bang. but hoyle argued that all elements were synthesized in stars. on the other hand, gamow argued that all elements were synthesized in the big bang. however, the various models of big-bang nucleosynthesis failed to produce elements like 12c and higher (in atomic weight), and left stars as the only cosmic site for synthesis of 12c and heavier nuclei. 4 the nuclear barrier two nuclear barriers exist in the synthesis of the elements from hydrogen up (see fig. 2). the barriers are the non existence of a stable a=5 and a=8 nuclei as shown in the figure. this means that the synthesis of the elements, if started from hydrogen, must jump over these nuclei.236 chapter 8. how nature overcomes its own barriers figure 8.1: the light elements in the n, z plane. stable nuclei are painted brown. unstable elements with long lifetime are painted yellow. unstable nuclei with very short lifetime are painted red. the a=z+n=5 and a=z+n=8 nuclear barriers are shown as straight lines. the nuclear forces do not yield a stable nucleus for these combinations of protons and neutrons. there is only one nucleus with a=4 stable or unstable. although it is very stable and has a large binding energy, it has no excited state, only the ground state. 1h z n 1 2 3 4 1 2 3 4 5 6 7 8 5 6 7 8 14c 15n 16o 17o a=8 barrier 18o 9 10 7be 3.10-22s h he li be b c n o 5.10-21s 4.10-22s 8.10-19s10-17s 0.84s 177ms 8.7ms 8.10-22s 807ms 3.10-21s 119ms 12.3 yr 20.3m 5730yr 2.45s 0.75s 20ms 174ms 14ms 9ms 19.29s 11ms 9.97m 0 finally, bethe examined the triple body reaction, namely, the three ↵ particles interact simultaneously with one another to produce the carbon nucleus. since collisions of an ↵-particle with one other particle, proton or alpha, do not lead to stable nuclei the alternative was to assume a triple collision of which three types were plausible: (a) 4he + 2p ! 6be, (b) 24he + p ! 9b, and (c) 34he ! 12c. the first two reactions were rejected because they do not lead to a stable nucleus. the third reaction leads directly to 12c. however, bethe knew from eddington’s models that the temperatures in main sequence stars are around 2 ⇥ 107k, while the triple collision of ↵-particles requires according to bethe’s estimates, temperatures of the order of 109k, which are way beyond the range of temperatures according to eddington, in main sequence stars. hence, bethe dropped the idea of a three body reaction. in 1951 von weizsacker1 discussed the problem and claimed that the energy source can still be gravitation if only the condensation is extremely large2, which is essentially a milne type model. weizsacker noted that there were giants among the old population of stars as defined by baade. namely, these stars must have a very long life time. consequently, these stars must be low mass stars. if giants are main sequence stars which have exhausted their hydrogen fuel in the core and energy is not produced in the core any longer, then there need not be any temperature gradient in the core. weizsacker thought that the fusion of h into he is the only process that could operate in stars because he believed that there is no way to overcome the a=5, 8 barriers. consequently, nuclear energy was not an option for these stars because of the assumption that they exhausted their hydrogen and no other fusion can take place. from this point of view, weizsacker put the giants and the white dwarfs in the same category of stars. still, weizsacker added a reservation that in view of results known at his time, there is a possibility for hydrogen burning outside the isothermal core3. however, the idea weizsacker put forward was that the di↵erence between white dwarfs and giants should be that giants have masses above the chandrasekhar 1von weizsacker, c.f., apj, 114, 165, (1951) 2jordan, p., die herkunft der sterne, 1947, p 38. 3richardson, r.s. & schwarzschild, m. apj, 108, 373, (1948) gamow, g. & teller, e., phys. rev. , 55, 791, (1939) & gamow, g. & keller, g., rev. mod. phys. ,17, 125, (1945) & gamow, g. phys. rev. 67, 120, (1945) figure 2: the nuclear barriers at a=5 and a=8, namely the non existence of stable nuclei with these number of protons and neutrons. many attempts and suggestions to overcome the barriers were suggested. we mention here only bethe’s attempt, namely a three body reactions. bethe knew from eddington’s stellar models what are the central temperatures and densities in stars and soon realized that a 3-body reaction is much too rare under such conditions. we note that eddington’s results were derived without reference to what is the energy source of stars (which he did not know but hypothesized, already in 1919, that it must be the fusion of hydrogen into helium). in fig. 3 we show the structure of all nuclei with n+z=8. the instability of the a=8 nucleus implied that any fusion reaction leading to this nucleus will not create it. the so formed nucleus may live a short time but eventually it decays.8.1. unsuccessful attempts to overcome the a=8 barrier 237 12b5 12c6 12n7 17.42mev 13.37mev β+ βenergy the n+z=12 system z=5 z=6 z=7 τ1/2=11.00msτ1/2=20.20ms figure 8.2: the a=12 nuclei system. the diagram explains why of all nuclei with 12 protons and neutrons, the 12c is the most stable one. the other nuclei with a=12 are all unstable and decay via �+ or �� into 12c. the energies above the ground state of carbon are given in mev. also given the half-lifetime of the unstable nuclei. after ajzenberg-selove and lauritsen 2008. 8he 8li 8be 8b 8c 4he+4he -0.0918 3.03 11.35 16.9217.02 16.36 26.3228.09 reference level energy z2 3 4 5 6 0 figure 8.3: the energy levels of the nuclear system with a=8 for di↵erent atomic numbers z. the nucleus 8b can decay into an excited state of 8be, which may decay eventually to the 8be ground state. but the ground state of 8be is above the state of two free ↵ particles (colored green) and hence, the fast breakdown of 8be is unavoidable. consequently, 8be does not exist in nature. limiting mass4 and hence, have enough gravitational energy in the contraction towards extremely high densities, even as high as nuclear densities5. however, no detailed calculations were carried out, just speculation. weizsacker attempts and ideas to explain the giants were typical to the hopeless situation in front of the insurmountable a=5, 8 barriers. in 1949 gamow published a paper on relativistic cosmology6 in which he brought up an idea wigner communicated to him in private. another ingenious method of crossing the mass 5 crevasse was proposed by e. wigner. it is known as the method of the ’nuclear chain bridge’. wigner’s plan is that all that is required for building a chain bridge is an assumption that there was originally one single nucleus on the right-hand side of the crevasse. such an assumption can easily be granted argued gamow, since some building up is still maintained across the crevasse by the reaction 4he +3 t !7 li + � in spite of the low probability of its occurrence. gamow published his rejection of wigner’s idea in a book7 just when the salpeter and hoyle started the work on the triple ↵ process which ended few years later with the detailed nuclear physics. gamow gave no reference to where wigner published his suggestion. 4chandrasekhar, s., mnras, 95, 207, 226, 676, (1935) 5nuclear densities are densities at which the nuclei touch each other. the radius of the nucleus is about 10�5 the radius of the atom, namely, the radius of the outer occupied electronic shells. the atom has an infinite number of electronic shells with radius increasing to infinity. but as the number of electrons in each atom is finite, they occupy only the lowest in energy levels and for this reason the actual atoms has a finite radius, the radius of the last occupied level. normal matter densities on the earth are ⇠ 1g/cm3. if the matter is compressed to densities as high as 1015gm/cm3 the nuclei touch each other and form one gigantic nucleus. this is nuclear matter. 6gamow. g., rev. mod. phys., 21, 367, (1949) 7gamow. g., the creation of the universe, viking press, new york, 1952. figure 3: the relative energies of the ground states of the n+z=8 nuclei. the numbers are the energies in mev relative to the ground state of 8be, which has the lowest ground state energy of all a=8 nuclei. however, the state of two free α’s has still lower energy. hence, there is no stable nucleus with a=8. 5 why nuclear physicists were interested in the problem? the fundamental problem in nuclear physics at the beginning of the nineteen thirties was the nuclear structure. it was already known that the α particle is the most bound nucleus as it has the highest binding energy per nucleon. similarly, nuclei like 12c,16 o,20 ne etc have a higher binding energy than their neighboring nuclei. the question was therefore, are these so called α nuclei composed of α particles 238 chapter 8. how nature overcomes its own barriers 8.2 the pursuit after the structure of the carbon nucleus figure 8.4: two possible structures of the carbon nucleus. on the left, the nucleons move randomly inside the nucleus. on the right, there are three clusters of ↵ particles and the ↵ particles move randomly inside the nucleus. figure 8.5: the structure of 14n according to the revised ↵-particle nuclear model. the story starts as early as 1917, when harkins8 observed that the binding energies of the so called ↵ nuclei, (12c,16o,20ne,24mg, . . . ) are particularly large. consequently he suggested a periodic table for nuclei (cf. fig.??). the basis for this periodic table was harkin’s idea that the basic building block of nuclei is the ↵-particle. harkin’s original idea was put forward before the neutron was discovered. after the discovery of the neutral particle the model was modified to: the nucleus is made of a core of ↵ particles and up to 3 nucleons moving around it (cf. fig.??) consequently, the following fundamental question was raised: to what extent a nucleus of type 4n+2 would yield a nucleus of type 4n, where n = 1, 2, 3, . . . and an ↵ particle, if bombarded with nucleus with atomic weight 2, namely a deuterium. in symbols the reaction is: 4n+2x2n+1 + 2d1 ! 4ny2n + ↵, where x is any nucleus and y is the element the precedes the element x in the periodic table. the di↵erence between the two models is fundamental. the ↵ particle is fully symmetric and has zero spin, hence, it must follow the bose-einstein statistics. on the other hand, the protons and the neutrons both have spin 1/2 and hence, follow the fermi-dirac statistics. obviously the behavior of the particles in the potential well and how they fill up the levels is completely di↵erent in two the cases. the di↵erence should express itself in the binding energy as well as in the energy levels. if there is a potential well and the particles moving inside obey the fermi-dirac statistics, we can expect periodicities in the properties. on the other hand, if the ↵ particles preserve their spin while they move in the nucleus, then they do not behave like bosons and can all stay in the same nuclear level. obviously, the binding energy in such a case is larger than in the case of individual protons and neutrons (because in the latter case the nucleons are spread over many energy levels while in the first case they are all in the lowest most bound level.) the idea that nuclei are composed of ↵ particles emerges from the fact that the ↵ particles is extremely stable and we do not know that it has any excited levels. like deuterium which is composed of a neutron and a proton does not have any excited state, only a ground state. hence the helium nucleus is not unique from this point of view. the binding energy of a deuterium is 2.225mev while that of an ↵ particle amounts to 28.3mev, namely, significantly more than just two deuterium nuclei put together. it seems that the potential well inside which the ↵ particle resides is very deep and still does not posses any excited state. lauritsen and crane9 investigated this point in 1934 and indeed, did not discover any 8harkins, w.d., j. amer. chem. soc., 39, 856, (1917), phys. rev. 15, 85, (1920) 9lauritsen c.c. & crane, h.r. prl, 46, 537, (1934) figure 4: the two possible options for the structure of the carbon nucleus. on the left we see 12 nucleons moving independently of each other and on the right we see groups of 4 nucleons moving as a bound unit. or of just an equal number of protons and neutrons, as shown in fig. 4. in particular, is the excited state of 12c a three body state? consequently, attempts to find the energy level structure of the excited 12c were 312 who discovered the hoyle level? carried out long before any astrophysical interest in the problem arose. actually, even before bethe discovered how the cn cycle powers the sun (today we know that the cno cycle contributes about 4% of the total energy produced by the sun and the pp chain contributes the rest.) 6 the history of the discovery of the 12c nuclear levels already in 1933 lewis et et al. experimented with the reaction:14n+2d → 12c+4he. the nucleus of 12c so formed has significantly more energy than the ground state as it forms in an excited state. the decay of the excited state to the ground is performed by one or more emissions of γ photons. in principle, if you measure the energy of the γ′s you can easily figure out the energies of the energy levels in the newly formed nucleus. lewis et et al. did not measure any γ′s as they did not have the equipment, they however, discovered the emitted α particles. as they did not detect all particles emitted in the reaction they found that the emitted α particles have about half the energy difference and it was not known where the other half was lost. lawrence et al (1935) repeated the experiment, again without any device to measure γ′s. however, they measured the energies of the α′s and found two groups of α particles having different energies, and so were able to infer that 12c has two energy levels: at 3.8mev and 4.7mev. actually, the interpretation of the experiment was not complete. as shown in fig. 5, there are two possibilities to interpret this experiment. 0 0 3.8 3.8 8.5 4.7 ground state 00 figure 5: the interpretation of lawrence et al. result. one alternative can be two levels at 3.8 and 8.5mev with allows transitions between these two levels and forbidden transition directly from the 8.5mev level to the ground state. the other alternative is two levels with allowed direct transition to the ground state and forbidden transition between the levels. lawrence et al assumed the latter case but as we will see that in reality it was the first alternative. crane and lauritsen observed γ’s from the reaction: 11b+2d → 12c+p. these experiments which were carried out in the early 1930th made it clear that 12c has excited states but their energy was not known to better than ±1mev . 8.5. back to new developments in the structure of 12c 241 table 8.1: bethe’s estimate for the lifetime of the 8be nucleus as a function of the energy excess above the state of two free ↵ particles (in seconds). the second row gives the crossing time. energy excess in kev 50 100 200 300 400 r = 2.5 ⇥ 10�13cm 4 ⇥ 10�13 3 ⇥ 10�14 2 ⇥ 10�15 2 ⇥ 10�19 5 ⇥ 10�20 crossing time (sec) 4 ⇥ 10�22 2.8 ⇥ 10�22 2.0 ⇥ 10�22 1.6 ⇥ 10�22 1.4 ⇥ 10�22 r = 2.5 ⇥ 10�13cm 7 ⇥ 10�14 4 ⇥ 10�17 3 ⇥ 10�19 3 ⇥ 10�20 1 ⇥ 10�20 crossing time (sec) 8 ⇥ 10�22 5.6 ⇥ 10�22 4 ⇥ 10�22 3.2 ⇥ 10�22 2.8 ⇥ 10�22 8.5 back to new developments in the structure of 12c αα αα3 +8 bebe + 7.366 7.275 7.68 4.43 12c 7.1 7.8 figure 8.6: the energy levels of the 12c nucleus relative to the rest mass energy of 8be + ↵ and 3↵. the level at 7.68mev can decay into a 8be + ↵ or 3↵. the green color span the range where the various experiments gave an indication of an energy level. all energies are in mev. the correct explanation was put forward five years later, in 1940, and by gaerttner and pardue25, then in the kellogg radiation laboratory in cal-tech. using the same nuclear reaction, 14n+2d ! 12c+↵, gaerttner and pardue discovered that on top of the emerging ↵, also � rays at 1.9, 3.1, 4.0, 5.3 and 7.0mev were produced and explained their origin as due to excited levels in 12c at energies of 4.32 and 7.2 ± 0.4mev above the ground state. the authors even stated that the level at 7.2mev is weakly coupled with the ground state, namely, the probability for a transition from the 7.2mev state to the ground state is very small and was not observed. here we note that the energy of 8be + ↵ is 7.367mev above the ground state of 12c. hence only a level above this rest mass energy plus the kinetic energy can be directly reached by the 8be+↵. at stellar temperatures of the order of 108 � 109k the nuclei have kinetic energy of about 0.01 � 0.1mev, so that the kinetic energy is not the dominant one.26 we conclude that for the colliding 8be and ↵-particle to enter into an energy level of 12c, the energy must be above 7.366mev but not by very much. the knowledge of the structure of the 12c nucleus at that time is shown in fig.??. the green zone spans the uncertainty in the location of the energy level just above the energy of 8be+↵ or 3↵. since the reaction rate is very sensitive to the exact value of the energy level, accurate positions are mandatory. most nuclear reactions at low energy have two quite independent steps: formation and decay. • the formation: so far we discussed the probability of formation. due to the strong interaction between the particles and the relatively long time the particles stay together, the 0nucleus forgets how the particular level was reached0. the newly formed excited 12c lives for a while, exactly like the 8be nucleus lives for a while, before it decays. nuclear physicists call the new nucleus the 0compound nucleus0. • the decay: the new nucleus may have several modes of decay. it can disintegrate back into the original constituents or lose energy in one way or another and descend into a bound state, provided there is one, or even the ground state. no bound nucleus can be formed without any loss of energy. the most common way of losing energy is by emitting a �, however, other ways, though with lower probabilities, exist. 25gaerttner, e.r., & pardue, l.a. , phys. rev., 57, 386, (1940) 26the relevant particles are those with energies equal to the gamow peak and not with the average energy. figure 6: the structure of the 12c nucleus as known in 1940. the level at 7.68mev can decay into a 8be+α or 3α. the green color spans the range where the various experiments gave an indication of an energy level. all energies are in mev. in 1940 gaerttner & pardue of the kellogg laboratory at caltech investigated the reaction 14n+2d → 12c+α and discovered that on top of the emitted α particles also γs with energies 1.9,3.1,4.0,5.3 & 7.0 mev were emitted. it became clear already at this epoch that there exists a level at ∼ 7.2mev but it is weakly coupled to the ground state, namely the transition to the ground state was too weak to be observed! hence, only an upper limit to the rate of transition could be found. the implication was that indeed, if the reaction product goes to excite this level in 12c, then extremely few 12c nuclei would decay from this state to the ground state. it appeared therefore, that from stellar nucleosynthesis this is not likely to be the way 12c forms. but this question of transition probability was not yet raised. in the same year holloway and moore (1940) repeated the experiment 14n+2d → 12c+4he and confirmed the existence of the levels at 4.37 & 7.62mev and suggested that in most cases the (excited) 12c∗ disintegrates by emitting an α particle. they wrote that: the corresponding excited state of 12c would be unstable against α emission, but it is still easily conceivable that such a state could not actually emit an α because 313 g. shaviv of selection rules. clearly, in the first case this is not the way to form carbon while if carbon is formed in this way we can claim that astrophysical situation implies that the channel in which 12c∗ disintegrates by emitting an α may exist but along with the decay to the ground state. as for our particular reaction, what holloway and moore argued was that in the reaction 8be+α↔12 c+γ the compound nucleus disintegrates mostly into the incoming channel. terrell (1950) examined the 9be+α → 12c+n and found no evidence for excited states in 12c. in the same year johnson (1952) investigated the 11b+2d→ 12c+n reaction and found the 4.4 & 9.6mev levels but not the one around 7mev. it should be realized that these experiments are very difficult and tricky and hence no wonder that it took such a long time to find the accurate structure of the nucleus of 12c. in 1950 hornyak et al. summarized the known data of the 12c nuclear structure as depicted in fig. 6. the 7.86mev level is shown but very weak, namely only rare transitions into it, and hence a problem to experimentalists. lauritsen and fowler were co-authors on this paper. in 1951 miller & cameron followed the motion of 8be nuclei in nuclear emulsion and observed their decay. they found a lifetime of 5 ± 1 × 10−14sec. this lifetime is 106 times longer than the two α’s mutual crossing time. this was the paper that put an end to a long line of papers that claimed alternatively that 8be is unstable and unstable. miller & cameron succeeded to watch the motion of the 8be nucleus in emulsion and see its decay. we mentioned above that α-like nuclei are expected to be more bound than their neighbors. here we have a nucleus composed of just two α nuclei and it is unstable! 7 the wrong solution some people claim that salpeter, who discovered the basis for the triple alpha process, must share the credit with öpik. öpik, according to this claim, solved the problem of the helium fusion to carbon already in 1951. the trouble was, so goes the claim, that öpik published his paper in the proc. royal irish acad. 1951. a seldom visited by astrophysicists journal. but öpik’s paper is wrong and not identical with that of salpeter. öpik, who had many important and very original contributions, apparently did not read the nuclear literature or ignored it, because he ignored the fact the 8be is unstable, a fact known already in 1951. so öpik assumed a 3 body collision. the α + α penetration takes about 0.8 × 10−20sec and the third α must collide within this time. clearly, the lifetime of 8be as assumed by öpik, is off by a factor of 106. this factor enters into the rate. moreover, despite the fact that the energy level in the 8be continuum was already known, öpik overlooked it. öpik assumed that he burning lasts 1014sec. the question then was at what temperature would helium burning last this time and with his wrong reaction rate öpik derived that helium burning takes place at 6 × 108k. this is known today as far off and it implies a discrepancy between the formation of 8be via two α′s and the formation of 12c, as we will shortly see. öpik’s paper did not attract the astrophysical community and from its publication in 1951 till 2009 öpik’s paper was cited just once, and it was by salpeter... in 1972 marshal wrubel wrote a review on ernst öpik’s contributions to red giants and did not mention his contribution to the 3α process. the uncertainty in the energy levels prevailed in 1950. guier and roberts looked at: 9be+α → 12c +n and claimed the level is at 7.8mev. the experiment was repeated with bertini joining the team, and no level was observed. in 1952 azjenberg & lauritsen prepared a compilation of all the experiments and provided the following summary in fig. 7. our particular level is well marked. 246 chapter 8. how nature overcomes its own barriers in a figure which provided the structure of energy levels in 12c. as can be seen from fig.??, a level at 4.43mev and a level at 7.5mev appeared as well as the quantum numbers j = 2+ and j = 0, respectively49. no parity is assigned to the upper level. the only reference given for this information is 0cloud-chamber investigation0 without the details of the paper. however, the only researchers to apply a cloud chambers on a close problem were crane, delsasso, fowler and lauritsen50 back in 1935. figure 8.12: the structure of 12c as was known in 1952. for the ease of reading this heavy with data figure, we marked energy level at 7.5mev with red and the level of 8be +↵ is marked with green. note that the spin of the level is given, indicating that the 8be+↵ can create the excited 12c nucleus. it is this coincidence which led later to philosophical hypothesis. from ajzenberg and lauritsen 1952. the data on the quantum numbers of the energy levels is important. it was well known that the ground state of 12c is j = 0+. it is also well known that a transition from a j = 0+ to j = 0+ is strictly forbidden. the spin of the photon is 1. hence a zero spin to a zero spin transition does not leave room for the photon, so that angular momentum can be conserved. hence, if a bound carbon nucleus is to be the end product, it is not su�cient to have this energy level because no direct transition from the 7.5mev state to the ground state is possible. another energy level above the ground state and below the level at 7.5mev must exist and must have the right quantum numbers so that the transition to the ground state can go through an intermediate state. 8.9 salpeter the solution is two plus one in the early nineteen fifties, willy fowler, who was already then the insatiable force behind the kellogg laboratory, in caltech, consulted extensively hans bethe, who was at cornell. after a while, bethe agreed to send to fowler one of his best young men and edwin salpeter (19242008) was his choice. salpeter spent the summer of 1951 in the kellogg laboratory. it is during this and subsequent stays that salpeter carried out his research on how helium can be synthesized into carbon. on october 1952 salpeter submitted his first short paper to the astrophysical journal51. in the same month of october, the physical review published a paper by ajzenberg and lauritsen, who worked in the same kellogg laboratory, in which the resonance level in 12c was marked at 7.5mev and with quantum number assignment of j = 0. no parity was given. salpeter submitted his paper after returning 49in 1950 azjenberg and lauritsen had the level at 7.mev and it is not clear why the level 0moved0 half an mev upward. 50crane, h.r., delsasso, l.a., fowler, w.a., & lauritsen, c.c., phys. rev. 48, 100, (1935) 51salpeter, e.e. apj, 115, 326, (1952) figure 7: the structure of the 12c nucleus as summarized in 1952. the energy level under discussion is marked in red and is at 7.5mev. note that the authors assigned the level j = 0, which is identical with that of the ground state. but 0→ 0 transitions are forbidden. 314 who discovered the hoyle level? 8 salpeter enters the game salpeter entered the game in 1951 just after the publication of the bethe-salpeter equation. it was upon fowler’s request for help in the theory, that bethe decided to send his distinguished young physicist salpeter to the kellogg laboratory at caltech. salpeter spent two summers in caltech. on october 1951 salpeter submitted his first paper to the apj: 12c had no level around 7.6mev. on october 1951 ajzenberg & lauritsen submitted a paper to physical review in which 12c had a level at 7.5mev with j=0 (no known parity). two of the most important results for the triple alpha process were published at the same time by people from the same laboratory in two different journals and no citation was given to one another. they simply did not know of each other. when gamow considered in 1938 the possible energy source of ms stars he assumed, in an attempt to overcome the a=5 barrier, that: 24he ↔ 8be, namely the reaction is in a dynamic equilibrium and assumed 8be to be stable. salpeter was unaware of this publication of gamow but knew already that 8be is unstable. so salpeter, facing the same dilemma as gamow, assumed that the two α′s go into the 95kev level (which was known already to salpeter) in the continuum and the so formed nucleus lives long enough (just 10−14sec which were inferred from the width of the level) for a third α to collide and create a 12c nucleus. salpeter realized that 10−14sec is orderes of magnitude longer than the two α′s self-crossing time and hence his treatment was justified because 8be lives a long time before it decays and the assumption of equilibrium is fully justified. if so, there is no need for a cross section! next, salpeter assumed that the 12c nucleus ”somehow decays” in flight (no level in 12c was known to certainly exists) into the ground state of 12c. salpeter stressed that he assumed no resonances in 12c,16 o,20 ne,24 mg . . .. salpeter felt uneasy about it and wrote that: the nuclear γ-ray width for the formation of 12c (but not the one for 8be) is required. this width has not yet been measured, and the position of resonance levels was not known accurately enough and an estimate of 0.1ev was used for this width. hence the correct production rate could be smaller by a factor of as much as 10 or larger by as much as 1000. thus the reaction rate known in the literature was estimated ignoring the possible existence of unknown resonances. two comments: in 1954 öpik wrote a paper about wd and the 3α. he wrote that: the lifetime of the temporary nucleus 8be formed is assumed equal to ∼ 8 × 10−21sec being an estimate of the duration of penetration. the lifetime of true 8be is probably much shorter, about 10−22sec . . . no resonance capture is assumed in this case. moreover, öpik complained that salpeter did not cite him and added: his method of calculation is not quite clear from his brief note. it seems that the reaction 2α → 8be∗ he has treated in a manner similar to ours, where as in 8be+4he → 12c +γ he has postulated a resonance process. the outcome is a formula yielding 1.4× 1013 times higher an energy generation with practically similar temperature as our formula. how many errors can be written in a single sentence? 8.12. the new experiment 249 7.59 4.43 0+ 2+ 0+ gγ gγ4.43 3.16 12c figure 8.13: the status of the level structure of 12c after beghian et al. 1953. figure 8.14: the clear evidence for the two groups of � rays as discovered by beghian et al. 1953. known and documented by researchers from kellogg, as described before. however, many of the required details were still missing and above all fowler did not trust the experimental results. the abstract was presented in the american physical society in albuquerque, new mexico, september 2-7, 1953. the sensational paper was the last one in the last session. the session itself was on nuclear physics not astrophysics. it was a victory to astrophysics and hoyle, in particular in front of skeptical fowler63, that the location of a nuclear level that wandered so much from one experiment to the other, could be determined from observing the stars. shortly after, two papers were published, one by the experimentalists in the physical review and one by the theoretician in the astrophysical journal supplement. this triumph forged the fowler-hoyle collaboration that contributed immensely to nuclear astrophysics for many years to come. the exact reference is an abstract by hoyle, dunbar et al.64 with the title: a state in 12c predicted from astrophysical evidence. the idea was that: the observed 0cosmic0 ratio of he:c:o can be made to fit the yield calculated for these reactions if the reaction 8be + ↵ ! 12c + � has a resonance near 0.31mev, corresponding to a level at 7.68mev in 12c. the abstract also claimed that: a level had previously been reported at 7.5mev, based on ajzenberg and lauritsen 1952. in the same abstract they report about the experiment which led to the discovery of the level at 7.68 ± 0.03mev. the mode of decay of the level is not discussed. 8.12 the new experiment dunbar et al.65 repeated the 14n + 2h ! 12c + ↵ experiment once more using a new special double focusing magnetic spectrometer and discovered that the excited level is at 7.68 ± 0.03mev as can be seen from fig.??. unfortunately, they did not give the quantum numbers of the levels, and it was impossible to determine whether the reaction a stable 12c could be formed. this sophisticated and accurate experiment settled for good the question where is the level but could not answer the crucial question: can a stable 12c be formed? 63salpeter, e.e., publ. astron. soc. australia, 25, 1, (2008) 64hoyle, f., dunbar, d.n.f., wenzel, w.a. & whaling, w., phys. rev, 92, 1095, (1953) 65dunbar,d.n.f., pixley, r.e., wenzel, w.a., & whaling,w., phys. rev, 92, 649, (1953) figure 8: the very nice discovery of the energy levels by beghian et al (1953). in 1953 beghian et al investigated the 9be+α → 12c+n reaction. they detected two groups of γ rays: at 3.16mev and at 4.43mev and concluded that: 12c has two levels: at 4.43 & 7.59mev (the first alternative is shown in fig. 5) . they did not find any γ rays with energies close to 7.5mev. hence they concluded that the probability of the 7.59mev level to decay to the ground state is < 1/2500. willy fowler did not trust any of the previous measurements of the carbon level and searched for a way to carry out a trustful experiment. 8.12. the new experiment 249 7.59 4.43 0+ 2+ 0+ gγ gγ4.43 3.16 12c figure 8.13: the status of the level structure of 12c after beghian et al. 1953. figure 8.14: the clear evidence for the two groups of � rays as discovered by beghian et al. 1953. known and documented by researchers from kellogg, as described before. however, many of the required details were still missing and above all fowler did not trust the experimental results. the abstract was presented in the american physical society in albuquerque, new mexico, september 2-7, 1953. the sensational paper was the last one in the last session. the session itself was on nuclear physics not astrophysics. it was a victory to astrophysics and hoyle, in particular in front of skeptical fowler63, that the location of a nuclear level that wandered so much from one experiment to the other, could be determined from observing the stars. shortly after, two papers were published, one by the experimentalists in the physical review and one by the theoretician in the astrophysical journal supplement. this triumph forged the fowler-hoyle collaboration that contributed immensely to nuclear astrophysics for many years to come. the exact reference is an abstract by hoyle, dunbar et al.64 with the title: a state in 12c predicted from astrophysical evidence. the idea was that: the observed 0cosmic0 ratio of he:c:o can be made to fit the yield calculated for these reactions if the reaction 8be + ↵ ! 12c + � has a resonance near 0.31mev, corresponding to a level at 7.68mev in 12c. the abstract also claimed that: a level had previously been reported at 7.5mev, based on ajzenberg and lauritsen 1952. in the same abstract they report about the experiment which led to the discovery of the level at 7.68 ± 0.03mev. the mode of decay of the level is not discussed. 8.12 the new experiment dunbar et al.65 repeated the 14n + 2h ! 12c + ↵ experiment once more using a new special double focusing magnetic spectrometer and discovered that the excited level is at 7.68 ± 0.03mev as can be seen from fig.??. unfortunately, they did not give the quantum numbers of the levels, and it was impossible to determine whether the reaction a stable 12c could be formed. this sophisticated and accurate experiment settled for good the question where is the level but could not answer the crucial question: can a stable 12c be formed? 63salpeter, e.e., publ. astron. soc. australia, 25, 1, (2008) 64hoyle, f., dunbar, d.n.f., wenzel, w.a. & whaling, w., phys. rev, 92, 1095, (1953) 65dunbar,d.n.f., pixley, r.e., wenzel, w.a., & whaling,w., phys. rev, 92, 649, (1953) does not exist! figure 9: the structure of 12c after beghian et al discovery. the direct transition from the 7.59mev to the ground state is forbidden. 315 g. shaviv the symmetry of the 12c ground state leads to a j = 0+ state. the state at question appears to have also j = 0+. angular momentum conservation do not allow the 0+ state to decay into the ground state which is also 0+. hence, if eventually the decay of this state leads to the ground state, there must be another intermediate level below the 7.59mev one with the proper spin, to which this level can decay. hoyle never mentioned these requirements nor allowed and forbidden transitions. he tacitly assumed that the 7.69mev level ’somehow’ decays to the ground state. 9 1953 kellogg phase i when martin schwarzschild and fred hoyle tried to evolve main sequence stars off the main sequence and derive the red giant, the modeling failed and they could not get the red giant branch. beside the failure to derive the branch, there was a problem with the composition. the rate of 12c + α (carbon conversion into 16o) was much greater than the rate of carbon formation and hence no carbon was left after helium burning. the model moved from helium to oxygen leaving no carbon. hence, hoyle argued that there should be a level at about 7.6mev which accelerates the reaction and leads to the formation of carbon (relative to its destruction). hoyle spoke only on the energy of the level and he knew at what energy in 12c it should be because he assumed it takes place via 8be + α. this is exactly the level we discuss here. 250 chapter 8. how nature overcomes its own barriers 8.13 hoyle: we must have carbon in our universe! in 1954 hoyle published an extensive research on the synthesis of the heavy elements66 and discussed the synthesis of carbon as the starting point. this is the same paper in which hoyle proposed how the synthesized elements spread in the galaxy, see sec. ??. hoyle followed salpeter and assumed the dynamic equilibrium for ↵ + ↵ *) 8be and applied statistical mechanics to find the abundance of the beryllium. as salpeter did not provide the equation and only quoted the result, hoyle cited himself for the equation of equilibrium.67 in that paper hoyle discussed the formation of the heavy elements under statistical equilibrium. no mention of gamow’s 1938 paper and his equilibrium 8be. figure 8.15: dunbar’s et al. 1953 result. a beautiful manifestation of the predicted 7.68mev level. once carbon is synthesized it can absorb an additional ↵ particle and become oxygen, which in turn can again absorb an ↵ particle and become neon: 12c + ↵ ! 16o + � followed by 16o + ↵ ! 20ne + �. in principle, the 20ne can capture another ↵ particle to form 24mg, but the increasing coulomb barrier reduces the rate so much that it is permissible to neglect the ↵ capture past oxygen. the crucial point is therefore, that carbon and oxygen are synthesized at the same time and not one after the other. thus, on one hand the carbon is synthesized and on the other it is destroyed. by the end of the day, the final amount of carbon depends on the ratio between the rate of formation and the rate of destruction. hence, hoyle defined a parameter:  = a ⇥ rate(12c + ↵ ! 16o) rate(3↵ ! 12c) where a is a numerical factor, so that relevant values of  will be of the order of unity. clearly,  depends on the temperature as well as on the properties of the energy levels in carbon and oxygen. of all the data which enters into the expression for , it is most sensitive to the eres = e � e(8be + ↵) because  ⇠ e �eres kbt = e � (e�e(8be+↵)) kbt , where e is the energy of the level in the 12c nucleus. all energies are above the ground state of 12c. the energy dependence is exponential. assuming the salpeter’s rate for the triple ↵ reaction and the problematic (see later) subsequent reaction 12c + ↵ !16 o, hoyle solved for the abundances of carbon and the results are shown in fig. ??. it can be seen from the figure that when  = 1/9 the amount of carbon produced by the time the helium is exhausted, is 1/3 which corresponds to an abundance ratio of c/o=1/2, the value hoyle took as the observed cosmic value. also, one can see that a small variation in  from 1/3 to 1/15 spans a carbon abundance which covers the observed value. on the other hand, if there would be no resonance at all in 12c, the value of  would have been orders of magnitude smaller and no carbon would be left at the 66hoyle, f., apjs, 1, 121, (1954) 67hoyle, f., mnras, 106, 343, (1946) figure 10: the structure of 12c after dunbar et al discovery. when hoyle came to kellogg in the first time he convinced ward whaling to look for this level and indeed whaling went to the lab and found the level exactly where hoyle claimed it must be. the level was rediscovered! hoyle spoke about the energy of the missing in calculation level and did not discuss any spin, selection rules etc. the abstract was presented in the american physical society meeting in albuquerque, nm, sep 2-7, 1953. the paper was presented in the session on nuclear physics not astrophysics. it was a victory for hoyle in particular in front of skeptical fowler. 10 how did hoyle predict the nuclear level in 12c hoyle assumed the that κ defined as: κ = a rate(12c + α→16 o + γ) rate(3α→ γ) = destruction formation is given and calculated the resulting mass fraction of 12c after the burning of helium into carbon. hoyle obtained in this way the results shown in fig. 11. it is easily seen that κ � 1 (the destruction is much faster than formation) yields no carbon at the end of helium burning. 8.14. the kellogg laboratory group phase ii 251 end of the helium burning.if the formation of 12c is much slower than its destruction, the end product if almost pure 16o. figure 8.16: the formation of carbon from helium as a function of hoyle’s parameter . this is the figure which convinced hoyle that 12c should have a resonance. in addition, hoyle carried out the inverse calculation in a style which is known today as 0reverse engineering0, namely what must t and eres be so as to get the observed abundance, and he found t = 1.4 ⇥ 108k and eres = 0.33mev (above the rest mass of 8be + ↵) which corresponds to e = 7.705mev in the 12c nucleus. in summary, hoyle was able to apply astrophysical arguments to solve the problem of the carbon energy level, the exact location of which wandered from one experiment to the other. shortly after the idea that such a resonance must exist or else, the cosmos will have no carbon to support life the way we are familiar with, was born. the fantastic story about how astrophysical consideration led to the prediction of a nuclear level triggered the invention of the anthropic principle68. 8.14 the kellogg laboratory group phase ii hoyle’s victory was not complete. cook et al.69 found it necessary to carry out a new experiment again because the experimental evidence on the character of the 7.7mev 12c state is not entirely clear. it seems well established that the state does not radiate directly to the ground state but rather cascades via the 4.43mev state. furthemore, cook et al added that one must (a) make sure that the 12c level can be formed by 8be+↵. the prerequisite for that are the right spin and parity and that there is a non vanishing probability that it decays by emitting these particles. (b) it must have a finite probability to decay to the lower excited state or the ground state. these questions should be best explored by bombarding 8be with ↵ particles, but since 8be is unstable, recourse must be made to study the two possible modes of decay of the excited state of 12c, namely 12c⇤ ! 8be + ↵ and 12c⇤ ! 12c + �. then one has to rely on the principle of reversibility of nuclear reactions. indeed, hoyle did not predict the quantum numbers of the level and without these the prediction is not terribly powerful the experiment cook et al. was innovative and di↵ered substantially from all previous ones. they created the radioactive isotope 12b, which has an energy of 13.378mev above the ground state of 12c and decays via a � decay (in contrast to a � decay) into all excited levels of 12c with lower energy and in particular into the two relevant levels for our discussion here, cf. fig.??. special arrangement was prepared to detect the emitted ↵’s using a strong focusing magnetic spectrometer. the basic problem cook et al. faced with the 7.68mev level was the following: it was established before that there is no direct transition to the ground state. on the other hand, no one observed that this level disintegrates into 8be + ↵70. there were merely conflicting estimates of the probability to emit 68the anthropic principle is a philosophical claim that the universe must be compatible with the existence of life as is observed. 69cook, c.w., fowler, w.a., lauritsen, c.c. & lauritsen, t., phys. rev., 107, 508, (1957) 70recall, nuclear reactions under astrophysical conditions are usually very slow because the energies are low. so the 8be+↵ yielding 12c and decaying back to the products was hopelessly slow and hence, not observed figure 11: the argument by hoyle that the resonance must exist. the paper by hoyle, dunbar et al had the title: a state in 12c predicted from astrophysical evidence. the abstract also admitted that: a level had previously been reported at 7.5mev, based on ajzenberg and lauritsen 1952. . on the other hand, the decay mode of the level a crucial point was not discussed at all. beghian discovery of the 7.59mev level was overlooked. but hoyles victory was not complete his friends did not accept the idea. could hoyle invert the process and learn nuclear physics from the stars? cook, fowler, t. lauritsen and c.c. lauritsen 1957 argued that:experimental evidence on the character of the 7.7mev state is not entirely clear. it seems well established that the state does not radiate directly to the ground state but rather cascades via the 4.43mev state. the authors added that: one must (a) make sure that the level can be formed by 8be + α. the spins should 316 who discovered the hoyle level? agree. (b) it must have a finite probability to decay to the ground state. note: the direct reaction cannot be investigated in the lab because the rate is very slow. consequently, the 12c level must be populated indirectly. cooks et al. had a sever technical problems: on one hand: it was established that there is no direct way to the ground state. on the other hand no one observed that the compound 12c nucleus disintegrates into 8be∗ + α. there were conflicting estimates of the probability to emit an α. uebergang and independently steffen, got that the excited 12c nucleus emits α at about << 50% of the cases while bent et al and independently hornyak got that it emits an α in >> 97% of the cases. 252 chapter 8. how nature overcomes its own barriers an ↵ particle. on one hand, uebergang71 and ste↵en et al.72 estimated the probability to be ⌧ 50% and on the other hand, bent et al.73 and hornyak74 estimated it to be � 97%. figure 8.17: cook et al. 1957 created the radioactive nucleus 12b which decays into 12c. most of the decays go into the ground state and only 1.3% go into the investigated level. cook et al. managed to get only an upper limit to the probability of decay into 8be + ↵. since this was by far the most probably mode of decay of this level, the exact value was crucial. so here they were forced to rely on russell, phillips and reich75 and heydenburg and temmer76 who found an upper limit which was about 250 times smaller than predicted. with the improved (lower) upper limit they were able to reach their most important result, namely, that the probability for � decay to the 4.43mev level is: 0.0010.0028. very small but not zero. next they found that the probability to decay through the emission of an electron-positron pair is about 10�5 and hence negligible. 8.15 salpeter-1957: completing the job salpeter’s second and updated paper77 was submitted together with the cook et al. paper and the two papers were published back to back. at the time, beginning of 1957, the spin of the 7.68mev level was not yet certain though very recent experiments seemed to provide the final proof of the quantum numbers of this level. fregeau and hofstadter78 were interested in using high energy electron beams to investigate the surface of nuclei and they considered that the 12c would be an ideal case. so they bombarded 12c with high energy electrons. this and subsequent works of this type won for hofstadter the 1961 nobel prize.79 fregeau and hofstadter treated already in 1955(!) the 4.43mev and 7.68mev levels of carbon as so well established, that they did not give any reference to prior experiments. as for the spin of the 7.68mev level, they state that: j = 0+ is not inconsistent with the experimental results that they found. the levels emerged very nicely in their electron scattering experiments. on the other hand, salpeter argued that the only possibilities were 0+ or 2+. if the 2+ was assumed then the probability for electron-positron decay (symbolized in nuclear physics as �e±) could be theoretically calculated and it was found to be 1000 smaller than the one obtained if 0+ was assumed and this 71uebergang, r.g., australian j. phys.,7, 279, (1954) 72ste↵en, k.g., hinrichs, o., & neuert, h., zeit. f. phys., 145, 156, (1956) 73bent, r. d., bonner, t. w., mccrary, j. h., ranken, w. a., phys. rev., 100, 771, (1955) 74hornyak, w.,f., bull. am. phys. soc. ser, ii, 1, 197, (1956) 75russell, j. l., phillips, g. c., & reich, c. w., phys. rev. 104, 135, 143, (1956) 76heydenburg, n.p. & temmer, g.m., phys. rev., 104, 123, (1956) 77salpeter, e.e., phys. rev., 107, 516, (1957) 78fregeau, j.h., & hofstadter, r., phys. rev., 99, 1503, (1955). ibid. 104, 225, (1956) 79the citation of the prize read for his pioneering studies of electron scattering in atomic nuclei and for his thereby achieved discoveries concerning the structure of the nucleons . figure 12: the final experiment by cook et al. 1957: creates the nucleus 12b and follow its decay into the 7.653mev level (only 1.3%). to overcome the problems cook et al 1957 created the radioactive nucleus 12b which decays into 12c. most of the decay goes into the ground state and only 1.3% decays into the investigated level. 11 1957 salpeter finishes the job remaining problems: what is the spin of the 7.68mev state? fregeau & hofstadter (1955) using electrons scattering from the nucleus (an experiment for which hofstadter got the nobel prize 1961), claimed that j=0+ is not inconsistent with experiment. so salpeter assumed j = 0+ or 2+. the latter yields a result which is about 1000 smaller than the first one. 8.15. salpeter-1957: completing the job 253 result contradicted the result of the cal tech experiment80. now came the critical question, what is the probability to decay back into the incoming channel, 8be + ↵. salpeter resorted to the wigner theory81 and calculated an upper limit for the case 0+ which was 40% higher than the one adopted by cook et al. the other possibility was proven by salpeter to contradict the experimental results. to further provide support to his estimates of the probabilities, salpeter derived the probabilities by assuming the ↵ model for the 8be nucleus. the numbers agreed. 3α 8 be+α q1=0.278 q2=0.094 j=0+ j=2+ j=0+ 7.654 4.43 0 γα γe+e-γγ figure 8.18: the structure of 12c assumed by salpeter in 1957. �↵ is the probability of decay emitting an ↵ particle, �� is the probability of decay emitting a � photon and �e± is the probability to decay by emitting an electron positron pair. this is after salpeter obtained the improved results of cook et al. 1957. finally came the question what is the probability �� to decay into the bound 4.43mev level. after all, this was the dominant mode to form a stable carbon nucleus. again, the estimate depended on the model for the carbon nucleus. if one assumed that the carbon nucleus was made of three ↵ particles, one got a very small probability to decay into the first excited state. so after some lengthy theoretical discussion salpeter adopted that the probability to decay into the ground state plus the probability to decay into excited state, namely the total probability to decay into the ground state, was 0.00014, quite small. salpeter made an additional crucial assumption. since the probability to decay back into the incoming channel (8be+↵) is by far the largest, or in other words, the leakage to modes of decay other than the mode of formation is extremely small, it is permitted to assume an equilibrium 8be + ↵ *) 12c ⇤ . the unbound 2 ↵’s are reluctant to absorb a third ↵ and become bound. once this is done and statistical mechanics can be used to calculate the abundance of the 12c nuclei, the details of the nuclear reaction became irrelevant! the probability to form carbon in the ground state is then the number of carbon nuclei in the excited state (as obtained form the equilibrium condition) times the probability that they decay to the ground state of carbon. at the end of january 1955 the american physical society had its annual meeting in new york. in a session on reactions of transmutation and nuclear energy level, salpeter presented preliminary results on the e↵ect of the 7.68mev82. by now, salpeter became aware of the ajzenberg and lauritsen coming up summary (it appeared in his paper as 0to be published0) of the energy levels of 12c and derived for the first time the full reaction rate. hayakawa et al.83 got the information from salpeter, who also informed them about the probability that the 7.68mev excited state decays to the 4.43mev level, and submitted their paper to the progress in theoretical physics japan, on july 1956 to be published november 1956. salpeter’s paper, on the other hand, was submitted march 1957 to be published july 1957, that is to say, over a year later. so before salpeter managed to publish his results in a journal, hayakawa et al. published the calculation of the rate including the excited state of 12c and wrote that: this rate is about 106 times larger than that given by salpeter. they meant salpeter 1952. they continued to state that: such a great di↵erence is due mainly to the fact that he did not take the e↵ect of the recently discovered resonance level in 12c into account. this is one of the most important conclusion obtained in our work. it may have been the most important 80most recent result: chemykh, m. and 5 authors, proc.13th int. symposium capture gamma-ray spect., aip conf. proc. 2009 is �± e = 6.2 ⇥ 10�5ev . 81blatt, j., & weisskopf, v., theoretical nuclear physics, john wiley & sons, inc. ny, 1952. 82salpeter, e.e., phys. rev. 98, 1183, (1955) 83hayakawa, s., hayashi, c., imoto, m., & kikuchi, k. prog. theor. physics, 16, 507, (1956) figure 13: the part of the energy schemes of the 12c nucleus relevant to the 3α reactions as was finally assumed by salpeter in his final paper in 1957 the structure of 12c as assumed by salpeter in 1957, is given in fig. 13. γα is the probability of decay emitting an α particle, γγ is the probability of decay emitting a γ photon and γe± is the probability to decay by emitting an electron-positron pair. this is a rare mode of decay and of no importance to our story here. this was the structure of 12c after salpeter obtained the improved results of cook et al 1957. salpeter made some critical assumptions: the disintegration channel 12c∗ decaying back into 8be + α is the dominant channel and all other possibilities are very small leakages. consequently, salpeter assumed a dynamic equilibrium, namely 12c∗ ↔8 be + α. if so, the concentration of 12c is determined from the equilibrium (small sensitivity to the energy of the level) and all the uncertainty is in the small leakage to the other channels. in particular, the is no need for a cross section,to evaluate the rate. the reaction is in a statistical equilibrium. on january 1955 salpeter presented the results in the new york meeting of the physical society. by now he became aware of the ajzenberg & lauritsen old result and cited it. fowler won the 1983 nobel prize (with chandrasekhar) for contributions to nuclear astrophysics, but fowler’s nobel speech was one long discussion about . . . hoyles contributions. as for salpeter, fowler commented that he ignored the 7.68mev state which is a very wrong claim. he ignored it when it was unknown to him. fowler was a great experimental nuclear physicists but without knowledge in statistical mechanics and he did not like that ’the nuclear physics’ was eliminated from the problem. 317 g. shaviv hoyle and salpeter shared the 1997 crafoord prize1 in particular for the physics of the triple α reaction. the process is called today the salpeter process and the energy level is called the hoyle level. fight for priority: salpeter informed hayakawa et al. about the probability that the 7.68mev state decays into the 4.43mev state. hayakawa et al hurried and submitted their paper to progress of theoretical physics japan in july 1956 in which they made just this claim. the journal published on november 1956. salpeter published his work only in 1957. surprisingly the japanese authors claimed that: this (meaning theirs) rate is 106 times greater than given by salpeter 1952. such a great difference is due mainly due to the fact that he did not take into account the 12c resonance. they did not mention that it was salpeter who told them about his work and the 12c level..... 12 is this the entire story? is this the entire story? no! what about the structure of 16o? following hoyle, we treated the reaction 12c + α16 → o + γ as well established. however, this is not the case. in 1974 dyer and barnes from caltech attempted to measure the 12c+α reaction. the next attempt was carried out in 1982 when kettner et al. from münster measured the reaction and discovered that it is 3 to 5 times faster then what dyer and barnes from caltech found. as a consequence, the most abundant specie at the end of helium burning was found to be 16o and not 20ne as the formation of 16o is faster than its destruction. langanke and koonin (1983) criticized the analysis and the conclusions of the experimenters and repeated the very long theoretical analysis of the experimental data. however, they could not resolve the discrepancy between the caltech data (dryer and barnes) and the münster data (kettner et al.) and fitted each experiment separately. thus, the münster data was 1.5 time higher than that of caltech, which in turn was 3 times higher than what stellar modelers used. as lankange and koonin wrote, such higher values , as those found in münster and caltech, lead to 16o rather than 12c, as the final product of helium burning, and in this way cast a shadow on hoyles argument. in fig. 15 we show a comparison between two recent experimental result and a theoretical fit. the red arrow shows the energy range in stars where this reaction takes place. so far this experimental discrepancy is not sett led. 8.18. carbon structure is half the story: the 12c + ↵ !16 o + � reaction 255 very high. due to the fact that these levels are rather wide86, they all contribute to the rate of the reaction. consequently, the locations of the levels up to about 10mev are important for the rate of 8be + ↵ at t < 109k. the higher in energy levels corresponds to such a high energy range that by the time the colliding species have enough energy to reach these levels, the temperature is so high that all nuclei disintegrate and hence, cannot fuse any further. in 1994 freer at el87 investigated whether the 12c 7.65mev level could decay directly into 3 ↵ in contrast of a decay to 8be + ↵ first and then the 8be would break into 2 ↵s. the results for this direct decay is less than 4%. this was an additional experimental proof that the triple alpha is not a three body reaction. the problems in getting accurate value for the probability for the 7.68mev level transition to the 4.43mev one continued to annoy physicists. the recent values are: alburger88 (3.3±0.9)⇥10�4, hall and tanner89 (3.5±1.2)⇥10�4, seeger and kavanagh90 (2.8±0.3)⇥10�4, and mak et al.91 (4.30±0.2)⇥10�4. it is di�cult to achieve high accuracy! 8.18 carbon structure is half the story: the 12c+↵ !16 o+� reaction αα12c+ 6.049 6.130 6.917 7.1157.162 j=1j=2+ j=3j=0+ j=0+ o16 figure 8.19: the structure of the oxygen nucleus 1952. based on ajzenberg and lauritsen 1952. we come to the destruction of carbon. the existence of excited levels in 16o was discovered by burcham and freeman92, who used the reaction 19f + p ! 16o + ↵ and found the 6.94mev and the 7.15mev levels. they however, did not determine the quantum numbers of the level. in 1950 millar, bartholomew and kinsey93 investigated the � rays from the decay of 16n ! 16o + e�. this radioactive isotope is produced in the cooling water of nuclear reactors via the reaction 16o + n ! 16n + p. the half lifetime of the isotope is 7.35 sec. the energy of 16n is so high that it can decay into the first two levels of 16o by emission of an electron. thus, they discovered � rays which corresponded to the level at 6.133 ± 0.011mev and 7.10 ± 0.02mev. these results were in good agreement with the values found by chao, tollestrup, fowler and lauritsen94 of 6.136 ± 0.030mev and 7.111 ± 0.03mev. to complicate the issue, they did not discover � rays which would correspond to the level at 6.91mev. they were however, able to determine the quantum numbers of the level as j = 1�. the situation became complicated once more. the 12c + ↵ have a restmass energy of 7.162mev, while the closest energy level in the 16o nucleus is at 7.115mev, that is to say, just below the threshold of the colliding particles. because all energy levels save the ground state, are not stable they have a certain width in energy. the width �e is related to the lifetime �t through the relation �e�t ⇠ h̄. the 7.115mev level in 16o is su�ciently wide to extend into energies slightly above the 86according to the uncertainty principle, the width of the level is connected to the life time of the system in that level. from a nuclear reaction point of view it means that if the energy of the colliding particles is within the wide range of the level, and not just equal to the prescribed energy, the reaction can proceed. 87freer, m., wuosmaa, a.h., betts, r.r., henderson, d.j., wilt, p., zurmuhle, r.w., balamuth, d.p., barrow, s., benton, d., li, q., liu, z., & miao, y., phys. rev. c, 49, 1751, (1994) 88alburger, d.e., phys. rev., 124, 193, (1961), who used the reaction 10b + 3he ! 12c + p. 89hall & tanner , nuclear phys.,53, 673, (1964), who used the reaction 10b + 3he ! 12c + p. 90seeger, p.a. & kavanagh, r.w., nucl. phys., 46, 577, (1963), who used the reaction 14n + 2d ! 12c + ↵ 91mak, h.-b., and 4 co-authors, phys. rev. c,12, 1158, (1975) 92freeman, j.m. & baxter, a.s., nature,162, 696, (1948). burcham, w.e., & freeman, j.m., phys. rev. 75, 1756, (1949) 93millar, c. h. , bartholomew, g. a. & kinsey, b. b., prl, 81, 150, (1951) 94chao, c. y. ,tollestrup, a. v. , fowler, w. a. & lauritsen, c. c. , phys. rev. 79, 108, (1950) figure 14: the structure of 16o based on ajzenberg & lauritsen 1952. the partial width of the relevant level at 7.115mev is not known because it is a very difficult measurement. the uncertainty in the level is marked by the grey zone around the level. the difficulty stems from the fact that the level lies just below the continuum and hence extremely difficult to feed in. the next question is where carbon is synthesized? or what happens if the carbon level were at another energy? would carbon still be formed? the answer is 256 chapter 8. how nature overcomes its own barriers 12c + ↵ threshold. thus the carbon plus the alpha combine to form the excited oxygen nucleus via the upper tail of the level. on the other hand, as the width of the level is large, the probability to breakup into 12c + ↵ is very small and as a matter of fact, was never observed. in 1974 dyer and barnes95 from caltech attempted to measure the 12c + ↵. the next attempt was in 1982 when kettner et al.96 from münster measured the reaction and discovered that it is 3 to 5 times faster then what dyer and barnes from caltech found. as a consequence, the most abundant specie at the end of helium burning was found to be 16o and not 20ne langanke and koonin97 criticized the analysis and the conclusions of the experimenters and repeated the very long theoretical analysis of the experimental data. they could not resolve the discrepancy between the caltech data (dryer and barnes) and the münster data (kettner et al.) and fitted each experiment separately. thus, the münster data98 was 1.5 time higher than that of caltech, which in turn was 3 times higher than what stellar modelers use. as lankange and koonin wrote such higher values , as those found in münster and caltech, lead to 16o rather than 12c, as the final product of helium burning, and in this way cast a shadow on hoyle’s argument. figure 8.20: the measured capture probability (in units of nano-barns) by the munster (1982) and the kellogg (1974) laboratories. the arrow marks the energy range at which the reaction take place in stars. the continuous lines are the theoretical fit by langanke and koonin 1983 and it includes the e↵ect of the resonance. 0 2 4 6 8 10 0.8 1 1.2 1.4 1.6 1.8 2 2.2 2.4 temperature in 109k 12c+α 16o+γ ra tio of pr ed ic te d re ac tio n ra te s kunz et al(2002) caughlan & fowler (1988) figure 8.21: the ratio between the newest rate calculated by kunz et al (2002) and the standard rate compiled by caughlan and fowler (1988) used in many calculation of stellar evolution. the ratio is given as a function of the temperature. 95dyer, p. & barnes, c. a., nuc. phys. a233, (1974) 96kettner, k.u. and 8 co-authors, z. phys. a, 308, 73, (1982) 97langanke, k. & koonin, s.e., nuc. phys. a410, 334, (1983). ibid. nuc. phys., a439, 384, (1985). the first paper was published when langanke was still in munster. the second paper was published after he joined koonin in caltech 98the probability for this reaction to take place at thermal energies (t = 2 ⇥ 108 or 300kev) was given by s(300kev ) = 350 kev barn (münster), 240 kev barn (caltech) and 80 kev barn in standard nucleosynthesis calculations at that time. figure 15: the measured capture probability (in units of nano-barns) by the munster (1982) and the kellogg(1974) laboratories. the arrow marks the energy range at which the reaction takes place in stars. the continuous lines are the theoretical fit by langanke & koonin 1983 and it includes the effect of the resonance. 1 the crafoord prize in astronomy and mathematics, biosciences, geosciences or polyarthritis research is awarded by the royal swedish academy of sciences annually according to a rotating scheme. the prize sum of sek 4 million makes the crafoord one of the worlds largest scientific prizes. 318 who discovered the hoyle level? given in fig. 16 for low mass stars and fig. 17 for high mass stars. we see that ’moving’ the level quite significantly changes the dominant stellar mass at which carbon is formed but not in a way that would required a revision of our ideas.258 chapter 8. how nature overcomes its own barriers -150 -100 -50 0 50 100 150 0.0001 0.001 0.01 0.1 1 10 100 1000 10000 c/ o δe-kev m=1.3msun m=5msun figure 8.22: the c/o ratio and obtained in the evolution of low mass stars (1.3m� and 5.0m�) upon a hypothetical change in the location of the resonance in 12c. -100 -50 0 50 100 2 4 6 8 10 δe-kev c/ o m=15msun m=25msun figure 8.23: the c/o ratio and obtained in the evolution of high mass stars (15m� and 25m�) upon a hypothetical change in the location of the resonance in 12c. 8.20 the c/o ratio today observations and what they imply not a single star without oxygen or without carbon was discovered. detailed observations have shown that the abundance ratio c/o varies from star to star. gradually it became clear that there is no universal value for the c/o abundance ratio which was the basis for hoyle’s analysis and di↵erent stars expose di↵erent ratios. for example, stars with extra high abundance of carbon do not show extra high abundances of oxygen107. examination of the gases ejected from low mass stars shows that when the metals are more abundance by about 50% the c/o ratio is lower by about 50%.108 the c/o ratio appears to be higher in stars with low abundance of heavy elements.109 finally, the c/o appears to vary in low mass stars from 0.2 to 13110. in short, the picture is more complicated and the last word has not yet been said. 8.21 the structure of 12c and the ↵ model: retrospect in 1971 brink111 concluded from the nuclear cluster model that 0our0 state forms a linear chain of three ↵-particles. further indication (from bombardment by electrons), imply that this state has an unusually large radius112. these properties enhance the probability of decay into three ↵ particles. this conclusion was supported in 1997 when pichler, oberhummer, csoto and moskowski113 who concluded that the 0+ level is a genuine three alpha resonance. if so, one would expect that the level would decay directly into three ↵’s and then salpeter’s equation for the nuclear statistical equilibrium may need a change. but the probability of decay directly into three alpha appears to be only about 4%. the reason for this is purely statistical, the phase space of 8be+↵ is that much bigger than the 3↵ mode, in layman terminology: all possible modes of decay have equal probabilities and the number of ways the system can decay into 8be + ↵ is much larger that the number of di↵erent ways it can decay into 3↵s. 107bujarrabal, v. & cernicharo, j., a&a, 288, 551, (1994) 108wang, w. & liu, x.-w., mnras, 381, 669, (2007) 109wahlin, r., and 6 co-authors, memorie della societa astronomica italiana, 77, 955, (2006) 110cohen, m. & barlow, m. j., mnras, 362, 1199, (2005) 111brink, in the alpha particle model of light nuclei, proc. ”enrico fermi” school course xxxvii, varenna, 1966. 112takigawa, n., & arima, a., nucl. phys., a168, 593, (1971) 113pichler, r., oberhummer,h., csoto, a., and moskowski, s.a., nucl. phys. a618, 55, (1997) figure 16: the c/o ratio obtained in the evolution of low mass stars (1.3m� and 5.0m�) upon a hypothetical change in the location of the resonance in 12c. we did not discuss the possible decay of the excited nucleus 12c∗ to 3α. we can, however, repeat hoyle’s argument and argue that the observations imply that this decay, though possible energetically and should take place, is very rare and hence neglected.258 chapter 8. how nature overcomes its own barriers -150 -100 -50 0 50 100 150 0.0001 0.001 0.01 0.1 1 10 100 1000 10000 c/ o δe-kev m=1.3msun m=5msun figure 8.22: the c/o ratio and obtained in the evolution of low mass stars (1.3m� and 5.0m�) upon a hypothetical change in the location of the resonance in 12c. -100 -50 0 50 100 2 4 6 8 10 δe-kev c/ o m=15msun m=25msun figure 8.23: the c/o ratio and obtained in the evolution of high mass stars (15m� and 25m�) upon a hypothetical change in the location of the resonance in 12c. 8.20 the c/o ratio today observations and what they imply not a single star without oxygen or without carbon was discovered. detailed observations have shown that the abundance ratio c/o varies from star to star. gradually it became clear that there is no universal value for the c/o abundance ratio which was the basis for hoyle’s analysis and di↵erent stars expose di↵erent ratios. for example, stars with extra high abundance of carbon do not show extra high abundances of oxygen107. examination of the gases ejected from low mass stars shows that when the metals are more abundance by about 50% the c/o ratio is lower by about 50%.108 the c/o ratio appears to be higher in stars with low abundance of heavy elements.109 finally, the c/o appears to vary in low mass stars from 0.2 to 13110. in short, the picture is more complicated and the last word has not yet been said. 8.21 the structure of 12c and the ↵ model: retrospect in 1971 brink111 concluded from the nuclear cluster model that 0our0 state forms a linear chain of three ↵-particles. further indication (from bombardment by electrons), imply that this state has an unusually large radius112. these properties enhance the probability of decay into three ↵ particles. this conclusion was supported in 1997 when pichler, oberhummer, csoto and moskowski113 who concluded that the 0+ level is a genuine three alpha resonance. if so, one would expect that the level would decay directly into three ↵’s and then salpeter’s equation for the nuclear statistical equilibrium may need a change. but the probability of decay directly into three alpha appears to be only about 4%. the reason for this is purely statistical, the phase space of 8be+↵ is that much bigger than the 3↵ mode, in layman terminology: all possible modes of decay have equal probabilities and the number of ways the system can decay into 8be + ↵ is much larger that the number of di↵erent ways it can decay into 3↵s. 107bujarrabal, v. & cernicharo, j., a&a, 288, 551, (1994) 108wang, w. & liu, x.-w., mnras, 381, 669, (2007) 109wahlin, r., and 6 co-authors, memorie della societa astronomica italiana, 77, 955, (2006) 110cohen, m. & barlow, m. j., mnras, 362, 1199, (2005) 111brink, in the alpha particle model of light nuclei, proc. ”enrico fermi” school course xxxvii, varenna, 1966. 112takigawa, n., & arima, a., nucl. phys., a168, 593, (1971) 113pichler, r., oberhummer,h., csoto, a., and moskowski, s.a., nucl. phys. a618, 55, (1997) figure 17: the c/o ratio obtained in the evolution of high mass stars (15m� and 25m�) upon a hypothetical change in the location of the resonance in 12c. 13 in retrospect in 1985 arnet and thielemann questioned the logic of hoyles original argument as the synthesized carbon may be fused into heavier nuclei or locked in wds. hence, we should re-think how carbon is synthesized and it is not clear that any remnant of the anthropic principle will prevail. however, hoyle’s reverse engineering methodology is right: if we see carbon in nature, there should be a way to synthesize it! today, the principle has its own life and the origin which triggered it is mostly forgotten. in any case the old justification that lead to its inception is not that valid. the story is told in more detail in shaviv (2011). references [1] ajzenberg, f. & lauritsen, t., rev. mod. phys.24, 321, (1952) in 1950 azjenberg and lauritsen had the level at 7.mev and it is not clear why the level ?moved? half an mev upward. [2] beghian, l.e., halban, h.h., husain, t., & sanders, l.g., prl, 90, 1129, (1953) submitted april, 1953 and published june 1953. [3] bethe, h.a. , rev. mod. phys., 9, 167, (1937). this extensive review of nuclear physics earned justifiably the title the bethes bible. doi:10.1103/revmodphys.9.69 [4] bothe, w., & becker, h., zeits. f. physik, 76, 421, (1932) doi:10.1007/bf01336726 [5] cook, c.w., fowler, w.a., lauritsen, c.c. & lauritsen, t., phys. rev., 107, 508, (1957) doi:10.1103/physrev.107.508 [6] crane,h.r., delsasso, l.a., fowler & lauritsen, c.c., phys. rev.,46, 1109, (1934) doi:10.1103/physrev.46.1109.2 [7] crane,h.r., & lauritsen, c.c., phys. rev.,45, 497, (1934) [8] dyer, p. & barnes, c. a., nuc. phys. a233, 495, (1974) doi:10.1016/0375-9474(74)90470-9 [9] gaerttner, e.r., & pardue, l.a. , phys. rev., 57, 386, (1940) doi:10.1103/physrev.57.386 [10] gamow, g., phys. rev., 53, 595, (1938) doi:10.1103/physrev.53.595 [11] guier, w.h., & roberts, j.h. , phys. rev. 79, 719, (1950) doi:10.1103/physrev.79.719 [12] hayakawa, s., hayashi, c., imoto, m., & kikuchi, k. prog. theor. physics, 16, 507, (1956) doi:10.1143/ptp.16.507 [13] holloway, m.g., & moore, b.l., phys. rev., 58, 847, (1940) doi:10.1103/physrev.58.847 [14] hornyak, w.f., lauritsen, t., morrison, p. & fowler, w.a., rev. mod. phys., 22, 291, (1950) doi:10.1103/revmodphys.22.291 [15] kettner, k.u. and 8 co-authors, z. phys. a, 308, 73, (1982) 319 http://dx.doi.org/10.1103/revmodphys.9.69 http://dx.doi.org/10.1007/bf01336726 http://dx.doi.org/10.1103/physrev.107.508 http://dx.doi.org/10.1103/physrev.46.1109.2 http://dx.doi.org/10.1016/0375-9474(74)90470-9 http://dx.doi.org/10.1103/physrev.57.386 http://dx.doi.org/10.1103/physrev.53.595 http://dx.doi.org/10.1103/physrev.79.719 http://dx.doi.org/10.1143/ptp.16.507 http://dx.doi.org/10.1103/physrev.58.847 http://dx.doi.org/10.1103/revmodphys.22.291 g. shaviv [16] kunz, r. and 7 co-authors, apj, 567, 643, (2002) doi:10.1086/338384 [17] johnson, v.r., phys. rev., 86, 302, (1952) doi:10.1103/physrev.86.302 [18] langanke, k. & koonin, s.e., nuc. phys. a410, 334, (1983). ibid. nuc. phys., a439, 384, (1985). [19] lawrence, e.o., mcmillan, e., & henderson, m.c., phys. rev, 47, 273, (1935) [20] lewis, g.n., livingston,m.s., & lawrence, e.o., prl, 44, 55, (1933) [21] miller, c., & cameron, a.g.w., phys. rev., 81, 316, (1951) [22] öpik e. proc. roy. irish acad. a54, 49, (1951). the paper was published over a year after it was read before the irish academy. [23] öpik, e.j., msrsl, 1, 131, (1954), les processus nuclaires dans les astres, communications prsentes au cinquime colloque international dastrophysique tenu liege les 10-12 septembre. [24] shaviv,g. the synthesis of the elements: the astrophysical quest for nucleosynthesis and what it can tell us about the universe (astrophysics and space science library) , springer, 2011. [25] terrell, j., phys. rev., 80, 1076, (1950) [26] wrubel, m.h., irish ajs, 10, 77, (1972) discussion tzumi hachisu: is the carbon-burning c/o ratio still uncertain? giora shaviv: the reduced width of the 16o level is still unknown and there are only guess on its value. sp any c/o ratio between 1/4 to -3/4 is to my mind plausible. in 2002 kunz et al. carried out an extensive theoretical analysis based primarily on kunzs experimental phd thesis. the result of kunz et differs significantly from caughlan & fowler known tables at low temperature which are the relevant temperatures for quiet helium burning. however, it is not the last word on the subject. 320 http://dx.doi.org/10.1086/338384 http://dx.doi.org/10.1103/physrev.86.302 who is who what is the hoyle level what is the anthropic principle the nuclear barrier why nuclear physicists were interested in the problem? the history of the discovery of the 12c nuclear levels the wrong solution salpeter enters the game 1953 kellogg phase i how did hoyle predict the nuclear level in 12c 1957 salpeter finishes the job is this the entire story? in retrospect acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0027 acta polytechnica ctu proceedings 4:27–32, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app self-absorption corrections based on monte carlo simulations kamila johnová faculty of nuclear science and physical engineering, czech technical university in prague, břehová 7, 115 19 prague, czech republic correspondence: kamila.johnova@fjfi.cvut.cz abstract. the main aim of this article is to demonstrate how monte carlo simulations are implemented in our gamma spectrometry laboratory at the department of dosimetry and application of ionizing radiation in order to calculate the self-absorption within the samples. a model of real hpge detector created for mcnp simulations is presented in this paper. all of the possible parameters, which may influence the self-absorption, are at first discussed theoretically and lately described using the calculated results. keywords: mcnp, self-absorption, gamma spectrometry. 1. introduction gamma spectrometry is powerful non-destructive method useful for samples containing gamma ray emitting radionuclides (spontaneous or induced gamma ray activity). due to the principles of gamma ray emission, energy of photons emitted during radioactive decay is specific for each radionuclide. this means that with a proper detection technique it is possible to identify what radionuclide is present in the sample. in addition, with a suitable efficiency calibration the amount of radionuclide in the sample can be estimated. gamma spectrometry can be applied in many scientific fields, like contamination studies, natural radioactivity, activation analysis, astroand high energy physics or geology studies. different applications require a different detection techniques and data analyses. this paper discuss a laboratory gamma spectrometry for natural samples and samples of natural origin. 1.1. interactions of gamma radiation with matter for the issue discussed in this paper three type of photon interactions are the most important: photoelectric absorption, compton scattering and pair production. the probability that a certain photon of a given energy will interact in the matter is expressed by its cross section. the cross section can sometimes be expressed in special unit barn = 10−28 m2. the sum of cross sections for all possible interaction is denoted as total cross section σt . the cross section is closely connected to the attenuation of photons in the matter. mono-energetic photon beam is along a path of length d attenuated exponentially, which is expressed by equation i = i0e −µd, where i0 is a number of photons in non-attenuated beam, i is a number of photons at the end of path d and µ is a linear attenuation coefficient. µ can be expressed in the terms of cross sections for individual interactions (τ -photoelectric absorption, σ-compton scattering, κ-pair production, σrs -elastic scattering) or in the term of total cross section σt µt ρ = na a (τ + σ + κ+ σrs) = na a σt , where µt means total attenuation coefficient (over all interactions), ρ is the density of material, na the avogadro constant and a is an average atomic mass. the expression µt ρ is called total mass attenuation coefficient. 1.2. self-absorption coefficient the previous text suggested that there has to be a certain level of self-absorption within the sample itself. based of the previous informations one can correctly assume that this effect depends on composition of the sample, measurement geometry, density of the material and energy of photons. in general, there are 3 ways how to estimate the self-absorption correction. estimation based on mass attenuation coefficients. several spectrum analysis programs give the user this option, where the library of mass attenuation coefficients is provided. this method is useful over the energy range, where the compton scattering is the dominant interaction. according to the fact, that mass attenuation due to compton scattering is almost independent of an atomic number, reasonable self-absorption correction can be made even for the sample of barely known composition. empirical estimation. this procedure can sometimes be useful for laboratories providing routine measurements. it is specially useful, when the sample of unknown composition and containing lowenergy emitting radionuclide need to be measured. 27 http://dx.doi.org/10.14311/ap.2016.4.0027 http://ojs.cvut.cz/ojs/index.php/app kamila johnová acta polytechnica ctu proceedings in this method three spectra have to be acquired: the sample itself, the sample with a point source place on its top and the point source without the sample. the method with its limitations is in detail described in [1]. using mathematical tools. with the information technology rapid development the mathematical methods, monte carlo in the first place, will probably soon replace all the other ways of estimating the self-absorption corrections. monte carlo algorithm generally is based on repeated random sampling. in the case of particle transport, the algorithm generates a particle and according to cross section database computes its whole path through the material until it leaves tracked volume or is fully absorbed. with a high number of repetition the final result of this simulation approximates very well the real situation. as the title of this article suggests, in this paper the last item will be further discussed. monte carlo method was previously applied to solve the problem of self-absorption successfully. one of the first works on this topic was [3]. many other articles folowed [4–6], etc. testing different geometries and different monte carlo codes. the following text will describe how this verified method was implemented at our department. 2. experimental equipment many different samples are measured in our laboratory, the most common are: environmental samples (possible contamination monitoring), building materials (radiation protection), soil and rock (geological studies). our equipment includes two hpge detectors designed and produced by canberra company. both of them are classical coaxial germanium detectors with a useful energy range 50 kev to 10 mev. the set up in our laboratory however is suitable for measurement in reduced energy range 50 kev to 3 mev since the laboratory usually works only with natural radioactivity or 137cs contamination. the main part of the detector is ge crystal with ntype and p-type contacts on its surfaces. application of certain potential to the contacts will cause the charge carriers (electrons and holes) move towards the electrodes. due to the very high purity of the ge crystal, only moderate bias is sufficient to “empty” the whole volume between the electrodes, creating so called depleted volume. this region becomes than an active area, where charge carriers, created by photon interactions, are swept by electric field and collected by electrodes. the pre-amplifier, which is incorporated in the cryostat, converts collected charges into voltage pulses. the height of this impulse is proportional to the energy deposited in the volume of the detector by photon interaction. one of the advantages of hpge compared to lithium-drifted detectors (second most common type of semiconductor detector) is that they do not need to be cooled at all time. the detector is stored without cooling, however during the measurement it is cooled in order to prevent thermally generated leakage current. in our laboratory the liquid nitrogen cooling system is used. the contact of ge crystal with the nitrogen (stored in dewar flask) is provided by so called cooling finger made of cu and cover with vacuum. the whole cooling system is called cryostat. the measurement itself can be realized in several geometries of the sample. our laboratory can provide a certified measurement in two geometries. first of them is so called marinelli beaker with a volume 600 ml. this geometry will be denoted as m600 in this article and it is commonly used geometry. the shape of this special container provides very good efficiency of measurement since it surrounds almost whole detector, see figure 1. the samples with volume smaller than 600 ml can be measured using less efficient geometry: a small container (volume 280 ml), which will be denoted as m280 in the rest of this paper. the smaller container can be seen as well in the figure 1. the calibrations of our gamma spectrometry systems are made using certified standards of activity produced by eurostandard cz (czech metrology institute). those standards are the same containers (both m600 and m280) filled with silicon rubber with dispersed known activity of known radionuclide. the spectra are acquired and processed by genietm 2000 analysis software, which is also a product of canberra. 3. monte carlo simulations the monte carlo simulation were implemented using mcnp code. mcnp (monte carlo n-particle) is a general-purpose code developed by los alamos national laboratory. its wide area of application includes radiation protection and dosimetry, shielding against radiation, nuclear criticality safety, detection technique, etc. in discussed problem an mcnp6, the latest release, was used. all geometry plots presented in this article were made using vised – a visual editor for mcnp [2]. 3.1. model of the detector the primer of mc (monte carlo) simulations was model of the detector itself. a rough model was created first using the data provided by the producer of the detector (canberra) in the technical documentation. for more details an x-ray scan of the detector was made. unfortunately some details like thickness of the dead layer or very thin layers generally could not be recognized from the x-ray picture very well. since the model did not still correspond to the reality (calculated and measured efficiencies differed with more than 10 % of relative error), the geometry had to be adapted experimentally. based on the previous experiences the thickness of the dead layer was alternated as was the volume of the vacuum 28 vol. 4/2016 self-absorption corrections based on monte carlo simulations figure 1. 3d visualization of detector model. yellow inner part is the crystal, the top green part represents the m600 (right) and m280 (left) container, blue part is the cooling finger. filled cell. after every change a new set of simulations was made and the results were compared to the measured efficiencies. the agreement of simulated and measured data was checked for m600 and m280 geometry in order to provide the most accurate model of the real detector. the final geometry can be seen in figure 1. 3.2. source and tally the source of radiation in the model was previously described marinelli beaker filled with different materials. both geometries: m600 and m280 were simulated. 3d visualization of the detector with m600 and m280 containers is in figure 2. the simulated photons were generated homogeneously in the whole volume of the container’s filling as it is shown in figure 2. the materials used as a filling of the containers were chosen in order to represent the whole spectrum of samples which are processed in our laboratory. selected materials are: silicon rubber (standards), water, blueberry, wood, soil, rock and brick. the energies of simulated photons were set based on the commonly analysed radionuclides, which are 238u and 232th decay chains, 40k and 137cs. the concentrations of these radionuclides, mainly 238u and 232th, are determined using large number of energy lines originating from different daughter products. all the necessary energy lines were simulated and are part of our database. for the needs of this paper only seven energies were chosen in order to demonstrate the behaviour of correction factor as a function of density and composition. the list of simulated energies is in table 1. in the case of need any other photon energy can be simulated. figure 2. the photons (blue dots) being emitted in the filling of m600 marinelli beaker. choosing tally (i.e. “what should be calculated”) was a simple task, since the objective was to compare simulated data with measured photopeak efficiencies. the best choice for this purpose is f8 type tally, which scores the number of impulses in certain geometry cell. f8 tally (as the other tallies) can be further specified by defining so called energy bins. energy bins provide an information about energy range in which the impulses should be counted. in this case the bin was set so it fully covers the full absorption peak. 29 kamila johnová acta polytechnica ctu proceedings energy [kev] radionuclide decay serie 186.21 226ra 238u 351.92 214pb 238u 661.66 137cs 137cs 727.17 212bi 232th 1460.81 40k 40k 1764.49 214bi 238u 2614.53 208tl 232th table 1. the example photon energies simulated for the needs of this paper. 3.3. data evaluation our approach to the problem allows two different ways of presenting the data. since the previous steps included creating a model of a real detector, complete efficiency curve can be calculated directly for each specific sample. the measured spectra would then be evaluated using this curve. this method is useful for very specific samples or samples that require high precision of measurement. for routine measurements the following way is preferred. the spectra are evaluated using one all-purpose calibration curve estimated by measurement of silicon rubber standards, which were described in the previous text. this process results in the activity a defined for fixed energy e by a = n t · y · ηstandard , where n is number of impulses in the full absorption peak, t is time of measurement, y is the yield of the energy line and ηstandard represents the photo-peak efficiency of the detector for silicon rubber standard. our objective is to estimate correction factor c = c(e, ρ, composition) so the activity of radionuclide in the sample asample can be calculated as asample = a · c = n t · y · ηsample , while ηsample means efficiency of the detector for sample. naturally ηsample = ηsample(e, ρ, composition). it is self-evident that at this point the required correction factor c equals c = ηstandard ηsample . (1) it was previously mentioned, that for fixed geometry the factor c is a function of energy e, density of sample ρ and composition of the material. the importance of those three variables can be forecast using cross section plot. it is one of mcnp option, which allows the user to plot the cross sections for any material and type of particle used in the model. the total cross sections (all interactions included) σt are plotted in figure 3 for all materials discussed in this paper. the detection system in our laboratory can detect photons within the energy range: 50–3000 kev, however energy lines below 100 kev are rarely processed. according to this fact and the information provided in figure 3, it can be assumed that considering the material composition there are only two groups of samples. first group contains “biological materials” or “biomass”, and is represented by wood, blueberries, water and silicon rubber. these materials consists of light elements only (h, o, c) and usually contains a significant amount of water. in can be expected that in the region 100–3000 kev, those samples will not need correction for composition, however the correction for density is still necessary. in another words only one correction curve (the correction factor as a function of density) will be sufficient for all the samples belonging into this group. the other group with similar cross sections contains again natural material but with a certain content of heavier elements (al, si, ca, fe, etc.). in this model this group is represented by brick, soil and rock. again in the region 100–3000 kev only one correction curve will be sufficient for all of these samples. only for lower energies and accurate measurements every material would need a special corrections. 4. results and discussion since this work uses the model of a real detector, it is appropriate at first comment on the comparison of simulated response of the detector with the measured one. it was already mentioned that the model of the detector had been experimentally modified in order to agree to the reality. the comparison of measured and simulated efficiency curves is in figure 4. this plot, made for m600 geometry, indicates a good agreement of measured and simulated data. taking into account the uncertainty of measured data caused mainly by errors in fitting and processing the spectra the model represent very well the real detector. the 5 % uncertainty of measured data is plotted in figure 4 by error bars. similar agreement of measured and simulated data was achieved for m280 geometry. as it was mentioned before the correction factor (1) is a function of composition, material density and energy. in section 3.3 some presumptions about the relation of c with those three parameters were made. in this part these assumptions, based on cross section data, will be confirmed using calculated results. at first the influence of composition of material will be discussed. the cross section plot in figure 3 denoted that the corrections for “biomass” materials as blueberry, wood or any other sample containing mainly h, o and c will be practically the same. the same statement should be valid for group of samples of natural origin containing heavier elements like (al, si, ca, fe, etc.). this group is represented by soil, rock and brick. figure 5 confirms those hypotheses. the correction factors within these two groups were practically the same, with less than 2 % difference. 30 vol. 4/2016 self-absorption corrections based on monte carlo simulations figure 3. the example of cross sections for materials used in the model. figure 4. comparison of measured and simulated efficiency (m600) curve for simulated detector. as a result of this, there are only two curves in this plot, each of them representing one of the groups mentioned above. it is also evident that the differences between the two correction curves are not so significant and for the most of the samples with relatively high uncertainty of measurement (around 10 %) one “mean” correction curve is more than sufficient. the cross section data in the figure 3 also suggested that the photon energy will be affecting the correction factors. the probability of photon interaction (total cross section) was dramatically dropping for low energies (10–70 kev) and continued decreasing slowly for the rest of energy region. this behaviour of cross section for all materials is reflected in figure 6, which plots the correction factor as a function of photon energy. while for the soil-rock types of samples the figure 5. correction factor for m600 as a function of density. composition influence. c is decreasing with energy, for the “biomass” group it is slightly increasing. the dependence of correction factor is logarithmic denoting that for higher energies (above 1500 kev) one correction curve (correction factor as a function of density) will be sufficient. the last parameter which will be commented in this article is a material density. as it was already shown in figure 5 this function is linear. figure 7 presents all correction factors for energies (radionuclides) listed in table 1. these corrections were calculated for m600 filled with brick. however as it was expected based on cross section plot and also proven in the results discussion above, the same curve can be used for soil and rock samples as well. in most of the cases the same corrections can be applied to other samples (wood, water solutions, etc.). 31 kamila johnová acta polytechnica ctu proceedings figure 6. correction factor for m600 as a function of photon energy. figure 7. correction factor for m600 geometry filled with brick. all the previous plots were based on the data calculated for m600 geometry. figure 8 shows the correction factors for smaller m280 geometry as s function of density. even though the behaviour of c = c(ρ) is the same (linear), the corrections itself are higher compared to the m600 geometry. 5. conclusions this article presents a way how the self-absorption problem is dealt with in our gamma spectrometry laboratory. the resulting correction factors c, defined by equation (1), were presented in figure 7, where c was plotted as a function of material density. presented simulations also proved that unless the high precision of measurement is required, the correction factor is independent of material composition. figure 8. correction factor for m280 geometry filled with brick. all the simulations were made using very accurate model of hpge detector. the comparison of measured and simulated efficiencies was plotted in figure 4. this model can be used further more for example for calculations of efficiency for non-standard geometry (geometry which is not calibrated using real certified standard of activity). references [1] g. gilmore. practical gamma-ray spectrometry. 2nd revised edition edition. wiley-blackwell, 2008. [2] r.a. schwarz, et al. graphical user input interface for mcnp. trans. am. nucl. soc. 69:401, 1993. [3] t. nakamura, t. suzuki. monte carlo calculation of peak efficiencies of ge(li) and pure ge detectors to voluminal sources and comparison with environmental radioactivity measurement. nucl. inst. and meth. in phys. res. 205(1):211–218, 1983. doi:10.1016/0167-5087(83)90191-6. [4] o. sima. monte carlo simulation versus semiempirical calculation of autoabsorption factors for semiconductor detector calibration in complex geometries. progress in nuclear energy 24:327–336, 1990. [5] f. sanchez, et. al. a monte carlo based method of including gamma slf-attenuation for the analysis of environmental samples. nuc. ins. and met. in phys. res. 61(4):535–540, 1991. doi:10.1016/0168-583x(91)95334-a. [6] r.m.w. overwater, et al. gamma-ray spectroscopy of voluminous sources corrections for source geometry and self-absorption. nuc. inst. and met. in phys. res. 324(1):209–218, 1993. doi:10.1016/0168-9002(93)90978-q. 32 http://dx.doi.org/10.1016/0167-5087(83)90191-6 http://dx.doi.org/10.1016/0168-583x(91)95334-a http://dx.doi.org/10.1016/0168-9002(93)90978-q acta polytechnica ctu proceedings 4:27–32, 2016 1 introduction 1.1 interactions of gamma radiation with matter 1.2 self-absorption coefficient 2 experimental equipment 3 monte carlo simulations 3.1 model of the detector 3.2 source and tally 3.3 data evaluation 4 results and discussion 5 conclusions references acta polytechnica ctu proceedings doi:10.14311/app.2017.9.0032 acta polytechnica ctu proceedings 9:32–38, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app real structure and residual stresses in advanced welds determined by x-ray and neutron diffraction karel trojana,∗, charles hervochesb, kamil kolaříka, nikolaj ganeva, pavol mikulab, jiří čapeka a ctu in prague, department of solid state engineering, faculty of nuclear sciences and physical engineering, trojanova 13, 120 00 prague 2, czech republic b nuclear physics institute, ascr, v.v.i., department of neutron physics, 25068 řež, czech republic ∗ corresponding author: karel.trojan@fjfi.cvut.cz abstract. the paper outlines the capability of x-ray diffraction (xrd) for evaluation of real structure changes and residual stresses (rs) on cross-section of advanced thick welds due to the welding of ferromagnetic plates. the results of neutron diffraction describe a three-dimensional state of rs and also verify previous assumptions of rs redistribution as a result of the surface preparation for determination 2d maps measured by xrd. keywords: laser and mag welding, residual stresses, x-ray diffraction, neutron diffraction. 1. introduction high local residual stresses existing in components could have vital influence on its properties. when a welded part with high local rs is machined the significant distortion may occur, due to the disruption of the equilibrium state of rs. on the other hand high tensile rs due to welding have a strong negative effect on the strength properties, especially under fatigue loading. therefore, the determination of the rs distribution in complex welded components is accentuated. recent practical approaches distinguish between local and global welding rs [1]. the local rs are resulting from the local heating and cooling processes in the weld metal and adjacent heat affected zone (haz). global rs exist in the entire component and they are resulting from shrinkage processes which occur in the whole component [1]. these global rs are affected by the stiffness of the component and the local shrinkage processes in the direction of black arrows in fig. 1. tensile rs around a single pass weld in a plane sample are expected due to the restraint which is generated by the cool adjacent zones in the base material of the plate [1]. therefore, the main direction of tensile rs due to shrinkage is applied along the weld. in the perpendicular direction, the tensile rs should reach lower values according to this model. for a complete description of the austenite phase, the transformation associated with a change in volume must be taken into consideration as a significant source of rs especially in high strength steels. the local compressive rs, which arise in the weld zone as a consequence of the restrained volume expansion during the transformation of austenite in martensite, bainite or ferrite, are superimposed to the global tensile rs figure 1. shrinkage tendency and constraint conditions in a single pass weld (schematically) [1]. explained according to the model described above (fig. 1) [1]. the increase in the cooling rate of the welded plates will lead to quenching and formation of local compressive rs. laser welding supplies into the weld lower heat input so that cooling of the weld is faster compared to the mag technology. the resulting distribution of residual stresses is a combined effect of hindered shrinkage and phase transformations. developed laser welding methods using high power diode lasers (hpdl) took over the capability to fill groove with cold or hot wire metal from metal active gas (mag) welding and thus to change mechanical properties of welds reducing their hardness due to the quenching [2]. profitable changes of real crystallographic structure and rs in comparison with conventional laser welds improve the results during impact and tensile test and mainly enhance fatigue life as a result of a favourable distribution of rs and its relaxation during welding in the weld zone and haz [3]. 32 http://dx.doi.org/10.14311/app.2017.9.0032 http://ojs.cvut.cz/ojs/index.php/app vol. 9/2017 real structure and residual stresses in advanced welds to verify the results obtained by xrd, where the samples were cut in two pieces, it is preferable to use the neutron diffraction. it has distinguished benefits such as the unique deep-penetration, threedimensional mapping capability, and volume-averaged bulk measurements characteristic of the scattering neutron beam for steel sample thickness up to 50 mm without cutting [4]. 2. experimental methods the analysed samples were prepared by a hpdl laser with cold wire and mag welding (metal active gas (mag) welding subtype of gas metal arc welding) from two 20 mm thick sheets made of s355j2 steel. the xrd measurements were performed by proto ixrd combo diffractometer with ω-goniometer and {211} diffraction line of α-fe was measured by crkα radiation. deformation of interplanar distances of variously rotated planes was converted to rs using the generalized hooke’s law according to the sin2ψ method. the corresponding neutron measurements were carried out on the diffractometer spn-100 of the nuclear physics institute which is installed at the channel hc-4 of the research reactor lvr-15 and operates at the neutron wavelength of 0.235 nm. the steca software [5] was used to extract and analyse diffraction patterns from the recorded area detector data. the diffraction peak {110} of α-fe was measured. the strain was calculated using the hooke’s law based on the angular deviation of the diffraction profile position from the value related to the stress-free sample. full widths of the measured diffraction lines at half of the maximum (fwhm ) were also evaluated for both methods. fwhm parameter depends on microstrains, crystallite size, density of dislocations and weight proportion of the hard phases. sample orientations during xrd and neutron diffraction are shown in figs. 2a and 2b. the direction of the arrows always indicates the direction of the measured rs. the rotation of measured planes during sin2ψ measurements is also shown in fig. 2a for xrd. equivalent direction are therefore l’ for xrd and t for neutron diffracton. the measurements were performed in three lines perpendicular to the welds. one line passes through the centre of the weld and the other two are located three millimetres below each surface, see red lines in fig. 2c. upper side of the plate is the site which was firstly welded. to determine the real structure and rs by xrd on the cross section, it was necessary to cut the plate in two parts (solid lines and dashed lines in fig. 2c) and the affected surface layer electrochemically etched. 3. experiment gradients of rs measured by xrd in two directions on the surface of welded plates with a depth of penetration of the used radiation into the sample approx. (a) . sample orientations during xrd. (b) . sample orientations during neutron diffraction. (c) . measured lines during neutron diffraction. figure 2. sample orientations during experimental methods. 4 µm are plotted in fig. 3. dependences of threedimensional state of rs determined by neutron diffraction technique related to the middle line and two lines with depth of three millimetres below both surfaces of laser and mag samples can be seen in figs. 4 and 5. the comparison of rs obtained by xrd in direction l’ and neutron diffraction in direction t is plotted in figs. 6 and 7. the comparison of fwhm obtained 33 k. trojan, ch. hervoches, k. kolařík et al. acta polytechnica ctu proceedings figure 3. surface residual stresses measured by xrd. by xrd in direction l’ and neutron diffraction in direction t is shown in figs. 8 and 9. the parameter x is the perpendicular distance from the axis of the weld in all graphs. the most significant tensile rs on the surface are in the direction s according to the predictions (see fig. 1 and 3) for both samples. tensile rs of the laser weld in the direction s exceed the yield strength of the used steel and for upper side even the tensile strength. this would suggest that the rapid cooling of laser weld created non-equilibrium hard phases with higher strength [6]. in l direction differently wide haz could be well observed. according to figs. 4 and 5 tensile rs within all the three measured lines obtained by neutron diffraction have the maximum in the longitudinal direction for both samples. rs in the laser weld at middle line exceeding 300 mpa and for mag in bottom line only 230 mpa. in the middle of the laser and mag weld, the distribution of rs in both remaining directions n and t is the same. shrinkage and other effects caused that rs were created in both directions homogeneously. in the middle of the laser weld according to figs. 6 and 7, rs obtained by neutron diffraction in the perpendicular direction to the weld reported more tension character than by xrd. this is most probably due to a significant contraction in the direction parallel to the weld. on the other hand in the case of the mag weld, there are compressive stresses. this could suggest a predominance of phase transformation during the formation of rs rather than shrinkage. for both welds, rs obtained by xrd reported higher compressive results than obtained by neutron diffraction. the only exception is the upper line for the mag weld, see fig 7. laser weld (according to the fig. 4) has a higher tensile residual stresses along the weld, therefore, redistribution after cutting the sample probably produced the greatest compressive stresses measured by xrd. after cutting the plate, the weld probably slightly dropped, and thus it caused compressive rs in the plane perpendicular to the weld. the comparison of the parameter fwhm using both methods exhibits in nearly all cases the same pattern, see figs. 8 and 9. change in the parameter fwhm for mag sample, which can be correlated with a width of haz, is recorded at a greater distance than for the laser weld. fwhm is in all cases for both methods higher for the laser sample, this would indicate a higher microstrain, density of dislocations and a greater amount of hard phases. 4. conclusions it was found from the residual stresses measured by neutron diffraction in three different sample orientations and in three different depths under the surface that the greatest gradient of residual stresses is in the direction parallel to the weld. according to the literature study and our results, greater tensile residual stresses exhibits the laser weld in almost all measured lines. furthermore, the results describing haz width (changes in values of rs and fwhm ) are very similar for both analytical methods (xrd and neutron diffraction). both diffraction methods are able to complement each other. furthermore, the resulting residual stresses gradients obtained using both methods with a different approach are in certain correlation. each method (xrd and neutron diffraction) describes the outcome of residual stresses in different context. the redistribution of rs during the cutting has not yet been accurately described, so further measurements and verification using mathematical modelling will be needed. we are currently performing the validation of measurement on the second mag sheet. acknowledgements measurements were carried out at the canam infrastructure of the npi ascr řež supported through mšmt project no. lm2011019 and czech science foundation gačr through the project no. 14-36566g entitled as multidisciplinary research centre for advanced materials. this work was supported by the student grant competition ctu in prague grant no. sgs16/245/ohk4/3t/14. the authors thank to matex pm for supplying the laser weld. 34 vol. 9/2017 real structure and residual stresses in advanced welds (a) . laser — upper line. (b) . laser — middle line. (c) . laser — bottom line. figure 4. rs for laser sample along three measured lines obtained by neutron diffraction. (a) . mag — upper line. (b) . mag — middle line. (c) . mag — bottom line. figure 5. rs for mag sample along three measured lines obtained by neutron diffraction. 35 k. trojan, ch. hervoches, k. kolařík et al. acta polytechnica ctu proceedings (a) . laser — upper line. (b) . laser — middle line. (c) . laser — bottom line. figure 6. comparison of rs obtained by xrd in direction l’ and neutron diffraction in direction t along three measured lines for laser sample. (a) . mag — upper line. (b) . mag — middle line. (c) . mag — bottom line. figure 7. comparison of rs obtained by xrd in direction l’ and neutron diffraction in direction t along three measured lines for mag sample. 36 vol. 9/2017 real structure and residual stresses in advanced welds (a) . laser — upper line. (b) . laser — middle line. (c) . laser — bottom line. figure 8. comparison of fwhm obtained by xrd in direction l’ and neutron diffraction in direction t along three measured lines for laser sample. (a) . mag — upper line. (b) . mag — middle line. (c) . mag — bottom line. figure 9. comparison of fwhm obtained by xrd in direction l’ and neutron diffraction in direction t along three measured lines for mag sample. 37 k. trojan, ch. hervoches, k. kolařík et al. acta polytechnica ctu proceedings references [1] t. nitschke-pagel, k. digler. sources and consequences of residual stresses due to welding. mater sci forum pp. 2777–2785, 2014. doi:10.4028/www.scientific.net/msf.783-786.2777. [2] m. sokolov, a. salminen, m. kuznetsov. laser welding and weld hardness analysis of thick section s355 structural steel. mater design 32(10):5127–5131, 2011. doi:10.1016/j.matdes.2011.05.053. [3] c. lachmann, t. h. nitschke-pagel, h. wohlfahrt. nondestructive characterization of residual stress relaxation and fatigue processes in cyclically loaded welded joints. pp. 1400–1409. oxford, uk, 2000. [4] w. woo, et al. neutron diffraction measurements of residual stresses in a 50 mm thick weld. mater sci eng a 528(12):4120–4124, 2011. doi:10.1016/j.msea.2011.02.009. [5] c. randau, u. garbe, h. g. brokmeier. stresstexturecalculator: a software tool to extract texture, strain and microstructure information from area-detector measurements. j appl cryst 44(3):641–646, 2011. doi:10.1107/s0021889811012064. [6] n. jia, et al. an in situ high-energy x-ray diffraction study of micromechanical behavior of multiple phases in advanced high-strength steels. acta mater 57(13):3965– 3977, 2009. doi:10.1016/j.actamat.2009.05.002. 38 http://dx.doi.org/10.4028/www.scientific.net/msf.783-786.2777 http://dx.doi.org/10.1016/j.matdes.2011.05.053 http://dx.doi.org/10.1016/j.msea.2011.02.009 http://dx.doi.org/10.1107/s0021889811012064 http://dx.doi.org/10.1016/j.actamat.2009.05.002 acta polytechnica ctu proceedings 9:32–38, 2017 1 introduction 2 experimental methods 3 experiment 4 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.9.0013 acta polytechnica ctu proceedings 9:13–18, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app influence of machining technologies on values of residual stresses of oxide cutting ceramics jakub němeček∗, kamil kolařík, jiří čapek, nikolaj ganev department of solid state engineering, faculty of nuclear science and physical engineering, czech technical university in prague ∗ corresponding author: j.nemecek91@gmail.com abstract. currently, the intensive development of engineering ceramic and effort to replace sintered carbides as cutting materials are in progress. with the development of the sintering technology it is now possible to produce compact ceramic cutting samples with very good mechanical properties. the advantage of these materials is their easy accessibility and low purchase price. in this work, the influence of the finishing machine technology on the values of surface residual stresses of cutting ceramic samples al2o3+tic were studying. the samples were supplied by moscow state university of technology stankin. measurements made in the x-ray diffraction laboratory at the department of solid state engineering were performed for both the phases. the influence of the parameters of machining to residual stresses was studied and the resulting values were compared with each other. keywords: cutting ceramic; machining technology; x-ray diffraction; residual stresses. 1. introduction ceramic tools have been used since the stone age, when sandstone containing large amounts of silica blades was used, for example for the sharpening of knives, razor blades or other tools. this material was used henceforward as abrasive wheels during the ages of cutting weapons for sharpening of swords, knives and other blades. only recently these grinding tools have been replaced by other modern materials for example by sic or diamond. at the beginning of the 20th century, the first use of al2o3 ceramics as a cutting tool occurred. over the years, its development had moved to a level at which we were able to replace, for example, sintered carbides using those ceramic materials. this effort has been caused by the mechanical properties of aluminium oxide and the easy availability of the starting materials [1, 2]. the aim of this paper is to study the real structure of al2o3+tic oxide cutting ceramic. the microstrains and a size of crystallites was measured and influence of machining technologies on the macroscopic residual stresses was studied. 1.1. preparation of samples the starting materials and their properties have been known for a long time. the problem was how to make compact samples with the desired mechanical properties and dimensions. the current production process consists of three parts: first, grinding the starting material to a powder with grain size of the order of 100 nm, second, sintering the powders into a compact form and third, the surface treatment of the samples to the desired dimensions. an important technological aspect of the properties of cutting ceramics is the grain size of the starting powders. if the individual grain size is approximately the same (if they have ideal spherical shape), the uniform distribution and the pore size are gained more easily during forming and thereby for uniform compaction throughout the volume and easier reorganization of the particles during sintering. preference is also to achieve the smallest grain size of the sample, because it leads to faster material transport [3]. the sintering process is very similar to that used for sintered carbides. the powder is pressed below the melting point into a compact body, see figure 1. but the main difference is the absence of a binder which during sintering formed a liquid phase, because it would cause degradation of mechanical properties. today, ceramic is most commonly sintered into rods of cross section of finite samples and then cut to the desired dimensions. individual plates are then variously surface treated and shaped [4]. 2. x-ray diffraction analysis of macroscopic residual stresses in cooperation with the moscow state technological university stankin that provides manufacturing technology, the influence of machining technologies on the value of residual stresses in samples of al2o3+tic oxide cutting ceramics were investigated in x-ray diffraction laboratory of the department of solid state engineering of fnspe ctu in prague. all experimental errors were around 10 % of absolute value of measurement. 2.1. grinding by diamond disc after sintering, all samples were ground using a diamond wheel. an effect of displacement of the workpiece on the lift at constant cutting speed, feed rate 13 http://dx.doi.org/10.14311/app.2017.9.0013 http://ojs.cvut.cz/ojs/index.php/app j. nemecek, k. kolarik, j. capek, n. ganev acta polytechnica ctu proceedings figure 1. scheme of creation technology of cutting ceramic sample: refinement powders (wet grinding), evaporation, pressing, sintering [5]. sample fd, displacement on the lift [mm/displ.] ap, depth of cut [mm] 1 0.5 0.04 2 1.0 0.04 3 1.5 0.04 table 1. parameters of grinding by diamond disc. figure 2. scheme of grinding by diamond disc [5]. of the workpiece in the cutting direction and depth of cut was observed. grinding parameters are given in table 1, where cutting speed vc = 30 m/s and feed rate f = 12 m/min. values of residual stresses were determined in two orthogonal directions l (direction of the grinding wheel) and t (direction of displacement on the lift). because of unidirectional grinding anisotropy of values was observed in both directions. different values are due to the different structure of al2o3 (trigonal) and tic (cubic) and the different number of slip planes (see table 2). 2.2. thermal annealing of the samples after grinding by diamond disc next samples were ground by diamond disc with the same machining parameters and then thermally anfigure 3. structure of al2o3 (up) and tic (down). nealed at 800 ◦c. it is evident from table 3 that the values of the macroscopic residual stresses decreased considerably. in contrast, the value of microstrains and grain size given by the parameter fwhm remained almost unchanged. 2.3. air abrasive machining in this method of machining, air of high pressure with added cutting microparticles is jetted on a rotating sample. the effect of air pressure changes on the residual stress in the sample was studied (table 4) with constant time of blasting t = 60 s and rotates per minute rpm = 50. the obtained values (table 5) show that when a pressure increases from 2 to 2.5 bars a decrease of compressive residual stresses (stress relaxation) is ob14 vol. 9/2017 influence of machining technologies on values of residual stresses al2o3 tic l direction rs mnkα (0210) l direction rs crkα (311) sample σn [mpa] σs [mpa] fwhm [2θ] sample σn [mpa] σs [mpa] fwhm [2θ] 1 -216 33 0.787 1 -518 77 0.759 2 -182 39 0.693 2 -536 77 0.741 3 -165 37 0.859 3 -530 74 0.708 t direction rs mnkα (0210) t direction rs crkα (311) sample σn [mpa] σs [mpa] fwhm [2θ] sample σn [mpa] σs [mpa] fwhm [2θ] 1 -436 36 0.804 1 -776 67 0.668 2 -470 30 0.709 2 -805 93 0.759 3 -580 37 0.772 3 -938 89 0.679 table 2. the values of normal (σn ) and shear (σs) residual stresses after grinding by a diamond disc. al2o3 tic l direction rs mnkα (0210) l direction rs crkα (311) sample σn [mpa] σs [mpa] fwhm [2θ] sample σn [mpa] σs [mpa] fwhm [2θ] 12 -185 19 0.666 12 -516 91 0.965 13 -203 16 0.888 13 -290 40 0.609 14 -199 30 0.889 14 -289 112 0.847 t direction rs mnkα (0210) t direction rs crkα (311) sample σn [mpa] σs [mpa] fwhm [2θ] sample σn [mpa] σs [mpa] fwhm [2θ] 12 -303 20 0.781 12 -599 71 0.782 13 -359 6 0.802 13 -474 57 0.613 14 -342 27 0.769 14 -473 104 0.908 table 3. the values of normal (σn ) and shear (σs) residual stresses after thermal annealing. sample p, air pressure [mpa] 4 1.5 5 2.0 6 2.5 table 4. parameters of air abrasive machining. figure 4. scheme of air abrasive machining and a picture of machining chamber [5]. served. it is probably a result of overcoming the yield strength of the material. perhaps machining process with higher pressure values influences deeper sub-surface layers of material. the energy required for crack propagation is therefore higher for these seemingly lower pressure residual stresses. to confirm this assertion, a depth-profile analysis of residual stresses by sequential force-free etching of surface layers is needed. rotational movement of the specimen during the machining leads to an isotropic stress distribution i.e., the values in both the directions l and t are similar. 2.4. water jet machining water jet machining (wjm) is based on the same principle as air abrasive machining, when a focused beams of water is jetted out by varying the pressure on the rotating sample (see figure 6 and table 6). other parameters: time of blasting t = 60 s, distance of samples l = 2 mm, number of nozzles n = 50. it is evident, that for applied values of pressure jetting the yield strength value have not been overcome. the values of residual compressive residual stresses increase steadily with increasing pressure in contrast to the samples after air abrasive machining. due to the rotating of the samples an isotropic residual stress distribution is achieved again (see table 7). 15 j. nemecek, k. kolarik, j. capek, n. ganev acta polytechnica ctu proceedings al2o3 tic l direction rs mnkα (0210) l direction rs crkα (311) sample σn [mpa] σs [mpa] fwhm [2θ] sample σn [mpa] σs [mpa] fwhm [2θ] 4 -352 34 0.787 4 -799 117 0.965 5 -367 45 0.694 5 -928 111 0.609 6 -242 32 0.827 6 -278 83 0.847 t direction rs mnkα (0210) t direction rs crkα (311) sample σn [mpa] σs [mpa] fwhm [2θ] sample σn [mpa] σs [mpa] fwhm [2θ] 4 -295 42 0.781 4 -737 119 0.641 5 -389 44 0.802 5 -899 123 0.890 6 -284 36 0.769 6 -283 69 0.611 table 5. the values of normal (σn ) and shear (σs) residual stresses after air abrasive machining. sample p, pressure [mpa] 7 1.5 8 2.0 9 2.5 table 6. parameters of water jet machining. figure 5. scheme of water jet machining. 2.5. laser shock peening during machining by laser the samples are heated and it results in stress relaxation. increased power (see table 9) will lead to higher temperatures, and thus to higher stress relaxation. furthermore, it is possible to observe the influence of the laying of individual spots (overlapping) on the anisotropy of distribution of residual stresses. 2.6. stress tests — the effect of friction after grinding of samples by diamond disc their surface was loaded by rotating steel disk at different time intervals. the influence of time of friction on values of residual stresses was investigated (see table 10). figure 6. scheme of linear and surface laying of spots for laser shock peening [5]. 3. microstrains and crystallite size simultaneously with the measurement of the macroscopic residual stresses, determination of crystallite size and microstrains was provided using the rietveld analysis. all results are demonstrated in [6]. from the measured values is evident that crystallite size after thermal annealing and after laser machining increased, which is probably due to recrystallization during these treatments. a decrease of microstrains is observed after air abrasive machining when the yield point was overcome and the grain sizes increased. after stress tests by steel disc the largest crystallite size al2o3 are observed, that could be again due to thermal relaxation and recrystallization of the surface. 4. conclusions values of residual stresses of cutting ceramics al2o3+tic were analysed in two perpendicular directions. the influence of machining technologies to residual stresses was studied in both the phases. anisotropy and different values for the two phases during grinding by diamond disc were obtained, and 16 vol. 9/2017 influence of machining technologies on values of residual stresses al2o3 tic l direction rs mnkα (0210) l direction rs crkα (311) sample σn [mpa] σs [mpa] fwhm [2θ] sample σn [mpa] σs [mpa] fwhm [2θ] 7 -99 38 0.712 7 -406 118 0.644 8 -149 42 0.733 8 -363 74 0.691 9 -255 47 0.732 9 -568 118 0.765 t direction rs mnkα (0210) t direction rs crkα (311) sample σn [mpa] σs [mpa] fwhm [2θ] sample σn [mpa] σs [mpa] fwhm [2θ] 7 -85 43 0.790 7 -374 116 0.644 8 -166 50 0.752 8 -364 88 0.689 9 -238 45 0.668 9 -484 108 0.669 table 7. the values of normal (σn ) and shear (σs) residual stresses after water jet machining. al2o3 tic l direction rs mnkα (0210) l direction rs crkα (311) sample σn [mpa] σs [mpa] fwhm [2θ] sample σn [mpa] σs [mpa] fwhm [2θ] 10.1 -53 31 0.731 10.1 -318 111 0.594 10.2 31 31 0.717 10.2 -259 96 0.657 10.3 -29 23 0.757 10.3 -200 106 0.637 10.4 -62 17 0.751 10.4 -220 95 0.568 t direction rs mnkα (0210) t direction rs crkα (311) sample σn [mpa] σs [mpa] fwhm [2θ] sample σn [mpa] σs [mpa] fwhm [2θ] 10.1 -155 9 0.856 10.1 -509 148 0.619 10.2 -125 9 0.868 10.2 -448 135 0.545 10.3 -71 42 0.737 10.3 -367 135 0.543 10.4 -48 39 0.704 10.4 -288 123 0.618 table 8. the values of normal (σn ) and shear (σs) residual stresses after laser shock peening. sample p, power [w] 10.1 2 10.2 5 10.3 10 10.4 15 table 9. parameters of laser shock peening. pulse frequency f = 30 khz, displacement sx = sy = 40 µm. the thermal relaxation of macroscopic residual stresses after thermal annealing was also measured. for air abrasive cutting overcoming of the yield stress was found out with increasing the pressure to 2.5 mpa. due to rotational movement during air abrasive machining and water jet machining the values of surface residual stresses are isotropic. samples machined by laser exhibit thermal relaxsample t, time of loading [s] 11.1 2 11.2 6 11.3 12 table 10. parameters of stress tests. ation of residual stresses. at the same time, the found anisotropy of state of residual stresses is due to overlapping of laser-processed areas. on the samples after the loading tests thermal relaxation of residual stresses was observed. it was shown that titancarbide is more sensitive to load than aluminium oxide. for more detailed information see [6]. acknowledgements this work was supported by grant student grant competition ctu no. sgs16/246/ohk4/3t/14 and grant agency of the czech republic (no. 14-36566g). 17 j. nemecek, k. kolarik, j. capek, n. ganev acta polytechnica ctu proceedings al2o3 tic l direction rs mnkα (0210) l direction rs crkα (311) sample σn [mpa] σs [mpa] fwhm [2θ] sample σn [mpa] σs [mpa] fwhm [2θ] 11.1 -42 27 0.693 11.1 -453 64 0.655 11.2 3 21 0.606 11.2 -129 76 0.530 11.3 -78 40 0.596 11.3 -242 49 0.577 t direction rs mnkα (0210) t direction rs crkα (311) sample σn [mpa] σs [mpa] fwhm [2θ] sample σn [mpa] σs [mpa] fwhm [2θ] 11.1 -145 17 0.612 11.1 -348 95 0.580 11.2 -15 19 0.610 11.2 -190 59 0.563 11.3 47 24 0.649 11.3 -240 66 0.446 table 11. the values of normal (σn ) and shear (σs) residual stresses after stress testing. references [1] r. kumar, et al. synthesis and characterization of al2o3+tic nano-composite by spark plasma sintering. international journal of refractory metals and hard materials 577:9–15, 2016. [2] z. yin, et al. friction and wear behaviors of al2o3+tic micro-nano-composite ceramic sliding against metals and hard materials. international journal of refractory metals and hard materials 577:9–15, 2016. [3] a. humár. materiály pro řezné nástroje. first printing. mm publishing, 2008. [4] c. b. carter, m. g. norton. ceramic materials: science and engineering. second edition. springer science and business media, 2013. [5] m. university stankin. materials for experimental measurement. [6] j. němeček. studium reálné struktury oxidových řezných keramik. 18 acta polytechnica ctu proceedings 9:13–18, 2017 1 introduction 1.1 preparation of samples 2 x-ray diffraction analysis of macroscopic residual stresses 2.1 grinding by diamond disc 2.2 thermal annealing of the samples after grinding by diamond disc 2.3 air abrasive machining 2.4 water jet machining 2.5 laser shock peening 2.6 stress tests — the effect of friction 3 microstrains and crystallite size 4 conclusions acknowledgements references 234 acta polytechnica ctu proceedings 2(1): 234–237, 2015 234 doi: 10.14311/app.2015.02.0234 the nova v5584 sgr: a short review r. poggiani 1 1department of physics, università di pisa corresponding author: rosa.poggiani@df.unipi.it abstract the nova v5584 sgr was discovered during 2009 october. it has been monitored in different domains of the electromagnetic spectrum: optical, infrared and x-rays. the optical and infrared observations suggest that v5584 sgr is a fe ii nova that formed dust. no x-ray emission was observed around the time of maximum. keywords: cataclysmic variables -novae optical spectroscopy individual: v5584 sgr. 1 introduction nova sagittarii no. 4 was discovered by nishiyama and kabashima (2009) on 2009 october 26 and later designated v5584 sgr (samus, 2009). v5584 sgr is a classical example of multi-wavelength astrophysics, since it has been observed in different parts of the electromagnetic spectrum: optical, infrared and x-rays. the very early optical spectroscopic observations secured by kinugasa et al. (2009), maehara et al. (2009), fujii (maehara et al., 2009), munari et al. (2009) in the optical and by raj et al. (2009) in the infrared showed that v5584 sg is a fe ii nova, in the context of the classification by williams et al. (1991), williams (1992). spectra secured by russell et al. (2010) during 2010 february showed that dust formation had occurred. poggiani (2011) has monitored v5584 sgr during the late decline. v5584 has been investigated in the optical domain by the stony brook/smarts consortium (walters et al., 2012). the present paper reviews the history of v5584 sgr observations. 2 light curve the photometric evolution and the main parameters of v5584 sgr has been reported by poggiani (2011) and will be briefly summarized below for completeness. the v band light curve is reported in fig. 1. the epoch of maximum is mjd=55134.208 (2009 october 29), while the decline time by two magnitudes is 27±2 days, making v5584 sgr a moderately fast nova, according to the classification by payne-gaposchkin (1957). the reddening of v5584 sgr is 0.82±0.12. the estimated distance of v5584 sgr is in the interval 5.8-7.1 kpc. the absolute magnitude at maximum is in the range -7.2....7.7, while the white dwarf mass is in the range 0.8-0.9 m�. all parameters extracted by the analysis of the light curve suggest that v5584 sgr is a fe ii nova, according to the classification by della valle & livio (1998). the spectroscopic observations described below will provide further evidence for the classification. 55100 55150 55200 55250 55300 55350 55400 55450 55500 time (mjd) 8 9 10 11 12 13 14 15 16 17 v m a g n it u d e figure 1: v band photometry of v5584 sgr 3 optical spectroscopy spectroscopic observations of v5584 sgr around maximum have been secured by different authors. kinugasa et al. (2009) observed hα and fe ii lines in emission with p cyg profiles on 2009 october 27. the presence of hα in emission was confirmed by maehara et al. (2009) on the same day. munari et al. (2009) observed a highly reddened absorption continuum on october 28, with hα and fe ii showing an emission component and the same continuum with faint emission from balmer ad fe ii multiplets on october 29. it was suggested that v5584 sgr was a fe ii nova caught around maximum, according to the classification by williams et al. (1991), williams (1992). v5584 sgr has also been observed at the higashi-hiroshima observatory with the 234 http://dx.doi.org/10.14311/app.2015.02.0234 the nova v5584 sgr: a short review kanata telescope (uemura, 2009) on october 31 and november 3, 5 1. the intensity of emission lines progressively strengthened, while the continuum decayed. v5584 sgr is part of the stony brook smarts spectral atlas of southern novae that includes data of more than sixty novae (walters et al., 2012). their observations of v5584 sgr on november 11 showed balmer lines, fe ii multiplets and o i. poggiani (2011) has observed v5584 sgr during the late decline (after the seasonal gap) at the loiano observatory, italy, using the 152 cm telescope and the bfosc imager and spectrograph. the observation of june 4 is reported in fig. 2. the spectrum has been secured using grism #4 that has a range 4000 to 8500 å and a resolution of 3.97 å/pixel, reduced with bias and flat frames, extracted using the optimal extraction method by horne (1986), calibrated in wavelength with an hear lamp and corrected with the instrumental response. the spectrum shows a prominent hα transition, intense forbidden lines of [o iii], [n ii] and the high ionization line [fe vii] 6087, typical of a nova in the nebular stage a0 (williams et al., 1991; williams 1992). the same pattern of lines has been observed by the smarts consortium on october 17. figure 2: optical spectrum of v5584 sgr during the nebular stage (poggiani, 2011) the line profiles are a signature of the ejecta distribution. optically thin winds and optically thin shells show rounded and rectangular line profiles, respectively. the profile of hα at two epochs (labelled with the number of days elapsed from maximum) is reported in fig. 3 (poggiani (2011)). the profiles show a red wing, probably explained by the emerging of [n ii] 6584. the rest wavelength is coincident with the 0 km/s label. the observations of v5584 sgr during the nebular stage are part of a monitoring program (poggiani, 2012) active since 2005 at the loiano observatory, italy, using the 152 cm telescope and the bfosc imager and spectrograph. the most part of the spectra are secured with grism #4 to build an homogeneous data set of spectra over the range 4000 to 8500 å. the monitoring aims to build a spectral atlas and includes most novae observable at the telescope latitude that underwent outburst after 2005. other sources are v1663 aql, v1722 aql, v2362 cyg, v2467 cyg, v2468 cyg, v2491 cyg, v407 cyg, kt eri, v959 mon, v2670 oph, v496 sct, v5558 sgr, v458 vul, v459 vul. the novae are observed at several epochs, from the early decline to the nebular stage and on the way to quiescence. figure 3: line profiles of hα during the nebular stage (poggiani, 2011) the importance of monitoring of novae over long time intervals has been addressed by several contributors at this conference (pagnotta, 2013), (ederoclite, 2013), (tappert, 2013). at the moment of writing v5584 sgr is very far from quiescence. at the moment of discovery, corelli (2009) showed that nothing was visible at the nova position on a palomar plate with limiting magnitude 21. 4 infrared observations the relevance of observations of novae in the infrared has been discussed by banerjee and ashok (2012) and by chesneau and banerjee (2012). banerjee and ashok (2012) suggest that the fe ii and he/n classes share a set of common spectral lines in the near infrared, namely hydrogen, helium, nitrogen and oxygen. on the other hand, there is a clear signature belonging only to novae of fe ii class, the presence of strong carbon lines: thus the near infrared observations can provide an additional suggestion of the spectroscopic class of a nova. several novae, mostly novae belonging to fe ii class, produce dust during the decline. the dust presence is marked by a rise of infrared emission and can become apparent also as a dip in the optical light curve. the last signature is not necessarily observed, since dust can be arranged as an optically thin shell. 1http://f.hatena.ne.jp/kanataobslog/20091106162703 235 r. poggiani infrared observations of v5584 sgr have been secured by raj et al. (2009) on october 29 at mt. abu telescope showed paschen, brackett, o i, c i, n i lines with p cyg profiles, whose components wew separated by about 550-650 km/s. the emission components strengthened, while the absorption components faded by november 3. the transitions observed in spectra are typical of the fe ii class novae, providing an independent confirmation of the classification of v5584 sgr. the following observations in the infrared were secured after the seasonal gap. on 2010 february 10 russell et al. (2010) observed v5584 sgr in the region 3-14 µm with aeos telescope, discovering that the nova had formed dust since the previous observations. the infrared continuum was dominated by the thermal emission of the dust at a temperature of 880±50 k; no details of the dust composition or the derivation of the temperature are reported. the above infrared observatons provide a clue that was not available due to the lack of observations during the seasonal gap. 5 x-ray observations the importance of x-ray observations of novae has been addressed by several authors, also at this conference (ness, 2013), (orio, 2013). v5584 sgr has been observed with the monitor of all-sky x-ray image (maxi) (shimanoe et al., 2010). the system is on board of iss and uses two high sensitivity x-ray detectors, the gas slit camera (32 ccd chips) and the solid state slit camera (a xenon filled proportional conunter). maxi scans all sky every 92 minutes. shimanoe et al. (2010) have searched the prompt x-ray emission at the ignition of the thermonuclear runaway. the authors suggested that classical novae could emit x-rays at the outburst in analogy to the type i x-ray bursts of x-ray binaries. the observations included several peculiar novae: v1723 aql, v407 cyg, v2673 and v2674 oph, v1722 aql, kt eri, v496 sct. the authors have focused on the archive data in the energy band 1.5-4 kev, the lowest energy available, assuming that nova outbursts preferentially emit soft x-rays. they also investigated the 4-10 kev and 10-20 kev bands. no prompt emission was detected in the three bands for any nova. there are no reported x-ray observations of v5584 sgr at later stages, when supersoft emission could have occurred. 6 conclusions v5584 sgr is a standard fe ii nova. the sinergy of observations in different domains allowed a classification of the spectral class and the discovery of dust production during the seasonal gap. acknowledgement the author thanks the organizers for the invitation to this very stimulating workshop. thanks to the tac committee of the loiano observatoy for the allotted time and to i. bruni for his precious assistance. the author is grateful to the anonymous referee for the careful comments. references [1] banerjee, d. p. k. and ashok, n. m.: 2012, basi 40, 243. [2] chesneau, o. and banerjee, d. p. k.: 2012, basi 40, 267. [3] corelli, p.: 2009, cbet 1994, 1. [4] della valle, m. & livio, m.: 1998, apj 506, 818. doi:10.1086/306275 [5] ederoclite, a.: these proceedings [6] horne, k.: 1986, pasp 98, 609. doi:10.1086/131801 [7] kinugasa, k. et al.: 2009, iauc 9089, 2. [8] maheara, h. et al.: 2009, iauc 9089, 3. [9] munari, u. et al.: 2009, cbet 1999, 1. [10] ness, j. u.: these proceedings [11] nishiyama, k. & kabashima, f.: 2009, iauc 9089, 1. [12] orio, m.: these proceedings [13] pagnotta, a.: these proceedings [14] payne-gaposchkin, c.: 1957, the galactic novae, north holland, amsterdam. [15] poggiani, r.: 2011, astrophy. space sci. 333, 115. doi:10.1007/s10509-011-0595-z [16] poggiani, r.: 2012, mem. sait 83, 753 [17] raj, a. et al., 2009: cbet 2002, 1. [18] russell, r. w. et al.: 2010, iauc 9118, 2. [19] samus, n. & kazarovets, e. v.: 2009, iauc 9089, 4. [20] shimanoe, j. et al.: 2010, the first year of maxi: monitoring variable x-ray sources, 4th international maxi workshop held november 30 december 2, tokyo, japan [21] tappert, k.: these proceedings 236 http://dx.doi.org/10.1086/306275 http://dx.doi.org/10.1086/131801 http://dx.doi.org/10.1007/s10509-011-0595-z the nova v5584 sgr: a short review [22] uemura, m. on behalf of the kanata team: 2009, asp conf. ser. 404, 69 [23] walters, f. m. et al.: 2012, pasp 124, 1057. doi:10.1086/668404 [24] williams, r. e. et al.: 1991, apj 376, 721. doi:10.1086/170319 [25] williams, r. e.: 1992, aj 104, 725. discussion martin henze: you described x-ray observations and mentioned soft band of 1.5-4 kev in which soft x-rays would be expected. i just wanted to comment that in this band we would not expect to see supersoft x-ray emission which normally does not go above 1 kev. rosa poggiani: the maxi astronomers stated that they were looking for soft x-ray emission in the above energy range. i agree that to detect the x-ray emission you are mentioning you should use another instrument jan-uwe ness: the maxi collaboration was looking for prompt emission. 237 http://dx.doi.org/10.1086/668404 http://dx.doi.org/10.1086/170319 introduction light curve optical spectroscopy infrared observations x-ray observations conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.13.0061 acta polytechnica ctu proceedings 13:61–65, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app the effect of plasticizer on mechanical properties of the cement paste with fine ground recycled concrete jaromír hrůza∗, zdeněk prošek czech technical university in prague, faculty of civil engineering, thákurova 7, 166 29 prague 6, czech republic ∗ corresponding author: jaromir.hruza@fsv.cvut.cz abstract. this article deals with the usage of recycled concrete, which arises from the demolition of concrete structures. the work is focused on the development of mechanical properties (young's modulus, compressive and flexural strength) depending amount of plasticizer in the mixture. in the experiment were prepared three sets of samples with different amounts of plasticizer (0, 0.5 and 1.0 wt. % of cement). each pair always contained reference samples (only cement) and 35 wt. % of fine ground recycled concrete. one of the main reasons for the use of finely ground recycled concrete was a certain substitution of cement in the mixture, which is the most expensive component. development of young's modulus was measured by the nondestructive method. the aim of the experiment was to determine the effect of plasticizer on the resulting physical and mechanical properties of cement pastes with fine ground recycled concrete. keywords: recycled concrete, young's modulus, plasticizer, mechanical properties, cement replacement. 1. introduction already since the first production of concrete, which has become the most widely used composite material, attempts have been made to improve the properties of this material. for adjustment of various concrete properties are used plasticizers, delayers or accelerators of solidification and hardening, aerating additives, hydrophobic additives, waterproofing and anti-frosting additives, etc. however, it is often the case that the use of the additives or admixtures to improve the desired properties cause the deterioration of others properties, and it is, therefore, necessary to evaluate the positive and also negative aspects of the used additives. the use of plasticizers for the adjustment of cement-based composites is currently relatively widespread due to the reduction of the water coefficient and the achievement of greater strengths, for example in high-performance concrete. plasticizers are organic macromolecular substances adsorbing on the surface of cement grains, allowing them to change their electric charge, disperse particle agglomerates and thereby modify the consistency of fresh concrete [1]. with recycled concrete and plasticizing additives, we meet in the area of high-performance concrete. a relatively large number of studies are focused on the use of recycled concrete aggregates in highperformance concrete, where recycled concrete is mostly a natural stone replacement [2–5]. this is the use of recycled concrete in the form of gravel of different fractions. the use of recycled fine concrete aggregates is not so widespread because it is work with fine ground recycled concrete which is overshadowed by the use of coarse recycled aggregate and brings more problems in designing the mixture in terms of water absorption. this is the reason why much less experts deal with this topic [6–8]. the use of fine ground recycled concrete in cement paste mixtures with a plasticizer and without the use of aggregate is practically not found. 2. materials and methods in the experiment was made the design of cement mixtures with fine ground recycled concrete, plasticizer and water. the aim was to propose basic mixtures with identical or similar workability. this means that the water-cement ratio has varied with each mixture (w/c = 0.23 to 0.38) due to the substitution of 35 wt. % of fine ground recycled concrete (fgrc) as the absorption requirements of fgrc for water is far greater than for cement. the water-cement ratio adjustment to achieve the desired processability of the mixture was also influenced by the added amount of plasticizer (0, 0.5 and 1.0 wt. % of cement). the polycarboxylate-based plasticizer has been used to reduce the water-cement ratio to achieve greater strengths and less pore formation in the matrix, which is also affected by the amount of mixing water. the plasticizer was added to the fresh mixture which was prepared by hand mixing. fine ground recycled concrete was used as a filler with certain bonding properties of unhydrated cement grains in fgrc. as a binder was used the portland cement cem i 42.5 r from radotín (prague, cz) 61 http://dx.doi.org/10.14311/app.2017.13.0061 http://ojs.cvut.cz/ojs/index.php/app jaromír hrůza, zdeněk prošek acta polytechnica ctu proceedings set weight of weight of w/c weight of plasticizer plasticizer cement fgrc water [wt. %,of [g] [g] [-] [g] [g] cement] a (cem) 1000 0 0.30 300 0.00 0.0 b (cem + fgrc) 650 350 0.38 380 0.00 0.0 c (cem + 0.5plast) 1000 0 0.25 250 5.00 0.5 d (cem+fgrc+0.5plast) 650 350 0.35 350 3.25 0.5 e (cem + 1.0plast) 1000 0 0.23 230 10.00 1.0 f (cem+fgrc+1.0plast) 650 350 0.32 320 6.50 1.0 table 1. overview of the mixtures composition at a weight of 1000 g mixture. figure 1. bulk density of the produced samples, standard deviation. was used. fine ground recycled concrete was obtained from road gutters. the road gutters were coarsely crushed to particle-size fraction 0–63 mm. for the intended use as a filler, or partial replacement of cement, the fraction of 0–16 mm was separated by sieving and further was modified by high-speed grinding. the composition of the proposed mixtures and the weight of the individual components for the sample production are shown in table 1. the reference set labeled as a is made only of cement and water. the pair of sets a + b, c + d and e + f differ by the amount of plasticizer contained, and each pair contains a mixture without and with 35 wt. % of fgrc (table 1). the water-cement ratio was calculated from the dry mixture. the prepared mixture was subjected to the spillage test and then placed into molds of dimension 160×40×40 mm. samples, which were made for this experiment, had been stored for 28 days in air at room temperature. the resonance method was used for measuring of the young's modulus of elasticity of the samples. it is a method of nondestructive character, which is together with measurement speed its advantage. the method is based on calculating of the dynamic modulus and dynamic shear modulus from the measured basic resonance frequencies of longitudinal, lateral (flexural) and torsional oscillation. the resonance frequencies were measured in the laboratory using a measuring assembly brüel&kjær, which consisted of an acceleration sensor brüel&kjær type 4519-003, impact hammer brüel&kjær type 8206, measuring station brüel&kjær fron-end 3560b-120 and the control notebook [9]. the flexural strength of cement mortar samples was tested by a destructive method a three-point bend. for bending tensile testing was used apparatus the heckert type fp100 with a maximum possible loading force of 100 kn with a press speed of 6 mm/min. the distance of the support supports of the test beams was 100 mm. the resulting flexural strength of a given set is an arithmetic mean of 3 measurements. compressive strength was determined on fractured samples (halves) after the flexural strength test. the compression strength test load over the previous test was 20 mm/min. mea62 vol. 13/2017 the effect of plasticizer on mechanical properties ... figure 2. the dependence of the dynamic young's modulus on the amount of plasticizer (plasticizer in wt. % of cement) and fine ground recycled concrete in time (longitudinal oscillation), standard deviation. figure 3. the dependence of the dynamic young's modulus on the amount of plasticizer (plasticizer in wt. % of cement) and fine ground recycled concrete in time (flexural oscillation), standard deviation. surement of the compressive strength was performed on five samples from each set. 3. experimental results from the bulk density overview in figure 1, can be observed a clearly visible trend in each pair of samples (a + b, c + d, e + f). we see that samples without finely ground recycled concrete have a higher bulk density than those in which 35 wt. % cement is replaced by recycled concrete. further, we can notice the increase in the values of bulk density with the increasing amount of added plasticizer. from these results, it can be assumed that the plasticizer affects the increase of bulk density. the following graphs (figure 2, figure 3) show the development values of the dynamic modulus of elasticity of each set depending on the age of the concrete (from 1 to 28 days) with 0 and 35 wt. % recycled concrete (fgrc) and various amounts of plasticizer (0, 0.5 and 1.0 % by weight of cement). as first the values for longitudinal oscillation were evaluated for each set (figure 2). to check the accuracy of the results the values for flexural oscillation were also evaluated (figure 3). because the values of both graphs (figure 2 and figure 3) are almost identical, we can say that the measurement was done properly. from the presented results of the development of the dynamic modulus of elasticity (figure 2, figure 3) we can see that the dynamic moduli of elasticity of all mixtures are approximately the same, only the set e exceeds 20 gpa. this also confirmed that 35 wt. % fgrc will not adversely affect the resulting values. an interesting finding is the higher values of set d with the addition of recycled concrete (fgrc) and 0.5 wt. % of the plasticizer compared to the reference set (a). we can only assume that the presence of plasticizer has caused higher values of dynamic young's modulus. this means that the mixture (set d) with 35 wt. % of the cement replacement with fine ground recycled concrete achieves a higher modulus of elasticity due to the reduced water-cement ratio. we can also notice a sharp increase in values after the first day of age for the sets e and f, i.e. the mixtures with 1.0 wt. % of plasticizer. the phenomenon of this kind is only visible for mixtures containing the largest amount of plasticizer. it is likely that the plasticizer caused a robust jump of values of dynamic young's modulus between first and seventh day. if we compare the blends with the added plasticizer, we see a slight improvement in the case of a larger amount of plasti63 jaromír hrůza, zdeněk prošek acta polytechnica ctu proceedings figure 4. flexural strength of 28-day old samples, standard deviation. figure 5. compressive strength of 28-day old samples, standard deviation. cizer in the mixture. when comparing mixtures b, d and f, we conclude that the plasticizer affects the resulting values of dynamic young's modulus relatively little (max. about 1.2 mpa). the flexural strength (figure 4) was improved with samples without recycled concrete (a, c, e) with increasing amounts of plasticizer. on the other hand, we can’t see virtually any difference or increasing trend of samples with fine ground recycled concrete (b, d, f). it has been found that the plasticizer does not affect the flexural strength of the cement pastes with recycled concrete. from the compression strength graph (figure 5), is visible the decrease of compression strength of the samples with the added plasticizer without recycled concrete. thus, we can observe the adverse effect of the plasticizer on the compressive strength of the samples only with cement. if we focus on samples with fine ground recycled concrete and plasticizer, we will see a slight decrease in compressive strength of set d with 0.5 wt. % plasticizer. on the other hand, the set f with the largest amount of plasticizer shows an overall improvement and an increase of strength about 5.1 mpa compared with the samples without plasticizer (set b). 64 vol. 13/2017 the effect of plasticizer on mechanical properties ... 4. conclusions the purpose and objective of the experiment were to design cement mixtures with an acceptable amount of fine ground recycled concrete and plasticizer to determine the effect of the plasticizer on the resulting mechanical and physical properties. mixtures of similar consistency and workability were designed by adjusting the water-cement ratio for each mixture. based on the results of the tests presented in this experiment were drawn the following conclusions: • the bulk densities of mixtures with the fgrc are smaller than the bulk densities of the reference mixtures. • adding the plasticizer increases the bulk density of all mixtures. • the added plasticizer practically does not affect the dynamic modulus of elasticity of samples with fgrc. • improved compressive strength after addition of 1.0 wt. % plasticizer. • the greater amount of plasticizer (1.0 wt. %) affects compressive strengths more favorably than smaller amount of plasticizer (0.5 wt. %). acknowledgements this was financially supported by the czech science foundation research projects gacr 17-06771s and by the czech technical university in prague project sgs16/201/ohk1/3t/11. the authors also thank the center for nanotechnology in civil engineering at the faculty of civil engineering, czech technical university in prague and the joint laboratory of polymer nanofiber technologies of the institute of physics, academy of science of czech republic, and the faculty of civil engineering, czech technical university in prague. references [1] m. zajíček. chemické přísady do betonu a malt. 2008 [cit 2016-11-17] available from: http://www asb-portal cz/stavebnictvi/materialy-a-vyrobky/cihlytvarnice/chemickeprisady-do-betonu-amalt 2008. [2] a. ajdukiewicz, a. kliszczewicz. influence of recycled aggregates on mechanical properties of hs/hpc. cement and concrete composites 24(2):269–279, 2002. [3] t.-y. tu, y.-y. chen, c.-l. hwang. properties of hpc with recycled aggregates. cement and concrete research 36(5):943–950, 2006. [4] b. v. kumar, h. ananthan, k. balaji. experimental studies on utilization of recycled coarse and fine aggregates in high performance concrete mixes. alexandria engineering journal 2017. [5] p. pereira, l. evangelista, j. de brito. the effect of superplasticizers on the mechanical performance of concrete made with fine recycled concrete aggregates. cement and concrete composites 34(9):1044–1052, 2012. [6] e. ledesma, j. jiménez, j. fernández, et al. properties of masonry mortars manufactured with fine recycled concrete aggregates. construction and building materials 71:289–298, 2014. [7] z. zhao, s. remond, d. damidot, w. xu. influence of fine recycled concrete aggregates on the properties of mortars. construction and building materials 81:179–186, 2015. [8] c. neno, j. d. brito, r. veiga. using fine recycled concrete aggregate for mortar production. materials research 17(1):168–177, 2014. [9] j. hrůza. design of masonry elements with use of recycled concrete. prague 2016. 65 acta polytechnica ctu proceedings 13:62–66, 2017 1 introduction 2 materials and methods 3 experimental results 4 conclusions acknowledgements references vol. 3/2016 characterization of ultrasonic assisted adhesive joints rainer pauskaa,∗, umut cakmaka, rainer lottesb, zoltan majora a johannes kepler university, faculty of engineering and natural sciences, institute of polymer product engineering, altenbergerstraße 69, 4040 linz, austria b magna cosma engineering europe ag, r&d department, weikersdorf, austria ∗ corresponding author: rainer.pauska@jku.at abstract. joining experiments using different adhesives were carried out. in addition to the adhesive, the specimens were also treated with ultrasonic waves to improve the load carrying capacity of the joined parts. lap joint shear tests have been conducted to quantify this improvement. keywords: ultrasonic, adhesion, adhesives, epoxy. 1. introduction products are becoming more complex and sophisticated in order to meet consumer needs while the environmental impact has to be reduced. focusing on automotive industry components, the challenge is to exploit lightweight design concepts and provide the expected comfort standards. a consequence of this is the multi-material (hybrid) design approach, even for non-crucial sub-components. a particular important process in the assembly of these parts is the joining. for thermoplastics the joining techniques are divided into mechanical joining, adhesive bonding and welding. joining with adhesives is becoming more popular and proper automated bonding processes without any further time consuming surface preparations are needed [1]. this work presents an advanced ultrasonic assisted joining technique. an external ultrasonic field applied to the bonding area has been shown to improve the adhesive dispersing as well as the curing kinetics [2, 3]. here, we have adopted the ultrasonic-assisted bonding technology and investigated the influence of the process parameter on the load-carrying capacity. for this purpose, we have selected a polyamide (pa) reinforced with glass fibre and optimized the ultrasonic joining parameters (joining force, time and ultrasound wave amplitude) in order to bond two samples with each other. it should be mentioned, that the selected pa shows no significant bonding strength when it is bonded without ultrasonic-treatment. this observation highlights the capability of the bonding technique. the objective of this work is to gain fundamental insights of the relationship between the ultrasonic joining parameters and the final joint’s load-carrying capacity. this relationship is crucial for the understanding of the potential and limitation of ultrasound assistance during bonding. consequently, process parameters can be adjusted in order to achieve desired mechanical behavior of the interface. 2. materials the studied polymers were polyamide 12 reinforced with 50 vol. % short glass fibre (pa12gf50). they were provided as multipurpose specimen according to iso 20753-a1. adhesives based on cyanacrylat, polyurethane and epoxy were tested due to their compatibility with the ultrasonic treatment. 3. ultrasonic-assisted bonding this section provides a brief introduction to an ultrasonic welding machine and introduces the concept used for the optimization and characterization of the ultrasonic assisted adhesive joints. 3.1. ultrasonic-welding device all the specimens were manufactured on an ultrasonic welding device stapla k35 xt (schunk sonosystems, heuchelheim, germany). this device was adopted and modified in order to perform adhesive bonding. figure 1 shows the machine, which was used to treat the prepared specimen with ultrasonic waves. in this figure the main components of the ultrasonic joining machine are shown. the ultrasonic joining parameters are adjustable on the control unit. a brief description of the parameters which were assumed to be most important for this study is included as follows: • amplitude: defines the amount of energy transferred into the joint during the process and is adjustable in % of possible maximum. • joining force: defines the pressure applied on the joining parts during the process and can be adjusted in newton. • joining time: defines how long the ultrasound and the joining force are active. has to be adjusted in seconds. the actual us welding device consists of a converter which transforms the high voltage output of the control unit to a mechanical wave, a booster and a pneu51 r. pauska, u. cakmak, r. lottes, z. major acta polytechnica ctu proceedings matic cylinder. the sonotrode is the actual "tool" of the machine. during processing the sonotrode is moved towards the upper surface of the specimen till it establishes contact with the part. after the preselected joining force is applied the ultrasonic generator is activated and the process starts. figure 2 shows the sonotrode and the clamping system in detail. figure 2. specimen clamping system. one specimen is placed in the clamps and an adhesive layer is applied on its surface. before the start of the joining process another specimen is placed on top of the clamped specimen with the adhesive layer between them. the two parts are now fixed and the joining process can take place. 3.1.1. optimization of joint properties a large number of process as well as environmental factors influences the final bonding quality. figure 3 illustrates the approach to optimize the joint properties. here, we mainly focused on the parameters of the external induced ultrasonic-treatment in order to enhance the interface between the adhesive and the pa12gf50. the ultrasonic joining parameters were assumed to be the most important factor for the optimization of the bonding quality. furthermore, a suitable geometry for the joining process and a proper selected adhesive were also considered for the optimization of the joint properties. figure 3. approach for the optimization of the joint properties. the three factors shown in figure 3 are systematically studied hereafter: geometry joining with an ultrasonic device is hardly possible without an optimization of the part geometry. multipurpose specimens have plane surfaces and hence are hard to process with the ultrasonic joining (welding) technique. in addition, plane surfaces consequently slip during the ultrasonic-treatment. this has to be avoided and an appropriate geometry has to be developed. only the upper part of the multipurpose specimen is used for this investigation, since preparation cost of the part should be as low as possible. the idea is to find a geometry which prevents slip and offers compatibility with the ultrasonic joining process. a good approach to a suitable ultrasonic joining geometry is to mill the surface and leave a chamfer (ideally triangle shaped with a sharp tip) which prevents slipping and can be molten up easier compared to the plain surface during the joining process. figure 4 shows one of four (a-d) options for ultrasonic appropriate geometry which had been tested. as already mentioned the surface was prepared with a milling tool and on the edges a chamfer was left over. the left side of the figure shows the specimen after milling. on the right side a partial cut through the chamfer can be seen. as already mentioned slipping of the parts during the ultrasonic joining process is problematic. the chamfer prevents the slipping and contributes to properly conduct the ultrasonic joining process. selection of a proper adhesive to evaluate which of the studied adhesives (cf. "materials") are suitable for the treatment with ultrasonic waves, optical assessments after ultrasonic-treatment were conducted. for the purpose of studying the influence of ultrasonic-treatment on the adhesive, the polymeric specimens were not bonded. so, the final mechanical properties of the adhesives were not determined and remain unknown. a thin film of each adhesive was applied on the surface of a specimen and treated with ultrasonic waves. the sonotrode established contact with the surface of the adhesive and ultrasound was induced directly into it. a reference sample was also prepared under the same environmental conditions, but without ultrasonic-treatment. after the adhesives were cured, the ultrasonic-treated specimen were compared to the reference sample. the main criteria for this optical comparison (assessment) were: • appearance of the adhesive after curing (colour) • crack formation through adhesive layer • compatibility with material. influence of ultrasonic joining device parameters as already mentioned the joining time, amplitude and joining force were assumed to be the most important parameters for the investigation. the joining force defines the pressure applied by the sonotrode 52 vol. 3/2016 characterization of ultrasonic assisted adhesive joints figure 1. ultrasonic joining device. pdfill p df editor w ith free write r and tools figure 4. geometry option a. onto the surface of the part and using a higher joining force usually results in a greater mechanical strength of the bonding. here, we bonded two specimens of same material and realized a lap shear joining. the displacement resulting from the melting of the specimens in contact is defined by either the force or the time parameters (depending in which mode the process is operated). the specimen created in this step had an adhesive layer between them. the ultrasonic stimulus should also have a positive influence on the interface quality between the adhesive and the pa12 surface. we conducted a pre-study to determine the optimized ultrasonic joining parameter in order to achieve joints with enhanced load-carrying capacity. by focusing on these three main factors during the conducted experimental studies, the process sensitivity regarding changes of these factors is analysed. consequently, the impact of these factors (process parameters) on the final mechanical behaviour of the bonding is determined. 3.2. testing the lap joint shear test was done on a modular test setup (testbench, bose corp., electroforce systems group, mn, us). figure 5 shows the lap joint shear test setup in detail. in this illustration the lap joint shear test setup can be seen with a mounted specimen in the clamp. for all the experiments a testing speed of 5mm/min was used according to astm d1002-01. figure 5. specimens bonded by the adopted ultrasonic joining device. to meet all the prerequisites for the lap joint shear test the lower side of the clamping unit, where the load cell was mounted, was aligned in order to avoid (minimize) bending loading at the bonded area. 4. results 4.1. first ultrasonic joining parameter optimization after the pre-study was done specimen with the found parameters were created. the adhesive best suited for the ultrasonic treatment was a two component epoxy type which was used for all the conducted experiments. a part of the results is shown in figure 6. this figure illustrates some of the results generated from the first ultrasonic welding parameter optimization. the influence different parameter settings have on the load-carrying capacity is shown. different joining forces n were applied while ultrasound amplitude a and joining time t remain unchanged. higher joining force resulted into higher load-carrying capacity. the spikes in the slope of the green line are caused by slip of the clamp during measuring. experiments with optimized geometry have not been conducted in this 53 r. pauska, u. cakmak, r. lottes, z. major acta polytechnica ctu proceedings figure 6. comparison of the load-carrying capacity of specimens bonded with varying ultrasonic parameters. first experimental series. 4.2. second ultrasonic parameter optimization and first geometry experiments in this second experimental series the potential of this joining technique is explored. figure 7 shows a comparison of specimen created with untreated adhesive, adhesive with ultrasonic treatment and different geometry possibilities without the use of an adhesive between the joining parts. the geometry specimen are bonded by the material melting up during the joining process. this was done to explore how much the geometry can contribute to the total load carrying capacity of a combined sample (ultrasonic treated adhesive, geometry). figure 7. normalized load-carrying capacity improvement comparison. the column on the left side represents the specimens which have been joined just by the use of an adhesive. their average load carrying capacity value was used as reference to normalize the values of the other specimen. comparison shows a significant raise in the load-carrying capacity between the three left columns. a more detailed optimization of the ultrasonic joining parameters improved the load-carrying capacity by a large amount compared to untreated and specimen belonging to the first optimization attempt. the first geometry specimen created (a-d) did not provide a load-carrying capacity as high as the optimized samples created with ultrasonic treated adhesive did. results of latest unfinished experiments showed, geometry also has a high potential to increase the load carrying capacity of the joining parts more than what can be seen in figure 7. if parametrization of the ultrasonic joining device is done correctly and the geometry matches the application higher load carrying capacities can be achieved. to further increase the specimen’s load-carrying capacity a combination of ultrasonic assisted adhesion and an application matching geometry joined with the adopted ultrasonic joining parameters will be examined. this combination is assumed to offer even higher load carrying capacity than the specimens tested till now. 5. conclusions based on a systematic parameter study, the influence of three main factors (geometry, adhesive, ultrasonictreatment parameters) on the final bonding quality was examined. moreover, the potential of ultrasonicassisted bonding was highlighted throughout experimental studies. in figure 7 the significant improvement of load-carrying capacity can be seen. comparing the treated specimen of the second optimization with the untreated reference samples load carrying capacity was improved approximately five times. basically, the ultrasonic-treatment parameters have the highest impact on the final bonding quality for 54 vol. 3/2016 characterization of ultrasonic assisted adhesive joints both the geometry and ultrasonic treated adhesive. here, the load-carrying capacity was determined from lap shear measurements and was used as a measure of the bonding quality. as the utilized geometry was not according to the respective lap shear test standard (astm d1002-01), the bond strength was not evaluated. the performed mechanical experiments were only for relative comparisons within the here studied specimens. bond strength has to be determined in future works and compared to data achieved by other bonding technologies. list of symbols a amplitude n joining force t joining time references [1] j. czarnecki, m. hayek-boelingen, h.-j. gudladt, h. schenkel. kontaminationstolerantes kleben aktueller stand der entwicklung. adhäsion kleben & dichten 48(4):36–39, 2004. doi:10.1007/bf03255632. [2] m. hayek-boelingen. boelingen, m. (2004). wege zum kontaminationstoleranten kleben. ph.d. thesis, universität der bundeswehr münchen, neubiberg, germany, 2004. [3] j. holtmannspötte, m. wetzel, j. czarnecki, h.-j. gudladt. how acoustic cavitation can improve adhesion. ultrasonics 52(7):905–911, 2012. doi:10.1016/j.ultras.2012.02.013. 55 acta polytechnica ctu proceedings doi:10.14311/app.2016.3.0035 acta polytechnica ctu proceedings 3:35–38, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app identification of damaged zones in c/pps specimens subjected to fatigue loading based on high-resolution thermography petr koudelkaa,∗, daniel kytýřa,b, nela fenclováa,b, martin šperlb a czech technical university in prague, faculty of transportation sciences, konviktská 20, 120 00 prague 1, czech republic b czech academy of sciences, institute of theoretical and applied mechanics, prosecká 76, 190 00, prague 9, czech republic ∗ corresponding author: koudelka@fd.cvut.cz abstract. in this study high resolution thermography is used for identification of damaged zones in carbon fiber/polyphenylene sulfide (c/pps) long fiber composite specimens with induced impact damage subjected to tensile fatigue loading. image processing techniques were applied on thermographs from all loading cases to obtain segmented images of the damaged location that were then used for calculation of the heated area. results show that the considered method can be used to identify heated area in the vicinity of damage with high confidence at low number of cycles where no significant fatigue effect is present in the material. keywords: fatigue, damage, long fiber composite, c/pps, thermography. 1. introduction composites with different matrix materials reinforced by short or long fibers have been widely used as structural materials thanks to their favorable mechanical properties (particularly relative stiffness and strength) for several decades. one of very popular composite compounds widely used in aviation industry consists of polyphenylene sulphide (pps) matrix and carbon fiber reinforcement. the material is commonly used for production of both external and internal aircraft components because of its excellent mechanical properties, chemical resistance to aerospace fluids, low density and good resistance to heat and flames [1]. micrograph of damaged composite structure after material failure is depicted in figure 1. figure 1. detail of damaged structure obtained by scanning electron microscope, the plies are consisted of yarn with individual 5µm fibres. still, application of this material in airframes is limited by its relatively low impact resistance and fragile behavior that have to be thoroughly investigated before its operational deployment [2]. in the life-cycle of an airframe, damage from impacts may be inflicted during flight or ground maintenance. this in combination with unique nature of composites and high cycle fatigue may lead to unexpected failure due to damage accumulation in the material’s microstructure [3]. in this study high-resolution thermography has been used to observe dynamically loaded damaged specimens in order to quantify thermal characteristics of the damaged area and to evaluate suitability of considered approach for ndt inspection/damage tolerance analysis [4–6]. thus, primary goal of this study was to identify lowest possible stress level for reliable assessment of the damage in low number of loading cycles. 2. materials and methods 2.1. specimen description the c/pps material used in this study consists of 8-ply of carbon fabric with volume fraction of fibres approximately 60 %, overall density 1.35 g · cm−3 and quasi-isotropically distributed fibres. surface of the samples was covered by thin glass fibre cloth protecting the core against uv light, surface damage and chemical influences. set of eight dog bone shaped specimens were prepared using numerical controlled water jet cutter from two plates of c/pps material (dimension 160×160 mm) with thickness 2.5±0.1 mm. overall length of specimens was 160 mm. distal part with width 25 mm was used for best possible fixation in mechanical grips whereas central part with length 105 mm and width 20 mm was subjected to the initial loading and thermographically investigated. 35 http://dx.doi.org/10.14311/app.2016.3.0035 http://ojs.cvut.cz/ojs/index.php/app p. koudelka, d. kytýř, n. fenclová, m. šperl acta polytechnica ctu proceedings 2.2. initial damage before dynamic loading the specimens were subjected to impact loading to impose initial damage under controlled conditions using instrumented drop tower. experimental setup with maximal impact energy 50 j was used in configuration with steel spherical impactor having diameter 15 mm. impact energy of 15 j was set to inflict initial damage in the central part of the sample leading to imprint diameter in range of millimeters and depth in range tens of micrometers. the geometrical characteristics of imprints were identified using laser profilometry method [7]. 2.3. experimental setup for the investigation of thermal response to the mechanical loading mikrotron (russenberger prüfmaschinen, germany) resonant testing machine was employed. loading was performed in tensile mode at four stress levels with mean load 4.5, 5.0, 5.5, 6.5, 8.0 kn and amplitude 2.0, 3.0, 4.0, 4.5, 5.0, 6.0 kn in sinusoidal cyclic force. testing frequency was approximately 75 hz. highest stress level did not exceed 35 % of tensile strength of the material and fully elastic behaviour during loading cycles was assumed. one of damage degradation parameter obtained from resonant excitation is cycle dependent decrease of natural frequency. according to our previous study eigenfrequency decrease lower than 0.05 % indicates no damage inflicted in the material’s microstructure. over the whole testing campaign this level was not exceeded as can be seen from graph of natural frequencies plotted against number of cycles (figure 2). −0.02 −0.01 0 0.01 0.02 0.03 0.04 0.05 0 10000 20000 30000 40000 50000 ∆ na tu ra l f re qu en cy [h z] loading cycles 6.5 ± 6.0 kn 8.0 ± 6.0 kn 5.5 ± 5.0 kn 5.0 ± 4.5 kn 4.5 ± 4.0 kn 8.0 ± 4.0 kn 5.0 ± 3.0 kn 8.0 ± 2.0 kn figure 2. variation of natural frequency as a function of number of cycles. the test was performed at constant room temperature 22 ◦c. loading scene was observed using scientific-grade thermal imaging camera sc7650 (flir systems, usa). the device is equipped with insb cooled sensor with pixel pitch 15µm and resolution 640 × 512 px. the device allows acquisition of images in temperature range −20 to 300 ◦c with full frame sampling frequency 100 hz. in this work full frame resolution and 0.5 hz acquisition frequency was used. control of the camera and acquisition of figure 3. experimental setup for thermographical observation of dynamic loading. specimen initial damage 1 1 1 1 figure 4. distribution of rois in thermograph for segmentation and area calculation: 1) background temperature, 2) specimen temperature, 3) heated area. thermographs was performed using gige interface. experimental setup is depicted in figure 3. 2.4. image processing procedure thermographs were subjected to image processing procedures in order to identify the damaged zone and to calculate the heated area in its vicinity. adaptive identification technique based on the median value of the background (blue areas in figure 4) was used for differentiation of the sample and background. median of specimen’s temperature was then found and area with temperature higher than 105 % of the median temperature was subjected to investigation (red area in figure 4). standard morphological opening and closing procedures with circular structuring element were applied on the identified heated areas to improve accuracy of impacted area calculation. in result all holes in the identified area smaller than 3 px2 were morphologically closed and areas smaller than 10 px2 were neglected from the calculation. visualisation of a series of thermographs subjected to investigation using image processing techniques is shown in figure 5. 3. results during the thermographically observed experiments it has been found out that normalized peak temperature (temperature of specimen relative to ambient temperature) converges to constant value in less than 50 000 36 vol. 3/2016 identification of damaged zones in c/pps based on thermography loading cycles. in figure 6 dominant influence of the amplitude compared to mean value of applied load to the maximal temperature is clearly visible. in case of the highest loading level temperature of the specimen reached absolute value of 45 ◦c corresponding to less than 50 % of the material’s glass transition temperature. therefore negative thermal effects influencing the material properties (particularly the assumed elastic behavior) during the test were avoided. figure 5. example of a series of acquired thermographs showing heating of the damaged zone during cyclic loading at 1 s (left), 32 s (middle) and 200 s (right); temperature scale is in ◦c. 1 1.2 1.4 1.6 1.8 2 2.2 0 10000 20000 30000 40000 50000 m a x im u m t e m p e ra tu re t o b a c k ro u n d r a ti o loading cycles 6.5 ± 6.0 kn 8.0 ± 6.0 kn 5.5 ± 5.0 kn 5.0 ± 4.5 kn 4.5 ± 4.0 kn 8.0 ± 4.0 kn 5.0 ± 3.0 kn 8.0 ± 2.0 kn figure 6. ratio of specimen to ambient temperature as a function of number of cycles. threshold temperature higher than 105 % of average specimen temperature (calculated from the yellow area in figure 4) was chosen for identification of the local damaged zone. according to acquired results significant increase of the temperature in damaged zone became observable after only a few hundred of loading cycles. after that peak temperature in the damaged zone rose sharply together with average temperature in the entire volume of the samples. this average temperature reached its maximum equal to temperature after approximately 10 000 loading cycles yielding the thermal footprint of the samples homogeneous. hence higher number of loading cycles was unnecessary for our study. identified damaged zones for all loading cases are depicted in figure 7. it can be seen that minimal loading level 5 ± 4.5 kn was sufficient for reliable identification of the dam 0 20 40 60 80 100 120 140 0 10000 20000 30000 40000 50000 id e n ti fi e d a re a r a ti o 5 x 1 0 − 5 loading cycles 6.5 ± 6.0 kn 8.0 ± 6.0 kn 5.5 ± 5.0 kn 5.0 ± 4.5 kn 4.5 ± 4.0 kn 8.0 ± 4.0 kn 5.0 ± 3.0 kn 8.0 ± 2.0 kn figure 7. variation of identified heated area in the vicinity of damage as a function of number of cycles. aged zone in the vicinity of impact due to its apparent heating. detailed plot of identified heated area in the vicinity of damage and median temperature of specimens for two representative loading cases is shown in figures 8 and 9. here increase of the loading to 6.5 ± 6 kn shows significant increase of the relative heated area (ratio of identified heated area in the vicinity of damage to total area of specimen) of magnitude more than 30 times. this together with the fact that in all cases number of loading cycles lower than 10 000 was sufficient for identification of the influenced zone indicates that the proposed method is suitable for non-destructive inspection of c/pps long-fiber composites. 0 0.5 1 1.5 2 2.5 3 3.5 4 4.5 0 10000 20000 30000 40000 50000 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 id e n ti fi e d a re a r a ti o 5 x 1 0 -5 m a x im u m t e m p e ra tu re t o b a c k ro u n d r a ti o loading cycles area temperature figure 8. evolution of identified heated area during mean temperature of specimen during 5 ± 4.5 kn loading. 4. conclusions it can be seen that in majority of loading cases the material exhibits consolidation and hardening in the first 50 000 cycles. for the two cases where combination of mean force and amplitude causes damage accumulation image processing methods have been applied on thermographs to obtain segmented images of the damaged location. from the segmented 37 p. koudelka, d. kytýř, n. fenclová, m. šperl acta polytechnica ctu proceedings 0 20 40 60 80 100 120 140 0 10000 20000 30000 40000 50000 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2 2.1 id e n ti fi e d a re a r a ti o 5 x 1 0 -5 m a x im u m t e m p e ra tu re t o b a c k ro u n d r a ti o loading cycles area temperature figure 9. evolution of identified heated area during mean temperature of specimen during 6.5 ± 6 kn loading. images heated areas were calculated together with specimen/background temperature ratio and plotted against number of loading cycles. it is apparent that heated area in the vicinity of damage can be identified with high confidence at low number of cycles (10 000) where no significant fatigue effect is present in the material. the considered inspection method is thus suitable for ndt inspections or damage tolerance analysis. acknowledgements the research was supported by grant agency of czech technical university in prague (projects no. sgs15/225/ohk2/3t/16, 1051505f014 rpmt 2015 43e), by technology agency of the czech republic (project no. ta03010209) and by rvo: 68378297. references [1] m. favarolo: proceedings of sampe 2010 conference, 2010. [2] p. koudelka, t. fíla, t. doktor, d. kytýř, j. valach, et al.: inspection of post impact fatigue damage in carbon fibre composite using modulus mapping technique, key engineering materials, 606:245-248, 2014. doi:10.4028/www.scientific.net/kem.606.245 [3] r. aoki, j. heyduck, developments in the science and technology of composite materials, 633-642, 1993. [4] j. p. gallagher, usaf damage tolerant design handbook, flight dynamics laboratory, air force wright aeronautical laboratories, 1984. [5] m. naderi, a. kahirdeh, m.m. khonsari: dissipated thermal energy and damage evolution of glass/epoxy using infrared thermography and acoustic emission, composites part b: engineering, 43(3):1613-1620, 2011. doi:10.1016/j.compositesb.2011.12.013 [6] e.z. kordatos, d.g. aggelis, t.e. matikas: monitoring mechanical damage in structural materials using complimentary nde techniques based on thermography and acoustic emission, composites part b: engineering, 43(6):2676-2686, 2012. [7] kytýř, d., fíla, t., šleichrt, j., doktor, t., šperl, m. assessment of post impact damage propagation in carbon-fibre composite under cyclic loading. materials and technology, 48(5):777-780, 2014. 38 http://dx.doi.org/10.4028/www.scientific.net/kem.606.245 http://dx.doi.org/10.1016/j.compositesb.2011.12.013 acta polytechnica ctu proceedings 3:35–38, 2016 1 introduction 2 materials and methods 2.1 specimen description 2.2 initial damage 2.3 experimental setup 2.4 image processing procedure 3 results 4 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2016.3.0011 acta polytechnica ctu proceedings 3:11–14, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app analysis of welded polypropylene structures: combination of experiments and simulations theresa distlbacher∗, martin reiter, zoltan major johannes kepler university, faculty of engineering and natural sciences, institute of polymer product engineering, altenbergerstraße 69, 4040 linz, austria ∗ corresponding author: theresa.distlbacher@jku.at abstract. the effect of joining by extrusion welding on the tensional stiffness and strength of a polypropylene copolymer was analysed. short-term and creep tests with laboratory specimens were conducted. welded joint sub-components were simulated with the finite element method and the results were validated by experiments. keywords: thermoplastic welding, extrusion-welding, fem, welded structure. 1. introduction extrusion welding is a joining technology suitable for manufacturing of large and complex polymeric structures. filler material is plasticised by a small extruder and the welding partners are pre-heated locally to soften the parent material in the joining area. the molten filler then is deposited in the weld gap between the joining partners. consolidation and solidification of the melt gives the joint its strength. [1] this technology is well established in the industry but there is hardly any information available about the impacts of this process on the material properties and the mechanical behaviour of welded components. the presented work examined conceivable altering of the material in terms of true stress true strain relation. also possible implication to the joint geometry was determined by analysing stiffness and strength of subcomponents based on finite element method (fem) simulations combined with experimental tests. 2. material under examination was a semi-crystalline polypropylene copolymer with enhanced low temperatures impact resistance. mechanical short-term tension tests were performed and elastic-plastic material models for the fem based on the experimental results were developed. 2.1. material testing two types of cylindrically laboratory specimens with a diameter of 8mm and a gauge length of 30mm were prepared. figure 2-a shows drawings of the laboratory specimen types, the reference specimen type (a.1), without any weld and the weld specimen (a.2) containing an extrusion k-weld. short-term uni-axial tensile tests at ambient temperature were performed with a tension rate of 1mm/s. figure 2-b illustrates the longitudinal strain on the surface of the specimen measured with a digital image correlation system during testing. a concentration of strain can be observed at the location of the k-weld. evaluations of strains in longitudinal and transversal direction were done locally in those areas highlighted in figure 2b by a rectangle. in further data processing steps a logarithmic measure for true strain was used. ε(t) = ln(1 + εl(t)) (1) true stress is related to the actual minimum cross section of the specimen and was calculated according to the following equation. σ(t) = f (t) a(t) = f (t) εt(t)2a0 (2) current values for the cross section can be derived by multiplying the initial cross section with the squared current transversal strain. 2.2. material modelling from the true stress-strain relations, the constitutive parameters for an isotropic multi-linear elastic-plastic material model were determined. figure 1. experimental results from tensile tests with parent and weld materials and the resulting material models. 11 http://dx.doi.org/10.14311/app.2016.3.0011 http://ojs.cvut.cz/ojs/index.php/app t. distlbacher, m. reiter, z. major acta polytechnica ctu proceedings figure 2. drawing of laboratory specimens: without weld (a.1), with k-weld (a.2); longitudinal strain measured during testing (b). an illustration of the experimentally determined true stress over true strain and the material model curves for parent material and extrusion k-weld can be seen in figure 1. this graph outlines a reduction in stiffness as well as strength of the welded material compared to the parent material. the elastic-plastic material model is an appropriate representation of the polymeric material’s behaviour, even though the model is primarily applied for a large variety of metals. polymeric materials exhibit not only elastic and plastic but also viscous behaviour ([2],[3]). viscoelasticity is not included in this simple model. therefore, an arbitrary chosen apparent young’s modulus and a yield point were defined for the fe software nx nastran (siemens plm software inc./usa). these apparent values should not be confused with the actual, physical ones resulting from tension tests. table 1 lists the physical and apparent mechanical behaviours of the parent material. physical apparent e [mpa] 1534 1530 σy [mpa] 29.9 15.3 εy [-] 0.04 0.01 table 1. physical and apparent parent material properties. basic models like this are convenient in use and could be capable also for representing some polymeric materials in special cases. in this work it was used because no unloading or dynamic effects were simulated. the application furthermore requires the analysis of time dependent behaviour (relaxation, creep, rate dependency), this simple model is not applicable and advanced models have to be utilized. 3. subcomponent the extrusion welding technology is not only used for butt-joints but more often to manufacture more complex joint-geometries like t-joints. therefore, weld samples were manufactured according to the standard of the german welding society (dvs [4]). a t-joint figure 3. t-joint geometry. geometry as shown in figure 3 was analysed. one meter long weld samples were made by joining a 20mm and a 15mm thick extruded polypropylene copolymer sheet via extrusion welding technology. then, subcomponents with a length of 60mm were cut off these weld samples. 3.1. subcomponent testing the experiments were conducted with the servohydraulic testing system mts 852 damper test system (mts systems corporation, eden prairie, usa). figure 4. subcomponent test setup. 12 vol. 3/2016 analysis of welded polypropylene structures figure 5. fe stress results of the 2-material (left) and the reference model (right). figure 6. fe model of the t-joint. figure 4 depicts the experimental set-up. the subcomponents were locked into position by the fixing frame, which is mounted on the non-moving side of the testing machine. the 15mm thick plate was fixed by a grip connected to the actuator, moving downwards in displacement controlled mode with a speed of 1mm/s. the force was measured with a load cell located above the fixing frame. 3.2. subcomponent fe modelling to simulate the above described experiment a standard 3d structural fem procedure was applied. geometrically modelling of the t-joint was done by 3d cad. preand postprocessing of the simulation were performed in the commercial fem software nx nastran (siemens plm software inc./usa). from figure 6 we can see the meshed model. sheet and weld material were modelled as separate parts and were connected by the surface-to-surface-gluing condition. the plunger was modelled to move with -1mm/s (enforced displacement constraint), while the subcomponent was fixed by a boundary condition locking all figure 7. experimental and fe analysis results. degrees of freedom. the parameters of the material models described in section 2.1 were assigned to the mesh. two different simulation sub-cases were created: • 2-material model: the k-weld material model was assigned to the weld geometries and the parent material model was assigned to the sheets. • reference model: the parent material model was assigned to the sheet and the weld geometries. the sub-cases are identically in terms of mesh, boundary conditions and applied load. also the same solver, the nx nastran’s solution type sol106, a basic nonlinear implicit solver was used. 3.3. results and validation in figure 7 the measured force is plotted against displacement of the plunger for the experiment, the 2-material fe model and the fe reference model. one can see a nearly linear increase in force until a displacement of 1.5mm. the simulation fits the experiment very well in this region. above a force 13 t. distlbacher, m. reiter, z. major acta polytechnica ctu proceedings figure 8. local validation of the subcomponent reference model fe analysis at an actuator displacement of 2mm. of 15 kn the curves level off until they reach another nearly linear region. the experimentally evaluated curve shows a negative slope and the simulated ones still exhibit a slight upwards trend. difference between experiment and simulation in the force-displacement graph might be caused by the ideal representation of the fixing in the simulation. the fe results of the 2-material model and the reference model are nearly equal. evaluation of the stress distribution on the subcomponent’s surface was done to find out possible local effects provoked by the second material model. in figure 5 the stress von mises at a displacement of 2mm of the 2-material model is compared to those of the reference model. elements where the stress has reached the physical yield stress of 29.9mpa are visualized in grey. yield is already reached in those regions where the fixing constraint starts. in general one cannot see a significant differences between 2-material model and reference model in the stress distribution. only a slightly reduced stress in the lower weld toe can be observed for the 2-material model, which is a result of the more flexible weld material. locally the simulation results were validated by comparing the measured major strain at the surface of the subcomponent with the simulated one, see figure 8. the experimentally measured and the simulated maximum strain was found at the same location, where the clamping of the 15mm thick sheet starts. a maximum strain of 0.17 was measured and the simulated strain was 30% smaller. 4. conclusions this work has shown that with validated data a material model for extrusion welded structures can be easily generated, to analyse larger welded structures by fem. the elaborated material models take a nonlinear stress-strain behaviour of parent and weld material into account. a significant change in stiffness and strength of the examined material resulting from the extrusion welding process was found. due to the nature of extrusion welding process imperfections in the weld seam and interface are difficult to avoid. these irregularities and voids are crucial for the structural integrity. considering such effects in fe analysis would allow further structural improvements and reliable lifetime predictions. in future works the focus will be given to fracture mechanical analyses, including the crack propagation in the extrusion weld. list of symbols a cross section a0 initial cross section e young’s modulus f force ε true strain εl longitudinal strain εt transversal strain εy strain at yield σ true stress σy yield stress acknowledgements this work is part of a master thesis carried out at the institute of polymer product engineering (johannes kepler university, linz-austria) in cooperation with the rosenbauer ag (leonding-austria). the author gratefully thanks the institute and the company for initiation of this research topic and for the scientific as well as the financial support. references [1] d. a. grewell, a. benatar, j. b. park. plastics and composites welding handbook. carl hanser verlag, munich, 2003. [2] r. s. lakes. viscoelastic materials. cambridge university press, 2009. [3] y.-h. lin. polymer viscoelasticity: basics, molecular theories, experiments and simulations. world scientific publishing company, new jersey, 2nd edn., 2010. [4] fügen von kunststoffen taschenbuch dvs merkblätter und richtlinien. dvs-verlag, düsseldorf, 13th edn., 2012. 14 acta polytechnica ctu proceedings 3:11–14, 2016 1 introduction 2 material 2.1 material testing 2.2 material modelling 3 subcomponent 3.1 subcomponent testing 3.2 subcomponent fe modelling 3.3 results and validation 4 conclusions list of symbols acknowledgements references 133 acta polytechnica ctu proceedings 2(1): 133–138, 2015 133 doi: 10.14311/app.2015.02.0133 observing cvs and lmxbs with salt: updates and recent results david a. h. buckley1 1southern african large telescope, c/o south african astronomical observatory, po box 9, observatory 7935, cape town, south africa corresponding author: dibnob@salt.ac.za abstract i present an overview of the ongoing observational programs utilizing the southern african large telescope (salt), focussing on magnetic cataclysmic variables and low mass x-ray binaries. salt’s instruments and capabilities are well suited to time resolved studies of the accretion phenomena exhibited in these systems. initial observations, using salticam, have been used to derive high time resolution (∼100ms) eclipse light curves, with high signal-to-noise, of polars. recently this work has been extended to time resolved spectroscopic studies, utilizing the salt robert stobie spectrograph (rss), allowing an opportunity to probe how the emission lines change during eclipse. a program to search for and characterize quasi-periodic oscillations (qpos) in magnetic cvs using the saao 1.9-m telescope, begun in 2012, has been expanded to include observations with a photon counting camera (bvit) on salt. a multi-longitude campaign involving salt, other saao facilities plus the eso ntt, was carried out in march/april 2012 on the enigmatic gamma ray source, xss j12270–4859, which has revealed the that system exhibits spectral line variations, from absorption to emission, seemingly over timescales of < 1 h. keywords: cataclysmic variables polars intermediate polars optical spectroscopy photometry x-rays individual: fl cet, ex hya, hu aqr, xss j12270-4859. 1 introduction the southern african large telescope (salt) is one of five 10-m class segmented mirror telescopes and the only one situated in the southern hemisphere. at the last palermo cv meeting in 2011, i summarized the capabilities and the status at that time (buckley 2012) and presented some early science results. since then salt has entered full time science operations (in november 2011) and has begun to steadily increase its scientific productivity (up to ∼60 refereed publications). there are still some remaining issues to resolve, however, notably implementation of a mirror edge sensing system to allow active control of the primary mirror array. this is currently under development and the first batch of new inductive edge sensors will be installed early in 2014, while the final ones will be installed late in 2015. this will lead to much improved image quality and, more importantly its retention during an observation. similarly there are improvements being made to the throughput of the main work-horse salt science instrument, the robert stobie spectrograph (rss), which should greatly improve its performance, particularly in the blue (320 400nm). this is being achieved by fabrication of new collimator optics and opto-mechanics, designed to avoid the optical fluid contamination problems that have led to the current throughput under-performance. these new optics are expected to be installed by mid-2014. salt is a 100% queue-scheduled telescope, where all observations are undertaken in a service observing mode by salt staff. this modus operandi lends itself to target-of-opportunity observations and synoptic monitoring campaigns, both of which are often appropriate for observations of cataclysmic variables and related objects. for example, to cover specific phase intervals, to coordinate with x-ray or other satellite observations, to monitor a system through an outburst or accretion state change, etc. just such observations have already been carried out with salt and some examples are discussed in this paper. 1.1 high speed photometry with salticam salticam employs frame transfer (ft) ccds, which allows for fast acquisition and imaging. it also has a moving occulting mask which allows for 3 imaging modes: full field imaging, frame transfer mode (half of the field is imaged) and a specialized high-speed mode, 133 http://dx.doi.org/10.14311/app.2015.02.0133 david a. h. buckley where a narrow slot is imaged. the latter, known as ”slot mode”, allows for high-speed (up to ∼12.5hz) photometry and has been used extensively for observing cvs, x-ray binaries and related systems. figure 1: the 11-m southern african large telescope (salt), consisting of 91 × 1.2 m (corner-to-corner) hexagonal mirror segments. this mode allows for just 144 rows of the ccd mosaic to be illuminated, equivalent to ∼20 arcsec × 10 arcmin rectangular region on the sky. the object of interest, plus ideally a nearby (< a few arcmin) constant source (i.e. a comparison star), are placed in the centre of this slot, which can be achieved by rotating the instrument to the desired position angle. the illuminated region of the ccd is then exposed (typically with exposure times ranging from 80 – 1000 ms) and then quickly (within a few ms) row-shifted into the storage array, while another exposure begins. thus exposed slot regions are sequentially moved through the storage array to the serial readout register. during the next exposure, the latest exposed region to reach the bottom of the chip is readout in a time < the exposure time, which is dependent on the on-chip binning factor (usually 4 × 4 pixels). 1.2 time resolved spectroscopy with rss like for all current salt instruments, the robert stobie spectrograph (rss) resides at salt’s prime focus (f/4.2). the advantages of this include maximizing the performance at short wavelengths (< 400 nm), by avoiding use of optical fibres, and ability to conduct fabryperot imaging spectroscopy. rss was designed to have a range of capabilities and observing modes, each one remotely and rapidly reconfigurable. figure 2: the narrow occulting slot that can be moved just in front of the salticam ccds to allow for high time resolution (down to ∼80 ms) photometry. in keeping with the overall philosophy of exploiting those areas where salt has a competitive edge, the instrument has a range of capabilities, many well suited to cv and lmxb studies, including: � wavelength coverage from 320 to 900 nm for the initial uv-vis configuration (a second near ir arm, extending to 1.7 µm, is under construction). low to medium resolution spectroscopy (up to r ∼6000 with 1 arcsec slits) using efficient and tuneable vph gratings. � narrow band, tuneable filter and fabry-perot imaging. � high time resolution (∼0.1 sec) spectroscopic and polarimetric modes. � imaging and spectropolarimetry (linear, circular and all stokes modes), time resolved modes plus low resolution (r ∼50) wide-field imaging spectropolarimetry. high time resolution spectroscopy is achieved using a similar slot-mode option, as for salticam. however, rather than the mask being just above the detector, it is placed at the telescope’s focal plane, coplanar with the spectrograph’s slit. this allows for the spectrum of the variable target to be imaged in a narrow rectangular region and then shuffled into the storage array at the end of the exposure. three 2k × 4k ccds are mosaiced to allow spectra to be obtained over the entire 8 arcmin fov (e.g. for mos). figure 3 shows the arrangement of 134 observing cvs and lmxbs with salt:updates and recent results the slot with respect to the ccd mosaic, where the slot is placed just above the imaging / storage boundary. figure 3: schematic showing the region on the ccd where time resolved rss spectra are recorded using a focal plane mask together with the spectrograph slit. spectra of the target and sky are obtained in the rectangular region, which shuffled down across the frame transfer boundary at the end of a short exposure. 2 time-resolved studies of polars the first high-speed observations conducted with salt were mostly of eclipsing magnetic cataclysmic variable stars (mcvs), specifically polars. these systems emit the bulk of their luminosity (from x-rays to the optical / ir) from small accretion regions near the magnetic pole(s) of a strongly magnetized (∼101 to 102 mg) white dwarf. the dominant emission components in such systems includes hard (> 10 kev) thermal bremsstrahlung x-rays from an accretion shock just above the white dwarf surface. a fraction of this radiation is reprocessed in the white dwarfs photosphere into softer x-rays, uv and optical radiation. in some systems, ballistic ”blobs” of accreting material bury into the white dwarf’s photosphere, thermalize and contribute to the soft x-ray/extreme uv component. shock cooling occurs through polarized optical/ir cyclotron emission. polars therefore present a wealth of multi-wavelength observational opportunities, which are being exploiting with salt. 2.1 light curves of eclipsing polars in eclipsing polars, the size, structure and location of accretion regions can be determined from high time resolution (sub-second) photometry. since 2005 observations have been carried out with salticam to obtain continuum eclipse curves with unprecedented time resolution and signal to noise. an example is for the eclipsing system fl cet, with a 1.45 h orbital period (o’donoghue et al. 2006). an eclipse egress light curve, taken with salticam in ”slotmode” with 112 ms data sampling, is shown in fig. 4. the intensity steps are due to the progressive re-appearance of two accretion hot-spots near the magnetic poles, which take ∼1.5 s to be uncovered. these data have been fitted with a model based on the likely masses of the component stars, as derived from the eclipse parameters and orbital period, plus the orbital inclination of the system (i) and the co-latitudes of the accretion spots (β1 and β2). figure 4: salticam eclipse egress light curve of fl cet, showing the re-appearance of two accretion spots. other polars are also being systematically observed in order to derive similar quality light curves from which to determine the accretion geometries. an example is shown below for the system hy eri, which has been observed in both high and low accretion states. figure 5: eclipse light curves of hy eri, at high (upper curve) and low (lower curve) accretion states. 2.2 spectra of eclipsing polars since 2011 the eclipse light curve program has been extended to spectroscopic investigations of the emission lines of eclipsing polars, using rss in time-resolved spectroscopy mode. the aim of these observations is to probe the mass transfer flow from the secondary star to the white dwarf, specifically where it changes from a 135 david a. h. buckley ballistic to a magnetically controlled trajectory. the geometry of this so-called ”threading region” varies from system to system and is dependent on the accretion rate and magnetic field topology. previous attempts at probing the nature of the threading region (e.g. hakala et al. 2002, bridge et al. 2004) have often been frustrated by the problem of unambiguously determining the accretion stream structures from the 1-d data derived from broad band eclipse light curves. these new salt observations are aimed to address this issue and resolve details of the mass transfer stream through high time resolution emission line spectroscopy. such data will lead to stream eclipse light curves as a function of wavelength and hence radial velocity, enabling the structure of the mass transfer stream to be determined. doppler tomographic techniques will be applied to these data in order to attempt to map the positions of the line emitting regions. recently a new ”inside-out” doppler tomography technique has been devised (e.g. see kotze & potter; these proceedings). eventually we plan to undertake phase resolved spectropolarimetric observations of these systems, using rss (when the polarimetric modes are re-activated in 2014). these observations will probe the phase dependent cyclotron emission, giving us an independent view of the polarized emission arising from the accretion spots. during low states it may also be possible to study the polarization of the zeeman lines from the white dwarf and the accretion halo. figure 6: an example of time resolved (10s) trailed spectroscopy of the eclipsing polar hu aqr. 2.3 qpos in magnetic cvs in 2012 a program to study quasi-periodic oscillations (qpos) in magnetic cvs was instigated at saao, mostly using the new electron multiplication ccd (emccd) cameras (shoc) on the saao 1.9-m telescope. the aim is to search for and characterise the nature of the optical qpos, which have typical periods of a few seconds. the commonly held understanding is that they are due to plasma oscillations in the magnetically confined accretion columns which constrain the accreted plasma before it cools and settles onto the surface of the magnetic white dwarf. the qpo frequency is thought to be related to the physical parameters inside the column (or sub-columns), particularly the shock height, accretion rate and magnetic field strength. this work will hopefully lead to a better understanding of the physics underlying the qpos, taking the study from being purely phenomenological to one based on quantitative physical parameters. in conjunction with this observational program, we expect that the experimental results from a parallel program of simulating accreting columns in the laboratory will yield further relevant insights (e.g. michaut et al. 2012). the project involves new technology detectors, namely emccds, which have both good qe and fast timing capability (e.g. ∼10 ms). these detectors are superior to those used in the first studies of polar qpos (e.g. larsson 1989, and references therein), which relied on pmt (photomultiplier tube)-based instruments. high time resolution photometry of mcvs have recently been carried out at salt, utilizing the newly installed (in 2012) berkeley visible image tube (bvit), a photon counting instrument using a microchannel plate (mcp) detectors (buckley et al., 2010, welsh et al. 2011). while not of particularly high qe, compared to a ccd, bvit is capable of time tagging photons to ∼50 ns, and is ideal for studying extremely fast variability (e.g. pulsars). short (typically ∼1 h) bvit observations have been made of several mcvs, but the only positive detection to date has been for the intermediate polar, ex hya, where a ∼100 s qpo (and possibly its harmonic), were detected (fig. 7). figure 7: a salt observations of ex hya using bvit which revealed a ∼100/50 s qpo. 136 observing cvs and lmxbs with salt:updates and recent results 3 salt spectroscopy of xss j12270-4859 figure 8: salt spectra of xss j12270-4859, averaged over ∼1 h on 4 different nights. the enigmatic fermi gamma ray source, xss j122704859 (e.g. bonnet-bidaud et al. 2012, and references therein), was the subject of a saao-eso observing campaign in march/april 2012, utilizing the ntt, salt and several smaller saao telescopes. spectroscopy was carried out with salt over 6 nights, contemporaneous with ntt spectroscopy. in addition, high speed u-band photometry and jhk imaging was also undertaken. xss j12270-4859 was first suggested to be an intermediate polar (butters et al. 2008), but this was not confirmed from follow-up suzaku and xmm observations. the system exhibits x-ray flares and dips, somewhat reminiscent of exo0748-676, but without any phase dependency and no spectral changes. the x-ray spectrum is also characterized by a weakly absorbed power law, with no cut-off up to 100 kev and no fe lines. the system has been suggested to be similar to a microquasar (e.g. cyg x-3, but it is not as variable in x-rays) or possibly a millisecond pulsar (e.g. psr 1023+0038), but no spin period has been detected to date. the salt spectra were obtained during ∼1 h tracks, with 300 s repeat exposures. they show significant changes, often over the timescale of an exposure, sometimes exhibiting weak emission lines of the balmer series, hei and heii, and other time showing balmer and other absorption features, as can be seen in fig. 8. radial velocity variations of the combined spectra indicate a possible ∼7 h orbital period, which is under investigation. the high speed photometry also shows variations on a similar timescale, but with periods of enhanced flickering possibly occurring at the same orbital phase. 4 future plans in 2014 it is planned to extend the salt observational work on cvs and related objects to include time resolved polarimetric imaging and spectropolarimetry. polarized continuum flux variations will be used to probe the cyclotron emission, for example using the stokes imaging technique (see potter et al. 2004). this will be combined with doppler and roche tomography and eclipse mapping to assist in building detailed models of mcvs, and may include using relevant particle or mhd codes. following the launch of the indian x-ray satellite, astrosat (in 2014), it is planned to begin coordinated observations using salt to undertake contemporaneous optical observations of mcvs, lmxbs and related objects. astrosat will have both, hard and soft x-ray instruments, the former with excellent sensitivity and energy range, plus a uv imaging telescope. adding such data will allow for a comprehensive multiwavelength analysis of these systems. 137 david a. h. buckley acknowledgement the work summarized in this paper represents a number of collaborative salt projects with various colleagues, including jean marc bonnet-bidaud, hannes breytenbach, domitilla de martino, marissa kotze, darragh o’donoghue and stephen potter, to name a few. the research of the author is supported by nrf rated researcher and incentive funding awards. the observations presented were carried out using the southern african large telescope. references [1] bonnet-bidaud, j.m., et al.: 2012, mem. s.a. it., 83, 742. [2] bridge, c.m., et al., 2004, mnras, 351, 1423. doi:10.1111/j.1365-2966.2004.07884.x [3] buckley, d.a.h., swart, g.p & meiring, j.g., 2006, proc. spie, 6267, 62670z. doi:10.1117/12.673750 [4] buckley, d.a.h., et al., 2010, poprc. spie, 7735, 77359-1. [5] butters, o.w., et al., 2008, a&a, 487, 271. [6] kotze, e. & potter, s.b., 2013, these proceedings. [7] larsson, s., 1989, a&a, 217, 146. [8] michaud, c., et al., 2012, mem. s.a. it., vol. 83, 665. [9] o’donoghue, d., et al., 2006, mnras, 372, 151. doi:10.1111/j.1365-2966.2006.10834.x [10] potter, s.b., et al., 2004, mnras, 348, 316. doi:10.1111/j.1365-2966.2004.07379.x [11] welsh, b., et al., 2011, iau symp. 285, 99. discussion paula szkody: can you give more information on the qpo in ex hya? is it seen in the lines or continuum? david buckley: the qpo was detected using salt and bvit with a broad-band r-filter, so includes both continuum and hα. the characteristic period was ∼100 s, or more likely, its harmonic. 138 http://dx.doi.org/10.1111/j.1365-2966.2004.07884.x http://dx.doi.org/10.1117/12.673750 http://dx.doi.org/10.1111/j.1365-2966.2006.10834.x http://dx.doi.org/10.1111/j.1365-2966.2004.07379.x introduction high speed photometry with salticam time resolved spectroscopy with rss time-resolved studies of polars light curves of eclipsing polars spectra of eclipsing polars qpos in magnetic cvs salt spectroscopy of xss j12270-4859 future plans acta polytechnica ctu proceedings doi:10.14311/app.2016.3.0056 acta polytechnica ctu proceedings 3:56–59, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app determination of thermal response of carrara and sneznikovsky marble used as building material veronika petráňováa,∗, jaroslav valacha, alberto vianib, marta peréz estébanezb a institute of theoretical and applied mechanics as cr, v.v.i., prosecka 76, prague, czech republic b institute of theoretical and applied mechanics as cr, v.v.i., centre of excellence teläŋ, batelovska 485, teläŋ, czech republic ∗ corresponding author: petranova@itam.cas.cz abstract. physical weathering of marble, widely used as a cladding material on buildings, is one of the most common damaging mechanism caused by anisotropic thermal expansion of calcite grains. the extent of marble deterioration depends mainly on stone fabric and texture. dry cuboids of carrara marble and marble from dolni morava quarry were subjected to microscopic analysis and thermal cycling, to determine the thermal expansion related to stone fabric and predominant lattice orientation of grains (i.e. texture). keywords: marble, anisotropic thermal expansion, thermal dilatation. 1. introduction marble has been predetermined as building and decorative natural stone since antiquity because of its good workability and unique visual appearance. these properties are related to the composition of carbonate sediments and to the nature and intensity of the recrystallization process under the regional metamorphosis conditions. marble is considerably vulnerable to both chemical and physical weathering by reason that this type of stone predominantly consists of carbonate minerals calcite caco3 and dolomite camg(co3)2. periodic temperature variations, together with changing in moisture can cause serious damage to the stone structure, finally leading to the complete stone decay. the enormous sensitivity of marble to variations in temperature originates in the thermal response of calcite crystals. while the dolomite crystals subjected to thermal cycling expand only, the calcite crystals show anisotropic thermal dilatation introduced by thermal cycles, i.e., it expands along c axis during heating and contracts in other directions. however, cooling of calcite crystals leads to the opposite effect, i.e., contraction along the c axis and expansion in the other directions as is illustrated in figure 1. both mechanisms are considered as the major cause of creation and propagation of cracks along the grain boundaries in the stone. thermal expansion can be expressed using the thermal expansion coefficient α, describing the length change per unit of temperature. the coefficient value depends on the considered temperature interval. to quantify the extent of stone elongation, the residual strain ε is more suitable [1]. the preferred lattice orientation of calcite grains i.e. texture is one of the most important stone characteristics, essentially influencing thermal response in different spatial directions. marble with strong texture is generally more vulnerable to thermal weathering, which can be enhanced by significant differences between the α values along the cand a-axis of individual calcite grains [2]. thermal expansion of marble is measurable at low temperatures enabling simulation the climate conditions in the central europe. nevertheless, experimentally obtained thermal dilatation values often deviated from calculation based on theoretical models considering only the texture variations in a marble. another important parameters are grain shapes, grain sizes and the type of grain boundaries because of the strong influence on the rate of stone decay. a certain directional relationship between the shape preferred orientation (spo) of calcite grains and their lattice preferred orientation (lpo) can extensively intensify the thermal response of marble. for example, marble with lpo parallel to spo exhibits a strong thermomechanical response because of the large concentration of maximum principal stress in the direction of shape elongation. thermal stresses during heating can initiate the formation of new cracks or widening of preexisting cracks or pores. microcracking formation can also be influenced by grain size since the level of marble decay is also connected with the number of adjacent grains and with the grain boundaries [3–5]. however, thermal response and consequently the rate of physical deterioration of marble depends also on other stone characteristics, including the ratio of calcite and dolomite, moisture content, porosity and pore size distribution of the investigated marble [6]. depending on all the mentioned stone characteristics, the thermal response of marble after cooling down to room temperature can be determined as isotropic or anisotropic, with or without residual strain [1]. 56 http://dx.doi.org/10.14311/app.2016.3.0056 http://ojs.cvut.cz/ojs/index.php/app vol. 3/2016 thermal response of carrara and sneznikovsky marbles figure 1. anisotropic thermal expansion of calcite crystals. adopted from [1]. 2. materials and methods testing of the thermal response was performed on two structurally different marble types. the first one from the carrara area in northern italy was chosen for its simple fabric. the second one sneznikovsky marble was taken from dolni morava quarry in the czech republic. the texture as well as the shape and size of grains was investigated by optical microscopy and electron back-scattered diffraction (ebsd) method in a scanning electron microscope (sem, fei quanta 450, fei corp., usa). for the sem-ebsd investigations, slide specimens of marble were coated with a thin layer of carbon to protect against specimen charging. to evaluate the dependence of dilatation on the sample’s microstructure, two pairs of perpendicular cuboids a-a, b-a, c-1 and c-4 (6 x 6 x 20 mm) were prepared from the original marble blocks. the orientation of the cuboid samples is depicted in figure 2. thermal expansion measurements were performed using a vertical dilatometer (l75 pt linseis corp., germany). the specimen elongation was measured after each 1 °c step. the cuboid samples were subjected to heating and cooling cycles, ranging in temperature from -40 to 100 °c. the cycles were repeated 7 times for specimens a-a, b-a and c-1 and 5 times for specimen c-4. the temperature interval was gradually increased for the a-a, b-a and c-1 specimens. the interval for specimen c-4 remained stable in all 5 cycles (from -40 to 100 °c). the values for the thermal expansion coefficient α values were calculated using equation (1). the length change in 4l was determined within a temperature interval 4t , from 18 °c to the maximum temperature in the considered cycle, i.e. for cycle 1, the maximum temperature was 33 °c, whereas for cycle 7, it was 100 °c. to determine α, only a positive temperature range was selected, because the results from the range below the freezing point were not reliable. α = 4l l4 t (1) figure 2. orientation of cuboid specimens, a-a and b-a is sneznikovsky marble and c-1 and c-4 is carrara marble. the symbols and their physical meanings are listed at the end of the paper. 3. experimental results based on optical and sem-ebsd observations, the carrara marble exhibits a weak texture in both directions (x-y and x-z). specimens c-1 and c-4 contain calcite grains with a nearly uniform size of around 0.3 mm with straight polygonal grain boundaries and no shape preferred orientation. contrary to carrara, sneznikovsky marble exhibits cracking, predominantly on planes parallel to the x-y plane. the microfabric of 57 v. petráňová, j. valach, a. viani, m. peréz estébanez acta polytechnica ctu proceedings figure 3. a microfabric of investigated samples, b orientation of calcite grains in b-a sample. figure 4. dependence of relative extension on the temperature. the investigated marble types is illustrated in figure 3. the size of the calcite grains in the a-a and b-a specimens is not uniform; grains in sizes up to 4 mm with sutured grain boundaries can be found. as in the carrara specimen, both perpendicular planes of sneznikovsky marble contain grains with no shape preferred orientation. the elongation of the cuboid specimens was expressed as relative extension, i.e. percentage difference between 4t for each temperature step and original length of the specimen. the highest relative extension of 0.18% was observed in c-4 at 100 °c in the first cycle. in the other cycles (2-5) the value was equal to 0.16%. specimen c-1 showed an increasing trend over the temperature and reached its maximum relative extension of 0.14% at 100 °c. regarding the coefficient α, specimen c-4 also showed the highest average value of 12.5 · 10−6k−1. specimen c-1 achieved the most significant difference in α, varying from 3.9 · 10−6k−1 to 11.3 · 10−6k−1. the results are illustrated in the figures 4 and 5. the first cycle of the measurements performed on the specimen c-1 was excluded from the results. values obtained from the first cycle performed in c-1 specimen weren’t included to the results. during the 7 cycles in specimens a-a and b-a relative elongation also showed an increasing trend, but the maximum values were more different than in the carrara marble. at 100 °c in cycle 7, the relative figure 5. thermal expansion coefficient α of investigated specimens, loaded in the 18-100 °c temperature interval. the value marked "a" represents an average value of α determined by [7] on large set of marble specimens. extension in specimen a-a was equal to 0.15% while in b-a it was just 0.10%. the α coefficients determined for the sneznikovsky marble were not as variable as in the carrara type. in the a-a sample, α reached an average value of 10 · 10−6k−1 and in the b-a sample of 5 · 10−6k−1. based on the relative extension difference between corresponding cycles, an α variation of 5 · 10−6k−1 was determined, which can be attributed to the observed anisotropy in the sneznikovsky mar58 vol. 3/2016 thermal response of carrara and sneznikovsky marbles ble, i.e. the x-y orientated plane in specimen a-a was more fissured. 4. conclusions it can be concluded that simultaneous microscopic and dilatometry investigations can help in elucidation of thermally induced degradation of marbles. based on the results, the thermal response and generation of damage caused by accumulation of residual strains related to stone fabric and texture in investigated marbles will be determined on a larger set of perpendicular specimens, heated and cooled in the positive range of temperatures (i.e. from 20 to 100 °c). investigations carried out on both specimen types reveal an increasing rate of thermal expansion with increasing temperatures. in presence of a temperature gradient, this characteristic can contribute to the well known bowing effect on marble slabs. list of symbols α thermal expansion coefficient [ k−1] 4l difference between the actual specimen length and the length at the room temperature [m] l length of the specimen at the room temperature [m] 4t temperature difference between the actual and the room temperature [k] acknowledgements the research has been supported by czech science foundation (project no. p105/12/g059). references [1] m. steiger, a. charola. weathering and deterioration. in the stone in architecture, chap. 4., springer-verlag, 2011. doi:10.1007/978-3-642-14475-2_4 [2] s. siegesmund, k. ullemeyer, t. weiss, e.k. tschegg. physical weathering of marbles caused by anisotropic thermal expansion. inter j earth sci 89(1):170-182, 2000. [3] v. shushakova, e.r. fuller jr, s. siegesmund. influence of shape fabric and crystal texture on marble degradation phenomena:simulations. env earth sci 63(7-8):1587-1601, 2011. doi:10.1007/s12665-010-0744-7 [4] b. leiss, t. weiss. fabric anisotropy and its influence on physical weathering of different tyes of carrara marbles. j struct geol 22(11-12):1737-1745, 2000. [5] u. akesson, j.e. lindqvist, b. schouenborg, b. grelk. relationship between microstructure and bowing properties of calcite marble claddings. bull eng geol env 65(1):73-79, 2006. [6] e. cantisani, e. pecchioni, f. fratini, c.a. garzonio, p. malesani, g. molli. thermal stress in the apuan marbles: relationship between microstructure and petrophysical properties characteristics. inter j rock mech min sci 46(1):128-137, 2009. doi:10.1016/j.ijrmms.2008.06.005 [7] a. zeisig, s. siegesmund, t. weiss. thermal expansion and its control on the durability of marbles. in the natural stone, weathering phenomena, conservation strategies and case studies, chap. 2., the geological society of london, 2002. 59 http://dx.doi.org/10.1007/978-3-642-14475-2_4 http://dx.doi.org/10.1007/s12665-010-0744-7 http://dx.doi.org/10.1016/j.ijrmms.2008.06.005 acta polytechnica ctu proceedings 3:56–59, 2016 1 introduction 2 materials and methods 3 experimental results 4 conclusions list of symbols acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.13.0016 acta polytechnica ctu proceedings 13:16–19, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app parallel approach to solve of the direct solution of large sparse systems of linear equations michal bošanský∗, bořek patzák czech technical university in prague, faculty of civil engineering, thákurova 7, 166 29 prague 6, czech republic ∗ corresponding author: michal.bosansky@fsv.cvut.cz abstract. the paper deals with parallel approach for the numerical solution of large, sparse, non-symmetric systems of linear equations, that can be part of any finite element software. in this contribution, the differences between the sequential and parallel solution are highlighted and the approach to efficiently interface with distributed memory version of superlu solver is described. keywords: linear equation solver, domain, parallelization, threads, distributed memory, communication. 1. introduction many engineering problems lead to large-scale problems. the solution of these problems is being limited by available resources. in many cases, the parallel and distributed computing paradigms can be successfully used to enable solution of large and complex problems, which are not possible to solve on single machine with one processing unit [1]. the traditional serial computers permit to run simulation codes only sequentially and often have limited memory. parallelization can significantly reduce computational time by more efficient use of modern hardware. any parallel algorithm is based on idea of the partitioning the work into the set of smaller task which can be solved concurrently by the simultaneous use of multiple computing resources. parallel computers can be classified, for example, by type of memory architecture. the shared, distributed, and hybrid memory systems [2] exist. in the shared memory system, the main memory with a global address space is shared between all processing units which can directly address and access the same logical memory. the global memory significantly facilitates the design of parallel program, but the memory bus performance is limiting factor for scalability with increasing number of processing units. in distributed memory systems, the memory is physically distributed to individual processing units and there is no global address space. when a processor needs to access data on another processor, it is usually the task of the programmer to explicitly define how and when data is communicated. the cost of communication compared to local memory access can be very high, on the other hand, the advantage is that the overall memory is scalable with increasing number of processors. hybrid systems combine the features of shared and distributed memory system, providing global, shared memory for reasonably small number of processing units that are combined into the distributed memory system. the design of parallel algorithms requires the partitioning of the problem into a set of tasks, that can be processed concurrently. the partitioning of the problem can be either fixed (static load balancing) or can change during the solution (dynamic load balancing) [3]. the latter option is often necessary to achieve a good load balancing of individual processors and consequently also reasonable scalability. the scalability of computation is often regarded as one of the most important goals of parallel computing. the parallel algorithm is considered as scalable, when by using increasing number of processing threads, the execution time is monotonically decreasing, ideally in a linear trend. however, when individual computing threads are mutually dependent, the ideal scalability is difficult to obtain due to the overhead of parallel algorithm (necessary synchronization and communication between threads that is not present in serial code) and due to the fact that some parts of the overall algorithm are essentially serial. in addition to the achieved speedup, the parallel computing allows to solve large, complex problems that do not fit into a single, even well equipped machine. the superlu library provides parallel implementation of the direct solver [4]. it provides serial, multithreaded (shared-memory), and distributed memory version. the implementation and performance of the multithreaded version has been reported by the authors in [5, 6]. in this papers, the focus is on distributed version of superlu based on message passing interface (mpi) [7]. numerical modeling using high performance computers brings in new opportunities. many engineering problems lead to solution of sparse linear system of equations. this is also the case of the finite element method (fem) which is used here as an representative example. in fem the differential equations are converted to the algebraic system of equations by using variational methods with the help of decomposition of the problem domain into sub-domains called elements 16 http://dx.doi.org/10.14311/app.2017.13.0016 http://ojs.cvut.cz/ojs/index.php/app vol. 13/2017 direct solution of large sparse systems of linear equations 68 0 2 11 00 0 3 5 09 2 6 0 04 0 0 13 17 0 0 3 k = k_nzval 8 6 2 11 3 5 9 2 6 4 13 7 1 3 k_colind 1 2 4 5 4 5 1 3 4 1 5 1 2 3 k_row_ptr 1 5 7 10 12 21 3 4 5 1 2 3 4 5 figure 1. the compressed row format of matrix schema. and smart choice of interpolation functions. for linear elasticity problem, considered here, the resulting algebraic equations, represent the discrete equilibrium equations at nodes of the computational mesh k ∗ r = f, (1) where k is the global stiffness matrix, f is global vector of external forces, and r is vector of unknown displacements. one of the key feature of the fem is that the stiffness matrix is typically positive definite, symmetric matrix with sparse structure, which is a consequence of using interpolation and test functions with limited nonzero support. the efficient algorithm for solving linear system must exploit the symmetry and sparse structure, by saving considerable memory and cpu resources. there exist number of different storage schemes for sparse matrices. the most widely used are skyline, compressed row, and compress column formats. in this contribution, the compressed row format will be used. this choice comes from superlu library, which requires the sparse matrix in this format on input. in the compressed row format, only nonzero entries of the sparse matrix are stored in one dimensional array. additional integer array is needed to store column indices of the stored values. in practical implementation, the one dimensional arrays storing nonzero values are merged together into a single array containing all nonzero entries, row by row. the same applies for arrays of column indices. an additional array with size equal to number of rows is needed to point to the beginning of each row record, see fig. 1. 2. implementation superlu interface as noted already in the previous section, the distributed memory programming model does not provide global address space and global memory accessible by all processing nodes, but the memory is distributed among the processing units. for large problems, it is therefore essential to establish a distributed representation of the sparse matrix. this feature is also supported by superlu library, allowing the user to split the global sparse matrix stored in comprow format into blocks, representing compressed row storage for consequent, non-overlapping groups of rows, which are distributed across computing nodes. we assume, that the decomposition of the discretized problem domain has been established and individual, non-overlapping sub domains (partitions) are assigned to and stored locally on individual computing nodes. the so called node-cut strategy is assumed, where the cut dividing the problem domain runs through the nodes. nodes on mutual partition boundaries are called shared nodes, the nodes inside individual partitions are so-called local nodes. each processing node is responsible for assembling its contribution to the global system matrix by summing up the contributions from individual elements. to minimize the communication, it is natural that each processing node will assemble and maintain in its local memory the block of global stiffness matrix rows corresponding to unknowns on its partition. this is uniquely defined for local nodes, which are exclusively shared by local elements on individual partitions. for shared nodes, which are shared by elements from multiple partitions, the ownership has to be defined. in this work, the partition with lowest rank sharing the shared node is the owner of shared node and thus responsible of maintaining the corresponding row entry of the global stiffness matrix. it is clear that for shared nodes, the contributions to the corresponding row have to be received from partitions sharing particular node. the assembly process requires to establish global, unique numbering of equations across computing nodes in addition to the local numbering on individual partitions. the assembly process of the global, distributed system matrix requires basically two steps: set up of data structures required to store the block of compressed row records on individual partitions and the assembly process itself based on localization of individual element contributions into global equilibrium equations according to their connectivity. 2.1. initialization of data structures for distributed matrix this phase should determine the required size of arrays used to store all nonzero entries of the global matrix. the nonzero contributions of each element can be identified from element code numbers. the code numbers represent simultaneously the numbering of equilibrium equations and numbering of corresponding unknowns. the individual values in the stiffness matrix represent nodal forces caused by corresponding unit displacement. the entry in element stiffness matrix representing the nodal force contributing to k-th equilibrium equation and being multiplied by displacement located in global displacement vector at l-th position, should be added to position (k,l) in the global matrix. by assuming that element contributions are full matrices, one can initialize the nonzero structure of the global stiffness matrix using element 17 michal bošanský, bořek patzák acta polytechnica ctu proceedings 1 (0 ,1 ) 1 2 (2 ,3 ) 5 (8 ,9 ) 3 (4 ,5 ) 4 (6 ,7 ) 6 (1 0, 11 ) 7 (1 2, 13 ) 8 (1 4, 15 ) 0 2 3 4 5 6 7 8 9 10 11 12 13 14 15 1 0 2 3 4 5 6 7 8 9 10 11 12 13 14 15 g # 1 #2 g g # 3 2 5 3 4 6 7 8 # 1 # 2 # 3 4 6 42 # 2 6 k# 1 k# 2 k# 3 -n od e -s ha re d no de # 3 # 3 # 3 # 2 # 2 4 1 f1 f2 10 2 3 4 5 6 7 1 0 2 3 4 5 6 7 32 8 9 6 7 10 11 3 2 8 9 6 7 10 11 76 10 11 12 13 14 15 7 6 10 11 12 13 14 15 { { p1 p2 p3 figure 2. example of simple problem consisting of three elements distributed into different computing nodes, illustrating the global sparse matrix structure and its distribution. 18 vol. 13/2017 direct solution of large sparse systems of linear equations code numbers. in distributed case, each partition is responsible for initializing and prealocating its block structure of compressed rows records. in case of the compressed row storage, the number of nonzero entries in each row has to be determined together with corresponding nonzero column positions of the individual entries. each processing node is responsible for initialization and assembly of the assigned block of rows. this block is composed from local contributions, as well as from shared node contributions from neighboring partitions. therefore, the overall initialization can be divided into (i) local stage, where the local contributions to nonzero pattern are identified (from the partition elements), and (ii) communication stage, where contributions from neighboring partitions are received for locally maintained rows, corresponding to equilibrium equations for shared nodes. any partition has to therefore keep its locally maintained block of compressed rows and also block compressed rows corresponding to shared nodes not being locally maintained. these two blocks can be stored separately. in the initial stage, the block structure is initialized on every partition using only the contributions from local elements. the row entries, that correspond to the shared nodes which are not locally maintained are then communicated (send) to the corresponding partition maintaining corresponding row. after the sending the data, the contributions from neighboring partitions are received containing the contributions to the locally maintained shared equations. non-blocking communication [8] is used to send/receive the contributions. non-blocking communication allows to utilize the potential overlap of communication and computation, which is utilized in the actual implementation. after finishing the communication stage, each partition has fully initialized data structure for locally maintained block of rows. 2.2. assembly of the global distributed matrix after finishing the initialization step, in which memory has been allocated for every non zero entry of the global distributed stiffness matrix, one can proceed with the actual assembly of the matrix from the element contributions. this is done in a similar fashion to the previous step. on each partition the contributions from local elements are assembled. then, the rows corresponding to shared nodes not being locally maintained have to be sent to the partition maintaining corresponding row. finally, each partition has to receive remote contribution to the locally maintained rows of shared nodes. this process is illustrated on fig. 2. in this example, the problem is composed of three elements (corresponding to sub domains as well) and eight nodes, from which five are local on individual partitions and three nodes are shared. 2.3. assembly of the global right hand side the process of assembling the global right hand side vector is very similar to the process of assembling the stiffness matrix, but in many aspects is simpler, do to the assembly of local vector contributions. the global vector is again distributed among partitions, the distribution corresponds to the distribution of matrix rows. the contributions from local elements are assembled first, then those corresponding to rows maintained on remote partitions are communicated and contributions from neighbors are received and entries updated. by finishing the steps described above, the distributed sparse matrix, represented by locally maintained blocks of row entries on individual partitions, can be directly passed into superlu routines. 3. conclusions in this work the algorithm of assembling the distributed sparse matrix in row-column format is described, in order to develop the interface to the distributed superlu solver. the evaluation of the performance and scalability is the subject of ongoing work. the authors also aim to compare the efficiency of the distributed solver to the efficiency of the multithreaded superlu version. acknowledgements this work was supported by the grant agency of the czech technical university in prague, grant no. sgs16/038/ohk1/1t/11 – advanced algorithms for numerical modeling in mechanics of structures and materials. references [1] b. patzak. parallel computations in structural mechanics. české vysoké učení technické v praze, 2010. [2] c. hufhes, t. hughes. parallel and distributed programming using c++. pearson education, 2003. [3] b. patzak, d. rypl. parallel adaptive finite element computations with dynamic load balancing. proceedings of the first international conference on parallel, distributed and grid computing for engineering 2009. [4] x. s. li, j. w. demmel, j. r. gilbert, et al. superlu users‘ guide program interface. http://crd.lbl.gov/ xiaoye/superlu/, september 1999. [5] m. bosansky, b. patzak. evaluation of different approaches to solution of the direct solution of large, sparse systems of linear equations. advanced materials research 1144(1144):97–101, 2016. [6] m. bosansky, b. patzak. on parallelization of linear system equation solver in finite element software. engineering mechanics 2017 1(1):206–209, 2017. [7] p. s. pacheco. a user‘s guide to mpi. univ. of san francisco, 1997. [8] t. saif, m. parashar. unferstanding the behavior and performance of non-blocking communications in mpi. department of electrical and computer engineering, rutgers university, 2002. 19 acta polytechnica ctu proceedings 13:16–19, 2017 1 introduction 2 implementation superlu interface 2.1 initialization of data structures for distributed matrix 2.2 assembly of the global distributed matrix 2.3 assembly of the global right hand side 3 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0064 acta polytechnica ctu proceedings 7:64–68, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app experimental identification of an elasto-mechanical multi-degree-of-freedom-system using stochastic signals simon schleiter∗, okyay altay, sven klinkel rwth aachen university, faculty of civil engineering, chair of structural analysis and dynamics, mies-van-der-rohe-str. 1, 52074 aachen,germany ∗ corresponding author: schleiter@lbb.rwth-aachen.de abstract. the determination of dynamic parameters are the central points of the system identification of civil engineering structures under dynamic loading. this paper first gives a brief summary of the recent developments of the system identification methods in civil engineering and describes mathematical models, which enable the identification of the necessary parameters using only stochastic input signals. relevant methods for this identification use frequency domain decomposition (fdd), autoregressive moving average models (arma) and the autoregressive models with exogenous input (arx). in a first step an elasto-mechanical mdof-system is numerically modeled using fem and afterwards tested numerically by above mentioned identification methods using stochastic signals. during the second campaign, dynamic measurements are conducted experimentally on a real 7-story rc-building with ambient signal input using sensors. the results are successfully for the relevant system identification methods. keywords: system identification, civil engineering structures, stochastic signal, ambient signal, fdd, arma, arx. 1. introduction starting with the 19th century, aesthetic and economic challenges have induced an impulsive interest on the design of the dynamic behavior of civil engineering structures, as the new constructions are getting higher and slenderer. hence the calculation of relevant system parameters, such as natural frequencies, damping ratios and modal shapes, become more important. in many cases it is necessary to identify system parameters after construction, so that the use of experimental methods becomes essential to get the current behavior. generally, all experimental methods can be distinguished between either time or frequency domain. the investigated models in this paper are the frequency domain decomposition (fdd) in frequency domain, autoregressive moving average models (arma) and the autoregressive models with exogenous input (arx), both in time domain. to describe the system response accurately, the output data should be known as well as the excitation data. but in most cases the determination of the excitation data is very costly for civil engineering structures. for instance, the detection of the wind induced excitation or microseism requires a simultaneous measurement using several sensors. whereas the arx-model is using excitation data in the calculation, the arma-model, as well as the fdd are neglecting any excitation signal. in this case an assumption must be made. the excitation may only be a broad band excitation, otherwise there is no interpretation of the results possible. especially for this case the fdd has been developed by brincker [1]. for complex structures the use of arma-model and fdd are recommendable and mostly unavoidable. a numerical implementation of all presented models is possible and is executed in this paper. results are validated on the basis of two examples: one on a numerically simulated 4-dof system and the other one on an experimentally analyzed 7-story real structure. aim of these applications is to show upcoming problems for the presented system identification methods and potential for further research on this topic. 2. system identification methods: fdd, arma, arx the frequency domain method (fdd) is based on the spectral power density, which can be used to describe signals in frequency domain. it is approved that the spectral density of the excitation signal (gxx) and of the response signal (gyy) can be decomposed by the frequency response function (h), all terms depend on the circular natural frequency and the exponent ∗ illustrates the complex conjugate tensor as t represents the transpose, as follows: gyy(ω) = h∗(ω)gxx(ω)ht (ω) (1) using some mathematical transformations and the assumption of broad band excited systems a single value decomposition of this formulation yields the modal shapes and the natural frequencies of the system. for further information the lecture of brincker [1] is recommended. damping ratios can be calculated 64 http://dx.doi.org/10.14311/app.2017.7.0064 http://ojs.cvut.cz/ojs/index.php/app vol. 7/2017 example of an article with a long title figure 1. structure of the 4-dof system. by extensions of this system, such as enhanced fdd (efdd) or curve fitting fdd (cfdd) explained in brincker et al. [2] and jacobsen et al. [3]. based on the time domain, the aim of armaand arx-models is to recreate the time signal by correlation coefficients. this correlation coefficients or parameters can describe the complete system behavior with the assumption of periodic behavior. additionally, it is possible to create the frequency response function (frf) for each signal by knowing these parameters. using this frf, working from now on in the frequency domain, the modal shapes can be calculated by an algorithm as well as the natural frequencies. damping ratios are calculated by the so called half power method, mentioned in he et al. [4], also using the above-mentioned frf. a detailed overview of these and more models based on time domain is given in ljung [5] and a closer explanation of the functionality of the frf in he et al. [4]. 3. application examples to validate these methods, a numerical application of a 4-dof system (see figure 1) was conducted. for this a cantilever beam was simulated in a fe-program with four similar masses distributed in the same distance to each other. to simulate a measurement, ambient input signals were generated and afterwards used as excitation signals for the structure. by using the numerical response signals, the methods were applied. as a validation of the methods, an identification in the fe-program itself using modal analysis gave the natural frequencies and the damping ratio shown in table 1 and 2, illustrated as fe-values. the results of the fe-calculation (modal analysis) are in good agreement to the used identification methods (arma, arx, fdd). the modal shapes are shown in figure 2, where the -1 -0.5 0 0.5 1 0 1 2 3 4 d eg re e of f re ed om 1. eigenmode arma fe, arx, fdd -1 -0.5 0 0.5 1 0 1 2 3 4 d eg re e of f re ed om 2. eigenmode arma fe, arx, fdd -1 -0.5 0 0.5 1 0 1 2 3 4 d eg re e of f re ed om 3. eigenmode arma fe, arx, fdd -1 -0.5 0 0.5 1 0 1 2 3 4 d eg re e of f re ed om 4. eigenmode arma fe, arx, fdd figure 2. comparison of the modal shapes of the 4-dof system. reference modal shapes can be compared with the modal shapes of the different applications. except the arma-model the applications give exactly the same results compared to the fe-reference values. in contrast a certain percentile difference for the armamodel can be realized. it only can describe the modal shapes in a rough shape and could only be accepted for preliminary design purposes. in a second application a first plausibility check of fdd has been conducted experimentally, based on real measurement data. in this example a 7-story rc-building (see figure 3) is investigated. the measurement data is acquired by using three identical bi-directional geophones, measuring the velocity (sensitivity of 100 v/m/s).the measurement goal was the estimation of natural frequencies of the bending mode shapes. therefore the sensors were located in the sixth 65 s. schleiter, o. altay, s. klinkel acta polytechnica ctu proceedings natural frequency [hz] fe fdd arx arma 1. eigenmode 1,2 1,3 1,2 1,2 2. eigenmode 7,7 8,0 7,7 7,7 3. eigenmode 19,3 20,1 19,3 19,3 4. eigenmode 28,4 29,7 28,4 28,5 table 1. comparison of the natural frequencies of the 4-dof system. damping ratio [%] fe fdd arx arma 1. eigenmode 1,0 1,0 0,9 2. eigenmode 1,1 1,5 1,1 1,1 3. eigenmode 1,9 1,9 2,2 2,1 4. eigenmode 2,5 2,5 2,7 2,7 note: the used algorithm according to the fdd makes a determination of the damping ratio for low frequencies impossible and thus for the first eigenmode. table 2. comparison of the damping ratios of the 4-dof system. figure 3. experimentally investigated 7-story rcbuilding. [6] story on one axis and a distribution over the short building side was not necessary (see figure 4). a detailed system identification only would be possible by using more measurement points. in this application the fdd method only investigates the applicability for complex civil structures and possible upcoming problems. load-bearing walls of the structure are illustrated in red in figure 4. an interaction of the x-direction with the ydirection is expectable for some modes, but for the sake of simplicity the modes are investigated separate for each direction. table 3 shows the results of natural frequencies and damping ratios for the x-direction and table 4 according to the y-direction. the results show that there is an interaction caused by non-symmetry and varied stiffness contribution between the second modes of xand y-direction. the significant variation of the damping ratio down to 0.5 % for the second eigenmode can be interpreted as that it is probably not a bending mode shape like the first and the third eigenmodes. the identified damping ratios are obviously lower than the standard values for rc-buildings indicating the drawbacks of the presented methods for the estimation of the strucnatural frequency [hz] damping ratio [%] 1. eigenmode 1,9 1,2 2. eigenmode 2,8 1,3 table 3. natural frequencies and damping ratios of the x-direction of the rc-building. natural frequency [hz] damping ratio [%] 1. eigenmode 2,1 1,2 2. eigenmode 2,6 0,5 3. eigenmode 4,3 2,0 table 4. natural frequencies and damping ratios of the y-direction of the rc-building. tural damping. since these eigenmodes are decoupled the damping ratio can be completely different compared to the bending eigenmodes. at this stage using the measurement results of the sixth floor, only a preliminary general identification of the eigenmodes in y-direction can be concluded, as in x-direction all measurement points lie on the same axis. a more sophisticated system identification can be done by including additional measurement points, also in vertical direction. the results of the modal shapes by application of the fdd are shown in figure 57. it can be seen, that the first and the third modes both can be interpreted as the bending modes and thus the second mode shows a torsional behavior. 66 vol. 7/2017 example of an article with a long title y staircase corridor offices lecture hall staircaseoffices offices offices officesrestrooms x y mp 1 xmp 2 mp 3 x y 9,00m29,60m44,70m 10,00m 7,60m figure 4. floor plan of the story 6 of the rc-building. direction of motion figure 5. 1st modal shapes of 7-story rc-building identified by using fdd. direction of motion figure 6. 2nd modal shapes of 7-story rc-building identified by using fdd. 4. conclusion in this paper different system identification methods for civil engineering are introduced and verified both on numerical and experimental examples. the three presented models are the frequency domain decomposition (fdd), the autoregressive moving average models (arma) and the autoregressive models with exogenous input (arx), which either use the time domain or the frequency domain. special attention is paid to the type and existence of the excitation signal, which has an influence on the models and the accudirection of motion figure 7. 3rd modal shapes of 7-story rc-building identified by using fdd. racy of the results. it is found that the arma-model achieves less exact results than other methods, so that they should be preferred, if they are applicable. the first validation example presents the system identification of a numerical 4-dof system model, yielding good agreement with the fe-values. second example shows the results of an experimental investigation carried out on the 6th floor of a 7-story rc-building, which allows a preliminary identification of its behavior. 5. future work in order to increase the applicability of the system identification methods for civil engineering structures some further research goals need to be accomplished. the algorithms used so far are valid for simple structures without considering the interaction of multiple directions. for real structure applications these methods should be transferred to complex models by modifying the algorithms. a further innovative approach would be the stepwise investigation of a building, e.g. ambient system responses are measured for several points on separate time windows. the time dependence of the measured data can be corrected by using signal processing methods. hence compared to other methods the "incremental identification method" (iim) is a low-cost method, which needs a less extensive measurement preparation by using only one sensor with a numerically affordable data evaluation algorithm. 67 s. schleiter, o. altay, s. klinkel acta polytechnica ctu proceedings acknowledgements the authors gratefully acknowledge the financial support of the daimler and benz foundation. references [1] r. brincker, l. zhang, p. andersen. modal identification from ambient responses using frequency domain decomposition. proc of the int modal analysis conf imac xviii 2000. [2] r. brincker, c. e. ventura, p. andersen. damping estimation by frequency domain decomposition. proc of the int modal analysis conf imac xviv 2001. [3] n.-j. jacobsen, p. andersen, r. brincker. applications of frequency domain curve-fitting in the efdd technique. proc of the int modal analysis conf imac xxvi 2008. [4] j. he, z.-f. fu. modal analysis. butterworth heinemann, oxford, 2001. [5] l. ljung. system identification. prentice hall, new jersey, 1987. [6] rwth aachen university. 68 acta polytechnica ctu proceedings 7:64–68, 2017 1 introduction 2 system identification methods: fdd, arma, arx 3 application examples 4 conclusion 5 future work acknowledgements references acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0089 acta polytechnica ctu proceedings 4:89–96, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app evaluation metrics applied to accident tolerant fuel cladding concepts for vver reactors martin ševečeka,b,∗, mojmír valachc a department of nuclear reactors, faculty of nuclear sciences and physical engineering, czech technical university in prague, v holešovičkách 2, praha 8, czech republic b alvel a.s., opletalova 37, praha 1, czech republic c ujv řež, a.s., department of severe accidents and thermomechanics, nuclear power and safety division, hlavní 130, řež, 250 68 husinec, czech republic ∗ corresponding author: martin.sevecek@fjfi.cvut.cz abstract. enhancing the accident tolerance of lwrs became a topic of high interest in many countries after the accidents at fukushima-daiichi. fuel systems that can tolerate a severe accident for a longer time period are referred as accident tolerant fuels (atf). development of a new atf fuel system requires evaluation, characterization and prioritization since many concepts have been investigated during the first development phase. for that reason, evaluation metrics have to be defined, constraints and attributes of each atf concept have to be studied and finally rating of concepts presented. this paper summarizes evaluation metrics for atf cladding with a focus on vver reactor types. fundamental attributes and evaluation baseline was defined together with illustrative scenarios of severe accidents for modeling purposes and differences between pwr design and vver design. keywords: nuclear fuel, accident tolerant fuel, evaluation metrics, lwr, vver. 1. introduction after the events at the fukushima daiichi npp, enhancing the accident tolerance of lwrs became a topic of high interest in many countries. the goal of accident tolerant fuel (atf) development is to develop alternative fuels to further enhance the safety, competitiveness, and economics of nuclear power. the world’s leader in atf development are the u.s., where in 2012, the congress directed to doe to: • develop enhanced fuels and cladding for lwrs to improve safety in the event of accidents in the reactor or spent fuel pools. • emphasize and fund activities aimed at the development and near-term qualification of meltdownresistant atf that would enhance the safety of present and future generations of lwrs. • create a plan for development of meltdown-resistant fuels leading to reactor testing and utilization by 2020. other countries (e.g. france, south korea, china) have been conducting their own atf research with similar goals. recently, russia introduced its plan for atf development with a focus on vver reactors. activities related to the atf development are also coordinated by international organizations as iaea or oecd/nea. the initial effort is focused on applications in operating lwr reactors (pwr, bwr, and vver). the goal set by the u.s. or south korea is to insert a lead test assembly (lta) into a commercial reactor by 2022. other countries including russia or the czech republic have not defined their specific goals, yet. this paper summarizes an evaluation methodology, proposed set of metrics, related tests and illustrative accident scenarios for the evaluation of vver atf cladding concepts. the metrics are based on the detailed evaluation approach proposed in the [1], with an emphasis given on the fuel cladding, vver reactors, and their departures from standard pwr reactor design. the evaluation methodology will be applied to assess each atf cladding concept relative to the current vver fuel system and will be described in details in future technical report. 1.1. atf definition atf fuels are according to the oecd/nea [2] defined as fuels that can tolerate a severe accident in the reactor core for a considerably longer time period than the current uo2 – zr alloy fuel system, while maintaining or improving the fuel performance during normal operations and operational transients. 1.2. coping time each concept will be evaluated besides other characteristics based on its ability to increase the “coping time” under severe accident conditions. where coping time is according to the oecd/nea defined as [2]: the time to significant loss of geometry such that the fuel can no longer be cooled or cannot be removed from the reactor. for each concept, there will be an analysis of failure modes and effects (fmea) performed to determine the onset of particular initiating event that leads to severe accident. however, the common baseline has to be set and general illustrative scenarios defined. 89 http://dx.doi.org/10.14311/ap.2016.4.0089 http://ojs.cvut.cz/ojs/index.php/app martin ševeček, mojmír valach acta polytechnica ctu proceedings 1.3. development strategy the strategy for atf development includes three phases: (1.) feasibility assessment and down-selection (laboratory experiments; code updates; assessment of economical, operational, safety, fuel cycle, and environmental impacts using evaluation metrics). (2.) development and qualification (atf fabrication; irradiation; safety basis testing; qualification and licensing). (3.) commercialization (technology transfer to industry). any new atf concept must comply with current safety and performance constraints, fuel cycle impacts or additional lwr design constraints. moreover, it’s attributes should be better in comparison with the current fuel system to achieve comparable or better performance in normal and accident conditions. for that reason, the quantitative metrics have to be developed and described in details taking into account also the requirements of utilities, fuel vendors, and regulatory bodies. 1.3.1. challenges in developing atf one of the main concerns is a definition of testing and qualification requirements. individual attributes are not equal, which requires concepts prioritization and determination which attributes to test and what metrics are needed to evaluate attribute compliance. if new atf concept should be accepted by utilities and vendors, it must be capable of integration into the current nuclear fuel cycle system (figure 1). the challenge is to get the best performance at each step of nuclear fuel cycle, and to understand how it affects other parts of the system. figure 1. atf shall not negatively (economically or technically) impact fuel cycle technologies. for that reason, integrated evaluation approach has to be adopted. 2. attributes of atf the attributes for mitigation of fuel failure during severe accidents provide fundamental guidance for atf evaluation. it may not be necessary to improve fuel system in all attributes. some attributes may provide substantial enhancement in accident tolerance, while others may provide only marginal benefits. the desired attributes highlight the performance of the fuel under normal and accident conditions. key attributes for a fuel system demonstrating enhanced accident tolerance include reduced steam reaction kinetics, lower hydrogen generation rate, and reduction of the initial stored energy in the core. the desired behaviors should be accomplished while maintaining or improving cladding thermo-mechanical properties, fuel-cladding interactions, and fission-product retention. in some cases, the described consequences of accident conditions may be concept-specific (e.g. hydrogen generation in the current zr alloy-uo2 fuel system). other atf concepts could present additional effects not expressed here (e.g. generation of co in case of sic) that must be considered in evaluation of the proposed system. a brief description of the desired attributes is provided in this section and summarized in figure 2. figure 2. major issues that need to be addressed in establishing accident tolerant fuel attributes. candidate fuel systems must first not harm, which means that the fuels must perform as well as or better than the current fuel system. moreover, the fuel system must additionally provide a comparable or improved response to aoos (anticipational operational occurences), dbas (design basis accidents) and bdbas (beyond design basis accident). 2.1. hydrogen generation rate hydrogen generation in the reactor core can lead to energetic explosions similar as in fukushima-daiichi accident. under a high-temperature steam environment, it is not possible to avoid hydrogen generation with standard zr-alloys. rapid oxidation of cladding results in free hydrogen generation. this exothermic reaction increases the cladding temperature, which further accelerates free hydrogen generation. a related issue is the diffusion of free hydrogen into the unoxidized portion of the cladding, resulting in enhanced embrittlement and potential cladding failure. the desired alternative is a cladding material that resists oxidation or reduces the rate of oxidation resulting in a slower hydrogen generation rate. materials with lower heat of oxidation are important due to the limitation of temperatures during an accident. materials that are less susceptible to hydrogen diffusion 90 vol. 4/2016 evaluation metrics for vver atf fuels may address the rapid embrittlement issue typical for standard zr alloys. 2.2. fission product retention cladding provides an important barrier between fission products and primary circuit. the potential release of fission products to the environment has to be avoided, therefore, retention within the fuel is of the highest importance. while total retention may not be possible, higher partial retention would be a substantial improvement. the desired improvement is to prevent melting or dispersion of the fuel by utilization of hightemperature/strength cladding materials that would retain cladding integrity beyond the current limitations of zr-alloy cladding. 2.3. cladding reaction with steam when cladding is exposed to steam at high temperature, multiple issues need to be considered: hightemperature steam interaction with zr-alloy cladding, an exothermic oxidation reaction, hydrogen generation, and degeneration of the structural integrity of the cladding. atf materials should demonstrate enhanced tolerance to radiation and oxidation under hightemperature exposure while specifically considering mechanical strength and structural integrity at the end of life and when exposed to high-temperature steam for an extended duration. 2.4. fuel-cladding interactions pellet cladding chemical interactions (pcci), pellet cladding mechanical interactions (pcmi) and fuel heating are important properties that must be understood during normal operation and accident conditions for all new fuel concepts. the desired design option is to develop fuels with reduced pcci and pcmi, with lower operating temperatures relative to the zr alloy-uo2 system, with higher melting point, and with structural integrity at high temperatures. chemical and physical compatibility of cladding and fuel for all proposed concepts must be ensured. 3. constraints on development of enhanced atf except for a few rare events, the current uo2-zr fuel system meets all performance and safety requirements while keeping nuclear energy economically competitive. any new atf concept should be compliant with and evaluated against current design, operational, economic, and safety requirements. fuel cycle considerations must also be considered, especially for concepts that represent a significant departure from the current technology. a brief summary of the constraints is illustrated in figure 3. figure 3. constraints on new fuel designs. the main constraints include: • potential atf geometry deviations and compatibility with co-resident fuel. • evaluation of all potential accident condition parameters, including: . fmea completion to ensure that any potential atf operating vulnerabilities are recognized and mitigated as possible. . completion of a § 50.59-like process (changes, tests and experiments section from the 10cfr50 regulation) to illuminate any necessary licensing or logistical preparations for operation of the atf in a commercial lwr. the process and its guidance is described in [3]. • quantifying the recommended minimum additional coping time to be provided by the atf. • the need to include a metric to address those concepts that require enrichment greater than 5 wt%. • the mission of the utility is not to test new fuels. any atf operation must necessarily address and minimize impacts on the utility by ensuring full compatibility with co-resident fuel and reactor components, and by limiting perturbations of the normal operation of the plant. • nuclear industry has optimized the current zr-uo2 which represents a large financial investment. the additional cost of atf must be relatively low. at present, it is not feasible to determine quantitative results. 3.1. backward compatibility atf concepts must be suitable for use in existing lwrs. longer term concepts may be considered in conjunction with the near-term focus. proposed fuel concepts should not require plant modifications to the current reactors. they should be compatible with existing fuel handling equipment, fuel rod or assembly geometry, and co-resident fuel in existing lwrs. 3.2. impact on operations a concept must maintain or extend plant operating cycles, reactor power output, and reactor control. re91 martin ševeček, mojmír valach acta polytechnica ctu proceedings figure 4. a diagram that describes an approach to assessing enhanced accident attributes of a proposed fuel design. ducing the availability or power output would be unacceptable to utilities. to maintain current operation, some of the fuel system concepts would require higher fuel enrichment. while the impact of higher enrichment is fairly well understood from a technical perspective, regulatory and safeguard issues have to be addressed. 3.3. economic impacts any atf concept is likely to be more expensive than the current uo2-zr system, at least initially. fuels that require higher enrichment are especially likely to cost more. increased enrichment could additionally require modifications to fuel fabrication facilities. therefore, it is important to carefully assess the economic impact of the new technology and to determine how much additional fuel cost the utilities will accept. on the other hand, increasing burnup and power densities (power upgrades) could reduce or mitigate the negative economical impacts. 3.4. safety impact performance of a new fuel system will be compared to the performance of the uo2-zr alloy system which defines a baseline for the atf evaluation. the performance must be shown to be similar to or better than of the current system. 3.5. fuel cycle impact atf must adhere to regulations and policies, for both the fuel fabrication facility and the operating plant, with respect to technical, regulatory, equipment, and fuel performance considerations. a new atf system could also have an impact on the back-end of the fuel cycle. the storage, repository performance of the fuel or possibility of reprocessing must not be degraded. 4. metrics and related testing the metrics determine a clear technical methodology for evaluation that can be used to rank two or more concepts. the approach has to be simplified due to the complex multiphysics behavior of nuclear fuel and the large set of performance requirements that must be met. dozens types of atf cladding ranging from metallic to fully ceramic cladding each with very different material properties and behavior has been studied. each concept has to be evaluated and compared to determine the concept viability, and prioritize resources to obtain the cladding with the best compromise in terms of properties and behavior in both nominal and accidental conditions. 4.1. desired cladding properties, behavior and performance the cladding of a nuclear fuel has three fundamental functions: (1.) confinement of fissile material and fission products within the fuel rod. (2.) not affecting chain reaction (low absorption cross section). (3.) efficient heat transfer from the fuel to the coolant. to fulfill these three functions a new ideal cladding material needs to have certain properties and exhibit specific behaviors as follows: fabricability: • compatibility with fabrication facilities; material availability; welding/sealing behavior. thermo-mechanical behavior: • high thermal conductivity, strength, and ductility; leak-tightness throughout plant operation (impermeable to fission gas and fission products). corrosion behavior: • high corrosion resistance in vver reactor environment; high corrosion resistance in high temperature steam; low h2 production and low hydrogen embrittlement. chemical compatibility: • compatibility with fuel, coolant, and the fuel assembly components; no eutectic. irradiation behavior: • stable or predictable thermal, mechanical, and corrosion behavior under irradiation; dimensional stability; low irradiation embrittlement; low thermal neutron absorption cross-section; low activation. back-end behavior: • low tritium permeation; no impact on the reprocessing; satisfactory storage behavior. new atf cladding material will not exhibit all presented ideal properties. for that reason, a baseline for evaluation and assessment of various concepts has 92 vol. 4/2016 evaluation metrics for vver atf fuels to be established. this corresponds to the metrics described further. 4.2. metrics definition the metrics are divided into three sections: (1.) material properties inherent to the material. (2.) material behavior observed through standardized tests or experiments for normal and accident conditions. (3.) material behavior observed through standardized tests for accident conditions. note that, material behavior can depend also on particular reactor type and its performance. 4.2.1. inherent material properties the inherent material properties that should be compared are mainly thermal and neutronic properties: high melting/sublimation temperature; high thermal conductivity; optimal heat capacity/enthalpy; optimal thermal expansion coefficient to ensure dimensional stability; thermal neutron absorption crosssection. there are other concept-specific inherent properties. for example in case of multi-layer coating, compatibility between different materials has to be ensured. additionally, eutectic temperature might decrease the melting temperature of the cladding so it should be avoided. 4.2.2. normal operation behavior in contrast with the inherent physical properties described above, the behavior of the materials has to be assessed through tests with standardized conditions to enable direct comparison and evaluation of the various concepts. long-term corrosion tests are proposed to evaluate the corrosion behavior in normal operating conditions in a different chemical environment. an acceleration of kinetics is likely under irradiation which has to be also investigated. the important data to assess are: visual inspection – potential delamination of coatings; corrosion kinetics – weight change, oxide thickness; water chemistry analyzes; hydrogen pick-up. mechanical tests suggested for mechanical behavior evaluation are: tensile tests; internal pressure creep tests; internal pressure burst tests; leaktightness behavior; fatigue tests – thermal cycling, internal pressure load cycling. 4.2.3. accident conditions behavior first, tests simulating normal operating conditions will be performed. later, the material performance under selected accident conditions will be assessed. specific tests selected to determine accident performance of candidate cladding materials are series of standard tests simulating ria and loca conditions. for example: high temperature oxidation, isothermal internal pressure burst tests at multiple temperature set points, dynamic internal pressure burst tests with increasing temperature until cladding failure, rapid burst test with increasing temperature until cladding failure, tensile tests at elevated temperature, internal burst tests, tensile test at elevated temperature etc. 5. evaluation baseline at the beginning of the evaluation, it is recommended to establish a common understanding of the current state-of-the-art cladding. key characteristics and performance criteria were identified, with quantitative values assigned where possible. all of the parameters are zr alloy specific, some are reactor design and reactor performance (chemistry regime, power changes) specific. however, there can be common baseline for most of lwrs defined with only small uncertainties. 5.1. baseline for normal operating conditions generally accepted characteristics of zr-based alloys during normal operations are [4]: • fission product retention: 10−6 pin failure rate, radiation tolerant: up to 10 dpa, 1022 n/cm2 fast (>1 mev), dimensional stability: max 1 % axial elongation. • thermal conductivity λ: ∼17.4 w/m k, heat capacity cp: 293 j/kg k, heat transfer coefficients: coolant/cladding coupling (reactor design dependent). • corrosion performance: oxide growth ≤100 µm, hydrogen content ≤800 wppm, maximum limit on corrosion product buildup (linked to water chemistry specifications), galvanic corrosion limits, requirement for all corrosion products to be harmless to other system components. • tritium release into coolant: limit for tritium permeation not established, but “low” permeation is desirable, <10 % of the total tritium generated permeating into the coolant could be reasonable. vendors assume that less than 2 % of this tritium permeates through zr-based alloy cladding to the coolant (e.g. for ss-316, the permeation could be as high as 90 %). • hydrogen pick-up: typical for zr-based alloys, depends on corrosion level and varies with alloy from 100 ppm to 800 ppm (600 ppm should be acceptable under normal operating conditions). • mechanical criteria – ductility: currently 1 % minimum of total elongation; modern alloys show uniform elongation up to 5 % and total elongation up to 20 %; yield strength: current as-fabricated alloys, ∼150–400 mpa at 340 ◦c, ultimate tensile strength: 437 mpa at room temperature (zry-4), creep strain limit: 0.66 % (zry-4); resistance to crack propagation (fracture toughness). 93 martin ševeček, mojmír valach acta polytechnica ctu proceedings • fretting wear: <10 % of wall thickness; debris wear resistance; fabricable: weldable, thin-walled tube that maintains hermeticity. • pci interaction behavior: includes consideration of fission product interactions (possible scc), oxide layer on the inside of the clad (∼10 micron). • burnup limit: peak rod average: 62 mwd/kg u. 5.2. baseline for accident conditions the accident performance of zr-based cladding differs from the normal operation behavior. the main current metric for fuel system performance is that the cladding should maintain post-quench ductility by limiting the peak cladding temperature to 1204 ◦c and the maximum oxidation level to 17 % of the cladding wall thickness. it has been shown that the temperature and oxidation limits result in maintaining ductility for as-fabricated and very low burnup cladding. changes underway nrc regulatory guides and iaea guidelines will limit the oxidation level for dbas based on pre-dba hydrogen content (e.g. 4 % for 600 wppm hydrogen content) [5]. under beyond bdba loca conditions, cladding will be subjected to higher temperatures and oxidation levels. zr-based cladding alloys would experience longer times at increasing temperatures, higher oxidation rates, higher hydrogen release rates, and higher internal heat-of-oxidation rates. key performance measures for fuel behavior during accident conditions include coping time, behavior under elevated temperature conditions over long periods of time, and material oxidation [6]. the relevant temperatures for lwr severe accidents which result in the formation of liquid phases due to melting or chemical interactions are summarized in figure 5. • coping time under dba and bdba – lbloca conditions: from 50 to 300 sec at 1204 ◦c, sbloca conditions: ∼1 hr at ≤1050 ◦c. • elevated temperature issues – melting temperature: ∼1760 ◦c, temperature for eutectic formation (decrease of melting point, effects on other components), runaway oxidation – relates to heat of oxidation and acceleration of the oxidation process. • steam oxidation kinetics: oxidation rate and associated heat of oxidation, performance considered for time at elevated temperature and maximum temperature, breakaway oxidation may occur at elevated temperature (e.g. time at ∼1000 ◦c before breakaway oxidation occurs should be defined). • hydrogen production and release: <1 % zr-metal conversion. • maintain ductility following dba: most important accident performance criterion under licensing standards, regulation specifies at least 1 % ductility post-quench. • high temperature mechanical properties: balloon and burst are not currently defined as a fuel failure and are not limited in the licensing criteria; while only a fraction of rods burst, those that do typically burst at ∼800 ◦c; burst may occur at lower temperature with higher burnup due to higher internal pressure; burst is a ductile failure; size of ballooning and burst opening can be important to the results of the failure. • severing and/or shattering the cladding with subsequent fuel release are considered as a failure; creep performance must be also considered. • flow blockage under accident scenarios: required calculation for licensing, related to maintaining coolable geometry, flow blockage may result from swelling / ballooning of cladding. • thermal shock resistance: current cladding alloys do not shatter until they have reached high oxidation levels (>17 % of the cladding wall thickness consumed by oxidation), standard test applied to determine thermal shock performance. figure 5. lwr severe accident-relevant melting and chemical interaction temperatures which result in the formation of liquid phases [7]. the goals of evaluation are associated with defining requirements for down-selection among options during the feasibility assessment. it includes identification of important attributes for atf, understanding the common baseline for evaluation and map the merit of the attributes against potential operational or safety envelope benefits which are presented in the previous sections. it is also required to define safety analyzes including accident scenarios to quantify the target 94 vol. 4/2016 evaluation metrics for vver atf fuels values of particular atf fuel characteristics which are presented in the next section. 6. illustrative scenarios for atf evaluation two “bounding scenarios” for bdba evaluation are proposed. they cover wide range of severe accidents and at the same time are not too prescriptive and specific to a particular npp design. modeling of these scenarios will utilize one of the initiating events and will continue until a defined point of failure as defined in by the coping time definition (see section 1.2) for particular atf concept. the two scenarios applicable to vver reactors are: • long-term station blackout: high-pressure scenario; it will be calculated to the point of reactor pressure vessel failure. • large-break loca: low-pressure scenario with high decay power and limited availability of emergency cooling systems. the proposed scenarios are intended to provide bounding cases for fuel performance. each atf concept will be evaluated by fuel performance and system analysis codes in regard to the two illustrative scenarios. all atf evaluations should be allowed to progress to the point defined by the coping time definition with considering failure modes and effects for particular atf concept. the goal of the evaluation is to estimate the potential increase in coping time that is offered by the atf concept and to assess potential outcomes (e.g. fuel failure, coolability, cause of failure). following completion of bounding (most severe) analyzes, more detailed studies for these illustrative scenarios should be performed to develop a better understanding of the impact of additional variables as burnup, time after scram when core cooling is lost etc. 6.1. high pressure scenario – sbo the high-pressure sbo (station blackout) scenario for atf evaluation purposes for vver-1200 reactor is defined as: • loss of all sources of ac supply. • feed water supply is unavailable. • turbine isolation valve is activated, pressure in the steam generators (sgs) increases. • after exceeding the pressure limit the quick-acting pressure reducing system opens. • a failure of the quick-acting pressure reducing system is postulated – system stays open after pressure decreases. • loss of coolant in sgs leads to decay heat removal passive system failure. 6.2. low pressure scenario – lbloca + sbo the low-pressure scenario for atf evaluation purposes for vver reactors is defined as: • guillotine rupture of the primary circuit’s cold leg near the reactor inlet with sbo. • decay heat removal passive system (dhrs) and emergency core cooling system are in operation. operation of the hydro accumulators is assumed. the decay heat removal passive system and emergency core cooling system operate according to their design characteristics: eccs – up to water volume exhaustion, dhrs – up to the end of nitrogen absorption due to eccs operation. total operation time of these systems is approximately 24 h from the accident start. 7. vver fuel specifics the russian design pressurized water reactors called vver have specific differences in comparison with western pwrs. it is recommended to adopt all evaluation metrics with both illustrative scenarios presented above and define additional vver specific metrics. the main differences of the vver fuel and primary circuit include: • different water chemistry, • hexagonal geometry and arrangement of the fuel assemblies, • various cladding and fuel materials . e110 alloy, e635 alloy, . annular pellet, different dopants, only gd-based burnable absorbers, • assembly shroud – in case of vver-440 fuel assemblies, • different control rod materials. the main difference between vvers and pwrs can be observed in nominal operation due to different chemistry of primary circuit and different material composition. while pwrs use lioh for chemistry control, vvers use koh. this difference in chemistry regime leads to slightly different test conditions for normal operation corrosion tests. however, in accident conditions the performance of vvers is similar to that of pwrs. therefore it is not necessary to define additional vver-specific metrics for accident conditions. 8. conclusion to develop new accident tolerant fuel systems an evaluation and prioritization of atf concepts has to be performed at the end of the first development phase. the prioritization will allow researchers and decision makers to focus resources on most promising concepts. due to the complicated complex multiphysics behavior of nuclear fuel it is not possible to test all the required characteristics for each concept. for that 95 martin ševeček, mojmír valach acta polytechnica ctu proceedings reason, evaluation metrics have to be defined. a good starting point for atf evaluation establishment is a common understanding of the current state-of-the-art zr-cladding and its performance in bdba conditions. it is a baseline for evaluation and assessment of various concepts. evaluation of atf cladding must consider the complete fuel system (including fuel cycle) and should encompass all performance regimes for the fuel, including: fabrication, normal operation and aoos, dbas, bdbas, and used fuel storage, transportation, and disposition. there are numerous attributes within each regime that must be considered in evaluating the fuel system performance. key attributes for the cladding were discussed in sections 4 and 5, along with a summary of standard tests recommended for measuring specific properties and characterizing performance under the specified conditions. it may not be possible to improve the current state-of-the-art fuel system in all attributes and regimes, significant improvement in some of the key attributes may outweigh modest performance gains or modest vulnerabilities in other attributes. a detailed list of proposed attributes for evaluation is provided together with metrics and standardized tests. the attributes summarized in this document, can be used as a qualitative guide to assess the performance of candidate materials relative to the current state-of-the-art materials and relative to one another. evaluation baseline for common understanding of the current cladding was presented. to further determine the common understanding of atf performance two severe accidents were defined and described. based on the illustrative scenarios the coping time can be calculated and atf concepts evaluated. most of the metrics and attributes are generally applicable for all lwr reactors but some attributes as chemistry regime are reactor-specific and for that reason additional metrics and standardized test were defined for vver types of reactors. detailed more prescriptive approach for evaluation of atf cladding for vvers will be described in future technical report. acknowledgements this work was supported by the grant agency of the czech technical university in prague, grant no. sgs ohk4-008/16. references [1] s. m. bragg-sitton, j. carmack, f. goldner. evaluation metrics applied to accident tolerant fuels. tech. rep., idaho national laboratory (inl), 2014. [2] egatfl. light water reactor accident tolerant fuel: evaluation metrics and technology readiness level definition. tech. rep., oecd/nea, 2016. [3] usnrc. 1.187, regulatory guidance for implementation of 10cfr50.59. tech. rep., 2000. [4] m. billone, y. yan, t. burtseva, et al. cladding embrittlement during postulated loss-of-coolant accidents. tech. rep., argonne national laboratory (anl), 2008. [5] g. youinou, r. s. sen. enhanced accident tolerant fuels for lwrs–a preliminary systems analysis. tech rep 2013. [6] l. braase. enhanced accident tolerant lwr fuels national metrics workshop report. tech. rep., idaho national laboratory (inl), 2013. [7] p. hofmann. current knowledge on core degradation phenomena, a review. journal of nuclear materials 270(1):194–211, 1999. 96 acta polytechnica ctu proceedings 4:89–96, 2016 1 introduction 1.1 atf definition 1.2 coping time 1.3 development strategy 1.3.1 challenges in developing atf 2 attributes of atf 2.1 hydrogen generation rate 2.2 fission product retention 2.3 cladding reaction with steam 2.4 fuel-cladding interactions 3 constraints on development of enhanced atf 3.1 backward compatibility 3.2 impact on operations 3.3 economic impacts 3.4 safety impact 3.5 fuel cycle impact 4 metrics and related testing 4.1 desired cladding properties, behavior and performance 4.2 metrics definition 4.2.1 inherent material properties 4.2.2 normal operation behavior 4.2.3 accident conditions behavior 5 evaluation baseline 5.1 baseline for normal operating conditions 5.2 baseline for accident conditions 6 illustrative scenarios for atf evaluation 6.1 high pressure scenario – sbo 6.2 low pressure scenario – lbloca + sbo 7 vver fuel specifics 8 conclusion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2016.3.0065 acta polytechnica ctu proceedings 3:65–70, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app load bearing capacity of the glass railing element elizabeta šamec∗, domagoj damjanović, joško krolo university of zagreb, faculty of civil engineering, fra a. k. miošića 26, zagreb, croatia ∗ corresponding author: elizabeta.samec@gmail.com abstract. in this paper some basic physical and mechanical properties of glass as structural material are presented. this research is about specifically manufactured glass railing element that will be a part of a pedestrian bridge construction in zagreb, croatia. load bearing capacity test of the glass railing element is conducted within the faculty of civil engineering in zagreb and obtained experimental results are discussed and compared to the ones provided by the numerical model. taking into account the behaviour of laminated glass and results of experimental and numerical testing, glass railing element can be regarded as safe. keywords: glass railing element, load bearing capacity test, wind load, modulus of elasticity, numerical model. 1. introduction when we have glass elements that are specifically manufactured for construction projects it is highly important to perform laboratory testing in order to confirm their load capacity. necessity for laboratory testing follows from potential unexpected breakdown under the load due to special properties of the glass as a construction material. unlike steel, plastic and wood, glass has no plastic properties and consequently no yield point [1]. because of the property of pure elasticity with brittleness the glass cannot be permanently deformed by load and it fails without warning as shown on a stress-strain curve (fig. 1). failure always happens in tension because it has high compressive strength [2]. the cause of the glass failure is not necessarily concentrated impact; fracture may occur due to bending stress, thermal stress or deformation. a fracture which occurs will depend on the number of surface defects, the duration of the load, the size of the tensed surface and the stress level. by increasing the dimensions of the glass elements the number of imperfections will increase as well [3]. this kind of behaviour is undesirable for a construction material. despite possible problems with brittle behaviour and unexpected breakdown, application of structural glass has undergone remarkable development in the last twenty years. the opportunities and attractiveness that this type of material provides have been recognized and glass has become more than “window material”. the subject of this research is the glass railing element designed for the pedestrian bridge construction planned to be built in zagreb, croatia. usually for tempered glass guardrails, live loads caused by use and wind loads need to be considered. other loads such as a permanent load, snow load, and seismic load are insignificant because of their low range compared to the overcharge caused by use or wind [4]. in this case, the wind is also the main load on the glass element, figure 1. stress-strain diagram for steel, glass and plastic [2]. so it is necessary to test the bearing capacity of the glass railing element under the influence of the wind. in most cases glass will behave entirely elastic until the moment of fracture and this kind of behaviour is expected to be confirmed by experimental analysis. the literature review in [1] shows that earlier research has been conducted on behaviour, strength, analytical and numerical modelling of laminated glass with pvb but still the knowledge required to use laminated glass as a load bearing element in every-day construction, is not sufficient. the aim of this paper is to gain a deeper knowledge of the behaviour of laminated glass by experimental investigations and by numerical model simulation. to pursue the proposed study, load bearing capacity test was performed on the glass railing element in the scale 1:1. corresponding finite element numerical models were created in the software sap 2000 to discuss and compare displacements in the points most affected by the wind influence. the main question that needs to be answered is whether the glass railing element can be regarded as safe to install on the pedestrian bridge. therefore, safety factor is calculated and expected 65 http://dx.doi.org/10.14311/app.2016.3.0065 http://ojs.cvut.cz/ojs/index.php/app e. šamec, d. damjanović, j. krolo acta polytechnica ctu proceedings figure 2. bridge plan. figure 3. glass railing element with positions of attachment details. behaviour under the wind load is tested on a life-size sample of the glass railing element. 2. bridge project details 2.1. bridge construction the future pedestrian bridge is planned to be built in miramarska street in zagreb. the railing elements are going to be put along the bridge to protect the pedestrians from the influence of wind and to ensure their safety. the plan of the future bridge is shown in fig 2. 2.2. railing element the glass element consists of two 10 mm thick tempered glass panes bonded by interlayer (polyvinyl butyral-pvb). the stiffness of laminated glass depends on the shear strength of the panes and the pvb foil. factors that influence the behaviour of these connections are load duration, intermediate layer thickness, temperature and position of the intermediate layer with respect to the center of gravity. the behaviour of laminated glass is different under the long-term and short-term load. under the influence of short-term load, laminated glass acts as a composite carrier. under the influence of long-term load, the load is distributed on two panes due to their rigidity because of the deformation of the interlayer. in the case of a breakdown, glass fragments remain linked to the pvb layer. therefore, laminated tampered glass figure 4. detail 1: spider fitting (up), detail 2: inox clamps connecting the element to the main steel profile (down). is chosen for the railing element of the pedestrian bridge. the dimensions of the railing element are 213.4 x 107.5 cm. the element is attached to the bridge construction at four points. as you can see in the fig. 3 and fig. 4, the element is put in the inox glass clamps on the bottom, and on the handlebar section it is fixed to the handlebar with two spider fittings. 2.3. wind load as mentioned in the introduction, the wind load is authoritative load and calculation of the design value used in laboratory and numerical analysis is further described below. the design value is calculated according to croatian valid norm for wind load hrn en 1991-1-4:2012/ na2012. depending on the sensitivity of construction on the dynamic impulse, two procedures exist to calculate wind load: • simplified procedure: applies to structures that are insensitive or moderately sensitive to dynamic impulse, • detailed procedure: applies to structures sensitive to dynamic impulse which have the value of the dynamic coefficient greater than 1.2. 66 vol. 3/2016 load bearing capacity of the glass railing element figure 5. load bearing capacity test. figure 6. positions of measurement points (up) and load distribution (down). for the construction of the pedestrian bridge in zagreb the simplified method is applied since the construction is not sensitive to dynamic impulse. simplified calculation implies that the wind action is taken as a replacing static load. for the bridges, the wind pressure is calculated from the forces in all horizontal directions. to determine the wind load on the glass railing element according to hrn en 1991-1-4:2012/ na2012 the following parameters are required: • basic wind speed: vb = 20 m/s • height above the ground: h = 5 m • field category: iv. the design value of the wind load determined by the project designer is 1 kn/m2. 3. load bearing capacity test the load bearing capacity of the element (in the scale 1:1) was tested on one sample until breakdown in the structural testing laboratory operating at the figure 7. breakdown of the glass railing element. faculty of civil engineering in zagreb. the testing was conducted on the universal testing machine zwick z600. during the test, displacements and strains were measured using lvdt sensors (p) and strain gauges (t) as shown in fig. 6 (up). the sample was tested in the horizontal position and the wind load was simulated with two types of loading. the first type is a continuous load (1 kn/m2) on the surface between the supports (107.5×120.3 cm) which was applied with 12 weights during the whole test. the second one is a linear load (qpok) applied on the console part with the help of the previously mentioned machine zwick z600. the two types of loading can be seen on the fig. 5. the bending moment at the handlebar section provoked by the design value of wind load (f=1 kn/m2) on the surface of the console part of the glass element (fig. 6) is calculated as follows: m = f ∗ a2 2 2 = 1 ∗ 0.9312 2 = 0.433 knm/m. (1) the linear load (qpok) applied in the experiment must cause bending moment at the support (handlebar section) equivalent to the one caused by the assumed wind force calculated above: m = qpok ∗ a2/2, (2) qpok = m a2/2 = 0.433 0.466 = 0.93 kn/m. (3) knowing the required value of liner load (qpok) concentrated force (fpok) on the steel element is according to fig. 6 (down): fpok = qpok ∗ b = 0.93 ∗ 1.075 = 1.0 kn. (4) in this way continuous load on the whole surface of the railing element that would be provoked by wind 67 e. šamec, d. damjanović, j. krolo acta polytechnica ctu proceedings figure 8. bending test for glass canopy specimens [5]. sample strain [‰] e [mpa] 1 0.60 38 833 2 0.58 40 167 3 0.56 41 607 table 1. results of the bending test at the glass canopy specimens [11]. is simulated. by using a machine to apply fpok we were able to continually increase the force until the breakdown of the sample. the linear load is applied by increments of 0.5 kn until the force value of 2.0 kn, after which it is applied continuously until breakdown. after each load stage, the element is unloaded to determine the existence of any permanent displacements and strains. when the force reached the value of 6.55 kn, breakdown started rapidly expanding through the sample (fig. 7). the safety factor of the glass element can be calculated as the ration between failure load and design load. sf = 6.55 kn 1.00 kn = 6.55 . (5) 4. simulation of load bearing capacity test in sap 2000 as well as the laboratory test, a numerical model was made in sap 2000. a numerical modelling of laminated glass by finite element method is complex, mainly because of the very thin interlayer in comparison with other dimension and because of the large difference in modulus of elasticity of glass ply and interlayer material, especially for pvb [1]. the failure of a laminated glass sheet can be subdivided in five phases [5]: (1.) elastic behavior of the glass plies. (2.) the first glass ply is broken, the other is still intact; the interlayer is not damaged. (3.) the second glass ply fails; the interlayer behaves elastically. (4.) the interlayer behaves plastically; the splinters are kept together by the interlayer. (5.) the interlayer fails by reaching its failure strength or by cutting from the splinters. while phase (1.) can be modelled with analytical or numerical methods, phases (2.) to (5.) are more figure 9. numerical model in sap2000 for fpok = 1.00 kn (up) and fpok = 6.55 kn (down). (u-displacement, r-rotation, 1-x axis, 2-y axis, 3-z axis) complex to simulate. as shown in [5] several material models based on finite elements can be found in the literature to simulate the failure of the glass as well as of the interlayer. models with one shell element through the thickness use layered materials with integration points over the thickness. in [6] a material model for the glass which allows a two dimensional failure is presented. a combination of two shells and one solid element through the thickness can be found in [7]. authors [8], [9] and [10] present 3d models with solid elements which allow using a detailed material law for the interlayer. the aim of the paper is just to compare displacement results in points most affected by wind, so it is concluded that a single thin plate model describes the behaviour of laminated glass for the current application well enough, and it is not expensive in terms of time and problem size. since the test to determine mechanical properties was not performed for this specific railing element, modulus of elasticity was chosen based on the previously known test results. these results are obtained in the same laboratory during the test conducted for the construction of glass canopy [11]. for the glass canopy analysis a bending test was performed on three laminated tempered glass specimens consisting of two 10 mm thick tempered glass panes as shown in fig 8. during the test, strains were measured using strain gauge in the middle of the sample. from the obtained data, modulus of elasticity was calculated using hooke's law. results of this testing are summarized in the table 1, and since the railing element also consists of two 10 mm thick tempered glass panes, the chosen value of modulus of elasticity for this numerical model is e= 40 000 mpa. supports are defined in reliance to fig. 4 and they have prevented displacements in all three directions (x, y and z) while the rotation angle is free around all three axes [12]. the first numerical analysis was made for the load of 1 kn/m2 on the surface between the supports and linear load qpok corresponding fpok= 1.00 kn as it is 68 vol. 3/2016 load bearing capacity of the glass railing element loading experiment sap 2000 force displacement u3 fpok = 1.00 kn 8.00 mm 6.70 mm fpok = 6.55 kn 58.54 mm 60.80 mm table 2. comparison of experimental and numerical displacement results. shown in the fig. 6 (down) and described earlier. the second numerical analysis was conducted in the same way for the maximum load at breakdown fpok= 6.55 kn obtained during the experimental testing. models and given results are shown in fig. 9. 5. results results obtained by the load bearing capacity test are processed and shown in force-strain (fig. 10) and force-displacement diagram (fig. 11). from the force-strain diagram obtained during the experimental analysis, we can confirm that the glass behaved linearly elastic without any damages until breakdown. after all phases of loading, the residual strains were within the boundaries of 4% and the residual displacements within the limits of 10%. even though the displacements were measured during the test at 6 points (p1-p6), the most interesting points to compare obtained experimental and numerical results are points p1 and p2. in those points wind will cause the biggest displacement since they are the top points of the free console part (fig. 6 (up)). in the numerical model there will be no difference between the displacement of the point p1 and p2 so the point p2 is chosen due to an easier display of numerical results. the comparison of the displacement results obtained by numerical and experimental analysis at the measurement point p2 is given in table 2. in fig. 8 displacement gained from numerical model is marked with u3. from the table we can see that the obtained experimental and numerical results differ by less than 15%. as already discussed in the previous section, the simple single plate model is chosen. the thin plate model does not take into account a fact that laminated glass is three layer composite, instead the modulus of elasticity is defined for whole element. the test to determine the mechanical parameters was not performed, so the chosen value of modulus of elasticity based on the comparison of previously known test results can differ for two main reasons. the first reason is that even though the thickness of the glass panes was the same in both cases, different glass is used in manufacturing canopy and railing elements. secondly, we do not know exactly what impact interlayer has on the modulus of elasticity of composed element. figure 10. force-strain diagram. figure 11. force-displacement diagram. 6. conclusion the combination of hard glass with a soft interlayer limits the use of laminated glass as structural load carrying element due to difficult behaviour prediction. glass has a modulus of elasticity several thousand times larger than the interlayer material, which makes the behaviour and the modelling complex. with the simple single thin plate model used in this study, where modulus of elasticity for the whole laminated glass sheet was chosen based on the previous similar testing, gained results for displacement differ from experimental ones by less then 15%. the results show that for studies which include stress-failure models, taking into account the interaction behaviour of glass with interlayer is compulsory. it is also important to perform the test to determine mechanical parameters for each composed glass element because their accuracy can considerably influence the quality of the numerical model. in future studies it is necessary to observe the influence that thickness of interlayer has on the modulus of elasticity of laminated glass elements. the proper understanding of the interaction behaviour will enable wider usage of laminated glass as load carrying element. the safety factor of tested railing element reached in regard to the design wind load is k = 6.55. the glass railing element can endure six times higher load than anticipated so we can conclude that there are high 69 e. šamec, d. damjanović, j. krolo acta polytechnica ctu proceedings reserves in the bearing capacity of tested glass element. since the test was performed at the room temperature and pvb is highly temperature dependent material, by taking into account the weather conditions on the bridge we can expect the safety factor to be lower. considering the behaviour of laminated glass during the test and results of experimental testing compared to numerical ones, glass railing element can be regarded as safe. list of symbols vb basic wind speed [m/s] fpok concentrated force in the experiment [kn] f design wind load [knm/m2] h height above the ground [m] qpok linear load in the experiment [kn/m] m moment on the handlebar section [knm/m] sf safety factor [/] references [1] akter s. t., khani m. s. characterisation of laminated glass for structural applications. master thesis, 2013 [2] “saint gobain”. updated mar. 2015, accessed 13 apr. 2015. http://uk.saint-gobain-glass.com [3] neugebauer j. design of glass structures, scientific symposium: future trends in civil engineering, zagreb, croatia, 2014. [4] “manual for design of guardrails”. accessed 05 jun. 2015. http://www.allium.com/pdf/manuel-en.pdf [5] larcher m., solomos g., casadei f., gebbeken n. experimental and numerical investigations of laminated glass subjected to blast loading. international journal of impact engineering 2012; 39:42-5 doi:10.1016/j.ijimpeng.2011.09.006 [6] müller r., wagner m. berechnung sprengwirkungshemmender fenster und fassadenkonstruktionen. bauingenieur 2008;81(11):475-87 [7] sun d., andrieux f., ockewitz a., klamser h., hogenmüller j. modelling of the failure behaviour of windscreens and component tests. 5th european lsdyna users conference, 25-26 may, 2005. [8] morison c., zobec m., frenceschet a. the measurement of pvb properties at high strain rates, and their application in the design of laminated glass under bomb blast. isiems 2007, international symposium on interaction of the effects of munitions with structures, 17-21 september,orlando, us, 2007. [9] bennison s.j., jagota a., smith c.a. fracture of glass/poly(vinyl butyral)(butacite)laminates in biaxial flexure. journal of the american ceramic society 1999; 82(7):1761-70. [10] duser a.v., jagota a., bennison s.j. analysis of glass/polyvinyl butral laminates subjected to uniform pressure. journal of engineering mechanics 1999; 125(4):435-42. doi:10.1061/(asce)0733-9399(1999)125:4(435) [11] rak m., damjanović d., krolo j.: report on testing the glass beam, universitiy of zagreb, faculty of ce., 2013. [12] “sap 2000” 16 eval, computers and structures, inc., 2013. 70 http://dx.doi.org/10.1016/j.ijimpeng.2011.09.006 http://dx.doi.org/10.1061/(asce)0733-9399(1999)125:4(435) acta polytechnica ctu proceedings 3:65–70, 2016 1 introduction 2 bridge project details 2.1 bridge construction 2.2 railing element 2.3 wind load 3 load bearing capacity test 4 simulation of load bearing capacity test in sap 2000 5 results 6 conclusion list of symbols references 265 acta polytechnica ctu proceedings 1(1): 265–268, 2014 265 doi: 10.14311/app.2014.01.0265 first hints of pressure waves in a helical extragalactic jet: s5 0836+710 manel perucho1 1departament d’astronomia i astrof́ısica. universitat de valència. c/dr. moliner 50, 46100, burjassot, valencian country, spain. corresponding author: manel.perucho@uv.es abstract one of the open questions in extragalactic jet astrophysics is related to the nature of the observed radio jet, namely whether it traces a pattern or the flow structure itself. in this paper i summarize the evidence collected for the presence of waves in extragalactic jets. the evidence points towards the peak of emission in helical jets corresponding to pressuremaxima of a wave that is generated within the core region and propagates downstream. making use of a number of very long baseline interferometry (vlbi) observations of the radio jet in the quasar s5 0836+710 at different frequencies and epochs, perucho et al. (2012a) were able to observe wave-like behavior within the observed radio-jet. the ridge-line of the emission in the jet coincides within the errors at all frequencies. moreover, small differences between epochs at 15 ghz reveal wave-like motion of the ridge-line transversal to the jet propagation axis. the authors conclude that the helicity is a real, physical structure. i report here on those results and discuss them in the light of new results recently announced by other authors that confirm the presence of waves in the close-by object bl lac (cohen et al., in preparation). keywords: galaxies: jets hydrodynamics instabilities quasars: individual: s5 0836+710. 1 introduction the parsec-scale structure of jets in active galactic nuclei (agn) is mainly observed in the radio band, using the vlbi technique. the nature and properties of the emitting region as related to the flow are still scarcely known. jets can be interpreted as flows because the larmor radius of particles is very small when compared to the spatial scales of the problem studied (blandford & rees 1974). this interpretation has different implications: such systems, which are composed of magnetic fields and particles propagating along the jet channel are expected to host the growth of different hydrodynamical and/or magnetic instabilities. the instabilities have been claimed to be the cause of many of the structures observed (knots, bendings, helices; see e.g., reviews in hardee 2006, 2011, perucho 2012). the instabilities are waves triggered by any external or internal perturbation that grow in amplitude with distance, as they are advected with the flow. thus, if instabilities do really grow in jets, we would expect to observe wave-like structures and motions in extragalactic jets. perucho et al. (2012a) used observations of the jet in s5 0836+710 at different frequencies and epochs and showed that theridge line of this jet behaves as expected if it is interpreted as a pressure wave. aaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaa aaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaa aaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaaa the luminous quasar s5 0836+710 is at a redshift z = 2.16 and hosts a powerful radio jet extending up to kiloparsec scales (hummel et al. 1992). at this redshift, 1 mas ' 8.4 pc (see, e.g., mojave database). vlbi monitoring of the source showed kink structures (krichbaum et al. 1990) and yielded estimates of the bulk lorentz factor γj = 12 and the viewing angle αj = 3◦ of the flow at milliarcsecond scales (otterbein et al. 1998). the jet was observed at 1.6 and 5 ghz with vsop (vlbi space observatory program, a japanese-led space vlbi mission), and oscillations of the ridge-line were also observed (lobanov et al. 1998, 2006). these oscillations were interpreted as kelvin-helmholtz (kh) instabilities (lobanov et al. 2006, perucho & lobanov 2006). the source has also been monitored by the mojave program (lister et al. 2009). finally, it has been suggested that the lack of a collimated jet structure and hot-spot at the arcsecond scales is due to jet disruption, as indicated by the growth in the amplitude of the helical structure (perucho et al. 2012b). 265 http://dx.doi.org/10.14311/app.2014.01.0265 manel perucho 2 evidence for waves in the jet of s5 0836+710 here i summarize the evidence that points to the presence and development of waves in the jet of s5 0836+710, as given by perucho et al. (2012a). the different observations of the jet at different frequencies ranging from 1.6 ghz to 43 ghz, for a given epoch, give the same ridge-line positions within the errors. it needs to be determined whether the small scale ripples in the ridge-line are caused by uv-coverage effects at the different epochs/frequencies, which is plausible. however, the large scale motion coincides for all frequencies and this can only happen if the observed structure corresponds to a physical one. in addition, high resolution images at 15 ghz confirm that the ridgr-line position does not necessarily coincide with the centre of emission of the radio jet, as expected from an asymmetric pressure maximum triggering a helical instability in the jet. within the first milliarcsecond, high resolution images of the jet allowed the measurement of transversal displacements, which show a clear wave-like oscillation pattern with distance. the obtained ridge-line velocities at these scales are superluminal, but this is due, according to the authors, to: 1) relativistic wave velocities, 2) a small-scale oscillation of the core, very difficult to detect in this distant source, but observed in others (e.g., m 81, see mart́ı-vidal et al. 2011), and 3) displacements of the ridge-line being smaller than the errors in the determination of the position. the amplitude of the oscillation grows along the jet propagation direction, which can be due to the coupling to an unstable mode of the kh or current-driven (cd) instabilities. the evidence collected in the previous paragraph led the authors to conclude that the ridge-line of the jet is tracing a pressure-maximum of a wave within the jet, and that even the radio-core is subject to the oscillation produced by the wave. recently, cohen et al. (2013) presented new results of the nearby source bl lac (in the conference the innermost regions of relativistic jets and their magnetic fields, held in granada 10th-14th june, 2013), using long-term monitoring of the source at 15 ghz (cohen et al. in preparation), which confirm that the ridge-line of emission within the jet shows a wave-like behavior. in this case, the authors claim that the oscillation of the ridge-line is caused by a strong magnetic field. in addition, grossberger et al. (2012, and private communication) have followed the ejection and evolution of components in the broad-band radiogalaxy 3c 111 and shown that the position angles of the injected components vary with time and fill a wide channel after several years. this channel is wider than the observed jet at each epoch. this result also points to an oscillation of the bright regions of the jet (necessarily the same as that identified with the ridge-line in other works) within a wide channel in which the observed radio jet is embedded. 3 discussion 3.1 on the nature of the waves given the evidence found for the presence of waves in jets, we can now ask which kind of waves these are and what is their origin. regarding the latter, it is still unclear whether the waves show any regular periodical pattern or not, but the long-term oscillations could be attributed to periodical or quasi-periodical processes in the injection region, such as precession. shorter-term oscillations can be attributed to perturbations triggered by asymmetries in the jet itself or in the ambient medium, lateral winds or entrainment of clouds that rotate around the galactic centre from a side of the jet, for instance. however, all these processes are extremely difficult to detect and isolate. as far as the nature of the waves, there is (already) open debate as to whether they are magnetic or purely hydrodynamical waves. the claim that the waves correspond to magnetic instabilities is based on the fact that the observed radio components seem to follow the ridgeline as they propagate (cohen et al., in preparation): if the jet ridge line is identified with a kink instability in the magnetic field of a magnetically dominated jet, the flow would be forced to follow this kink. however, let us consider the possibility that the ridge-line corresponds to the pressure maximum produced by the kink (e.g., mizuno et al. 2011). this implies that within a given jet cross-section we can find a high-pressure region and a low-pressure one. in this case, the passage of a ballistic component following a straight path along the jet, could enhance the emission of the whole jet, but the effect would be more visible on the ridge-line (high-pressure region). as a result, any radio-component fitted to the region would be centered there. perucho et al. (2006) showed, via numerical simulations, that an asymmetric perturbation at the base of a relativistic jet propagates downstream and naturally creates a pressure maximum helix, which can eventually distort the jet flow and force it into a helical path. in this view, injected components associated with perturbations in flow density at injection that produce shock waves, end up following the helical path when they have dissipated most of their kinetic energy. previous to this, they propagate ballistically. a long-standing cross-debate about jet physics is related to the ballistic nature of the flow in apparently helical radio jets. this point again introduces a difference in behavior, but still not a way to distinguish, 266 first hints of pressure waves in a helical extragalactic jet: s5 0836+710 between a kinetically dominated flow and a magnetically dominated one. if the jet is strongly magnetized, the flow will always follow the field lines and will thus have a twisted path if the field is helical, whereas in the kinetically dominated case, the flow could follow a straight stream-line even if the radio-jet shows a helical structure (because it corresponds to the bright high pressure region within a wide channel). this is true while the amplitude of the instability is not large, but when it grows to nonlinear values, the jet flow starts to deviate from its original trajectory by the pressure gradients within the jet (see, e.g., nakamura & meier 2004, mizuno et al. 2011, perucho et al. 2005, 2006 for the different cases). thus, a purely hydrodynamical jet could produce observational patterns similar to a strongly magnetized jet, and further work is needed to understand the physics behind the ridge-line dynamics. moreover, even if no perturbations are injected in the jet, i.e., the flow is close to stationary, then the fitted components in the radio jet would all be associated with the ridge-line (see, e.g., hardee 2003), just because it corresponds to the brightest regions within the jet. if the ridge-line corresponds to a propagating wave, then the fitted-components would also move along the jet and, of course, on top of the ridge-line. it is thus crucial to disentangle whether the components correspond to waves propagating along the jet and whether or not they follow the ridge-line for understanding its nature. 3.2 the case of s5 0836+710 the wave associated with the ridge-line could couple to a growing instability, as indicated by the growth in amplitude of the helix with distance in the case of s5 0836+710. it is difficult to distinguish between current-driven (cd) instability and kh instability modes, both being solutions to the linearized relativistic, magnetized flow equations and both being possible sources of helical patterns. recent work on cd instability by mizuno et al. (2011) shows that a helical kink propagates with the jet flow if the velocity shear surface is outside the characteristic radius of the magnetic field, i.e., approximately the radius at which the toroidal magnetic field is a maximum. if the observed pattern corresponds to a cd kink instability, the observed transversal oscillation in the jet of 0836+710 requires that the kink be moving with the flow and implies that the transversal velocity profile is broader than the magnetic field profile, i.e., the velocity shear surface lies outside the characteristic radius of the magnetic field. thus, in this case the jet would have a magnetized spine surrounded by a particle dominated outer region and a cd kink in the spine would move with the flow.. the measurement of the opening angle reveals a very similar value at all frequencies for which we have significant measurements, which would favor the radio-jet tracing the whole channel, because the coincidence in the opening angles is less probable in the case of the radio jet corresponding to different regions across the jet. thus, it seems that the radio emission is generated in the same region across the jet at all frequencies and that the jet flow indeed follows a helical path. as stated above, non-ballistic motion is compatible with a magnetically dominated flow, but also with the development of kh-instability modes to large amplitude, because they can dissipate kinetic energy into internal energy and decelerate the flow. it has been reported that the development of the helical kh instability can force the jet flow into a helical path, albeit different from the helicity of the pressure maximum, the latter showing larger amplitude (hardee 2000). the larger the lorentz factor of the flow and the shorter the wavelength of the mode, the more different is the helicity of the flow as compared to that of the pressure maximum. this can be understood in terms of the larger inertia of the jet flow with increasing lorentz factor (hardee 2000, perucho et al. 2005). in summary, the fact that the flow is non-ballistic when the amplitude of the perturbation is large does not necessarily imply that the flow is magnetically dominated and that the waves are magneto-sonic waves. 3.3 the core one other important consequence of the work presented in perucho et al. (2012a) is the possible small-scale oscillation of the radio-core around an equilibrium position. this effect has been reported by mart́ı-vidal et al. (2011) for m 81, using the phase-referencing technique, and it could have important implications for the nature of the radio-core. 4 conclusions it is possible to associate the ridge-line of emission of helical jets to wave patterns tracing a (thermal or magnetic) pressure maximum produced by the growth of instabilities. the core of the jet could well also be oscillating and this motion should be tested and corrected in order to study the parsec-scale kinematics of the radio-components in jets. further combined observational and theoretical studies like this one are required to get more information on the nature of the growing instability and on the properties of the jet flow. acknowledgement i acknowledge financial support by the spanish “ministerio de ciencia e innovación” (micinn) grants aya2010-21322-c03-01 and aya2010-21097-c03-01. i 267 manel perucho also acknowledge p.e. hardee, j.m. mart́ı, m. cohen, and d.l. meier for interesting discussions on the topic. references [1] blandford, r.d., rees, m.j.: 1974, mnras 169, 395. doi:10.1093/mnras/169.3.395 [2] cohen, m.h., et al.: 2013, in the innermost regions of relativistic jets and their magnetic fields. http://jets2013.iaa.es/sites/jets2013.iaa. es/files/imagecache/granada may2013 v3.ppt [3] grossberger, c., kadler, m., wilms, j., et al.: 2012, acpol 52, 18. [4] hardee, p.e.: 2000, apj 533, 176. doi:10.1086/308656 [5] hardee, p.e.: 2003, apj 597, 798. doi:10.1086/381223 [6] hardee, p.e.: 2006, in proceedings of relativistic jets: the common physics of agn, microquasars and gamma-ray bursts, eds.: p.a. hughes and j.n. bregman, aip conference proceedings 856, 57. [7] hardee, p.e.: 2011, in proceedings of iau symposium 275: jets at all scale, eds.: g. romero, r. sunyaev and t. belloni, iau conference series 275, 41. [8] hummel, c.a., muxlow, t.w.b., krichbaum, t.p., et al.: 1992, a&a 266, 93. [9] krichbaum, t.p., hummel, c.a., quirrenbach, a., et al.: 1990, a&a 230, 271. [10] lister, m., aller, h.d., aller. m.f., et al.: 2009, aj 137, 3718 [11] lobanov, a.p., krichbaum, t.p., witzel, a., et al.: 1998, a&a 340, 60. [12] lobanov, a.p., krichbaum, t.p., witzel, a., zensus, j.a.: 2006, pasj 58, 253. [13] mart́ı-vidal, i., marcaide, j.m., alberdi, a.: 2011, a&a 533, a111. [14] mizuno, y., hardee, p.e., nishikawa, k.-i.: 2011, apj 734, 19. doi:10.1088/0004-637x/734/1/19 [15] nakamura, m., meier, d.l.: 2004, apj 617, 123. doi:10.1086/425337 [16] otterbein, k., krichbaum, t.p., kraus, a., et al.: 1998, a&a 334, 489. [17] perucho, m.. mart́ı, j.m., hanasz, m.: 2005, a&a 443, 863. [18] perucho, m., lobanov, a.p., mart́ı, j.m., hardee, p.e.: 2006, a&a 456, 493. [19] perucho, m., lobanov, a.p.: 2007, a&a 469, l23. [20] perucho, m.: 2012, in proceedings of high energy phenomena in relativistic outflows iii (heproiii), eds. j.m. paredes, m. ribó, f.a. aharonian and g.e. romero, ijmps 8, 241. [21] perucho, m., kovalev, y.y., lobanov, a.p., hardee, p.e., agudo, i.: 2012a, apj 749, 55. doi:10.1088/0004-637x/749/1/55 [22] perucho, m., mart́ı-vidal, i., lobanov, a.p., hardee, p.e.: 2012b, a&a 545, a65. discussion sergio colafrancesco: is there any radio polarization measurement that can be used to better describe the helical structure of the jet and, if so, what are the constraints that can be set on the acceleration mechanisms at the base of the jet? manel perucho: krichbaum et al. (1990) reported polarization measurements and claim that the field is aligned with the jet axis. if their interpretation is correct, it would be difficult to attach the helical morphology of the jet to the magnetic field. nevertheless, new polarization measurements should be performed to check whether the magnetic field plays any crucial role in the generation of the helical structure. regarding your second question, it is difficult to observe the acceleration region in this jet, but we have evidences of component acceleration in other agn jets, included in the mojave sample. herman marshall: if the perturbations are unstable and disrupt the jet at kpc scales, how do you explain that most jets seem to propagate to tens or hundreds of kpc? manel perucho: in that sense, this is a unique object, because it is classified as an frii in terms of its radio luminosity, but its morphology denies (see perucho et al. 2012b). this is one of the reasons why we think that, in this sole case, the jet could be destroyed by the growth of the instability, unlike all other known frii jets for which we can observe the kiloparsec scale structure. 268 http://dx.doi.org/10.1093/mnras/169.3.395 http://dx.doi.org/10.1086/308656 http://dx.doi.org/10.1086/381223 http://dx.doi.org/10.1088/0004-637x/734/1/19 http://dx.doi.org/10.1086/425337 http://dx.doi.org/10.1088/0004-637x/749/1/55 introduction evidence for waves in the jet of s5 0836+710 discussion on the nature of the waves the case of s5 0836+710 the core conclusions 230 acta polytechnica ctu proceedings 2(1): 230–233, 2015 230 doi: 10.14311/app.2015.02.0230 life after eruption: best of 2009–2013 c. tappert1, a. ederoclite2, l. schmidtobreick3, n. vogt1 1departamento de f́ısica y astronomı́a, universidad de valparáıso, chile 2centro de estudios de f́ısica del cosmos de aragón, teruel, spain 3european southern observatory, santiago, chile corresponding author: claus.tappert@uv.cl abstract from our ongoing survey to study the post-nova population we present details on the four objects v728 sco, ar cir, v972 oph and x cir. keywords: cataclysmic variables novae individual: v728 sco ar cir v972 oph x cir. 1 introduction in 2009 we have begun a survey on post-novae that had erupted before 1980, in order to address the lack of identified post-nova systems. scope, methods and the current state of the survey are presented by ederoclite et al. elsewhere in this volume. in the present article we take a closer look at four objects from our survey with peculiar properties that deserve further investigations. a detailed analysis of three of these systems, v728 sco, ar cir and v972 oph, can be found in tappert et al. (2013a, b), and we here only briefly summarize the results. 2 v728 sco the cv corresponding to nova sco 1862 was recovered as a v = 18.5 mag object roughly 2 arcmin north-west of its suspected position (tappert et al. 2012). its spectrum presents – for an old nova – unusually strong emission lines. photometric time-series revealed the object to be eclipsing with an orbital period porb = 3.32 h. this places v728 sco within the regime of the sw sex type systems, cvs that are characterized by very high mass-transfer rates ṁ (e.g., rodŕıguez-gil et al. 2007a, b; see also schmidtobreick & tappert, this volume). furthermore, old novae in general are expected to run high ṁ due to irradiation of the secondary star by the eruption-heated white dwarf (kovetz et al. 1988), and in general this is confirmed by observations (iben et al. 1992). for example, the old nova rr pic, with porb = 3.48 h, does indeed share the characteristics of an sw sex star (schmidtobreick et al. 2003a, 2008). v728 sco, on the other hand, appears to have a lower ṁ than expected. evidence for this does not only stem from the spectroscopic appearance, but also from the long-term behaviour that shows the system to vary between a low and a ∼1.5 mag brighter state. while the data coverage is still very sparse, it looks like this brighter state is in general short-lived and bears resemblance to the outbursts of dwarf novae. analysis of one eclipse that was observed in the low state provided an estimate of the radius of the eclipsed source to r = 0.09 r�, which is significantly larger than any feasible solution for a white dwarf. we interpret this result as the presence of a hot inner disc, such as has been invoked by schreiber et al. (2000) to explain the low-amplitude high-frequency outbursts that are observed in some post-novae and nova-like stars (e.g., honeycutt et al. 1998), and would also fit the longterm behaviour of v728 sco. our eclipse data provide the first direct evidence for the presence of such disc. 3 ar cir ar cir was a comparatively slow nova that erupted in 1906. it was recovered by duerbeck & grebel (1993). time-series spectroscopy taken by us on three consecutive nights in 2012 yielded porb = 5.14 h. the spectrum shows a moderately strong hα emission line on a red continuum, the latter being very probably entirely caused by interstellar reddening rather than due to the contribution of the secondary star. the r-band brightness shows a clear modulation with porb and an amplitude of ∼0.3 mag, indicating that the inclination is comparatively high. the hα line profile shows an intriguing variability in that at certain orbital phases, and strongest at phase 0.5 (corresponding to the maximum of the r-band light curve), a p cyg component becomes visible in the form of a high-velocity blue absorption and a red emission component. we interpret 230 http://dx.doi.org/10.14311/app.2015.02.0230 life after eruption: best of 2009–2013 this as an optically thick outflow and determine a rough estimate of the projected outflow velocity to 700 ± 100 km/s. 4 v972 oph time-series spectroscopic observations of this post-nova (nova oph 1957) yield an orbital period porb = 6.75 h thus making it a member of the minority of novae with comparatively long orbital periods (see ederoclite et al., this volume). examination of the profile of the hα emission line reveals an additional emission at ∼6580 å. this component moves roughly parallel to the main hα component. this practically excludes scenarios of an additional hα component from the secondary star or from the hot spot, as well as a nebular line like [nii] λ6584. the absence of an absorption line blueward of hα lets an origin in an outflow, such as assumed for ar cir, also appear unlikely. instead we tentatively identify that line with the cii λλ6578/6583 doublet. to our knowledge, this is the first time that this line is observed in a cv in this form (it had also be identified as originating in the outflowing material of the helium nova v445 pup; iijima & nakanashi 2008). while carbon emission has been observed before in some post-novae (e.g., schmidtobreick et al. 2003b, bianchini et al. 2012), this concerns mostly the blue part of the spectrum. unfortunately the available spectra of v972 oph by zwitter & munari (1996) and ringwald et al. (1996) that cover that range have too low s/n to confirm the presence of such lines in v972 oph. the weakness of the hα emission line (which has an equivalent width of 2 å) certainly helped in the detection of the cii line. this raises the question whether this line is not more frequently present in cvs, but hidden away in the wings of a stronger hα emission. a quick examination of seven novae finds three more systems with likely excess emission at ∼6580 å. as a caveat we note that this list includes ar cir, where we find an outflow as a more likely explanation. however, the other systems lack an accompanying blue emission or absorption component that would suggest such phenomenon as the origin. 5 x cir the eruption of nova cir 1927 was reported by becker (1929). the aftermath of the nova is little studied. duerbeck (1987) classifies it as a slow nova with t3 = 170 d. woudt & warner (2002) identified a possible candidate for the post-nova due to short-term variability, but a spectrum taken by mason & howell (2003) revealed that object to have a reddish continuum without emission lines. our ubvr photometry from may 2009 (fig. 1, top) allows for a number of candidates based on colour and distance from the reported coordinates. in 2012 we obtained spectroscopic data for five of them with the mos mode of fors2 at the eso-vlt (ut1). the post-nova was confirmed to be an object roughly 1.2 arcmin north-west of its suspected position. the spectrum shows comparatively strong emission lines (equivalent width of hα ∼30 å) of the balmer and hei series (fig. 1, bottom). 0.0 0.5 1.0 1.5 v −r [mag] −0.5 0.0 0.5 1.0 1.5 u − b [m ag ] 4000 5000 6000 7000 8000 wavelength [å] 5 10 fl ux [1 0− 17 er g cm −1 s− 1 å −1 ] figure 1: top: colour-colour diagram of the field (4.5×4.5 arcmin) of x cir. the confirmed post-nova is marked by a circle. bottom: low-resolution spectrum of the post-nova. while being situated in a promising place in the colour-colour diagram, the later confirmed post-nova was not our best candidate, but in fact rather represented the very bottom of our list. the reason for this is that our photometric data showed a larger point-spread function (psf) than for the other stars in the field, indicating an extended object. this was later confirmed by the 2d spectroscopic data. an examination of the latter showed that the emission lines appear to be confined to the one part of the spectroscopic psf that corresponds to the eastern part of the photometric psf. our preliminary conclusion is therefore that the extension is not due to a shell, but that this is an unresolved (< 0.5 arcsec) visual binary. the spectrum of x cir presents a prominent heii 4686 line, and even, albeit much weaker, heii 5411 (fig. 2). such strong presence of heii is often a signature of a magnetic system. on the other hand, the hei lines are distinctively double-peaked with a deep central valley, indicating the presence of an accretion disc. a possible explanation is that x cir is an intermediate polar. the heii 5411 line is also a transient feature. in our three spectra, taken with a time separation of ∼3 h between the first and the second, and ∼24 h between the second and the third, the line is strongest in the first (which is the one in fig. 2), not detected in 231 c. tappert et al. the second, and weakly present in the third spectrum (fig. 1). since the individual integration times amount to 15 min, this could be an orbital effect. the heii lines and the balmer lines are single-peaked, suggesting that at least a major part of their profile has an origin different from that of hei. 5400 5600 5800 wavelength [å] 1.0 1.2 n or m al is ed fl ux heii hei? ? 7000 7200 7400 wavelength [å] hei ? figure 2: close-up on the spectrum of x cir. the label mark the line identifications; a question mark is used for the three unidentified lines. note the deep central valleys in the double-peaked profile of the two present hei lines. we furthermore find three emission lines that we have not yet been able to identify (fig. 2). taking into account the observed shift of the identified lines, we estimate their corresponding rest wavelengths to ≥5678, ≥5805, ≥7233, respectively. examining lists of spectral lines (e.g., coluzzi 1999) does not present obvious suspects for an identification. we note that the profiles are also single-peaked, so that these probably do not originate exclusively in the accretion disc. we derive the ’quiescent’ brightness of x cir in the v filter to 19.3 mag. the reported photographic value of the eruption maximum is 6.5 mag (duerbeck 1987). assuming that the effect of the difference between the filters is < 0.5 mag, this yields an eruption amplitude > 12 mag. this places it a bit off the fit to the rateof-decline / eruption-amplitude relation (ederoclite et al., this volume; note that x cir is not yet included in their figure), but still within the larger scatter. 6 summary we have presented four post-novae with apparently peculiar properties. v728 sco is one of the few objects that defies the general trend that post-novae are cvs with very high mass-transfer rates (ṁ). finding such objects will be very important to answer the question whether post-novae in general have high ṁ as a consequence of the nova eruption, or if high ṁ cvs are just more likely to erupt as a nova. v728 sco is furthermore deeply eclipsing, which presents an excellent and rarely found opportunity to determine accurate system parameters of a nova. ar cir, on the other hand, while with more than 100 yr having passed since its eruption can already be counted among the ’old’ old novae, apparently still drives such high ṁ that it causes an outflow of material that is visible in the optical spectrum. since our data only covers the spectral range next to hα it would be interesting to examine other spectral ranges and lines for this phenomenon to gain more information on the outflow. in v972 oph we detect an unusual emission line that we attribute to carbon. we argue that such line could in principle be more frequent in cvs because it can be easily hidden in the wings of the usually strong hα emission that is exceptionally weak in v972 oph. the currently available data on the blue spectral range has too low s/n to examine it for other tracers of the presence of carbon in v972 oph, thus a higher quality spectrum of that region would be most welcome. the carbon line in v972 oph moves parallel to hα and thus likely originates in the accretion disk or the bright spot, or on the secondary star itself. in any case it represents material from the secondary. it was either accreted from the expelled material during the nova eruption or produced in the secondary, which then could not have formed as a late-type main-sequence star, but must have undergone some nuclear evolution prior to its semi-detached cv phase. thus, the study of carbon in (not only) post-novae bears relevance for our understanding on cv evolution. the results on x cir are still somewhat preliminary. the strong balmer lines argue for a comparatively low ṁ , the prominent presence of heii could point to a magnetic white dwarf, but at least is evidence for a hot region somewhere in the system, while the double-peaked hei profiles indicate the presence of an accretion disc. a number of emission features yet remain to be identified which means that these lines are at least very rarely observed in cvs. finally, the spectral appearance, the transient nature of heii 5411 and the double-peaked hei lines suggest a high inclination. there is therefore a good chance that the orbital period will be accessible comparatively easily via time-series photometry. we hope that this presentation motivates further studies of those systems. while their properties may appear peculiar, they might not be exclusive to those objects. because the number of detailed studies on post-novae is still fairly small, we cannot yet be certain if they are more representative of the rule or the exception. acknowledgement this research was supported by fondecyt regular grant 1120338 (ct and nv). ae acknowledges support by the spanish plan nacional de astrononomı́a y astrof́ısica under grant aya2011-29517-c03-01. 232 life after eruption: best of 2009–2013 references [1] becker, f.: 1929, astron. nachr., 237, 71. [2] bianchini, a., saygac, t., orio, m., et al.: 2012, a&a, 539, a94. [3] coluzzi, r.: 1999, vizier online data catalog, 6071. [4] duerbeck, h.w.: 1987, space sci. rev., 45, 1. doi:10.1007/bf00187826 [5] duerbeck, h.w., grebel, e.k.: 1993, mnras, 265, l9. doi:10.1093/mnras/265.1.l9 [6] honeycutt, r.k., robertson, j.w., turner, g.w.: 1998, aj, 115, 2527. [7] iben, jr., i., fujimoto, m.y., macdonald, j.: 1992, apj, 384, 580. doi:10.1086/170900 [8] iijima, t., nakanashi, h.: 2008, a&a, 482, 865. [9] kovetz, a., prialnik, d., shara, m.m.: 1988, apj, 325, 828. [10] mason, e., howell, s.b.: 2003, a&a, 403, 699. [11] ringwald, f.a., naylor, t., mukai, k.: 1996, mnras, 281, 192. 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[21] woudt, p.a., warner, b.: 2002, in: classical nova explosions, hernanz, m. & josé, j., eds., aip conf. proc., vol. 637, p.532. [22] zwitter, t., munari, u.: 1996, a&as, 117, 449. discussion christian knigge: a comment on v728 sco: i think this is totally consistent with being a ”normal” sw sex star. it has the same v-shaped eclipse in the high state (and may be self-occulting), and several sw sex stars, like dw uma, also show high-state / lowstate behaviour. claus tappert: it is true that the high-state eclipse very much resembles that of sw sex stars. but i would argue that the other properties do not. we do not see any high-velocity wings (this might arguably be due to the quality of the spectra), and the emission lines are distinctively double-peaked. we need more long-term data to see if the system spends more time in low or high state, but so far my best bet would be that v728 sco is in a somewhat transitory phase, not quite sw sex, not quite dwarf nova. 233 http://dx.doi.org/10.1007/bf00187826 http://dx.doi.org/10.1093/mnras/265.1.l9 http://dx.doi.org/10.1086/170900 http://dx.doi.org/10.1111/j.1365-2966.2006.11245.x http://dx.doi.org/10.1111/j.1365-2966.2007.11743.x http://dx.doi.org/10.1046/j.1365-8711.2003.06523.x http://dx.doi.org/10.1111/j.1365-2966.2008.13641.x introduction v728 sco ar cir v972 oph x cir summary acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0072 acta polytechnica ctu proceedings 7:72–75, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app semi–automated assessment of micromechanical properties of the metal foams on the cell-wall level nela krčmářováa,b,∗, jan šleichrta, tomáš doktora, daniel kytýřa,b, ondřej jiroušeka a czech technical university in prague, faculty of transportation sciences, konviktská 20, prague 1, 155 00, czech republic b the institute of theoretical and applied mechanics as cr, prosecká 76, prague 9, 190 00, czech republic ∗ corresponding author: krcmarova@fd.cvut.cz abstract. metal foams are innovative porous material used for wide range of application such as deformation energy or sound absorption, filter material, or microbiological incubation carrier. to predict mechanical properties of the metal foam is necessary to precisely describe elasto–plastic properties of the foam on cell–wall level. indentation with low load is suitable tool for this purpose. in this paper custom designed instrumented microindentation device was used for measurement of cell-wall characteristics of two different aluminium foams (alporas and alcoras). to demonstrate the possibility of automated statistical estimation of measured characteristics the device had been enhanced by semi-automatic indent positioning and evaluation procedures based on user-defined grid. vickers hardness was measured on two samples made from alporas aluminium foam and one sample from alcoras aluminium foam. average vickers hardness of alporas foam was 24.465 hv1.019 and average vickers hardness of alcoras was 36.585 hv1.019. keywords: metal foam, vickers hardness, cell-wall, indentation under low loads. 1. introduction metal foams are biomimetic porous materials with cellular inner structure that find wide range of applications from deformation energy absorption to noise attenuation, where their very high specific stiffness greatly improves overall effectiveness of constructions [1, 2]. homogenization approach has been proposed as a method for prediction of their mechanical properties on both cell-wall level and at macroscale [3– 6]. however for calculation of macroscopic (effective) mechanical properties by homogenization, mechanical characteristics at the lower level of the foam’s hierarchical microstructure (i.e. cell-wall level) have to be assessed with high precision and reliability. here microindentation is a suitable tool for assessment of required elasto-plastic material properties (for cellwall thicknesses from few hundreds of microns) with the possibility for extension to statistical estimation when automated indents’ positioning and evaluation procedures are introduced. 2. materials and methods 2.1. specimen description and preparation closed-cell aluminium foams with similar compound al 97.0 %, ca 1.5 %, ti 1.5 % (measured using energydispersive x-ray spectroscopy) pore size 2 − 4 mm and wall thickness 100 − 200µm sales denominated as alporas® (shinko wire co., ltd., japan) and sample 1 sample 2 sample 3 material alporas alcoras alporas width 48 mm 41 mm 44 mm height 21 mm 21 mm 23 mm thickness 10 mm 11 mm 13 mm table 1. dimensions of the specimen alcoras® (alcarbon, germany) were subjected for the testing [7]. inner structure of aluminium foam is depicted in fig. 1. figure was obtained using scanning electron microscopy mira ii (tescan, czech republic). region of interest was chosen according to avoid large pores and structural defect. the structural defects were mainly connected with alcoras sample. from the delivered slabs cuboids with minimal thickness of 12 mm (to ensure sample integrity) were sectioned using water cooled oscillating diamond saw (isomet 1000, buehler gmbh, germany). dimensions of each specimen are listed in tab. 1. low cutting speed 3 mm · min−1 minimised surface damage. samples were embedded into mounting compound (varikleer, buehler gmbh, germany). grinding and polishing procedure employing silicon carbide grinding discs (320, 800, 1200, 4000 grains per square inch) and diamond suspension (1µm) was performed to remove 1 mm surface layer which could be influenced by sectioning and to obtain plan-parallel faces 72 http://dx.doi.org/10.14311/app.2017.7.0072 http://ojs.cvut.cz/ojs/index.php/app vol. 7/2017 assessment of micromechanical properties of metal foams figure 1. inner structure of aluminium foam obtained by scanning electron microscopy. with minimal surface roughness necessary for proper indentation. 2.2. indentation testing 2.2.1. indentation device description indentation testing was performed using custom designed indentation device developed and constructed on department of mechanics and material fts ctu. indentation device is suitable for hardness measurement by low loads from 10 n up to 100 n. limitation of the device by applying lower loads are: i) inaccuracy of the load recorded by load–cell and ii) insufficient accuracy of the control of the indentation axis. device consists of three independent motorised axes. two of them are designed for precise positioning of the specimen with accuracy 10µm. third axis is indentation axis equipped by load–cell with positioning accuracy 1.5µm. device is controlled by load or displacement using gnu/linux software system linuxcnc with custom made graphical user interface. device is equipped with ccd camera (manta g–504b, avt, germany) with a resolution of 2452 × 2056 px attached to a light microscope (navitar imaging, inc., usa) that provided a magnification of up to 24 ×. the acquisition of the projections was controlled by in-house-built opencv based plug-in integrated to control software [8]. indentation device is depicted on fig. 2. this camera is used for the indent place estimation as well as to make a photo of the indent that is than used for hardness measurement. due to high resolution ccd camera, calibrated indentation tip alignment and precise positioning of the specimen, indentation of the selected location of the specimen’s surface is allowed with high accuracy. for verification of the device accuracy of hardness measurement indentation in calibration hardness plate was performed. device overall error estimated by calibration meafigure 2. experimental setup. surement was 1.3 %. maximal measurement error for indentation devices is according to standard set to 3 %. it can be advantageously used for measuring hardness of metal foams because indentation is possible only in places with a sufficient width and depth of the specimen, which means joints of the walls. 2.2.2. experiment procedure description suitable places for indentation on the sample surface were identified using ccd camera and subsequently indentation was automatically performed at these selected locations. after the indentation image data of each indent were captured. the detail of an indent is depicted on fig. 3. indentation load was set to 10 n and this value was reached in 10 s. first indent was used as a testing indent to find indentation speed to respect the condition of reaching maximal force value in 10 s. this indent was removed from data set and hardness value of this indent was not evaluated. all other indents were displacement controlled with given speed identified by the testing indentation. course of the indentation was therefore: i) 10 s loading up to 10 n, ii) 10 s holding on the indentation load and iii) unloading with the same speed as the loading phase. on each specimen was created a series of about 50 indents on the interconnections of the walls. the foam microarchitecture with poresize 2 − 4 mm ensure avoiding that the plastic zones of the indents don’t affect each other. because of size of interconnection and limited minimal indentation force normative 2.5× diameter distance from sample edge can’t be meet during experimental procedure. size of thus generated imprints of the indenter was about 270µm and their 73 n. krčmářová, j. šleichrt, t. doktor et al. acta polytechnica ctu proceedings figure 3. right: marked area of the imprint obtained by semi–automatic evaluation method. depth was about 39µm. 2.2.3. evaluation of the experimental data positioning accuracy of the indentation axis does not allow automated evaluation of the hardness from the full position-load curve using oliver–pharr method [9]. therefore hardness was assessed using traditional method by measuring the imprint dimensions and evaluated as vickers hardness: hv = f a ≈ 0.1819f d2 , (1) where f is indentation load in n, a is resulting indentation area of the imprint of the indenter in mm2 and d is average length of the diagonal of the imprint of the indenter in mm. as indentation load is taken the maximal force value registered by the load– cell. length of the diagonals in pixels was measured from the image of each imprint of the indenter using semi–automatic method in matlab software. image of the calibration pattern was used for conversion of the diagonal length in pixels to millimetres. highlighted imprint of the indenter is depicted on fig. 3 3. results elasto-plastic material properties of two types of aluminium foam was measured by vickers hardness. indentation was performed on cell walls and their connections to ensure sufficient place for indentation. in order to get precise information about micromechanical properties of the foam about 50 indents were carried out at each of the three specimens. due to foam nature of specimens the under surface area can be formed by cavity which is not visible on the surface and thus some indents were deformed and these vickers hardness values are omitted from the data set. those indents are usually easily recognised by highly deformed shape of indents. success of the indention was about 60 %. hardness values calculated using equation 1 are listed in tab. 2. sample 1 sample 2 sample 3 material alporas alcoras alporas indent 1 24.630 41.507 18.149 indent 2 33.008 35.490 29.839 indent 3 25.204 36.360 24.817 indent 4 23.027 32.990 23.672 indent 5 21.665 31.514 20.633 indent 6 22.818 34.447 22.967 indent 7 22.211 30.213 23.779 indent 8 24.547 30.254 16.826 indent 9 35.845 49.110 15.233 indent 10 33.856 47.130 13.301 indent 11 27.067 45.138 15.093 indent 12 33.404 28.928 24.319 indent 13 25.699 38.507 33.361 indent 14 21.559 24.547 13.418 indent 15 25.510 41.085 25.044 indent 16 27.996 37.927 16.167 indent 17 32.651 42.484 18.410 indent 18 29.958 30.323 19.584 indent 19 31.472 32.506 24.322 indent 20 21.663 43.721 21.050 indent 21 23.802 34.975 24.192 indent 22 30.054 32.557 31.487 indent 23 34.450 28.754 15.765 indent 24 29.011 45.065 26.474 indent 25 21.114 33.645 15.346 indent 26 40.693 24.999 indent 27 39.462 26.053 indent 28 35.017 indent 29 39.386 indent 30 33.801 avarage 21.641 36.585 27.289 table 2. values of measured vickers hardness by indentation load 10 n as can be seen from the hardness values summarised in tab. 2 vickers hardness of alporas aluminium foam is about 30 % lower than vickers hardness of alcoras aluminium foam. 3.1. comparative measurement to ensure reliability of the indentation process with non-standarded indents size digital microscope vhx74 vol. 7/2017 assessment of micromechanical properties of metal foams figure 4. indent surface inspection and indent profile reconstruction equipped by digital microscope. 5000 (keyence, japan) was employed for indented surface inspection and indent profile reconstruction (see fig. 4). indentation depth ≈ 40µm was obtained from indent profile using keyence proprietary software. this value corresponds to results of the analysis presented in 2.2.2. the profile is not significantly effected by surrounding embedding resin. 4. conclusions vickers hardness measurement was performed on three samples of aluminium foam on cell-wall level. one sample was aluminium foam alcoras and two samples were made of aluminium foam alporas. about 50 indents were created on each sample on the cell– walls or their interconnections with indentation load 10 n. success of the indentation was about 60 % other indents were deformed due to wrong position on the sample surface what was not possible to avoid prior the indentation. indentation was carried out using custom designed indentation device equipped with load–cell and ccd camera. camera was used for identification of appropriate place for indentation and for acquisition of image data of each imprint. vickers hardness was evaluated from image data using semi–automatic procedure in software matlab. average vickers hardness of the sample 1 (alporas foam) was 21.641 ± 5.496hv1.019, where hv is denotation for vickers hardness and value 1.019 indicates indentation load in kgf. average vickers hardness for sample 3, which was also made from alporas, was 27.289±4.731hv1.019. average vickers hardness of the third sample, which was made from alcoras foam, was 36.585±6.061hv1.019. vickers hardness of alcoras aluminium foam is about 30 % higher than vickers hardness of alporas aluminium foam. information about elasto–plastic properties of the aluminium foams alporas and alcoras on cell–wall level can be used for calculation of macroscopic mechanical properties by homogenization. acknowledgements the research was supported by the czech science foundation (research project no. 15-15480s), by czech technical university in prague (research project no. sgs15/225/ohk2/3t/16) and by institutional support rvo: 68378297. keyence is kindly acknowledged for providing of digital microscope vhx-5000. references [1] t. miyoshi, m. itoh, s. akiyama, a. kitahara. alporas aluminum foam: production process, properties, and applications. advanced engineering materials 2(4):179–183, 2000. doi:10.1002/(sici)15272648(200004)2:4<179::aid-adem179>3.0.co;2-g. [2] m. idris, t. vodenitcharova, m. hoffman. mechanical behaviour and energy absorption of closed-cell aluminium foam panels in uniaxial compression. materials science and engineering: a 517(1–2):37 – 45, 2009. doi:http://dx.doi.org/10.1016/j.msea.2009.03.067. [3] p. koudelka, t. doktor, j. valach, et al. effective elastic moduli of closed-cell aluminium foams homogenization method. 11th imeko tc15 youth symposium on experimental solid mechanics 2012 pp. 244–250, 2012. [4] s. li, d. qian, m. l. and. multiscale mechanics and mechanics of biological materials. [5] v. králík, j. němeček. micromechanical properties of porous material based on metal foam. chemicke listy 105(17):s672–s675, 2011. [6] m. geißendörfer, a. liebscher, c. proppe, et al. stochastic multiscale modeling of metal foams. probabilistic engineering mechanics 37:132–137, 2014. doi:10.1016/j.probengmech.2014.06.006. [7] t. fíla, d. kytýř, p. koudelka, et al. micro-mechanical testing of metal foam cell walls using miniature threepoint bending. key engineering materials 586:120–124, 2014. doi:10.4028/www.scientific.net/kem.586.120. [8] g. bradski. the opencv library. dr dobb’s: the world of software development 2000. http://www.drdobbs.com/open-source/the-opencvlibrary/184404319. [9] w. oliver, g. pharr. an improved technique for determining hardness and elastic modulus using load and displacement sensing indentation experiments. journal of materials research 7(06):1564–1583, 1992. 75 http://dx.doi.org/10.1002/(sici)1527-2648(200004)2:4<179::aid-adem179>3.0.co;2-g http://dx.doi.org/10.1002/(sici)1527-2648(200004)2:4<179::aid-adem179>3.0.co;2-g http://dx.doi.org/http://dx.doi.org/10.1016/j.msea.2009.03.067 http://dx.doi.org/10.1016/j.probengmech.2014.06.006 http://dx.doi.org/10.4028/www.scientific.net/kem.586.120 acta polytechnica ctu proceedings 7:70–73, 2017 1 introduction 2 materials and methods 2.1 specimen description and preparation 2.2 indentation testing 2.2.1 indentation device description 2.2.2 experiment procedure description 2.2.3 evaluation of the experimental data 3 results 3.1 comparative measurement 4 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2016.6.0028 acta polytechnica ctu proceedings 6:28–33, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app mapping the surroundings as a requirement for autonomous driving martin steininger∗, christoph stephan, christian böhm, fabian sauer, roland zink faculty of electrical, media and computer engineering, deggendorf institute of technology, 94469 deggendorf, germany ∗ corresponding author: martin.steininger@stud.th-deg.de abstract. motivated by the hype around driverless cars and the challenges of the sensor integration and data processing, this paper presents a model for using a xbox one microsoft kinect stereo camera as sensor for mapping the surroundings. today, the recognition of the environment of the car is mostly done by a mix of sensors like lidar, radar and cameras. in the case of the outdoor delivery challenge robotour 2016 with model cars in scale 1 : 5, it is our goal to solve the task with one camera only. to this end, a three-stage approach was developed. the test results show that our approach can detect and locate objects at a range of up to eight meters in order to incorporate them as barriers in the navigation process. keywords: microsoft kinect, mapping, 3d mapping, robotour, autonomous driving. 1. introduction in addition to the extensive launch of full electric vehicle (fev) autonomous driving is deemed to be a key research and development trend in the automotive industry. the entire industry is working on the topic and has already developed first solutions for automatic braking, line keeping (i.e. audi “active lane assist” or bmw “active assist”) or even autopilots for driverless cars like tesla motors’ “autopilot” or google’s “driverless car” [1]. the used navigation and self-driving algorithms run on maps [2] and require very accurate digital (geo-)data of the environment [3]. therefore, the spatial coverage of the surroundings as a basis for autonomous navigation of the vehicle is common to all applications. consequently, autonomous driving – regardless of the respective task such as automatic braking, adaptive cruise control, lane keeping or autonomous driving – requires detection and imaging of the space which it will pass through. photo cameras, lidar-, radaror other sensors continuously detect and measure the surrounding of the car, creating a digital spatial image of the area (map). combined with positioning services like gps or galileo, the location of the vehicle can be determined and set in relation to surrounding objects such as other vehicles or obstacles. however, it is not an ordinary cartographic map resulting from the permanent mapping process but digital images that are stored temporarily as server frames for the navigation. the navigation of the car finally relies on mathematical functions (algorithms) to pass through the digital and real space on the shortest (spatial) or fastest (time) way. this paper addresses the issue of the space detection which is considered as an essential basis of autonomous driving and robot navigation (see for example [4]) and describes the use of a microsoft x-box one kinect stereo camera for autonomous driving for the outdoor delivery challenge robotour 2016 (robotika.cz). we present an approach for mapping the surroundings including the three steps (1) 3d capturing, (2) projection and filtering and (3) object detection. the hardware and the approach are implemented on a four wheel drive off-road buggy, scale 1 : 5. the main hardware consists of a congatec ts180 com express module. for the main processing, it communicates with the x-box one kinect and a raspberry pi and displays the crucial information on a krämer v-800 touchscreen. the raspberry pi reads the sensor values from the gps and the bosch bno055 and transmits them to the congatec module. it receives the steering and speed values from the congatec module, which are transmitted to the freescale kl25z microcontroller, which in turn controls the rc-car model via pwm signals. 2. approach the development path of the approach to map the surroundings for an autonomous driving vehicle should be well-defined to avoid inconsistencies. the first step is answering the question which hardware will be used to detect objects. with the goal to use only a kinect camera as sensor, the approach relies on the processing of the depth, and standard images. both data represent a 2d respectively 3d model of the environment. the approach is characterised in three development steps: • 3d capturing, • projection, • object recognition. 28 http://dx.doi.org/10.14311/app.2016.6.0028 http://ojs.cvut.cz/ojs/index.php/app vol. 6/2016 mapping the surroundings as a requirement for autonomous driving 3d capturing obstacle detec on projec on and ltering kinect camera figure 1. spatial mapping of the current surroundings. it is developed to simplify complex processes, describe them in a proper way and visualize all of the main development steps in a manner that is easy to understand. according to the development steps, the approach is divided into three processes, see figure 1. at first, the kinect camera films the space in front of the vehicle in order to gather potential obstacles. the second step contains the projection of the depth images on a 2d ground plane. at last, the obstacles or object will be recognized during the third step. the three main steps will be explained below. 3. related work in 2002 sebastian thrun (see [5]) showed that the problem of terrain mapping is to generate a spatial model of a robot’s or vehicle’s environment using sensors and cameras. concerning this point there are several more subproblems: • measurement noise, • robot must choose its way during mapping process, • environment changes over time, • possibly the hardest problem — the so called data association problem: correspond sensor measurements to the same physical object in the real world. “mapping is largely considered the most difficult perceptual problem in robotics.” [5, p. 6]. in 1989 herbert et al. already presented the so called locus algorithm to build terrain maps based on a single active range sensor, by “computing the intersection of the surface observed by the sensor with the vertical line passing through (x, y)” [6, p. 998]. frankhauser et al. [4, p. 2] introduced an elevation mapping approach from a “robot-centric perspective” with relative distances to the robot and a permanent update process of the entire elevation map with information about the motion of the robot. kleiner and dornhege presented their autonomous driving vehicle for urban search and rescue (usar) with two different methods. first the rapid mapping of a large-scale environment by wheeled robots, and second the mapping of rough terrain by tracked robots [7]. hornung et al. [6] developed an open source library to represent the environment in memory using octrees. the cells of the discretized space can have one of the following states: unknown, free or occupied. to map the sensor data into the octree they use a probabilistic sensor model. thrun et al. [8] describes stanley, the winner of the 2005 darpa grand challenge. the robot was built by stanford university researchers and uses laser figure 2. overview of the kinect camera. range finders as well as radar sensors for sensing the environment. the evaluation of the sensor data is supported by artificial intelligence and machine learning algorithms. 4. 3d capturing as a 3d sensor is a rather expensive component, the kinect is a cheap alternative compared to the functions it provides. the camera is doing most of the calculations on its own soc, thus reducing the processing effort for the main unit. the first version of microsoft kinect camera was developed by prime sense, an israeli 3d sensing company, which was bought by apple in 2013. after that, microsoft created its own system based the existing prime sense technology [9]. 4.1. overview the kinect camera has an array of sensors, which can be divided into three categories: a depth sensor (green), a colour sensor (red) and an audio sensor (blue), as seen in figure 2. the audio sensor is not used for the 3d reconstruction. the colour sensor consists of a cmos camera with an infrared light filter. the main use of the colour sensor is the track detection. the colour image can be mapped with the depth information, although the resolution of the colour sensor is higher than that of the depth sensor. that is the reason why there are multiple colour pixels per one depth pixel. if there are more depth pixel, than colour pixels, the colour pixels need to be split into multiple smaller pixel, with the same information. the depth sensor consists of a cmos camera and an infrared led blaster. the cmos camera is filtered so that it just sees near-infrared light which is emitted by the infrared led blaster. all the information is processed in a specially designed soc (figure 3). this allows the soc to process a depth map containing all the depths for every pixel and map the colour pixel to it. the result of the processing is a data stream containing an audio, a video, and a depth stream. 29 m steininger, c. stephan, c. böhm et al. acta polytechnica ctu proceedings figure 3. 3d reconstruction of the kinect [11, 12]. 4.2. 3d reconstruction there are multiple ways of reconstructing the depth information from an image. the classic way needs two calibrated cameras at a defined distance. this allows for calculating the distance to the object with trigonometry formulas. the difficulty will be in differencing the objects resulting in the so called correspondence problem which “refers to the problem of ascertaining which parts of one image correspond to which parts of another image, where differences are due to movement of the camera, the elapse of time, and/or movement of objects in the photos.” [10]. the kinect overcomes this problem by using a method called “time of flight”. in this method the travel time of infrared light, which is emitted by a led, is measured for each pixel, as seen in 3. “a strobed infrared light illuminates the scene, the light is reflected by obstacles, and the time of flight for each pixel is registered by the infrared camera. internally, wave modulation and phase detection is used to estimate the distance to obstacles (indirect tof)” [13]. the problem is that the infrared light can be washed out by other near-infrared light sources like sunlight, resulting in the kinect not being able to detect the infrared light and losing the depth information. 5. projection and filtering the kinect camera is mounted on the chassis in an arbitrary fixed angle, tilted to the cars chassis. the exact angle in which the camera is mounted to the ground is not known. it can be measured, but to be independent from that setting, the ground plane coefficients, which are returned from the kinect, are used. the coordinate system of the returned 3d point cloud (as camera coordinate system in the following; indicated with a car subscript) does not match with the coordinate system of the car (as car coordinate system in the following; indicated with a camera subscript). in figure 4 both coordinate systems are shown. the body-frame which can be requested from the camera contains a four-dimensional vector representing the floor coefficients by ~pcoeff = (a;b;c;d). figure 4. the camera coordinate system (green) and the car coordinate system (blue) [11, 12]. these coefficients are combined in (1) to receive the plane equation for further mathematical operations: 0 = ax+by + cz +d (1) in a first step, the distance of every point to the ground is calculated. a point is considered to be a part of the ground if a certain limit is not exceeded. therefore they are removed from the point collection if the distance to the ground is smaller than a certain distance. the remaining points are processed in the following steps. in the next step, each frame of the kinect has a resolution of 512 by 424 and can thereby result in a large amount of 3d-pixels. a pixel is returned, if it is in the specified range of the camera. the nearest distance the camera returns a pixel for is about half a meter. the maximum distance is about eight meters. so there are quite a large number of points waiting to be computed. the rather small computing system with limited processing power on the car must handle this in real-time. for the presented project, a real-time reaction is defined with a latency of a few hundred milliseconds. to reach this goal, one issue is making the algorithm faster. this could be realised by: • removing as many points as possible to save energy and processing effort converting the points from one coordinate system to another, • adjusting processes how the data is processed step by step, • using a programming language with small processing overhead. to reduce the further processing effort the points get filtered next. a new parameter named mindistance is introduced in the gui (graphical user interface) where the points must have a greater distance from 30 vol. 6/2016 mapping the surroundings as a requirement for autonomous driving the camera than that value, to prevent recognising parts of the car as obstacles. this is needed due to the current setting of the car. there may be points above the height of the car so that the car can drive beneath. these points get removed if they are above a maximum height from the ground plane which is defined as a parameter named maxheight. obstacles far away are also not interesting for the process at the moment. in the same way points far away are also not interesting and get filtered with an allowed maximum distance named maxdistance. in this section some functions are introduced to simplify the explanation of the coordinate transformation. the first three equations deal with projections. project a vector v onto another vector vonto (2), also a vector v onto a plane e : 0 = (~x− ~r) · ~n (3) and a point with position vector ~x onto a plane (4): fv2v(~vorig, ~vonto) : ~vproj = ( ~vorig � ~vonto |~vonto| ) (2) fv2p(~vorig) : ~vproj = ~vorig − fv2v (~vorig, ~n) · ~n (3) fp2p(~xorig) : ~xproj = ~xorig − fv2v (~xorig − ~r, ~n) (4) next the normalisation is defined in (5): fn(~vorig) : ~vnorm = ~vorig |~vorig| (5) since the source coordinate system of the kinect is in three dimensional space and the destination system is only two dimensional, it is necessary to project every detected 3d-pixel onto the ground plane. in the three dimensional coordinate space of the kinect we define a two dimensional coordinate space for the new coordinate system. the new coordinate system can be seen as a plane in the original space. therefore an origin and also two vectors for the two axes of that coordinate system are needed. the two dimensional coordinate system for the obstacle detection is implemented within the three dimensional coordinate system of the kinect camera. the camera position perpendicular above the ground is origin: ccamera = fp2p(o) with o as the origin of coordinate system. the axes are defined as ex = fn (fv2p ((0; 0;−1))) and ey = fn (fv2p ((−1; 0; 0))). in figure 4 you see the orientation of the axis. now, (6) can be used to project all points into the new car coordinate system: pcar = ( fv2v (pcamera − ccamera, ex) fv2v (pcamera − ccamera, ey) ) (6) next, the obstacle detection will use these projected points and create a barrier along the nearest edge of the recognized obstacles. 6. obstacle detection when implementing algorithms for autonomous vehicles it is mandatory to detect and tag obstacles in front of the craft. as described, a depth image is 0 0.5 1 1.5 2 2.5 3 3.5 4 0 1 2 3 4 5 6 7 8 l o g a ri th m ic s c a lin g o f d is ta n c e distance (m) figure 5. logarithmic distance scaling for image size reduction purposes. provided by the kinect camera from where each single depth pixel is projected to a ground plane with each having the correct distance and position to the camera’s point of view during the first stage of image processing. as a first step, the depth points contributed by the kinect camera and the projection to the ground plane are transformed into a 2d image. the next three steps described in this section include: • distance scaling, • gaussian functions, • and the actual object and obstacle detection. 6.1. distance scaling the project team faced problems concerning computing power: the large number of pixels coming from a depth frame provided by the kinect camera exceeded the available and limited hardware. for the purpose of reducing the computing effort for processing the gaussian function (see subsection 6.2) the project team decided to scale the projected image’s size by its height logarithmically. as shown in figure 5, the scaling of distances allows to have more detailed image information in a closer range to the camera’s origin than in a larger distance to this specific point. the distance we get from the kinect camera is a floating point number, the index we need to reference a pixel within and on the image is an integer. if the distance is only rounded to the next integer value there is one pixel per meter. because of this a parameter is introduced which represents the resolution of the image’s distances. the scaled value is divided by this value to get the index as an integer, after rounding of this new integer we get the correct index value for the image. for example, 0.5m in reality are mapped to an index value of 0.585 after the scaling, while 8m in the real world, which is the kinect camera’s maximum recognition distance, correspond to an index value 3.171 logarithmically scaled. 31 m steininger, c. stephan, c. böhm et al. acta polytechnica ctu proceedings g(x,y) x y g(x,y) figure 6. gaussian distribution in 2d. as can be seen in figure 7 the opening angle of the camera is segmented with a specific resolution, which can be set as a parameter. every segment is mapped to a single rectangular column into the projected image. the advantage of this approach is that near distance pixels are richer in detail than more distant pixels. 6.2. gaussian function the next step is to smoothen the depth image to reduce single error pixels or noise and smoothen pixel clouds for further and more precise computations and calculations. although there are several options for smoothing images, the chosen solution is the gaussian filter g(x, y) = 1 2πσ2 e − x2+y2 2σ2 (7) in (7), the gaussian function for two dimensions is shown. where x is the distance from the origin on the horizontal axis and y is the distance from the origin on the vertical axis, and σ is the standard deviation of the gaussian distribution. the distribution can be seen in figure 6 for two-dimensional gaussian functions. this formula produces a surface of concentric circles with a gaussian distribution from the center point. the new value of each pixel is set to a weighted average of that specific pixel’s neighborhood. the original pixel’s value receives the highest gaussian value and neighborhood pixels receive smaller weights as their distance to the original pixel increases. this results in a blur effect [14, 15]. figure 7 shows three identical depth frames which are already projected to a ground plane (you see the frames in a top view) and transformed into a gray image. on the left-hand side, the single frame is displayed without any filtering or blurring. there are many false pixels, noise and distortion. a gaussian filter is already used in the middle frame, nevertheless quite a lot noise and other false pixels can be seen. the approach works in practice but still needs a little fine tuning. therefore a smoother configuration of the gaussian settings was used. the third frame on the right-hand side displays very little distortion, noise and false pixels, but provides clearly identifiable pixel clouds. these pixel clouds mostly represent objects or other obstacles in the range of the kinect camera. 1 2 3 figure 7. three identical frames with no gaussian filtering in frame 1, minimal gaussian filtering in frame 2 and for the project’s obstacle detection best gaussian filtering settings in frame 3. 6.3. detect obstacles the last step before actually being able to detect obstacles is removing unnecessary pixels which still are in the image after applying a gaussian filter. in the scope of the project a parameter was added to set a tolerance for still existing false or error pixels: threshold. it’s inevitable to do so, due to the fact that there are not only black and white pixels anymore (values 0 and 255) because of the gaussian filtering but also values in between. the final step is to find objects in the distancescaled and gaussian filtered image. after preparation of the given depth image with gaussian filtering and logarithmic distance scaling, the final step for finding and detecting objects in range is to find pixel clouds with a defined minimal distance (parameter in algorithm: mindistancebetweenobstacles in meters) to other clouds and therefore to other obstacles. when a pixel cloud (respectively an obstacle) is detected with no other obstacle in range of mindistancebetweenobstacles, it is marked as a detected obstacle. 7. conclusions the autonomous driving requires the continuous mapping of the surroundings. the presented approach and the hardware setting show that the mapping can be done with a kinect camera in the case of model cars in a scale up to 1 : 5. with the 3d capturing of the surroundings, the projection and filtering and obstacle detection, it is possible to get a temporary map of the car’s environment as a basis for the navigation process. the navigation itself relies on the a*-algorithm and uses the projected map including the detected 32 vol. 6/2016 mapping the surroundings as a requirement for autonomous driving obstacles as the digital weighted spatial information. in a next step, we are planning to test the whole configuration and the navigation process under different conditions, i.e. different surfaces or different weather conditions. the aim is to obtain feedback on the use and the performance of the stereo camera and the navigation algorithm. beyond the self-driving car, the presented approach can be implemented in other vehicles, like unmanned aerial vehicles (uav), autonomous underwater vehicles (auv) or even in robots for different services. references [1] a. m. kessler. elon musk says self-driving tesla cars will be in the u.s. by summer the new york times, 2015. [2] a. fisher. google’s road map to global domination the new york times, 2013. [3] a. geiger, p. lenz, r. urtasun. are we ready for autonomous driving? the kitti vision benchmark suite. in ieee conference on computer vision and pattern recognition (cvpr), pp. 3354–3361. 2012. doi:10.1109/cvpr.2012.6248074. [4] p. fankhauser, m. bloesch, c. gehring, et al. robot-centric elevation mapping with uncertainty estimates. in international conference on climbing and walking robots (clawar), epfl-conf-198746. 2014. doi:10.1142/9789814623353_0051. [5] s. thrun, et al. exploring artificial intelligence in the new millennium. vol. 1, chap. robotic mapping: a survey, pp. 1–35. 2002. [6] m. herbert, c. caillas, e. krotkov, et al. terrain mapping for a roving planetary explorer. in ieee international conference on robotics and automation, pp. 997–1002. 1989. doi:10.1109/robot.1989.100111. [7] a. kleiner, c. dornhege. real-time localization and elevation mapping within urban search and rescue scenarios. journal of field robotics 24(8-9):723–745, 2007. doi:10.1002/rob.20208. [8] s. thrun, m. montemerlo, h. dahlkamp, et al. stanley: the robot that won the darpa grand challenge. journal of field robotics 23(9):661–692, 2006. doi:10.1002/rob.20147. [9] primesense, 2016. page version id: 710008223. [10] correspondence problem, 2015. page version id: 661209488. [11] s. design. rc-xd (call of duty: black ops) 3d warehouse. [12] t. plus. kinect from microsoft 3d warehouse. [13] p. fankhauser, m. bloesch, d. rodriguez, et al. kinect v2 for mobile robot navigation: evaluation and modeling. in international conference on advanced robotics (icar), pp. 388–394. 2015. doi:10.1109/icar.2015.7251485. [14] m. s. nixon, a. s. aguado. feature extraction and image processing. newnes, oxford ; boston, 1st edn., 2002. oclc: ocm49045100. [15] l. g. shapiro, g. c. stockman. computer vision. prentice hall, upper saddle river, nj, 2001. 33 http://dx.doi.org/10.1109/cvpr.2012.6248074 http://dx.doi.org/10.1142/9789814623353_0051 http://dx.doi.org/10.1109/robot.1989.100111 http://dx.doi.org/10.1002/rob.20208 http://dx.doi.org/10.1002/rob.20147 http://dx.doi.org/10.1109/icar.2015.7251485 acta polytechnica ctu proceedings 6:28–33, 2016 1 introduction 2 approach 3 related work 4 3d capturing 4.1 overview 4.2 3d reconstruction 5 projection and filtering 6 obstacle detection 6.1 distance scaling 6.2 gaussian function 6.3 detect obstacles 7 conclusions references acta polytechnica ctu proceedings doi:10.14311/app.2017.8.0001 acta polytechnica ctu proceedings 8:1–4, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app the interaction of human osteoblast-like saos-2 cells with stainless steel and si(100) coated by silicalite 1 films ivan jirkaa,∗, marta vandrovcováb, jan plšeka, lucie bačákováb a heyrovský institute of physical chemistry, ascr, v.v.i. dolejškova 3, 182 23 prague 8, czech republic b institute of physiology, ascr, v.v.i., vídeňská 1083, 142 20 prague 4, czech republic ∗ corresponding author: ivan.jirka@jh-inst.cas.cz abstract. interaction of osteoblast-like saos-2 cells with polished stainless steel coupons and si(100) wafers covered by a film of densely intergrown a, b oriented silicalite-1 crystals is investigated. due to their unique chemical, mechanical and biological properties these films are promising new anti-corrosive coating for bone replacement. biocompatibility of silicalite 1 film is affected by its morphology and wettability. the surface properties of silicalite 1 film is controlled by synthesis conditions and postsynthetic modifications. the morphology of the film (number of a oriented crystals) is tuned by time of synthesis. wettability of the film is tuned by heat treatment in a stream of air at 300 ◦c. the silicalite 1 film is proved to be biocompatible. the number of adhered saos-2 cells increases with the number of a oriented crystals observed for the film grown on stainless steel and with increased wettability of heat treated samples. obtained results demonstrate possible ways of preparation of anti-corrosive silicalite-1 coatings with optimized cytocompatibility. keywords: biocompatibility, silicalite-1 film, outer zeolite surface, wettability. 1. introduction metals and metal alloys are nowadays the most frequently used implant materials [1]. their substantial drawback is the evolution of metal species into the body. great attention has thus been paid to developing suitable surface modifications, which do not lower the biocompatibility of the material and simultaneously suppress evolution of the metal species. silicalite-1 coating (sc ) has been found to be prospective in this area [2]. various physical-chemical parameters, including wettability and morphology, influence the biocompatibility of prosthetic materials [3]. possibility the optimization of these parameters by the mode of synthesis and post-synthetic treatments of sc to get its maximal biocompatibility is demonstrated in this paper. our preliminary data of tuning the wettability and morphology of sc by selection of support and the mode of synthesis are presented. 2. experimental the scs were synthesized in situ on the polished surface of stainless steel foil and si(100) wafer from reaction mixture of tetrapropyl-ammonium hydroxide (tpa, 1m solution in h2o, sigma aldrich), tetraethylorthosilicate (teos, ≥ 99.0 %, aldrich) and deionized water as described in [4]. the reaction mixture was aged for 2 hours. the synthesis proceeded 3 hours (sc on si(100), referred as to sc-si(100)) and 6 hours (sc on stainless steel, sc-ss) at 165 °c. the supports and synthesis conditions used enabled the preparation of the samples with substantially different surface morphologies. a portion of the synthesized samples were heated at 300 °c in a stream of dry air. the heattreated samples were abbreviated as sc-si(100)-300 and sc-ss-300. static water drop contact angle θ measurements using the see system (brno, masaryk university, czech republic) were utilized to characterize the wettability of sc. the morphology of the samples was characterized by near-field scanning electron microscopy (fesem, s 4800-1, hitachi). the human osteoblast-like saos-2 cells were seeded on the sample surfaces as described in our earlier study [5]. briefly, the samples were sterilized in a hot air sterilizer (2 hours, 120 °c), inserted into 24well cell culture plates, and seeded with the cells at a density of 15,000 cells/cm2 and in 1 ml of mccoy's 5a medium with 15 % fetal bovine serum and 40 µg/ml of gentamicin. 3. results and discussion sem images of the samples sc-si(100) and sc-ss are depicted in figure 1. while the sc-si(100) was mostly composed from a compact layer of intergrown b oriented crystals covered by a small number of a oriented crystals, a high concentration of a oriented crystals on compact layer of intergrown b oriented crystals was observed on the sc-ss. no morphological changes were induced upon heating. typical results of water drop contact angle measurements are summarized in figure 2. the θ values of sc-ss and sc-si(100) were comparable; i.e. 84°± 3°and 66°± 2°, respectively. heat treatment induced 1 http://dx.doi.org/10.14311/app.2017.8.0001 http://ojs.cvut.cz/ojs/index.php/app i. jirka, m. vandrovcová, j. plšek, l. bačáková acta polytechnica ctu proceedings (a). (b). (c). (d). figure 1. sem image of sc-si(100) (top) and sc-ss (bottom). left: a centre of the films: left, right: a periphery of the films. (a). (b). (c). (d). figure 2. water drop contact angle of sc-si(100) (top) and sc-ss (bottom) before (left) and after treatment at 300 °c. 2 vol. 8/2017 the interaction of human osteoblast-like saos-2 cells figure 3. immunofluorescence staining of vinculin, a protein of focal adhesion plaques (green) in human osteoblastlike saos-2 cells on day 3 after seeding on sc-si(100) (a) or sc-ss (b). the actin cytoskeleton is stained in red with phalloidin-tritc, and the cell nuclei are stained in blue with dapi. leica tcs spe dh 2500 confocal microscope. substantial lowering of the θ value, which was similar for sc-ss and sc-si(100), i.e., 32°± 3°and 43°± 3°, respectively. the morphology of the saos-2 cells on the sample sc-ss and sc-si(100) is shown in figure 3. the cells on both surfaces are of similar morphology, i.e. they are well-spread and polygonal, with welldeveloped vinculin-containing focal adhesion plaques and f-actin cytoskeletons. the number of saos-2 cells (n(saos-2)) on the surfaces of sc-ss and sc-si(100) on day 1 and 3 after seeding is depicted in figure 4. the n(saos-2) on the zeolite samples are compared with the cell numbers on polystyrene dish (ps). on day 1 after seeding, the number on both sc samples is equal (sc-si(100) or higher (sc-ss) than on ps ; i.e. the zeolite samples are bioactive. comparable values of n(saos-2) are observed on the sc-ss and sc-si(100) before and after heat treatment of the samples on day 1, after seeding (figure 4). however, a substantial increase of n(saos-2) on sc-si(100)300 and particularly sc-ss-300 in comparison with non-heated samples and ps was evident in day-3 after seeding. 4. conclusion silicalite-1 films are biocompatible materials. their interaction with saos-2 cells is influenced by surface wettability and topography. the number of adhered saos-2 cells depends on synthesis conditions of zeolite coating and on its post-synthetic modification. the cell number increases with increasing numbers of a oriented zeolite crystals on the surface of sc and increasing surface wettability. obtained results are prospective in the optimization of sc outer surface to reach its maximal cytocompatibility. acknowledgements supported by grant agency of the czech republic (grant no.16-02681s). references [1] x. liu, p. k. chu, c. ding. surface modification of titanium, titanium alloys, and related materials for biomedical applications. materials science and figure 4. comparison of the n(saos-2) on days 1 and 3 after seeding on the surfaces of the samples sc-ss, sc-si(100) and ps before (a) and after heat treatment (b) of the samples at 300 °c. engineering: r: reports 47(3-4):49 – 121, 2004. doi:http://dx.doi.org/10.1016/j.mser.2004.11.001. [2] r. s. bedi, d. e. beving, l. p. zanello, y. yan. biocompatibility of corrosion-resistant zeolite coatings for titanium alloy biomedical implants. acta biomaterialia 5(8):3265 – 3271, 2009. doi:http://dx.doi.org/10.1016/j.actbio.2009.04.019. [3] l. bacakova, e. filova, m. parizek, et al. modulation of cell adhesion, proliferation and differentiation on materials designed for body implants. biotechnology advances 29(6):739 – 767, 2011. doi:http://dx.doi.org/10.1016/j.biotechadv.2011.06.004. [4] z. wang, y. yan. oriented zeolite {mfi} monolayer films on metal substrates by in situ crystallization. microporous and mesoporous materials 48(1-3):229 – 238, 2001. doi:http://dx.doi.org/10.1016/s1387-1811(01)00357-2. 3 http://dx.doi.org/http://dx.doi.org/10.1016/j.mser.2004.11.001 http://dx.doi.org/http://dx.doi.org/10.1016/j.actbio.2009.04.019 http://dx.doi.org/http://dx.doi.org/10.1016/j.biotechadv.2011.06.004 http://dx.doi.org/http://dx.doi.org/10.1016/s1387-1811(01)00357-2 i. jirka, m. vandrovcová, j. plšek, l. bačáková acta polytechnica ctu proceedings [5] m. vandrovcova, i. jirka, k. novotna, et al. interaction of human osteoblast-like saos-2 and mg-63 cells with thermally oxidized surfaces of a titanium-niobium alloy. plos one 9(6):1–15, 2014. doi:10.1371/journal.pone.0100475. 4 http://dx.doi.org/10.1371/journal.pone.0100475 acta polytechnica ctu proceedings 8(0):1–4, 2017 1 introduction 2 experimental 3 results and discussion 4 conclusion acknowledgements references 222 acta polytechnica ctu proceedings 2(1): 222–225, 2015 222 doi: 10.14311/app.2015.02.0222 early super soft source spectra in rsoph j.-u. ness1 1xmm-newton science operations centre, esa, po box 78, 28691 villanueva de la cañada, madrid, spain corresponding author: juness@sciops.esa.int abstract recent swift x-ray monitoring campaigns of novae have revealed extreme levels of variability during the early super-softsource (sss) phase. the first time this was observed was during the 2006 outburst of the recurrent nova rs oph which was also extensively covered by grating observations with xmm-newton and chandra. i focus here on an xmm-newton observation taken on day 26.1, just before swift confirmed the start of the sss phase, and a chandra observation taken on day 39.7. the first observation probes the evolution of the shock emission produced by the collision of the nova ejecta with the stellar wind of the companion. the second observation contains bright sss emission longwards of 15 å while at short wavelengths, the shock component can be seen to have hardly changed. on top of the sss continuum, additional emission lines are clearly seen, and i show that they are much stronger than those seen on day 26.1, indicating line pumping caused by the sss emission. the lightcurve on day 39.7 is highly variable on short time scales while the long-term swift light curve was still variable. in 2007, we have shown that brightness variations are followed by hardness variations, lagging behind 1000 seconds. i show now that the hardness variations are owed to variations in the depth of the neutral hydrogen column density of order 25%, particularly affecting the oxygen k-shell ionization edge at 0.5 kev. keywords: cataclysmic variables recurrent novae spectroscopy x-rays individual: rs oph. 1 introduction the 2006 outburst of the recurrent symbiotic nova rs oph has attracted a large number of observers to study the outburst in unprecedented detail and many wavelength bands. in particular the coverage in x-rays has considerably improved since the previous outburst in 1985 by initiating the first high-density x-ray monitoring of a nova with the x-ray telescope (xrt) on board swift, starting on day 3.38 after initial explosion (bode et al. 2006a). early shock emission originated from kinetic energy from the nova ejecta that were dissipated in the slow, dense stellar wind of the giant companion. the expected x-ray spectrum is that of a collisional plasma which was confirmed by spectral models to the low-resolution exosat spectra taken in 1985 (figure 3 in (o'brien et al. 1992)) and the swift/xrt spectra (bode et al. 2006b). the x-ray grating spectrometers on board xmm-newton (reflection grating spectrometer rgs) and chandra (lowand high energy transmission grating spectrometers letgs and hetgs) allow spectral lines to be resolved, and in simultaneous rgs/hetgs spectra taken on day 13.8 after the initial explosion (2006 february 12.83), bremsstrahlung continuum, h-like and he-like emission lines, and numerous fe lines could be identified. a detailed analysis exploring the information from the emission lines yielded the distribution of electron temperatures and abundances (ness et al. 2009). further grating observations were taken, e.g., on days 26.1, 39.7, 54.0, 66.9, and 111.7 that were guided by continued dense swift monitoring (see table 1 in ness et al. 2009 and top of figure 2 in osborne et al. 2011). during the xmm-newton observation on day 26.1, a jump in count rate was discovered by (nelson et al. 2008) that was exclusively attributed to additional soft emission, possibly indicating the start of the sss phase. the bremsstrahlung continuum has faded and become softer, and also the ratios of h-like to he-like emission line strengths have shifted in favor of the he-like lines, indicating a cooling trend in the shocked plasma (ness et al. 2009). the swift observations of the ∼ 60 day sss phase are described in (osborne et al. 2011). between days ∼ 30 and 45, the x-ray count rate was highly variable between ∼ 10 counts per second (cps) and 200 cps, and then stabilized at ∼ 300 cps (figure 2 in osborne et al. 2011). this was a new discovery and was later also observed in other novae and might be a general phenomenon. during this high-amplitude phase, a chandra observation was taken on day 39.7, without yet knowing about the risks of observing during times of fainter emission. while this was the case, the soft emission was still bright enough for a well-exposed grating spectrum that was first presented by (ness et al. 2007). the blackbody-like continuum contained deep absorp222 http://dx.doi.org/10.14311/app.2015.02.0222 early super soft source spectra in rs oph tion lines from highly ionized species such as o viii and n vii that were blue shifted by ∼ 1200 km s−1. the line profiles contained clear signs of emission lines in the red wings (figure 5 of ness et al. 2007) which could either come from residual shock emission or are part of p cyg profiles. during this observation, the nova was also highly variably on shorter time scales, and (ness et al. 2007) reported that the hardness variations followed the same upand down trends but lagged 1000 seconds behind (see fig. 1). figure 1: reproduction of figure 8 from (ness et al. 2007). the chandra light curve on day 39.7, taken during the early high-amplitude variability phase, was also highly variable on shorter time scales. the hardness ratio, shown in the bottom, evolved with the same variability patterns but lagged 1000 seconds behind the brightness variations. reproduced by permission of the aas. i focus here on two new aspects: 1) the emission line components on top of the sss continuum (shown in figure 5 of ness et al. 2007), compared to the same lines before the sss phase started, are much stronger than expected from a cooling plasma (sect. 2.1). 2) closer inspection of the brightness/hardness changes during the day 39.7 observation show that the hardness changes are due to changes in the depth of the o i absorption edge. modeling shows that the overall column density increases with decreasing brightness (sect. 2.2). 2 observations and analysis a full log of all xmm-newton and chandra grating observation that were taken of the 2006 outburst of rs oph is given in table 1 in (ness et al. 2009) out of which i focus on the ones taken with xmm-newton between 2006 march 10, 23:04 and march 11, 02:21 (obsid 0410180201) and with chandra 2006 march 24, 12:25 15:38 (obsid 7296). the calibrated spectra are shown in direct comparison in fig. 2 using the same flux units without rescaling. figure 2: comparison of a pre-sss spectrum of rs oph taken on day 26.1 and an sss spectrum taken on day 39.7. in the top panel the entire wavelength range is shown in logarithmic units, illustrating that at short wavelengths, below ∼ 15 å, the spectra are similar, only showing a decline the bremsstrahlung continuum component from day 26.1 to day 39.5. in the panels below, narrow wavelength regions are shown where the pre-sss spectrum is added to the median of the day 39.7 spectrum in the same flux units. while short-wavelength lines have hardly changed, the excess emission lines on top of the sss continuum are much stronger than before the start of the sss phase. 2.1 contributions of shock emission to sss continuum spectrum in the top panel of fig 2, the full spectra are shown in logarithmic units to overcome the great contrast in brightness between the two observations. at wavelengths <∼ 15 å, the two spectra are similar in nature, mainly differing in the brightness of the continuum. the weaker continuum on day 39.7 can be explained by the continuation of the fading trend of the shocks that has already been established from the observations between days 13.8 and 26.1. the strengths of the emission lines have hardly changed. at wavelengths >∼ 15 å, the emission lines seen on day 26.1 were outshone by the bright continuum on day 39.7, and it is not intuitively clear how they have evolved. in the panels below, four lines are shown in more detail in linear units. the open histograms in the panels below represent the day 39.7 spectrum while the colored shades are the day 26.1 spectrum, added to the median flux of the day 39.7 spectrum, taken over the narrow wavelength range selected 223 j.-u. ness for each panel. the mg xii/xi lines have faded from day 26.1 and the ne x line at 12.1 å is about equally strong at both times while these lines have become somewhat narrower. the panels further below show that the lines on top of the sss continuum have become stronger from day 26.1 to 39.7, depending on the strength of the continuum. the fe xvii line at 15 å, in the wien tail of the sss continuum, is only slightly stronger while the o viii and n vii lines, near the peak of the sss continuum, are much stronger, defying the general trend of fading emission from the shocks. a similar result has been found by (schönrich & ness 2008) who show in their figure 1 the evolution of the volume emission measure for various emission lines as a function of their peak formation temperature assuming collisional equilibrium. the line fluxes of o vii and o viii from the observation taken on day 39.7 yield clearly discrepant values, orders of magnitude brighter than in observations without sss emission, while those emission lines that arise at shorter wavelengths are consistent with the other observations. 2.2 spectral changes with variability during early sss phase the high-amplitude variations during the early sss phase are still not understood, leaving all options open such as changes in absorption, in intrinsic brightness, temperature, or in the rate of mass loss. a first approach to narrow down the options, i present the spectra and how they changed with variability. during the early variability phase of rs oph, a short chandra observation taken (day 39.7), and the spectral evolution is illustrated in fig. 3. the light curve, already shown in fig. 1, is shown in the right, turned around by 90o clockwise to follow the vertical time axis in downward direction. the blue dotted line is the hardness light curve from the bottom panel of fig. 1 that was rescaled to fit in the same graph. along the same vertical time axis, a series of adjacent letgs spectra are shown in the central panel with wavelength along the horizontal axis and flux encoded in a color scheme, where increasing flux is represented by colors light green, yellow, orange, red, dark blue to light blue. in the top panel, two spectra are shown that have been integrated over the time intervals marked with horizontal dashed lines in the central panel shaded areas in the right panel. the colors of the dashed lines and shades correspond to the plot style of the spectra in the top, thus light blue and orange shadings in the right correspond to the light blue shade and orange thick line in the top, respectively. the two spectra have been normalized to coincide in the wavelength range 15 − 22 å. ness et al. (2007) had extracted spectra from time intervals of bright and faint episodes, roughly corresponding to the time intervals 0.3−1.0 hours of elapsed time (bright) and 1.1− 2 hours, respectively, and found differences in the spectral shape. i have now chosen time intervals that are shifted by 1000 sec in order to probe the hardness light curve rather than the intensity light curve. the two normalized spectra in the top clearly show that the variability in hardness is purely owed to changes in the depth of the o i edge at 22.8 å, yielding the steeper edge 1000 sec after a lowflux episode. ness et al. (2007) had found changes in o i on longer time scales between the grating observations taken on days 39.7, 54.1, and 66.9 and explained these by changes in the degree of ionization of oxygen. only neutral oxygen produces the deep edge at 22.8 å while ionized oxygen is more transparent to x-rays, leading to a flatter edge. the intense soft continuum x-ray source can ionize the neutral elements in the surroundings and thus make them more transparent. on the other hand, if the continuum source fades, the surrounding material recombines, leading to an increase in the o i edge. figure 3: dynamic spectrum for the chandra observation of rs oph taken on day 39.7 after the 2006 outburst. the zero-th order light curve is shown to the right with three colored shades marking time intervals from which the spectra in the top have been extracted. line labels that belong to strong transitions are included. the central image is a brightness spectral/time map that uses a color code from light green to light blue representing increasing flux values. the changes in the depth of the o i absorption edge could be caused by changes in the degree of ionization of circumstellar oxygen. ness et al. (2007) argued that the observed time lag of 1000 seconds is consistent with the time scale for ionization/recombination in a plasma with density ∼ 1011 cm−3. since all circumstellar material would experience the same changes in their degree of ionization, this would lead to an overall change in nh. another possibility is a non-uniform radial distribution of the oxygen abundance within the ejecta that could be caused by beta decay of oxygen isotopes produced during cno burning. if during times of brigher and fainter emission, different regions of the photosphere are visi224 early super soft source spectra in rs oph ble, the difference in the oxygen abundance would only affect the depth of the o i absorption edge. in fig. 4, i test these two scenarios in the top and bottom panels, respectively. shown is the normalized faint/soft spectrum in orange shadings (orange line in the top panel of fig. 3) while the black curve represents a modification of the brighter/harder spectrum, trying to reproduce the faint/soft spectrum. in the top panel of fig. 4, the black curve was computed by dividing the bright/hard spectrum itself by the transmission coefficients calculated from the warm absorption model developed by [?], and then normalized. the faint/soft spectrum is qualitatively well reproduced assuming a value of nh = 6 × 1020 cm−2, indicating that the change in hardness can be explained by an increase of nh by this amount. the full amount of the hydrogen column was found by [?] as nh = nh,ism + nh,cs = 4.7 × 1021 cm−2, consisting of the well-known interstellar component nh,ism = 2.4 × 1021 cm−2 and an additional circumstellar component nh,cs. an increase by 6 × 1020 cm−2 thus corresponds to ∼ 26% of nh,cs. figure 4: testing two hypotheses to explain the spectral changes between hard/bright (blue shades in top panel of fig. 3) and soft/faint (orange thick line in fig. 3) spectra by the black thin lines. the normalized soft/faint spectrum is shown as orange shadings while the black line corresponds to two types of modifications of the bright/faint spectrum, also normalized (see text). top: overall increase of nh by 26% of nh,cs. bottom: increase only of o i column by changes in o abundance of 15%. in the bottom panel of fig. 4, the black curve was computed by first dividing the bright-hard spectrum by the transmission coefficients of an absorber with nh = 4.7 × 1021 cm−2, assuming cosmic abundances and then multiplying by the coefficients resulting from the same absorption model assuming a modified oxygen abundance. the faint/soft spectrum is well reproduced up to ∼ 27 å, but the black curve drops well below the faint/soft spectrum at longer wavelengths. the better agreement between the black line and the faint/soft spectrum in the upper panel demonstrates that an overall increase of nh has occurred rather than a change in the oxygen abundance alone. 3 summary and conclusions a comparison of grating x-ray spectra before and after the start of the sss phase shows that the emission lines that were seen on top of the sss continuum are not simply a continuation of the early shock emission. only emission lines that arise at wavelengths were strong continuum emission is present are amplified compared to the pre-sss level, strongly suggesting photoexcitation effects. the line profiles in the early sss spectrum of rs oph can thus be understood as p cyg profiles. the early high-amplitude variability in rs oph and other novae still awaits an explanation. the chandra observation during a minimum of these variations revealed that variability also occurs on shorter time scales. the comparisons in this article show that the hardness changes following brightness changes are consistent with variations in nh of ∼ 26% which can be explained by variations in the overall degree of ionization caused by the changes in intensity and thus variations in the effectiveness of photoionization. references [1] bode, m. f., obrien, t. j., davis, r. j., et al. 2006a, iaucirc, 8675, 2 [2] bode, m. f., obrien, t. j., osborne, j. p., et al. 2006b, apj, 652, 629 doi:10.1086/507980 [3] nelson, t., orio, m., cassinelli, j. p., et al. 2008, apj, 673, 1067 doi:10.1086/524054 [4] ness, j.-u., starrfield, s., beardmore, a., et al. 2007, apj, 665, 1334 doi:10.1086/519676 [5] ness, j.-u., drake, j. j., starrfield, s., et al. 2009, aj, 137, 3414 [6] o'brien, t. j., bode, m. f., & kahn, f. d. 1992, mnras, 255, 683 doi:10.1093/mnras/255.4.683 [7] osborne, j. p., page, k. l., beardmore, a. p., et al. 2011, apj, 727, 124 doi:10.1088/0004-637x/727/2/124 [8] schönrich, r. a. & ness, j.-u. 2008, in asp conf. series, 401, 291; rs ophiuchi (2006) and the recurrent nova phenomenon, ed. a. evans, m. f. bode, t. j. obrien, & m. j. darnley [9] wilms, j., allen, a., & mccray, r. 2000, apj, 542, 914 225 http://dx.doi.org/10.1086/507980 http://dx.doi.org/10.1086/524054 http://dx.doi.org/10.1086/519676 http://dx.doi.org/10.1093/mnras/255.4.683 http://dx.doi.org/10.1088/0004-637x/727/2/124 introduction observations and analysis contributions of shock emission to sss continuum spectrum spectral changes with variability during early sss phase summary and conclusions 283 acta polytechnica ctu proceedings 1(1): 283–287, 2014 283 doi: 10.14311/app.2014.01.0283 the hiscore project m. tluczykont2, m. brückner1, n. budnev3, o. chvalaev3, a. dyachok3, s. epimakhov2, o. gress3, d. hampf2, d. horns2, a. ivanova3, n. kalmykov4, e. konstantinov3, e. korosteleva4, v. kozin4, m. kunnas2, l. kuzmichev4, b. lubsandorzhiev5, r. mirgazov3, r. monkhoev3, r. nachtigall2, m. panasyuk4, a. pakhorukov3, v. poleschuk3, a. porelli6, v. prosin4, v. ptuskin7, g.i. rubtsov5, p.s. satunin5, yu. semeney3, d. spitschan2, a. skukhin4, l. sveshnikova4, m. tluczykont2, r. wischnewski6, a. zagorodnikov3, v. zirakashvili7 1institute for computer science, humboldt-university berlin, rudower chaussee 25, 12489 berlin, germany 2institute for experimental physics, university of hamburg, luruper chaussee 149, 22761 hamburg, germany 3institute of applied physics isu, irkutsk, russia 4skobeltsyn institute for nuclear physics, lomonosov moscow state university, 1 leninskie gory, 119991 moscow, russia 5institute for nuclear research of the russian academy of sciences 60th october anniversary st., 7a, 117312, moscow, russia 6desy, platanenallee 6, 15738 zeuthen, germany 7izmiran, moscow, russia corresponding author: martin.tluczykont@physik.uni-hamburg.de abstract a central question of astroparticle physics, the origin of cosmic rays, still remains unsolved. hiscore (hundred*i square-km cosmic origin explorer) is a concept for a large-area wide-angle non-imaging air shower detector, addressing this question by searching for cosmic ray pevatrons in the energy range from 10 tev to few pev and cosmic rays in the energy range above 100 tev. in the framework of the tunka-hiscore project, first prototypes have been deployed on the site of the tunka-133 experiment, where we plan to install an engineering array covering an area of the order of 1 km2. on the same site, also imaging and particle detectors are planned, potentially allowing a future hybrid detector system. here we present the hiscore detector principle, its potential for cosmic ray origin search and the status of ongoing activities in the framework of the tunka-hiscore experiment. keywords: cosmic rays gamma rays instrumentation pevatrons. 1 introduction ever since their discovery, cosmic rays have triggered numerous experiments aiming at answering the questions about cosmic ray composition, spectral distribution, and about their origin. ground-based experiments measure cosmic ray or gamma ray induced air showers via particle or radiation detectors on the ground. the hiscore (hundred*i square-km cosmic origin explorer) concept (tluczykont et al. 2011), is based on the non-imaging air cherenkov technique, sampling the cherenkov radiation emitted by charged air shower particles. planned as a distributed array of sensitive light collecting stations (0.5 m2), with a wide field of view (0.60-0.84 sr) and a very large instrumented area (up to 100 km2), hiscore will cover gamma ray energies above 10 tev and spectral and composition measurements of cosmic rays from 100 tev up to the eev range. the main goal of hiscore is to find the cosmic ray pevatrons, that accelerate cosmic rays up to pev energies, and that are expected to emit gamma rays with a hard spectrum up to several 100 tev. air shower measurements at these energies open up several other research possibilities, (tluczykont et al. 2011). in the present paper, we describe the hiscore detector concept, its potential for a search for cosmic ray pevatrons, and the status of tunka-hiscore, currently (april 2013) in its deployment phase on the site of the tunka-133 experiment (berezhnev et al. 2012). 2 detector concept the hiscore detector is conceived as a distributed array of non-imaging light collecting stations. the array geometry planned for the tunka-hiscore engineering 283 http://dx.doi.org/10.14311/app.2014.01.0283 martin tluczykont et al. array is shown in figure 1. 150 m 106 m figure 1: array layout planned for the tunkahiscore engineering array. in the standard layout (simulated configuration) four 8 inch pmts are used per station (red squares). additional stations with larger pmts (10 or 11 inch) are envisaged for the engineering array (blue squares). first results of tests with different array layouts have shown that a graded array with a dense core and decreasing density toward the array edge provides significantly better angular resolution and maximizes the effective area. at the heart of each station, four 8 inch photomultipliers (pmts) measure the cherenkov light from secondary air shower particles. each pmt is equipped with light concentrators (winston cones) with a half opening angle of 30◦, covering a field of view of 0.84 sr. at reconstruction, a quality acceptance cut of 25◦ results in an effective field of view of 0.6 sr. the total light collection area of one station is 0.5 m2. after preamplification, the pmt signals are clipped and summed before passing a comparator. this clipped sum trigger concept prevents false triggers caused by large signal fluctuations from night sky background light or afterpulses. the signal amplitudes are digitized in time using a readout system based on the drs 4 (domino ring sampler) chip, operated at a sampling frequency of 1 ghz and a depth of 1µs. signal amplitude, timing, rise time, and width of the arrival time distribution are used for the reconstruction of the direction, energy and nature of the primary particle. for a good reconstruction quality, the relative time-synchronization is required to be better than 1 ns between all stations of the distributed array. during one year, the 0.6 sr viewcone of the detector covers a total area of π sr for more than 200 h observation time. while this area is much larger than areas typically covered in scans performed by imaging cherenkov telescope arrays, it is fixed by the location of the experiment. in order to overcome this deficit, we plan to reorient the detector stations after a few years of operation, tilting the detector axis in north-south direction, as illustrated in figure 2, extending the sky coverage and partly deepening the exposure. figure 2: schematical view of a tunka-hiscore detector station. the tilting mechanism will allow to access a larger fraction of the sky as compared to observations pointing at the zenith alone. detail (right): each of the four optical channels consists of a pmt with a light concentrator (winston cone). 3 sensitivity the sensitivity of the hiscore standard layout was computed on the basis of a full simulation (tluczykont et al. 2011) and reconstruction algorithms (hampf, tluczykont & horns 2013). we require a detection at the level of 5 standard deviations and at least 50 gamma rays, leading to the point-source survey sensitivity shown in figure 3. the blue area corresponds to the sensitivity of the hiscore non-imaging array in its standard configuration (8 inch pmts, 150 m interstation spacing). the upper edge of the sensitivity range was obtained using conservative assumptions, assuming a ratio α of the solid angles of signal to background regions of unity. the gamma ray survival probabilities are 0.68 for the angular point-source cut, and 0.6 for the hadron rejection cut. more optimistic assumptions were made for the lower bound of the dark shaded area. here, α << 1 and the angular cut was relaxed to an efficiency of 1 in the background free regime, above 2 pev. for direct comparison, the survey sensitivity of cta (dubus et al. 2013) is shown as a dashed area, and the lhaaso sensitivity adapted from cao et al. 2010 with an additional requirement of at least 50 gamma rays is shown as dash-dotted curve. since the gamma-hadron rejection is poor when using the nonimaging technique alone, the impact of an improvement of the hadron rejection efficiency is significant. for illustration, the cyan area shows the sensitivity range when including an improvement of the hadron rejection by a factor of 10. such an improvement is realistic when combinining the hiscore concept with imaging or muon detectors. imaging detectors have proven 284 the hiscore project their gamma-hadron separation power up to several 10s of tev. at higher energies with a rising average number of muons per air shower, muon detectors become more and more efficient for hadron rejection. hiscore will open up the pevatron energy range and allow detailed spectral measurements of the continuation of known gamma-ray sources in the multi-tev to pev energy regime. at these energies, the absorption of gamma rays (e+e− pair production) in the interstellar radiation field (isrf) around 100 tev and the cosmic microwave background (cmb) around 3 pev are significant. the level of gamma ray attenuation depends on the density of the radiation fields and the distance of the objects, and can be as low as few percent. moreover, the density of the cmb being known, the absorption expected at pev energies from the cmb might open up a new method for distance estimation using gamma ray observations. energy / tev -110 1 10 210 310 410 -1 s -2 in te gr al fl ux / er g cm -1410 -1310 -1210 -1110 -1010 hiscore cta survey lhaaso point-source, 1 year )νicecube milagro sources, 5 years ( kascade u.l. mgro j1908+06 hess j1908+06 hiscore figure 3: hiscore sensitivity as compared to data on mgro j1908+06 from milagro (abdo et al. 2007) and h.e.s.s. (aharonian et al. 2009), and the sensitivity of icecube to neutrinos from milagro sources (gonzalez-garcia et al. 2009). also given are an upper limit from kascade (antoni et al. 2004), and sensitivities for experiments cta (dubus et al. 2013) and lhaaso (cao et al. 2010). recently, the icecube collaboration reported the detection of 28 neutrinos (e.g. whitehorn 2013), in excess of the atmospheric and prompt neutrino expectations, but compatible with a pevatron like spectrum. these findings are a strong additional motivation for our search for galactic cosmic ray pevatrons. 4 status of tunka-hiscore 4.1 detector components different solutions are available for the individual detector components. the photomultipliers (pmts) are required to sustain a high level of noise and to operate at a gain level of 104 105. currently, 8 inch pmts fulfilling these requirements are available from emi, electrontubes and hamamatsu (including a modified 6-stage prototype). the winston cones are assembled similarly to the construction of a wine barrel in stripes along the optical axis, using reflective sheets of alanod 4300up material. in the currently operating prototypes (april 2013), standard tunka-133 preamplifiers are in use. an analog summator for the station trigger system (see section 2) was tested in laboratory and in the field. in its final implementation, the trigger board includes clipping and triggering. further three trigger solutions are available: fadc trigger onboard the tunka-133 readout, fpga based trigger on-board the white rabbit board, and amplitude discrimination on-board the drs 4 evaluation board. all three alternative triggers use the analog sum as input. two readout systems are in operation: the standard fadc readout (200 mhz) used by tunka-133, and the drs 4 evaluation board (1 ghz). 4.2 prototype results the first tunka-hiscore prototype station (2 pmt channels) was deployed in the tunka valley in april 2012. two additional detector stations were deployed in october 2012. joint operation with tunka since then provided first cross-calibration data and experience with components. the tunka-133 fadc and the drs 4 evaluation board readout were tested in parallel in spring 2013. runs with varying thresholds were performed in order to measure the integral trigger rate as a function of the trigger threshold (epimakhov et al. 2013). as can be seen in figure 4, the expectations for the cosmic ray branch and the noise wall can be reproduced. threshold [mv] 210 t rig ge r ra te [h z] 1 10 210 310 410 510 610 710 figure 4: the trigger rate (station 4) as a function of the trigger threshold, measured with the drs 4 evaluation board in spring 2013 (epimakhov et al. 2013). red squares: dead-time corrected data, red dashed line: cosmic ray triggers, black points: estimation of nsb triggers from baseline fluctuations, black dashed curve: the nsb noise wall. 285 martin tluczykont et al. similar measurements using the fadc readout yield consistent results (wischnewski et al. 2013). an effective quantum efficiency of 0.06 could be derived from the latter measurement. this translates into a threshold for cherenkov light detection of 0.6 photons/m2, which corresponds to an energy threshold of slightly less than 100 tev when using the fadc trigger (25 ns discriminator response). the final system will have a faster response. we also plan to use faster preamplifiers, larger pmts, and geo-magnetic shielding for the pmts, ultimately lowering the energy threshold of the hiscore stations to the 10–30 tev energy range. tests of the white rabbit (wr) system show that the time precision and stability at the 200 picos level measured in the laboratory can be reproduced at the tunka site (brückner et al. 2013). the observed time difference distribution of wr-tagged events is consistent with the observation of air showers with the given viewing angle of the tunka-hiscore stations (wischnewski et al. 2013). 5 conclusion and outlook using the new large-area wide-angle non-imaging hiscore detector concept, we plan to access the pevatron gamma ray energy range (10 tev – several 100 tev) and also address cosmic ray physics around the knee region. the tunka-hiscore experiment has started the deployment of detector stations in the tunka valley in siberia. 3 prototype stations are in operation, and further 6 stations will be deployed by the end of 2013. the construction of an engineering array that will cover an area of 1 km2 is planned for the near future. different alternatives for the station design (8 inch or 10 inch pmts) and for the array layout (graded array) are considered. a combination with small imaging telescopes (2-3 m2 mirrors, 10◦ field of view) is planned to complement the tunka-hiscore array. furthermore, the installation of muon detectors and fluorescence telescopes at the tunka site is considered for the future, improving gamma hadron separation and cosmic ray composition, and leading to a multi component extended air shower array in the tunka valley in siberia. acknowledgement we acknowledge the support of the russian federation ministry of education and science (g/c 14.518.11.7046, agreements n 14.b25.31.0010, n 14.b37.21.0785, and n 14.37.21.1294, g/c 14.740.11.0890, p681, contract n 14.518.11.7046), the russian foundation for basic research (grants 11-0200409, 13-02-00214, 13-02-12095, 13-02-10001, 12-0210001, 12-02-91323), the president of the russian federation (grant mk-1170.2013.2), the helmholtz association (grant hrjrg-303), and the deutsche forschungsgemeinschaft (grant tl 51-3). we thank gavin rowell for valuable discussions. references [1] abdo, a. a., allen, b., berley, d., et al.: 2007, apj l., 664, l91 doi:10.1086/520717 [2] aharonian, f., akhperjanian, a. g., anton, g., et al.: 2009, a&a, 499, 723 [3] antoni, t., apel, w. d., badea, a. f., et al.: 2004, apj, 608, 865 doi:10.1086/420736 [4] berezhnev, s. f., et al. (tunka collaboration): 2012, nima, 692, 98 [5] brückner, m., et al.: 2013, to appear in proc. of icrc, rio de janeiro, brazil, 1158 [6] cao, z., bi, x. j., cao, z., et al.: 2010, 38th cospar scientific assembly, 38, 2322 [7] dubus, g., contreras, j. l., funk, s., et al.: 2013, aph, 43, 317 [8] epimakhov, s., brückner, m., budnev, n. et al.: 2013, to appear in proc. of icrc, rio de janeiro, brazil [9] gonzalez-garcia, m. c., halzen, f., & mohapatra, s.: 2009, aph, 31, 437 [10] hampf, d., tluczykont, m., & horns, d.: 2013, nimpa, 712, 137 doi:10.1016/j.nima.2013.02.016 [11] moskalenko, i.v., porter, t.a., strong, a.w.: 2006, apjl, 640 l155 doi:10.1086/503524 [12] tluczykont, m., hampf, d., horns, d., et al.: 2011, adv. sp. res., 48, 1935 doi:10.1016/j.asr.2011.08.004 [13] whitehorn, n. h.: 2013, fermilab astro seminar [14] wischnewski, r., berezhnev, s., brückner, m., et al.: 2013, to appear in proc. of icrc, rio de janeiro, brazil, 1164 discussion (from memory) questioner: at these high energies, gamma rays are absorbed in low energy radiation fields. how can you expect sources in the 100 tev energy range? martin tluczykont: the strength of the attenuation depends on the location of the object within our galaxy. an object located at the far side of 286 http://dx.doi.org/10.1086/520717 http://dx.doi.org/10.1086/420736 http://dx.doi.org/10.1016/j.nima.2013.02.016 http://dx.doi.org/10.1086/503524 http://dx.doi.org/10.1016/j.asr.2011.08.004 the hiscore project the galaxy behind the galactic center was shown (moskalenko et al. 2006) to be absorbed at the 50 % level. any other object located closer to the sun, or off-center the galactic disk, will be less absorbed, down to only few %. 287 introduction detector concept sensitivity status of tunka-hiscore detector components prototype results conclusion and outlook 226 acta polytechnica ctu proceedings 2(1): 226–229, 2015 226 doi: 10.14311/app.2015.02.0226 when a nova becomes old a. ederoclite1, c. tappert2, l. schmidtobreick3, n. vogt2 1centro de estudios de f́ısica del cósmos de aragón (cefca), plaza san juan 1, planta 2, 44001, teruel, spain 2instituto de f́ısica y astronomı́a, universidad de valparaiso, av. gran bretaña 1111, valparaiso, chile 3european southern observatory, alonso de cordova, santiago, chile corresponding author: aederocl@cefca.es abstract here we present the preliminary results of a project aimed at unveiling the nature of classical novae decades after their eruption. the ultimate goal of this project is to describe the population of cataclysmic variables which give rise to nova explosions. so far, in four years of observations, we have concentrated on novae in the southern hemisphere, where we increased by 100% the amount of objects spectroscopically confirmed and increased by 1/5 the amount of objects with known orbital period. keywords: cataclysmic variables classical novae optical spectroscopy photometry. 1 introduction classical novae (cne) are the result of a thermonuclear runaway on the surface of a white dwarf which is accreting mass from a less evolved companion (for a review, see bode & evans, 2008). it is common to define cne as a “subclass of cataclysmic variables” which is a fair statement in both historical and observational terms but it is not quite physically appropriate: a cnexplosion is a phase during the life time of a cataclysmic variable (cv). according to the “hibernation scenario” (shara et al., 1986), post-nova cvs are expected to go through a phase of high mass transfer (triggered by the irradiation of the hot wd) and, eventually, the system gets to separate and spends 90-99% of the inter-explosion time in a quiescent “detached” state (prialnik 1986). it is clear that the use of the term “quiescence” for an oldnova system is very vague and it is the reason why it is used in quotes throughout this work. for a review on old novae, see pagnotta (2013). this project started four years ago trying to answer some fundamental questions: • how does the population of old novae look like? • how does the population of old novae compare to cvs? • do short-period old novae exist in a significant number? • what is the role of magnetic fields on the cnoutburst? despite their brightness at maximum light, the study of novae in “quiescence” is still largely incomplete (again, see pagnotta, 2013). it is important to note that, before this project started, only 39 old novae (out of the 204 novae which exploded before 1980) had a measured orbital period. so far, our project has focused mostly on the southern hemisphere (i.e. targets with δ < 20◦), where, before the start of our project, out of 153 reported novae, 34 lacked identification of the target in “quiescence”, 9 were confirmed but their period was unknown and 24 had a known orbital period. the remaining 86 did not even have a candidate. here we describe the methodology and some early results related with the population which has been recovered so far. for the description of selected targets, see schmidtobreick & tappert (2013) and tappert et al. (2013c) . 2 the methodology our project consists of three phases: the photometric identification of the nova candidate, the spectroscopic confirmation and the period determination through time-series spectroscopy. the target list has been derived mainly from the downes et al. (2005) catalogue. we selected those novae which had exploded before 1980. the selection is made to allow some time after the nova explosion for the characteristics of the underlying cv to become accessible. 226 http://dx.doi.org/10.14311/app.2015.02.0226 when a nova becomes old 1 2 3 4 5 10 20 50 porb(h) 0 2 4 6 8 10 12 14 16 18 this project, n=8 periods of novae before 1980, n=39 1 2 3 4 5 10 20 50 porb(h) 0 5 10 15 20 25 all periods of novae n=78 figure 1: left: period histogram of novae which exploded before 1980. the black histogram is the addition from this project. right: period histogram of all novae (i.e. including those which exploded after 1980). the dotted vertical lines refer to the period gap and the dashed vertical line to the period minimum. we do not include in our sample recurrent novae (rne). these represent thermonuclear explosions analogous to cne but which occur on much shorter recurrence times. the large majority of those rare stars (only a dozen is known in our galaxy) harbour well-evolved secondary stars which sets them somewhat apart from other cvs. as our project primarily originated with the idea of testing the predictions of the hibernation scenario, rne are not included in our analysis. we obtain ubvr photometry of the region of sky where a nova has been reported. here we are taking advantage of the fact that an old nova, as any cv, has a spectrum which is the sum of three components (the white dwarf, the main sequence companion and the accretion disk). this is the same discovery strategy which is being used in large photometric surveys, like sdss (see szkody, 2013). we obtain spectroscopy of those targets whose location in the colour-colour diagram, does not follow the one of the stars. this is “weighted” by the distance from the reported position (i.e. not necessarily the bluest object in the field is the first candidate for follow up spectroscopy, in case there is another object which is closer to the reported position). low-resolution spectroscopy (r = λ ∆λ ' 500) is enough to resolve cvs emission lines and to cover a spectral range (∼4000–9000å) which includes the most relevant lines for cv classification. time-series is obtained once the target has been spectroscopically confirmed. in some cases, time-series photometry is carried out (e.g. tappert et al., 2013b) but, in general, we perform time-series spectroscopy with r = λ ∆λ ' 2500 in the hα region. in order to keep a log of the observations and share the results within a group which is geographically spread over two continents, an internal webpage is being maintained. here we keep a list of our targets, observing logs, and description of the results for each target. 3 results 3.1 the period distribution the left panel of fig.1 shows the histogram of the pre1980 novae. in grey, the periods that can be obtained in the literature and, in black, the addition due to this project. the right panel of fig.1 shows the histogram of all the novae (also the ones which exploded after 1980). the periods of post-1980 novae are from ritter & kolb (2003). qualitatively, the two histograms are very similar: there are few sources with periods within the period gap and a handful of sources below the period gap. there is a “clustering” of sources right above the period gap (just in the period region where sw sex stars belong, see schmidtobreick & tappert, 2013) and less sources at longer periods. this is an interesting result by itself, since our sample is selected on the basis that the targets are back in “quiescence”. the only significant difference is the number of objects found in the 5 – 10 hours period range, which can be easily ascribed to small-number statistics. as we already mentioned, very few objects are within (or below) the period gap. this is consistent with old novae being in a high-mass transfer phase, as predicted by the “hibernation” scenario. it is also worth noting that the overall shape is consistent with the modelling by townsley & bildsten (2005), which assumes that novae occur mostly in high mass accretion rate systems. 227 a. ederoclite et al. 3.2 the role of magnetic fields as we mentioned in the previous section, there are very few objects with periods<3 hours, and, as it can be seen from fig.2, these objects are mostly magnetic. among the 47 pre-1980 old novae with a measured period, only v1500 cyg (1975) and cp pup (1942) are catalogued as am her stars and have periods of 3.36 hours and 1.68 hours, respectively. 0 5 10 15 non magnetic systems am her 1 10 porb(h) 0 5 10 15 non magnetic systems ip 0 5 10 15 non magnetic systems dq her figure 2: the histograms of the magnetic systems which are observed to have harboured a nova explosion. in white, for comparison, the histogram of nonmagnetic systems. in the upper panel, the am her, in the middle panel the dq her systems and, in the lower panel the intermediate polars. the classification is either from ritter & kolb (2003) or from tappert et al. (2012,2013a). although the number of magnetic systems is still small (hence we cannot draw firm conclusions) it is promising that polars and intermediate polars are located in a similar region of the period histogram as in the “classical” cv period histogram. moreover, as mentioned by tappert et al. (2013b), 7 out of 10 novae in the gap may be magnetic. this is in agreement with the population model by townsley & bildstein (2005), who suggest that novae within the period gap are mostly magnetic. araujo-betancor et al. (2005) derive that the total ratio of known magnetic to nonmagnetic cvs is ∼22% (at all periods). the high number of magnetic cvs within the gap, if confirmed, may imply a different evolution through the gap between magnetic and nonmagnetic systems. 3.3 the explosion amplitude from downes et al. (2005), one can derive that the average explosion amplitude is 12.57±2.47 mag. combining our data with data from downes et al. (2005), ritter & kolb (2003), duerbeck (1987), one can try to compare the explosion amplitude (i.e. the difference between the magnitude at maximum and the magnitude in “quiescence”) with the rate of decline (see fig.3). this has already been done by vogt (1990). in fig.3, we show the data from vogt (1990) plus data from our project and post-1980 novae from ritter & kolb (2003). it is interesting to note that our data points (the red squares) fall in the same region as the others. the straight line is the fit from vogt (1990) to the points in his paper and is still valid with the inclusion of the new points. −0.5 0.0 0.5 1.0 1.5 2.0 2.5 3.0 3.5 4.0 log t3 4 6 8 10 12 14 16 18 20 d e lt a m figure 3: rate of decline (as measured by the t3 parameter) vs. explosion amplitude (difference between the magnitude at minimum and the magnitude at maximum). the red squares are from this project. the line is not a fit to the present data-set but to the data presented in vogt (1990). the two objects which seem to deviate from the relation are v1500 cyg (1975) and v458 vul (2007). the first one, as mentioned in the previous section, is an am her star. the second one showed a very irregular light curve, with three repeated peaks. these two examples suggest that the scatter in this relation is likely due to two independent causes: on one hand, the magnitude at “quiescence” depends on the structure of the accretion disk (if any) and the magnitude at maximum light (and the rate of decline) may be misestimated due to a series of factors (e.g. bad sampling or dust formation) which are quite typical in novae. warner (1987) has already 228 when a nova becomes old suggested that, for a better comparison of the explosion amplitude, one should take into account, at least, the orbit inclination of the system. another important caveat is that some old novae are observed to decrease their “quiescent” brightness (see e.g. vogt 1990, and references therein, or johnson et al. 2013) and, therefore, fig.3 should be considered in a more dynamical context. 4 summary and future perspectives we have presented a project aimed at the recovery, classification and characterisation of classical nova systems decades after the explosion. during this project, which started four years ago, we have already significantly increased the number of identified and spectroscopically confirmed classical novae (novae without an identified progenitor decreased by 24% and the number of spectroscopically confirmed increased by 100%). finally, we have also increased by 1/5 the number of pre-1980 oldnovae with known orbital period. we plan to finalise the southern part of our project during the next two years and to focus on targets in the northern hemisphere. once the program will be completed, this sample will be crucial in the study of the evolution of classical novae towards quiescence, the study of cn-progenitors as a subclass of the cnpopulation and the development of of the “nova populations” framework (della valle 2002 and references therein). for better sharing the results of our project, we are planning on providing access through the virtual observatory to the reduced data, thus sharing a database with basic parameters (position, brightness, type,. . . ), the spectra used for characterisation and finding charts. this data release will represent a significant legacy for the cv community. acknowledgement the cefca is funded by the fondo de inversiones de teruel, supported by both the government of spain (50%) and the regional government of aragón (50%). this work has been partially funded by the spanish ministerio de ciencia e innovación through the pnaya, under grants aya2006-14056 and through the icts 2009-14. ct and nv acknowledge financial support by fondecyt regular grant 1120338. references [1] araujo-betancor, s. et al.: 2005, apj, 622, 589 [2] bode, m. & evans, n.: 2008, “classical novae”, 2nd edition, cambridge astrophysics series, no 43, cambridge: cambridge university press, 2008 [3] della valle: 2002, aipc, 637, 443 [4] downes, r. et al.: 2005, jad, 11, 2 [5] duerbeck, h.: 1987, space sci. rev. 45, 1 doi:10.1007/bf00187826 [6] johnson, c. et al.: 2013, apj, 780l, 25 [7] pagnotta, a.: 2013, this workshop [8] prialnik, : 1986, apj, 310, 222 [9] ritter h., kolb u. 2003, a&a, 404, 301 doi:10.1086/164762 doi:10.1111/j.1365-2966.2012.21054.x [10] schmidtobreick, l. & tappert, c.: this workshop doi:10.1093/mnras/stt139 [11] shara, m. et al. 1986 apj, 311, 163 doi:10.1093/mnras/stt1747 [12] szkody, p.: 2013, this workshop [13] tappert, c. et al.: 2012, mnras, 423, 2476 doi:10.1086/430594 [14] tappert, c. et al.: 2013a, mnras, 431, 92 doi:10.1086/168866 [15] tappert, c. et al.: 2013b, mnras, 436, 2412 [16] tappert, c. et al.: 2013c, this workshop [17] townsley, d. & bildsten, l.: 2005, apj, 628, 395 [18] vogt, n.: 1990, apj, 356, 609 [19] warner, b.: 1987, mnras, 227, 23 229 http://dx.doi.org/10.1007/bf00187826 http://dx.doi.org/10.1086/164762 http://dx.doi.org/10.1111/j.1365-2966.2012.21054.x http://dx.doi.org/10.1093/mnras/stt139 http://dx.doi.org/10.1093/mnras/stt1747 http://dx.doi.org/10.1086/430594 http://dx.doi.org/10.1086/168866 introduction the methodology results the period distribution the role of magnetic fields the explosion amplitude summary and future perspectives acta polytechnica ctu proceedings doi:10.14311/app.2017.10.0012 acta polytechnica ctu proceedings 10:12–15, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app features regarding interaction of anchor piles such as “titan” and “geoizol” with soils mikhail. i. nikitenkoa,∗, igor p. dubatovkab a stroitechnorm, stroikompleks, 220037, minsk, ul. filimonov, 8-105. belarus b monorakurs, 220116, minsk, pr. dzerzhynsky, 104b. belarus ∗ corresponding author: michnikit@gmail.com abstract. the article describes the experience of using anchors at a deep excavation for the construction of a multifunctional complex in minsk. the authors describe the features of the device and the testing of the pressure grouted anchoring structure of “geoizol” (according to the “titan” type system). keywords: deep excavation pit; underground retaining wall; anchor piles titan, geoizol.. 1. introduction cut-off diaphragm wall was used for the protection of the deep excavation in the construction of a multifunctional complex in minsk. these walls were anchored with anchors at one, two or three levels. [1] “geoizol” anchors according to “titan” type were used for anchoring of the diaphragm walls. these piles were installed with the help of pressure grouted technology [2–8] . as these anchor piles differ from conventional continuous pressure grouted anchors the nature of these differences will be described. at the end the advantages and disadvantages of the described anchor piles during their installation and application are specified. 2. construction site multifunctional complex (ifc) is situated in the northeast of minsk. the geotechnical site conditions were described as rather complicated, composed from different horizons, as holocene, mogilev, slavgorodskiy, dniprovskiy, which contains mostly moraine sediments of different compositions. starting from boulders up to fine sandy loam, arranged not only in layers, but sometimes in the shape of closed lenses. top aquitard are moraine loam mogilev sub horizon, lower moraines slavgorod sub horizon. between them is artesian water, non-aggressive to concrete. the amount of pressure was 9.0 – 13.6 m. 3. constructive solution of anchor “titan” piles and “geoizol” the design of the anchor rod comprises a steel tubular rod with a helical knurled outer surface consisting of joined screw couplings units, and on the bottom of which at the end there is screwed a drill bit with outlet holes, and at the top there is a lock nut with a spherical contact surface which rests on the construction plate (fig. 1). in this design concept the hollow anchor rod figure 1. structural elements of anchor piles “titan” and “geoizol” combines the functions of a drilling rod when drilling wells through a progressive rotational movement of the rod with a drill bit, and an injector for injecting into the cavity a cement slurry, which, under pressure erodes at the bottom soil and under agitation then plugging the borehole, creating a hardening of shaft piles. subsequently the rod reinforces the pile and on pulling out it provides a recognizable tensile force. 12 http://dx.doi.org/10.14311/app.2017.10.0012 http://ojs.cvut.cz/ojs/index.php/app vol. 10/2017 features regarding interaction of anchor piles with soils 4. sequence of operations when constructing the type of anchor piles “titan” and “geoizol” the technological operations of the device anchor piles in the soil include borehole drilling to the projected depth of the tubular rod in rotation together managed with drilling crown and soil displacement. this is pumped through the rod chamber plugging cement slurry which erodes soil and facilitates drilling of the downhole, fills it and prevents soil collapse. when the cement slurry strength attains at least 70 % of that designated (in sand 14 days during solution without plasticizer c-2 and 7 days with plasticizer), all are subject to tension anchor piles. in clayey soils a drainage solution is needed. figure 2. excavation pit overview and installation of anchoring piles. after the excavation of the construction site on the level of the first row of anchors, horizontal i beam was applied together with large steel plates, fig. 2. after that the anchoring piles were constructed. the lengths of anchor piles with diameter 0.25 m, was at first level 15 m and 12 m for the second level. the lengths of the workers (root) segments were 8.4 m and 6.9 m. they were located in the strata of sandy loam. 5. anchoring piles testing anchors testing should evaluate the shear strength of sandy loam along the trunks and roots of the anchoring piles and help a confirmation of shear strength used during the stability of retaining wall design. first three anchors are designed to identify the role of the injected grout composition to set them quality strength after 7 days, and also for definition of the actual barrel shape and diameter. to prove this the anchors were excavated (see fig. 3). the excavation was carried out by inspection and measurements. the control showed that their trunks are roughly cylindrical in shape with a diameter of 0.25 m without separation of free and working root segments. it was established that the strength of cement grout in all samples was similar, reaching over 70 % of the calculated value. the arrangement for the pull-out tests is shown on fig. 4. maximum tensile force was 549 kn, indicating the average shear strength along perimeter and length of anchoring part equal to 140 kpa. two other testing anchors were left in ground for 28 days. for one of them the hardening accelerator was used and the second anchor was constructed without hardening accelerator. no significant differences were observed. 6. advantages and disadvantages of the anchor of the “titan” piles or “geoizol” testing of 5 anchoring piles and their excavation allows some statement about the application of these anchors. advantages are as follows: • structural design ensures that the high strength hollow rod with knurling screw on the outer surface and with cross-cut bit at the bottom allows insertion of the anchor into ground, followed by injection of grouting cement slurry under high pressure. slurry primarily wash away soil at the bottom, supports borehole stability and after hardening guarantee good contact with rod surface; • minimal elongation of high strength anchor rod during loading; • low risk of corrosion. however there are also some shortcoming as: . the creation of a local broadening on the lower end of the pile, i.e., working in the root zone is problematic, since the liquid cement slurry further pumping of denser high-pressure pressure leads approximately to the same stem diameter across the length of the borehole, with the exception of more intensive compressible soil layers; . the huge over expenditure of cement due outpouring of wellhead in the process of drilling or during injection; . hardening cement slurry is excluded because it is difficult to rotate the rod with the drill bit, while increasing their water-cement ratio (w / c) sedimentation processes are amplified. up to now experiences in low permeable ground leads to the recommendation to use drainage to drain excess of water from the slurry injected with a great value of w/c in accordance with the inventions as are no 1281635, 1527378 and 139 2203 see [3],[6]. application of geotextile sleeve can fulfil this drainage role. 13 mikhail. i. nikitenko, igor p. dubatovka acta polytechnica ctu proceedings figure 3. removing from the ground (a) the form of excavated three anchor piles (b). fragment of anchor piles body remaining in the ground (c), measurement of the diameter on the contact with the stem (d). figure 4. assembling panels of support system for two experienced anchor piles and sampling testing for one of them. 7. conclusions testing of the anchoring piles of the type “titan” and “geoizol” on the construction site in minsk, make it possible to specify not only advantages of this system, but also some shortcomings. to partly eliminate the shortcomings some recommendations were proposed namely draining geotextile sleeve with local tire rings along the length of the roots and packers. references [1] p. posobie. designing and organizing the pile and wall in trench. 14-01 for snb 5.01.01-99. architecture and construction ministry of belarus, minsk, 2002. [2] p. posobie. design and construction of bored piles. 13-01 for snb 5.01.01-99. architecture and construction ministry of belarus, minsk, 2002. [3] p. posobie. designing and construction of injection anchor and piles. 18-04 for snb 5.01.01-99. architecture and construction ministry of belarus, minsk, 2005. 14 vol. 10/2017 features regarding interaction of anchor piles with soils [4] tkp. foundations and underground structures, constructed with the use of inkjet technology. terms of design and construction. 45-5.01-45-2006 (02250). architecture and construction ministry of belarus, minsk, 2006. [5] m. i. nikitenko. continuous pressure grouted piles and anchors in the construction and reconstruction of buildings and structures. belarusian national technical university, minsk, 2007. [6] a. g. malinin. application of anchor “atlant” piles in underground construction. earth science 2:248–254. [7] c. a. ritov. effective modern device technology of continuous pressure grouted piles and injecting anchors. information bulletin 16(1):7–14. [8] c. zolotov. about the bases of the device anchor piles titan. construction and real estate pp. 1–3. 15 acta polytechnica ctu proceedings 10:12–15, 2017 1 introduction 2 construction site 3 constructive solution of anchor ``titan'' piles and ``geoizol'' 4 sequence of operations when constructing the type of anchor piles ``titan'' and ``geoizol'' 5 anchoring piles testing 6 advantages and disadvantages of the anchor of the ``titan'' piles or ``geoizol'' 7 conclusions references 81 acta polytechnica ctu proceedings 2(1): 81–85, 2015 81 doi: 10.14311/app.2015.02.0081 activity of the polar am her (rx j1816.2+4952): a short review v. šimon1,2, a. henden3 1astronomical institute, academy of sciences of the czech republic, 25165 ondřejov, czech republic 2czech technical university in prague, fel, prague, czech republic 3aavso, 49 bay state road, cambridge, ma 02138, usa corresponding author: simon@asu.cas.cz abstract we show that am her displays the transitions between the high and low states with an intermittently existing dominant cycle with length between 400 and 800 days. moreover, these transitions accumulate in clusters, which produces an additional long cycle after smoothing; a single isolated short episode of the low state does not suggest a break of this cycle. the seasons of existence of the cycle can be controlled by the lifetime of the active regions (e.g. prominences, spots) on the donor. in some high-state episodes, a higher luminosity of the bremsstrahlung emission is not accompanied by a higher optical (cyclotron+stream) emission. part of the bremsstrahlung emission can be buried in some episodes. changes of the structure of the accretion region(s) are necessary to explain the variations of the optical and x-ray activity in the high-state episodes of am her. keywords: cataclysmic variables polars activity emission mechanisms optical x-rays individual: am her. 1 introduction am her is the prototype of polars (e.g. [19]). its activity is dominated by the large-amplitude long-term variations: alternating high and low states of the optical brightness usually on the timescales of months and years (e.g. [8, 21, 10]). a small accreting region (about 0.1 of the radius of the white dwarf (wd)) near the magnetic pole of this object is the source of radiation and polarization of polar via several processes: cyclotron (accretion column – mainly optical and ir emission), thermal (soft x-rays – surface of the wd heated by the accreting region), bremsstrahlung (accretion column – hard x-rays) (e.g. [19, 15]). the conditions in this region and the mass accretion rate play an important role in governing the observed activity. 2 long-term activity in the optical band fig. 1a shows the long-term activity of am her in the optical band spanning about 32.7 years. the data come from the aavso international database (massachusetts, usa) [6]. the highly variable orbital modulation has a large amplitude mainly in the high state (e.g. [9, 10]), so the character of the long-term activity is less discernible. fig. 1a therefore shows the hec13 fit running through the orbital modulation (each point is a smoothed value of brightness in the night of observing).the division between the high and low states is 14.3 mag(v ). the properties of the statistical distribution of brightness of the high states strongly evolve with time (fig. 1cd). the typical high-state brightness is near the middle of the distribution on the magnitude scale in most time segments. the low states often show skewness of brightness toward the brighter magnitudes. the fuzzy bright edge of the high-state brightness, smoothed over the orbital modulation, in the histogram suggests that the high state is not a uniquely defined level of luminosity of am her (fig. 1cd). it is questionable whether any “unperturbed” state of the system exists et all. a typical strength of the active regions (large loops of magnetically confined gas near the donor due to its magnetic activity [9] and star spots [13, 7]) during the high state is therefore needed (the times of the quite quiescent donor are thus very rare). in the scenario proposed by [21], this statistical distribution also suggests a typical configuration of the magnetic field of the whole system (donor+wd), around which the system balances during the high state of activity. the brightness of the low states in am her often stabilizes at the baseline level. the mass transfer via roche lobe overflow almost ceases, only clumpy accretion onto the wd from the donor’s wind remains [3, 9]. the strong skewness of brightness in fig. 1cd can emerge if the hec13 fit runs through the variably recurring brightenings. 81 http://dx.doi.org/10.14311/app.2015.02.0081 v. šimon, a. henden moving averages (ma) of brightness with various filter half-widths q enable to search for the evolution of the optical activity of am her on timescales of several years, significantly longer than the duration of the individual episodes of the high or low states (fig. 1). the transitions between these states tend to occur in clusters in am her. smoothing then reveals a long cycle because of the variable clustering of the episodes of the low states. since the borders of these clusters are fuzzy, a smooth profile of the cycle results when ma are applied. a single isolated short episode of the high or the low state does not suggest a break of this cycle since the cycle is caused by the repeating accumulations of these transitions in clusters. some long cycles thus may not be easily discernible without investigating the variations of the parameters of activity, which ma enable (fig. 1ab). figure 1: (a) the long-term activity of am her in the optical band (aavso data [6]). hec13 fit runs through the orbital modulation. the mapping is divided into segments. the smooth lines represent the moving averages (ma). (b) residuals of the ma. (c, d) examples of the strikingly different statistical distributions of brightness. see sect. 2 for details. search for the cycle-length in the transitions between the high and low states from fig. 1a was carried out also with the weighted wavelet z-transform (wwz) developed by [1]. this method enables one to determine the period and amplitude of unevenly sampled time series. wwz indicates whether or not there is a periodic fluctuation at a given time at a given frequency f (fig. 2a). the wwz-transform really finds that the transitions between the states are not quite chaotic. a dominant cycle in the transitions really exists. however, the cycle-length of the transitions is not stable and this cycle is not conclusively detected in some time segments. fig. 2b shows the best cycle-length, determined from f that has the biggest value of wwz at a given time (only the segments in which the amplitude is larger than 60 percent of its peak value in the investigated range of f). in summary, this cycle is characteristic only for a limited time segment. it is intermittent and unstable in length. moreover, the wwz-method shows also another temporarily existing shorter cycles in fig. 2a. for comparison, the cycles of 178 d, 1836 d, 830 d and 1520 d were found by fourier analysis by [11]. the differential rotation of the lobe-filling donor (modeled by [18]) can influence the position of the above-mentioned active regions on the donor with respect to the l1 point. the breaks of the cycle of the transitions between the high and the low states in am her can be caused by a limited lifetime of the above-mentioned active regions connected with the activity of the donor. figure 2: (a) wwz-transform of the light curve of am her from fig. 1a. (b) the best cycle-length. see sect. 2 for details. 3 optical and hard x-ray intensities in the high states in am her, increase of the mass transfer rate from the donor (giving rise to a high-state episode) also establishes specific division of the emission into various spectral regions during the accretion process (fig. 3) (see our analysis in [17] for details). the properties of the emitting region(s) on the wd are established in the 82 activity of the polar am her (rx j1816.2+4952): a short review early phase of the high-state episode (but not reproduced for every episode) of am her. a higher luminosity of the bremsstrahlung emission may not be always accompanied by a higher optical (cyclotron+stream) emission in a given episode of the high state (the intensities in both of these bands were averaged over the orbital period) [17]. this can significantly differ even for two consecutive episodes (fig. 3bc). this relation of intensities is representative for the whole such episode. purely geometric effects (asynchronous rotation of the wd, precession of the wd spin axis) cannot explain the observations – gradual evolution of the x-ray and optical intensities with time would be needed (see [17] for details). we propose the following scenario. the source of the bremsstrahlung emission is confined to a smaller region than that of the cyclotron emission. part of the bremsstrahlung emission is buried in some high-state episodes. since there is no smooth transition of the ratio of the optical and hard x-ray intensities [17], it suggests that the role of several modes of accretion is worth considering. figure 3: (a) part of the asm/rxte (1.5–12 kev) [12] light curve of am her (15-d means). the mean levels and their standard errors are marked. (b, c) intensities of the optical (afoev data, the intensity i = 1 for 14.3 mag) and hard x-ray (1.5–12 kev) (asm/rxte data) emissions in two consecutive episodes of the high state. a higher luminosity of the hard x-ray emission may not be always accompanied by a higher optical emission in a given episode. 4 role of the accretion modes the orbital modulation of am her displays significant changes in both the optical and x-ray spectral regions. unexpected mode of the x-ray (soft: 0.1–0.31 kev, hard: 1.9–8.5 kev) orbital modulation was observed in two observing runs of the same optical high state by [4]. it suggested a two-pole accretion mode in which the primary pole was the dominant emitter of the hard x-rays while the secondary pole was dominant in the soft x-rays. the accretion mode is representative only for a given high-state episode of am her [14]. a short episode of the high state (but less bright than most other highstate episodes) displayed a single-pole accretion mode with a self-occultation of the primary pole, resulting in a deep primary minimum in the bands between e = 0.6 and 10 kev, but no sign of the secondary minimum. the subsequent brighter high state displayed a two-pole accretion mode with a shallow primary minimum in the 2– 30 kev band, suggesting the big dimensions of the accretion region. the secondary minimum occurred only in the soft band (1–2 kev), suggesting that the secondary pole is the dominant emitter of the soft x-rays. the same situation as those observed in one of the previous high states by [4], that is the primary pole dominant in the hard x-rays and the secondary one dominant in soft x-rays, thus repeated. also cyclotron emission undergoes peculiar changes with the accretion mode. in the above-mentioned bright high state observed by [14], cyclotron emission from a region at the primary accreting pole dominated in the v -band [2]. since a two-pole accretion was determined from polarization of the optical emission for another high-state episode by [20], it suggests that the accretion modes are very unstable in am her. changes of the structure of the accretion region(s) are necessary to explain the variations of the optical and x-ray orbital modulation in the individual episodes of the high state in am her. the accretion modes (singlepole accretion, two-pole accretion) vary with time; they may be characteristic for a given high-state episode, but not for another one. since the properties of the accretion region at the primary pole largely differ from those at the secondary pole, these changes of the accretion modes contribute to the complicated long-term activity. the transition from the high to the low state is accompanied by dramatic changes of the size and structure of the cyclotron-emitting accretion region in am her (fig. 4). a decrease of the dimensions of the accretion region(s) during the transition emerges from these facts: the rises and declines between the extremes of brightness (especially of the branches of the primary minimum) become progressively steeper, the amplitude 83 v. šimon, a. henden of the modulation increases, the eclipse of the primary pole becomes very prominent. during the final phase of the high-state episode, the properties of the cyclotronemitting region do not scale exactly with the optical luminosity. am her appears to have the primary accreting region close to the position which is close to the grazing eclipse; a slight increase of its vertical and/or horizontal dimensions (and variable position) can give rise to a highly variable orbital modulation. this is visible not only for the site of the cyclotron emission (fig. 4), but also for the site of the bremsstrahlung emission which can increase so much that it even becomes temporarily uneclipsed in some high states [16]. figure 4: dramatic changes of the orbital modulation during transition from the high to the low state of am her (ccd v -band aavso data). time in jd– 2 400 000 is given in the legend. the orbital ephemeris of [5] is used. 5 conclusions in am her, the optical emission displays cycles in the transitions between the high and low states, which are detectable only for the limited time segments. in addition to the intermittent cycle of the transitions, accumulation of episodes of the low states in clusters produces an additional, long cycle of activity. a single isolated short episode of the low state does not suggest a break of this cycle. this has a consequence for the structures and their lifetimes on the donor and/or the changes of the configuration of the magnetic field in the whole system. the configuration of the accreting matter influences the emission of am her in various spectral bands. the accretion modes (single-pole accretion, two-pole accretion) vary with time (from one high-state episode to another). also the changes of the accretion region(s) and/or accretion modes are necessary to explain the relation between the optical and x-ray emission in the high states. acknowledgement this study was supported by grants 13-33324s and 13394643 provided by the grant agency of the czech republic. this research has made use of the observations provided by the asm/rxte team, the swift/bat team, the aavso international database (massachusetts, usa) and the afoev database (strasbourg, france). we thank the variable star observers worldwide whose observations contributed to this analysis. we used the code developed by dr. g. foster and available at http:// www.aavso.org/winwwz. we thank prof. petr harmanec for providing us with the code hec13. the fortran source version, the compiled version and brief instructions on how to use the program can be obtained via http:// astro.troja.mff.cuni.cz/ftp/hec/hec13/. references [1] foster, g.: 1996, aj, 112, 1709 [2] gänsicke, b. t., et al.: 2001, a&a, 372, 557 [3] gänsicke, b. t., et al.: 2006, apj, 639, 1039 doi:10.1086/499358 [4] heise, j., et al.: 1985, a&a, 148, l14 [5] heise, j., verbunt, f.: 1988, a&a, 189, 112 [6] henden, a.: 2011, aavso database [7] hessman, f. v., et al.: 2000, a&a, 361, 952 [8] hudec, r., meinunger, l.: 1976, ibvs, 1184, 1 [9] kafka, s., et al.: 2008, apj, 688, 1302 doi:10.1086/592186 [10] kafka, s., hoard, d. w.: 2009, pasp, 121, 1352 doi:10.1086/648579 [11] kalomeni, b.: 2012, mnras, 422, 1601 doi:10.1111/j.1365-2966.2012.20736.x [12] levine, a. m., et al.: 1996, apj, 469, l33 [13] livio, m., pringle, j. e.: 1994, apj, 427, 956 doi:10.1086/174202 [14] matt, g., et al.: 2000, a&a, 358, 177 84 http://dx.doi.org/10.1086/499358 http://dx.doi.org/10.1086/592186 http://dx.doi.org/10.1086/648579 http://dx.doi.org/10.1111/j.1365-2966.2012.20736.x http://dx.doi.org/10.1086/174202 activity of the polar am her (rx j1816.2+4952): a short review [15] michaut, c., et al.: 2012, mmsai, 83, 665 [16] priedhorsky, w., et al.: 1987, a&a, 173, 95 [17] šimon, v.: 2011, newa, 16, 405 doi:10.1016/j.newast.2011.03.001 [18] scharlemann, e. t.: 1982, apj, 253, 298 doi:10.1017/cbo9780511586491 [19] warner, b.: 1995, cataclysmic variable stars, cambridge univ. press, cambridge [20] wickramasinghe, d. t., et al.: 1991, mnras, 251, 28 [21] wu, k., kiss, l. l.: 2008, a&a, 481, 433 85 http://dx.doi.org/10.1016/j.newast.2011.03.001 http://dx.doi.org/10.1017/cbo9780511586491 introduction long-term activity in the optical band optical and hard x-ray intensities in the high states role of the accretion modes conclusions acta polytechnica ctu proceedings doi:10.14311/app.2016.5.0038 acta polytechnica ctu proceedings 5:38–40, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app selected aspects of etcs-l3 deployment petr koutecký czech technical university in prague, faculty of transportation sciences, department of transport telematics, konviktská 20, prague, czech republic correspondence: koutepe1@fd.cvut.cz abstract. this paper focuses on selected problem areas in the implementation of etcs l3, analyz-es their impacts and offers a number of possible solutions as a basis for pilot testing. it compares the suitability of each solution and summarizes their advantages and disadvantages. keywords: ertms, etcs l3, odometry, its-r. 1. introduction control and command systems on the railways have undergone a relatively long development. on the one hand, the development is driven by increasing demands on safety, reliability, smoothness and fuel economy, on the other hand, the development was mainly limited by technical capabilities of the time in the past. the development possibilities of electronics and especially microprocessor technology and computing power have allowed in recent years to increasingly address the question of optimizing the control process quality and minimizing the necessity of the human factor’s intervention, which in earlier times was not possible to such an extent. this technical progress, pressure on cost cutting and the european union requirements for the interoperability of the railway networks have created the need for addressing the management and security of railway services in new ways. introducing new systems brings the need of identifying and addressing the potential risks and technical challenges associated with the transition to the new system. the aim of this paper is to point out possible problems in the implementation and deployment of etcs l3 on the conventional railway network and suggest possible solutions to these problems with the specification of advantages and disadvantages of the various options. 2. requirements for the full implementation of intelligent transport systems on railways (hereinafter its-r) and for the purposes of this article, we consider the target state to be a state in which the following conditions are met: (1.) there is a bidirectional data connection to the train (between mobile and stationary parts), (2.) the integrity check of the train using technical means on the vehicle is ensured, (3.) all locomotives are equipped with an on-board unit (obu) etcs. when projecting these demands while considering the current trend and the commitments of the european union member states in the field of the railway network interoperability, the ertms system on application level 3 (l3) is a suitable candidate for addressing the command and control system (ccs). 2.1. substantiation of the requirements requirements specified in the previous section are based primarily on the overall concept of its-r. the need for a data connection to the train is given mainly by the necessity of the existence of such a data transfer connection between the stationary and mobile parts of the etcs l3 system. however, the data connection can also be used with other subsystems in the its-r concept, such as the transmission of data for the ato system, transmission of diagnostic data, etc. another requirement – to ensure the train integrity – is another necessary condition for the etcs l3 system’s activity, where the existence of detection devices already disregarded. the third requirement requiring full equipment of the cabin section in all vehicles is again given by application level 3 of the etcs system, where mixed traffic (such as with l2) is operationally unacceptable after removing the signals. only the connection and fulfillment of all three requirements above at the same time gives us the opportunity to fully start taking advantage of etcs l3 âăş primarily to use the opportunity to minimize the infrastructure elements (signals, track circuits, axle counters). such minimization has several far-reaching impacts – reducing the investment demand compared to the situation where application level 2 (or even one) of the etcs system is installed to achieve the desired safety parameters; according to [1] by approximately 25% compared with l2. it is necessary to emphasize that etcs l1 and l2 are "only" an extension of conventional interlocking equipment and block signaling system and track security equipment. in practice this leads to duplication of some functions in rbc and ixl. this delivers increased investment and operating costs for the construction and operation of two parallel systems and also reduces the possibilities of 38 http://dx.doi.org/10.14311/app.2016.5.0038 http://ojs.cvut.cz/ojs/index.php/app vol. 5/2016 selected aspects of etcs-l3 deployment figure 1. required odometry accuracy [2] the system – especially if a link rbc -> ixl is not implemented for l2. only etcs l3 is not an extension of the current ixl – it is thus possible to leave out the riding principle in a fixed block and train ride control using the signals. 3. definition of problem areas 3.1. the accuracy of the odometer a key part of the function of determining train location in the etcs system is an odometer and doppler radar. since this is a safety-relevant function, it is necessary to consider a possible error in the given position in a safer direction. according to the specification [2], the required accuracy is expressed by the formula according to the traveled distance s: sdiff = 5 + 0.05xs[m] the position is specified (error is null) always after reading a balise group and the error refers to the distance traveled from that point. for the operation of the etcs system in its current form it is therefore necessary to count with this error in determining the usable length of each track. in addition, the position of the end of the train must be added to this inaccuracy in the case of etcs l3, e.g. for track length of 600 m it is necessary to consider an error of up to 35 m, and vacate the space behind the railroad switch signal at least by this distance in order for the railroad switch stretch to be regarded as vacant. this again reduces the usable length of the track. 3.2. train handling the method for determining train location and sections occupancy in the stretch of etcs l3 makes it necessary to address potential problems arising from the train handling, such as splitting, joining and shunting of train cars. the simplest situation occurs when joining and separating sets of coherent units, where with regard to the assumed equipment of all driving vehicles it will be possible to locate both parts and detect their integrity after division. however, this does not apply to the movement of parts of the train set and keeping a part of the train on the station track or to the train profiling into multiple parts. in such a situation, the vacancy of the concerned part of the infrastructure cannot be safely determined only with the use of the etcs l3 system’s technical means. 4. suggested solution 4.1. the accuracy of the odometer to increase the usable length of the transport rails, it may be necessary to increase the accuracy of the positioning system. with current specifications, this problem can be solved by placing one or more locators inside the balises of a long track section. this will split it into several smaller sections, where the odometer’s inaccuracy is proportionately smaller. another possibility is the gradual tightening of the requirement for maximum permissible error in the etcs odometer (now 5m + 5%). similar devices used in the cbtc systems achieved accuracy of about 1% according to [3] already (using e.g. a doppler radar with multiple antennas). 4.2. train handling the problem with train division, shutting down of train cars, and shifts can be solved in principle several ways, which will be discussed in the following text. the advantages and disadvantages of various options and a comment on the possible applicability are also mentioned. 4.2.1. confirmation of occupancy by human operators the occupancy of selected parts of the infrastructure can be confirmed with the participation of the human factor. this principle is used according to [4], e.g. in ertms regional in sweden. after confirming the section’s occupancy with the human factor, the ride through the stretch is possible only in the staff responsible mode with speed restrictions. after the first train passes, the stretch is already considered vacant from the point of view of previous manipulation, and the ride of the following trains is no longer restricted. the disadvantages of this solution are obvious – the need for participation of the human factor, the risk of failure is limited by limiting the speed for the next train. this thereby decreases the throughput performance parameter. however, this solution may be suitable for regional routes with limited speed and sporadic shifts. 4.2.2. partial equipment with detection resources in case of frequent handling, using conventional detection devices (track circuits, axle counters) at this point is offered as a solution to the question of detecting the occupancy of the infrastructure’s section. the disadvantage regarding the involvement of the human factor on detecting the occupancy of the section is thus eliminated, the disadvantage being the need to install detection devices, albeit to a very limited extent. 39 petr koutecký acta polytechnica ctu proceedings 5. evaluation, conclusion the article pointed out several questions that will be necessary to address within the preparation of the possible pilot deployment of etcs l3. the solution’s suitability in some cases depends on the local situation and the nature of the track on which the system will be deployed; all possible situations cannot generally always be covered. in the near future it is also possible to expect verification of the related technologies that could help contribute as another alternative to solving open points (e.g. use of satellite positioning systems instead of fixed balises, use of modern communication technology instead of gsm-r, etc.) in the event of a positive outcome. 6. abbreviation • ato ... automatic train operation • cbtc ... communication based train control • ccs ... command and control system • ertms ... european rail traffic management system • etcs ... european train control system • gsm-r ... global system for mobile communications-railway • its-r ... intelligent transport system-railway • ixl ... interlocking • obu ... on-board unit • rbc ... radio block centre references [1] w. coenraad. level 3 : from high speed vision to rural implementation [online], 2011. http://www.irse.org/knowledge/publicdocuments/ 2011_09_29_ertms_level_3_from_high_speed_ vision_to_rural_implementation.pdf. [2] ertms/etcs performance requirements for interoperability, subset-041, issue 3.1.0, 2012, unisig [online]. http://www.era.europa.eu/document-register/ documents/set-2-index014-subset-041%20v310.pdf. [3] ertms level 3 risks and benefits to uk railways, final report; transport research la-borator [online], 2010. http: //www.trl.co.uk/media/773946/cpr798_-_ertms_ level_3_risks_and_benefits_to_uk_railways.pdf. [4] ertms regional functional requirements specification, version 03.08, uic, 2009. 40 http://www.irse.org/knowledge/publicdocuments/ 2011_09_29_ertms_level_3_from_high_speed_vision_to_rural_implementation.pdf http://www.irse.org/knowledge/publicdocuments/ 2011_09_29_ertms_level_3_from_high_speed_vision_to_rural_implementation.pdf http://www.irse.org/knowledge/publicdocuments/ 2011_09_29_ertms_level_3_from_high_speed_vision_to_rural_implementation.pdf http://www.era.europa.eu/document-register/documents/set-2-index014-subset-041%20v310.pdf http://www.era.europa.eu/document-register/documents/set-2-index014-subset-041%20v310.pdf http://www.trl.co.uk/media/773946/cpr798_-_ertms_level_3_risks_and_benefits_to_uk_railways.pdf http://www.trl.co.uk/media/773946/cpr798_-_ertms_level_3_risks_and_benefits_to_uk_railways.pdf http://www.trl.co.uk/media/773946/cpr798_-_ertms_level_3_risks_and_benefits_to_uk_railways.pdf acta polytechnica ctu proceedings 5:38–40, 2016 1 introduction 2 requirements 2.1 substantiation of the requirements 3 definition of problem areas 3.1 the accuracy of the odometer 3.2 train handling 4 suggested solution 4.1 the accuracy of the odometer 4.2 train handling 4.2.1 confirmation of occupancy by human operators 4.2.2 partial equipment with detection resources 5 evaluation, conclusion 6 abbreviation references acta polytechnica ctu proceedings doi:10.14311/app.2016.3.0060 acta polytechnica ctu proceedings 3:60–64, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app numerical method for estimation of tensile load in tie-rods kseniia riabova∗, luca collini, rinaldo garziera university of parma, parco area delle scienze, 181/a, parma, italy ∗ corresponding author: kseniia.riabova@studenti.unipr.it abstract. the work introduces a two-phase method for determination of axial loads in tie-rods. the method described here consists of an experimental activity and an automated numerical calculation. the influence of considering an elastic winkler-type bed to model the tie-rod constraint inside the wall has been investigated. the algorithm used for calculation involves a solution of a functional minimization problem, where the tensile load and the stiffness of elastic foundation at the edges are used as optimization parameters and the error function, which describes the deviation between the frequencies measured and those calculated using finite element method, is minimized. qualitative analysis of the results showed a significant reduction of the error compared to models with different boundary conditions. the method showed to be conservative for the strength evaluation of the rods, because the optimal values of tensile loads appeared to be higher than the load in perfect encastre conditions. keywords: tie-rods, non-destructive technique, numerical method. 1. introduction tie-rods are structural elements used in a wide range of civil constructions. one of purposes they serve is to provide support for masonry arches and vaults in ancient buildings (e.g. churches, castles, etc.), which are known to lurch and founder course of time. tierods are subjected to axial tension and, thus, help the building resist occurring lateral loads exerted by structural elements, walls and facades. over the years deformation of masonry walls and some displacements in the building may cause significant changes in the axial loads of tie-rods. in the extremes this can lead to either failures in tie-rods structural integrity, or to laziness of tie-rods that stop carrying out their duty when they loose loads. that is why regular monitoring of tie-rods condition is of a great importance. the goal of the presented work is to determine axial loads acting on the tie-rods of the fifteenth century casa romei located in ferrara, emilia-romagna, italy, and thus to evaluate their functionality and reliability. an approach based on an experimental investigation and a numerical method is introduced to serve this purpose. 2. previous studies some attempts have been made throughout the years to develop an appropriate non-destructive technique for and indirect estimation of the tensile load in tierods. previous studies [1–3] report a method that combined static and dynamic force identification. tierods were modeled as simply supported euler beams with rotational springs of similar stiffness added on each edge. the stiffness of the spring and the force were the two unknowns obtained from the system of equations, built with a static equation for deflection and a dynamic equation for natural frequencies. another study [4] introduced a static approach for force identification. the experiment consisted of measuring three vertical displacements and strains variations at three sections of the tie-rod under a concentrated load; in [5] an algorithm to identify the axial tensile force in ancient tie-rods by using the first three natural frequencies is developed. the tie-rod was modelled as an euler beam of uniform cross-section, neglecting the shear deformation and rotary inertia, and was assumed to be simply supported at the ends with additional rotational springs. recently, maes et al. [6] introduced a method that enables definition of axial loads in slender beams with unknown boundary conditions, taking into account affects of rotational inertia of the beam and masses of sensors. however, it requires data from five or more sensors along the length of the beam to determine all the introduced unknown of the inverted problem. a similar technique of the axial force identification was developed by li et al. [7] focusing on studies of euler-bernoulli beams and takes into account bending stiffness effects. rebecchi et al. [8] established an analytical method of processing experimental data from five instrumented sections of a prismatic slender beam, which showed excellent results in estimation of the axial load in tie-rods. the method does not require any exact value of effective length of the beam, but neglects both rotary inertia and shear deformations effects in the solution for beam vibrations. for cases of similar beams, tullini et al. [9–11] proposed a static method of axial force identification. the analytical algorithm makes use of any set of experimental data 60 http://dx.doi.org/10.14311/app.2016.3.0060 http://ojs.cvut.cz/ojs/index.php/app vol. 3/2016 estimation of tensile load in tie-rods represented by flexural displacements or curvatures measured at five cross-sections of the beam subjected to an additional concentrated lateral load. again, gentilini et al. [12] developed a procedure that combines dynamical testing with fem simulations using added masses. the method was tested out for tie-rods of various length and load intensity, showing reliable results. livingston et al. [13] identified the tensile force in prismatic beams of uniform section by using modal data and assuming rotational and vertical springs at each end of the beam. shear deformation and rotary inertia were neglected (according to the euler beam model). 3. estimation method in the present study authors intend to introduce a method of health monitoring of tie-rods inserted in ancient monumental masonry buildings. the method consists of an in-situ experimental activity and an automated two-parameter optimization algorithm which allows to evaluate the axial load in tie-rods with a good precision. the technique is basically a simply executed frequency-based identification method that allows to minimize the estimation error. about six natural frequencies can be easily identified with a simple test by experimentally measuring the frequency response functions (frfs) of the tierods with instrumented hammer excitation. further a parametric finite element model of a tie-rod is developed in the fem analysis software abaqus. the part of a tie-rod hidden inside the masonry wall is assumed to have a length of 0.2 m and the constraints given to this part are modelled as elastic foundations (winkler bed). the tensile force and the stiffness of the foundation are chosen as the unknown parameters. in some cases the length of the rod inserted inside the masonry wall can be also assumed as unknown. the sought axial load, as it is explained subsequently, is obtained through an optimization routine that minimizes the deviation between corresponding experimentally determined eigenfrequencies and those calculated by fem. the authors have previously tested the present technique with some variations over different buildings and situations [14–16]. the novelty introduced in the present work is the optimization with respect to the stiffness of the winkler bed type boundary conditions. 3.1. experimental part the tie-rods investigated during the case study have been installed at different points along the lifespan of casa romei (see fig. 1), therefore they differ in dimensions, cross-section shapes and material condition. measurements of geometrical characteristics and of natural frequencies were performed for each reachable tie-rod of the building. the natural frequencies were obtained from the analysis of response to dynamical excitation applied to tie-rods in horizontal plane for a more accurate estimation of the axial load. since figure 1. inner yard of casa romei. figure 2. a typical frf plot (acceleration amplitude vs. frequency). the studied rods are much stiffer in the vertical plane, tests in vertical direction were not performed. the used instrumentation was composed by tools listed in tab. 1. the signal from accelerometers was handled by the dynamic signal acquisition module national instrument (ni) 9234 and acquisition software developed in labview and further elaborated in matlab resulting in the frequency response functions (frf) for each tierod. frf for a ground floor tie-rod pt4 is presented in fig. 2. another important part of the experimental activity was to measure accurately the geometric characteristics of tie-rods, i.e. cross-section dimensions and lengths. for the further study it was assumed that the cross-section remains the same along all the length of a rod. the tested rods are crafted in iron for which the characteristics vary insignificantly, thus the material data was assumed as follows: e = 2 × 1011 n/m2, ρ = 7850 kg/m3, υ = 0.3. the main parameters e and υ appear in the frequencies under the square root, so even some variation in these values can only have a minor influence on the natural frequencies. for the further analysis first six natural frequencies were identified for each tie-rod by means of peakpicking from frfs. six eigenmodes are providing 61 k. riabova, l. collini, r. garziera acta polytechnica ctu proceedings tool manufacturer model sensitivity impact hammer brel&kjaer 8202 4pc/n accelerometer pcb 356a01 0,01 v/(m/s2) accelerometer pcb 356a01 0,01 v/(m/s2) table 1. list of experimental tools. an over constrained problem, thus the higher modes were not taken under consideration in this research. besides that, identification of higher modes might appear inaccurate due to larger possible measurement errors. 3.2. numerical part since the extremities of tie-rods are built into the masonry walls in a way that hardly leaves a possibility to be certain about the end constraints, as a first iteration, boundary conditions for the edges were modeled as plain fixed and/or simply supported. in both cases for any range of optimization parameters (length and force) and weight coefficients the error function reaches minimum every time for the minimal length in the range, i.e. for the measured length. this means that the minimum is forced. investigation of the function in symbolic mathematics package maple 13.0 showed good correspondence of the results obtained from fem with analytical models of a string and a beam under axial load. also the error function has an absolute minimum that lies however below the length measured. this kind of behavior proves that the bcs are irrelevant. the real conditions on the edges of tie-rods are unknown and may vary from one rod to another, because they are fixed inside masonry walls in a way that is hard to determine using non-destructive techniques. however, certain attempts can be made in order to develop a generalized parametric model suitable for numerical determination of loads in tie-rods. in order to determine the loads, tie-rods are modeled in fem software abaqus using 3d beam elements that incorporate timoshenko beam theory (b31), which allows to take into account shear deformation and rotational inertia effects. the cross section is assumed to be constant along each rod. as a first step a pretension load n is applied to the beam and as a second step modal analysis is performed. since the value of the pretension load is the subject of search, it has to be tuned to make the results of modal analysis in fem reach a good agreement with experimentally defined frequencies. however, manual tuning of the load is not considered to be an option in this case, because there is no certainty about the boundary conditions at the beam edges. this problem is overcome by means of a parametric fem model and an optimization tool for computing. in fem model the measured length of the tie-rod is represented by 50 beam elements; boundary conditions are assumed to be an elastic bed and, thus, are represented by 5 spring elements on each edge of the beam, acting in the direction of considered vibrations. also the displacement in direction x (tie-rod axis) is restrained. the sketch of the assumed model is displayed in fig. 3. stiffness of each spring element together with the sought load are chosen as optimization parameters in the problem stated. the optimization program requires a set of experimentally obtained frequencies, ranges of stiffness and force with sizes of steps for each and also a set of weight coefficients for frequencies, that define importance of the corresponding frequency for the analysis. combinations of parameters form a grid and the program launches abaqus input file for each nod of this grid and then extracts and filters natural frequencies. vibrations in z direction only are of our particular interest due to testing that was carried out in the horizontal plane. optimization criteria for the problem is represented by the residual error between experimentally defined frequencies and those obtained from fem analysis. the error e is calculated according to the following formula: e = √√√√ n∑ k=1 p2 k(fexp k − ff em k )2 (1) where pk is a weight arbitrary given to each frequency. the optimal values of stiffness of the elastic bed and of axial force deliver minimum value of the error function. the optimization process starts from a reasonable value of the load which can be predicted as an optimal load for a simplified model with fixed ends, i.e. for infinite stiffness of the elastic bed at the constraints. the second step to be done is now to vary the stiffness of the spring bed, and optimize their value to minimize again the error. this implies a refinement process of the parameters along what we call zooming technique [15]. operatively, the algorithm defines a matrix of values and refines grid of parameters to be solved just where local minima of the error as defined in eq. 1 are found. a typical graphic of the surfaces representing the error distribution is presented in eq.4. here the error values are plotted with respect to stiffness and axial load, for a specific tie-rod. the free length l, and length of lf (in fig. 3) are kept constant. the clear minima of the error functional can be observed. 62 vol. 3/2016 estimation of tensile load in tie-rods figure 3. sketch of the computational model. figure 4. error as function of bed stiffness and axial load for different sets of weight coefficients. the error which represents the difference between numerical and experimental frequencies is calculated from the eq. 1. each of the differences (in hz) between couples of frequencies is multiplied by a weight pk in order to allow us to assign higher (or lower) importance to some frequencies rather than the others. the set of weights is then arbitrary chosen, but generally, the first frequencies, or just the fundamental one, have greater importance. a sensitivity analysis showed that the minima of the error functional eq. 1 with respect to the sought tensile load is not influenced by the weights set (see fig. 4). the variation of the error is depicted in fig. 5, wherefrom it can be observed that the minimum value of the error is reached for the optimal elastic bed stiffness and is reached for the up to higher load compared to the encastre boundary conditions, thus, the method reveals to be conservative for the strength evaluation of the rods. the values of error vary from one tie-rod to another, this shows that the model with winkler bed boundary conditions fits better for some of the rods, however these errors were less than those calculated for ordinary fixed or simply supported boundary conditions. for a couple of tie-rods though a perfect encastre boundary condition at the walls appeared to be the best approximation which was demonstrated by an improvement in the error value compared to the case when a set of springs was modelled at their extremities. figure 5. influence of the elastic bed stiffness on the minimal error. 4. conclusions in this work an optimization process is shown and discussed in determining the axial load in structural iron tie-rods. the influence of considering an elastic winkler-type bed to model the tie-rod constraint into the wall has been investigated. this constitutes the major novelty of this work, with respect to the previous studies. structural assessment of the overall building stability is enabled by the described method throughout the identification of axial loads in tie-rods via experimental and numerical activity. in particular, the introduced computational model is able to take into account even unknown boundary conditions that are typical for tie-rods installed in ancient buildings. furthermore, from the simulations it was concluded that the variation of tensile load shifts the set of frequencies (higher the load, higher the frequencies), while the change in elastic bed stiffness changes the distance between natural frequencies. and finally, the conclusion about the method convergence can also be made based on the fact that different sets of weight coefficients bring to minor changes in the sought axial load in tie-rods. references [1] c. blasi. sulla determinazione del “tiro” nelle catene mediante prove statiche e dinamiche. atti iii congresso nazionale assirco 1988. [2] c. blasi. determining the axial force in metallic rods. structural engineering international (iabse) 4:241–246, 1994. 63 k. riabova, l. collini, r. garziera acta polytechnica ctu proceedings [3] s. sorace. parameter models for estimating in-situ tensile force in tie-rods. journal of engineering mechanics 122:818–825, 1996. [4] s. briccoli bati. experimental method for estimating in situ tensile force in tie-rods. journal of engineering mechanics 127:1275–1283, 2001. [5] s. lagomarsino. the dynamical identification of the tensile force in ancient tie-rods. engineering structures 27:846–856, 2005. [6] k. maes. identification of axial forces in beam members by local vibration measurements. journal of sound and vibration 332:5417–5432, 2013. doi:10.1016/j.ijrmms.2008.06.005. [7] s. li. vibration-based estimation of axial force for a beam member with uncertain boundary conditions. journal of sound and vibration 332:795–806, 2013. [8] g. rebecchi. estimate of the axial force in slender beams with unknown boundary conditions using one flexural mode shape. journal of sound and vibration 332:4122–4135, 2013. doi:10.1016/j.jsv.2013.03.018. [9] n. tullini. dynamic identification of beam axial loads using one flexural mode shape. journal of sound and vibration 318:131–147, 2008. [10] n. tullini. bending tests to estimate the axial force in tie-rods. mechanics research communications 44:57–64, 2012. [11] n. tullini. bending tests to estimate the axial force in slender beams with unknown boundary conditions. mechanics research communications 53:15–23, 2013. [12] c. gentilini. nondestructive characterization of tie-rods by means of dynamic testing, added masses and genetic algorithms. journal of sound and vibration 332:76–101, 2013. doi:10.1016/j.jsv.2012.08.009. [13] t. livingston. estimation of axial load in prismatic members using flexural vibrations. journal of sound and vibration 179:899–908, 1995. doi:10.1016/j.jsv.2012.10.019. [14] m. amabili. estimation of tensile force in tie-rods using a frequency-based identification method. journal of sound and vibration 329:2057–2067, 2010. [15] m. amabili. a hybrid method for the nondestructive evaluation of the axial load in structural tie-rods. nondestructive testing and evaluation 26(2):197–208, 2011. [16] l. collini. load and effectiveness of the tie-rods of an ancient dome: technical and historical aspects. journal of cultural heritage 16:597–601, 2015. 64 http://dx.doi.org/10.1016/j.ijrmms.2008.06.005 http://dx.doi.org/10.1016/j.jsv.2013.03.018 http://dx.doi.org/10.1016/j.jsv.2012.08.009 http://dx.doi.org/10.1016/j.jsv.2012.10.019 acta polytechnica ctu proceedings 3:60–64, 2016 1 introduction 2 previous studies 3 estimation method 3.1 experimental part 3.2 numerical part 4 conclusions references acta polytechnica ctu proceedings doi:10.14311/app.2017.10.0007 acta polytechnica ctu proceedings 10:7–11, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app correlation relationships for the hypoplastic model for fine grained soils tomáš kadlíček∗, tomáš janda, michal šejnoha department of mechanics, faculty of civil engineering, czech technical university in prague, thákurova 7/2077, 166 29 prague, czech republic ∗ corresponding author: tomas.kadlicek@fsv.cvut.cz abstract. the paper is concerned with our ongoing research effort devoted to the development of reliable computational tools for the calibration of advanced constitutive models of soils. at present, such software is available for the hypoplastic model of clays applicable to soft soils. this software provides a stepping stone for the determination of potential links between individual model parameters and fundamental characteristics of soils. identifying such links would allow for tuning the model without performing time consuming experiments, particularly in the case of an initial design. some preliminary results are presented in the paper. keywords: hypoplasticity, fine grained soils, constitutive modeling, correlation. 1. introduction the theory of hypoplasticity has been receiving considerable attention in recent years, particularly for its capability of well simulating the basic characteristics of soils resulting in reliable predictions at a structural level. these characteristics include not only the dependency of stiffness on the void ratio, but also the stiffness dependency on strain and the loading history. such relationships are hardly available with frequently used elastoplastic models of the mohr-coulomb (mc). these are generally adopted in fem simulations because of their simplicity and straightforward links to basic strength parameters such cohesion and the angle of internal friction, which are included in regular laboratory test protocols or available in common material databases. to provide a similar comfort or at least considerably simplify the use of hypoplastic models is the principal objective of our current research focusing particularly on the masin hypoplastic model for fine grained soils (hc) [1] and the von wolffersdorff hypoplastic model for coarse grained soils (vw) [2]. in particular, two specific directions are investigated. the first aims at creating easy to use calibration software built upon standard oedometric and triaxial laboratory tests. the second option assumes a calibration procedure in the form of tables or graphs enabling the determination of model parameters on the basis of specific input data. knowing the link between the model parameters and more standard soil parameters creates the basis for the development of such a tool. this objective is examined in this paper and some preliminary results are presented. 2. hypoplastic model for fine grained soils the theory of hypoplasticity can be considered a possible alternative to the theory of elastoplasticity. unlike elastoplasticity, it does not separate an elastic and plastic deformation, but its deformation is controlled by the evolution of state variables, namely pressure and the void ratio. consequently, hypoplasticity exhibits a distinct nonlinear deformation both in primary loading and elastic unloading. the state variables are bound in the e×q×p (e âăş void ratio, q deviatoric stress, p mean stress) space, where all admissible states are enclosed by the so called state boundary surface (sbs). the hc model defines five material parameters: λ∗, κ∗, n, ϕc and ν. these parameters can be calibrated on the basis of simple oedometric and triaxial laboratory tests. when properly tuned the model provides reliable and accurate predictions of the soil response in the solution of real engineering tasks. the first three parameters: λ∗, κ∗ and n are closely related to the oedometric test. as seen in fig. 1, the parameter λ∗ controls the slope of the normal consolidation line (ncl). the position of ncl in the ln p× ln(e+ 1) space is driven by the parameter n. clearly, recall fig. 1, its value corresponds to the mean pressure p = 1 kpa. the third parameter κ∗ represents the slope of the swelling line followed upon unloading as also evident from fig. 1. for more details, the interested reader is referred to [1] and [2]. the remaining two parameters ϕc and î¡ are typically determined on the basis of the triaxial test. in the case of fine grained soils, an undrained triaxial test accompanied by measuring the pore pressure is preferred. the critical state friction angle ϕc is dis7 http://dx.doi.org/10.14311/app.2017.10.0007 http://ojs.cvut.cz/ojs/index.php/app t. kadlíček, t. janda, m. šejnoha acta polytechnica ctu proceedings figure 1. parameters λ∗, κ∗ and n in the ln p × ln(e+ 1) space figure 2. critical friction angle ϕc in the t′ × s′ space played in fig. 2. the effective stresses t′ and s′ in fig. 2 are written as s′ = σ′1 + σ′3 2 t′ = σ′1 − σ′3 3 (1) the last parameter î¡ is related to the ki/gi ratio, where ki is the bulk modulus in isotropic compression and gi is the shear modulus in undrained shear for a test starting from the isotropic normally compressed state. obtaining a reliable prediction of this parameter requires a parametric study. the result of such a parametric study in terms of an equivalent deviatoric stress plotted as a function of the vertical strain is shown in fig. 3. additional details are available in [1] and [2]. further details on the proposed calibration procedure for both hc and vw models, developed as well as validated on the basis of a large ensemble of laboratory tests, are provided in [3]. in the next section, limiting our attention to the hc model, the model parameters determined for a representative set of soil samples will be correlated with a selected set of other, easily determined, soil characteristics. 3. hc parameters’ correlations soils can be characterized and classified according to the particle-size distribution and atterberg limits. in order to determine the size distribution of particles in a specimen the sedimentation test (for grain sizes < 0.063 mm) and measurements of the amount of particles passing a particular sieve size can be performed to derive the grain size distribution curve. the atterberg limits are determined as the values of mass moisture content of a soft soil and are defined as follows: • shrinkage limit ws is the water content where an ongoing loss of moisture is not followed by any additional volume reduction • plastic limit wp is the water content where cylindrical samples of soil being 3mm in diameter fall apart in pieces 8-10mm long • liquid limit wl is the water content where a groove made in soil placed in the casagrande device merges at a length of 10mm after 20 drops. in the present study, the results from oedometric and triaxial measurements and index tests carried out on eight samples of soft soils were exploited. while the first set of experiments was employed in the calibration procedure to assess the values of individual model parameters, the actual soil classification was based on the index tests. the resulting values are listed in tab. 1. apart from model parameters and the atterberg limits wl and wp, the table also offers the percentage content of fine soil particles fwith the diameter d < 0.063mm. the particle-size distribution is also plotted in fig. 4 for the sake of clarity. when searching for possible correlations between the model parameters and the selected soil characteristics it has been proven convenient to adopt parameters calibrated on the basis of reconstituted soil samples. these samples were prepared from the original undisturbed soil by changing the sample paste consistency up to a water content of 1.5 ×wl while completely disrupting their original internal structure and as such losing any information about the prior loading history. the values of model parameters are nevertheless the same as those which would have been found when adopting the original undisturbed samples. the relationships between the values of hc parameters and the index characteristics, see fig. 5 and 6, can be conveniently specified in terms of the coefficient of correlation r ∈ (−1; 1). recall that the correlation reflects the noisiness and direction of a linear relationship of two random variables, but not the slope of that relationship. when there is no obvious relationship 8 vol. 10/2017 correlation relationships for the hypoplastic model figure 3. evolution of the equivalent deviatoric stress q as a function of the vertical strain εa for various values of ν table 1. parameters of the hc model and selected parameters from index tests for reconstituted soil samples figure 4. particle-size distribution for eight samples of sampled soils 9 t. kadlíček, t. janda, m. šejnoha acta polytechnica ctu proceedings figure 5. correlations between hc parameters and index characteristics (correlation), the coefficient of correlation is equal to 0. in the case of a perfect direct (increasing) correlation, r approaches 1 and in the case of a perfect inverse (decreasing) correlation, r approaches -1. thus, the closer the coefficient is either to -1 or 1, the stronger the correlation between the two variables. tab. 2 shows the coefficient of correlation for all five hc model parameters and the selected index characteristicswl andwp, and the percentage content of fine soil particles f . a relatively strong (direct) correlation is observed for the model parameters λ∗ and n and the content of fine soil particles f . this is also confirmed by the plots in fig. 5(a,b) showing no apparent scattering. remember that the parameters λ∗ and n control the position of ncl in the ln p × ln(e+1) space. both tab. 2 and the plots in fig. 5(c,d) suggest the parameter κ∗ be more dependent on the plasticity index wp and the liquid limit wl. the same conclusion, although not directly visible from tab. 2, can be drawn for the parameter v, see fig. 5(e,f). for this parameter, the value of the coefficient of correlation is polluted by the results derived from the soil sample labeled as “praha a”, which falls off the more or less linear relationship. this specimen 10 vol. 10/2017 correlation relationships for the hypoplastic model table 2. correlation values r figure 6. correlations between hc parameters and index characteristics shows the lowest values of the atterberg limits and the lowest content of fine soil particles f . unlike the first four parameters associated more or less with the compressive response of soil, the critical state friction angle ϕcv does not seem to show any correlation with the selected index characteristics, see both tab. 2 and fig. 6(g). however, its determination is rather simple from a standard triaxial test with no need for additional optimization. 4. conclusion although drawing a solid conclusion as to the direct link of the hc model parameters to other, more standard, soil parameters would require a considerably larger set of experiments, the potential of this goal has been clearly confirmed by this study. in particular, a relatively strong correlation of the hc model parameters λ∗, κ∗, n and ν and the selected index parameters or the particle size distribution data can be found. while limiting our attention to the hc model we expect that a similar study performed for the vw model can lead to similar conclusions. obviously, this must be supported by a much larger set of data to be examined. we expect such information to grow with the help of a web application which not only provides calibration software, but opens a way to collected results from laboratory measurements all over the world. [4] 5. acknowledgement the financial support from projects ta04031603 and sgs16/038/ohk1/1t/11 is gratefully acknowledged. references [1] d. mašín. clay hypoplasticity with explicitly defined asymptotic states. acta geotechnica 8(5):481–496, 2013. doi:10.1007/s11440-012-0199-y. [2] d. mašín. a hypoplastic constitutive model for clays. international journal for numerical and analytical methods in geomechanics 29(4):311–336, 2005. doi:10.1002/nag.416. [3] m. šejnoha, t. kadlíček, t. janda. calibration of hypoplastic models for soils. in engineering mechanics 2015, vol. 821 of applied mechanics and materials, pp. 503–511. trans tech publications, 2016. doi:10.4028/www.scientific.net/amm.821.503. [4] p. a. von wolffersdorff. a hypoplastic relation for granular materials with a predefined limit state surface. mechanics of cohesive-frictional materials 1(3):251–271, 1996. doi:10.1002/(sici)10991484(199607)1:3<251::aid-cfm13>3.0.co;2-3. 11 http://dx.doi.org/10.1007/s11440-012-0199-y http://dx.doi.org/10.1002/nag.416 http://dx.doi.org/10.4028/www.scientific.net/amm.821.503 http://dx.doi.org/10.1002/(sici)1099-1484(199607)1:3<251::aid-cfm13>3.0.co;2-3 http://dx.doi.org/10.1002/(sici)1099-1484(199607)1:3<251::aid-cfm13>3.0.co;2-3 acta polytechnica ctu proceedings 10:7–11, 2017 1 introduction 2 hypoplastic model for fine grained soils 3 hc parameters' correlations 4 conclusion 5 acknowledgement references acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0085 acta polytechnica ctu proceedings 7:85–90, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app modeling of anisotropic growth and residual stresses in arterial walls anna zahna, daniel balzania,b,∗ a technische universität dresden, institute of mechanics and shell structures, 01062 dresden, germany b dresden center for computational materials science (dcms), 01062 dresden, germany ∗ corresponding author: daniel.balzani@tu-dresden.de abstract. based on the multiplicative decomposition of the deformation gradient, a local formulation for anisotropic growth in soft biological tissues is formulated by connecting the growth tensor to the main anisotropy directions. in combination with an anisotropic driving force, the model enables an effective stress reduction due to growth-induced residual stresses. a method for the imitation of opening angle experiments in numerically simulated arterial segments, visualizing the deformations related to residual stresses, is presented and illustrated in a numerical example. keywords: biomechanics, multiplicative anisotropic growth, residual stresses, opening angle. 1. introduction as living biological medium, arterial tissue is known to adapt to changes in its mechanobiological environment in order to improve the load-bearing capacities. such adaptation processes originate from growth and remodeling and may be indicated by the existence of residual stresses under externally load-free conditions. those residual stresses can be uncovered by extracting an arterial segment from the body and slicing it in radial direction. typically, the segment contracts in axial direction and springs open to a degree which depends on various factors, for example the height of the blood pressure [1]. being associated with a reduction of stress gradients in loaded states, residual stresses need to be included in numerical simulations to obtain a predictive stress distribution. computational methods to reduce stress gradients by incorporating residual stresses are proposed in the literature [2–5]. these methods are however rather engineering approaches, as no biological processes are included to obtain the residual stresses. focusing on growth as part of the adaptation processes, the addition of material, resulting in increasing wall thicknesses and diameters, is related to a reallocation of the stresses which may therefore allow for an optimized load bearing behavior. for the purpose of modeling these effects, an anisotropic growth model based on the multiplicative decomposition of the deformation gradient into a growth tensor and a remaining elastic part is presented. in this context, different approaches for anisotropic growth in soft biological tissues have been published, see e. g. [6, 7], where the anisotropy of the growth mechanism is based on the definition of macrostructural growth directions as for instance the radial direction. although the anisotropy of the material is taken into account, isotropic strainor stress-based quantities are used as driving forces in the evolution equations characterizing the growth tensor. decomposing the growth tensor itself into two parts related to the main material anisotropy directions, the presented growth model establishes a relation between the growth tensor and the fibrous tissue structure, which yields a local formulation and therewith supersedes a geometry-specific definition of the growth directions. aiming at rendering the growth and stress reduction mechanism more effective, an anisotropic stress-based driving force is formulated. in addition, a procedure for the calculation of the deformations related to growth-induced residual stresses in numerically simulated arterial walls is developed. the entire framework is illustrated with the aid of a numerical example on an idealized arterial segment. 2. computational framework having been introduced in the context of biomechanics by rodriguez et al. [8] in 1994, the multiplicative decomposition f = fefg of the deformation gradient f into a growth part fg and an elastic part fe is nowadays a common approach for the description of growth in soft biological tissues. the growth deformation is assumed to be stress-free, such that stresses arise only from the elastic part ce = f−t g cf−1 g of the strains. utilizing constitutive equations for hyperelastic materials, the stress tensor se in the intermediate configuration can be computed from se = 2 ∂ψ ∂ce . here, the formulation for fiber-reinforced soft biological tissues by balzani et al. [9] is applied, whereby polyconvexity of the strain energy function and thus ellipticity and existence of minimizers are ensured. the growth behavior is governed by the specific form of the growth tensor, which involves one or several local variables referred to as growth factors ϑi. the evolution equations for these growth factors ϑ̇i = kϑ(ϑi)φi(zi), are formulated as function of the growth-driving quantity φ(zi) and the growth function kϑ including the time-dependency. 85 http://dx.doi.org/10.14311/app.2017.7.0085 http://ojs.cvut.cz/ojs/index.php/app anna zahn, daniel balzani acta polytechnica ctu proceedings in this section, a model for anisotropic growth, relating the growth tensor fg to the anisotropy directions of the fibrous tissue material, is presented in subsection 2.1. applying this framework to idealized arterial segments under internal pressure, residual stress distributions that qualitatively reflect experimental observations can be generated. in subsection 2.2, the focus is directed on the numerical calculation of the deformations which arise from resecting and slicing previously simulated, residually stressed arterial segments. 2.1. model of anisotropic growth related to two fiber families an effective approach to reduce stresses is the enlargement of the cross-sectional area. accounting for this, the basic form fg = ϑi + (1− ϑ) a⊗a, describing a deformation with factor ϑ in all directions perpendicular to the direction given by the vector a, is chosen among different existing approaches for the growth tensor, see e. g. [10]. in constitutive material models for arterial tissues, two main fiber directionsa(a) with a = 1, 2 are usually considered to approximate the complex layer-wise arrangement of collagen fibers. assuming the anisotropy of growth to be linked with the fibrous tissue composition, a multiplicative decomposition of the growth tensor fg = f (ii) g f (i) g (1) into two separated parts f (a) g = ϑ(a)i + ( 1− ϑ(a) ) m (a) with (2) m (a) = a(a) g ⊗a(a) g , a = i, ii (3) is considered in order to account for two different anisotropy directions defined by the vectors a(i) g and a (ii) g . this formulation is based on the assumption that in arterial walls, even in patient-specific ones, a stress state exists with one negative principle stress showing in radial direction and two positive principle stresses in a plane of tensile loading (which coincides with the axial-circumferential plane in perfect-tube arteries). this can be supposed to be the reason for the observation that mainly two collagen fiber families, oriented in directions within this plane, occur in arterial walls. the resulting tissue structure might enable an optimized load-bearing mechanism, cf. [11, 12]. in more detail, these two fiber families may favorably be oriented symmetrically with respect to the direction of the highest principal stresses and thus, growth perpendicular to these directions would be desired by the tissue to reduce the stresses. consequently, the growth orientation vectors a(a) g are defined as angle bisectors of the fiber direction vectors according to a(i) g = a(1) +a(2) ||a(1) +a(2)|| and (4) a(ii) g = a(1) −a(2) ||a(1) −a(2)|| . (5) for the determination of the growth factors ϑ(a), two evolution equations ϑ̇(a) = kϑ(ϑ(a))φ(a)(z(a)), a = i, ii (6) have to be considered. therein, the function kϑ(ϑ(a)) =  k+ ϑ [ ϑ+ − ϑ(a) ϑ+ − 1 ]m+ ϑ , φ(a) > 0 k− ϑ [ ϑ(a) − ϑ− 1− ϑ− ]m− ϑ , φ(a) < 0, (7) which has been adopted from lubarda & hoger [13], scales the growth velocity by a factor k+/− ϑ and restricts the range of the growth factors to [ϑ−, ϑ+]. the function φ(a)(z(a)) defines the quantity which induces growth. recent publications examining stressdriven growth [6, 7, 14] propagate the utilization of the trace of the elastic part of the mandel stress given by φ(cese) = cese : i as measure for the pressure acting on the arterial wall. since this quantity is isotropic, it appears not to be adequate in combination with the anisotropic growth tensor and is therefore modified as follows. using the projections of the elastic part of the mandel stress into the anisotropy directions a(a) g , φ(a)(cese) = cese : m (a) e (8) with m (a) e = a(a) g ⊗a(a) g , (9) it can be ensured that growth in the plane perpendicular to a(a) g is only emerging if the stress in this direction is nonzero. the index “e” indicates, that the structural tensors m (a) e refer to the intermediate configuration. however, being eigenvectors of the growth tensor, the growth orientation vectors a(a) g do not change their direction during the transformation to the intermediate configuration, thus m (a) e = m (a). involving strain and stress quantites in the intermediate configuration, i. e. ce = f−t g cf−1 g and se = 2 ∂ψ ∂ce , the functions φ(a) depend on both growth factors ϑ(a), yielding a coupled system of evolution equations (6). using an euler backward scheme as for instance done in [7], the approximations ϑ̇(a) ≈ ϑ (a) n+1 − ϑ (a) n ∆t , a = i, ii (10) are adopted in order to compute the growth factors belonging to the actual time step n + 1. note that the index n + 1 is skipped from now on and only 86 vol. 7/2017 modeling of anisotropic growth and residual stresses in arterial walls quantities at the last time step are denoted by the index n. consequently, the local residuals r(i) := −ϑ(i) + ϑ(i) n + kϑ(ϑ(i))φ(i)(ϑ(i), ϑ(ii)) ∆ t, r(ii) := −ϑ(ii) + ϑ(ii) n + kϑ(ϑ(ii))φ(ii)(ϑ(i), ϑ(ii)) ∆ t have to fulfill r(i) = r(ii) = 0. to solve these nonlinear equations, a local newton iteration, characterized by index k, is performed. the linearized residuals linr(i) = r(i)∣∣ ϑ(a),k + ∂r(i) ∂ϑ(i) ∣∣∣∣∣ ϑ(a),k ∆ϑ(i),k+1 + . . . . . . ∂r(i) ∂ϑ(ii) ∣∣∣∣∣ ϑ(a),k ∆ϑ(ii),k+1 = 0, linr(ii) = r(ii)∣∣ ϑ(a),k + ∂r(ii) ∂ϑ(i) ∣∣∣∣∣ ϑ(a),k ∆ϑ(i),k+1 + . . . . . . ∂r(ii) ∂ϑ(ii) ∣∣∣∣∣ ϑ(a),k ∆ϑ(ii),k+1 = 0 are solved for the incremental updates ∆ϑ(i) and ∆ϑ(ii), and ϑ(i) and ϑ(ii) are updated until an appropriate abort criterion is fulfilled. during this iteration, the incremental updates are calculated by ∆ϑ(i),k+1 = r(i) a (i,i) ϑ ∣∣∣∣∣ ϑ(a),k − a (i,ii) ϑ a (i,i) ϑ ∣∣∣∣∣ ϑ(a),k ∆ϑ(ii),k+1, (11) ∆ϑ(ii),k+1 = a (i,i) ϑ r(ii) −a(ii,i) ϑ r(i) a (i,i) ϑ a (ii,ii) ϑ −a(i,ii) ϑ a (ii,i) ϑ ∣∣∣∣∣ ϑ(a),k , (12) where the abbreviations a (i,i) ϑ = −∂r (i) ∂ϑ(i) , a (i,ii) ϑ = − ∂r (i) ∂ϑ(ii) , a (ii,i) ϑ = −∂r (ii) ∂ϑ(i) , a (ii,ii) ϑ = −∂r (ii) ∂ϑ(ii) are used. thus, the derivatives of the functions kϑ and φ(a) with respect to the growth factors have to be provided. differentiating eqs. (7) and (8) leads to ∂kϑ(ϑ(a)) ∂ϑ(a) =  m+ ϑ ϑ(a) − ϑ+ kϑ(ϑ(a)), φ(a) > 0 m− ϑ ϑ(a) − ϑ− kϑ(ϑ(a)), φ(a) < 0 (13) and ∂φ(i) ∂ϑ(j) = ∂cese ∂ϑ(j) : m (i) e = ( ∂ce ∂ϑ(j)se +ce ∂se ∂ϑ(j) ) : m (i) e (14) = ( ∂ce ∂ϑ(j)se +ce ( 1 2 ĉ e : ∂ce ∂ϑ(j) )) : m (i) e with i = i, ii and j = i, ii. herein, ĉe = 2 ∂se ∂ce is the elastic part of the tangent moduli in the intermediate configuration. the remaining unknown derivative of the strain ce with respect to the growth factor ϑ(a) has to be computed according to the chain rule by ∂ce ∂ϑ(a) = ∂ce ∂fg : ∂fg ∂ϑ(a) = ∂ce ∂fg : ∂fg ∂f (a) g : ∂f (a) g ∂ϑ(a) . (15) the first part is given through ∂ce ∂fg = −f−t g �ce −ce � f −t g (16) and the relations ∂fg ∂f (i) g = f (ii) g � i, (17) ∂fg ∂f (ii) g = i � (f (i) g )t , (18) ∂f (a) g ∂ϑ(a) = i −m (a), a = i, ii (19) can be derived for the other parts.1 combining eqs. (17)/(18) and (19), the results ∂fg ∂ϑ(i) = f (ii) g − f (ii) g m (i), (21) ∂fg ∂ϑ(ii) = f (i) g −m (ii)f (i) g (22) are obtained and all required parts for the incremental updates of the growth factors in eqs. (11)–(12) are determined. given the final values of ϑi and ϑii, the 2nd piolakirchhoff stress s = f−1 g sef −t g can be identified performing a pull back of se to the reference configuration. 2.2. visualization of residual stresses anticipating the results of the numerical example in section 3, where an idealized arterial segment under constant internal pressure is examined using finite element calculations, the question arises, how to determine the deformations which are related to residual stress states. in order to permit these deformations, a change of the boundary conditions is required, for instance the release of the right edge of a residually stressed arterial segment as shown in figure 1, which enables the opening of the segment by the angle ϕ. dealing with highly nonlinear material behavior and large deformations, this final deformation state can not be determined in one calculation step, thus a special procedure has to be applied. here, this procedure is proposed as follows. 1the symbol � is defined such that the relation (a �b)︸ ︷︷ ︸ =:d : (a⊗ b) = aa⊗bb, dijkl = aikbjl (20) is valid, which for instance results in the calculation rule abc = ( a �ct ) : b. 87 anna zahn, daniel balzani acta polytechnica ctu proceedings ϕ ϕ 2 figure 1. definition of the opening angle ϕ in an idealized, symmetric arterial geometry. (1.) define the initial boundary value problem including the discretization of the unstressed configuration, apply the loads stepwise and hold them constant until a growth equilibrium state is reached. (2.) deactivate growth and remove the loads stepwise to determine the residually stressed state. due to growth, the obtained geometry differs from the initial reference configuration. (3.) save this grown, unloaded configuration by storing the nodal coordinates as well as the fiber orientation vectors and the residual cauchy stress σres := (detf )−1fsf t at the integration points. (4.) use the saved nodal coordinates and fiber orientation vectors to define a new boundary value problem with boundary conditions that allow for the expected deformation. (5.) restore σres at each integration point and keep it throughout the following calculation. (6.) apply the residual stresses internally by updating the stress tensor according to s ← s + floadsres, where fload is a load factor ranging from 0 to 1, while growth is deactivated. in each step, the stress sres = det[f ]f−1σresf −t has to be computed corresponding to the actual deformation state. following this procedure, the wanted deformation state will arise in absence of external loads. 3. numerical example in a previous comparative study [15], an arterial segment with internal pressure and an axial displacement of 15% of the initial length was considered for a comparison of two different forms of the growth tensor and two different driving forces. each of the approaches was able to provoke growth-induced circumferential stress smoothening, but the approach presented in subsection 2.1 turned out to be the most effective, generating the most beneficial stress distributions at the lowest growth requirement, measured by the determinant of the growth tensor. therefore, a similar boundary value problem making use of this approach will be analyzed here in more detail, focussing in particular on the simulation of the opening artery. the half of a one-layered idealized arterial segment, reinforced by two fiber families arranged with angles of ± 30◦ with respect to the circumferential direction, is exposed to an internal pressure of 16 kpa (120mmhg). as an approximation of the natural conditions in the c1 [kpa] ε1 [kpa] ε2 [-] α1 [kpa] α2 [-] 17.5 499.8 2.4 30 001.9 5.1 table 1. material parameters for arterial tissue, adjusted by brands et al. [16] to the model from [9]. ϑ+ [-] k+ ϑ [-] m+ ϑ [-] ϑ− [-] k− ϑ [-] m− ϑ [-] 1.1 1.0 3.0 0.9 1.0 3.0 table 2. growth parameters used for the simulation of an idealized arterial segment. body, an axial displacement is additionally applied and three different values, namely 10%, 15% and 20% of the initial length, are compared. the material and growth parameters are chosen as given in tables 1 and 2, respectively. the load is applied within 1 s and subsequently held constant until t = 12 s, letting the arterial segment grow. in figure 2, the resulting stress distributions (solid lines) are shown and compared with the stress distributions obtained without including growth (dashed lines). for each value of axial strain, the circumferential stress distribution is significantly smoothened, which reduces the stress peak at the inner surface. the axial stress distributions are smoothened as well and moreover, a distinct stress reduction can be observed which is a consequence of the axial component of growth, compensating the axial deformation. the final axial stress level differs strongly in dependence on the axial displacement: the higher the axial displacement, the higher the axial stresses. examining the growth deformation in terms of the determinant of the growth tensor, depicted in the contour plots in figure 2, it can be observed that the volume change due to growth increases slightly with increasing axial displacement, being nevertheless in the same range. removing the internal pressure while maintaining the axial displacement, the stress distributions given in figure 3 are obtained. being thus not free of external loads in the axial direction, there are non-zero axial stresses in the non-growing reference segments in this state. in the growing segments, non-zero circumferential and axial stresses occur, which are – despite the existence of the axial load – referred to as residual stresses in this contribution. showing circumferential tensile stresses at the outer surface, each of the considered arterial segments is expected to open after a radial cut. the axial stresses in the segments are positive as well, provoking an axial contraction when releasing the axial constraint. the deformations related to these operations are depicted in figure 4. depending on the axial displacement, different opening angles and maximal values of axial strain are obtained. with increasing axial displacement, the opening angle reduces and the axial contraction rises. in the opened segments, the circumferential stresses have vanished. 88 vol. 7/2017 modeling of anisotropic growth and residual stresses in arterial walls -20 0 20 40 60 80 100 120 140 160 180 radial position [mm] 6.5 7 7.5 (a) -20 0 20 40 60 80 100 120 140 160 180 radial position [mm] 6.5 7 7.5 (b) -20 0 20 40 60 80 100 120 140 160 180 radial position [mm] 6.5 7 7.5 (c) 1.34 1.36 1.38 det(fg) 1.33 1.4 radial stress [kpa] circumf. stress [kpa] axial stress [kpa] radial stress, no growth circumf. stress, no growth axial stress, no growth figure 2. radial, circumferential and axial stress distributions as well as growth deformation at t = 12 s in an arterial segment exposed to an internal pressure of 16 kpa and different axial displacements of (a) 10 %, (b) 15 % and (c) 20 % of the initial length. the dashed lines indicate the stresses of a non-growing arterial segment. ra d ia l s tr e s s [ k p a ] -5 -4 -3 -2 -1 0 1 2 3 4 5 radial position [mm] 6.5 7 7.5 (a) c ir c u m f. s tr e s s [ k p a ] -2.5 -2 -1.5 -1 -0.5 0 0.5 1 1.5 2 2.5 radial position [mm] 6.5 7 7.5 (b) a x ia l s tr e s s [ k p a ] -10 -5 0 5 10 15 20 25 30 35 radial position [mm] 6.5 7 7.5 (c) uz = 0.10 l uz = 0.15 l uz = 0.20 l uz = 0.10 l, no growth uz = 0.15 l, no growth uz = 0.20 l, no growth ra di al ci rc um f. ax ia l figure 3. residual stresses in (a) radial and (b) circumferential direction, as well as (c) stresses in axial direction at t = 12 s after removing the internal pressure while keeping up the axial displacement. the stress distributions provoke the axial contraction and opening of a resected, radially sliced arterial segment as it is observed in experiments. (a) (b) (c) -0.5 -0.2 0 0.2 0.5 circumf. stress [kpa] -0.59 0.61 ϕ = 11.06◦ max εz = −1.24 % ϕ = 9.77◦ max εz = −4.63 % ϕ = 8.36◦ max εz = −8.00 % figure 4. deformation states associated to the residual stresses in arterial segments loaded by an internal pressure and axial displacements of (a) 10 %, (b) 15 % and (c) 20 % of the initial length. the wireframe shows the undeformed reference configuration, whereas the second chart form the inside shows the grown state after removal of the pressure. the indicated values of axial strain have been computed with respect to that deformed configuration. 89 anna zahn, daniel balzani acta polytechnica ctu proceedings 4. discussion and conclusion generating favorable results in specific cases as seen in section 3, the performance of the presented model is still strongly dependent on the boundary value problem, especially on the choice of the fiber orientation vectors and on the boundary conditions. the approximation of realistic conditions is difficult for both issues. subjected to remodeling processes, fibers in arterial tissue reorient according to the requirements of their mechanobiological environment. this effect of improving the load-bearing behavior is not included in the current framework so far, such that remodeling caused changes of the growth-inducing stresses and their consequences on growth can not be considered. therefore, the interaction between growth and remodeling processes is a topic which should be taken into account to further improve the model. the axial boundary conditions assumed in this contribution are a vague approach to approximate the natural state of arteries in the body, where axial strains and stresses are existent. thus, one could also have decided to apply axial stresses instead, unknowing which is the best way to mimic the unmeasurable, real conditions. another point with respect to the axial direction shall be mentioned. in contrast to the circumferential direction, where unloading and slicing are two different operations, the compution af axial residual stresses is tricky and demands further meditation. to be able to simulate the contraction after resecting the artery, the applied axial displacement has not been removed in the presented numerical example when computing the “residually” stressed state. doing so, the requested release of the axial constraint could be performed in the modified boundary value problem. if indeed real residual stresses are the matter of interest, the axial loading has to be removed together with the internal pressure, which is only possible when applying an axial stress instead of a displacement. then, the arterial segment can already deform in axial direction during the unloading process, such that no further cutting, revealing the deformation associated to axial residual stresses, is possible afterwards. a third topic for further examinations is the development of a procedure to adjust the growth parameters, which have been chosen arbitrarily until now. acknowledgements the authors appreciate funding from dfg through the institutional strategy “the synergetic university” of tu dresden. references [1] t. matsumoto, k. hayashi. response of arterial wall to hypertension and residual stress. in k. hayashi, a. kamiya, k. ono (eds.), biomechanics. springer, 1996. [2] d. balzani, j. schröder, d. gross. simulation of discontinuous damage incorporating residual stresses in circumferentially overstretched atherosclerotic arteries. acta biomaterialia 2:609–618, 2006. doi:10.1016/j.actbio.2006.06.005. [3] h. weisbecker, d. m. pierce, g. a. holzapfel. a generalized prestressing algorithm for finite element simulations of preloaded geometries with application to the aorta. int j numer method biomed eng 30:857–872, 2014. doi:10.1002/cnm.2632. [4] j. schröder, s. brinkhues. a novel scheme for the approximation of residual stresses in arterial walls. archive of applied mechanics 84:881–898, 2014. doi:10.1007/s00419-014-0838-x. [5] j. schröder, m. von hoegen. an engineering tool to estimate eigenstresses in three-dimensional patientspecific arteries. comput methods appl mech engrg 306:364–381, 2016. doi:10.1016/j.cma.2016.03.020. [6] s. göktepe, o. j. abilez, e. kuhl. a generic approach towards finite growth with examples of athlete’s heart, cardiac dilation, and cardiac wall thickening. journal of the mechanics and physics of solids 58:1661–1680, 2010. doi:10.1016/j.jmps.2010.07.003. [7] p. sáez, e. peña, m. a. martínez, e. kuhl. computational modeling of hypertensive growth in the human carotid artery. computational mechanics 53:1183–1196, 2014. doi:10.1007/s00466-013-0959-z. [8] e. k. rodriguez, a. hoger, a. d. mcculloch. stress-dependent finite growth in soft elastic tissues. journal of biomechanics 27(4):455–467, 1994. doi:10.1016/0021-9290(94)90021-3. [9] d. balzani, p. neff, j. schröder, g. a. holzapfel. a polyconvex framework for soft biological tissues. adjustment to experimental data. int j solids struct 43:6052–6070, 2006. doi:10.1016/j.ijsolstr.2005.07.048. [10] e. kuhl. growing matter: a review of growth in living systems. j mech behav biomed mater 29:529–543, 2014. doi:10.1016/j.jmbbm.2013.10.009. [11] i. hariton, g. debotton, t. c. gasser, g. a. holzapfel. stress-driven collagen fiber remodeling in arterial walls. biomechanics and modeling in mechanobiology 6:163–175, 2007. doi:10.1007/s10237-006-0049-7. [12] s. fausten, d. balzani, j. schröder. an algorithmic scheme for the automated calculation of fiber orientations in arterial walls. computational mechanics 2016. doi:10.1007/s00466-016-1321-z. [13] v. a. lubarda, a. hoger. on the mechanics of solids with a growing mass. int j solids struct 39:4627–4664, 2002. doi:10.1016/s0020-7683(02)00352-9. [14] e. kuhl, r. maas, g. himpel, a. menzel. computational modeling of arterial wall growth. biomechanics and modeling in mechanobiology 6:321–331, 2007. doi:10.1007/s10237-006-0062-x. [15] a. zahn, d. balzani. modeling residual stresses in arterial walls based on anisotropic growth. proceedings in applied mathematics and mechanics 16:115–116, 2016. doi:10.1002/pamm.201610046. [16] d. brands, a. klawonn, o. rheinbach, j. schröder. modelling and convergence in arterial wall simulations using a parallel feti solution strategy. computer methods in biomechanics and biomedical engineering 11:569–583, 2008. doi:10.1080/10255840801949801. 90 http://dx.doi.org/10.1016/j.actbio.2006.06.005 http://dx.doi.org/10.1002/cnm.2632 http://dx.doi.org/10.1007/s00419-014-0838-x http://dx.doi.org/10.1016/j.cma.2016.03.020 http://dx.doi.org/10.1016/j.jmps.2010.07.003 http://dx.doi.org/10.1007/s00466-013-0959-z http://dx.doi.org/10.1016/0021-9290(94)90021-3 http://dx.doi.org/10.1016/j.ijsolstr.2005.07.048 http://dx.doi.org/10.1016/j.jmbbm.2013.10.009 http://dx.doi.org/10.1007/s10237-006-0049-7 http://dx.doi.org/10.1007/s00466-016-1321-z http://dx.doi.org/10.1016/s0020-7683(02)00352-9 http://dx.doi.org/10.1007/s10237-006-0062-x http://dx.doi.org/10.1002/pamm.201610046 http://dx.doi.org/10.1080/10255840801949801 acta polytechnica ctu proceedings 7:85–90, 2017 1 introduction 2 computational framework 2.1 model of anisotropic growth related to two fiber families 2.2 visualization of residual stresses 3 numerical example 4 discussion and conclusion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.12.0001 acta polytechnica ctu proceedings 12:1–4, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app an issue of intelligent road transport in kazakhstan kairatolla k. abishev∗, ruslan b. mukanov, asylbek zh. kasenov, almagul n. baltabekova s.toraighyrov pavlodar state university, pavlodar city, republic of kazakhstan ∗ corresponding author: kairatolla76@gmail.com abstract. the article reviewed the road transport sector of the republic of kazakhstan and found a significant role in ensuring road transport of freight and passengers. shown needs to improve the work of transport-communication complex of the republic of kazakhstan on the basis of using the latest information and communication technologies. described advantages of realization of several intellectual transport technologies. presented modern level of using satellite navigational systems on the automobiles, in addition written some automation and informational aspects of controlling transport processes. also presented measures to solve technological rearmament problem of the republic of kazakhstan. keywords: the republic of kazakhstan, automobile transport, intelligent transport systems, dispatching system. 1. introduction the republic of kazakhstan is entering a new phase in the reform of its economy, defining the purpose a significant increase in the efficiency of the national development system. message from the president of the republic of kazakhstan n.a. nazarbayev to the people has become a new strategic project on the path of accelerated development of the national economy, in close collaboration with the world of the global economy. presenting in his letter deeply thoughtful and detail-calculated economic and social strategy for the further successful movement of the people of kazakhstan to the prosperity, peace and the achievement of higher goals, the president gave her the name of "nurly zhol – path to the future". this program is intended to be the growth engine of the national economy in the upcoming years to improve the welfare and quality of life of every citizen in kazakhstan. according to the president, the most important area for the development of kazakhstan’s is the transport and logistics infrastructure. improving the transport sector is more than urgent for kazakhstan in conditions when there is a problem of intensification of trade and economic cooperation with europe and east asia. the introduction of intelligent transport systems will facilitate the organization of international transport, cargo tracking, and reduce the time of delivery, provide high performance and security of transport and logistics processes. 2. main part transport plays the most important role in the republic of kazakhstan life. on one hand, it is a very big territory (2725 thousand. km2), low density of its population (an average of about 6 people / km2), very big distances between sources of raw materials and production resources. in this situation, transport and communication complex provide not only the economic but also the political integrity of the country. on the other hand, the geographical location in the heart of the eurasian continent, far from the main labor and capital markets result in the inevitable growth of the transport component in the export-import operations.it consequently leads to a weak integration into the global economic system. the geopolitical location of kazakhstan between the capacious and dynamically developing markets of europe, east and south-east asia provides a chance to compensate this, by bringing transcontinental transit on the territory of the country[1]. 2.1. the road transport role in the common transport complex of the republic of kazakhstan as we can see the world and now the domestic experience, road transport is maximally adapted to function in today’s world. automobile transport is an inseparable and a very important component of transport significant role in transport and communication complex of the republic of kazakhstan. among its most important, the following characteristics can be outlined: a. popularity and wide availability, b. high maneuverability and speed of passenger transportation and goods delivery, c. possibility of door-to-door delivery without the necessity of any additional interim operations with goods, 1 http://dx.doi.org/10.14311/app.2017.12.0001 http://ojs.cvut.cz/ojs/index.php/app k.k.abishev, r.b.mukanov, a.zh.kasenov, a.n.baltabekova acta polytechnica ctu proceedings d. providing of near to zero-option short-distance service (delivery within the city and to the suburbs, and also those in rural areas), e. high degree of adaptation to different technological processes – both in industry and service sector, f. relatively low capital capacity. given the conditions mentioned above, the automobile transport is considered an inseparable component of all modern transport technologies including the integrated and multimodal transportation. the goods transportation activity in the republic of kazakhstan follow increasing trends in terms of capacity of delivered goods. according to rok statistics agency [2], 3 627,9 million tons of goods have been shipped via transport networks of the republic of kazakhstan from january to december in 2014, which is 3.7% more than within the same period in 2013. the cargo turnover for the given period was evaluated as equal to 487.4 billion t/km, 21293,00 billion pf passengers have been transported (which is 6.5% more than during january-december 2013), passenger turnover was 249,6 billion t/km (increase per 6.8% compared to 2013). according to the agency data, the proportion of automobile transport in relation to both transportation volumes and goods turnover has been increasing each year. currently, the automobile segment occupies 86,23% from total amount of delivered goods, 7,54% belong to railway transport and 6.09% – to pipelines, and 0.14% – to the other means of transport (air, internal water transport) – see figure1. figure 1. distribution of total transportation volumes among the means of transportation. as shown by international and domestic experience, automobile transport is ultimately adapted to be functioning in the conditions of market demand and supply. it can be proved by the fact that transport and communication complex was the primary choice for realization of privatization[3]. 2.2. necessary improvement for transport and communication complex of the republic of kazakhstan at this level of social development, there is a need for technological improvement of the transport process caused by a number of additional factors. first of all, the increased density of vehicular traffic as a result of development of economic and cultural ties and the accompanying increase in the process of trade flows and mobility. in these conditions, for this time the intensification of all areas of human activity is becoming increasingly important factor of time and therefore introduces the task to improve traffic speed. meanwhile, the transport infrastructure capabilities tend to lag behind the need to provide quality transportation in the face of increased intensity and speed. this often leads to the occurrence of accidents involving property damage, injuries and deaths. the traffic growth creates many problems for instance, traffic control, associated with the need to make responsible decisions in conditions of high traffic density of vehicles that often becomes one of the causes of accidents caused by human error. from this perspective, the technological improvement of the transport process is essential and urgent in order to achieve goals for the society improving the safety of vehicles[4]. thus, the introduction of modern information and communication technologies in transport significantly reduces the influence of the human factor[5][6]. 2.3. intelligent transport systems in the republic of kazakhstan intelligent transport systems – this is the system integration of modern information and communication technology and automation with transport infrastructure, vehicles and users, focused on safety improvment and efficiency of the transport process, comfort for operators, drivers and transport users. the introduction of intelligent technologies in the transport sector of kazakhstan made in the individual modes of transport and aimed at solving corporate problems. realization of certain intelligent transport technologies, and finally the formation of intelligent transport systems both have social and economic objectives, they are: a. traffic safety improvement and, as a consequence, the reduction of social wastes in the transport sector b. reduction in transport costs in the economy and other spheres of transport services, c. improvement of the environment and saving human and material (f.e. energy) resources. the strategic aim of the creation of intelligent system of road transport is the creation in the city: republics of interconnected intelligent systems that control traffic of transport vehicles and special emergency services, housing management. the strategic goal can also determine the formation of the republic competitive "road corridors", equipped with priority its technologies: movement controlling systems, traffic management systems that provide 2 vol. 12/2017 an issue of intelligent road transport in kazakhstan figure 2. ansdu work scheme, based on the satellite navigation. driver information about road surface, traffic conditions, the recommended routes of driving in the real situations on the roads, the availability and location road service areas, roadside services and other[5]. one of the main directions of development of transport technologies in the passenger transport sector of the republic of kazakhstan is the introduction of computer-based navigation systems of dispatching management. these systems use the location of vehicles with the signals of global navigation systems gps and glonass. dispatching system based on satellite navigation systems allow operational management of transportation, fixing transport work by the transmission and processing of information about the location of vehicles, access to that information for all interested participants of the transport process. schematic diagram of the operation of the automated dispatch control navigation systems based on satellite navigation is shown in figure2. installation of navigation systems on public passenger transport are focused not so much on the movement of the vehicle itself, but rather on comfort and safety of passengers[7]. 3. conclusion the need of the introduction of modern innovative technologies in all parts of the economy is one of the circumstances to improve its efficiency in the republic of kazakhstan. it is fully recognized by the government at the highest level and has repeatedly emphasized on public statements of the president of republic of kazakhstan. as for technological modernization of the transport industry of the republic of kazakhstan, the following tasks should be solved: (1.) formation of a single information space, (2.) training of qualified personnel to work in the new technological environment, (3.) the formation of regulatory and legal framework, standardization and harmonization of requirements for technical solutions in the field of information support of transport activities. solving these problems is very important to improve the operation of transport. references [1] m. bekmagambetov, r. zhumagulov. the transport system of kazakhstan in modern conditions. almaty, 2008. [2] http://www.stat.gov.kz, last accessed may 2016. [3] k. k. abishev, r. b. mukanov. improving road traffic safety in the republic of kazakhstan (rok). driver-car interaction and safety 2014, pg. 43-46. [4] m. novák, z. votruba, m. svítek, p. bouchner. improvement of bus and truck driving safety. (2007) conference proceedings – ieee international conference on systems, man and cybernetics, 1, art. no. 4273847, pp. 310-315. 3 http://www.stat.gov.kz k.k.abishev, r.b.mukanov, a.zh.kasenov, a.n.baltabekova acta polytechnica ctu proceedings [5] m. m. bekmagambetov. intelligent transport systems in the republic of kazakhstan. almaty, 2013. [6] p. bouchner, j. faber, m. novák, et al. human decision aspects in interactions with artificial systems. (2009) proceedings of the 2009 euro american conference on telematics and information systems: new opportunities to increase digital citizenship, eatis ’09, art. no. 1551749. [7] v. m. vlasov. transport telematics in the road sector. moscow-madi, 2013. 4 acta polytechnica ctu proceedings 12:1–4, 2017 1 introduction 2 main part 2.1 the road transport role in the common transport complex of the republic of kazakhstan 2.2 necessary improvement for transport and communication complex of the republic of kazakhstan 2.3 intelligent transport systems in the republic of kazakhstan 3 conclusion references acta polytechnica ctu proceedings doi:10.14311/app.2017.11.0022 acta polytechnica ctu proceedings 11:22–30, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app comparative analysis of bearing capacity of reinforced and non-reinforced railway embankment josef jíra∗, jitka jírová, michal micka, jitka řezníčková department of mechanics and materials, faculty of transportation sciences, ctu in prague ∗ corresponding author: jira@fd.cvut.cz abstract. a comparative analysis using the programme ansys (fem) deals with the generation of the computation model and with the assessment of the influence of the geogrids and the vertical lime-cement columns on the bearing capacity and deformation of the railway embankment on the less load-bearing subsoil. the graphic outputs give an overview of the field layout of equivalent stresses and deformation in the construction of the railway substructure. keywords: computation model, geogrid, lime-cement columns, embankment, subsoil, bearing capacity, deformation, equivalent (von misses) stress. figure 1. reinforced geogrid tensar ss. 1. introduction in the case of railway earthworks is a measure of the reliability and safety of the bearing capacity of the substructure and permanent way with a guaranteed track geometry, there should not be an unexpected track depression or the settlement of an embankment etc. modernization of the existing railway routes to bear higher axle loads requires an increase in bearing capacity of the subgrade system. one possibility to increase the bearing capacity of a railway body is to introduce geogrids, see figure 1 and 2. vertical or inclined lime-cement columns are also used for increasing bearing capacity of the subsoil [1, 2]. by using the geogrid we can avoid the problems connected with the conventional way of extracting earth in subsoil and its substitute with loose earth of good quality. the geogrids are typical of open structures where the surface of the holes covers more than 40% of the total area. the reinforcing function of the geogrids lies in using the membrane effect, i.e. the forces in the area of the reinforcement, which have a favourable effect on tensile stresses in the soil construction. tensar company’s extensive experience with the modernization of the european railway corridors are figure 2. reinforced geogrid tensar ss. fully and very effectively used in the railway construction in the czech republic. the geogrids tensar ss are widely used in the reconstruction of the existing rail network. effectiveness of tensar ss geogrids was confirmed by a number of independent surveys, which conditions of non-reinforced and reinforced layer were simulated. structural benefit of tensar geogrids ss is to reinforce the unbound layers of railroad tracks. granular material piled and compacted over the geogrid openings penetrating through the geogrid, so grains of soil and the geogrid fit together and creates the effect of mutual gearing between grains of soil and the geogrid. the geogrid tensar ss creates composite together with a material bed foundation, which is effective even on the underlying ground consisting of peat or soft silt and restricts horizontal movement of the material in the ballast and minimizing the penetration of fine particles from the subsoil. the lime-cement columns are applied in the case of building with less bearable subsoil, see figure 3 and 4. their task is to help in the absorption of loads, to improve the overall mechanical properties and thus to prevent future unwanted displacements of foundation and other building complications. there 22 http://dx.doi.org/10.14311/app.2017.11.0022 http://ojs.cvut.cz/ojs/index.php/app vol. 11/2017 comparative analysis of bearing capacity figure 3. vertical lime-cement columns – technology colmix [3]. are vertical or inclined columns which they are oblique to the horizontal plane at an acute angle. length the columns prevails over other dimensions. the manufacturing process of columns can be of two types – wet and dry process. the wet process is mixing soil with cement suspension – suspension is prepared in a central mixing pump is conveyed to the mixingdrilling tools. lime, ash or gypsum is used in the dry method. jet grouting is another suitable method for increasing the bearing capacity of foundation soil. the method enables also besides the creation of larger diameter columns takes small diameter drilling, which is suitable for use on construction sites are cramped conditions. the application range of lime-cement columns is large, covers an area of clay with very small grains after gravels with relatively large grains. colmix patented technology belongs to the group deep soil mixing (dsm). it is suitable for the stabilization of road and railway embankments and removing unwanted traffic settlement structures in low stringency (clay) soils. on the site, which is intended to stabilize, it is necessary to perform in situ analysis of soil (analysis in the field) and the result of the strength requirements and the pilots to determine the composition of the binder mixture. in case colmix may be used the mortar with possibility to change the cement components and calcium hydroxide (or these components may be used separately). to embed the pile to land need special equipment drill soil that is mixed with the binder mixture and form it after finishing a compact mass in the shape of a column. interaction figure 4. vertical lime-cement columns – technology colmix [3]. of the columns and the surrounding soil occurs when loading to improve geotechnical properties. examination of the bearing capacity or stability of such adjusted constructions is usually verified in an experimental way. experience from abroad shows that it is necessary to monitor the railway embankment settlement in the case of a non-bearing subsoil [4, 5], even if the embankment is reinforced. therefore various experimental models are also used to study the influence of ballast bed construction on the bearing capacity and to test the reinforcing effect of the geogrids and columns. it can be also solved by numerical methods [3, 6], mostly by the fem (finite element method). the aim of this work was to verify the numerical modelling of behaviour of a railway embankment reinforced by geogrids and lime-cement columns when using the ansys programme. on the model of a simple ground body the process of model creation, choice of definite elements, definition of material features, and application of contact elements, definition of marginal conditions and load and setting the parameters of computation were verified. the computation models of the reinforced and non-reinforced railway embankment were used for the comparative analysis of the bearing capacity and deformation. 23 j. jíra, j. jírová, m. micka, j. řezníčková acta polytechnica ctu proceedings figure 5. the scheme of layers in the model of reinforced earthworks. 2. computation model of reinforced embankment 2.1. geometric model the finite-element method (fem) has been successfully used to assess the performance of geosynthetics and lime-cement columns in the strengthening of soft soils. geometric models were created for all cases in the workbench design modeller. a suitable model railway body was a need to establish for numerical calculations. the railway body in the embankment was selected for representing computational model; the scheme is compiled in figure 5. creating this body carried out in accordance with czech regulations and railway literature [7]. as part of the superstructure we modelled the concrete sleepers and a gravel ballast bed. the substructure includes the embankment of impervious soil, a geogrid and columns (both for the cases where the calculated mechanical phenomena were analysed in the reinforced rail track in the case of the non-reinforced railway body is not in it). two layers of cohesive soils having unfavourable properties were used in the base of the computational model in figures 5 and 6. they also interfere with columns, in the case of the reinforced model in figure 6. the aim of this research was to develop a spatial model. it is therefore necessary to attach the crosssection a third dimension so as to be solved the problem in 3d. for all layers of reinforced and unreinforced models (i.e. a ballast bed, an embankment, a geogrid, the first layer and the second layer of subgrade soil) was chosen length of the computational model 5, 139 m. this value is needed for entering symmetric boundary conditions of the program ansys – the front and rear wall of the space model of the railway body. the axial distance between sleepers is 0, 600 m in the ballast bed. spatial spacing columns is a parameter chosen as a variable, depending on the analysis performed. figure 6. the model of the embankment with a geogrid and lime-cement columns. 2.2. modelling soil for modelling the properties of the embankment and subsoil material the classic dp model – drucker prager for geological materials is used. the material inputs are: modulus of elasticity e, poisson’s ratio µ, density ρ, angel of internal friction φ and cohesion c. therefore the computation is materially non-linear. this model is used most often and provides good results. the disadvantage of it is that it does not involve the possibility to express hysteresis curve for repeated load. on the contrary the advantage is that we can use tabular material standard values according to specification of soils used. in ansys two more material models for geological material of plasticity can be used. the edp model – extended drucker prager – takes into account the reinforcement of the material within the loading process. the edp cap model supplements the edp model with the conditions of plasticity for volume pressure and tension. the models are sensitive to proper specification of input parameters and can only be gained from laboratory tests for given material. if the material constants are for the study purposes used to convey behaviour of the soil close to the dp model, i.e. for consolidated soil, the results in transformation of the soil construction are very similar. in all cases under investigation, we use of concrete sleepers, the ballast bed was with well grained gravel, the embankment contained gravel mixed with finegrained soils and subsoil contained clays. material composition of the bottom structure (figure 5 and table 1) was considered with different material properties for the model type 1 and for the model type 2 in the calculation, i.e., that the material substructure was calculated with lower or higher modulus of elasticity (see the value in the bracket) for clay f4 and f6. also the lime-cement columns were considered for lower quality soil substructure with the value of the modulus of elasticity of 26 mpa or 60 mpa (model type 2) for higher quality of soil. 24 vol. 11/2017 comparative analysis of bearing capacity material modulus of elasticity e [mpa] poisson’s ratio µ [ ] density ρ [kg/m3] angle of internal friction φ [ °] cohesion c [mpa] geogrid 450 gravel 0/32 55 0.3 1950 30 0 gravel 32/50 100 0.35 2000 36 0 clay f4 80 (90) 0.35 1850 25 0.015 clay f6 50 (60) 0.4 1750 19 0.016 columns 26 (60) 0.3 1750 25 0 table 1. material properties of each layer of the model type 1 and (type 2). figure 7. the concrete sleeper [mm]. material characteristics of the concrete sleeper in figure 7 are: density ρ = 2500 kg/m3, e = 20000 mpa, poisson’s ratio µ = 0, 2. 2.3. fem model the model of the railway body and performed calculations were carried out using the finite element method (fem) – ansys software in version 12.1. finite element network was created automated methods in workbench. parametric studies were performed in the module ansys – workbench 14 too. all structures in the rail track in the ansys program were modelled as volumes. those will then assign material properties. it is a convenient way of considering the relatively fine particles in soils. geometrically soils are made up of prismatic volumes; volume sleepers have a specific shape and the columns are introduced as cylindrical volumes. the reinforcement of the geogrid tensar ss is modelled as a thin plate of constant thickness which is mostly stressed by normal tensile forces and the bending stiffness is insignificant. the geogrid tensar ss30 type (figure 8 and table 2) was used for the comparative analysis of bearing capacity. contact surfaces were formed at the interface between the volumes. their number depends on the structural complexity of the model. other values have e.g. the model with the geogrid and columns and other are for models without one of these reinforcing elements. contact elements of the "bonded" were used figure 8. shape and sizes of geogrid tensar ss30. size value [mm] size value [mm] al 39 tj 5.0 at 39 tlr 2.2 wlr 2.3 tt r 1.3 wt r 2.8 table 2. sizes of geogrid tensar ss30. in all cases. using these contact elements prevents shearing at the contact surfaces and cannot lead to separation of two volumes. 3. analysis of behaviour of reinforced and non-reinforced embankment the verification of the computational model was done by parametric studies for four configuration model: 25 j. jíra, j. jírová, m. micka, j. řezníčková acta polytechnica ctu proceedings (i) the embankment without reinforcement, (ii) the embankment with the geogrid, (iii) the embankment with the geogrid and the lime-cement columns and (iv) the embankment with the geogrid and the lime-cement columns sheathed the geogrid. the parametric study was conducted for the columns of diameter d = 0, 6 m which had longitudinal and transverse distance of 1, 65 m. the load was applied to the spatial computational model as the pressure on the area sleeper. this area has sizes 0, 204 m x 0, 401 m and settles on it the bottom rail. the axle load of the standard load train is 250 kn and the wheel force is equal to half of this value – 125 kn, which was taken to work. the position of the wheel between the two sleepers is considered, which results in half of the wheel force per sleeper. the wheel force once repeated over a distance 2, 284 m – there are considered two axles. the graphic outputs were carried out for above mentioned unreinforced and reinforced embankments and two types of material composition of the subgrade. for the total comparative analysis there are chosen graphic outputs: (i) equivalent (von misses) stress in the subgrade, (ii) tensile stress of geogrid in the embankment, (iii) total deformation of the embankment and the lime-cement columns. a number of parametric studies of non-reinforced and reinforced embankments were performed with different parameters, e.g. the equivalent stress (von mises) and vertical and horizontal stresses were analysed. from all figures it is possible to see that the reinforcement of the railway embankment has a favourable effect on the bearing capacity of the subgrade. the graphic outputs give a clear overview of the field layout of equivalent stresses and deformation in the construction of the railway substructure. the maximal equivalent stress (von misses) of the subgrade is 20% lower if the embankment is only reinforced by the geogrid, but it is 30% larger if the embankment is reinforced by the geogrid and columns. reinforcing embankment with vertical columns has a very positive effect on the tensile stresses in the membrane of a geogrid, because heads of the vertical columns serve as a distribution platform for loaded geogrid. this arrangement allows uniform load transfer from the upper to the subsoil. the maximal tensile stresses are in the geogrid 8% smaller and they are spread over a much smaller area. the total deformation of the superstructure (practically settlement) is lower about 2 mm if the embankment is reinforced by the geogrid and the columns sheathed a geogrid than for the non-reinforced embankment. a comparative analysis shows that the reinforcement of the embankment, especially columns is important mainly for poor soils in the railway embankment, i.e. for soils with poorer material characteristics and low bearing capacity. when the more qualitative soil is used for the construction of the embankment then the reinforcement of the geogrid is sufficient to improve the stiffness of the railway embankment too. the geogrid is able to be prestressed because of activation of the membrane effect. that is usually made manually and in the tensed position the geogrid is fixed with individual clasps or with a grid with spikes infixed into the subsoil. 4. conclusion the possibility of using the ansys programme for modelling the behaviour of earthworks with geogrids and vertical lime-cement columns was demonstrated. the bearing capacity of the railway earthworks has great importance for railway practise. the calculation using drucker-prager model of soil enables through a gradual increasing in loading in load steps attain the state of stress and deformation close to the limit state at which sliding areas and big displacements. the stiffness of the soil construction, which can be derived from the values of load and vertical displacements, is an important value. there are expected to improve useful properties of the embankment when the rail body is only reinforced by the geosynthetic grid. consideration when evaluating the results is focused on all variants unbearable subsoil. as for sleepers, so at ballast and embankment is taken for granted that they are able to periodically transmit the resulting rail loads. four basic configurations of the railway body were taken into account: • the embankment without reinforcement (labelled in figure 14 as e), • the embankment with the geogrid (e +g), • the embankment with the geogrid and the limecement columns (e +g+ c), • the embankment with the geogrid and the columns sheathed a geogrid (e +g+ sc). computational modelling has shown the usefulness of reinforcement of the embankment by geogrids and vertical lime-cement columns, which leads to a reduction of settlement and stress state of the soil layers within the rail body. it is assumed that a rail body reinforced columns exhibits greater resistance to loading. using vertical lime-cement columns is very significant for increasing bearing capacity of subsoil. the geogrids and the columns can be also used in the case of building a new railway. comparison of total deformation of the embankment for types with lower or higher values of the modulus of elasticity of the lime-cement columns showed much lower settlement values of the embankment reinforced by the geogrid and the columns with higher values of modulus of elasticity, if we compare two types of different moduli of elasticity of columns. decreasing the values of settlement is from 15% to 19% according to type of reinforcing of the embankment. 26 vol. 11/2017 comparative analysis of bearing capacity figure 9. total deformation of the non-reinforced embankment. figure 10. total deformation of the embankment reinforced by the geogrid. 27 j. jíra, j. jírová, m. micka, j. řezníčková acta polytechnica ctu proceedings figure 11. total deformation of the embankment reinforced by the geogrid and the columns. figure 12. total deformation of the embankment with the geogrid andthe columns sheathed a geogrid. 28 vol. 11/2017 comparative analysis of bearing capacity figure 13. stress field σx of the geogrid of the embankment reinforced by the geogrid and the columns sheathed a geogrid. figure 14. total deformation of the embankment for all four types of structure and for two types of subgrade with various modulus of elasticity. 29 j. jíra, j. jírová, m. micka, j. řezníčková acta polytechnica ctu proceedings acknowledgements this work has been supported by research plan msm6840770043. references [1] g. femandes, e. palmeira, r. gomes. performance of geosynthetic-reinforced alternative sub-ballast material in a railway track. geosynthetics international 15, 2008. [2] j. zheng, b. cheng, y. lu, et al. the performance of an embankment on soft ground reinforced with geosynthetics and pile walls. geosynthetics international 16, 2009. [3] j. pajkrt. space model of the part of the railway track with lime-cement columns. faculty of transportation sciences ctu, prague, 2011. [4] l.briancon, h.girard, d.poulain. slope stability of lining systems – experimental modeling of friction at geosynthetic interfaces. geotextiles and geomembranes 20, 2002. [5] r. holý, m. kalika, j. kaliková, et al. system for simultaneous object identification and sector indoor localization oidsil in. proceedings of 2014 international conference on intelligent green building and smart grid. piscataway: ieee operations center, 2014. isbn 978-1-4673-6123-1. [6] o. jiroušek, j. jíra, o. hrdlička, et al. numerical modelling of the reinforcing effect of geosynthetic material used in ballasted railway tracks. proc. imeche, part f: journal rail and rapid transit, 224 (f4), 2010. doi10.1243/09544097jrrt319. [7] track substructure s4, technical regulations. railway infrastructure administration, state organisation. 30 acta polytechnica ctu proceedings 11:22–30, 2017 1 introduction 2 computation model of reinforced embankment 2.1 geometric model 2.2 modelling soil 2.3 fem model 3 analysis of behaviour of reinforced and non-reinforced embankment 4 conclusion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2015.1.0057 acta polytechnica ctu proceedings 2:57–61, 2015 © czech technical university in prague, 2015 available online at http://ojs.cvut.cz/ojs/index.php/app on sampling based methods for the dubins traveling salesman problem with neighborhoods petr váňa∗, jan faigl dept. of computer science, czech technical university in prague, technická 2, 166 27 prague, czech republic ∗ corresponding author: vanapet1@fel.cvut.cz abstract. in this paper, we address the problem of path planning to visit a set of regions by dubins vehicle, which is also known as the dubins traveling salesman problem neighborhoods (dtspn). we propose a modification of the existing sampling-based approach to determine increasing number of samples per goal region and thus improve the solution quality if a more computational time is available. the proposed modification of the sampling-based algorithm has been compared with performance of existing approaches for the dtspn and results of the quality of the found solutions and the required computational time are presented in the paper. keywords: dubins vehicle, dubins maneuver, dtsp, dtspn. 1. introduction path planning for a non-holonomic vehicle is a fundamental problem of surveillance mission where an unmanned aerial vehicle (such as a fixed-wing) is requested to visit a given set of locations. the basic model of such a vehicle with the limited turning radius is called the dubins vehicle [1] for which the combinatorial problem of finding optimal sequence of visits to the locations is known as the dubins traveling salesman problem (dtsp) [2]. in this paper, we consider a generalized problem of the dtsp where the particular waypoints to be visited can be selected from a set of possible locations. due to the similarity of this problem with the so-called traveling salesman problem with neighborhoods [3], the problem is called as the dubins traveling salesman problem with neighborhoods (dtspn) [4]. the dtspn is a suitable problem formulation to address surveillance missions with unmanned aerial vehicles, where it is required to take a camera snapshot (or other type of measurement) of each target location. such a snapshot can be acquired from some distance of the target location and thus it is not necessary to visit the location exactly. it is rather a more suitable to select the waypoints in such a way that all locations are covered while the total cost of the final path is minimal. there are several approaches to address the dtsp and also the dtspn in the literature [2, 4–6] including our work [7]. therefore, in this paper, we provide an overview of the existing approaches to address the dtspn and compare their performance according to the trade-off between the solution quality and computational requirements. in particular, we focus on the sampling-based algorithm [4] which is able to provide high quality solutions for very high number of samples. however, more samples increase the computational burden, and therefore, the algorithm is not directly suitable for real-time applications. on the other hand, we can get a quick estimation of the solution quality using only few samples. this has motivated us to modify the original algorithm [4] to provide a first solution quickly that is then improved if a computational time is left. the paper is organized as follows. a brief introduction to the problem background is presented in the next section. the addressed problem is formally introduced in section 3. a brief overview of the existing approaches to solve the dtspn is provided in section 4. the proposed modification of the samplingbased approach is presented in section 5 together with the analysis of its computational complexity. evaluation results of the comparison of the existing approaches with the proposed modification are reported in section 6. finally concluding remarks are denoted to section 7. 2. related work the problem of curvature-constrained path planning has been studied years ago and the fundamental work has been published in 1957 by dubins. in [1], he proved that the optimal path between two configurations q1, q2 ∈ se(2) consists of only straight line segments and segments with the minimum turning radius. he also showed that only 6 maneuvers can be optimal, which can be further divided into two main types: • ccc type: lrl, rlr; • csc type: lsl, lsr, rsl, rsr; where c stands for a circle turn (r – right, l – left) and s for a straight segment. even though the optimal path for dubins vehicle between two configurations is known and it is straightforward to compute, this is not sufficient to directly solve the dtsp. it is because the orientation of the vehicle at the waypoints is not known and thus it must be determined together with the optimal sequence of 57 http://dx.doi.org/10.14311/app.2015.1.0057 http://ojs.cvut.cz/ojs/index.php/app petr váňa, jan faigl acta polytechnica ctu proceedings visits to the waypoints. moreover, the optimal orientation depends on the sequence and vice-versa, which make the problem difficult to address. probably the simplest approach to address the dtsp is the alternating algorithm (aa) proposed in [2]. in this approach, headings are established in the way that even edges are connected by straight line segments and odd edges are connected by dubins maneuvers. in addition, the authors show that the length of the optimal solution of the dtsp can be bounded by ltspκdn/2eπρ, where ρ is minimum turning radius, ltsp is the length of the optimal solution of the euclidean tsp, n is the number of the goals, and κ < 2.658. based on the similar idea, authors of [5] proposed a receding horizon algorithm called the look-ahead (la) approach. the heading is determined with respect to the next point in the sequence. this algorithm investigates each point only once, and therefore, the la approach is very fast and suitable for real-time application while the authors reported better results than the aa. the optimal solution of the dubins planning to visit a given sequence of waypoints that are at the distance longer than 4ρ is presented in [8]. the approach is based on the convex optimization; however, the optimization needs to be solved several times because of possible alternation of the maneuvers directions. the authors bound the number of possible combinations to 2n−2 for n waypoints. the dtspn is a generalization of the dtsp, where each goal is extended by a neighborhood (goal region). as the dtsp is known to be np-hard [6], also its generalization the dtspn is np-hard. 3. problem definition the addressed problem is motivated by surveillance missions with fixed-wing aerial vehicles, which are nonholonomic vehicles due to their kinodynamic constraints. these vehicles are often modeled as the dubins vehicle [1], which can go only forward at a constant speed and has a minimum turning radius ρ. the configuration space of such a vehicle can be represented as se(2), where each configuration q ∈ se(2) is a triplet (x, y, θ), where (x, y) is the vehicle position in a plane and θ ∈ s1 is the orientation of the vehicle. the mathematical model of the dubins vehicle can be formulated as follows: ẋ ẏ θ̇  = v  cos θ sin θ u ρ  , |u| ≤ 1, (1) where v is the vehicle forward velocity, ρ is the minimum turning radius, and u is the control input, u > 0. now, we can introduce the dtspn [9] a more formally. let r = {r1, . . . rn} be a set of n regions ri ⊂ r2 that are requested to be visited by the dubins vehicle and let σ = (σ1, . . . , σn) be an ordered permutation of {1, . . . , n}. we define a projection from se(2) to r2, i.e., p(q) = (x, y), and let qi be an element of se(2) whose projection lies in ri. the dtspn is path planning problem where the dubins vehicle has to visits each region ri while satisfying the kinodynamic constraints of (1). every optimal path has to intersect each goal region ri in at least one configuration qi. hence, we can treat the dtspn as an optimization problem over all possible permutations σ and configurations (q1, . . . , qn) as follows: problem 3.1 (dtspn). minimize σ,q l(qσn , qσ1) + n−1∑ i=1 l(qσi , qσi+1) subject to p(qi) ∈ ri, i = 1, . . . , n where l(qi, qj) is the dubins distance between qi and qj . in this paper, we are focused on the problem with regions ri that are mutually exclusive. hence, we can define the minimum distance constraint dk such that for all i, j ∈ {1, 2, . . . , n}, i 6= j,∀pi ∈ ri,∀pj ∈ rj : ||pi − pj || > kρ. (2) in particular, we are focused on the problem for which the minimum distance dk is equal to 4ρ, which is denoted as the d4 constraint in the rest of this paper. problem instances of the dtspn with the d4 constraint have special properties that are shown and used in [7] to find high quality solutions. in this paper, we also consider d4 problems and compare the existing solutions with the sampling based methods. an overview of the existing methods is provided in the next section. 4. existing methods in literature, we can find several different approaches to address the dtspn. the existing approaches can be divided into three main classes: 1) the decoupled methods; 2) sampling-based methods; 3) and evolutionary methods. representatives of each particular class are briefly described in the following subsections. 4.1. decoupled methods a decoupled method addresses the dtspn by decomposition of the problem into two sub-problems. first, the permutation of the visits to the requested areas (locations) is found independently on the dubins path planning. the second sub-problem is to find a particular visiting configuration of each location. in this way, the original dtspn is transformed to the dtsp with point locations to visit. in [10], the authors address the dtspn by solving the euclidean tsp where cities represents centers of the regions to be visited. once such a permutation is found, the final solution is constructed using the aa [2]. 58 vol. 2/2015 the dubins traveling salesman problem with neighborhoods authors of [7] also consider a solution the etsp to estimate the permutation of the visits. but instead of simple aa, the proposed local iterative optimization (lio) is used to find a significantly better solution. 4.2. sampling-based methods sampling-based methods [4, 11] are another class of existing approaches to address the dtspn. similarly to the decoupled methods, also sampling-based methods are based on existing approaches for the tsp variants; however, in this case a single representative of each region is not considered as in [10] but each region is rather sampled by a particular number of random samples (including the orientation of the vehicle). the samples can be determined in the whole region or only on its boundary. then, the samples of different regions are connected by the dubins maneuver to form a roadmap. such a roadmap is considered as an instance of the generalized asymmetric tsp (gatsp). if the gatsp is solved to the optimum, the sampling-based methods are resolution complete [11]. since the optimal solution of the gatsp can be computationally very demanding, existing heuristic for the tsp can be a more suitable option. the generated gatsp can be solved by its transformation to the asymmetric tsp (atsp) using the noon-bean transformation [12]. then, the transformed atsp can be solved by existing algorithms, e.g., the linkernighan heuristic algorithm [13]. 4.3. evolutionary methods the last class of existing approaches are genetic programming based algorithms. the general idea of these methods is to encode a solution by a chromosome in which the goal permutation and the configurations of the visits are stored. similarly to another approaches, only configurations on the boundary of the regions are considered in these evolutionary methods. probably the first evolutionary approach to the dtspn was published in [14]. the authors adapted the ordered crossover operator (ox) and added two new mutation operators (orientation shift and position shift) to optimize visiting configurations. relatively recently, the genetic approach from [14] was modified into a memetic algorithm in [15]. the authors used similar operators and added a local improvement of individuals in the population by optimizing the position of visiting points. the authors used aa as heuristic algorithm to speed up the algorithm. 5. modification of existing sampling-based algorithm the main issue of sampling based algorithms for the dtspn is that they require a fixed number of samples, which need to be established in advance. we propose an iterative schema to avoid this issue and set the number of samples progressively, which provides first solutions very quickly. moreover, if there is some additional computational time, the algorithm can iteratively improve the solution by adding more samples, which results to obtain a first solution quickly that is further improved. in the basic sampling-based algorithm, a roadmap with (n ·m)2 edges is created where n is the number of regions to be visited and m is the number of samples per region. for each edge one dubins maneuver is constructed. since the noon-been transformation does not change the number of vertices, the overall time complexity of generating an instance of the atsp can be bounded by o((n ·m)2). a solution of the generated atsp can be found by the available lkh solver. according to the author of the lkh, the time complexity of the lkh is approximately o(n2.2 atsp ) [16]. hence, the expected total time complexity is o((n ·m)2.2). the time complexity to solve the atsp is greater than a roadmap generation, and therefore, we do not need to explicitly consider the construction of the roadmap in the estimation of the required computational time based on the number of samples. based on the relation of the required number of operations on the number of samples, we can establish a sequence of the increasing numbers of the samples needed to find an initial solution quickly and improve its quality later. the sampling-based algorithm works with the constant number of samples given a priory, we can run the sampling based algorithm repeatedly with an increasing number of samples. since the time complexity of the algorithm is nearly quadratic, an inverse function for the number of samples mk according to the number k of the particular iteration can be defined as: mk ≈ √ 2k. (3) after rounding the mk to an integer value, it gives us the following series of the numbers: m = {1, 2, 3, 4, 6, 8, 11, 16, 23, 32, 45, 64, . . .}. (4) figure 1 provides influence of the required computanumber of samples per region 0 100 200 300 400 500 600 700 800 t im e [s ] 10 -2 10 -1 10 0 10 1 10 2 10 3 etsp + lio sample + atsp figure 1. the average required computational time (from 20 trials) for the instance of the dtspn with 4 circle regions and d4 constraint. tional time on the number of samples per each region 59 petr váňa, jan faigl acta polytechnica ctu proceedings to visit. we plot the required computational time on the number of samples per each region to visit. in this case, a simple problem with 4 regions and d4 constraint is considered and the computational time is compared with the etsp+lio algorithm proposed in [7]. 6. results the performance of the proposed modification of the sampling based algorithm has been evaluated in a series of scenarios. the evaluated instances of the dtspn were generated randomly for convex regions satisfying the d4 constraint. several shapes of the regions have been considered: points, disks with the radius equal to ρ, ellipses with the semi-axis 2ρ and 0.5ρ, and convex polygons with up to 6 vertices created from a circle with the radius ρ. a relatively high and uniform density of the regions for the d4 constraint has been considered by generating centers of the regions inside a bounding box with the side 6 √ nρ, where n is the number of the regions to be visited by the dubins vehicles. an example of the examined problems is depicted in figure 2. (a) . d4 convex regions (b) . d1 convex regions figure 2. examples of the randomly generated instances of the dtspn. the examined algorithms are denoted as follows. the newly proposed modification of the samplingbased algorithm is denoted sample+atsp. the algorithm is compared it with the evolutionary approaches [14] and [15] denoted as genetic and memetic, respectively. in addition, we implemented three variants of the decoupled approach based on the solution of the etsp utilized as the heuristic estimation of the permutation of the visits to the regions. the first decoupled approach is denoted as etspn+aa and it is based on the alternating algorithm (aa) [2]. the second method is denoted as the etsp+lio [7] and is based on local optimization of position and heading of the waypoints. the last method is derived from the etsp+lio, but only local iterative optimization of the heading is considered, this method is denoted as the etspn+holio. the quality of found solutions has been evaluated regarding a dedicated computational time for problems with n = 20 and n = 40 regions with the d4 constraint. the quality is measured as the ratio of the path length found by the particular algorithm to the solution provided by the etsp+lio algorithm, similarly as in [7]. all instances were generated randomly, and therefore, 50 trials have been solved for each problem and the algorithm variants. the achieved results are depicted in figure 3 for the 20 regions and in figure 4 for the 40 goal regions. time [s] 10 -2 10 -1 10 0 10 1 10 2 r el at iv e le n g th o f th e so lu ti o n 1 1.1 1.2 1.3 1.4 1.5 etsp + lio etspn + holio etspn + aa memetic genetic sample + atsp figure 3. average ratio of the tour length (from 50 trials) according to the etsp+lio solution for the dtspn with n=20 convex regions. plots start from the time when the first solution is available. time [s] 10 -2 10 -1 10 0 10 1 10 2 r el at iv e le n g th o f th e so lu ti o n 1 1.1 1.2 1.3 1.4 1.5 etsp + lio etspn + holio etspn + aa memetic genetic sample + atsp figure 4. average ratio of the tour length (from 50 trials) according to the etsp+lio solution for the dtspn with n=40 convex regions. plots start from the time when the first solution is available. all the algorithms have been implemented in c++ and tested on a single core of the intel core i5-m480 cpu running at 2.67 ghz. the processor was accompanied with 4 gb ram. 6.1. discussion the presented results show that the proposed modification of the sampling-based algorithm can be considered as a meaningful alternative to the evolutionary based algorithms. in the case of the high number of regions to visit (n = 40), the modified samplingbased algorithm has even superior results to the both genetic and memetic algorithms, while it is less computationally demanding. in the results depicted in figures 3 and 4, the etsp+lio algorithm achieved the best results among 60 vol. 2/2015 the dubins traveling salesman problem with neighborhoods the evaluated algorithms. this is caused by the fact, that all instances of the dtspn were generated with non-overlapping regions with the d4 constraint and the etsp+lio has been designed on top of the properties of the optimal solution of such a problem and thus it directly searches for good solutions [7]. 7. conclusions in this paper, we proposed a modification of the sampling-based algorithm for the dtspn. the proposed algorithm repeatably executes the original sampling-based algorithm with an increasing number of the samples per each region. by this modification, the newly developed algorithm provides the first solution very quickly that can be further improve if more time is available. this makes the algorithm suitable in situations where a solution has to be found quickly and where the maximum time that can be dedicated for the computation is not known in advance. we also compared the modified algorithm with other existing approaches on the randomly generated instances of the dtspn with the d4 constraint. the modified algorithm provides better results than the implemented evolutionary algorithms while it is less computationally demanding. a further comparison of the algorithms’ performance in the instances of the dtspn where regions to visit are closer or overlapping is a subject of our future work. acknowledgements the presented work has been supported by the czech science foundation (gačr) under research project no. gp13-18316p. references [1] l. e. dubins. on curves of minimal length with a constraint on average curvature, and with prescribed initial and terminal positions and tangents. american journal of mathematics pp. 497–516, 1957. doi:10.2307/2372560. [2] k. savla, e. frazzoli, f. bullo. on the point-to-point and traveling salesperson problems for dubins’ vehicle. in proceedings of the american control conference, pp. 786–791. ieee, 2005. doi:10.1109/acc.2005.1470055. [3] a. dumitrescu, j. mitchell. approximation algorithms for tsp with neighborhoods in the plane. j algorithms 48(1):135–159, 2003. [4] j. t. isaacs, d. j. klein, j. p. hespanha. algorithms for the traveling salesman problem with neighborhoods involving a dubins vehicle. in american control conference (acc), 2011, pp. 1704–1709. ieee, 2011. doi:10.1109/acc.2011.5991501. [5] x. ma, d. a. castanon. receding horizon planning for dubins traveling salesman problems. in 45th ieee conference on decision and control, pp. 5453–5458. 2006. doi:10.1109/cdc.2006.376928. [6] j. le ny, e. feron, e. frazzoli. on the dubins traveling salesman problem. ieee transactions on automatic control 57(1):265–270, 2012. doi:10.1109/tac.2011.2166311. [7] p. váňa, j. faigl. on the dubins traveling salesman problem with neighborhoods. international conference on intelligent robots and systems (iros) pp. 4029–4034, 2015. [8] x. goaoc, h.-s. kim, s. lazard. bounded-curvature shortest paths through a sequence of points using convex optimization. siam journal on computing 42(2):662–684, 2013. doi:10.1137/100816079. [9] j. t. isaacs, j. p. hespanha. dubins traveling salesman problem with neighborhoods: a graph-based approach. algorithms 6(1):84–99, 2013. doi:10.3390/a6010084. [10] x. yu, j. hung. optimal path planning for an autonomous robot-trailer system. in 38th annual conference on ieee industrial electronics society (iecon), pp. 2762–2767. 2012. doi:10.1109/iecon.2012.6389140. [11] k. j. obermeyer, p. oberlin, s. darbha. samplingbased path planning for a visual reconnaissance unmanned air vehicle. journal of guidance, control, and dynamics 35(2):619–631, 2012. doi:10.2514/1.48949. [12] c. e. noon, j. c. bean. a lagrangian based approach for the asymmetric generalized traveling salesman problem. operations research 39(4):623–632, 1991. doi:10.1287/opre.39.4.623. [13] s. lin, b. w. kernighan. an effective heuristic algorithm for the traveling-salesman problem. operations research 21(2):498–516, 1973. doi:10.1287/opre.21.2.498. [14] k. j. obermeyer. path planning for a uav performing reconnaissance of static ground targets in terrain. in aiaa guidance, navigation, and control conference, pp. 10–13. 2009. doi:10.2514/6.2009-5888. [15] x. zhang, j. chen, b. xin, z. peng. a memetic algorithm for path planning of curvature-constrained uavs performing surveillance of multiple ground targets. chinese journal of aeronautics 27(3):622–633, 2014. doi:10.1016/j.cja.2014.04.024. [16] k. helsgaun. lkh solver 2.0.7. http://www.akira.ruc.dk/~keld/research/lkh. [cited 31 mar 2015]. 61 http://dx.doi.org/10.2307/2372560 http://dx.doi.org/10.1109/acc.2005.1470055 http://dx.doi.org/10.1109/acc.2011.5991501 http://dx.doi.org/10.1109/cdc.2006.376928 http://dx.doi.org/10.1109/tac.2011.2166311 http://dx.doi.org/10.1137/100816079 http://dx.doi.org/10.3390/a6010084 http://dx.doi.org/10.1109/iecon.2012.6389140 http://dx.doi.org/10.2514/1.48949 http://dx.doi.org/10.1287/opre.39.4.623 http://dx.doi.org/10.1287/opre.21.2.498 http://dx.doi.org/10.2514/6.2009-5888 http://dx.doi.org/10.1016/j.cja.2014.04.024 http://www.akira.ruc.dk/~keld/research/lkh acta polytechnica ctu proceedings 2:57–61, 2015 1 introduction 2 related work 3 problem definition 4 existing methods 4.1 decoupled methods 4.2 sampling-based methods 4.3 evolutionary methods 5 modification of existing sampling-based algorithm 6 results 6.1 discussion 7 conclusions acknowledgements references 21 acta polytechnica ctu proceedings 2(1): 21–25, 2015 21 doi: 10.14311/app.2015.02.0021 the ritter-kolb catalogue and its impact on research into cvs, lmxbs and related objects h. ritter1, u. kolb2 1max–planck–institut für astrophysik, d–85741 garching, germany 2department of physical sciences, the open university, milton keynes mk7 6aa, united kingdom corresponding author: hsr@mpa-garching.mpg.de abstract in the first part of this paper, the ritter-kolb catalogue (rkcat for short), its history and a few examples of its application to research in the field of cataclysmic variables are briefly described. in a second part we look forward to possible future applications of rkcat for the study of cataclysmic variables, low-mass x-ray binaries and related objects. last but not least we also briefly comment on the future of the rkcat service itself. keywords: cataclysmic variables cataclysmic binaries low-mass x-ray binaries post-common envelope binaries catalogues. 1 introduction thirty years after the first public circulation of the catalogue of cataclysmic binaries, low-mass x-ray binaries and related objects, the so-called ritter catalogue or rcat for short (ritter 1982) it is perhaps a good time to look back at its history and some of its applications to research in the field of cataclysmic variables (cvs), lowmass x-ray binaries (lmxbs) and related objects, and at the same time to also look ahead to possible future applications of what later became to be known as the ritter-kolb catalogue (ritter & kolb 2003), hereafter rkcat for short. but before discussing the history and the future of rkcat let us briefly summarize for those who are not familiar with rkcat what rkcat actually is, i.e. its purpose, which information it does provide and how it can be accessed. 1.1 rkcat: what is it? ever since it was conceived rcat (up to 1998) and later rkcat (from 1998 onwards) has provided a comprehensive compilation of detached and semi-detached postcommon envelope binaries with known (or suspected) orbital periods. the restriction to systems with “known orbital period” is important for two reasons: first, knowing the orbital period of a binary not only provides important information about the object in question, but it is usually also a sure sign for the object having undergone serious examination to some degree, and that more is known about it than just its position on the sky, its apparent magnitude, and that it may be variable. second, restriction to systems with known orbital period also considerably limits the number of objects to be dealt with which is anyway growing at an alarming rate (see below). among the semi-detached systems we then have cvs (with at least one white dwarf (wd) component) and lmxbs (with either a neutron star or a black hole primary and usually a non-degenerate companion, but low-mass wds do also occur). among the detached systems, in rcat/rkcat referred to as “related objects”, we have “white dwarf”-red dwarf binaries and “white dwarf”-”white dwarf” binaries (double degenerates), where a “white dwarf” is either a genuine wd or an immediate precursor of a wd such as a sdbor sdostar. not included in rcat/rkcat among the detached systems are binary radio pulsars although some of them do in fact match the criteria for inclusion among the “related objects”. the reason for excluding binary radio pulsars is because they are well documented elsewhere (manchester et al. 2005).1 1.2 rkcat: what does it contain? rkcat provides information about each object in tabular form, a list of references to the most relevant recent literature, a list of references to published finding charts and a comprehensive cross reference list of alias object designations. in the tables (separate for cvs, lmxbs and related objects) we provide object designations, the position on the sky (α, δ), information about the object 1the data are available electronically at http://www.atnf.csiro.au/research/pulsar/psrcat. 21 http://dx.doi.org/10.14311/app.2015.02.0021 h. ritter, u. kolb type/subtype, apparent magnitudes, periods (above all the orbital period, but also the superhump period and the spin period of the wd (in cvs), or of the neutron star (in lmxbs)), the spectral types of the components as well as other orbital and stellar parameters (orbital inclination, mass ratio, masses, radii) to the extent that these quantities are known. the purpose of the cross reference list of alias object designations (appropriately called “whoswho”) is to help avoid confusion about object idendity. many objects have a long history during which they have been given many different names by different authors. thus confusion about an object’s idendity can simply arise because earlier authors can of course not refer to later object designations. but also going backwards in the literature does not always reveal even the more common alias names. the “whoswho” list is an attempt to remedy that situation and to nail down an object’s idendity in addition to its identification on a finding chart. the most recent release of rkcat at the time of writing (ritter & kolb 2003, update rkcat7.20 as of 30 june 2013) contains information about 1093 cvs, 104 lmxbs and 483 related objects, i.e. of 1680 objects in total. 1.3 rkcat: how can it be accessed? whereas earlier editions of rcat/rkcat appeared in print (ritter, 1982, 1983, 1984, 1987, 1990; ritter & kolb 1995, 1998) the current (7th) edition (ritter & kolb 2003) is available in electronic form only from websites at the open university (ou) at http://physics.open.ac.uk/rkcat and at the max-planck-institut für astrophysik (mpa) at http://www.mpa-garching.mpg.de/rkcat, and in slightly different form but with the same content from the strasbourg astronomical data center (cds) at http://cdsarc.u-strasbg.fr/viz-bin/cat?b/cb. the main difference between the versions provided by the ou/mpa websites and the cds website is that the former provide the tables in a two lines per object format with delimeters which allows for easy visual inspection of the tables on a computer screen, whereas the cds tables come in a one line per object format which (even without the delimiters) is much too wide for that purpose. rather they are designed to be processed electronically. many more copies of rkcat are available from various other websites. but because the contents of these copies is beyond our control we do not take responsibility for the content of any other than the abovementioned sources. 2 a brief history of rcat/rkcat compiling data on cvs for what was later to become rcat actually began already in 1973, i.e. 40 years ago, as part of the first authors’s (hereafter hr) phd project (ritter 1977). although at that time there was no intention whatsoever to produce a catalogue, compiling data on cvs, lmxbs, and related objects continued also beyond the end of the phd project, and it was around 1978/79 that rumors about the existence of this compilation began to spread among colleagues, some of whom did not hesitate to ask for copies. dutifully, hand-written copies of the compilation were produced and circulated among a few priviliged individuals. in that context, one must realize that at that time neither the internet nor email did exist, and electronic storage of data on computers was unavailable the storage media of choice were either hand-written files or punched cards and consequently, there was no easy way of editing and updating such a data base. bogdan paczynski was among the first to whom a copy was sent upon his request. and based on the distribution of the orbital periods of the 43 cvs known at that time he must have realized the sharp drop of the number of cvs shortward of an orbital period of ∼ 80min, and not long after that went on explaining the physical significance of the minimum orbital period of cvs in the context of cv evolution (paczynski 1981; paczynski & sienkiewicz 1981, 1983). this was probably the first direct application of the immediate precursor of rcat to cv research. around 1981 personal storage accounts and screen editors on computers became finally available. therefore, the data of the cv compilation were migrated to permanent electronic storage and editing. from that time on it not only became much easier to update the compilation but also to produce printed copies of it. as a consequence, so to speak as a test, soon after having gone electronic, the first and second edition of rcat were produced and circulated in preprint form among a relatively large number (∼ 200) of colleagues and libraries (ritter 1982, 1983). the positive response to the catalogue then lead to the publication of the 3rd edition printed in a refereed journal (ritter 1984). with data on cvs thus becoming widely available it took not long before another of the remarkable properties of the cv period distribution, i.e. the period gap, was addressed and an explanation for it in terms of cv evolution was given (spruit & ritter 1983; rappaport, vebunt & joss 1983). around 1987, when the 4th edition of rcat (ritter 1987) was published it was also realized, not least thanks to x-ray observations with exosat, that the distribution of the orbital periods of the synchronized and non-synchronized magnetic cvs, i.e. of the am her stars and the intermediate polars, are significantly dif22 the ritter-kolb catalogue and its impact on research into cvs, lmxbs and related objects ferent and that this could be accounted for in terms of standard cv evolution by the fact that on average the mass transfer rate in cvs decreases with orbital period (hameury et al. 1987). with the publication of the 5th edition of rcat (ritter 1990) another interesting property of the period distribution of cvs became apparent, namely the peculiar distribution of the orbital periods of am her stars below the period gap with 6 am her stars piling up within a very narrow period interval of only 2 min, the so-called period spike (see fig. 1 in ritter & kolb 1992). in that paper we had also given a detailed analysis of the period spike and explained its position and width as a natural consequence of cv evolution in the context of the disrupted magnetic braking hypothesis. although at that time the am her period spike was considered to be statistically highly significant and thus worth studying, now, more that 20 years later and with many more systems known, we must admit that there is no such spike and that we were just fooled by a statistical fluke. with the 6th edition of the catalogue (ritter & kolb 1998) two major changes occurred. first, because the amount of work connected with updating the catalogue had increased so much that additional support, in particular for servicing the newly established catalogue websites, was needed, ulrich kolb (uk) stepped in, and so rcat became rkcat. since then uk has been mainly responsible for the maintenance of our websites. second, beginning with the 6th edition the data became available in electronic form only, and no more than a brief introduction to the catalogue has appeared in print. finally since 2003, the 7th edition of rkcat (ritter & kolb 2003) has become available, the data again in electronic form only. the catalogue websites of the 7th edition are now updated regularly, currently every 6 months, and at the time of writing the 20th update (release 7.20) is available. the development of rcat/rkcat over the past 35 years is perhaps best illustrated by plotting the number of objects contained in the catalogue as a function of time, as is shown in fig. 1. as is readily seen, the number of objects has been steadily and exponentially increasing with a growth rate of ∼ 9%/year over the past 30 years! 3 some examples of possible future applications of rkcat before going to discuss a few specific possibilities for future applications of rkcat, let us briefly make two rather general comments concerning rkcat and its future use. • the first comment is a warning, namely that based on the criteria according to which objects enter the catalogue, no subset of the objects listed in rkcat represents a statistically well-defined sample. one has to keep this in mind when e.g. comparing results of population synthesis calculations with distribution functions extracted from rkcat. • the second general comment is that by now the number of objects contained in rkcat is larger by a factor 10 to 20 than it was 20 30 years ago, i.e. when the first applications of rcat to problems of cv evolution were made. what this means is that now the contents of rkcat allows for statistically meaningful studies of the properties of various subsets of cvs, lmxbs or related objects, which because of too small numbers of objects had not been possible a decade or two ago. figure 1: number of cvs (open squares), lmxbs (open triangles), and related objects (filled diamonds), as well as the total number of objects (filled circles) contained in rcat/rkcat and its precursors as a function of time. let us now turn to just a few specific possible future applications of rkcat. 1. it has long been known that the average orbital period of age zero post common envelope wd-rd binaries, i.e. of the binary central stars of planetary nebulae and systems where the wd is still so hot that it gives rise to a noticeable reflection effect on the companion, is systematically longer (by about a factor of 2) than the average orbital period of the remaining detached post common envelope wd-rd binaries. the qualitative explanation for this is that post common envelope binaries undergo orbital evolution as a consequence of 23 h. ritter, u. kolb loss of orbital angular momentum. in that context it is important that now rkcat contains a relatively large number of detached wd-rd post common envelope binaries with reasonably accurately known binary parameters. based on these data it should be possible to investigate the angular momentum loss of post common envelope wd-rd binaries in more detail, e.g. its dependence on properties of the rd, i.e. whether it is evolved or fully convective or not, and maybe even quantify it. 2. the period distribution of dwarf novae shows an undisputable dearth of systems in the period range 3h . porb . 4h which is not predicted by the standard cv evolutionary paradigm, i.e. the disrupted magnetic braking hypothesis, in combination with the disc instability model for dwarf nova outbursts. a satisfactory explanation for this phenomenon is so far lacking. in the framework of the disc instability model this could be accounted for only if the mass transfer rate is decreasing less strongly with orbital period than the critical mass transfer rate for dwarf nova outbursts as a cv evolves from longer to shorter orbital periods. this, in turn, implies that the angular momentum loss time scale must decrease with the orbital period, contrary to what standard prescriptions of magnetic braking, e.g. verbunt & zwaan (1981) or mestel & spruit (1983) predict. the ratio of the number of dwarf novae to novalike systems as a function of orbital period, on the other hand, should allow for an empirical calibration of the angular momentum loss rate as a function of orbital period. 3. as the absence of a clear period gap in the period distribution of am her systems suggests, the strong magnetic field of the wd interferes with the loss of mass and angular momentum via a stellar wind from the companion star with the result that magnetic braking in magnetic cvs is significantly weaker than in non-magnetic cvs. therefore, if below the period gap angular momentum loss via magnetic braking is comparable to that caused by gravitational radiation, as has been argued e.g. by knigge, patterson & baraffe (2011), and if magnetic braking is also weaker in am her stars below the gap, one would expect that also the minimum period of am her stars is systematically shorter than that of non-magnetic systems. therefore, by a careful examination of the period distributions of magnetic and non-magnetic cvs below the gap it should be possible to get more insight into the evolution of cvs below the gap. clearly, the above list of possible future applications of rkcat is not exhaustive. what we hope for is that our colleagues working with rkcat will come up with many more and even more ingenious applications of rkcat for the research in the field of compact binaries than we have just given. 4 the future of rkcat apart from discussing future appliactions of rkcat we think that writing this paper provides us also with an exellent opportunity to briefly address the possible future of rkcat itself. in that context it is important to be aware of the following facts: • the number of objects in rkcat has been growing exponentially at a steady rate of ∼ 9%/yr over the past 30 years (see fig. 1), and so has the amount of work that has been going into rkcat. and there is no reason to expect that this will be much different in the near future. • already now, servicing the catalogue data base is practically a full-time job for hr. • hr is already several years beyond formal retirement age. taken these three points together it is obvious that hr will definitely not be able to provide this service for many more years. if rkact or something akin to it should be continued beyond hr’s definitive retirement from that job then it is clear that in view of the first two points above some changes in how this service is and in what should be provided are unavoidable. the all decisive question to the cv community then is: who is prepared to continue with rkcat and in which form? anybody out there? acknowledgement hr would like to thank franco giovanelli for inviting him to attend this workshop and thus for providing him an opportunity to talk about the past and future of rkcat. references [1] hameury, j.m., king, a.r., lasota, j.p., ritter, h.: 1987, mnras 231, 535. [2] knigge, c., baraffe, i., patterson, j.: 2011, apjs 194, 28. 24 the ritter-kolb catalogue and its impact on research into cvs, lmxbs and related objects [3] manchester, r.n., hobbs, g.b., teoh a., hobbs, m.: 2005, aj 129, 1993. doi:10.1111/j.1745-3933.2006.00242.x [4] mestel, l., spruit, h.c.: 1987, mnras 226, 57. [5] paczynski, b.: 1981, aca 31, 1. doi:10.1017/cbo9781139164245 [6] paczynski, b., sienkiewicz, r.: 1981, apj 248, l27. doi:10.1086/421295 [7] paczynski, b., sienkiewicz, r.: 1983, apj 268, 825. [8] rappaport, s., verbunt, f., joss, p.c.: 1983, apj 275, 713. doi:10.1086/382481 [9] ritter, h.: 1977, phd thesis, univ. hamburg. doi:10.1086/590491 [10] ritter, h.: 1982, catalogue of cataclysmic binaries, low-mass x-ray binaries and related objects, first edition, preprint mpa 22. doi:10.1046/j.1365-8711.1999.02926.x [11] ritter, h.: 1983, catalogue of cataclysmic binaries, low-mass x-ray binaries and related objects, second edition, preprint mpa 51. [12] ritter, h.: 1984, a&as 57, 385. [13] ritter, h.: 1987, a&as 70, 335. [14] ritter, h.: 1990, a&as 85, 1179. doi:10.1046/j.1365-8711.2000.03780.x [15] ritter, h., kolb, u.: 1992, a&a 259, 159. [16] ritter, h., kolb, u.: 1995, in x-ray binaries, w.h.g. lewin, j. van paradijs, e.p.j. van den heuvel (eds.), cambridge astrophysics series 26, cambridge university press, p. 578. [17] ritter, h., kolb, u.: 1998, a&as 129, 83. doi:10.1086/341696 [18] ritter, h., kolb, u.: 2003, a&a 404, 301. [19] spruit, h.c., ritter, h.: 1983, a&a 124, 267. doi:10.1088/0004-637x/721/2/1356 [20] verbunt, f., zwaan, c.: 1981, a&a 100, l7. discussion ashley pagnotta: regarding the future of rkcat, have you considered working with the aavso? their vsx is not nicely curated like rkcat but is a possible future home. hans ritter: up to now i had not approached anybody or any organisation regarding the future of rkcat. this is actually the first time that i have spoken in public about that problem. christian knigge: just a comment on the topics you suggested for further study, which i think are really interesting. regarding pmin for magnetic cvs, boris gaensicke, retha pretorius and i have all looked at this a bit and have not seen the expected difference to non-magnetic cvs. [note added: i think this is mostly unpublished – the only relevant publication i am aware of is pretorius, knigge & schwope 2013, mnras, 432, 570, where fig. 1 shows that the period minimum for magnetic cvs is consistent with that for all cvs, which are dominated by non-magnetic systems. but we don’t really discuss that in the text.] also, in fig. 18 of knigge, baraffe & patterson (2011) we plot the dwarf nova fraction versus porb and find that not only is it zero just above the gap, but going from shorter to longer orbital periods it declines monotonically through the gap, which is very surprising. — 25 http://dx.doi.org/10.1111/j.1745-3933.2006.00242.x http://dx.doi.org/10.1017/cbo9781139164245 http://dx.doi.org/10.1086/421295 http://dx.doi.org/10.1086/382481 http://dx.doi.org/10.1086/590491 http://dx.doi.org/10.1046/j.1365-8711.1999.02926.x http://dx.doi.org/10.1046/j.1365-8711.2000.03780.x http://dx.doi.org/10.1086/341696 http://dx.doi.org/10.1088/0004-637x/721/2/1356 introduction rkcat: what is it? rkcat: what does it contain? rkcat: how can it be accessed? a brief history of rcat/rkcat some examples of possible future applications of rkcat the future of rkcat 311 acta polytechnica ctu proceedings 1(1): 311–315, 2014 311 doi: 10.14311/app.2014.01.0311 sifap: a new fast astronomical photometer filippo ambrosino1, franco meddi1, roberto nesci 2, corinne rossi1, silvia sclavi1, ivan bruni3 1dipartimento di fisica università la sapienza, p.le a. moro 5, 00185 roma, italy, 2inaf-iaps, tor vergata, roma, italy, 3istituto nazionale di astrofisica, osservatorio astronomico, via ranzani 1, 40127 bologna, italy. corresponding author: filippo.ambrosino@roma1.infn.it abstract a fast photometer based on sipm technology was developed and tested at the university of rome “la sapienza” and at the bologna observatory. in this paper we present the improvements applied to our instrument, concerning new cooled sensors, a new version of the electronics and an upgraded control timing software. keywords: instrumentation: photometer stars: pulsars. 1 instrument description the general description of our 3-channel photometer sifap (silicon fast astronomical photometer) is presented in meddi et al. (2011; 2012). we only remind here that each channel is dedicated to a different target: variable source (channel 0), nearby sky (channel 1) and reference star (channel 2). a gps receiver sends a pulse per second (pps) to a micro processor (µp) which in turn produces a signal that we call gated pps. this last is used both to drive two leds in order to have an optical temporal marker and to synchronize our custom electronics. during the last year we replaced the old hamamatsu multi pixel photon counter (mppc) modules with new ones, having the sensor cooled by a built-in peltier cell 1; we modified our electronics and to increase the uninterrupted acquisition time and to reduce the sampling gate duration from 0.55 ms down to 0.1 ms. the new block diagram of the instrument is shown in figure 1. the thermo-electric cooled system allows to reach a fixed working temperature of -10 ◦c, with a large reduction of the mean dark count. the s/n ratio is improved by a factor 3 with respect to the previous one. the modules have limited geometrical dimensions and low weight so they can be directly located at the exit pupil of the telescope. other characteristics of the new sensors are similar to the old ones: pixel size of 50µm for a total active area of 1 mm2 and photon detection efficiency with a maximum value of about 50% at wavelength of 440 nm2. the built-in electronics of each hamamatsu module can generate three types of output: pulse count via usb interface already processed in time windows of 1 ms, analog and discriminated. we use the last one to feed our electronics which uses a new protocol for data exchange between a field programmable gate array and a µp and a new data storage support. the integration time windows for this output are now 0.1 ms. we called this electronics p3e, which stands for pulsar pulse period extractor. the pointing and the signal maximization procedures and the fast pre-analysis to check the pulsating behavior of the pointed source are described in meddi et al. (2012). 1 http://www.hamamatsu.com/resources/pdf/ssd/c11208 series kacc1176e03.pdf 2http://www.hamamatsu.com/resources/pdf/ssd/s11028 series kapd1026e04.pdf 311 http://dx.doi.org/10.14311/app.2014.01.0311 filippo ambrosino et al. figure 1: general block diagram of sifap mounted at the telescope. the gps antenna is located outside the dome. hamamatsu mppc sensors are integrated in their modules, p3e units are fed by the discriminated output. each couple of mppc sensor and p3e unit is dedicated to a different target: variable source (mppc0 and p3e0), nearby sky (mppc1 and p3e1) and a reference star (mppc2 and p3e2). figure 2: fft applied to the whole raw data acquired by p3e0 on 2012, december 19. 312 sifap: a new fast astronomical photometer figure 3: fundamental frequency and period values of the crab pulsar signal obtained by our data with applied the heliocentric corrections compared with those computed from jbo ephemeris. the uncertainties on the jbo values are due to a numerical interpolation procedure. the quoted errors on our data are statistical only. figure 4: crab pulsar light curve folded by the xronos task efold for p3e0 (2012, december 19) corrected data. 2 data analysis and results on 2012 december 19 we observed the crab pulsar with the loiano telescope, for one hour. to optimize the pointing of the target, we performed a quick pre-processing analysis on a short acquisition of the data (∼ 100 s), based on autocorrelation and fft techniques. we then analyzed the whole data set with a fft analysis to estimate the spin period of the pulsar. in figure 2 we show the amplitude spectrum of the crab pulsar signal obtained from data collected 313 filippo ambrosino et al. by p3e0. we used the xronos package of the high energy astrophysics science archive research center (heasarc) to apply the heliocentric correction (task earth2sun) and to determine the best fitting period for the crab pulsar signal (task efsearch). in figure 3 we compare the jodrell bank observatory (jbo) ephemeris3 prediction for the fundamental frequency and period of the crab pulsar signal with the estimates of the same quantities obtained by our barycentered data. the agreement between the two results is within 300 µhz for the fundamental frequency and 300 ns for the spin period. such discrepancy can not be justified without taking into account systematic effects, which are explained in terms of the clock drift which depends on the temperature. this drift is estimated by measuring the time interval between the two optical markers generated by the gated pps signal, the first at the beginning and the second one at the end of the acquisition. taking into account such effect, the differences for the spin period are reduced below 15 ns. systematic uncertainties are due to i) the propagation of the gated pps signal trough the cables and ii) the rising edge of leds. such systematic uncertainties produce a total delay of about 320 ns. finally, the accuracy on the pulse output time of the pps signal which is ±0.001 ms at the rising edge of the pulse itself. all these effects are not included in the numerical computation of the uncertainty on the period obtained by applying the barycentric correction. the crab light curves were obtained by using the task efold on the barycentered data; the result for p3e0 is shown in figure 4. the shape of the primary and the second peak, and their flux ratio, are in good agreement with the literature data (e.g. golden et al., 2000; zampieri et al., 2011). the sky and reference star measurements were processed in the same way as the ones belonging to the target to look for spurious signals which might interfere with the astronomical signal from the crab nebula: no evidence of periodicity was detected. 3 conclusions we built a fast photometer able to collect data of periodic signals with high time accuracy integrating in time windows down to 0.1 ms. with the loiano 1.5 m telescope we derived the period and a high s/n light curve of the crab pulsar with a measurement duration of about 1 hour. in these conditions we obtained a fair agreement with the fundamental frequency and the spin period calculated from the jbo database. we intend to upgrade our custom electronics aiming at reaching shorter time sampling keeping a good s/n ratio. our final goal would be to compare fast optical measurements with the γ-ray, x-ray, ir and radio ones to explore more deeply the structure and the phenomena occurring in the emitting regions of pulsars. in particular, we want to study how the spin period slows down (dissipative process) and the amount of the eventual phase delay among the peaks in the various band (phase shifting process). we need to collect high quality data with a 0.001 ms time windows to be able to perform these kind of investigations. to this purpose we modified our gps system to reach a more accurate determination of the absolute time scale (within 100 ns) by using a burst of n gated pps signals instead of the single one presently used. we started with theoretical computation of the minimum possible time sampling for a v ∼ 16 mag object as a function of the telescope diameter. the results indicate that it could be possible to measure objects of the same magnitude as the crab pulsar with similar s/n ratio in time windows shorter than 0.1 ms. for instance, with a 5 m telescope the integration time could be reduced down to 0.01 ms. moreover it is mandatory to have larger telescopes in order to have enough detectable photons and higher resolution on the absolute timing by adopting a military class gps antenna which would be able to reach at least 1 ns accuracy. in this case it would be necessary to upgrade the optical time marker by substituting standard leds with laser ones. acknowledgement the authors thank the bologna observatory for the logistic support and the technical assistance during the observations. the universita’ di roma “la sapienza” supported the project. this research has made use of the simbad database operated at cds, strasbourg, france. references [1] golden a., shearer a., redfern r. m., beskin g. m., neizvestny s. i. et al., 2000, a&a, 363, 617 [2] meddi f., ambrosino f., rossi c., nesci r., sclavi s. et al., 2011, acta polytechnica, 51, n.6, 42. [3] meddi f., ambrosino f., rossi c., nesci r., sclavi s. et al., 2012, pasp, 124, 448. doi:10.1086/665925 [4] zampieri l., germana c., barbieri c., naletto g., cade a. et al., 2011, adv. space res., 47, 365. doi:10.1016/j.asr.2010.07.016 3http://www.jb.man.ac.uk/pulsar/crab.html 314 http://dx.doi.org/10.1086/665925 http://dx.doi.org/10.1016/j.asr.2010.07.016 sifap: a new fast astronomical photometer discussion b. aschenbach: how do you explain that the second harmonic in the amplitude spectrum is higher than the first one? f. ambrosino: the amplitude of the single harmonic depends on the shape of the light curve; in the case of the crab pulsar in one period there are two emission peaks of different intensity and with a phase shift of about 0.45. 315 instrument description data analysis and results conclusions acta polytechnica ctu proceedings doi:10.14311/app.2016.3.0019 acta polytechnica ctu proceedings 3:19–24, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app the effect of support plate on drilling-induced delamination navid zarif karimia,∗, hossein heidaryb, parnian kianfarc, mahmud hasanic, giangiacomo minaka a university of bologna, via fontanelle 40, forli, italy b university of tafresh, tehran road 1, tafresh, iran c amirkabir university of technology, hafez 424, tehran, iran ∗ corresponding author: navid.zarif@unibo.it abstract. delamination is considered as a major problem in drilling of composite materials, which degrades the mechanical properties of these materials. the thrust force exerted by the drill is considered as the major cause of delamination; and one practical approach to reduce delamination is to use a back-up plate under the specimen. in this paper, the effect of exit support plate on delamination in twist drilling of glass fiber reinforced composites is studied. firstly, two analytical models based on linear fracture mechanics and elastic bending theory of plates are described to find critical thrust forces at the beginning of crack growth for drilling with and without back-up plate. secondly, two series of experiments are carried out on glass fiber reinforced composites to determine quantitatively the effect of drilling parameters on the amount of delamination. experimental findings verify a large reduction in the amount of delaminated area when a back-up plate is placed under the specimen. keywords: drilling, composite materials, delamination, support plate. 1. introduction glass fiber reinforced plastics (gfrps) have been extensively employed in many engineering applications because of their outstanding advantages over other materials. the machining and specially drilling of gprps have become very important due to the need for assembling of subcomponents made from these materials. but, composite materials are difficult to machine due to some particular characteristics of them like non-homogeneous, anisotropic and abrasive fibers. this causes significant damages in drilling process such as matrix cracking, fiber breakage, fuzzing and thermal degradation. among the damages caused by drilling, delamination is considered as one the most crucial, which results in lowering of strength against fatigue and subsequently reducing the longterm performance of composite structures [1, 2]. several techniques have been suggested to reduce delamination in drilling process that each has its own advantages and limitations. one of the frequently used methods is to place a support plate under the specimen. during supported drilling, in contrast to unsupported drilling, the specimen is not free to bend due to constraints imposed by back-up plate. in drilling with back-up plate, the thrust force increases suddenly and severely as the chisel edge begins to penetrate into the specimen and it continues until the full penetration of cutting lips. at this point actual material removal takes place and the force reaches its steady state value, until delamination occurs. in this stage, delamination causes the force to decrease stepwise, each step associates to a crack opening. unlike supported drilling, during drilling without back-up plate, the force increases gradually at the beginning of process. this is mainly because the real feed rate is much lower than the adjusted feed due to relative movement of drill bit and workpiece. as the drill bit approaches the last uncut plies, the stress due to the thrust force exceeds its critical value and all the uncut material is burst open [3]. until now, many researchers have attempted to reduce drilling induced delamination. hocheng and dharan used linear elastic fracture mechanics to determine the critical thrust force for twist drilling as push-out delamination begins to propagate [4]. hocheng and tsao proposed some analytical models for different drill bits including candle stick drill, saw drill, core drill and step drill to determine the thrust force at the beginning of delamination growth [5, 6]. based on these models, they realized the delamination can be reduced by lowering the thrust force or distributing the force outward from the center [7]. in a similar work, they studied the effect of exit back-up plate on drilling-induced delamination when using a slot drill bit and a core drill bit [8]. they showed that the critical thrust force is increased when using a back-up plate, hence delamination is less likely to happen. many efforts have been made to reduce the thrust force exerted by drill bit on the specimen, while few researchers studied the effect of support plate on thrust force and associated delamination. this paper investigates the effect of back-up plate on drilling-induced delamination both analytically and experimentally. 19 http://dx.doi.org/10.14311/app.2016.3.0019 http://ojs.cvut.cz/ojs/index.php/app n. zarif karimi, h. heidary, p. kianfar et al. acta polytechnica ctu proceedings 2. experimental procedure 2.1. delamination measurement chen presented an index to evaluate the amount of delamination called conventional delamination factor [9]. however, this factor is not proper because the crack size does not represent the damage magnitude appropriately and also this procedure does not indicate the damage area. davim et al. suggested a superior approach to determine the delamination factor called the adjusted delamination factor fda which is expressed as eq. (1) [10]. the first part of eq. (1) shows the size of the crack contribution and the second part shows the damage area contribution. fda = α dmax d0 + β amax a0 (1) where the coefficients α and β can be calculated as below: β = ad a0 −amax α = 1 − β (2) where d0 is the nominal diameter of the hole, dmax is the maximum diameter of the damage hole, a0 is the area related to the nominal hole, amax is the area related to the maximum diameter of the delamination zone and ad is the delaminated area. 2.2. materials and tools the composite plates were produced by hand lay-up method with araldite ly556 epoxy resin reinforced with 60 % e-glass unidirectional fiber. the density of epoxy resin and glass fibers were 1.12 g/cm3 and 292 g/m2, respectively. tensile strength and tensile modules of resin were 80 mpa and 2.7 gpa, respectively, and for glass fibers were 2150 mpa and 74 gpa, respectively. the composite laminates had 16 plies and a thickness of 5 mm. the holes were drilled at the center of plates by standard hss twist drills 10 mm. during unsupported drilling, a back-up plate of 5 mm thick was positioned under the specimens. an appropriate clamping system was used to fix the specimens and back-up plate in the drilling machine, shown in figure 1. the specimens and back-up plate were fixed in position by tightening four screws at the corners. 2.3. plan of experiments in the present study, taguchi method was used to design drilling experiments. three parameters, feed rate, cutting speed and drill point angle were selected and three levels for each parameter were suggested based on our preliminary researches [11–14]. after determination of parameters and correspond levels, a proper orthogonal array need to be selected. the orthogonal array chosen was the l9. after conducting experiments, the signal to noise ratio (sn) needs to be calculated for each experiment to determine the effect of each parameter. according figure 1. experimental setup. to this method, the optimization is done by using three signal to noise ratios; smaller is better, larger is better and nominal is better. notice that, regardless of what approach is taken, always higher value of the signal to noise ratio is better. in this investigation, the delamination factor needs to be minimized; hence, smaller is better definition of the signal to noise ratio was used. sni = −10 log( ni∑ i=1 y2 i ni ) (3) where i is the experiment number and ni is the number of trials for experiment i [15]. 3. results and discussion 3.1. theoretical analysis of critical thrust force the energy balance equation at the onset of delamination propagation is: dud = dw − du (4) in which du is the infinitesimal strain energy, dw is the infinitesimal work done by the thrust force fth and drill displacement of dx and dud is the infinitesimal strain energy absorbed by crack growth which are as following: dw = fth · dx dud = gic · da (5) where da is the change in the delamination area and gic is the critical strain energy release rate in mode i, which is assumed to be constant according to saghizadeh and dharan [16]. 3.1.1. critical thrust force in drilling without support plate figure 2 depicts the schematic of delamination in unsupported drilling. in figure 2, fth is the thrust force exerted by a twist drill at the center of plate, x is the displacement of drill, h is the thickness of 20 vol. 3/2016 the effect of support plate on drilling-induced delamination figure 2. the schematic of delamination for unsupported drilling. specimen, h is the uncut depth under tool, and a is the radius of crack (delamination). in this model, two assumption are considered; the isotropic behavior and pure bending of the laminate. according to the classical plate theory, for a circular plate with clamped edges and concentrated force the amount of deflection can be expressed as [17]: w(r) = fth 16πm [2r2 ln r a + (a2 − r2)] (6) which is written in polar coordinate system (r is radius). m = eh3/(12(1 − ϑ2)) is flexural rigidity of the plate, e is modulus of young, and ϑ is ratio of poisson. the stored strain energy, the work done and the strain energy absorbed by crack growth are expressed as below equations, respectively. u = f 2 tha 2 32πm du = f 2 tha 16πm da (7) w = fthw(0) = f 2 tha 2 16πm dw = f 2 tha 8πm da (8) ud = gic ·a = gicπa 2 dud = gic2πada (9) now it is possible to calculate the critical thrust force at the onset of crack propagation by replacing eqs. (7), (8) and (9) in the energy balance eq. (4) as shown below: fth = π √ 32gicm (10) in order to prevent delamination, the thrust force exerted by the drill bit on the specimen which is related to the material properties and the uncut thickness should not go over this value. 3.1.2. critical thrust force in drilling with support plate figure 3 depicts the schematic of delamination in drilling with back-up plate. in figure 3, fb is the thrust force with back-up, r is the upward reaction force from the back-up plate, b is the radius of the applied ring force of back-up and c is the drill radius, x is the displacement. for an edge clamped circular plate under the action of a concentrated force in center and upward circular force, the amount of deflection can be expressed as: w1(r) = fb 16πm [2r2 ln r a + (a2 − r2)]− − r 8πm [(r2 + b2) ln b a + 1 2(1 − b2 a2 )(a2 + r2)] 0 6 r 6 b (11) w2(r) = fb 16πm [2r2 ln r a + (a2 − r2)]− − r 8πm [(r2 + b2) ln r a + 1 2(1 + b2 a2 )(a2 − r2)] b 6 r 6 a (12) using boundary conditions, w(b) = 0, we get: r = fb [b2 ln b a + ( b2−a2 2 )] [2b2 ln b a + ( a4−b4 2a2 )] (13) by replacing r into the plate deflection equations, eq. (11) and eq. (12), the total stored strain energy and work done by external forces can be derived as follow: u = π[ ∫ b 0 [m(∂ 2w1 ∂r2 + 1 r ∂w1 ∂r )2]rdr+ + ∫ a b [m(∂ 2w2 ∂r2 + 1 r ∂w2 ∂r )2]rdr] du = ∂u ∂a da (14) w = fbw(0) = fb [ fba 2 16πm − r 8πm (b2 ln b a + + (a 2 − b2 2 ))] dw = ( f 2 ba 8πm − rfb 8πm a2 − b2 a )da (15) finally, by calculating dud from eq. (14) and replacing dud and dw in the energy balance equation, eq. (4), we get: fb = π √ 32gicm b a (16) where a and b are defined as follow: 21 n. zarif karimi, h. heidary, p. kianfar et al. acta polytechnica ctu proceedings figure 3. the schematic of delamination for supported drilling. b = [a4 − b4 − 8a2b2 ln b a ]× × [64b4a4 ln(a2b2) − 128a4b4 ln b ln a+ 16a6b2 ln b a + + 16a2b6 ln a b + a8 + b8 − 2a4b4] (17) a = 3(a12 − b12) + 72a10b2 ln b a + 192a4b8 ln a ln b+ + 3072a6b6 ln a 2 + b b2 + a + 768a4b8 ln a 2 + b b2 + a − − 288a8b4 ln a ln b− 704a6b6 ln b+ 192a2b10 ln a ln b+ + 73a4b4(a4 − b4) + 32a2b2(a8 − b8) + 64b4a8 ln b a + + 144a6b6 ln b a + 56a2b10 ln b a + 352a6b6 ln a2b2− − 96a2b10 ln a2b2 + 144a8b4 ln a2b2 + 1024a6b6 ln b3 a3 + + 256a4b8 ln b3 a3 + 768a4b8 ln a ln b− 16b12 ln a2b2+ + 32b12 ln a ln b− 384a4b8 ln a2b2 (18) 3.2. experimental results the graphs of thrust force and the scanned images of delamination in drilling with and without support plate at a feed rate of 0.025 mm/rev, spindle speed of 1600 rpm and drill point angle of 130 ◦ are shown in figure 4. it is believed that the thrust force applied by the drill on the specimen causes delamination and it occurs when the thrust force goes beyond its critical value. however, the graphs of the force in figure 4 clearly indicate this is only true for drilling with a support plate. during unsupported drilling the force is lower than in supported drilling, whereas the delamination is more extensive, which suggests that in unsupported drilling a different mechanism is in play, and other factors must be considered. these factors can be the dynamics of the workpiece, and the way in which the force is applied. the measured adjusted delamination factor (fda) and the corresponding signal to noise ratio (sn) determined using taguchi method smaller is better for figure 4. the graphs of thrust force and the scanned images of delamination in drilling with and without support plate. figure 5. comparison of fda in drilling with and without back-up. the two cases of drilling, supported and unsupported, are reported in table 1.symbols i and ii in table 1 represent two measured values for fda. the t-test on the mean values of adjusted delamination factor demonstrates significant differences between the means in these two cases (t0 = 8.00 > t0.005,34 = 2.73). to assist in the practical interpretation of this experiment, it is helpful to construct a graph of average responses at each experiment condition described in table 1. this graph is shown in figure 5. from figure 5, a significant difference in adjusted delamination factor for supported drilling and unsupported drilling can be observed so that in all drilling tests, the average value of delamination is reduced when applying a back-up plate. this reduction is in the range of 8-27 % for different drilling conditions. this reduction is mainly due to the reduction in matrix crack growth as a result of upward reaction of back-up plate. the values of sn data for the adjusted delamination factor for unsupported and supported drilling are given in table 1 and shown in figure 6. for unsupported drilling, the most important parame22 vol. 3/2016 the effect of support plate on drilling-induced delamination test no. parameters unsupported supported feed rate(mm/rev) speed (rpm) angle (◦) fda(1) fda(2) s/n fda(1) fda(2) s/n 1 0.025 800 90 1.41 1.37 -2.86 1.04 1.05 -0.34 2 0.025 1250 118 1.25 1.28 -2.04 1.07 1.06 -0.55 3 0.025 1600 130 1.30 1.26 -2.14 1.11 1.07 -0.75 4 0.05 800 118 1.49 1.52 -3.55 1.09 1.09 -0.87 5 0.05 1250 130 1.20 1.21 -1.62 1.10 1.11 -1.25 6 0.05 1600 90 1.33 1.28 -2.31 1.16 1.15 -0.75 7 0.1 800 130 1.49 1.58 -3.73 1.15 1.14 -1.40 8 0.1 1250 90 1.32 1.30 -2.35 1.18 1.17 -1.17 9 0.1 1600 118 1.36 1.33 -2.57 1.22 1.25 -1.83 table 1. l9 orthogonal array of taguchi and experimental results. figure 6. effect of process parameters for (a) unsupported drilling, (b) supported drilling. ters affecting the delamination factor are the spindle speed followed by feed rate. the optimum process parameters on the delamination are obtained as feed rate at level 1 (0.025 mm/rev), spindle speed at level 2 (1250 rpm) and drill point angle at level 3 (130 ◦) when drilling without back-up plate. however, when the back-up plate is applied, the effect of feed rate on delamination increases so that it becomes the most important parameter followed by spindle speed, figure 6 (b). the cause of this phenomenon can be attributed to the cutting mechanism and the relative movement of the tool and specimen. it is observed that the optimal value of the feed rate should be kept at low level in order to minimize the delamination factor. the optimum process parameters on the delamination are obtained as feed rate at level 1 (0.025 mm/rev), spindle speed at level 1 (800 rpm) and drill point angle at level 3 (130 ◦) for supported drilling. 4. conclusions in this paper, the effect of exit support plate on delamination in drilling of glass fiber reinforced composites is studied. a comprehensive analysis of the critical thrust force in drilling with and without back-up plate is presented based on three theories i.e. energy conservation theory, elastic bending theory and linear elastic fracture mechanics. the experimental results confirm the effects of delamination reduction when using a back-up plate under the specimen. this reduction is in the range of 8-27 % for different drilling conditions. this reduction is attributed to the crack growth suppression by upward reaction of back-up plate. references [1] r. m. jones. mechanics of composite materials. crc press, 1998. [2] d. liu, y. tang, w. l. cong. a review of mechanical drilling for composite laminatesc. composite structures 94(4):1265–1279, 2012. [3] e. capello. workpiece damping and its effect on delamination damage in drilling thin composite laminates. journal of materials processing technology 148(1):186–95, 2004. [4] h. ho-cheng, c. k. h. dharan. delamination during drilling in composite laminates. journal of manufacturing science and engineering 112(1):236–9, 1990. [5] h. hocheng, c. c. tsao. comprehensive analysis of delamination in drilling of composite materials with various drill bits. journal of materials processing technology 140(1):335–9, 2003. [6] h. hocheng, c. c. tsao. effects of special drill bits on drilling-induced delamination of composite materials. international journal of machine tools and manufacture 46(1):1403–16, 2006. [7] h. hocheng, c. c. tsao. the path towards delamination-free drilling of composite materials. journal of materials processing technology 167(1):1251– 64, 2005. doi:10.1016/j.ijmachtools.2005.10.004. [8] h. hocheng, c. c. tsao. effects of exit back-up on delamination in drilling composite materials using a saw drill and a core drill. international journal of machine tools and manufacture 45(1):1261–70, 2005. 23 http://dx.doi.org/10.1016/j.ijmachtools.2005.10.004 n. zarif karimi, h. heidary, p. kianfar et al. acta polytechnica ctu proceedings [9] w.-c. chen. some experimental investigations in the drilling of carbon fiber-reinforced plastic (cfrp) composite laminates. international journal of machine tools and manufacture 37(1):1097–108, 1997. [10] j. p. davim, j. c. rubio, a. m. abrao. a novel approach based on digital image analysis to evaluate the delamination factor after drilling composite laminates. composites science and technology 67(1):1939–45, 2007. [11] n. zarif karimi, h. heidary, m. ahmadi. residual tensile strength monitoring of drilled composite materials by acoustic emission. materials and design 40(1):229–36, 2012. [12] n. zarif karimi, h. heidary, g. minak, m. ahmadi. effect of the drilling process on the compression behavior of glass/epoxy laminates. composite structures 98(1):59– 68, 2013. doi:10.1016/j.compstruct.2012.10.044. [13] h. heidary, n. z. karimi, m. ahmadi, et al. clustering of acoustic emission signals collected during drilling process of composite materials using unsupervised classifiers. journal of composite materials 49(5):559–71, 2015. doi:10.1177/0021998314521258. [14] n. zarif karimi, g. minak, p. kianfar. analysis of damage mechanisms in drilling of composite materials by acoustic emission. composite structures 131(1):107– 14, 2015. doi:10.1016/j.compstruct.2015.04.025. [15] r. k. roy. a primer on the taguchi method, second edition. society of manufacturing engineers, 2010. [16] h. saghizadeh, c. k. h. dharan. delamination fracture toughness of graphite and aramid epoxy composites. journal of engineering materials and technology 108(1):290–5, 1986. [17] j. n. reddy. mechanics of laminated composite plates and shells: theory and analysis. crc press, 2004. 24 http://dx.doi.org/10.1016/j.compstruct.2012.10.044 http://dx.doi.org/10.1177/0021998314521258 http://dx.doi.org/10.1016/j.compstruct.2015.04.025 acta polytechnica ctu proceedings 3:19–24, 2016 1 introduction 2 experimental procedure 2.1 delamination measurement 2.2 materials and tools 2.3 plan of experiments 3 results and discussion 3.1 theoretical analysis of critical thrust force 3.1.1 critical thrust force in drilling without support plate 3.1.2 critical thrust force in drilling with support plate 3.2 experimental results 4 conclusions references acta polytechnica ctu proceedings doi:10.14311/app.2016.6.0018 acta polytechnica ctu proceedings 6:18–27, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app framework for ad hoc network communication in multi-robot systems khilda slyusar∗, miroslav kulich czech technical university in prague, zikova 1903/4, 166 36 prague, czech republic ∗ corresponding author: slyuskhi@fel.cvut.cz abstract. assume a team of mobile robots operating in environments where no communication infrastructure like routers or access points is available. the robots have to create a mobile ad hoc network, in that case, it provides communication on peer-to-peer basis. the paper gives an overview of existing solutions how to route messages in such ad hoc networks between robots that are not directly connected and introduces a design of a software framework for realization of such communication. feasibility of the proposed framework is shown on the example of distributed multi-robot exploration of an a priori unknown environment. testing of developed functionality in an exploration scenario is based on results of several experiments with various input conditions of the exploration process and various sizes of a team and is described herein. keywords: multi-robot systems, distributed exploration, ad hoc network, limited communication, cooperation. 1. introduction one of the key issues when designing a robotic system involving more than one entity is how these entities communicate. the majority of current multi-robot solutions are centralized (i.e., they have a central element through which all messages between robots are passed) or assume an unlimited communication range allowing to send messages directly between two arbitrary robots. this setup has many advantages, but also several drawbacks. it can be hard, costly or even impossible to prepare external communication infrastructure assuring one-to-one communication accessibility in hostile, unexplored or large environments. moreover, robustness of centralized systems which are highly dependent on a single node is low. finally, it might be difficult to exchange information in large systems consisting of many robots as their communication capacities are limited and a number of messages is high. some other arguments as well as real-world applications where ad hoc networks improved or might improve performance, scalability and robustness of robotic teams can be found in [1]. elkady et al. [2] give a nice survey of robotic middlewares. besides centralized client-server architecture employed, e.g. in player/stage/gazebo [3], ace/tao library [4], implementation of corba (common object request broker architecture) standard [5], is used for peer-to-peer communication in middlewares like claraty [6], miro [7], orocos [8]. alternatively, the ice framework by zeroc [9] for remote procedure calling (rpc) can be used as it is already done in the orca project [10]. both zeroc ice and corba do not provide communication between directly inaccessible nodes in a decentralized fashion and although extensions for ad hoc networks exist [11] they were not used in the mentioned robotic middlewares. communication in robot operating system (ros) [12], the mostly popular robotic framework, is peer-to-peer, but this communication is mediated by so called rosmaster. this node provides naming and registration services and enables individual ros nodes to locate one another. once the nodes locate each other, they communicate directly. also ros does not provide routing of messages between inaccessible nodes. on the other side, several works were presented which describe application of mobile ad hoc networks with routing in robotics. witkowski et al. [13] present a cell-based network with master nodes in each cell and routing between distant nodes is provided through these master nodes which are distributed uniformly in the environment. the authors validate the approach on two scenarios. while measuring of the signal quality of wlan and bluetooth communication nodes in indoor environments with different kind of wall materials is the aims of the first one, the second experiment deals with radio-based positioning of robots in a dynamic environment. corell et al. [14] study a wireless coverage problem with minimal requirements to hardware of robots. as a communication middleware they use optimized link state routing (olsr) [15] which provides tcp/ip routing for the resulting mesh network. a suite of algorithms that cover a defined area by a fully distributed robotic team, detect network disconnections, perform network repair, and repair area coverage is presented in [16]. finally, agrawal et. al [17] experimentally evaluate two routing protocols for a robotic swarm. the swarm aims to find a source of heat and a particle swarm optimization algorithm is employed as a search strategy. the aim of this paper is to give an overview of routing protocols in ad hoc networks and choose the most 18 http://dx.doi.org/10.14311/app.2016.6.0018 http://ojs.cvut.cz/ojs/index.php/app vol. 6/2016 framework for ad hoc network communication in multi-robot systems suitable for application in the multi-robot domain. the chosen protocol is than used in a design and realization of the framework for exploration of an a priori unknown environment which thus serves as a testbed for experimental evaluation of the protocol implementation. the rest of the paper is structured as follows. section 2 contains a structured list of requirements for a routing protocol, a classification of protocols, and describes the main representatives of the categories. then a comparative analysis of routing protocols is performed. analysis of three message-oriented middlewares (mom) describes in section 3. the general application architecture and using of selected measures is presented in section 4. section 5 contains results of the experiments, which allow to verify the implementation performance of the proposed architecture. the final evaluation of the paper is in conclusion. 2. ad hoc routing protocols a robot team forms an ad hoc network as it does not rely on a pre-existing infrastructure, while interaction between team members is done by a routing protocol. operation efficient of a distributed robotic system requests a routing protocol to meet certain requirements. the key assumption is fully distributed operations and the protocol should not depend on a central control node. due to high mobility of the nodes, the protocol should easily adapt to changes in network topology caused by movement of nodes. it also needs to be localized, since global exchange of routing information will require large overheads [18]. an important requirement is the absence of routing loops. a routing loop occurs when the packets continue to be routed in an endless circle of the nodes. the protocol should not contain them, otherwise the overall efficiency is reduced, the routing loop will spend more bandwidth and more computing power of each node in this loop. the protocol should take care about saving resources of network members. in addition, the protocol needs to be scalable, this means that its effectiveness should not depend on the number of members in the network. increase or decrease of the network should not affect its performance. it also needs to be adapted to any speed of nodes and any type of their movement. in conditions of high mobility the protocol must be able to quickly recalculate cost and build the path to the destination which will include the lowest number of other nodes. while building the path and forwarding of messages, it is necessary to effectively avoid outdated routes [19]. the rest of the section contains a brief description of few most commonly used routing protocols and their comparison based on the above requirements. the main purpose of this comparison is to select the routing protocol that is the most suitable for teams of mobile robots which establish a wireless mobile ad hoc network (manet) without any centralized structure. the routing protocols can be divided into proactive (table-driven), reactive (on-demand) and hybrid, which combines advantages of the first two categories. 2.1. proactive routing protocols table-driven protocols constantly maintain the relevance of the routes between sources and destinations. to maintain a correct view of the network topology a protocol of this type responds to every change in the structure by sending changes across the entire network. moreover, the protocol periodically sends route update messages to its neighbours. these protocols require to store routing information in one or more tables in each node [20]. these protocols do not scale well and control overheads are proportional to the number of nodes in the network. destination sequenced distance vector (dsdv) [21] is one of table-driven protocols and it is a loop-free modification of the bellmanford routing algorithm [22]. each node maintains a routing table that contains entries for the next hop on the shortest path to all reachable destinations. the protocol uses a sequence number attribute to ensure the freedom of cycles and to distinguish stale routes. dsdv uses two types of dumps with updates of the routing table which sends to all immediate neighbours. the first type is periodically sent full dump which contains all available information about the routing information. the second type is an immediately sent incremental dump which sends on route changes and contains only changes that have occurred since the last full dump. another proactive protocol is optimized link state routing (olsr) [15] protocol, which is based on basic link-state algorithm. every node maintains a network topology graph. each node has thus shorter routes to every destination immediately, when data transmission begins. to keep the relevance of the topology a node periodically floods hello messages about its available links to the others. olsr uses also topology control (tc) messages that contain information about one-hop neighbours. the main optimization lies in using of multipoint relays (mprs). it reduces message overhead, because only nodes which were chosen as mprs forward broadcast messages during the flooding process. 2.2. reactive routing protocols reactive protocols perform the process of route discovery only on request. the source floods the network with route query requests when a packet needs to be routed using distance vector routing or source routing. the problem of reactive protocols is the delay of packet transmission during the route discovery. on the other side, the route is discovered only when needed, i.e., it is generally less memory demanding compared to 19 khilda slyusar, miroslav kulich acta polytechnica ctu proceedings proactive protocols and requires relatively little control traffic overhead. dynamic source routing (dsr) [23] is an example of on-demand routing protocols. dsr supports two types of operations: route discovery, when the node is required to transfer the data to the destination with an unknown route, and route maintenance, that allows to determine that the network topology is changed. after the work of these mechanisms the sender knows the complete hop-by-hop route to the destination. all transmitted routes stored in a route cache decrease time of route discovery. the protocol allows multiple alternative routes to the same destination and allows each node to perform load balancing. another example of reactive protocols is temporally ordered routing algorithm (tora) [24] based on the link-reversal algorithm. tora performs three functions: route creation, when a node uses a height metric to establish a destination oriented directed acyclic graph, route maintenance, when a node reestablishes routes due to topology changes and route erasure, when it is necessary to erase invalid routes. the protocol builds loop-free routes and provides multiple routes to alleviate congestion. however, tora may produce temporary invalid routes, as well as the light-weight mobile routing protocol [25] which it is based on. 2.3. hybrid routing protocols hybrid protocols typically try to reduce delay of route discovery from reactive systems by creating some form of routing tables and reduce control traffic overhead from proactive systems [20]. zone routing protocol (zrp) [26] is a hybrid protocol, which uses a proactive approach to a close neighborhood and a reactive approach to remotely lying nodes of the network. in other words, each node divides the network into intrazone and interzone. the node immediately knows routes to all nodes within the intrazone. the discovery of such paths is produced by the algorithm similar to dsdv. if an initiator needs to send data to a recipient which is in the interzone the sender proactively maintains a route to the destination. this approach reduces latency in route discovery and decreases the number of control messages. ad hoc on-demand distance vector routing (aodv) [27] is also a hybrid protocol based on the principles of the dsdv and dsr protocols. the protocol sends a periodic hello message, maintains the route table with a maximal single route for each destination and uses the principle of sequence numbering, as dsdv routing protocol does. on the other side, aodv provides a similar route discovery procedure as in dsr. a route between nodes is established only if it is necessary to send the data and there is no active route to the destination, i.e., the routing protocol reduces network overhead as compared with the dsdv algorithm. moreover, the route discovery packets do not contain a complete sequence of nodes, that is an advantage compared to dsr. 2.4. comparison of routing protocols there are several criteria [28] for evaluating the performance of a routing protocol: • packet delivery fraction is calculated as the ratio between the number of received messages by the destination to the number of messages sent by the sender; • end-to-end delay is the average time that elapses between the first packet which was transmitted by the sender before the first data packet received by the destination. the metric includes the time of route discovery, transmission delay, queuing delay and propagation delay; • routing overhead is calculated as the ratio between the routing packets to the total number of packets transmitted by the sender; • throughput is the amount of successfully delivered data via a communication link per time. it is usually measured in bits per second. the article [28] discusses three routing protocols dsdv, aodv and dsr. testing is carried out on teams of robots, whose size ranges from 10 to 80 pieces. robots perform a task similar to the task of terrain exploration. each node chooses some point in the terrain and moves toward it. the article considers all four criteria. dsr and aodv show better value of packet delivery fraction than dsdv. the value is about 95% for a team of 10 robots and it tends to 100% with an increase in the team size. aodv shows the smallest value of end-to-end delay. dsdv is a proactive routing protocol, so it shows better results than dsr. the value of routing overhead for aodv is better than dsdv. however, dsr has the smallest routing overhead in comparison with the other two. throughput has the lowest value for proactive dsdv. both dsr and aodv show approximately the same results, but this metric for dsr is slightly higher. a performance comparison of aodv, olsr and zrp is described in [29]. the simulation is conducted for teams of robots with sizes of 25, 50, 75, 100, and provides measurement of all metrics, except the routing overhead. the packet delivery fraction for aodv is approximately 90%, while olsr and zrp have the values of 20-40%. moreover, aodv has the highest throughput, as compared to two other routing protocols. however, aodv shows a significantly larger end-to-end delay than the reactive olsr and the hybrid zrp. the publication [30] compares the performance of dsdv, tora, dsr and aodv. the maximum number of robots in the team in the simulation is 50. the article considers several metrics, which include packet delivery fraction. both dsr and aodv show excellent results for the packet delivery ratio, which 20 vol. 6/2016 framework for ad hoc network communication in multi-robot systems activemq apollo zeromq nanomsg open-source yes yes yes has detailed documentation yes yes only manual pages has new updates yes yes yes point-to-point message passing yes yes yes publish/subscribe message passing yes yes yes written in java c++ c transport protocol tcp, udp tcp, in-proc tcp, in-proc support brokerless model no yes yes complexity of use requires broker without without configuration pre configuration pre configuration table 1. a brief comparison of message oriented middlewares. ranged from 95 to 100% depending on the network load. aodv is selected for implementation of the exploration framework on the basis of the above mentioned comparisons. simulations use robot teams of various sizes and display measurement results that are close to the conditions of the real world. the main advantage of aodv is a high percentage of packet delivery to the destination. the routing protocol has a good throughput compared to the rest. the designed application does not send many unicast messages, so the inflated end-to-end delay and routing overhead are not important. that is, these values are acceptable for the terrain exploration problem. 3. message oriented middleware the exploration application uses message passing to communicate between team members. it is a technique for invoking behavior, which uses incoming messages from other processes to run a code. there are two types of message passing: synchronous and asynchronous. the synchronous approach implies that message exchange takes place at a time when applications are running simultaneously. it uses temporary sender blocking before receiving a response from a recipient and infinitely blocking in case of recipient unavailability. the robots move in the environment during the exploration problem solving and can get out of the communication range. in addition, the robot can be turned off, for example, due to the battery discharge. in such cases, the message sender is blocked. that is, synchronous approaches are not suitable for use in distributed robotic systems that solve exploration problem. the asynchronous approach does not require simultaneous operation of a sender and a recipient. the intermediate level of software provides all the operations for receiving, storing and sending of messages. the most known type of such software is messageoriented middleware (mom). table 1 provides a brief comparison of main parameters of these three widely used asynchronous message-oriented middlewares: activemq apollo [31], zeromq [32] and nanomsg [33]. as can be seen from the table, all three libraries are open-source and release new updates. the first two libraries are well documented and have a large community of users. the latter is improved and rewritten zeromq library, which currently has only the manual pages, but the number of nanomsg users is constantly growing. all considered libraries support binding for commonly used programming languages as java, c, c# and c++. zeromq and nanomsg have also bindings for ruby, go, haskell, perl, php and others. there are two main functionalities of moms: message queuing and publish/subscribe. the first approach is a point-to-point messaging model, that is, a message is sent from a sender to a recipient. publish/subscribe approach is a many-to-many messaging model. all three libraries include both types of message passing. the libraries support a wide range of transport protocols, but transmission control protocol (tcp), user datagram protocol (udp) and in-proc are relevant for the purposes of the application. all considered libraries support transfer of data over tcp. activemq apollo additionally supports udp, while the other two do not support it. zeromq and nanomsg can use in-proc transport protocol. it is an inter-thread transport, which is much faster than tcp and can transfer data between threads of a single application. the most important difference is that the basic principle of activemq apollo is to create and configure a broker. a distributed multi-robot system has no central node, which could be a broker. a possible solution is creation of a broker at each node of the network. however, this solution is cumbersome and requires excessive pre-configuration of brokers. contrariwise, 21 khilda slyusar, miroslav kulich acta polytechnica ctu proceedings zeromq and nanomsg support brokerless model. nanomsg library was developed by one of the key creators of the zeromq library and it fixes most of the zeromq drawbacks. the main one is the problem with fault tolerance. nanomsg provides a new pattern of communication that does not require redundant confirmation from a recipient in the model requestrouter that resembles the work of procedure calls. the library allows to set a timeout for an operation of sending messages. it allows to refuse the message sending, if it is not sent for some predetermined amount of time. on the contrary, zeromq does not provide the possibility to obtain information about the current status of the recipient before sending a message. moreover, the library does not allow to set a timeout on an attempt to send a message. thus, in case of a fall, the whole system of robots gradually stops because of waiting a response from each other. the nanomsg library was chosen for use in the application on the basis of the above comparison of the characteristics of the libraries. because the library doesn’t provide an implementation of udp, the transport protocol is proposed to implement using standard sockets. 4. distributed exploration exploration as a process of autonomous navigation of a mobile robot in order to build a model of an a priori unknown working environment in a shortest possible time is one of the fundamental problems in mobile robotics. in general, exploration is an iterative process that performs the following operations at each step: the robot receives information from its sensors, updates an internal model of the surrounding space on the basis of these data, selects the next goal for the navigation on the basis of the current knowledge, and gradually moves to the selected destination. the process continues until there are no more available goals, that is, all areas of the environment will be explored [34, 35]. the main source of optimization is preparation of a set of possible goals and selection of a next goal from them, which is the most favorable for exploration purposes. besides the tasks mentioned above, the problem of distributed terrain exploration by a multi-robot team requires solving the problem of communication between team members and the problem of coordination their actions. this is why we selected this task as a testbed for evaluation of the aodv routing protocol. information about the terrain which is exchanged between team members and the method of determining the set of possible navigation goals depends on an exploration approach that is selected for implementation. frontier-based exploration [34] is chosen as one of the most common and widely used approaches which also has the extension for the case of multi-robot exploration [36]. the approach is based on the concept of a frontier, which is a boundary between the already known part of the terrain and still an unknown part. the internal representation of the map is an occupancy grid, which uses bayesian based updating technique. the main advantage of the environment exploration by a multi-robot team is the ability to easily share knowledge about the terrain between its members. exploration of non-overlapping areas by different robots allows to raise efficiency of teamwork and reduce the total exploration time. each robot in the team conducts the current goal selection independently on the basis of its current knowledge of the environment and the goals of the other team members. a greedy algorithm is chosen as the most primitive and native approach. it means, that the closest frontier to the current position of the robot is selected as the goal. in addition, the selected goal should not lie in the areas of the current goals of the other team members, which have active communication link to the robot. after the goal selection the robot informs the others about the selected goal and reports the priority for this goal. if an other team member has the goal in the same area with a higher priority, it sends information about its current goal and forces the robot with a lower priority to choose another goal and generate a new plan. description of the software architecture of a single robot performing distributed exploration and communicating with other robots making use of aodv follows in the next paragraphs. while designing the application structure for a single robot it was assumed that the application can operate in two roles: robot and display. the application for a robot role controls a robot as it carries out reading of data from its sensors, produces the robot movement in the terrain, performs path planning and communication with other team members. the application for a display role is used to monitor and display the status of the multi-robot exploration process and can vary from the specific implementation. the application of this type is also a part of the mesh network, but it does not directly participate in the exploration. figure 1. proposed application structure. it is recommended to use aodv routing protocol based on the analysis result of routing protocols 22 vol. 6/2016 framework for ad hoc network communication in multi-robot systems from section 2. the application should have the tools to unicast and broadcast messages for aodv implementation. tcp is the most appropriate protocol for the purposes of sending messages between robots. flooding and sending hello messages can be realised with using less reliable udp, which however supports broadcasting. according to the results of a comparative analysis in section 3 nanomsg recommended for implementation as a mom. thus, the nanomsg library provides the transfer of messages between robots via tcp and uses in-proc for transfer of information between different parts within the application itself. because this library does not support the udp, broadcasting should be implemented by means of language in which the application will be realized. fig. 1 shows the proposed general structure of the application, and describes the relationship between it and the external environment. application operations have different frequency of launching and some of them can be called asynchronously. e.g., plan generation usually runs once per two seconds or on the request from the other robot. a command to control robot movement can be sent every 100 milliseconds. the optimal frequency of sending the heartbeat for the purposes of aodv is 1 second. moreover, it is desirable to receive messages from the other robots instantly. message sending is also necessary to make immediately to reduce the overall time of the terrain exploration. this means that the designed application could not be structured in a single loop. for these reasons, the structure is divided into 5 logical parts, which can be implemented as threads: motion control/visualization, path planning, timer, message processing and inbox messages part. these parts of the application share three data structures: map, current plan and scans archive. map keeps an internal representation of the application’s view about the environment and depends on the selected type of the exploration. in the case of frontier-based exploration, the map will be in the form of the occupancy grid. current plan is the path to a goal selected at this iteration of the exploration process in the form of a polyline. scans archive is a data structure that contains scans received from sensors of any robot of the team. that is, the structure stores local maps created by the robot and local maps created by other robots and transmitted via flooding. the principle of the transfer of local maps between robots during the terrain exploration of a multi-robot team is described in [36]. the application for a robot role is determined by using the motion control thread. it is responsible for receiving the current plan, sending signals to the robot motors for movement to the next selected goal, using the robot sensors to obtain scans, which are then stored in the scans archive and receiving new scans from the scans archive received from other robots. finally, the thread conducts a map update on the basis of these data. if the application is launched for the purpose of visualization of the exploration process, it uses a visualization thread. the application of this type does not create its own scans, so the scans archive contains only local maps received from the robots. this thread uses them to update the map, which is displayed on the screen after that. the path planning thread is the main component of each iteration of the terrain exploration process. this thread selects the next goal for the motion and makes the path to it. this plan is written to the shared structure. the thread uses the map to plan. the application uses a timer to generate the plan after a certain predetermined period. the timer is located in the timer thread. the message processing thread is the main connection between the robot and the rest of the team. it is responsible for sending messages to other robots about a new generated path or a new laser scan. it also receives messages from the inbox messages thread. the inbox messages thread deals with receiving messages from other team members and sending them in the messages processing thread. 5. experimental results for functional testing of the proposed framework, the application of a multi-robot team member was implemented. it is implemented in c++ and simulates the work of an exploration robot for experimental verification of the effectiveness of the proposed application structure. it imitates operations of the real robot equipped with a laser range-finder. the robots are controlled by a simple controller which guides the robot exactly along a planned path with a constant speed. ray casting was used to simulated a laser range-finder with no noise incorporated. behavior and properties of the implemented application were experimentally evaluated and its characteristics were compared with a single-robot exploration. the experiments were conducted using a device which has 32 central processing units (cpu) and has 8 gb of memory. all tests were performed in simulation on the map of an empty terrain that has a size of 20 by 20 meters. each cell of the occupancy grid has a size of 5 by 5 centimeters. it means that the occupancy grid has a size of 400 by 400 cells. various numbers of robots in the team are used to test the loading of the network. the team size is varied from one to ten. the application makes the terrain exploration as a single robot, if the team consists only of one robot. various ranges of communication links are used to test the effectiveness of teamwork. the communication range takes one of the values: 5, 10, 15 or 20 meters. the laser has a range of 1.5 or 2 meters. it allows to verify the functionalities performance with a larger number of steps of the exploration process on the same map. the experiments were performed three times for each system configuration. 23 khilda slyusar, miroslav kulich acta polytechnica ctu proceedings (a). (b). figure 2. dependence of the steps on the team size. the value of the laser range is: (a) 2 meters; (b) 1.5 meters. the time measurement of the exploration is made in steps, i.e the number of calls of the function that changes the robot position. this function is triggered periodically after a certain period of time. thus, a step is a convenient alternative to time. in addition, the usage of steps metric allows to maintain usable statistics of events that pass between sequential steps. 5.1. time of the exploration fig. 2 shows the dependence of the average exploration time for a team member on the number of robots in the team. the graph shows that any team work helps to reduce exploration time. in the beginning, both graphs show a reduction of the number of steps, then there is an increase in steps quantity. this is due to the fact that the robots have to excessively agree on the choice of a goal in bigger teams. as can be seen from fig. 3, a small team disperses at the beginning of the exploration and explores non-overlapping areas of the terrain. however, an excessive number of robots in the team causes the problem of determination of the non-overlapping areas. so robots are required to negotiate the rescheduling of their goals. the graph also shows that the decrease in the communication range increases the number of steps that are required to complete the terrain exploration. some scans from the other robots could not reach the robot because of lack of communication link due to the small value of the communication range. that is, the robot is forced to explore the given area by itself. it increases the overall time of the exploration. comparison of fig. 2(a) and fig. 2(b) shows that the ratio of the steps number and the team size remains constant regardless of the laser range. however, reducing the value of laser range increases the total number of steps. if the laser has a shorter range, then each scan provides less information about the environment. thus, it is necessary to make larger movements (a). (b). (c). (d). (e). (f). figure 3. the resulting paths after the exploration. the laser range of the first column is 2 meters, the second column is 1.5 meters. rows are separated by team size: (a)+(b) 1 robot; (c)+(d) 2 robots; (e)+(f) 5 robots. 24 vol. 6/2016 framework for ad hoc network communication in multi-robot systems and get more scans to obtain a complete map of the terrain. 5.2. plan generations fig. 4 shows the frequency with which the application is launching a new request for a new generation of the plan. a plan generation runs periodically by a timer part of the application, as described in section 4. in addition, it can be run by a request from an another team member. in this implementation, if two robots have the goal at the same area, the robot with a higher priority of the goal sends a request to the robot with a lower priority to select a new navigation goal and generate a plan to the selected goal. the launching frequency of generation of the plan is 20 steps in the application. the graphs shown on fig. 4 contain all plan generations, which had one member of the robot team during complete exploration of the environment. thus, all function values under the value of 20 steps means that the corresponding plan generation is launched on request from an another robot. fig. 4(a) shows that a single robot starts a process of path generation by approximately the same intervals. the increase of the team size leads to the fact that robots can compete for the goals in a particular region of the terrain. this can have both positive and negative effects. let’s consider the situation of the terrain exploration by a team that consists of ten robots and the communication range is 20 meters. this means that all robots agree on the choice of goals with the other robots. the first low part of the graph shown in fig. 4(d) corresponds to fig. 5(a). the robots start the goal selection. however, the current implementation of the goal choice requires to select the goal that does not lie close to the goals of other team members. this means that the distance between the selected goal and goal of another robot should be greater than the laser range. an example of such area is depicted in fig. 5(a) as the yellow circle. if each robot chooses a goal which does not overlap with the goals of the other robots, the plan generation is invoked periodically by the timer thread. that is, the robot does not encounter other robots and it made the right goal choice. the straight part of the plot with a step value, which is equal to 20, corresponds to fig. 5(b). then, most of the terrain is explored and the robots are in a small unexplored part of the environment (see fig. 5(c)). the weak point of the implemented simple prioritizing between the robots appears. at this point, the frequency of plan generation begins to increase. moreover, increasing the number of plan generations leads to increase in the number of steps that are necessary to complete the terrain exploration. it then leads to increase of the total exploration time. 6. conclusion this paper addresses the problem of communication in distributed multi-robot teams forming a mobile ad hoc network. a list of requirements for a routing protocol was drawn up. the comparative analysis of routing protocols has shown that aodv routing protocol is most suitable. in addition, the analysis of three moms was conducted and the nanomsg library was chosen as the most suitable for implementation. multi-robot exploration has been selected as a proofof-concept task. the general structure of the robot application which carries out exploration of an unknown environment in a multi-robot team and which communicates with other robots employing aodv has been proposed. to verify the proposed architecture and offered tools the application has been implemented and has been tested by series of experiments. thus, the paper describes the architecture of the application and possible means of implementation in a generalized form. the specific implementation can be done for different systems and written on a wide range of languages. in future, this application will be used for testing on the group of real robots that solves the problem of the exploration of an unknown environment. goal allocation was not addressed in the paper as it was out of scope of it. analysis and comparison of a variety of sophisticated goal allocation mechanisms will be another stream we would like to go in future. acknowledgements this work has been supported by the technology agency of the czech republic under the project no. te01020197 “centre for applied cybernetics”. access to computing and storage facilities owned by parties and projects contributing to the national grid infrastructure metacentrum, provided under the programme “projects of large infrastructure for research, development, and innovations” (lm2010005), is greatly appreciated. references [1] w. zhigang, l. liu, m. zhou. protocols and applications of ad-hoc robot 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2016 1 introduction 2 ad hoc routing protocols 2.1 proactive routing protocols 2.2 reactive routing protocols 2.3 hybrid routing protocols 2.4 comparison of routing protocols 3 message oriented middleware 4 distributed exploration 5 experimental results 5.1 time of the exploration 5.2 plan generations 6 conclusion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2016.5.0063 acta polytechnica ctu proceedings 5:63–68, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app monitoring of track sections with long-pitch corrugation jan valehrach∗, jaroslav šmíd brno university of technology, faculty of civil engineering, institute of railway structures and constructions, veveří 331/95, 60200 brno, czech republic ∗ corresponding author: valehrach@fce.vutbr.cz abstract. the focus of this paper lies on monitoring of the track sections with rail corrugations caused by wheel sliding. short waves on the running surface of the rail head on low rail are typical for this defect. long-pitch corrugation is a significant cause of vibration and noise pollution in the railway infrastructure. therefore it is very important to understand the formation and development of this imperfection of the rails. measurements were carried out in curves of small radii on several tracks in the czech republic. in addition to the measurement of the surface of the rail head a number of supplementary parameters was evaluated for each section, such as curve radius, superelevation, track gauge etc. and the speed of passing trains as well. this paper describes rail corrugation defect and its development. our early results are presented in the conclusions. keywords: long-pitch corrugation, rail, track, measurement, speed . 1. introduction during the past recent time the railway infrastructure administrators are pushed to change their approach to the maintenance of the sections affected by the long pitch corrugation. these defects were not as frequent as they are in these days and also some of them have not been considered as a serious problem for the operability of the track. there are more factors to blame, such as increases of the track speeds, higher track loads or also (predominantly in the close vicinity of the cities) higher frequency of the passenger trains. in addition, today’s customers are not only satisfied with just the travel from point a to b or with the shortest time of transfer. they also require more comfortable travelling. it is not very difficult to notice the imperfections of the track or the increased noise levels. and there is also the second aspect of the problem, which some say is even more important – that is the influence of the imperfections for the adjacent neighborhood, such as vibrations, noise and quakes, all significantly reducing the quality of life of the people living near tracks. there is no doubt about the negative effects of the long-pitch corrugation. everyone is able to recognize that the train is much louder when passing through the curve degraded by corrugations in comparison with the passage of the same curve after the replacement of the rails. the tracks with the long-pitch corrugation require more frequent and also more costly maintenance (such as rail grinding, replacement of the rails etc.). in order to fulfil interoperable function within europe the railway network has ”to ensure a safe and uninterrupted operation of trains achieving set levels of performance” [1]. accordingly, it is necessary to guarantee required quality of the railway infrastructure and to reduce maintenance cost to minimum. with the above mentioned reasons in mind we should endavour to understand the formation and development of this defect. 2. theory of formation of long-pitch corrugation the long-pitch corrugation, sometimes called also as ”short waves”, is a sinuous inequality of the running surface of the rail. distance between wave peaks is usually between 8 and 30 cm and the depth ranges between 0.1 and 1.2 mm. a typical location, where long-pitch corrugation could be found, is the lower rail in curves of radius less than 600 m, sometimes even 700 m [2, 3]. the cause of these corrugations is the difference in length that each wheel of the wheelset rolls along the curve on the low and high rail. this difference also causes the wheel slip, occurring mostly on the low rail. slip happens not only in the longitudinal direction, but also in the lateral direction. in most cases, long-pitch corrugation does not occur alone. such defects, which are accompanying the long-pitch corrugation, can be sorted to: • those supporting the development of long-pitch corrugation (such as side wear of the outer rail), • those emerging as a consequence of long-pitch corrugation (cracked clips). since the processes surrounding the long-pitch corrugation are not documented in their entirety it is often complicated to distinguish which defect is the cause and which is the consequence. therefore, the consecuting list of defects does not take into account the above mentioned division: damaged baseplates, sleepers with transverse cracks, missing parts of fastening, cracked sleeper screws, cracked clamps in rail 63 http://dx.doi.org/10.14311/app.2016.5.0063 http://ojs.cvut.cz/ojs/index.php/app jan valehrach, jaroslav šmíd acta polytechnica ctu proceedings figure 1. long-pitch corrugation in havlíčkův brod fastening, abraded ballast behind sleeper heads etc. 3. selection of locations and measurement appropriate sections for the monitoring of long-pitch corrugation, where typical signs of this defect occur, were chosen in association with the railway infrastructure administration of the czech republic (sždc). further criteria which have influenced the selection of sections originated from the identical or at least similar characteristics and features of curves, such as: • curve radius, • track cant, • traffic load and others. subsequently, an assessment of the available data for all the individual sections was conducted. the frequency of measuring was determined with consideration to previous maintenance work, rail traffic present and planned intentions of the sždc as well. the majority of sections are double tracks thus it is possible to compare two monitored locations on one track or one location on each track, for example in a measured curve. to be able to understand more thoroughly the development of the long-pitch corrugation it is also necessary to observe other factors, which influence the defect. one of these factors is the matter of variety composition of the trains (meaning the split up between passenger trains and freight trains). variety composition of the trains complicates the whole matter, since it adds more other unknown influences. that is the reason, why we try to rule this factor out if possible. it is less difficult to succeed when considering the case with one track; hence it is more likely that the track would be passed in both directions equally. this also allows us to compare two sections within one location between themselves. on the other hand, in the case of the double track there is no certainty that both tracks would be passed with the same amount of trains or even with the same rate between the passenger and freight traffic. as an example, in some cases we can distinguish the acceleration of trains in one track and deceleration or even stopping of trains in the second track (like when approaching an entry signal of railway station). that is why it is not possible to perform comparison between the sections in different tracks within one measuring location. in both cases the monitored sections are chosen by the presume of the influence on formation and development of long-pitch corrugation, by the track alignment, by the permanent way design itself (composition of the superstructure including the effects of tested design elements such as more elastic fastening to the sleepers, clips with increased fatigue limits, under sleeper pads) and by the substructure design (e.g. the influence of the bedrock, bridge structure etc.). the sections are monitored in regular intervals depending on the present state of development of defects, traffic volume, maintenance and repair works etc. the sections with recently replaced rails allow us to observe the formation and development of long-pitch corrugation in its initial stages. measurements were repeated after 3 months. in sections, where the defects are more developed, the time between the measurements was almost doubled, since the corrugations are more noticeable (deeper and significantly better visible). that allows us to measure each wave separately. on the other hand, the measurements in sections, where defects are not yet fully developed should be performed with increased frequency, so it is easier to cover the whole development process. as you can see on figure 2, the long-pitch corrugation forms very interesting shapes which are changing fluently throughout the curve. apart from the visual inspection (which confirmed the suitability of our selected locations) all of the sections are monitored and documented using the following methods: • visual inspection and photo documentation, • measurement of track geometry by the trolley krab, • measurement of wavy deformations of the rail head by the device salamander, 64 vol. 5/2016 monitoring of track sections with long-pitch corrugation figure 2. highlighted long-pitch corrugation by contaminant in havlíčkův brod • monitoring of the speed of trains and train compositions. the track geometry is measured to describe the current state of the track, which unfortunately in many cases does not correspond to the data found in the railway documentation. another reason for these measurements is the need for additional information such as track gauge, gauge widening etc. the microgeometry of the rail head, specifically wavy deformations, was measured using the device salamander. unfortunately, in some cases it was not technically possible to measure a curve as a whole, which is the reason, why only few selected sections were measured within these locations. measured data are evaluated by the device in accordance with en 13231-3 [4] in wave lengths: • 10 ÷ 30 mm, • 30 ÷ 100 mm, • 100 ÷ 300 mm, • 300 ÷ 1000 mm. this categorization is not fully appropriate for our purposes since long-pitch corrugation can appear with a wave length shorter than 100 mm [3], particularly in small radius curves. based on the theory of formation of long-pitch corrugation [6] , our own measurements and data comparison, it can be said that the two categories for 30 ÷ 100 mm and 100 ÷ 300 mm wave lengths can be merged together for the purposes of figure 3. trolley krab (track geometry) [5] and salamander (corrugations) monitoring long-pitch corrugation. in both zones, the same or very similar wave amplitudes are achieved. apart from the monitoring of the long-pitch corrugation of the rail head, other critical elements were evaluated as important and thus were observed: • compliance with technology of construction and maintenance works, • compliance with technology of works in stations, • composition of passing trains, • operation of rail vehicles with respect to the track speed. during the measurements, the influence of the difference between the track allowed speed and actual speed of the vehicles proved to be imperative. that is the reason for closer observation of the traffic with respect to the measured speed of trains. in some cases the track allowed speed, or sometimes cogitated as a designed speed, differs significantly from the actual speed of the vehicles. this phenomenon occurs more often these days, since there is an effort of the track designers to maximize the speed limits as much as possible (they tend to ”squeeze out” the most of the infrastructure) and mostly could be found on tracks with very heterogeneous traffic flow, consisting of the various ratios of the passenger and freight trains. the more freight trains pass throughout the section of the track, the bigger is usually the difference. generally, the difference between the allowed and actual speed produces a cant excess or cant deficiency. analogically, these values grow parallelly to the difference, so when the difference increases, the values increase accordingly. therefore, a weighted average of all speed measurements in a set section was calculated, when the mass of each train was taken into consideration. the masses of the trains for the purposes of the weighted averages have been obtained by two ways. the weight of passenger trains was taken from the passenger carriages charts and from the database of the train compositions. the mass of the freight trains could be found out from the mass normatives (which is the maximum allowable mass of the whole train). the problem is that the actual load on the train is not known and thus it is not possible to know the right mass of the train. therefore the masses of the freight trains were estimated with only one value around 1000 tonnes. this approach brings the significant amount 65 jan valehrach, jaroslav šmíd acta polytechnica ctu proceedings figure 4. the processed record from the device salamander shows a track, where in one part the rails were replaced and in the other part the rails with long-pitch corrugation were left. of uncertainty to the result, but on the other hand, according to higher order masses of the freight trains in comparison to the passenger trains, the sensitivity of the result to the changes of the masses is quite small. then for the calculation of the cant excess and the cant deficiency the following scheme was used. assuming a formula for speed of trains v = √ d ∗ r 11, 8 the cant excess then applies e = d − 11, 8 ∗ v 2 r and analogically for the cant deficiency i = 11, 8 ∗ v 2 r − d ideally, the effects of cant excess and deficiency should be balanced, especially with respect to train masses. however, in some sections cant excess markedly dominates. that happens for example in the vicinity of stations, where the trains are accelerating and have not yet reached the track speed or where the greatest amount of the track load consists of slow moving trains (usually freight trains). in such locations this leads to the overload of the railway superstructure and consequently results in increased occurrence probability of the defects. figure 5. cant in track no. 1 and in track no. 2 in curve a. 4. outputs 4.1. measuring location havlíčkův brod one of the monitored track locations is a part of the track no. 324 havlíčkův brod – kutná hora in between the km 224.394 and km 225.150 in approach to the station havlickuv brod from the direction kutna hora. the location consists of a double track with consecuting reverse compound curves. first curve is for the purposes of this work named a and is closer to the station. the second curve is named b and is located further from the station in direction kutná hora. the cant of the track was measured, using the device krab, which showed a different value of the cant for each track. the results of the train speed measurements were the differing speeds of trains in both tracks and both curves. after the calculation of the weighted averages, the data revealed the presence of cant excess in both tracks and both curves. the train speed in the curve a in the track no. 1 is affected by braking/accelerating near havlíčkův brod station. some freight trains heading from kutná hora stopped at the station head in such a way that the end of the train was standing in the curve (e = 2 mm). unfortunately, this situation is a common practice in havlickuv brod. it facilitates the document handover by the stopping of the locomotive just in front of the station building. the data proved that both rails are nearly under the same load, since the weighted average e/i was close to zero. the record of the wavy deformations for wave lengths 100 ÷ 300 mm is shown on figure 6 on the first line. for the curve a on track no. 2 the weighted average equals e = 27 mm. when comparing with the track no. 1 the wavy deformations reach the amplitudes twice as high (figure 6, second line). on the contrary the cant excess markedly dominates in the curve b in comparison to the curve a. the weighted average the curve b equals e = 57 mm. the state of microgeometry as shown on figure 6 (fourth line) is practically identical to the curve a of this track. the track no. 1 of the curve b is passed with almost all trains with an cant excess (e = 72 mm) since they have to reduce the speed according to a change of allowed speed between the curves. in the past, the railway infrastructure administrator tried to improve the situation by reducing the allowable 66 vol. 5/2016 monitoring of track sections with long-pitch corrugation figure 6. category of wavelengths 100 ãů 300 mm havlickuv brod (from the top: curve a of the first track, curve a of the second track, curve b of the first track and curve b of the second track). speed to 55 kph, nevertheless this action had an adverse effect. instead of going at 70 kph, the trains are decelerating to 55 kph already during the passage through the curve b. additionally; the freight trains which are approaching the station and intended to pass through the first turnout in the side direction have to be slowed down just before the pass of the entry signal at 40 kph, which is located in the middle of the curve b. this forces such trains to travel with the reduced speed for more than 500 metres before the station. the designed cant in the curve b of 142 mm is from that reason unnecessarily large and corresponds to the recommended cant dn1 for speed 75 kph (recommended cant is the value of the cant prescribed by the standard csn 73 6360-1 [7]). the allowable speed in this curve is on the other hand only 70 kph and moreover the speed, which is achievable realistically is even less – just 55 kph. surprisingly, the wavy deformation of microgeometry is less developed in this section in comparison to other measured sections (as it could be seen on the figure 6 (third line)). one of the possible explanations of this phenomenon may be the usage of the under sleeper pads, which were installed in this curve and only in the track no. 1. according to [8], it is possible to install under sleeper pads to affect the behaviour of sleepers in a desired zone of the frequency spectrum. this is the way how it is possible to suppress the generation of vibrations and noise emissions in these frequencies. part of the energy of dynamic processes is emitted from vibrating sleepers as noise. for newly built track with under sleeper pads an increased level of noise was measured (in just units db). such a track shows over time slower development of imperfections of the rail heads. as a consequence, the noise levels for these tracks are lower than for comparable tracks without under sleeper pads. for this reason, not only the noise pollution, but also other parameters, such as vibration parameters, sleeper and rail movements and development of irregularities of the rail head are monitored on the test sections in the czech republic. the railway superstructure in the location havlickuv brod consists of the rails 49 e1, fastenings e40 with clamps e14 in the curve a and skl40 in the curve b, then sleepers b 91s/1 on both tracks. the difference between used fastening systems could not be considered as a cause of the change in the defects, since the replacement of the fastening system was the result of the development of the defects and should have been the resolution of the problem. the long-pitch corrugation was found on both tracks. additionally, massive cracking of clamps skl14 occurs in the curve b. it is surmised that high value of the weighted average of cant excess contributes to defects of the clamps. despite of the fact that the above mentioned data indicated that higher values of cant excess have the most adverse effect on microgeometry, the slowest development of the long-pitch corrugation occurred in the curve b in track no. 1. 4.2. measuring location hady the monitored location hady is the opposite to the location havlíčkův brod in the means of the unequal cant excess. in this location the cant deficiency plays the main role. this section could be found on the track from brno to česká třebová between km 161.685 and km 164.485. during the year 2015 the rails of the track no. 1 have been replaced and the development of the long-pitch corrugation thus could be observed and measured since the time zero i. e. from the perfect condition. the measuring location consists of two sections, first is located in front of the tunnel a (curve a), the second is located in front of the tunnel b (curve b). both monitored sections lay only in the track no. 1, but the line is double track. the usual direction of the passing trains in the track no. 1 is from the tunnel b to the tunnel a, which is the heading from česká třebová to brno. figure 7 shows the comparison of development speeds of wavy deformations (here represented as a percentage of the boundary overrun of the rms limit value, rms = root mean square) in both curves in location hady. initial analyses of the data show significant differences in development of the long-pitch corrugation in the curves with small radii. considering the common structure and geometrical parameters of the track (curve radii 283 m and 261 m, cant 123 mm in both curves, fastening w14, sleepers b 91s etc.) and the railway superstructure they do not exhibit significant differences. the curve b (in front of the tunnel b) embodies the weighted cant deficiency i = 67 mm. the curve a (in front of the 67 jan valehrach, jaroslav šmíd acta polytechnica ctu proceedings figure 7. comparison of rms values [%] (to the left the measuring point in front of the tunnel a and to the right the measuring point in front of the tunnel b in location hady. tunnel a) shows the weighted cant deficiency i = 47 mm. unfortunately, these values have to be considered as tentative, since the train speeds were affected by the day time in which the measuring took place. the majority of the recorded trains were passenger trains; the freight trains pass this location mostly at nights due to very strong suburban traffic. also it has to be pointed out, that the track configuration is similar to that in the location havlíčkův brod (namely the curve a of the track no. 1). there is a turnout located just behind the measuring location and freight trains approach the station through the side direction of the turnout at 60 kph at maximum. passenger trains pass the turnout in straight direction at speeds up to 70 kph ( or up to 75 kph for trains using the cant deficiency 130 mm). when we take into consideration that the measured train speeds were just tentative, the calculation offers results, in which the values for cant deficiency are logically lower (for the section in front of the first tunnel). this partial conclusion shall be confirmed or refused as soon as possible. 5. conclusions various parameters were monitored on the two measuring locations. in the every curve there could be found a different combination of factors affecting the development speed of the long-pitch corrugation and in some curves a different track parameter can be the dominant factor. nevertheless, it can be declared at the present time and based on our measurements and observations, that the speed of passing trains undoubtedly plays the significant role on the development of defects. the adverse effect of the speed occurs in two forms: • the higher the value of the speed, the more significant the development of the defect, • the higher the value of the cant inequity occurs, the more significant is the defect. at the current state of the research it might be said that the higher the speed or the bigger the difference between the actual speed of the vehicle and the designed track speed, the faster and greater the development of the defects. the curve radius has to be considered as a fixed parameter at all times, since its change in order to reduce the development of the long-pitch corrugation is in most cases nearly impossible, we have to focus on another parameters. the composition of the railway superstructure and setting of the appropriate speeds of trains and also appropriate cant values seem to be promising factors. whether these parameters alone would be sufficient the following research will show. acknowledgements the presented results were obtained with the support of centre for effective and sustainable transport infrastructure (te01020168), student’s grant tender of the faculty of the civil engineering of the brno university of technology (fast-j-15-2860) and railway infrastructure administration, state organization (szdc s. o.). references [1] r. čech. interoperabilita a rozvoj ždc [online], 2015. [2016-02-11], https://www.fd.cvut.cz/personal/ tyfal/str/predmety/ikod-pr/ikod10.pdf. [2] c. esveld. modern railway track. 2nd ed. zaltbommel: mrt-productions, 2001. doi:isbn 90-800-3243-3. [3] h. funke. broušení kolejnic, 1992. [4] en 13231-3. railway applications track acceptance part 3: acceptance of reprofilling rails in track, 2012. [5] s. s. r. kžv. krab system [online]. [2015-12-26], http://kzv.cz/english/krab.php. [6] j. valehrach. skluzové vlny teorie a praxe, 2015. doi:isbn 978-80-214-5091-2. [7] čsn 73 6360-1. konstrukční a geometrické uspořádání koleje železničních drah a její prostorová poloha část 1: projektování, 2008. [8] plášek o., hruzíková m. přínos podpražcových podložek ke zvyšování kvality geometrických parametrů koleje, in zborník prednášok z konferencie s mezinárodnou úcastou pozemné komunikácie a dráhy, environmentálna kapacita pozemných komunikacií a dráh. košice, technická univerzita v košiciach, 2006. isbn 80-8073-602-2. 68 https://www.fd.cvut.cz/personal/tyfal/str/predmety/ikod-pr/ikod10.pdf https://www.fd.cvut.cz/personal/tyfal/str/predmety/ikod-pr/ikod10.pdf http://dx.doi.org/{isbn} 90-800-3243-3 http://kzv.cz/english/krab.php http://dx.doi.org/{isbn} 978-80-214-5091-2 acta polytechnica ctu proceedings 5:63–68, 2016 1 introduction 2 theory of formation of long-pitch corrugation 3 selection of locations and measurement 4 outputs 4.1 measuring location havlíckuv brod 4.2 measuring location hady 5 conclusions acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0079 acta polytechnica ctu proceedings 7:79–84, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app design of concrete chimneys via beam theory and nonlinear shell analysis franziska wehr∗, reinhard harte university of wuppertal, pauluskirchstr. 7, 42285 wuppertal, germany ∗ corresponding author: fwehr@uni-wuppertal.de abstract. this paper compares the load-bearing capacity of chimneys calculated via beam and shell theory. it becomes apparent that the design via beam theory is on the safe side for the vertical reinforcement of the chosen examples for h/d ratios larger than 30. for non-slender chimneys the design via beam theory overestimates the load distribution around the circumference and yields to wrong results. on the other hand a linear elastic shell calculation underestimates the load-bearing capacity of the chimney. however a realistic distribution of stresses in the cross section of a chimney can still be calculated using shell theory with nonlinear material properties. keywords: nonlinear, shell, reinforced concrete, chimney, material nonlinear. 1. introduction chimneys are one of the main components of thermal power plants. in design of industrial concrete chimneys the structural integrity is characterized by the ultimate limit resistance against wind action and the serviceability limit resistance against constraints caused by thermal effects. detailed investigations on damaged chimneys [1] have shown that mechanical actions like wind load are not the only reason for the observed crack patterns. these actions have to be accompanied by constraints due to thermal effects. 2. design of concrete chimneys via beam theory currently the design of concrete chimneys is regulated in codes such as the international cicind model code for concrete chimneys [2], the en 13084 – freestanding chimneys [3, 4] for europe and the aci 307-08 – code requirements for reinforced concrete chimneys [5] for the usa. a comprehensive comparison of the three codes can be found in [6]. all codes have in common that the design is performed via beam theory. a model of the whole chimney with a vertical beam and a circular cross section is used for the design of the vertical reinforcement and another model with a circular beam and a rectangular cross section for the design of the hoop reinforcement (fig. 1). this paper focuses on the ultimate limit state (uls) design according to cicind model code and the european standard en 13084 for the vertical reinforcement. for the vertical reinforcement only mechanical impacts have to be considered. this means that usually only dead loads g, wind w , seismic actions e, rotations of the foundation and second order effects need to be applied. according to [2] a temperature drop in the wall may be neglected if it is less than 60 k. table 1 shows the load combinations for uls design according to [2] and [4]. figure 1. design of concrete chimneys via two beam models (source: [2], modified) typical material properties for concrete (for example c30/37) and reinforcement (for example b500b) for the uls design are shown in fig. 2. the material properties listed in en 13084 [4] are referring to the eurocode [7, 8]. the diagrammed stresses in fig. 2 are already reduced by a safety factor γ and have to be looked upon as design values. the stress-strain-curve for concrete is identical for both considered standards, but the strain limit according to [2] is reduced to 3 ‰ instead of 3.5 ‰ according to [4]. both standards allow only compressive stresses for concrete in uls design. the stress-strain-curve for steel is defined to be symmetric for the compressive and tensile stresses in both codes. the steel-curves are identical up to a strain of 10 ‰. 79 http://dx.doi.org/10.14311/app.2017.7.0079 http://ojs.cvut.cz/ojs/index.php/app franziska wehr, reinhard harte acta polytechnica ctu proceedings verification leading combination of actions combination of actions action acc. to cicind [2] acc. to en 13084 [4] vertical strength inline 1.0g+ 1.6w + 1.0t 1.0g+ 1.5w + 1.0t wind combined vertical cross 1.0g+ 1.5wcross + 1.2w + 1.0t 1.0g+ 1.5wcross + 1.5w + 1.0t strength wind shear and flexural earth1.0g+ 1.4e + 1.0t 1.0g+ 1.0e + 1.0t strength quake table 1. combination of actions at uls for chimneys acc. to [6]. a) b) figure 2. stress-strain-curves of concrete (a) and reinforcement (b) acc. to [4], with reduced strain limits acc. to [2]. the internal forces of the chimney are calculated using a beam model with linear-elastic material properties according to both codes. the stress resultants are combined as shown in tab. 1. the design for the meridional reinforcement is performed by using the stress-strain-curves from fig. 2. but it is not only a matter how the meridional stress resultants are calculated, different approaches for the design of the cross section and reinforcement need to be considered as well. 3. comparison of beam theory and linear elastic shell theory further studies by [6] and [9] have revealed that for chimneys with large diameters the shell-like behavior becomes more important. it is apparent that the linear elastically calculated meridional forces of a chimney vary from a linear distribution for small diameters (fig. 3 a) to a nonlinear distribution for larger diameters (fig. 3 b). fig. 3 shows the load-bearing behavior figure 3. meridional internal forces at the bottom for slim (a) and wide (b) cylindrical shells exposed to wind load. of a slim and a wide cylindrical shell exposed to wind load, both calculated by shell theory. the side view of the meridional internal forces at the bottom of the slim cylinder (fig. 3 a) shows the linear behavior of the stress resultants, as we expect it from linear elastic stress resultant calculation via beam theory, whereas for the wide cylinder (fig. 3 b) the distribution of the meridional forces around the circumference differs significantly. it corresponds to the ovalization of 80 vol. 7/2017 design of concrete chimneys via nonlinear shell analysis figure 4. design via beam theory for a specific wind load. the circular cross section due to the reduced bending stiffness, resulting in tensile stress resultants (uplift) in both the windward and leeward side of the shell, whereas its side flanks are subjected to compressive stress resultants. the procedure of the design according to beam theory [10] is shown in fig. 4: a linear strain distribution is estimated for the calculated outer stress resultants according to the bernoulli hypothesis over the full diameter d of the chimney (fig. 4 a). this strain gradient (fig. 4 b) is varied until the respective sum of stresses in the concrete (fig. 4 c) figure 5. design via linear elastic shell theory for a specific wind load. and the chosen reinforcement (fig. 4 d) result in the same stress resultants as calculated with the beam model for the considered section. so the design according to beam theory includes an implicit nonlinearity when the stress-strain-curves for concrete and steel are applied. therefore the stress distribution for a cross section is nonlinear for outer stress resultants calculated by linear elastic beam theory (fig. 4). the design according to shell theory can be conducted with a linear internal stress resultant distribution over the cross section for chimneys with small diameters d (fig. 5 a). here t defines the wall thick81 franziska wehr, reinhard harte acta polytechnica ctu proceedings ness. the defining points for the design of the reinforcement lie in the area with maximum normal forces (fig. 5 a) as well as in the area with minimal normal forces for the compressive strength of concrete. the decisive tensile force causes a constant strain over the wall thickness t (fig. 5 b). therefore the concrete is cracked over the entire thickness (fig. 5 c) and the load can only be taken by the reinforcement (fig. 5 d). whereas the decisive compressive force can be taken up by concrete and reinforcement (fig. 5 c+d). the differences in the design between beam and shell theory are now demonstrated on the basis of an example chimney. the diameter d is varied while height h, wall thickness t and reinforcement ratio ρ remain constant. three different reinforcement ratios for the vertical reinforcement are considered. the chimney is stressed by dead load g and the wind load w is increased gradually until either the existing reinforcement is not able to carry the load anymore or the compressive strength of the concrete is exceeded. the maximum load factor λmax on wind load for the case of failure is plotted for each reviewed chimney with fed = 1.0 ·g+ λmax ·w = red. (1) the results are presented in fig. 7 (dotted and dashed lines). for both theories in case of a slender chimney the maximal load factor is bigger for smaller h/d ratios. but according to linear elastic shell theory for h/d-ratios smaller than about 15 the behavior changes. the reason for the smaller load bearing capacity of those chimneys is on the one hand the small reinforcement ratio for the hoop direction and on the other hand the shell-like behavior as mentioned before. according to beam theory the maximal wind load increases also for smaller h/d ratios, as well for the small h/d ratios not shown in fig. 7. the great dissimilarities can be explained by the different design concepts for beam and shell theory which are described in fig. 4 and 5. according to beam theory, the load is considered to act globally on the entire circular cross section whereas in shell theory the load is distributed around the circumference before performing the design for each point of the circular cross section separately. this results in a nonlinear stress distribution over the cross section according to beam theory and a linear stress distribution according to shell theory (fig. 8, black and yellow lines). for small h/d ratios the beam theory leads to wrong results, because of the consideration of a linear strain distribution. this causes a to stiff behavior of the cross section. since in reality stresses relocate from high stressed areas to parts with higher load-bearing capacities the solution of the beam theory seems to be more appropriate for small diameters. nevertheless it should be verified by nonlinear shell calculations whether the load distribution really occurs the way it is assumed by beam theory. a) b) figure 6. stress-strain-curves for concrete (a) and reinforcement (b) according to [8]. 4. design concept for concrete structures with nonlinear material behavior it is also possible to perform a cross section design using nonlinearly calculated stresses, or by performing a nonlinear ultimate load analysis [11]. by calculating the stress resultants with nonlinear material behavior internal forces that exceed the limit strength of concrete or reinforcement are eliminated and instead relocated to less stressed areas of the cross section. this can increase the calculated load-bearing capacity of a structure compared to linear elastic shell theory. the eurocode [8] gives some rules for a nonlinear calculation. the material properties shown in fig. 6 have to be used. they differ, especially for concrete, from the material properties for the design of a cross section. the displayed stress-strain-curves are already reduced by the global security factor for a nonlinear analysis in uls. for the nonlinear calculation according to [8] the same load combinations as listed in tab. 1 can be used. as it is not possible to do a superposition of the stress resultants calculated for the separate load cases, the internal forces have to be calculated for the decisive load combinations to include the nonlinear material properties. 82 vol. 7/2017 design of concrete chimneys via nonlinear shell analysis figure 7. load bearing capacity for predefined reinforcement acc. to beam theory, linear and nonlinear shell theory. 5. comparison of design via beam theory and nonlinear shell theory to compare the design results for a chimney obtained from beam theory with a nonlinear shell model the same procedure as described in chapter 3 is applied. the calculation is executed for different diameters while height and thickness remain constant. three different reinforcement ratios are considered. the chimney is at first loaded by dead load. in the next step the wind load is added incrementally until the failure of the chimney occurs at one or several points of the shell. the maximal load factor on wind load λmax is plotted for the failure case for each h/d ratio and results in the continuous lines shown in fig. 7. the figure clearly demonstrates that the calculated load-bearing behavior according to nonlinear shell theory is higher than according to beam theory for h/d ratios larger than 30. for smaller h/d ratios the beam theory allows higher load factors λmax than the nonlinear shell theory and thus will not be on the safe figure 8. comparison of meridional forces acc. to beam and shell design with respect to different ratios h/d. side. to compare the load-bearing behavior of beam and shell theory, fig. 8 shows the vertical stress resultants over the standardized cross section in case of maximum utilization for a vertical reinforcement ratio of 13.40 cm2/m. according to beam theory and linear shell theory the distribution of the normal forces is the same for all h/d ratios for the given geometry, whereas according to nonlinear shell theory the distribution of the internal forces differs subjected to the h/d ratios. the progression of the internal forces lies between the ones calculated by beam theory and linear elastic shell theory. for larger h/d ratios the nonlinear shell curves are similar to the beam solution. the beam theory distributes the stresses in the way that the maximum tensile strength of steel and the maximum compressive strength of concrete are utilized. it can be seen that for smaller h/d ratios the redistribution of the stresses around the circumference is overestimated in beam theory. then the nonlinear shell theory is more appropriate to describe the distribution of the 83 franziska wehr, reinhard harte acta polytechnica ctu proceedings stresses. thus for chimneys with h/d ratios smaller than 30, the calculated load-bearing capacity of the beam theory is not correct and on the unsafe side. 6. outlook the next step will be to find out whether the results for other geometries are comparable to the presented ones. the correctness of the results according to beam theory for the ring reinforcement also needs to be checked. if the results of further studies lead to similar results, the aim is to define a correction factor γcorr on wind loading as a function of slenderness ratio h/d and reinforcement ratio ρ. the factor shall then be applied to produce correct results for concrete chimneys by using beam theory even for non-slender geometries. acknowledgements the paper has presented intermediate results from the research project “validation of design procedure and safety concept of concrete chimneys via non-linear shell analysis”, financed by cicind. the support by cicind is gratefully acknowledged. references [1] p. noakowski, a. harling, m. breddermann, m. rost. rehabilitation of chimneys. cicind chimney book pp. 323–344, 2005. [2] cicind 2001. model code for concrete chimneys – part a: the shell, 2011. [3] en 13084-1:2007. free-standing chimneys – part 1: general requirements, 2007. [4] en 13084-2:2007. free-standing chimneys – part 2: concrete chimneys, 2007. [5] aci 307 2008. code requirements for reinforced concrete chimneys (aci 307-08) and commentary, 2008. [6] r. harte, o. pouran. interaction and intersection in research and development of cooling towers and concrete chimneys. cicind research project rp-2013-4c. bergische universität wuppertal, 2014. [7] en 1990:2002. eurocode – basis of structural design, 2002. [8] en 1992-1-1:2004. eurocode 2: design of concrete structures – part 1-1: general rules and rules for buildings, 2004. [9] f. lupi, h.-j. niemann. international standardization of wind actions on chimneys. cicind research project rp-2011-4. ruhr-universität bochum and niemann + partner bochum, 2013. [10] p. noakowski, m. breddermann, a. harling, m. rost. turmartige industriebauwerke – bemessungsgrundlagen der cicind, din en 13084 und din v 1056 mit beispielen und anwendungen. beton-kalender 2006 turmbauwerke, industriebauten pp. 225–318, 2006. [11] r. harte, w. krätzig, s.-y. noh, y. petryna. on progressive damage phenomena of structures. computational mechanics 25:404–412, 2000. 84 acta polytechnica ctu proceedings 7:79–84, 2017 1 introduction 2 design of concrete chimneys via beam theory 3 comparison of beam theory and linear elastic shell theory 4 design concept for concrete structures with nonlinear material behavior 5 comparison of design via beam theory and nonlinear shell theory 6 outlook acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.13.0001 acta polytechnica ctu proceedings 13:1–10, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app assessment of 2d-dic stochastic patterns jakub antoš∗, václav nežerka, michael somr czech technical university in prague, faculty of civil engineering, thákurova 7, 166 29 prague 6, czech republic ∗ corresponding author: jakub.antos@fsv.cvut.cz abstract. cost of experimental testing of materials and structures subjected to mechanical loading often constitutes a significant portion of a project budget. therefore a collection of data in a maximum possible amount is desirable. extensometers and strain-gauges attached to the specimen surface often fail and cannot provide full-field information about the development of displacements and strains. digital image correlation (dic) is capable of providing such information. unsuitable texture or artificially applied pattern, essential for dic analysis, can spoil the dic outcomes completely. an additional investment into preparation of new experimental testing can be avoided with the use of tools employing algorithms for stochastic pattern assessment. the development of such algorithms and their implementation into an open-source dic software is the goal of the presented research. keywords: digital image correlation, stochastic pattern, full-field displacement. 1. introduction the measurement of strains and displacements is utilized when investigating behavior of materials or specimens in laboratories, but also for assessment of existing structures. traditionally, contact measurement techniques have been used, but these introduce challenges in terms of accuracy, require sufficiently flat surface, and their attachment requires a lot of effort. the group of contact methods includes strain gauges, extensometers, or linear variable differential transformers (lvdts) [1]. contact methods techniques have a few drawbacks compared to optical full field monitoring: the strain must be within a certain range and is averaged over the strain-gauge length, the measurement is accomplished at discrete locations, and the investigated surface must be smooth enough to attach the gauge. quite recently alternatives to non-contact measurement have been developed. these include e.g., laser vibrometry, laser range finders, optical correlation methods, interferometry, moiré, or photo/videogrammetry [2, 3]. optical measurements, such as digital image correlation (dic), are capable of capturing even the most complex deformation until the ultimate material failure [3, 4]. because of that reason, optical methods became accepted in the field of experimental solid mechanics. the availability of compact and sensitive light sources, detectors, optical components, and powerful computers have been promoting the use of dic in both commercial and academic research. the full-field data can be easily processed and provides data valuable for engineers who are used to employing finite element programs in their calculations. 2. digital image correlation dic became indispensable to monitoring and analyzing a development of displacement or strain fields over time by matching stochastic pattern of deformed images with respect to a reference one [5]. the method is capable of capturing strain localization on a surface of a loaded structure (such as plasticity or cracking) in any direction. as dic tools for 3d analysis emerge [6], the method is becoming more versatile and widely used in the industry and research. dic is not only limited to the relative measurement of discrete points as conventional contact methods and is frequently more accurate than monitoring by means of extensometers or strain-gauges that often suffer from imperfect attachment to the measured surface. moreover, the use of dic can significantly reduce the cost of the experiment. dic reached its maturity during last decade owing it to the fast and successful development and elaboration of computers, digital cameras and specialized software for image processing. dic has even been characterized as “a major development in the art of experimental mechanics” [7]. the boom of dic has been reflected in the emergence of new commercial and open source software to perform dic with differently optimized correlation functions and calculation methods, most recently summarized by pan et al. [8]. 2.1. dic algorithms dic utilizes a correlation algorithm to obtain displacements and subset deformations by identifying areas of matching grey-scale values between the speckle pattern in each subset of deformed and underformed (reference) images (figure 1). to facilitate the correlation, a stochastic speckle pattern must be applied (if not present naturally) to a specimen surface in order to provide a random grey-level variations at 1 http://dx.doi.org/10.14311/app.2017.13.0001 http://ojs.cvut.cz/ojs/index.php/app j. antoš, v. nežerka, m. somr acta polytechnica ctu proceedings the sufficient quality of which is fundamental to the precision of the measured displacement data. it is well established that the trade-off between the data resolution and precision is affected by the quality of a pattern. to perform dic, each image must be divided into a grid of interrogation cells, or subsets, containing a finite number of pixels. resolution of the data is maximized by reducing the size of the subsets, but as the interrogation cell size decreases, the uncertainty in the strain measurement increases due to a reduction in the number of features to track within the subset [9]. therefore, the resolution and accuracy of the displacement and deformation fields are limited by the total number of pixels within the images. the center position of each target subset is obtained through searching the peak position of the correlation coefficient field and its deformation is calculated using an iterative approach [10, 11]. dic has traditionally utilized subset-based local approach [5] that has been very well developed and widely used in commercial or academic dic packages. however, there are certain drawbacks that make the method useless for some applications, such as experiments producing high strain gradients [12]. the reason is non-continuity of the displacement field, as the displacements of the subsets are sought separately. therefore smoothing of the noisy displacement field is required [8, 9, 11]. a local polynomial smoothing over a rectangular area (strain window) is usually employed [8]. the amount of smoothing is controlled by the subset size, step size, and strain window size. the results are then highly dependent on setting these parameters by a user [13]. an alternative global approach has been developed quite recently based on the procedures used in the finite element method (fem) [14, 15]. using the global dic approach, a complete element mesh is tracked on images, ensuring c0-continuity1, resulting in elimination of noise in strain fields. this method was initially proposed by cheng et al. [16] and later besnard et al. developed the q4-dic [17] with implementation of a bilinear (q4) or quadratic (q8) mesh. the global algorithms may be refined using user experience, or using adaptive mesh refinement [18]. 2.2. dic accuracy the accuracy of dic is an issue frequently discussed by both, theoreticians and experimentalists [19, 20]. although originally restricted to the size of one-pixel, various sub-pixel techniques have been proposed and used to improve the method accuracy. the most popular techniques include curve-fitting, gradient-based and newton-raphson algorithms. the last two cases are based on the identification of the parameters that define the mapping of a subset of pixels in order to 1ci differentiability class corresponds to the existence of i derivatives of a function. the class c0 consists of all continuous functions. figure 1. example of the subset tracking procedure using dic. maximize the image correlation. the results show that the newton-raphson approach is considered as the most accurate and stable. other interesting approaches such as genetic algorithms, finite element interpolations and b-splines are reported in [8] but they generally appear to have a lower performance. bing et al. [21] compared performance of three most used sub-pixel techniques by simulating image distortions, demonstrating the suitability of newton-rapson approach. besides the choice of the most suitable dic algorithm, other factors substantially influence the dic accuracy. the measurement errors may be classified into two categories: (i) systematic experimental errors such as bad calibration and setting of image acquisition system and (ii) errors produced by correlation algorithm. the experimental errors are related to variations in illumination and the quality of the acquisition system, i.e., the noise during the acquisition and digitalization, image distortion, or position of the camera with respect to the monitored surface. the errors related to the correlation algorithms arise from inappropriate selection of correlation methods or input parameters, such as subset size, correlation function, sub-pixel algorithm, shape function, or interpolation scheme. 3. stochastic pattern assessment a majority of research into the accuracy of dic is focused on correlation algorithms and processing parameters (recall section 2.2), such as subset size [22], shape function selection [23], or methods of obtaining sub-pixel accuracy [24]. less attention has been paid to the effect of the quality of the speckle pattern. it is important for the artificial pattern or natural texture to be adjusted in accordance with the expected displacement field in order to maximize measurement 2 vol. 13/2017 assessment of 2d-dic stochastic patterns accuracy, as speckles can be both too large and too small for the particular measurement [25]. quantitative error analysis [26–29] shows that the measurement error depends crucially on the presence of large intensity gradients within the pattern. therefore, the technique in most cases requires a specimen preparation procedure to enhance the surface texture, since the natural one does not provide a required quality in terms of intensity gradients and speckle-size distribution. pattern assessment has been discussed by a few authors [5, 30, 31], offering a number of methods to evaluate the quality of applied patterns. pan et al. [32] presented a number of assessment criteria based upon the local subset intensity gradients [20] and the global mean intensity gradient (mig) throughout the image. the latter criteria showed a good agreement to results obtained numerically. the benefit of applying the global criteria is that these are astraightforward. high mig values typically result in smaller bias and less dispersion in dic measurements. on the other hand, crammonde et al. [33] objected that global parameters, such as mig, are not sufficient to evaluate strain accuracy. based on their findings, simple means of a randomness assessment is to employ the outcomes of the shannon entropy theory [34]. cintrón et al. [35] demonstrated that the speckle size should range from 2×4 px for a high accuracy in the strain measurement. the speckle size should have a lower limit according to the study by sutton et al. [5] of 3×3 px. in the presented study, various patterns produced by the spraying white / black dots on a contrast background were investigated. in addition, natural textures of various materials were studied as well, to demonstrate their performance. the knowledge of a texture suitability is essential when monitoring existing structures where application of artificial patterns is not possible. to eliminate the impact caused by image acquisition system (such as the distortion of the camera lens, lighting variation, etc.) during the experiment, numerical approach was utilized to investigate the relationship between shannon entropy, mean intensity gradient, values of correlation coefficient, and error in dic measurements. the explanation of the mentioned parameters is provided next. 3.1. normalized cross-correlation correlation between two signals (also reffered to as cross-correlation) is a standard approach to feature detection and image registration [36–38]). the normalized form of correlation takes into account intensities relative to the highest one, thus eliminating the sensitivity to changes in illumination intensity. however, it does not have a correspondingly simple and efficient frequency domain expression. for this reason, normalized cross-correlation must be computed in a spatial domain and fast spatial domain matching methods had to be developed. detailed description of cross-correlation equation is beyond the scope of this article. reader can find it in barnea et al. [39]. 3.2. mean intensity gradient (mig) mig was proposed by pan et al. [32] as a global parameter for evaluating the quality of a speckle pattern over the entire domain. both, a mean bias error and standard deviation of measured displacements are influenced by the mig of the speckle pattern. the speckle pattern with a large mig is supposed to produce small displacement measurement errors. mig is defined as δf = w∑ i=1 h∑ j=1 |of (xij)| 1 w ×h , (1) where w and h are the image width and height in pixels, |of (xij)| = √ fi (xij)2 + fj (xij)2 is the modulus of the local intensity gradient. fi (xij) and fj (xij) are the iand j-directional intensity derivatives at pixel (xij) respectively, which can be computed using a central difference algorithm. 3.3. shannon entropy a high shannon entropy value indicates a high level of texturing, or broadness in the greyscale distribution of the image, beneficial for maximizing the correlation function peak when a correct match has been found. the shannon entropy parameter is defined as [40] ψ = w∑ i=1 h∑ i=j f(xij)log (f(xij)) . (2) 4. assessment of patterns and textures randomly distributed speckles must not exhibit any preferential directions. high contrasts are required to provide sharp peaks in the correlation function. to test this requirement, initial synthetic tests on samples of 400×400 px were performed on six model patterns (figure 2). the patterns / textures were tested with respect to four quality indicators: value of cross-correlation coefficient for two different subset sizes (10×10 px and 30×30 px), shannon entropy, and mig. the summary of the investigated patterns and textures is provided in table 1. based on the values of normalized cross-correlation functions presented in the form of surface plots in figures 3 and 4, it can be concluded that the correlation function peaks can be highlighted by setting bigger subset size since these contain more distinct features. especially in the case of small subset size, 10×10 px, the correlation peaks on coarse textures could not be clearly identified. this could lead to huge errors of dic measurements in the case of significantly distorted images. however, the findings cannot be generalized, since in some patterns the cross-correlation correlation function does not exhibit any distinct peak 3 j. antoš, v. nežerka, m. somr acta polytechnica ctu proceedings (a) . fine spray pattern (b) . coarse air-brush pattern (c) . white sprayed dots (d) . natural texture of concrete (e) . masonry wall (f) . texture of wood figure 2. investigated artificial patterns (top) and natural textures (bottom). in for small subsets, while correlation of the larger one results in unique match and low value of mean correlation coefficient (cf. figures 3(b,f), 4(b,f), and table 1). therefore, the pattern assessment based on the the mean value of the cross-correlation function must be carried out for any subset size independently. moreover, a statistical information about number of peaks in the form of a decay in the power law distribution would provide more accurate description. based on observation of distribution of correlation coefficient a power law distribution can be assumed (figure 5, 6). the power law function is defined by equation yp = x−α p , where α is the decay parameter which provides information about the distribution of correlation coefficient over the investigated domain. larger α indicates smaller amount of unwanted correlation peaks which is desirable. it is also clear that neither shannon entropy nor mig are capable of providing clear indication of the pattern quality since these two are not in agreement — once the pattern is, relative to other ones, regarded as superior to others based on shannon entropy, mig provides completely different results, see table 1. therefore, new more universal criteria taking into account size, contrast, and size-distribution of speckles should be proposed. 5. virtual stretching of patterns and textures the artificial patterns and natural textures were tested in the proof-of-concept experiments carried out virtually on a computer by prescribing a constant deformation. special attention was paid to the ability of the pattern to provide high-accuracy measurements at deformations reaching 5%, at which poor patterns fail [41]. the evaluation and testing of patterns was performed using own matlab scripts by placing virtual extensometers at the edges of the tested samples. in this initial study the images containing 8-bit speckle patterns were virtually stretched up to 5% in 10 steps. image sequences were then evaluated in open-source 2d-dic software package ncorr [10] with the same setting of parameters. subset sizes of 10 px and 30 px were chosen to demonstrate the correlation between the mean correlation coefficient mentioned in the section 4 and measurement errors. as the number of speckles within the patterns increased, the measurement errors decreased. moreover, larger sized speckles provided lower error than patterns with smaller speckles. global pattern quality parameters were discussed and shannon entropy was used as an example to demonstrate that the global measures are not sufficient to assess the quality and 4 vol. 13/2017 assessment of 2d-dic stochastic patterns (a) . fine spray pattern (b) . coarse air-brush pattern (c) . white sprayed dots (d) . natural texture of concrete (e) . masonry wall (f) . texture of wood figure 3. correlation function values for 10×10 px subset size. 5 j. antoš, v. nežerka, m. somr acta polytechnica ctu proceedings (a) . fine spray pattern (b) . coarse air-brush pattern (c) . white sprayed dots (d) . natural texture of concrete (e) . masonry wall (f) . texture of wood figure 4. correlation function values for 30×30 px subset size. 6 vol. 13/2017 assessment of 2d-dic stochastic patterns γ(xij) α ψ δf sample 10×10 30×30 10×10 30×30 fine spray pattern (a) 0.152 0.054 0.847 0.959 5.524 121.182 coarse air-brush pattern (b) 0.190 0.107 1.009 1.046 5.413 127.614 white spray dots (c) 0.089 0.138 1.148 0.997 4.972 82.198 natural texture of concrete (d) 0.090 0.039 1.027 0.975 6.292 75.849 masonry wall (e) 0.200 0.187 0.879 0.939 4.250 50.914 texture of wood (f) 0.208 0.097 0.878 0.981 5.012 29.027 table 1. mean correlation coefficient, γ(xij), power law distribution decay parameter α, ψ, and δf for tested patterns / textures and different size of subsets. 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 correlation coefficient (in absolute value) [-] 0 0.5 1 1.5 2 2.5 3 f re q u e n c y [ -] ×104 (a) . subset 10×10 px (α = 0.847) 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 correlation coefficient (in absolute value) [-] 0 1 2 3 4 5 6 7 8 f re q u e n c y [ -] ×104 (b) . subset 30×30 px (α = 0.959) figure 5. distribution of correlation coefficient, fine spray pattern. 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 correlation coefficient (in absolute value) [-] 0 0.5 1 1.5 2 2.5 3 f re q u e n c y [ -] ×104 (a) . subset 10×10 px (α = 0.879) 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 correlation coefficient (in absolute value) [-] 0 0.5 1 1.5 2 2.5 3 3.5 f re q u e n c y [ -] ×104 (b) . subset 30×30 px (α = 0.939) figure 6. distribution of correlation coefficient, masonry wall. 7 j. antoš, v. nežerka, m. somr acta polytechnica ctu proceedings (a) (b) (c) (d) (e) (f) pattern / texture 0 0.5 1 1.5 2 2.5 3 3.5 d is p la c e m e n t e rr o r [% ] (a) . 1% deformation (a) (b) (c) (d) (e) (f) pattern / texture 0 0.2 0.4 0.6 0.8 1 1.2 d is p la c e m e n t e rr o r [% ] (b) . 5% deformation figure 7. displacement error for 10×10 px subset size. (a) (b) (c) (d) (e) (f) pattern / texture 0 0.5 1 1.5 2 2.5 3 3.5 4 4.5 d is p la c e m e n t e rr o r [% ] (a) . 1% deformation (a) (b) (c) (d) (e) (f) pattern / texture 0 0.5 1 1.5 2 2.5 3 3.5 4 4.5 d is p la c e m e n t e rr o r [% ] (b) . 5% deformation figure 8. displacement error for 30×30 px subset size. properties of the patterns. this is illustrated by comparing errors at different stretching magnitude for different speckle sizes (figure 7 and 8). 6. conclusions based on the research of crammond et al. 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[37] r. c. gonzalez, r. e. woods, b. r. masters. digital image processing, third edition. journal of biomedical optics 14(2):029901, 2009. doi:10.1117/1.3115362. [38] r. brunelli, t. poggio. face recognition: features versus templates. ieee transactions on pattern analysis and machine intelligence 15(10):1042–1052, 1993. doi:10.1109/34.254061. [39] d. i. barnea, h. f. silverman. a class of algorithms for fast digital image registration. ieee transactions on computers c-21(2):179–186, 1972. doi:10.1109/tc.1972.5008923. [40] d. lecompte, s. bossuyt, s. cooreman, et al. study and generation of optimal speckle patterns for dic. in proceedings of the sem annual conference and exposition on experimental and applied mechanics. 2007. [41] g. stoilov, v. kavardzhikov, d. pashkouleva. a comparative study of random patterns for digital image correlation. journal of theoretical and applied mechanics 42:55–66, 2012. 10 http://dx.doi.org/10.1016/0004-3702(73)90004-0 http://dx.doi.org/10.1117/1.3115362 http://dx.doi.org/10.1109/34.254061 http://dx.doi.org/10.1109/tc.1972.5008923 acta polytechnica ctu proceedings 13:1–10, 2017 1 introduction 2 digital image correlation 2.1 dic algorithms 2.2 dic accuracy 3 stochastic pattern assessment 3.1 normalized cross-correlation 3.2 mean intensity gradient (mig) 3.3 shannon entropy 4 assessment of patterns and textures 5 virtual stretching of patterns and textures 6 conclusions acknowledgements references 286 acta polytechnica ctu proceedings 2(1): 286–290, 2015 286 doi: 10.14311/app.2015.02.0286 rotation of the mass donors in high-mass x-ray binaries and symbiotic stars k. stoyanov1, r. zamanov1 1institute of astronomy and national astronomical observatory, bulgarian academy of sciences, 72 tsarigradsko shousse blvd., 1784 sofia, bulgaria corresponding author: kstoyanov@astro.bas.bg abstract our aim is to investigate the tidal interaction in high-mass x-ray binaries and symbiotic stars in order to determine in which objects the rotation of the mass donors is synchronized or pseudosynchronized with the orbital motion of the compact companion. we find that the be/x-ray binaries are not synchronized and the orbital periods of the systems are greater than the rotational periods of the mass donors. the giant and supergiant high-mass x-ray binaries and symbiotic stars are close to synchronization. we compare the rotation of mass donors in symbiotics with the projected rotational velocities of field giants and find that the m giants in s-type symbiotics rotate on average 1.5 times faster than the field m giants. we find that the projected rotational velocity of the red giant in symbiotic star mwc 560 is v sin i= 8.2± 1.5 km s−1, and estimate its rotational period to be prot = 144 306 days. using the theoretical predictions of tidal interaction and pseudosynchronization, we estimate the orbital eccentricity e = 0.68 − 0.82. keywords: stars: binaries: symbiotic stars: rotation stars: late type stars: binaries: close x-rays: binaries. 1 introduction a high-mass x-ray binary system consists of a compact object (a neutron star or a black hole) accreting material from an o or b companion star. they are divided into be/x-ray binaries (main-sequence star as a companion) and giant/supergiant x-ray binaries (giant or supergiant star as a companion). accretion of matter is different for both types of x-ray binaries. in the be/x-ray binaries, the compact object crosses the circumstellar disc and accretes matter from that disk. in the giant/supergiant x-ray binaries, the mass donor ejects a slow and dense wind radially outflowing from the equator and the compact object directly accretes the stellar wind through bondi-hoyle-lyttleton accretion. symbiotic stars are interacting binaries, consisting of an evolved giant (either a normal red giant in s-types symbiotics or a mira-type variable in d-types symbiotics) transferring mass to a hot and luminous white dwarf or neutron star. the symbiotic stars are surrounded by a rich and luminous nebula resulting from the presence of both an evolved giant with a heavy mass-loss and of a hot companion abundant in ionizing photons and often emanating its own wind. 2 synchronization and pseudosynchronization in a binary with a circular orbit the rotational period of the primary, prot, reaches an equilibrium value at the orbital period, porb = prot. in other words the synchronous rotation (synchronization) means that the rotational period is equal to the orbital period. in a binary with an eccentric orbit, the corresponding equilibrium is reached at a value of prot which is less than porb, the amount less being a function solely of the orbital eccentricity e. in practice, in a binary with an eccentric orbit the tidal force acts to synchronize the rotation of the mass donor with the motion of the compact object at the periastron pseudosynchronous rotation. to calculate the period of pseudosynchronization, pps, we use (hut 1981): pps = (1 + 3e2 + 3 8e 4)(1 − e2) 3 2 1 + 15 2 e 2 + 45 8 e 4 + 5 16e 6 porb. (1) 2.1 stars with radiative envelopes following hurley, tout & pols (2002) the circularization timescale for stars with radiative envelopes is: 1 τcirc = 21 2 ( gm1 r3 1 ) 1 2 q2 (1 + q2) 11 6 e2 ( r1 a ) 21 2 , (2) 286 http://dx.doi.org/10.14311/app.2015.02.0286 rotation of the mass donors in high-mass x-ray binaries and symbiotic stars where m1 and r1 are the mass and the radius of the primary respectively, q2 is the mass ratio m2/m1, and a is the semi-major axis. the second-order tidal coefficient e2 = 1.592 ×10−9m2.84 1 . the synchronization time scale is given as, τsync = kτcirc, (3) where k is: k ≈ 0.015 rg 1 + q2 q2 ( r1 a )2 . (4) for the gyration radius of the primary rg we adopt rg ≈ 0.16 for giants, and rg ≈ 0.25 for main sequence stars (claret & gimenez, 1989). 2.2 stars with convective envelopes following hurley, tout & pols (2002) the synchronization timescale for stars with convective envelopes is: τsyn ≈ 800 ( m1r1 l1 )1/3 m2 1 (m1 m2 + 1)2 r6 1 p 4 orb yr, (5) where l1 is the luminosity of the giant. the circularization time scale is: 1 τcirc = 21 2 ( k t ) q2(1 + q2) ( r1 a )8 . (6) in eq. 6, (k/t ) is:( k t ) = 2 21 fconv τconv menv m1 yr−1, (7) where renv is the depth of the convective envelope, menv is the envelope’s mass, and τconv = 0.4311 ( menvrenv(r1 − 1 2renv) 3l1 ) 1 3 yr (8) is the eddy turnover time scale (the time scale on which the largest convective cells turnover). the numerical factor fconv is fconv = min [ 1, ( ptid 2τconv )2 ] , (9) where ptid is the tidal pumping time scale given by 1 ptid = ∣∣∣∣ 1 porb − 1 prot ∣∣∣∣ . (10) the pseudosynchronization timescale is τps = (7/3(α 3)) τcirc, where α is a dimensionless quantity, representing the ratio of the orbital and rotational angular momentum: α = q2 1 + q2 1 r2g ( a r1 )2 . (11) for a red giant we adopt rg ≈ 0.3 (claret, 2007). in all equations, the masses, the radii and the lumunosities are in solar units. 3 high-mass x-ray binaries the orbital and stellar parameters of 13 high-mass xray binaries are given in table 1 and table 2 in stoyanov & zamanov (2009). we add 2 more objects 4u 2206+54 and mwc 148. the orbital and stellar parameters are taken from ribó et. al. (2006) and casares et al. (2012) respectively. using eq.2 and eq.3 we estimate the circularization and synchronization timescales. the results are given in table 1. the lifetime of a star on the main sequence can be estimated as τms = 1010(m�/m)2.5 years (hansen & kawaler, 1994). comparing these lifetimes with τsync from table 1, we see that among the be/x-ray binaries only for lsi+610303 is τsync ∼ τms . this is the only be/x-ray binary for which we can expect considerable changes of the rotation of the primary during the lifetime of the be star. the lifetime of the giant is comparable or longer then τcirc and τsync for the giant/supergiant systems with short orbital periods. the exceptions are v725 tau and bp cru, for which τsync and τcirc are longer than the lifetime of the giant/supergiant stage. on fig.1 in stoyanov & zamanov (2009) is plotted prot versus pps. the giant/supergiant systems are located close to the line pps = prot, while those with mass donors from spectral class v are far away from the equilibrium. in the be/x-ray systems bq cam, v635 cas, v725 tau and 4u 2206+54, the tidal force spinning down the donor star. for the system lsi+610303, the rotation of the mass donor is close to pseudosynchronization. this is the only be/x-ray binary in which τsync is comparable with the life-time of the binary. in the binaries x per and mwc 148, the neutron star is far away from the be star and the tidal force is weak. giant and supergiant systems are close to (pseudo)synchronization. in these binaries the rotation of the mass donors is influenced by the presence of the compact object. in lmc x-4 and cen x-3, the mass donors are synchronized and the orbits are circularized. with respect to the rotation of the mass donor, v725 tau is similar to the be/x-ray binaries. cyg x-1 is synchronized and almost circularized. v830 cen is pseudosynchronized but not circularized yet. the systems lsi+650010 and vela x-1 are close to pseudosynchronization and the tidal force accelerates the rotation of the mass donors. in the case of smc x-1, the tidal force acts as a decelerator of the rotation of the mass donor. in bp cru, a gas stream from the mass donor 287 k. stoyanov, r. zamanov exists, probably resulting from the strong tidal force and spin-up of the mass donor (leahy & kostka, 2008). table 1: calculated time scales. given here are the name of the object, synchronization time scale, circularization time scale, and the lifetime. object τsync [yr] τcirc [yr] lifetime [yr] be/x-ray binaries lsi+610303* 2.8×107 2.4×108 5.6×107 x per 6.2×1017 1.8×1021 1.1×107 bq cam 3.5×1011 7.6×1013 3.9×106 v635 cas 1.4×1011 9.5×1012 7.3×106 4u 2206+54 4.9×109 3.7×1011 7.3×107 mwc 148 1.2×1017 5.1×1020 9.8×107 giant systems v725 tau 2.8×1012 8.0×1014 4×105 lmc x-4 4.5×102 7.7×102 1×106 cen x-3 2.3×103 4.2×103 5×105 supergiant systems v830 cen 7.5×103 1.4×104 1×106 lsi+650010 1.3×104 3.9×104 1×106 vela x-1 1.0×104 2.8×104 3.9×105 smc x-1 3.3×104 8.2×104 8.8×105 bp cru 1.8×106 8.8×106 8×104 cyg x-1 < 1 < 1 1×105 *assuming neutron star as a secondary component. 4 s-type symbiotic stars 43 symbiotic stars have been observed with feros spectrograph at the 2.2m eso telescope of the la silla observatory (zamanov et al. 2007). the data for the rotation of 55 field red giants are taken from the literature. m giants in s-type symbiotics rotate faster than the field m giants. histograms of the available v sin i data for the red giants are plotted in fig.2 in zamanov & stoyanov (2012). for the field m0iii-m6iii giants we calculate a mean v sin i=5.0 km s−1, median v sin i=4.3 km s−1, and standard deviation of the mean σ = 4.0 km s−1. for the m0iii-m6iii giants in symbiotics, we get a mean v sin i= 7.8 km s−1, median v sin i=8.0 km s−1, and standard deviation of the mean σ =2.1 km s−1. there are 5 objects in our sample that deviate from the synchronization. these objects are rs oph, mwc 560, ch cyg, cd-43◦14304 and z and. in three of them collimated jets are detected: z and (skopal et al. 2009); ch cyg (crocker et al. 2002), mwc 560 (tomov et al. 1990). additionally to the jets, ejection of blobs are detected from rs oph and ch cyg (iijima et al. 1994). this confirms the suggestions that in the jet-ejecting symbiotics the mass donors rotate faster than the orbital periods. probably there is a link between the jets and the mass donor rotation. on fig.1 are plotted together the high-mass x-ray binaries and the s-type symbiotic stars. it shows that none of the objects in our sample is above the line of synchronization. figure 1: prot versus porb on a logarithmic scale. the blue circles indicates the high-mass x-ray binaries filled symbols for giant/supergiant systems and open symbols for be/x-ray binaries. the red triangles indicates the s-type symbiotic stars. 5 orbital eccentricity of mwc 560 mwc 560 is a symbiotic star, which consists of a red giant and a white dwarf (tomov et al. 1990). the most spectacular features of this object are the collimated ejections of matter with velocities of up to ∼ 6000 km s−1 (tomov et al. 1992) and the resemblance of its emission line spectrum to that of the low-redshift quasars (zamanov & marziani, 2002). the jet ejections are along the line of sight and the system is seen almost pole-on (i < 16◦). this makes it difficult to obtain the orbital eccentricity of the system in a conventional way. for the system we adopt rg = 140 ± 7 r�, lg ∼ 2400 l�, mg = 1.7 m�, mwd = 0.65 m�, porb = 1931± 162 day (gromadzki et al. 2007), renv = 0.9 rg 288 rotation of the mass donors in high-mass x-ray binaries and symbiotic stars and menv = 1.0 m� (herwig 2005). with the above values of the parameters assumed, we derive the semimajor axis of the orbit to be a ≈ 860 r�. using these parameters, we calculate from eq. 5 and eq. 6 the synchronization and circularization time scales: τsync = 2.6 × 104 yr and τcirc = 3.1 × 106 yr. the typical lifetime of a symbiotic star is τss ∼ 105 yr (yungelson et al., 1995). from the rate of accretion on the white dwarf, ṁacc ≈ 5× 10−7 m� (schmid et al. 2001), we can estimate, that it will take 106 yr to accrete ∼ 0.5 m� from the envelope of the red giant companion. because the giant also losses mass via stellar wind, we find that the lifetime of the symbiotic phase of mwc 560 should be τss ≤ 106 yr. for mwc 560 we have therefore the situation in which τps < τsyn < τss < τcirc. this means that the symbiotic phase is long enough that the tidal forces can (pseudo)synchronize the rotation of the red giant. on the other hand, the value of τcirc demonstrates that the symbiotic lifetime of mwc 560 is shorter than the circularization time, and therefore the orbit can be eccentric. this is in agreement with the observational evidences found by fekel et al. (2007) that the symbiotic stars with porb > 800 days tend to have eccentric orbits. the above implies that in mwc 560, the red giant is probably synchronized, but the orbit is not circularized. to determine the orbital eccentricity of mwc 560, we need to calculate prot for the mass donor. we analyzed 21 high resolution spectra of mwc 560 and obtained value for v sin i= 8.2 ± 1.5 km s−1. using rg = 140 ± 7 r� and i = 12◦ − 16◦, we calculate prot = 144 − 306 days. this value is less than the orbital period. mwc 560 should be close to synchronization or pseudosynchronization, and prot = pps. using eq. 1 we can estimate the orbital eccentricity to be e = 0.68 − 0.82. 6 conclusions using rotational velocity measurements and the theory of synchronization/pseudosynchronization we: (1) find that the be/x-ray binaries are far away from (pseudo)synchronization. the tidal force in the be/x-ray binaries acts as a decelerator of the rotation of the mass donors. the only be/x-ray binary which is close to pseudosynchronization is the lsi+610303. the objects containing mass donors of spectral class i and iii typically have prot ∼ pps and are close to (pseudo)synchronization; (2) demonstrate that the m giants in symbiotic stars rotate faster than the field giants. most symbiotics with orbital period less than 1000 d are synchronized; (3) show that the high-mass x-ray binaries and the s-type symbiotic stars are either on the line of synchronization or they are under the line. none of the objects in our sample is above the line of synchronization. (4) calculate that the orbit of the symbiotic star mwc 560 should be highly eccentric, with e ∼ 0.7. acknowledgement we thank the anonymous referee for constructive comments. this work was supported by the op “hrd“, esf and bulgarian ministry of education, youth and science under the contract bg051po001-3.3.06-0047. references [1] casares, j., ribó, m., ribas, i., paredes, j. m., vilardell, f., & negueruela, i.: 2012, mnras, 421, 1103 doi:10.1111/j.1365-2966.2011.20368.x [2] claret, a.: 2007, a&a 467, 1389 [3] claret, a., & gimenez, a.: 1989, a&as, 81, 37 [4] crocker, m. m., davis, r. j., spencer, r. e., et al.: 2002, mnras, 335, 1100 doi:10.1046/j.1365-8711.2002.05705.x [5] fekel, f. c., hinkle, k. h., joyce, r. r., wood, p. r., lebzelter, t.: 2007, aj 133, 17 [6] gromadzki, m., miko lajewska, j., whitelock, p. a., marang, f.: 2007, a&a 463, 703 [7] hansen, c. j., & kawaler, s. d.: 1994, stellar interiors. physical principles, structure, and evolution, springer-verlag [8] herwig, f.: 2005, ara&a 43, 435 doi:10.1146/annurev.astro.43.072103.150600 [9] hurley, j. r., tout, c. a., & pols, o. r.: 2002, mnras, 329, 897 doi:10.1046/j.1365-8711.2002.05038.x [10] hut, p.: 1981, a&a, 99, 126 [11] iijima, t., strafella, f., sabbadin, f., & bianchini, a.: 1994, a&a, 283, 919 [12] leahy, d. a., & kostka, m.: 2008, mnras, 384, 747 doi:10.1111/j.1365-2966.2007.12754.x [13] ribó, m., negueruela, i., blay, p., torrejón, j. m., & reig, p.: 2006, a&a, 449, 687 [14] schmid, h. m., kaufer, a., camenzind, m., rivinius, t., stahl, o., szeifert, t., tubbesing, s., wolf, b.: 2001, a&a 377, 206 [15] skopal, a., pribulla, t., budaj, j., et al.: 2009, apj, 690, 1222 doi:10.1088/0004-637x/690/2/1222 [16] stoyanov, k. a., & zamanov, r. k.: 2009, astronomische nachrichten, 330, 727 289 http://dx.doi.org/10.1111/j.1365-2966.2011.20368.x http://dx.doi.org/10.1046/j.1365-8711.2002.05705.x http://dx.doi.org/10.1146/annurev.astro.43.072103.150600 http://dx.doi.org/10.1046/j.1365-8711.2002.05038.x http://dx.doi.org/10.1111/j.1365-2966.2007.12754.x http://dx.doi.org/10.1088/0004-637x/690/2/1222 k. stoyanov, r. zamanov [17] tomov, t., zamanov, r., kolev, d., georgiev, l., antov, a., mikolajewski, m., esipov, v.: 1992, mnras 258, 23 doi:10.1093/mnras/258.1.23 [18] tomov, t., kolev, d., zamanov, r., georgiev, l., antov, a.: 1990, nature 346, 637 doi:10.1038/346637a0 [19] yungelson, l., livio, m., tutukov, a., & kenyon, s. j.: 1995, apj 447, 656 doi:10.1086/175908 [20] zamanov, r. k., bode, m. f., melo, c. h. f., et al.: 2007, mnras, 380, 1053 doi:10.1111/j.1365-2966.2007.12150.x [21] zamanov, r., marziani, p.: 2002, apjl 571, l77 doi:10.1086/341367 [22] zamanov, r. k., & stoyanov, k. a.: 2012, bulgarian astronomical journal, 18, 41 290 http://dx.doi.org/10.1093/mnras/258.1.23 http://dx.doi.org/10.1038/346637a0 http://dx.doi.org/10.1086/175908 http://dx.doi.org/10.1111/j.1365-2966.2007.12150.x http://dx.doi.org/10.1086/341367 introduction synchronization and pseudosynchronization stars with radiative envelopes stars with convective envelopes high-mass x-ray binaries s-type symbiotic stars orbital eccentricity of mwc 560 conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0033 acta polytechnica ctu proceedings 7:33–37, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app 1d hermite elements for c1-continuous solutions in second gradient elasticity christian liebold∗, wolfgang h. müller berlin university of technology, chair of continuum mechanics and materials theory, einsteinufer 5, 10587 berlin, germany ∗ corresponding author: christian.liebold@tu-berlin.de abstract. we present a modified strain gradient theory of elasticity for linear isotropic materials in order to account for the so-called size effect. additional material length scale parameters are introduced and the problem of static beam bending is analyzed. a numerical solution is derived by means of a finite element approach. a global c1-continuous displacement field is applied in finite element solutions because the higher-order strain energy density additionally depends on second gradients of displacements. so-called hermite finite elements are used that allow for merging gradients between elements. the element stiffness matrix as well as the global stiffness matrix of the problem is developed. convergence, c1-continuity and the size effect in the numerical solution is shown. experiments on bending stiffnesses of different sized micro beams made of the polymer su-8 are performed by using an atomic force microscope and the results are compared to the numerical solution. keywords: second gradient continuum, size effect, hermite finite elements. 1. introduction materials with intrinsic microor nano-structure can show size-dependent material behavior, which is reflected, e.g., by a stiffer elastic response to external forces when the size of the material body is reduced. a quantitative understanding of a possible size effect in microand submicrostructures is of great importance when modeling microand nano-electro-mechanical systems (mems/nems). driven by miniaturization, the need for saving materials and improving the performance, the requirement of reliability in simulation technologies increases. a size effect is reflected in a different elastic response to external loads if the size of the material body is reduced. experimental validation therefore is given in, e.g., [1–6]. second gradient (sg) continuum theories are used if, in the absence of strain gradients (in uniaxial tensile tests), the elastic behavior of the material is independent of the thickness of the sample [3]. they are applicable to so-called non-simple materials of the gradient type, for example, polymers at a small scale. since conventional continuum theories based on the cauchy continuum are not able to predict size effects, the present work deals with the modified strain gradient theory (msg) developed in, e.g., [7–9]. by employing the macroscopic rotation vector and second order derivatives of the displacement vector, msg-theory is able to account for quantities like rotation and curvature. a generalization of strain gradient continua has been developed by eringen, who proposed “nonsimple materials of gradient type [10]” in order to derive the corresponding higher-order material dependencies in a rational manner. the application of conventional finite element (fe) strategies may lead to inaccurate results, if finite element formulations are used which only fullfill global c0–continuity. the scope of this work is to use fe formulations based on hermite polynomials in order to fulfill global c1–continuity for solutions in the modified strain gradient theory. section 2 presents the strain energy function of the modified strain gradient theory and a one dimensional differential equation is derived by making use of the euler-bernoulli assumptions for slender beams. the finite element formulation based on hermite polynomials is presented in sect. 3 as well as the structure of the element stiffnessand system matrix. a numerical example for a loaded cantilever beam is then given in sect. 4. 2. modified strain gradient theory 2.1. strain energy function the present study starts with one of the three reduced forms of the strain energy densities for small deformations, usg, as postulated by mindlin (1962) [8]. the einstein summation convention on repeated indices is used and spatial partial derivatives in the cartesian coordinate system are denoted by commaseparated indices. mindlin’s second form of linear isotropic strain energy density reads: usg = α1εij εij + α2εkk εmm + β1ηijk ηijk + β2ηiik ηjjk + + β3ηiik ηkjj + β4ηijj ηikk + β5ηijk ηkji , (1) where εij = 1/2(ui,j + uj,i ) denotes the small strain tensor and ηijk = 1/2(uk,ij + uj,ki ) = εkj,i the gradient 33 http://dx.doi.org/10.14311/app.2017.7.0033 http://ojs.cvut.cz/ojs/index.php/app christian liebold, wolfgang h. müller acta polytechnica ctu proceedings of strain. α1 and α2 lead to lamé’s constants and β1,...,5 are five additional higher-order material constants [11]. σij and µijk denote the cauchy stress tensor and the higher-order stress tensor, respectively: σij = ∂usg ∂εij , µijk = ∂usg ∂ηijk . (2) the inclusion of the macroscopic rotation vector ϕi = 1/2εijk uk,j (εijk being the levi-civita symbol) leads to a reduction of the additional material constants from five to three. based on fleck & hutchinson (1997) [12] we introduce independent expressions of ηijk and decompose the second order displacement gradient into a symmetric part ηs ijk and a remaining part ηr ijk (which is not necessarily anti-symmetric): hj hj hj z~hj �� �� �� �� ηijk ηs ijk ηr ijk η̄ij χs ijχa ij η (0) ijk η (1) ijkχa ijεmm,i figure 1. scheme of decomposition ηijk = ηs ijk + ηr ijk , ηs ijk = 1 3 (uk,ij + ui,jk + uj,ki ) , ηr ijk = 2 3 (εikl η̄lj + εjkl η̄li ) + εkjl η̄li , (3) where η̄ij = ϕj,i is the gradient of rotation, which we decompose into its symmetric and anti-symmetric parts, χs ij and χa ij , respectively: χa ij = 1 2 (ϕi,j − ϕj,i ) , χs ij = 1 2 (ϕi,j + ϕj,i ) . (4) the tensor ηs ijk is further decomposed into its spherical and deviatoric part, η(0) ijk and η(1) ijk , cf., fig. 1 . the quantity η(0) ijk is related to χa ij and the dilatation gradient εmm,i in the following manner: η (0) ijk = 1 5 ( δij η s mmk + δjk η s mmi + δki η s mmj ) ηs mmi = εmm,i + 2 3εilnχ a ln , η (1) ijk = ηs ijk − η (0) ijk . (5) as shown in [13, 14] χa ij does not influence the strain energy if symmetry of the couple stress tensor µij is assumed. as a consequence the linear isotropic strain energy density for non-simple materials of gradient type reads: umsg = 2gεij εij + λεkk εii + 2g`2 0εmm,i εkk,i + + 2g`2 1η (1) ijk η (1) ijk + 2g`2 2χ s ijχ s ij , (6) where λ and g are lamé’s constants, whereas `0, `1 and `2 denote additional material length scale parameters. these parameters are chosen to be of the dimension of a length and squared in order to guarantee a positive definite problem in the energy minimization. the normalization of the higher-order terms by g is arbitrary. 2.2. governing euler-bernoulli differential equation by using the displacement field of an eulerbernoulli beam of length l, thickness t, crosssection a, young’s modulus e, and second moment of inertia i cf., fig. 2, ux = −zdw(x) dx , uy = 0 , uz = w(x), (7) l, ei, a w(x) dw(x) dx f xy z figure 2. bending line of a cantilever where w(x) characterizes the bending line and f denotes the force at the free end, eqs. (3)–(6) lead to the strain energy density of the body. by applying the principle of virtual work to the variation of the function w(x), a triple integration by parts leads to the ordinary differential equation (ode) of the problem [15]: s d4w dx4 −k d6w dx6 = 0 , ∀ x ∈ [0, l] . (8) the resulting ode is of rank six, where s = ei(1 + 4308 225 `2 t2 ) and k = 7 5ei` 2 (9) are given constants, if a rectangular cross-section and `0 = `1 = `2 = ` is assumed. 3. finite element implementation 3.1. weak form and discretization a multiplication of eq. (8) with a test function v(x) and triple integration by parts yields in the following weak integral form of the ode: l∫ 0 ( s d2w dx2 d2v dx2 +k d3w dx3 d3v dx3 ) dx = 0 . (10) now thegalerkinmethod is applied to discretize the interval [0, l] by using linear combinations of independent base functions φα for each element e = 1, . . . , n , which are uniformly defined on the element’s coordinate 0 ≤ ζ ≤ 1: ve(ζ) = ∞∑ β=1 φβ , we(ζ) = ∞∑ δ=1 ce δφδ . (11) the general element function of this method is derived by inserting eq. (11) in eq. (10), evaluated on the domain ζ: 1∫ 0 ∞∑ δ=1 ∞∑ β=1 ( sce δ d2φδ dζ2 d2φβ dζ2 +kce δ d3φδ dζ3 d3φβ dζ3 ) dζ =0 . (12) 34 vol. 7/2017 c1-continuous solutions in second gradient elasticity 3.2. hermite elements for global c1–continuity in order to solve the present weak form of the problem, the base functions need to be differentiable three times at least. in order to guarantee that information of second gradients of the trial function w(x) is included, we ask for global continuity of the first derivative of w(x), which is called c1–continuity of the solution. therefore, we choose a linear combination of four different hermite polynomials as follows: h1 = 2ζ3 − 3ζ2 + 1 , h2 = ζ3 − 2ζ2 + ζ h3 = −2ζ3 + 3ζ2 , h4 = ζ3 − ζ2, (13) h1 h2 h3 h4 0 ≤ ζ ≤ 1 figure 3. four hermite polynoms per element which allow to influence the first derivative at each boundary of the element independently. the unit element now is a linear combination of the four hermite polynomials: ve(ζ) = 4∑ β=1 hβ , we(ζ) = 4∑ δ=1 ce δhδ (14) where ce δ are four constants per element. 3.3. structure of the element stiffnessand system matrix by using hermite elements as base functions eq. (12) can be written in the following manner: 1∫ 0 4∑ δ=1 4∑ β=1 ( sce δ d2hδ dζ2 d2hβ dζ2 +kce δ d3hδ dζ3 d3hβ dζ3 ) dζ=0. (15) the element stiffness matrix ke reads: ke δβ = 1∫ 0 ( s d2hδ dζ2 d2hβ dζ2 +k d3hδ dζ3 d3hβ dζ3 ) dζ =  ke 11 ke 12 ke 13 ke 14 ke 22 ke 23 ke 24 sym. ke 33 ke 34 ke 44  = const. (16) and is a symmetric 4× 4 matrix with constant components that depend on the material data, beam geometry, and on the length of the element. in this approach we choose equidistantly distributed elements. by special assembling of the system matrix it is now possible to connect the boundary values of an element to its neighbors and, in addition, to bring together the first derivatives in between. this will be achieved by the following structure of the system matrix k: k =  k1 δβ + k2 δβ + k3 δβ + k ···δβ + kn δβ  . (17) due to the summation of the last entries, the specific components of neighboring elements are treated as equivalent. this refers to both, the components that represent direct node values as well as to the corresponding derivatives. the solution of the entire beam bending problem is now approximated by a linear system of equations: kc = f ⇒ k\f = c , (18) where c is the vector of element coefficients and f is a right hand side, in which the external force f is implemented (here, situated at the very last node n). the system is solved using the ”backslash” operator of the commercial program matlab (lu decomposition, etc.). 4. numerical example as an example we study bending of a cantilever beam, fixed at the left hand side and loaded with a single force at the free end, as presented in fig. 2 . material and geometry data is given in tab. 1 . the material length scale parameter ` is chosen according to a literature value [3] and to measurements performed by the authors with an atomic force microscope [16, 17]. t w l e `0 = `1 = `2 f 100µm 2t 20t 1.44gpa 17.6µm 1µn table 1. dimensions, loads and material parameters the boundary condition for the fixation has been implemented by canceling the first and second row and column of the system matrix eq. (17), since, regarding the first node of the first element, the current values of deflection and the derivative of the deflection line are equal to zero. 35 christian liebold, wolfgang h. müller acta polytechnica ctu proceedings er r ×10−5 0 5 10 15 20 0 40 80 120 160 number of elements n figure 4. convergence the test for convergence with respect to higher numbers of elements n yield positive results (cf. fig. 4). the relative error of tip deflections err= wn/w1−1 per increase of elements achieves values below 0.001h. lkmberlin university of technology faculty v – mechanical engineering and transport systems institute of mechanics chair of continuum mechanics and materials theory prof. dr. rer. nat. w. h. müller table: dimensions, loads and material parameters 𝑡 𝑊 𝐿 𝐸 ℓ0 = ℓ1 = ℓ2 𝐹 100µm 2𝑡 20𝑡 1.44 gpa 17.6µm 1µn 𝑤 [m m ] 𝑥/𝐿 d𝑤 d𝑥 𝑥/𝐿 d2𝑤 d𝑥2 𝑥/𝐿 d3𝑤 d𝑥3 𝑥/𝐿 dr.-ing. c. liebold | exnum 2016, liblice | 1d example 9/10 figure 5. deflection line the deflection line of the beam solution is presented in fig. 5 . five elements are shown so that a closer look at the solution of each element becomes possible, which consists of reconstructed trial functions, cf. eq. (14)2. figure 6 presents a plot of the first derivative of the reconstructed trial functions per element and clearly demonstrates continuity in between neighboring elements and therefore c1–continuity. lkmberlin university of technology faculty v – mechanical engineering and transport systems institute of mechanics chair of continuum mechanics and materials theory prof. dr. rer. nat. w. h. müller table: dimensions, loads and material parameters 𝑡 𝑊 𝐿 𝐸 ℓ0 = ℓ1 = ℓ2 𝐹 100µm 2𝑡 20𝑡 1.44 gpa 17.6µm 1µn 𝑤 [m m ] 𝑥/𝐿 d𝑤 d𝑥 𝑥/𝐿 d2𝑤 d𝑥2 𝑥/𝐿 d3𝑤 d𝑥3 𝑥/𝐿 dr.-ing. c. liebold | exnum 2016, liblice | 1d example 9/10figure 6. first derivative of the solution as expected the global solution is not c2–continuous. this is confirmed by the jumps between the elements in their second derivative in fig. 7. such jumps are also present in the third derivative in fig. 8, but invisibly small. lkmberlin university of technology faculty v – mechanical engineering and transport systems institute of mechanics chair of continuum mechanics and materials theory prof. dr. rer. nat. w. h. müller table: dimensions, loads and material parameters 𝑡 𝑊 𝐿 𝐸 ℓ0 = ℓ1 = ℓ2 𝐹 100µm 2𝑡 20𝑡 1.44 gpa 17.6µm 1µn 𝑤 [m m ] 𝑥/𝐿 d𝑤 d𝑥 𝑥/𝐿 d2𝑤 d𝑥2 𝑥/𝐿 d3𝑤 d𝑥3 𝑥/𝐿 dr.-ing. c. liebold | exnum 2016, liblice | 1d example 9/10 figure 7. second derivative of the solution lkmberlin university of technology faculty v – mechanical engineering and transport systems institute of mechanics chair of continuum mechanics and materials theory prof. dr. rer. nat. w. h. müller table: dimensions, loads and material parameters 𝑡 𝑊 𝐿 𝐸 ℓ0 = ℓ1 = ℓ2 𝐹 100µm 2𝑡 20𝑡 1.44 gpa 17.6µm 1µn 𝑤 [m m ] 𝑥/𝐿 d𝑤 d𝑥 𝑥/𝐿 d2𝑤 d𝑥2 𝑥/𝐿 d3𝑤 d𝑥3 𝑥/𝐿 dr.-ing. c. liebold | exnum 2016, liblice | 1d example 9/10figure 8. third derivative of the solution e ∗ [g pa ] thickness t [mm] figure 9. size effect for decreasing thicknesses the sensitivity of the implemented numerical model of the modified second gradient continuum was tested for incorporation of size effect by decreasing the thickness values, while all other dimensions were scaled in parallel according to tab. 1 . the solution of the tip deflection was used in a calculation of an equivalent young’s modulus, e∗, with a euler-bernoulli analytical beam model of the conventional cauchy continuum. as plotted in fig. 9, a size effect is clearly present. for small thicknesses the equivalent young’s modulus is calculated to be about three times larger than the usual one. 36 vol. 7/2017 c1-continuous solutions in second gradient elasticity 5. conclusions based on a modified strain gradient theory for linear isotropic materials we have evaluated the eulerbernoulli beam assumptions to derive the ordinary differential equation of the problem. the weak form was derived using test functions. third order hermite polynomials have been summed up for an element formulation: these are able to access and influence first derivatives between the elements. the element stiffness and system matrix have been formulated for the problem of a cantilever beam. the resulting system of linear equations was solved numerically to determine the coefficients of the trial functions for each element. the global solution was reconstructed element-wise and first, second and third order derivatives have been calculated. it was demonstrated, that this procedure guarantees c1–continuity of the solution. this is considered to be an important quality in second gradient theories. furthermore, the size effect, measured by the authors in previous work, could be reproduced by using similar material as well as geometry data. this provides the impetus for the development of a three dimensional finite element formulation of a strain gradient continuum on the basis of hermite elements. references [1] w. j. poole, m. f. ashby, n. a. fleck. micro-hardness of annealed and work-hardened copper polycrystals. scripta materialia 34(4):559–564, 1996. [2] x. h. guo, d. n. fang, x. d. li. measurement of deformation of pure ni foils by speckle pattern interferometry. mechanical engineering 27(2):21–25, 2005. [3] d. c. c. lam, f. yang, c. m. chong, et al. experiments and theory in strain gradient elasticity. j mech phys sol 51(8):1477–1508, 2003. [4] a. w. mcfarland, j. s. colton. role of material microstructure in plate stiffness with relevance to microcantilever sensors. journal of micromechanics and microengineering 15(5):1060–1067, 2005. [5] s. cuenot, c. fretigny, s. demoustier-champagne, b. nysten. surface tension effect on the mechanical properties of nanomaterials measured by atomic force microscopy. physical review b 69:01–05, 2004. [6] x.-f. li, b.-l. wang, k. y. lee. size effect in the mechanical response of nanobeams. j of adv research in mech eng 1(1):4–16, 2010. [7] r. toupin. elastic materials with couple-stresses. arma 11:385–414, 1962. [8] r. mindlin. effects of couple-stresses in linear elasticity. arma 11:415–448, 1962. [9] r. d. mindlin, n. n. eshel. on first strain-gradient theories in linear elasticity. international journal of solids and structures 4:109–124, 1968. [10] a. eringen. nonlocal continuum field theories. springer-verlag, new york 2010. [11] m. lazar. irreducible decomposition of strain gradient tensor in isotropic strain gradient elasticity. zamm z angew math mech 2016. doi:10.1002/zamm.201500278. [12] n. a. fleck, j. w. hutchinson. strain gradient plasticity. advances in applied mechanics, academic press, new york 33:295–361, 1997. [13] c. liebold, w. h. müller. measuring material coefficients of higher gradient elasticity by using afm techniques and raman-spectroscopy. advanced structured materials, springer berlin heidelberg 22:255–271, 2013. [14] f. yang, c. m. chong, d. c. c. lam, p. tong. couple stress based strain gradient theory for elasticity. international journal of solids and structures 39(10):2731–2743, 2010. [15] s. kong, s. zhou, z. nie, k. wang. static and dynamic analysis of micro beams based on strain gradient elasticity theory. international journal of engineering science 47:487–498, 2009. [16] c. liebold, w. h. müller. applications of strain gradient theories to the size effect in submicrostructures incl. experimental analysis of elastic material parameters. bulletin of ticmi 19(1):45–55, 2015. [17] c. liebold, w. h. müller. comparison of gradient elasticity models for the bending of micromaterials. elsevier, computational materials science 116:52–61, 2016. 37 http://dx.doi.org/10.1002/zamm.201500278 acta polytechnica ctu proceedings 7:33–37, 2017 1 introduction 2 modified strain gradient theory 2.1 strain energy function 2.2 governing euler-bernoulli differential equation 3 finite element implementation 3.1 weak form and discretization 3.2 hermite elements for global c1–continuity 3.3 structure of the element stiffnessand system matrix 4 numerical example 5 conclusions references acta polytechnica ctu proceedings doi:10.14311/app.2016.5.0029 acta polytechnica ctu proceedings 5:29–37, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app assets of model metro station and their criticality tomáš kertis∗, dana procházková czech technical university in prague, faculty of transportation sciences, praha, czech republic ∗ corresponding author: kertitom@fd.cvut.cz abstract. the paper deals with the identification of protected assets in the model metro station, which is a part of critical infrastructure in praha; and with the identification of their criticality. a metro station is used by a lot of people and it involves many expensive components and devices with interdependences which form a system of systems. the system, its components and fittings are very vulnerable to damages from disasters of many kinds. the first step of ensuring metro station safety is the identification of basic metro assets which are important for safe metro operation and for human (employee and passengers) security and environment safety; and the other is determination of criticalities of considered assets with taking into account all relevant sources of hazards. these facts are input data for further processes which are important for safe metro operation under the different conditions. keywords: safety, security, metro station, assets, disasters, criticality. 1. introduction a metro is very important means of transportation in cities. therefore, to its safety it is pursued special attention, and it is part of critical infrastructure, to which it is now concentrated special attention because especially at critical situation its status predetermines the capability of human society to ensure human survival [1]. metro is composed from fix and movable parts; the fix ones are structure element, stations and tunnels with many fittings; the movable ones are trains [2]. the paper takes into account the metro stations. each metro station is equipped by many technical devices and fittings that ensure metro operation and comfort space for passengers. from safety reasons it also involves support elements for safety operation of station; they are for instance construction design, operation devices and systems, control systems, protection systems, electronic devices like lifts, escalators, air conditioning, trains and systems for train control, communication systems, staff etc. mentioned elements including the humans and personnel staff of station are in interaction each other and they create complex system prone to harm [2]. moreover, the system is mostly part of whole transportation infrastructure connections with track and next stations, material, energetic and informatics flows, and number of served persons. it is reality that devices and fittings that are very vulnerable to damages from disasters of many kinds [3]. from the protection reasons in the practice it is necessary to identify the protected assets and to establish their criticalities taking into account all relevant disasters, i.e. the sources of hazards, and to consider possible risks. this procedure is a common part of formation of safety management systems in all systems, i.e. also in railway domain. the first step is the identification of basic metro assets that are important for safe metro operation and for human (employee and passengers) security; and the other is the determination of criticalities of these assets. 2. critical assets and critical infrastructure protection for ensuring the humans security and development, there is necessary the safe human system [3]. basic assets of human system called basic public assets are: human lives and health, property and welfare, environment, and also critical infrastructures and technologies. it means that the critical infrastructure is one of important asset of human system. therefore, its protection is specially ensured in the eu, usa, germany, canada etc. [1]. in the czech republic critical infrastructure it includes nine infrastructures [1] [4], i.e. infrastructure for: • energy (electricity; gas; heat energy; oil and petroleum products) supplies, • handling with water (drinking and industrial water; secure and manage the surface water and underground water resources; waste water system), • food supplies and agriculture operation (food production; care for food; agricultural production), • health care (pre-hospital emergency care; hospital care; the protection of public health; the production, storage and distribution of pharmaceuticals and medical devices), • transportation system (road; rail; air; water), • cyber-communication and information systems (fixed telecommunication network services; services of mobile telecommunication networks, radio communication and navigation; television and satellite 29 http://dx.doi.org/10.14311/app.2016.5.0029 http://ojs.cvut.cz/ojs/index.php/app tomáš kertis, dana procházková acta polytechnica ctu proceedings communications radio; postal and courier services; internet and data services), • the banking and financial sector (management of public finance; banking; insurance; the capital market), • emergency services (fire rescue brigade cr; units of fire protection for area coverage; police of czech republic; army of czech republic; radiation monitoring; forecasting, warning and mouthpiece for the service etc.), • public administration (state administration and self-administration; social protection and employment; the state social support and social assistance; performance of judiciary and prison system). the transportation infrastructure includes road, rail, air and water infrastructure. each of mentioned infrastructures is composed from elements and line structures. the protection of transportation infrastructure in the czech republic is only concentrated to the elements according to the crisis act (act no. 240/2000 col.). it means that metro station is key asset, and therefore, we deal with its safety. transportation system provides the transportation of persons and goods. it includes all modes of transport, which, under the coordination of the various transport systems work together and creates a logistical network. the transportation network, together with energy network can be considered as the foundation of economic prosperity of the state. the transportation network consists of separate parts that make up self-reliant closed units. each unit is a unit, the basis of which is the type of transport, accompanied by complex operational and administrative parts, which forms subsystems. the characteristic feature of technological units is their specialized ability to separate traffic operation. it is necessary to recognize that the individual parts are bound by the rules of their transport logistics, which coordinates the activities. in the czech republic the transport network consists of: rail transport system; the road transport system; the air transport system; and water transport system. transport system and its subsystems are vulnerable to natural disasters, the traffic accidents, technological accidents of facilities and buildings being in their vicinity, crimes, terroristic attacks, organizing accidents, war etc. [1] [3] [4]. figure 1 shows the processes that are sources of disasters [3]. to ensure safety of each entity, i.e. each infrastructure and their components it is necessary to manage the safety by the way as is expressed by process model in figure 2 [1] [5]. the safety needs to be formed on all levels of governance [3] [4] [5], as it is depicted in figure 3. the ways of coping with risks are shown in figure 4 [3] [4] [5]. each real system is composed from various heterogeneous subsystems, links and flows among them, so-called inter and intra-dependences. subsystems figure 1. sources of disasters in the human system [3]. figure 2. process model for formation of safety of entity under account [1] [5]. figure 3. levels of safety management [3] [4] [5]. figure 4. measures used for get over risks connected with disasters [3] [4] [5]. 30 vol. 5/2016 assets of model metro station and their criticality is possible categorized as controlled and control systems in the view of control. for improving system parameters (dependability, security, safety, etc.) the support systems are implemented, for instance a protection system reducing the risks. a subsystem can be classified as safety related, the safety related system carries out very important functions which failures or malfunctions could lead to improving the risks and event to accidents [6]. from the protection reasons on the concept of integral safety of complex technological facilities in the practice it is necessary to identify the protected assets and to establish their criticalities taking into account all relevant sources of hazards. 3. data on metro in praha and metro station model stations of metro in the praha capital are not the same; they have differences due to their locations in different site conditions and demands in the time of their building. all are threatened by disasters that threaten the praha capital, i.e. its buildings, structures and facilities, and locally also by specific phenomena that are associated with local conditions, which are connected with local vulnerabilities. therefore, for research needs we developed a model station that has characteristics that are common to all the stations of reference system taking into account the praha land-use plan [7] and the praha metro documentation [2] [8] [9] [10]. the structural parts of praha metro were constructed according to the building law (to 2006 act. no. 50/1976 col., from 2006 act no. 183/2006 col.), the engineering parts and cyber technique were harmonised with demand of building law so they might obtain permission for operation. the metro operation control is performed according to the standards [11] [12] and it satisfies requirements given in standards [13] [14] [15]. the model metro station contains all elements, links and flows that are same in all metro stations because they are determined by the requirements of mentioned building law; i.e. we follow general features and do not study the details in structure, devices, fittings of both, the technical and the cyber domains. the detail studies of individual stations reveal real vulnerabilities that cannot be open to the public from the safety reasons. such detail studies have been performed for the metro operator, and they are used for metro safety upgrade. the sources of phenomena that can damage the metro system will be discussed in the next chapter in which we use the advanced principle based on all-hazard-approach [16]. considering the principle defence-in-depth described for complex technological facilities in [17] we shall mostly concentrates to the management units that keep the sufficient level of safety at normal, abnormal and critical conditions. safety management system of metro (sms) has central control system and controlled systems in each metro model station, figure 5. it is very complex distributed system that involves controlled, control and protection subsystems, their interdependences, operation states and conditions. figure 5. control and controlled system in metro model station [6]. metro station has subsystems stationary, track and on-board. on the basis of results in [6] obtained by application of principles given in [17] we select the main metro station assets in individual main parts. technological parts and some support subsystems of controlled system include assets: (1.) energetic devices: transformer substations and distribution transformers, (2.) communication equipment: communication cables, vhf connection with trains; passengers information systems including automatic check-in; communication systems for passengers and staff; cctv, telephone, public address; clocks and fire alarms; protection systems and signalling, (3.) machinery: escalators; pump stations in nodes in stations and between them; elevators; workshops and warehouses maintenance stations, (4.) air conditioning, (5.) mobile machines and devices: rolling-stock; devices and substances for cleaning, including the containers, cleaning machines, ladders, scaffolding for cleaning the lighting systems; fire protection equipment, (6.) next important equipment: security keys and alarm buttons; equipment for fire alarm start; traction devices and lighting; track devices, the main water shut; moving stairs, plates, signal panel for machinery devices; closing equipment (shutters). praha metro control centre has denotation operation control centre occ. it has supervisory control and data acquisition (scada) system that monitors technological facilities and processes and enables their control. its variant used in the czech republic has denotation asdř-d (automatic dispatcher system for transport control). the scada has several parts that are responsible, for: transport (ugtms urban guided transport management and command / control system); energetic tasks; technologies; communication and lighting. the control system involves following assets: • train dispatcher (surveillance and control of trains); and occ nodes, station nodes, nodes for automatic route setting system – asdř-d, 31 tomáš kertis, dana procházková acta polytechnica ctu proceedings • energetic dispatcher – asdř-e, • technological dispatcher – asdř-t, • lighting system dispatcher – adrř-o, • communiation and protection systems dispatching, • fire dispatching, • depot dispatching for train services and maintenance. for a model metro station, the control system involves station that are also assets: • station nodes of control system, • station node for automatic route setting, • station nodes for connection of energetic and technological dispatching, • station nodes for central lighting control system, • station interacting with dispatchers (communication, protection, operation, fire men). in the railway practice context a protection system is primary understand as system needed to mitigation of risks connected with train operation. it is also asset. they are: • station protection systems (esa 11 m), • wayside protection systems (ažd 71, esa 11 m), • train protection systems (matra and on-board units). the metro stations also ready on flows that are also assets, it goes on: • energetic flow, • information flow, • central dispatching and station nodes of control system, • central dispatching and station communication units, • station nodes of control system and protection systems, • station nodes of control system and communication system, • protection systems and technologies (on the track and on-board)-telephone connection between central dispatching (occ) and station, • telephone connection between central dispatching and trains. controlled, control and support (protection) systems are not just electronical and mechanical devices, they can be also organization processes, other communication and information parts of the system, human resources and place which shall be taken into account in the assets identification context. in the czech practice the european directives and standards are respected for safety management of railway systems; there are taken in account: common safety methods [18] [19], en 50126-1 [13], clc/tr 50126-2 [20], en 62290 [14] [15], en 92267 [21]. railway domain is regulated by european directive 2004/49/ec [18] that establishes duties for national authorities. the mentioned directive refers also to railway interoperability and safety. according to the directive regulation 402/2013 on the common safety methods for risk assessment [19], there take into account only risks connected with human harm. reason is an effort to ensuring the safety of passengers, employees, level-crossing users, unauthorised persons on the track and to ensuring the total safety on the basis of the above categories. weakness of mentioned directive is that it does not consider other assets which affect to people lives and healthy, it means public assets, important technological parts, facilities, any processes and infrastructure functions. the directives are insufficient for critical infrastructure needs and it does not provide assets protection. moreover, mentioned directives are not apply to special railway systems like metro. railway standard en 50126 [13] defines the specification and demonstration of reliability, availability, maintainability and security (rams) for a railway system including the metro. the standard defines whole life cycle including the concept and design of the system, through operation, maintenance, reconstruction, and up to decommissioning of the system. risk management is included there, but it considers only risks affect to human, it means risk r = rate (of accidents) x degree of severity (of harm); according to clc/tr 50126-2:2007 [20] in this context harm may imply: human harm (causing injures, fatalities); and also environmental harm (damage to property, spread toxic substances, other impacts, etc.). most railway safety studies tend to concentrate on human harm. (clc/tr 50126-2:2007). security requirements to integral safety improving are not still covered. standard en 62290 [14] [15] defines requirement for urban guided transportation management and control / command system which is split into 5 degrees of automation. each degree of automation (goa) has specific demands and set of functional requirements. although a standardisation commission has been established, no standard with safety requirements has been prepared [21]. better approach is included in en 62267 [21] for fully automated guided transport (augt). the standard refer to en 50126 [13] about risk management but it imposes demand on assets protection. identified protected assets by the standard are: persons (passengers, staff, external emergency services, public); and property, shall be defined by railway authority and operator (infrastructure of whole system, trains, equipment, etc.) [22]. the european standard is intended to very short group of railway system and it does not establish methods for determining the protected assets. the characteristic pattern of model metro 32 vol. 5/2016 assets of model metro station and their criticality station is composed from data mentioned above and the facts that are summarised in [11] [12] [13] [14] [15] [18] [19] [20] [21] [22]. 4. disasters considered in research since in the czech republic there is held long-term use of building codes and high quality engineering practice there are metro stations relatively well protected against design disasters of natural and technological origin that belong to the term all-hazardapproach [16], which ensures fixed safety level in these cases. the problems are connected with further disasters that belong to the term all-hazard-approach [16] but they were been introduced into practice later. it involves the following types of disasters: • so called organisational accidents [3] [4] [5] [17] because these disaster sources have been considered since the end of 80s of last century, • having the origin in cyber domain or in interdependences of different nature in system [3] [4] [5] [17] because these disaster sources have been considered since the end 90s of last century, • damaging phenomena caused by intentional human activities as crime or terroristic attack [3] [4] [5] [17] because these disaster sources come to size after 2000. from above reasons last designated disasters were not considered in original designing the metro stations, and therefore, we will pay special attention to them. data for the research we obtained from the sources on the praha metro [2] [8] [10]. all above mentioned metro station assets are threatened by disasters. for praha capital and its facilities according to [5] [7] the following disasters are relevant: (1.) the results of the processes inside and outside the earth: flood; tornado; earthquake; liquefaction of the ground; landslide, (2.) the results of the human body, human behaviour and processes in human society: epidemics; pandemics; failure of the stability of human society (welfare disruption, criminality); assault; terrorist attack; attack using the chemical, nuclear, radiological and biological (cbrne) weapons; armed conflict; war, (3.) results of the processes and activities installed by people: industrial accident; accident during the transport or storage of hazardous substances; accident at transportation; failure of critical infrastructure; failure in economy; failure in cyber infrastructure; failure of supply chains; loss of serviceability, (4.) interaction of earth and environment to activities of people: disruption of bedrock stability due to vibration; air pollution; water pollution; rapid climate changes; migration of large groups of people, (5.) internal dependences in the human system (natural or man-made): organizational accident; failure of flows of raw materials and products; disturbance in the flow of energy; failure in the information flow. 5. method of determination of model netro assets criticality to ensure the safety of model metro station it is necessary to know the criticality of whole metro system and its components, i.e. in followed case it is the model metro station [17]. as it was said above, each metro station is threatened by disasters, i.e. its safety depends on the quality of the work with the risks [5] [17]. safety and risk are together in some way in relation, but they are not complementary variables (complementary value to the safety is the criticality [17]). the criticality is a result of the exposure to risk factors. there are analysed the different types of factors: factors of human activity, decision-making and management, factors in the nondistinguishability of reality (because there are random and knowledge uncertainties). according to [17] the criticality of technological system indicates a threshold value that means it the values are below this threshold, so the status is demanded (subcritical) and vice versa. the assessment of criticality of real system is not a trivial matter, because the elements and whole have different roles for different conditions of active, reactive, amplifying or dampening (but not additive), and among the sub systems of systems of system, which is a real entity, and each model metro station. therefore, in accordance with [17] for its determination we use the method of risk engineering the checklist [23], which for complex technological systems is given in table 1. because each system of systems (in our case metro station) is a very complex system, the behaviour of which cannot be easily predicted, so the assessments from the perspective of the different sectors are often different, and therefore, it is necessary to choose the method that conflicts does not override, but it is trying to reasonably consider them [23]. therefore, it was used the method, based on the expert opinion of five experts who knew enough the metro and its operation, have been independent and were from the areas: • safety and protection of human health at work, • protection of property, • economy of operation, • protection of passengers, • technical and functional safety of operation. the evaluation was carried out separately for each significant disaster using the value scale listed in table 2. 33 tomáš kertis, dana procházková acta polytechnica ctu proceedings i question asst note 1 1. has the technological facility to incorporate the principles of inherent safety? 2. has the control system of a technological facility (sms) set the basic control functions, alarms and the response of the operator set up so that the technological facility in normal (steady) state? 3. has management system (sms) instrumentation (built-in safety instructions) and relevant physical barriers, which at derogate from the normal state to keep technological system in a good condition, i.e. they prevent the occurrence of unwanted phenomenon? the operation is successful, when, after the occurrence of the abnormal state the technological facility will return to normal as a result of resilience or after the application of corrective measures (clean-up, repair, replacement of parts). 4. has management system (sms) for the case of loss of control, i.e. critical conditions measures for emergency response that mitigate impacts on technological facility system and ensure the capability to return to a normal state? operation of a technological object is successful, if it is a good continuity plan, which ensures that the technological facility shall ensure all the necessary tasks. 5. does management system (sms) for the case of loss of control, i.e. supercritical (beyond design, extreme) conditions the measures for: maintaining the operability of the technological system following its repair and maintenance; item and measures to ensure the protection of public assets (people, the environment and other assets) in the surroundings of technological facility? . ............................................................................................................................. ........ ..... n 1. has the technological facility to incorporate the principles of inherent safety? 2. has the control system of a technological facility (sms) set the basic control functions, alarms and the response of the operator set up so that the technological facility in normal (steady) state? 3. has management system (sms) instrumentation (built-in safety instructions) and relevant physical barriers, which at derogate from the normal state to keep technological system in a good condition, i.e. they prevent the occurrence of unwanted phenomenon? the operation is successful, when, after the occurrence of the abnormal state the technological facility will return to normal as a result of resilience or after the application of corrective measures (clean-up, repair, replacement of parts). 4. has management system (sms) for the case of loss of control, i.e. critical conditions measures for emergency response that mitigate impacts on technological facility system and ensure the capability to return to a normal state? operation of a technological object is successful, if it is a good continuity plan, which ensures that the technological facility shall ensure all the necessary tasks. 5. does management system (sms) for the case of loss of control, i.e. supercritical (beyond design, extreme) conditions the measures for: item maintaining the operability of the technological system following its repair and maintenance; item and measures to ensure the protection of public assets (people, the environment and other assets) in the surroundings of technological facility? table 1. identification of deficiencies for specific disasters in a given territory, i = 1, 2, ..., n, i.e. assessment of the criticality of the viewpoint of the application of access the defence-in-depth. 34 vol. 5/2016 assets of model metro station and their criticality criticality rate values [%] extremly high – 5 more than 95 very high – 4 70-95 high – 3 45-70 middle – 2 25-45 low – 1 5-25 negligible – 0 less than 5 table 2. value scale according to [17]. the resulting rates of criticality for each item and disaster are set as median [23] from particulars determined by individual experts. 6. criticality of assets in model metro station on the basis of the procedure described in the previous chapter it was obtained a set of values that are listed in table 3. the numbers in table 3 indicate the following rates of criticality: • 0 – given disaster does not have a direct impact on the metro station and its operation, • 1 – given disaster has low impact on the metro station and its operation, • 2 – given disaster has middle impact on the metro station and its operation, • 3 – given disaster has high impact on the metro station and its operation. from table 3, it follows that the rate of criticality is high in many cases. while it is moderate, i.e. it is not very high or extreme, it is necessary in the frame of public interest to supplement the measures in all cases where the criticality rate is high. on the basis of the data referred to such cases according to [17] [24] it is necessary to perform in all cases where the criticality rate is 3 the following: • the analysis of the ability/competence of operator of metro to handle with emergency situations in the station and in the infrastructure, • the inventory of available resources for quick and proper response to the emergency situation in a metro station in the subway, • the assessment of current vulnerability of items of metro stations and the entire metro subway, • the specification of the coordination of activities to support the continuity of subway stations and underground infrastructure, • the division of responsibilities for actions to promote the continuity of the subway stations and underground infrastructure, • the setting up the organisational instructions and features to support the renovation of subway stations and underground infrastructure, • the establishment of criteria for the selection of main features of elements of subway stations and underground infrastructure, • the determination of support processes that support the main features of subway infrastructure, • identification of key personnel, to ensure the continuity of the subway stations and underground infrastructure, • prioritizing the main functions on the basis of the criticality of time, sequence of key recovery processes and personnel capacity. 7. conclusion from the protection reasons on the concept of integral safety of complex technological facilities in the practice it is necessary to identify the protected assets and to establish their criticalities taking into account all sources of hazards. the results of performed research show that metro stations have a certain level of safety (according to [17] it holds that level (rate) of safety = 1 – criticality rate). however, it is necessary to carry out the measures referred to in the previous chapter, because there are items for which in the occurrence of large (i.e. beyond design extreme) disasters there are get to significant impacts of disasters, which have the ability to disrupt seriously the metro station and the entire infrastructure. it means that present standards and legislative do not provide sufficient range for integral safety, including the safety of important assets and systems that predispose sufficient human security and human society development. references [1] d. procházková. bezpečnost kritické infrastruktury, 2012. isbn 978-80-01-05103-0. [2] dopravní podnik v praze. dp kontakt: časopis zaměstnancøu dopravního podniku hl. m. prahy, akciové společnosti, 1999-2005. isbn 1212-6349. [3] d. procházková. strategické řízení bezpečnosti a udržitelného rozvoje území, 2011. isbn 978-80-7251-243-0. [4] d. procházková. krizové řízení pro technické obory, 2013. isbn 978-80-01-05292-1. [5] d. procházková. analýza a řízení rizik, 2011. isbn 978-80-01-04841-2. [6] t. kertis. bezpečnostní plán vybrané stanice metra, diploma thesis. praha 2015. [7] praha, hl. m. archives for strategis and land-use planning. [8] metroweb [online], 2015. [2015-03-15], http://www.metroweb.cz/. [9] kolektiv pracovníkøu metroprojektu praha a.s. publikace iv. [online], 2008. http://www.praha.eu/ public/0/a3/da/186337_4_publikace_iv._c2.pdf. [10] unicontrols a.s. case study: metro praha, 2014. 35 http://www.metroweb.cz/ http://www.praha.eu/public/0/a3/da/186337_4_publikace_iv._c2.pdf http://www.praha.eu/public/0/a3/da/186337_4_publikace_iv._c2.pdf tomáš kertis, dana procházková acta polytechnica ctu proceedings assets/disasters fl oo d ea rt hq ua ke li qu ef ac tio n of gr ou nd g as re le as e ep id em ic pa nd em ic w el fa re di sr up tio n c rim e in te nt di sr up tio n te rr or ist ic at ta ck a tt ac k w ith c b r n e a rm ed co nfl ic t w ar in du st ria la cc id en t le ak ag e of ha za rd ou s tr affi c ac ci de nt b la ck ou t d isr up tio n of ec on om y human lives and healthy 1 1 1 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 1 1 1 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 1 1 1 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 property and places 1 1 1 2 0 0 0 2 3 3 3 3 3 1 3 2 2 0 1 1 1 2 0 0 0 2 3 3 3 3 3 2 3 3 2 0 2 1 1 2 0 0 0 2 3 3 3 3 3 2 3 3 3 0 energetic devices 1 1 1 2 0 0 0 2 3 3 3 3 3 1 3 2 2 0 1 1 1 2 0 0 0 2 3 3 3 3 3 2 3 3 2 0 2 1 1 2 0 0 0 2 3 3 3 3 3 2 3 3 2 0 communication equipment 2 2 2 2 0 0 0 2 3 3 3 3 3 1 3 2 3 0 2 2 2 2 0 0 0 2 3 3 3 3 3 2 3 3 2 0 2 2 2 2 0 0 0 2 3 3 3 3 3 2 3 3 2 0 machinery 1 1 1 2 0 0 0 2 3 3 3 3 3 1 3 2 2 0 2 2 2 2 0 0 0 2 3 3 3 3 3 2 3 3 2 0 3 3 3 3 0 0 0 3 3 3 3 3 3 3 3 3 2 0 air conditioning 1 1 1 2 0 0 0 2 3 3 3 3 3 2 3 2 2 0 2 2 2 2 0 0 0 2 3 3 3 3 3 2 3 3 2 0 3 3 3 3 0 0 0 3 3 3 3 3 3 3 3 3 3 0 mobile machines and devices 1 1 1 1 0 0 0 3 3 3 3 3 3 3 3 3 3 0 1 1 1 2 0 0 0 2 3 3 3 3 3 2 3 3 2 0 2 1 1 3 0 0 0 3 3 3 3 3 3 3 3 3 0 0 next important equipment 1 1 1 1 0 0 0 3 3 3 3 3 3 3 3 3 3 0 1 1 1 2 0 0 0 2 3 3 3 3 3 2 3 3 2 0 2 1 1 3 0 0 0 3 3 3 3 3 3 3 3 3 0 0 station nodes of control systems of metro system 1 1 1 0 0 0 1 1 1 1 1 1 1 1 3 1 1 0 1 1 1 0 0 0 2 1 1 2 1 1 2 1 3 1 1 0 3 2 2 0 0 0 3 2 2 3 3 2 2 2 3 2 2 0 protection systems 1 1 1 0 0 0 1 1 1 1 1 1 1 1 3 1 1 0 1 1 1 0 0 0 2 1 1 2 1 1 2 2 3 1 1 0 3 2 2 0 0 0 3 2 2 3 3 2 3 3 3 2 2 0 linkages and flows 1 1 1 0 0 0 1 1 1 3 3 3 3 3 3 3 3 3 1 1 1 0 0 0 2 1 1 3 3 3 3 3 3 3 3 3 3 2 2 0 0 0 3 2 2 3 3 3 3 3 3 3 3 3 table 3. criticality of assets in metro station. [11] čr. čsn en 13816 (269389) doprava – logistika a služby – veřejná přeprava osob – definice jakosti služby, cíle a měření, 2003. [12] čr. čsn en iso 9001:2009 (01 0321) systémy managementu kvality – požadavky, 2009. [13] čr. čsn en 50126-1 (333502) drážní zařízení – stanovení a prokázání bezporuchovosti, pohotovosti, udržovatelnosti a bezpečnosti (rams): část 1: základní požadavky a generický proces, 2001. [14] čr. čsn en 62290-1:2006 (33 3530) drážní zavrízení – systémy řízení městské dopravy s vyhrazenou vodicí dráhou: část 1: systémové principy a základní pojmy, 2007. [15] čr. čsn en 62290-2:2011 (33 3530) drážní zařízení – systémy řízení městské dopravy s vyhrazenou vodicí dráhou: část 2: specifikace funkčních požadavkøu, 2009. [16] fema. guide for all-hazard emergency operations planning [online], 1996. http://www.fema.gov/pdf/plan/slg101.pdf. [17] d. procházková. bezpečnost složitých technologických systémøu, 2015. isbn 978-8001-05771-1. [18] eu. directive 2002/49/ec of the european parliament and of the council of 25 june 2002 relating to the assessment and management of environmental noise – declaration by the commission in the conciliation committee on the directive relating to the assessment and management of environmental noise, 2002. 36 http://www.fema.gov/pdf/plan/ slg101.pdf vol. 5/2016 assets of model metro station and their criticality [19] eu. regulation 402/2013 on the csm for risk assessment and repealing regulation 352/2009, 2002. [20] celenec. clc/tr 50126-2:2007 railway applications. the specification and demonstration of reliability, availability, maintainability and safety (rams). guide to the application of en 50126-1 for safety, 2013. [21] iec. project iec 62290-3 ed. 1.0: railway applications – urban guided transport management and command/control systems – part 3: system requirements specifications, 2015. [22] čr. čsn en 62267 (33 3532) drážní zařízení – automatizovaná městská doprava s vyhrazenou vodící dráhou (augt) – bezpečnostní požadavky, 2009. [23] d. procházková. metody, nástroje a techniky pro rizikové inženýrství, 2011. isbn 97880-01-04842-9. [24] d. procházková. základy řízení bezpečnosti kritické infrastruktury, 2013. isbn 978-80-01-05245-7. 37 acta polytechnica ctu proceedings 5:29–37, 2016 1 introduction 2 critical assets and critical infrastructure protection 3 data on metro in praha and metro station model 4 disasters considered in research 5 method of determination of model netro assets criticality 6 criticality of assets in model metro station 7 conclusion references 215 acta polytechnica ctu proceedings 1(1): 215–221, 2014 215 doi: 10.14311/app.2014.01.0215 highly magnetized accreting pulsars: are there accreting magnetars? pere blay1, pablo reig2, vı́ctor reglero1 1ipl, university of valencia, spain 2university of crete, greece corresponding author: pere.blay@uv.es abstract 2s 0114+650, gx 301-2, igr j16358-4726, x per, 4u 2206+54, sxp 1062, and 3a 1954+319 are thought to possess high magnetic fields. they have recently been named accreting magnetars, or highly magnetized accreting pulsars. in this work their properties are reviewed. within the context of their observational properties (mainly from integral data), and the recent models of accretion onto highly magnetized neutron stars, their similarities and differences are analyzed. the aim is to find a common framework to understand the evolution (in terms of past and present history) of these sources, and to establish the basis of a possible new kind of accreting sources. two of these sources, namely x per and 4u 2206+54, contain a massive main-sequence companion, while the rest are supergiant x-ray binaries or symbiotic systems. the variety of astrophysical scenarios represented by this set is wide, therefore the study of these systems is also important in order to establish commonalities between the different types of accreting x-ray pulsars and to study the possible evolutionary links between them. keywords: stars: binaries: close stars: magnetars stars: neutron x-rays: binaries. 1 introduction magnetars are neutron stars with bright persistent xray emission (on the order of lx ∼ 1033−36ergs−1) and spin periods on the order of a few seconds. they show a very drastic spin period evolution, with large spin period derivatives and a long-term spin down tendency. the fact that they are isolated objects, together with the difficulties in considering their rotational energy as the source of the observed bright x-ray emission, are key issues in order to postulate their highlymagnetized nature (with extreme magnetic fields, on the order or greater than ∼ 1014gauss). magnetars are usually grouped into two subclasses, namely anomalous x-ray pulsars (axps) and soft gamma-ray repeaters (sgrs). for a review of magnetars see, for example, panchapakesan (2003) and rea & esposito (2011). high mass x-ray binary systems (hmxrbs) contain a massive companion (≥10m�) and a neutron star or a black hole. the evolution of neutron stars in hmxrbs is affected directly by the wind plasma in which they are immersed (originating from the massive companion). the ambient plasma interacts with the magnetic field of the neutron star modifying its spin period evolution. neutron stars are born as rapid rotators. the ambient plasma removes rotational energy from the neutron star and transports it outwards and the neutron star suffers an spin-down process, which goes on until the ambient matter becomes radiative, cools rapidly, and accretion can take place. the time spent in this initial spin-down epoch will determine the final x-ray pulsar rotational period which will be an equilibrium period which resulting from the balance of two forces: the magnetic field pressure (which stops and drags the in-falling matter), and the inward pressure exerted by the ambient plasma. initial modelings (see, for example, illarionov and sunyaev, 1975) predicted that the slowest reachable pulse period of a neutron star in a binary system is on the order of ∼500 s. revisions of these initial models (see, for example, davies and pringle, 1981) relaxed this limit, allowing longer spin periods but only associated with higher neutron star magnetic fields. the possible presence of magnetars in some accreting hmxrbs, in which a slowly rotating neutron star has been found, has been proposed recently by a number of authors (see, for example, li & van den heuvel 1999, finger et al. 2010, reig et al. 2012, ikhsanov & beskrovnaya 2010, doroshenko et al. 2010, patel et al. 2007, popov & turolla 2012, bozzo et al. 2008). our goal is to compare the observational properties of these systems and determine which observational parameters are more suitable to derive the strength of the magnetic field. we also want to stress the difficulties in determining some of the properties of these systems when 215 http://dx.doi.org/10.14311/app.2014.01.0215 pere blay, pablo reig, vı́ctor reglero considering only the long-term analysis (i.e., comparing pulse periods from different epochs), or the temptation to identify spectral features as cyclotron resonant scattering features (crsf) and derive magnetic field values from their central energy. despite the small number of systems, the variety of astrophysical scenarios represented by this set is wide, from main sequence accreting binary systems (x per, sxp 1062 and 4u 2206+54) to supergiants (2s 0114+65 and gx 301-2), and even symbiotic systems (igr j16358-4726 and 3a 1954+319). in this sense, the study of these systems is important also to establish commonalities between the different types of hmxrbs and to study the possible evolutionary links between them. in this work we will review the observational properties of some of these systems and we will try to establish the scientific rational to develop a deeper analysis of their common properties and evolutionary status. due to the large inhomogeneity in the energy ranges and sets of data available in the literature, we have started an analysis of these systems by using integral/ibis/isgri1 data, setting up common energy ranges, spectral resolutions, and performing a homogeneous timing analysis. 2 the candidates a number of hmxrbs have already been proposed to contain highly magnetized neutron stars, namely 2s 0114+65 (li & van den heuvel 1999), 4u 2206+54 (reig et al. 2012, finger et al. 2010), x per (doroshenko et al. 2012), gx 301-2 (ikhsanov & finger 2012), igr j16358-476 (patel et al. 2007). there are also suggestions that sxp 1062 (fu & li 2012) and 3a 1954+319 (marcu et al. 2011) contain a highly magnetized neutron star. attempts have also been made to try to explain the properties of sfxts with the presence of a highly-magnetized neutron star with some degree of success (see bozzo et al. 2008 ) . a complete list of sources has been compiled in table 1. despite the fact that there are peculiarities in each of these systems which make difficult to group them as a kind (see, for example, reig et al. 2012, blay and reglero 2013), we can summarize their overall commonalities: • slowly rotating neutron stars (pspin slower than 500 s), with • high magnetic fields (larger than 1013 gauss) • most of them show a long-term spin-down tendency the neutron star properties in these systems are different from those of magnetars, for this reason the terms magnetar-like, or magnetar-descendant (making reference to a possible evolution from a neutron star born as a magnetar), have also been used to identify these sources (reig et al. 2012, blay and reglero 2013). table 1: list of sources. source pspin (s) porb (d) type 4u 2206+54 5560 19.2 ms donor x per 864 250 bexrb 2s 0114+650 9700 11.6 sxrb gx 301-2 680 41.498 sxrb igr j16358-4726 5880 −− symbiotic 3a 1954+319 19080 −− symbiotic sxp 1062 1062 ∼300 bexrb after 10 years of operations of the integral satellite, a very complete and homogeneous long-term database of observations of all these sources has been compiled. we have analysed all public observations in which 4u 2206+54, x per, 2s 0114+65, igr j16358476, and gx 301-2 were in the field of view of integral/ibis/isgri. the behavior of these source is similar in long time scales, with transient emission in the form of bursts or peaks and more or less continuous detection. they all show the typical behavior of wind accreting systems (although x per is a bex, it has been proposed that its behavior resembles that of wind-fed systems because of the large orbital distance, which will keep the neutron star away from the be disk, see doroshenko et al. 2012). the light curves, in every case, are complete enough to develop both short and long-term analysis of the spectral and timing properties of these systems. the magnetic properties of the neutron stars in these systems have been investigated/explained mainly in these terms: • spin period (neutron star evolutionary considerations) • spectral features (cyclotron resonant scattering features, crsf) 1integral (international gamma-ray laboratory) is an esa mission with contributions from usa and russia, with two high-energy imagers (ibis, working in the energy range 15 kev−10 mev , and jem-x sensitive in the 3−35 kev energy range) and one spectrometer (spi, sensitive in the range 20 kev−8 mev). ibis, in turn, has two detector layers, isgri, for the lower energy band,15 kev−1 mev, and picsit working in the 175 kev−20.4 mev energy range. a detailed description of the mission can be found in winkler et al. (2003) 216 highly magnetized accreting pulsars: are there accreting magnetars? with regard to the spin-period history, according to ikhsanov (2007), the maximum spin period reachable by a neutron star can be related to the intensity of its magnetic field and the quantity of accreted matter (i.e., mass accretion rate). the latter quantity is considered to be directly proportional to the x-ray luminosity of the source (see, for example, finger et al. 2010). the relationship between these quantities is: pmax = 15000µ 16/21 32 m −4/21 ns ( ṁ 1015gs−1 )−5/7s (1) where µ32 is the dipole magnetic moment (in units of 1032gcm−3) and mns the mass of the neutron star (in units 1.5m�), and ṁ is the mass accretion rate. a more recent calculation of quasi-spherical accretion by popov and turolla 2012, yields this relationship, directly in terms of the magnetic field intensity: b12 ∼ 8.1ṁ 1/3 16 v −11/3 300 ( p1000 porb,300 )11/2 (2) where b12 denotes the magnetic field in units of 1012 gauss, ṁ16 is the mass accretion rate in units of 1016gs−1, v300 is the wind velocity in units of 300kms−1, p1000 is the spin period in units of 1000s, and porb,300 is the orbital period of the system in units of 300d. on the other hand, a direct measurement of the magnetic field of the neutron star is possible when its high-energy spectrum shows crsfs. crsfs are due to the splitting of energy levels of the electron in the presence of a magnetic field. therefore the scattering of x-ray photons by these electrons is produced at quantized landau levels producing the absorption-like features seen in the x-ray spectra of many hmxrbs (see schönherr et al. 2007). the magnetic field strength can be calculated from the position of the crsf by the formula: ecrsf = 11.6 b12 (1 + z) (3) where z is the gravitational redshift. it should be noted that this redshift, and consequently the measured magnetic field, will depend on the height over the neutron star surface where the crsf is formed. in the next sections, we will review these methods when applied mainly to some of sources listed in table 1. 3 magnetic field determination via spin period evolution fig. 1 shows examples of spin period histories of 4u 2206+54, 2s 0114+650, igr 16358-4726, and x per. 53600 53700 53800 53900 54000 54100 54200 54300 mjd 5300 5400 5500 5600 5700 5800 p sp in ( s) 4u 2206+54 53000 53500 54000 54500 55000 55500 56000 mjd 2.00 2.25 2.50 2.75 3.00 p sp in (h ) 2s 0114+650 54000 54200 54400 54600 54800 55000 55200 55400 mjd 830 831 832 833 834 835 836 837 838 839 840 841 842 843 p sp in ( s) x per 53000 53500 54000 54500 55000 55500 56000 mjd 5780 5800 5820 5840 5860 5880 5900 p sp in ( s) igr j16358-4726 figure 1: spin period evolution of 4u 2206+54 (top panel), 2s 0114+650 (second panel from the top), x per (third panel from the top), and igr 16358-4726 (lower panel) as obtained from integral/ibis/isgri data in the 20-40 kev energy range. 217 pere blay, pablo reig, vı́ctor reglero 0.0001 0.001 0.01 0.1 1 fl ux ( co un t s -1 k ev -1 ) 20 40 60 80 100 120 140 160 180200 energy (kev) -0.04 -0.02 0 0.02 0.04 re si du al s 4u 2206+54 0.01 0.1 1 fl ux ( co un ts s -1 k ev -1 ) 20 40 60 80 100 120 140 160 180200 energy (kev) -0.4 -0.2 0 0.2 0.4 re si du al s 2s 0114+650 0.0001 0.001 0.01 0.1 1 fl ux ( co un t s -1 k ev 1 ) 20 30 40 50 60 70 80 90 100 200120 140 160 180 energy (kev) -0.02 -0.01 0 0.01 0.02 re si du al s x per figure 2: the 20-200 kev spectra of 4u 2206+54 (top panel), 2s 0114+650 (middle panel) and x per (bottom panel) extracted from integral/ibis/isgri data. the spectrum of 4u 2206+54 has been fitted with a bulk comptonization model with a χ2 red ∼ 1.4, no evidence of a feature around ∼30 kev can be seen, neither in the spectrum nor in the residuals. for 2s 0114+650 a bulk comptonization model has been used to fit the data with a χ2 red ∼ 1.2, again no evidence of a crsf at ∼30 kev is evident. for the case of x per, a comptonization model and two absorption features at 31.2 kev and 82.3 kev (indicated by arrows) have been used to fit the observed spectrum, with a χ2 red ∼ 1.1. in the case of 4u 2206+54, frequency derivative values derived by finger et al. (2010) and reig et al. (2012) are 1.5 × 10−14hz s−1 and 1.7 × 10−14hz s−1 respectively. finger et al. 2010 included an older bepposax measurement. from these spin-down measurements, finger et al. (2010) estimated a magnetic field of b∼ 1014 g. by using the relationship of ikhsanov (2007) they also derived a magnetic field for 4u 2206+54 on the order of 1014 g. reig et al. (2012) calculated a magnetic field strength on the same order of magnitude by considering the relationship of popov and turolla (2012). the upper panel of fig. 1 shows the spin period measurements from integral/isgri data of 4u 2206+54 in the period 53600 − 54300 mjd. during this epoch (see blay and reglero 2013) the data is compatible with no changes in the spin period of the system, as the pulse period measurements show large errors. the same thing happens for x per and 2s 0114+650 (second and third panels from the top, respectively), in which large errors in the spin period determination make the measurements compatible with no pulse period change. therefore we cannot report on magnetic field measurements from spin period changes for these three systems. the luminosity of 2s 0114+65 in the epoch shown in fig. 1 is 4× 1037ergs−1 (estimated from the model fitted to the spectrum shown in fig. 2), considering a distance to the source of 7.2 kpc (hall et al. 2000). therefore, the ikhsanov (2007) relationship yields a magnetic moment on the order of 1033 g cm−3, which yields a magnetic field strength of b ∼ 1015 g. the relationship from popov and turolla (2012), however, results in an unreasonable number when applied to this source. doroshenko et al. (2012) argue that, for the case of x per, according to the torques applied to the neutron star magnetosphere in the case of wind accretion, and taking into account the theoretical approaches of doroshenko et al. (2010), davidson and ostriker (1973), davies et al. (1979), and bisnovatyi-kogan (1991), the magnetic field in x per is expected to be on the order of b∼ 1014. we show in the lower panel of fig. 1 the spin period measurements made with integral/isgri data. for this source we can estimate the luminosity to be lx ∼ 1.09 × 1035ergs−1 in this epoch (estimated from the model fitted to the spectrum shown in fig. 2 ). as the luminosity of the source is closely related to the accretion rate, we can estimate the field strength of x per by using the relationship of popov and turolla (2012), yielding b∼ 1012 g, which falls within the range of normal neutron star magnetic fields. the relationship from ikhsanov (2007) results in a magnetic moment of µ ∼ 1030 g cm−3, which implies a magnetic field on the order of b ∼ 1012 g. we find, therefore, a discrepancy with the results of doroshenko et al. (2012). we cannot reproduce their calculations, however, because of the large errors in the spin period determination, which prevent the determination of a reliable frequency derivative, needed for the determination of the spin torques. for igr j16358-4726 we see in the lower panel of 218 highly magnetized accreting pulsars: are there accreting magnetars? fig. 1 that the source experiences large pulse period changes. it shows a spin-down between mjd∼53250 and mjd∼54000 of ν̇ ∼ 2.4× 10−14 hz s−1. according to the equation (9) from finger et al. (2010), which relates the magnetic moment of the neutron star with the measured spin-down, we find in igr j16358-4726 a minimum magnetic moment of µ ∼ 2 × 1032 g cm−3, which implies a magnetic field on the order of or larger than b∼ 1014 g. these calculations rely on a good measurement of the luminosity (or mass accretion rate) or of the changes in the spin period. the major uncertainty comes from the determination of the luminosity of the source, calculated from the source flux in a given energy range and the estimated distance to the source, which is usually subject to large uncertainties. with respect to the use of spin period changes, the estimates always rely on long-term or average behavior. on the one hand this is due to the poor knowledge of the short-term or detailed pulse period evolution in many cases, and, on the other hand, to the lack of a detailed and complete theoretical description of the wind accretion scenario. the efforts of postnov et al. (2013), however, try to fill this lack of good theoretical approximations. we will comment on that in the last section. 4 magnetic field determination via cyclotron resonant scatering features a more direct measurement of the magnetic field strength of the neutron star in these systems can be obtained by determining the position of the fundamental crsf seen in their x-ray spectra. crsf have been reported in gx 301-02 (la barbera et al. 2005, makishima and mihara 1992), 2s 0114+65 (wang 2010, bonning and falanga 2005), 4u 2206+54 (blay et al. 2005, , wang 2009, torrejón et al. 2004, masseti et al. 2004), and x per (this work, see fig. 2, doroshenko et al. 2010), see table 2. table 2 summarizes the crsf reported in these systems and the magnetic field strength measurement derived. table 2: crsfs and b determination. see references in the text. source ecrsf (kev) b (1012 gauss) 4u 2206+54 30 2.6 x per 31.2 2.7 2s 0114+650 22 1.9 gx 301-2 37 3.2 5 2s 0114+650 22(c) 1.9 we see in all cases that the magnetic field strength derived by this method is on the order of those found in other neutron stars in hmxrbs, i.e., 100 to 1000 times lower than those of the magnetars. we find, therefore, a discrepancy in magnetic field strength determination with respect to the methods shown in the previous section. one could think that the magnetic fields derived from spin period evolution are not properly calculated, in view of the more direct determination from crsf measurements. however the location of crsf is not free of ambiguities. in the case of 4u 2206+54 (see top panel of fig. 2), for example, this feature has been observed only marginally, and only at one epoch (see blay et al. 2005 and references there in). it has not been observed again (see blay and reglero 2013). therefore, although it has been assumed that the absorption observed was a crsf, this may not be the case. a similar situation applies to 2s 0114+65 (see middle panel of fig. 2), in which the detection of the possible crsf has only been marginal (see wang 2010) and not confirmed again. in the case of x per, doroshenko et al. (2010) show how instead of a crsf fundamental and its first harmonic (see bottom panel of fig. 2), the x per spectra can be very well described by a combination of two comptonization models (comptt+comptt, in xspec notation) demonstrating the possibility that the features observed may not be crsfs. therefore, at least in some cases, the possibility of finding magnetar-like magnetic fields in these systems is not ruled out by the reported observations of crsfs. 5 discussion and conclusion we have seen that in most cases the determination of the magnetic field strength of the neutron star is ambiguous, or even contradictory, when the result from different approaches are compared. we want to emphasize how different approaches may seem to result in different magnetic field strength estimates. an homogeneous and coherent approach is needed in order to determine if there are links between these systems (in terms of their spin period and binary evolution) and to support or discard the different theories trying to explain the puzzling presence of long spin periods in hmxrbs. there have been recent theoretical efforts in order to provide better modeling of the wind-accretion scenario. ikshanov and beskrovnaya (2013), for example, report on a likely explanation of the large spin-down shown in 4u 2206+54 by taking into account a higher than usual magnetic field of the companion star and, consequently, that the accreting material can be magnetized. the possibility of an optical companion with a large magnetic field had been already proposed by blay and reglero (2011). 219 pere blay, pablo reig, vı́ctor reglero the efforts of postnov et al. (2013) in modeling more accurately the wind accretion mechanism in hmxrbs also result in magnetic field estimations for 4u 2206+54 and sxp 1062 on the order of typical magnetic fields found in accreting x-ray pulsars (∼ 1012g). they explain the behavior of sources like gx 301-2 with the hypothesis of being older systems which have already reached their equilibrium period. together with an improvement in the modeling of wind accretion in hmxrbs, a better observational approach is needed in order to understand the behavior of these sources. multiwavelength campaigns (ir, optical, uv, x-rays) on these objects are needed (as simultaneous as possible) in order to determine the various parameters involved: obtain more accurate spectral classification and orbital solutions, measure accurate mass loss rates and wind velocity laws, etc. acknowledgement p. blay acknowledges funding from the spanish ministerio de economia y competitividad through project aya-2011-29936-c05. references [1] bisnovatyi-kogan, g. s. 1991, a&a, 245, 528 [2] blay p., ribó m., negueruela i., torrejn j. m., reig p., camero a., mirabel, i.f., & reglero v. 2005, a&a 438, 936 [3] blay p. and reglero v. 2011, bsrsl, 80, 634 [4] blay p. and reglero v. 2013, pos(integral 2012)012 [5] bonning e. w., falanga m. 2005, a&a, 436, l31 [6] bozzo e., falanga m., stella l. 2008, apj, 683, 1031 doi:10.1086/589990 [7] davidson, k., and ostriker, j. p. 1973, apj, 179, 585 [8] davies, r. e., fabian, a. c., and pringle, j. e. 1979, mnras, 186, 779 [9] davies r.e., and pringle j.e. 1981, mnras, 196, 209 [10] doroshenko v., santangelo a., suleimanov v., kreykenbohm i., staubert r., ferrigno c., klochkov d. 2010, a&a 515, a10 [11] doroshenko v., santangelo a., kreykenbohm i., and doroshenko r. 2012, a&a 540, l1 [12] finger m.h., ikhsanov n.r., wilson-hodge c.a., & patel s.k. 2010., apj, 709, 1249 doi:10.1088/0004-637x/709/2/1249 [13] fu l., li x.d. 2012, apj, 757,171 doi:10.1088/0004-637x/757/2/171 [14] fürst f., marcu d.m., pottschmidt k., grinberg v., wilms j., and cadolle bel m. 2011, pos(integrall 2010)017 [15] hall t. a., finley j. p., corbet r. h. d., thomas r. c., 2000, apj, 536, 450 doi:10.1086/308924 [16] harbel, f., sturm, r., & filipović, m. d. et al. 2012, a&a, 537, l1 [17] ikhsanov, n. r. 2007, mnras, 375, 698 doi:10.1111/j.1365-2966.2006.11331.x [18] ikhsanov n.r., finger m.h. 2012, apj, 753,1 doi:10.1088/0004-637x/753/1/1 [19] ikhsanov n.r., beskrovnaya n.g. 2010, astrophysics, 53-2, 237 [20] ikhsanov n. r. and beskrovnaya n. g.2013, arep, 57, 287 [21] illarionov a.f., and sunyaev r.a. 1975, a&a, 39,185 [22] koh d.t., bildsten l., chakrabarty d., et al. 1997, apj, 479, 933 [23] li x. d., van den heuvel e. p. j., 1999, apj, 513, l45 [24] la barbera, a., segreto, a., santangelo, a., kreykenbohm, i., & orlandini, m. 2005, a&a, 438, 617 [25] makishima k., mihara t. 1992, in magnetic fields of neutron stars, ed. t. tanaka & k. koyama (tokyo: universal academy press), 23 [26] marcu d. m., fürst f., pottschmidt k., et al. 2011, apj, 742, l11 doi:10.1088/2041-8205/742/1/l11 [27] masetti n., dal fiume d., amati l., del sordo s., frontera f., orlandini m., and palazzi e. 2004, a&a, 423, 311 [28] panchapakesan n. 2003, bull. astr. soc. india, 31, 19 [29] patel s.k., zurita j., del santo m. et al. 2007, apj, 657, 994 doi:10.1086/510374 [30] popov s.b., turolla r. 2012, mnras, 421, l127 doi:10.1111/j.1745-3933.2012.01220.x 220 http://dx.doi.org/10.1086/589990 http://dx.doi.org/10.1088/0004-637x/709/2/1249 http://dx.doi.org/10.1088/0004-637x/757/2/171 http://dx.doi.org/10.1086/308924 http://dx.doi.org/10.1111/j.1365-2966.2006.11331.x http://dx.doi.org/10.1088/0004-637x/753/1/1 http://dx.doi.org/10.1088/2041-8205/742/1/l11 http://dx.doi.org/10.1086/510374 http://dx.doi.org/10.1111/j.1745-3933.2012.01220.x highly magnetized accreting pulsars: are there accreting magnetars? [31] postnov k.a., shakura n.i., kochetkova a.yu., and hjalmarsdotter l., 2013, arxiv:1307.3032 [32] rea n., esposito p. 2011, in high-energy emission from pulsars and their systems, ed. d. f. torres & n. rea, astrophysics and space science proceedings (springer berl in heidelberg), 247 [33] reig p., torrejón j.m., & blay p. 2012, mnras, 425, 595 doi:10.1111/j.1365-2966.2012.21509.x [34] schönherr g., wilms j., kretschmar p., kreykenbohm i., santangelo a., rothschild r.e., coburn w., staubert r. 2007, a&a 472, 353 [35] torrejn j. m., kreykenbohm i., orr a., titarchuk l., and negueruela i. 2004, a&a, 423, 301 [36] wang, w. 2009, mnras, 398, 1428 doi:10.1111/j.1365-2966.2009.15200.x [37] wang w. 2010, a&a 516, a15 [38] winkler c., courvoisier t.j.l., di cocco g., et al. 2003, a&a, 411, l1 221 http://dx.doi.org/10.1111/j.1365-2966.2012.21509.x http://dx.doi.org/10.1111/j.1365-2966.2009.15200.x introduction the candidates magnetic field determination via spin period evolution magnetic field determination via cyclotron resonant scatering features discussion and conclusion acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0029 acta polytechnica ctu proceedings 7:29–32, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app deformation behaviour of gellan gum based artificial bone structures under simulated physiological conditions nela krčmářováa,∗, jan šleichrta, tomáš fílab, petr koudelkab, daniel kytýřb a czech technical university in prague, faculty of transportation sciences, department of mechanics and materials, konviktská 20, 120 00 prague 1, czech republic b institute of theoretical and applied mechanics as cr, v.v.i., prosecká 76, 190 00 prague 9, czech republic ∗ corresponding author: krcmarova@fd.cvut.cz abstract. the paper deals with investigation of deformation behaviour of gellan gum (gg) based structures prepared for regenerative medicine purposes. investigated material was synthesized as porous spongy-like scaffold reinforced by bioactive glass (bag) nano-particles in different concentrations. deformation behavior was obtained employing custom designed experimental setup. this device equipped with bioreactor chamber allows to test the delivered samples under simulated physiological conditions with controlled flow and temperature. cylindrical samples were subjected to uniaxial quasi-static loading in tension and compression. material properties of plain gg scaffold and reinforced scaffold buffered by 50 wt% and 70 wt% bag were derived from a set of tensile and compression tests. the results are represented in form of stress-strain curves calculated from the acquired force and displacement data. keywords: gellan gum scaffold, reinforcement, uni-axial loading, simulated physiological conditions. 1. introduction the worldwide incidence of bone disorders and conditions have trended steeply upward. especially high income regions are expected twofold increase between 2010 and 2020 [1]. this is the tribute for populations aging coupled with improper nutrient consumption and poor physical activity. globally more than 40 % of women and 30 % of men are at increased risk of emergence of bone disorders [2]. annually in the usa only, more than half a million bone defects are reported. worldwide the treatment cost reaches more than $2.5 billion. the bone disorders treatment using engineered bone tissue has been viewed promising and yet not fully exploited potential alternative to conventional use of autografts and allografts. artificial tissue is overcoming problems with donor site morbidity, loss of bone inductive factors and/or resorption during healing [3]. in general, several essential demands are placed on artificial structure: i) chemical biocompatibility without toxic effect ii) reduction of the stress shielding effect iii) successful diffusion of nutrients and oxygen iv) controlled degradation and resorption [4]. presented paper deals with uni-axial quasi-static testing of artificial spongy-like structure [5] proposed for bone tissue engineering purposes as a bone scaffold. the investigated gellan gum bioactive glass (ggbag) material combines organic (polysaccharitic) component with inorganic (silicon-calcium based) nanoparticles. this approach effectively enables for adaptation of physical and mechanical properties of the synthesized material according to the desired application [6]. the studied material was subjected to quasi-static loading in both tension and compression to evaluate its expected deformation response in interaction with human body. therefore the experiment was carried out under simulated physiological conditions using bioreactor with circulating synthetic plasma. 2. material bioactive-glass-reinforced gellan-gum is a promising material for wide use in bone tissue engineering [7]. originally the gellan-gum (microbial extracted polysaccharide) was used in food and pharmaceutical industry [8]. gg is composed of repeating units consisting of two d-glucose and one of each lrhamnose and d-glucuronic acid [9]. its main advantage is in ability to form highly porous 3d structures when properly cross-linked and fabricated [10]. material investigated in this study was synthesized at jozef stefan institute (slovenia) as porous spongylike structure buffered by bioactive glass (bag) nanoparticles [11]. during the production process gellan gum was dissolved in ultra-pure water by heating the solution for 30 minutes at 90 ◦c. to the hot gg solution a dispersion of bag was admixed and 0.18 wt% cacl2 was added. kept at high temperatures this mixture was then poured into required mould and let there to spontaneously jellify. finally the samples were frozen at −80 ◦c and freeze-dried. 29 http://dx.doi.org/10.14311/app.2017.7.0029 http://ojs.cvut.cz/ojs/index.php/app n. krčmářová, j. šleichrt, t. fíla et al. acta polytechnica ctu proceedings 3. methods for initial awareness about deformation characteristics of synthesized material set of quasi-static experiments was performed. the first goal was to demonstrate possibilities of in house developed experimental infrastructure for this purpose. expected collapse forces was in range of single newtons and precise loading plate positioning was required as well. to obtain more relevant results some modifications of the experimental devices in detail presented in 3.2 was carried out. using this adapted devices basic material properties and stress–strain response were obtained. 3.1. experimental procedure cylindrical samples with height h = 8.6 ± 0.4 mm, diameter d = 5.0 ± 0.1 mm and weight m ≈ 11 mg, ≈ 16 mg and ≈ 24 mg for plain gg scaffold, ggbag reinforced scaffold with 50 wt% and 70 wt% bag respectively were subjected to tensile and compressive loading under wet condition. for wet condition simulating physiological environment of human body infusion solution plasmalyte (bartex, czech republic) was used. loading plate displacement was set typically for 1000µm corresponding to deformation approx. 11 − 12 % sufficient for significant sample damage. loading rate was set to 2µms−1. force and position was read-out with sampling frequency 50 sps. 3.2. instrumentation in house developed indentation device for low-force indentation was adapted for tensile and compression test. originally the device was designed using modular aluminum profile (30 × 30 mm) frame bearing i) x and y motorized axis kk40 (hiwin, japan) for sample positioning with repeatability 10µm ii) indentation axis based on linear stage mgw12 (hiwin, japan) and linear actuator 43 series (haydon kerk, usa) with position accuracy 3µm and mounting for u9b/c series (hbm, germany) load-cell. this axis was upgraded using the linear actuator with position accuracy 1.5µm, encoder with resolution 0.5µm and load cell with nominal force 50 n (the most precise force transducer in u9b/c series). for testing under wet condition testing device was equipped with bioreactor with controlled flow and temperature of circulating fluid. from the heated reservoir is the fluid pumped to the basin surrounding the samples and loading plates. 3.3. strain calculation the investigated material exhibits very low stiffness, which, coupled with high porosity and suboptimal geometry of the samples, induces high potential for significant boundary effects. unfortunately full-field optical strain measurement of the wet samples placed in fluid basin was not possible using the available setup. therefore comparative measurements for contact and contactless strain evaluation methods was performed in previous studies [12, 13]. however production process of the gg-bag samples does not allow to reliably produce cylindrical samples, the diameter of specimens varied in average ±100µm, and the loaded faces were rough and not plan-parallel strain-stress curve derived directly from force transducer and encoder indicate relevant results. 3.4. stress calculation the stress σ in all experimental analysis was considered as engineering stress obtained using σ = f ac (1) where ac is cross-sectional area of the specimen calculated from minimal sample diameter measured before deformation. force f was acquired by the load-cell. for the purpose of stress calculations, samples were considered ideally cylindrical, neglecting all geometrical irregularities. 4. results material properties and deformation behaviour of plain gg scaffold and gg-bag reinforced scaffold with 50 wt% and 70 wt% bag content were studied in tensile and compression tests under dry and wet conditions. five experiments for each type of material and loading mode were performed. young’s modulus was calculated using linear regression applied on the elastic part of stress–strain diagrams. the calculated elastic properties and yield stresses are listed in tabs. 2–6. sample e [kpa] gg00 1 88.588 ± 0.147 gg00 2 119.507 ± 0.156 gg00 3 126.159 ± 0.142 gg00 4 93.571 ± 0.144 gg00 5 141.089 ± 0.146 gg00 mean 113.783 ± 22.219 table 1. elastic properties of plain gg samples for compression test sample e [kpa] gg00 1 56.343 ± 0.843 gg00 2 33.403 ± 0.209 gg00 3 36.383 ± 0.412 gg00 4 69.077 ± 0.945 gg00 5 70.436 ± 0.951 gg00 mean 53.129 ± 17.562 table 2. elastic properties of plain gg samples for tensile test 30 vol. 7/2017 deformation behaviour of wet gellan gum scaffold sample e [kpa] gg50 1 81.4518 ± 0.145 gg50 2 131.882 ± 0.137 gg50 3 70.8462 ± 0.141 gg50 4 113.892 ± 0.281 gg50 5 140.221 ± 0.201 gg50 mean 107.659 ± 30.528 table 3. elastic properties of gg samples with 50 wt% bag for compression test sample e [kpa] gg50 1 24.406 ± 0.090 gg50 2 27.156 ± 0.085 gg50 3 24.287 ± 0.080 gg50 4 23.719 ± 0.081 gg50 5 21.376 ± 0.089 gg50 mean 24.18 ± 2.061 table 4. elastic properties of gg samples with 50 wt% bag for tensile test sample e [kpa] gg70 1 134.424 ± 0.120 gg70 2 63.566 ± 0.077 gg70 3 79.592 ± 0.078 gg70 4 67.376 ± 0.083 gg70 5 65.131 ± 0.077 gg70 mean 82.018 ± 29.967 table 5. elastic properties of gg samples with 70 wt% bag for compression test sample e [kpa] gg70 1 22.7629 ± 0.080 gg70 2 23.4423 ± 0.082 gg70 3 20.9057 ± 0.081 gg70 4 21.1495 ± 0.101 gg70 5 22.7019 ± 0.079 gg70 mean 22.192 ± 1.105 table 6. elastic properties of gg samples with 70 wt% bag for tensile test all obtained results in form of enveloped stress– strain curves are plotted in figs. 1, 2. the stress– strain area for each type of the scaffold represents minimum and maximum stress for each strain value. 5. conclusion gg-bag samples with 0, 50 and 70 wt% fraction of reinforcing bag particles were subjected to tensile and compressive loading test to evaluate deformation response in simulated physiological condition. it was found out, that the ambient environment has significant influence on mechanical response of the material as the measured properties. the scaffolds wetted by 0 0.002 0.004 0.006 0.008 0.01 0.012 0 0.02 0.04 0.06 0.08 0.1 0.12 0.14 c o m p re s s iv e s tr e s s [ m p a ] compressive strain [−] egg00 = 0.113±0.022 mpa egg70 = 0.082±0.029 mpa egg50 = 0.107±0.030 mpa figure 1. stress–strain curves envelope of scaffolds under compressive loading 0 0.005 0.01 0.015 0.02 0 0.02 0.04 0.06 0.08 0.1 0.12 0.14 t e n s ile s tr e s s [ m p a ] tensile strain [−] egg00 = 0.053±0.017 mpa egg50 = 0.024±0.002 mpa egg70 = 0.022±0.001 mpa figure 2. stress–strain curves envelope of scaffolds under tensile loading the synthetic plasma solution exhibited radical loss of stiffness, where the elastic modulae decreased more than ten times [12]. no significant reinforcement effect of bag particles was observed during compression test. in case of tensile loading bag buffered samples unexpectedly exhibited lower elastic modulae and ultimate stresses compared to the plain gg samples. that could be given by scaffold cell-wall heterogenity and disintegrity caused by rigid nature of glass particles. it can be concluded that presented analysis proved use of the considered experimental methods together with available experimental infrastructure for the testing of gg based scaffolds. the most limiting part of the experimental setup is load-cell signal-to-noise ratio at desired loading level and generally suboptimal geometrical characteristics of the samples inducing shear stresses during loading. acknowledgements the research was supported by grant agency of the czech technical university in prague (grant no. sgs15/225/ohk2/3t/16), by interreg project com3dxct (atcz38) and by institutional support rvo: 31 n. krčmářová, j. šleichrt, t. fíla et al. acta polytechnica ctu proceedings 68378297. we would like to express our special thanks to ana grantar for sample synthesization. references [1] w. h. organization. world health statistics. who press, 2015. [2] w. h. organization. global recommendations on physical activity for health. who press, switzerland, 2010. [3] a. r. vaccaro, k. chiba, j. g. heller, et al. bone grafting alternatives in spinal surgery. the spine journal 2(3):206 – 215, 2002. doi:10.1016/s1529-9430(02)00180-8. [4] a. r. amini, c. t. laurencin, s. p. nukavarapu. bone tissue engineering: recent advances and challenges. critical reviews in biomedical engineering 40(5):363– 408, 2012. doi:10.1615/critrevbiomedeng.v40.i5.10. [5] l. polo-corrales, m. latorre-esteves, j. e. ramirezvick. scaffold design for bone regeneration. journal of nanoscience and nanotechnology 14(1):15–56, 2014. [6] e. r. morris, k. nishinari, m. rinaudo. gelation of gellan – a review. food hydrocolloids 28(2):373 – 411, 2012. doi:10.1016/j.foodhyd.2012.01.004. [7] m. bououdina. emerging research on bioinspired materials engineering. igi global, 2016. doi:10.4018/978-1-4666-9811-6. [8] d. hoikhman, y. sela. gellan gum based oral controlled release dosage formsa novel platform technology for gastric retention, 2005. wo patent app. pct/il2004/000,654. [9] j. t. oliveira, l. martins, r. picciochi, et al. gellan gum: a new biomaterial for cartilage tissue engineering applications. journal of biomedical materials research part a 93a(3):852–863, 2010. doi:10.1002/jbm.a.32574. [10] n. drnovšek, s. novak, u. dragin, et al. bioactive glass enhances bone ingrowth into the porous titanium coating on orthopaedic implants. international orthopaedics 36(8):1739–1745, 2012. doi:10.1007/s00264-012-1520-y. [11] a. gantar, l. da silva, j. oliveira, et al. nanoparticulate bioactive-glass-reinforced gellan-gum hydrogels for bone-tissue engineering. materials science and engineering c 43:27–36, 2014. cited by 13, doi:10.1016/j.msec.2014.06.045. [12] d. kytýř, t. doktor, o. jiroušek, et al. deformation behaviour of a natural-shaped bone scaffold. materiali in tehnologije 50(3):301–305, 2016. cited by 0, doi:10.17222/mit.2014.190. [13] j. šleichrt, m. adorna, m. neuhäuserová, et al. deformation characteristics of chopped fibre composites subjected to quasi–static tensile loading. acta polytechnica ctu proceedings 3:71–74, 2016. doi:10.14311/app.2016.3.0071. 32 http://dx.doi.org/10.1016/s1529-9430(02)00180-8 http://dx.doi.org/10.1615/critrevbiomedeng.v40.i5.10 http://dx.doi.org/10.1016/j.foodhyd.2012.01.004 http://dx.doi.org/10.4018/978-1-4666-9811-6 http://dx.doi.org/10.1002/jbm.a.32574 http://dx.doi.org/10.1007/s00264-012-1520-y http://dx.doi.org/10.1016/j.msec.2014.06.045 http://dx.doi.org/10.17222/mit.2014.190 http://dx.doi.org/10.14311/app.2016.3.0071 acta polytechnica ctu proceedings 7:29–32, 2017 1 introduction 2 material 3 methods 3.1 experimental procedure 3.2 instrumentation 3.3 strain calculation 3.4 stress calculation 4 results 5 conclusion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0080 acta polytechnica ctu proceedings 4:63–71, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app parcs/trace coupling methodology for rod ejection on vver 1000 reactor marek ruščáka,b,∗, guido mazzinib a polytechnic university of catalonia b research centre řež, hlavní 130, husinec-řež, czech republic ∗ corresponding author: marek.ruscak@cvrez.cz abstract. the rod ejection (re) is a design basis accident in accordance with nureg-0800 and usually studied using point kinetics. in this paper a methodology and a 3d kinetic model is prepared (parcs), coupled with a thermal hydraulic system code (trace) for simulating this accident scenario for general vver 1000 technology. keywords: parcs, trace, coupling, vver 1000, safety. 1. introduction the technology progress allows the industry to push the accuracy of calculations to the new level. alongside with the progress, there is an approach to simplicity. the current trend is to couple already existing codes to enable simultaneous complex scenarios and sub-sequential analysis. the thermo-hydraulic system code trace is the next generation code being a successor to relap, both of which however have the capability of coupling with the neutronics code parcs. the parcs/trace coupling for full vver 1000 reactor has never been done before in the czech republic with the cross sections generated by scale/triton. therefore a methodology had to be developed, which proved to be a challenge on its own regarding the lack of documentation for coupling models with hexagonal geometries. most of the geometrical, material and structural data are taken from a reference vver 1000 [1]. it is important to note, that results in this paper are not final and much longer process of model development will be required in order to submit the coupled model for validation. main objective of this paper is to demonstrate in a practical example of threedimensional accident scenario of vver 1000 reactor an acquisition of parcs code for 3d reactor kinetics and its coupling with system thermo-hydraulic code trace. 2. parcs code description parcs (purdue reactor core simulator) is a threedimensional (3d) reactor core simulator which solves the steady-state and time-dependent, multi-group neutron diffusion and low order transport equations in orthogonal and non-orthogonal geometries. parcs can be coupled directly to the thermal-hydraulics system code trace which provides the temperature and flow field information to parcs during the transient calculations via the few group cross sections. parcs is available as a standalone code for performing calculations which do not require coupling to trace or relap5. parcs can also be coupled to the relap5 systems code. a separate code module, genpmaxs, is used to process the cross sections generated by lattice physics codes such as triton (scale 6.1.2), helios, or serpent into the pmaxs format that can be read by parcs. parcs is composed of several cards such as cntl (control), xsec (cross-sections) and so on. parcs code is only concerned about neutronic definitions, most importantly the macroscopic cross sections, radial and axial fuel assembly maps, mashing and other parameters [2]. the most recent version of the parcs code is 3.2 (november 2015). although parcs is a very good tool for square geometry core lattice, there are still limitations concerning hexagonal geometry. by the fall the code application maintenance program (camp) of 2015 it is not possible to calculate pin power of hexagonal assemblies. also presented at the camp by dr. guido mazzini and by the author there is a limitation using gadolinium as a burnable absorber in the core in trace. there several additional issues concerning the coupling procedure, mainly due to a lack of proper guiding material provided by the code authors. in numerous cases impact and importance of several parameters can only be found by performing a sensitivity analysis on them, which requires significant amounts of time and therefore it is difficult to build a near-perfect model [3]. 3. trace code description the trac/relap advanced computational engine (trace – formerly called trac-m) is the latest in a series of advanced, best-estimate reactor systems codes developed under u.s. nuclear regulatory commission for analysing transient and steady-state neutronic-thermal-hydraulic behaviour in light water reactors. it is the product of a long term effort to com63 http://dx.doi.org/10.14311/ap.2016.4.0080 http://ojs.cvut.cz/ojs/index.php/app marek ruščák, guido mazzini acta polytechnica ctu proceedings bine the capabilities of the nrc’s four main systems codes (trac-p, trac-b, relap5 and ramona) into one modernized computational tool. it is able to analyse large/small break loss of coolant accidents (locas) and other system transients in both pressurized water reactors (pwrs) and boiling water reactors (bwrs). the version used in this analyses is trace v5 patch 4 released in 2014. for the user point of view, there are three major steps in performing a calculation in trace and those are: input processing, initialization and results. during the input processing, trace checks the user model and checks for errors. if the model passes the processing, it is initialized and again checks for possible boundary error as well as the model will be prepared for calculation. once the calculation is finished, there are several output files, among which there is the actual output, a restart file and a binary file containing all data to be read by apt plot. this process is shown in the figure 1 [4]. figure 1. phases of a trace calculation. 4. scale code description the scale code package is a comprehensive modelling and simulation suite for nuclear safety analysis and design. scale provides a “plug-and-play” framework with several computational modules including three deterministic and three monte carlo radiation transport solvers that are selected based on the desired solution strategy. scale includes current nuclear data libraries and problem-dependent processing tools for continuous-energy and multigroup neutronics calculations, multigroup coupled neutron-gamma calculations, as well as activation and decay calculations. in particular the triton module is used for the generation of cross-sections useful for parcs code. it is a control module in computation code scale 6.1.2. it uses several computational sequences like centrm, newt, bonami, etc., that are depending on user’s requirements. triton performs 2-d calculations for square and hexagonal geometry of the fuel assembly. its main computational features are cross-section calculation and isotopic compositions of the fuel assembly. in the centrm-based discrete ordinates (sn) option, the bondarenko self-shielding method is used to determine the problem-dependent multigroup cross-sections in the unresolved resonance energy range. the unresolved resonance calculation is performed by the bonami functional module. for the resolved resonance energy range, the centrm functional module is used to determine the 1d pointwise (105 energy groups) flux solution using the sn method [5]. 5. coupling procedure coupling procedure differs greatly with the lattice of the reactor. for square pitch all the user needs are parcs and trace inputs and graphical interface called snap in order to use the auto mapping feature. this auto mapping procedure generates a “map” file to be run with the coupled calculation. this automatic process is not however available for this case. therefore in case of hexagonal pitch this procedure has to be done manually. this means manually assigning each neutronic control volume (mesh) to the one of trace’s hydraulic and heat structure meshes. to do this by hand would require a substantial amount of time and this is why to achieve mapping a secondary script done in matlab is used. the general structure of the script has four main sections. the general constants such as number of radial rows or axial planes, number of assemblies, number of planes and the vessel id defined in the trace model. in the second section there are the radial definitions of both parcs and trace. first there is parcs radial numbering (given by stand alone parcs output) and then the parcs radial weight map (0.0–1.0) where on azimuthal boundaries the assembly weight is 0.5 and doubled (two assemblies by 0.5 instead of one by 1.0) and the central node is divided into 6 by 1/6. the trace radial th map and a heat structure (hs) map are defined according to a logic set in trace. the third section of the mapping script concerns the axial meshing and mapping. it is important to note, that the number of axial levels has to be same as in the geometry definition in both parcs and trace as well as the node numbering. usually the vessel component in trace has 1 to n nodes where the core (k) itself occupies only n − k nodes and the numbering has to respect the numbering in trace for the core. the mapping file includes a table in the following columns; vessel id, trace radial id, trace axial id, parcs radial and multiplication of radial and axial weights. after the mapping file is generated it is included with the parcs and trace inputs in order for the codes to recognize the geometry. in figure 2 there is a visualization of the mapping process, where colours correspond to individual sectors. strictly speaking the nodal definitions in both parc (core) and trace (th and hs) are put together. the sequence of calculation is shown in figure 3 on page 65. in this work there are two sets of cross sections generated by the scale and serpent 2 codes. later on the results will show the differences between the two and possible ways of improvement. once the cross sections are implemented with the parcs code, 64 vol. 4/2016 parcs/trace coupling methodology for rod ejection on vver 1000 figure 2. mapping procedure. geometry definitions of parcs and trace codes have to be the same. after ensuring that the geometry is same in either code, it is possible to begin the coupling process, which begins with mapping of the geometry definitions. in order to couple parcs and trace there are four files needed. the parcs and trace inputs (in the diagram they are shown as name.inp) and trace stand alone (sa) restart file are generated by the stand alone (sa) trace and of course the mapping file. with these files it is possible to run steady state (ss) coupled (c) calculation. this calculation outputs several files including the restart files of both parcs and trace, which are necessary for transient (tr) calculation. the ss, c restart files are then used for the tr, c calculation along with the transient inputs of parcs and trace. figure 3. calculation process. 6. model description 6.1. scale the model of fuel assembly is created by triton in scale 6.1.2 and the geometrical and material parameters from a vver 1000 type npp. there are six types of fuel assemblies with different enrichment as shown in the table 1 (page 66). in the first step it is necessary to define several parameters of the fuel, such as density, temperature and enrichment as well as cladding, which consist of 99 % zr and 1 % nb. moderator is comprised from main an additional materials. the main material is water (h2o) with density of 0.73 g/cm3, temperature 575 k and the additional material is boron with 1065 ppm. inside the fuel pellets there are the central holes filled with helium. the geometrical definition and parameters of the fuel assemblies and fuel pellets are defined as following. simulation of active length of fuel assembly as infinite because calculation code triton computes only 2d (radial) geometry. the inputs are shown in figure 4 and figure 5 on page 65. fuel assembly consists of nine nodes and each node has power level that depends on the active length power distribution. the analyses in scale are performed with average power and temperature distribution, also the calculation are done at time 0, practically after refuelling without the effect of xenon and samarium. the calculations are based on endf/b-vii.0 in 238 groups. the plots below are a visualization of defined geometry, where different colours represent different materials. figure 4. inputs of f130/f200 (left) and inputs of ff36g9/ff40g9 (right). figure 5. input of f30g9 (left) and input of f40g6 (right). there are five branches considered plus a reference one. the branch information is in the table 2 on page 66. these branches are used for calculation of the differential cross sections. the branches are fuel temperature (tf), moderator temperature (tm), moderator density (dm), control rod position (cr) and boron concentration (sb). 6.2. parcs the neutronic model of vver 1000 in the parcs code is fairly simple and short, compared to system codes or mc codes, such as mcnp. most of the parameters in the model are kept default. the only important parameter specified is the nodal kernel used, in this case the triangular polynomial expansion nodal (tpen) method. this method first decouples the 3-d defined geometry into 2-d axial and radial that are coupled through transverseleakages. the radial and axial configuration as well as 65 marek ruščák, guido mazzini acta polytechnica ctu proceedings fuel 1 [%] fuel 2 [%] fuel gd [%] gd [%] gd pins [–] f200 2.0 – – – – f130 1.3 – – – – f40g6 4.0 – 3.3 5 6 f30g9 3.0 – 2.4 5 9 ff36g9 3.6 3.3 3.3 5 9 ff40g9 4.0 3.6 3.3 5 9 table 1. fuel enrichment description. tf [k] tm [k] dm [g/cm3] cr sb [ppm] reference branch 980 575 0.73 out 1065 branch 1 980 575 0.73 in 1065 branch 2 980 575 0.73 out 565 branch 3 980 575 0.83 out 1065 branch 4 980 675 0.73 out 1065 branch 5 1080 575 0.73 out 1065 table 2. scale branch structure. control rod banks positions are also defined. the control rod configuration is set so the shut down clusters are fully withdrawn from the core, and the control clusters are fully inserted. core has to have same dimensions and meshing as in the trace model, in order to couple. therefore there are 14 axial nodes and 8 radial rings as shown in figure 6 on page 66 and table 4 on page 67. the description of figure 6 is shown in table 3 on page 66 [1, 6]. figure 6. core layout. colour fa type red f130 yellow f200 green f30g9 azur f40g6 blue ff36g9 purple ff40g9 table 3. colour description for core layout. the general configuration of control and scram banks is shown in figure 7 on page 66 where different colours indicate different groups. this model however does not include reflector, due to the complexity of implementation. whole trace figure 7. bank layout. model would have to be changed in order to include one additional ring containing the reflector. 6.3. trace the vver 1000 model developed by cvr was originally prepared for relap5mod3.3 code and subsequently converted for trace v5.0 code. it represents the primary and secondary systems, as well as the safety components of the plant. the model of the primary circuit consists first of the vessel component representing the reactor pressure vessel (rpv) as illustrated in figure 8 on page 67. radially, three zones nodalization scheme is adopted with two inner zones representing the lower plenum, the core, and the upper plenum. third (outer) zone models the downcomer. axially, 37 zones are modelled with 14 of them representing the active core. further, the model of the primary circuit consists of models of each individual primary system loop subdivided into hot leg pipes, horizontal steam generators hot and cold collectors and heat exchange tube bundles, loop seal pipes, reactor coolant pumps, and cold legs. to complete the primary circuit model the pressurizer, pressurizer surge and spray lines are modelled. the pressurizer power operated relive valve and safety valves are sim66 vol. 4/2016 parcs/trace coupling methodology for rod ejection on vver 1000 ulated. trace v5.0 pipe and valve components are used to model the secondary system steam lines up to the turbine. steam dump valves and steam generator safety valves are simulated individually. feedwater system model consists of the pipes and valves located in the containment. the plant model further contains the control components and trips to simulate actions of safety grade portions of i&c. figure 8. trace rpv model nodalization. the basic idea of this model development was to develop a tool for the licensing audit calculations of dba events included in chapter 15 of the sar [7]. as such, the model was systematically validated against the number of plant start up tests including the loss of flow (rcp trips), loss of feedwater, etc. with this, and considering that best-estimate codes are more accurate than severe accident codes in phases before core degradation started, the trace v5.0 model is a reference model for initial phases of the transients simulated [8]. the transient model is a reduced version of the steady state input, in order to reduce the computational costs. also it includes the small break loss of coolant accident (sbloca), (trip number 1005) which occurs at the point of ejection when the upper part of the control mechanism breaks and is ejected from the pressure vessel. this trip is set manually and the setpoint is time. the axial core control volume distribution is shown in the table 4 on page 67. this table does not include all rpv nodes, but only the active core, since the entire nodalization is not essential for the purposes of this work. the time steps are crucial part of the model, especially when coupling. the most important parameter is that the time step in trace should be about three orders greater then the timestep set in parcs, but small enough to allow the calculation to perform [4]. from experience however, trace terminates due to high time step, yet after rigorous sensitivity analysis the problem is not solved simply by reducing the time step even further. this particular problem will be one of a subjects of further study after this work. 7. results the results suffer from several code-based issues. probably the biggest impact has so called null factor, which acts as a balancing reactivity factor. in the case during the transient calculation, if the k-effective differs axial level mesh size axial level 14 46.3 axial level 13 25.5 axial level 12 25.5 axial level 11 25.5 axial level 10 25.5 axial level 9 25.5 axial level 8 25.5 axial level 7 25.5 axial level 6 25.5 axial level 5 25.5 axial level 4 25.5 axial level 3 37.73 axial level 2 13.27 axial level 1 29.55 table 4. trace axial distribution. from 1, this null factor acts to balance reactivities to achieve k-eff = 1. the bigger the difference between k-effective actual and 1, the bigger the null factor. another possible reason for these oscillations are the cross sections themselves and more tuning may be needed. this major reason is the lack of boron reactivity feedback, which still remains to be a problem. this is suspected to be the reason why the reactivity stabilizes at 0.2 $ (see figure 17). lastly the minor source of these oscillations is the instability transition of trace from steady state to transient calculation. because the access to the source code of either parcs or trace is limited, the only way of addressing these uncertainties is through benchmarking with existing results. when the control bank ejects, there is about 1 $ of positive reactivity inserted to the system, resulting higher neutron flux, this resulting in higher fuel temperature (figure 19) and also causing a rise of the doppler temperature. therefore the doppler effect introduces negative reactivity to the system, decreasing power. this heat is being transferred to the coolant, resulting in increase of coolant temperature (figure 18). when the temperature of the coolant (in this case light water) increases, the density decreases (figure 21) resulting in lower moderation hence decrease in flux, reactivity and power. this is the general behaviour, that occurs in all the peaks. the first peak, (figure 12) is so small, because the localised rise in coolant temperature is stopped when it is cooled down by rest of the coolant in the core. however quickly after the power start rising again and the whole process described above occurs again, however much more slowly. the final oscillations show simple balancing between moderator density and moderator temperature. by comparing the results with chapter 15 of final safety analysis report of an existing vver 1000, which unfortunately cannot be shown, the results are fairly comparable also with the results of [9]. by examining the flux behaviour we can see, that 67 marek ruščák, guido mazzini acta polytechnica ctu proceedings figure 9. averaged radial normalized power profile. figure 10. averaged thermal flux. in 100 seconds the flux increases during the transient. this can be seen in figure 10 on page 68. the flux shape is actually one of the major reasons why to use 3d calculations. by examining the flux plots below, most of the core has fairly low flux, in comparison to the area around the ejection point. by using the standard approach of point kinetics, the results would be averaged over the whole core, therefore lower then the actual highest peak. in the meantime, when the control bank ejects, the driving mechanism breaks and is ejected from the pressure vessel, resulting in a small break loca of a 50 mm diameter. the loss of coolant is represented by the mass flow in the figure 22, however for the duration of the transient, sb loca has very little effect as seen from the system pressure in figure 23. there are pressure oscillations close after ejection, however it stabilizes at the end of the transient. in order to calculate the main parameter, which is amount of energy per gram (cal/g), it is necessary to integrate over one second the relative power in the figure 11. averaged thermal flux after 100 s. ejection point and then multiply by the total power at peak [w] over number of assemblies (na, 163). using the hot channel radial peak factor (pf) 1.29 (given through internal communication with vver 1000 fa specialists) and dividing the total weight of fuel (approximately 500 kg) in one assembly by the number of pins (311). the general calculation is following, having time step (t) [s], average power (p ) [w] and normalized power at ejection point (rp) [–]. first it is important to calculate power in watts (wr) for the ejection point which is wr = p · rp · pf na . after that by integrating the wr curve per time and so getting the energy per time [j], it is necessary to convert to calories (1 j = 0.239 cal) and divide by weight of fuel in one pin in grams. the expected results should be similar to [9] which is 70.5 cal/g. the results are shown in figure 13 and it is possible to see, that the maximum value is 75 cal/g and therefore below the limit of 200 cal/g and also that it is reasonably similar to the results of [9], considering the differences in tested reactors. 68 vol. 4/2016 parcs/trace coupling methodology for rod ejection on vver 1000 figure 12. core power. figure 13. maximum energy deposited in fuel pin. figure 14. flux profile cross section at ejection point. figure 15. flux profile cross section at ejection point after 100 s. figure 16. axial normalized power. figure 17. reactivity. 69 marek ruščák, guido mazzini acta polytechnica ctu proceedings figure 18. coolant temperature at ejection point. figure 19. fuel temperature at ejection point. figure 20. maximal hot rod temperature. figure 21. coolant density at ejection point. figure 22. mass flow through the break. figure 23. system pressure. 70 vol. 4/2016 parcs/trace coupling methodology for rod ejection on vver 1000 8. conclusion the rod ejection accident scenario is a reactivity initiated accident and is also considered a design basis accident (dba). the general approach is to improve the existing models and methodologies in order to increase the precision of results. this goal is being approached from two sides, first to couple different codes (neutronics with thermal-hydraulics and also with material codes) together and second to transition from 1d calculations to 3d. this is increasingly possible with the increase in computer power, which allows to run much more complex calculations. there were two main goals to this paper. first, to establish a methodology for coupling parcs with trace for reactor with hexagonal lattice and second to run a rod ejection scenario on this coupled model.the general process was to create homogenized macroscopic cross sections for six different fuel assembly types, specifications of which were provided by the research centre rez and are considered confidential. the homogenized cross sections were calculated using a scale/triton code. after the cross sections were implemented into the parcs models, the parcs geometry definition had to be mapped with the one of trace. after that, a reference steady state coupled calculation was performed for each scenario separately. when the individual steady state calculations were done, the resulting restart data were inserted into the transient models. there were several challenges when coupling these codes for hexagonal lattice. the major one, which costed the most time is a lack of a proper guide on how to perform coupling without using graphical interface snap, which does not support hexagonal lattice. this issue is currently being solved with the authors of the code and hopefully a better user guide will be available in next years. second difficulty was the absence of auto-mapping function for hexagonal lattice, which had to be substituted by a matlab script. this can also be a source of uncertainty, because it is difficult to be sure, that the mapping was done correctly. lastly the code itself has a significant setback for the rod ejection calculation, which is a lack of pin power calculation for hexagonal lattice. because of this, the power is averaged over the whole assembly and therefore is lower, than the actual value. this can be however corrected using the peak factor as done in this paper. currently there are alternative neutronic codes, that can be coupled with trace, for example dyn3d, which can be coupled not only to trace, but also with relap and athlet codes. in the end, the future work to be done is firstly to improve the user guide for coupling parcs with trace for hexagonal lattice. the work done in this paper will undergo further tuning and a number of sensitivity analyses will be performed to achieve better results. firstly a database of cross sections will be created for multiple steps in the burnup cycle and secondly the trace model will have to be further modified for coupling. acknowledgements i wish to thank ing. miroslav hrehor for allowing me to perform my internship at the research centre rez and do my master thesis. also i wish to thank ing. milos kyncl for providing and assisting with the trace model and to ing. bruno miglierini and ing. vit kopecek for technical help. i would like to also thank the u.s. nrc for helping me with several technical issues with the coupling procedure. references [1] m. ruscak. simulation of reactor kinetics in nuclear power plant using simulator parcs. bachelor’s thesis, university of hradec kralové, 2014. [2] b. miglierini, m. ruscak, g. mazzini. practical acquiring of the parcs code for 3d analysis of neutronic behavior of vver1000/v320. vver 2013 conference, 2013. [3] t. downar, y. xu, v. seker. parcs v3.2, u.s. nrc core neutronics simulator. u.s. nuclear regulatory commision, 2014. um-ners-09-0001. [4] u.s. nuclear regulatory commision. trace v5.840 manual. division of safety analysis, office of nuclear regulatory research, u.s. nuclear regulatory commission, washington, dc. [5] radiation safety information computational center at oak ridge national laboratory. a comprehensive modeling and simulation suite for nuclear safety analysis and design. oak ridge national laboratory, 2011. ornl/tm-2005/39. [6] b. miglierini, g. mazzini, m. ruscak. 3d neutronic analysis of vver1000/v-320 using parcs code. in proccedings of the 2014 15th international scientific conference on electric power engineering (epe). 2014. doi:10.1109/epe.2014.6839473. [7] u.s. nuclear regulatory commision. nureg-0800, standard review plan for the review of safety analysis reports for nuclear power plants, lwr edition. u.s. nuclear regulatory commision, 2007. [8] m. r. guido mazzini, mylos kyncl. analyses of feed water trip with sbo sequence of vver1000 reactor. journal of nuclear engineering and radiation science 2016. doi:10.1115/1.4034144. [9] j. v. javier riverola, tomas nunez. realistic and conservative rod ejection simulation in a pwr core at hzp, eoc with coupled parcs and relap. in proceedings of the 2004 international meeting on lwr fuel performance, orlando, florida. 2004. 71 http://dx.doi.org/10.1109/epe.2014.6839473 http://dx.doi.org/10.1115/1.4034144 acta polytechnica ctu proceedings 4:63–71, 2016 1 introduction 2 parcs code description 3 trace code description 4 scale code description 5 coupling procedure 6 model description 6.1 scale 6.2 parcs 6.3 trace 7 results 8 conclusion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.10.0043 acta polytechnica ctu proceedings 10:43–47, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app modelling rock mass improvement using rock bolts jan pruška czech technical university in prague, faculty of civil engineering, thákurova 7/2077, prague 6, czech republic correspondence: pruska@fsv.cvut.cz abstract. anchor support currently represents a significant reinforcing technique in underground constructions. the principles of rock bolt reinforcement action are derived from various concepts of the underground excavation stability. in recent times, rock bolt design techniques have been complemented by numerical calculations procedures. the paper describes fem modelling of a rock bolt system for mechanical and grouted bolts. keywords: rock bolts, modelling, fem. 1. introduction in recent times, rock bolting represents a significant reinforcing method, especially in tunnelling. the main effect of rock bolting is in reducing and eliminating the impact of different types of failures that occur in the rock mass (schistosity, joints, cracks, etc.) so that the reinforced rock mass can restore the equilibrium disturbed by excavating an underground work. the effect of rock bolting on the rock mass is derived using a variety of methods to determine the stability of underground excavations and the rock bolt type considered (e.g. mechanical or resin). the design and verification of the structural behaviour of rock bolts can be made by any of the following methods: • empirical methods or using rock mass classification, • analytical solution (e.g. rock reinforcement contact problem), • simple calculations based on the fenner-pacher curve theory, • mathematical modelling (numerical solution of a contact problem), • models based on discontinuity mechanics theory, • probabilistic (stochastic) approach to determine the required loading of reinforcement anchorage. of the above methods, mathematical (numerical) modelling using the finite element method (fem) is commonly used in todayâăźs practice. generally, the design of bolts is a complex task that requires the knowledge of rock bolt materials, the anchor technology and the rock mass behaviour. 2. rock bolts modelling using fem the modelling of anchors and rock bolts by fem is more complicated compared with the modelling of the rock mass itself. this is mainly caused by the fact that rock bolts are divided by the type of anchor (simply into two main groups: point-anchored and anchored along its entire length or predominantly over the entire length). thus, the fem model must necessarily take into consideration the type of rock bolt, the anchoring method and the distribution of anchoring forces in the surrounding rock. it can be used for the following task: • modelling a rock bolt as a single element, • homogenization of the rock bolt’s area. in current tunnelling practice, rock bolts attached to the rock along their entire length predominate, thus, the methods using the homogenization of the rock bolt’s area are mostly used. 2.1. modelling of rock bolts using homogenization the principle of this procedure is based on the fact that anchors create a supporting ring in the rock mass near the excavation with characteristics of a thickwalled cylinder. the area of the supporting ring is modelled so that the elements of the finite element mesh in the supporting ring change their geomechanical properties by selecting equivalent isotropic material with improved cohesion. however, this procedure is not suitable for a clearly discontinuous rock mass (connection of rock blocks using rock bolts) because it does not consider the mechanical strength of the rock bolt’s area. czech practice uses the following procedure to increase cohesion in the rock bolt’s area. the increase of cohesion due to bolting is calculated according to the equation: cs = nu + sinϕ′ ak · 2 · cosϕ′ · γkc (1) where: nu loading capacity of the bolt [kn ], ak area per rock bolt [m2], ϕ′ effective angle of internal friction [°], γkc coefficient of bolting reliability [−]. 43 http://dx.doi.org/10.14311/app.2017.10.0043 http://ojs.cvut.cz/ojs/index.php/app jan pruška acta polytechnica ctu proceedings cohesion of equivalent isotropic material: ch+s = ch + cs (2) where: ch+s total cohesion of rock increased due to rock bolting, ch original cohesion of rock, cs cohesion increased due to rock bolting. if we need to take into the account the impact of the bolt on the discontinuity surface, a so-called virtual element can be used in fem. this virtual element models discontinuity surfaces using a conventional rectangular element with a height equal to the length of the plastic area in the bolt (fig. 1). it is assumed for the shear modulus calculation that a failure will occur in the bolt and at the discontinuity interface at the same displacement. the shear modulus was expressed e.g. by h. larsson [1]: gv p = τb uf · e · ab at + τj uf · e · aj at (3) where: gv p shear modulus of the virtual element, τb shear stress at the rock bolt failure, uf block displacement at the discontinuity interface, e height of the virtual element (length of the plastic area in the bolt), ab rock bolt area, aj discontinuity interface, τj shear stress at the discontinuity interface at failure, at total area of the rock with rock bolts (ab+aj). 2.2. modelling of rock bolts as discrete elements the problem of the formulation of a finite element that would describe the stabilizing effect of the rock bolt or rock anchors on the rock mass has been solved in various approaches since early fem numerical analyses (the first models were derived around 1968). thus, a number of special elements for describing rock bolts were developed (for bolts fixed at both ends or along their own length). these special elements are connected with specific special software or they require direct implementation in a programme code by the user. in the following part, one of the most used elements (attached to the rock along their own length) will be described. the principle of this element was presented in the thesis by ömer aydan in 1988 [2]. it is essentially a beam element (special bolt element), which has four nodes, two of which are connected to the anchor rod and the other two to the surrounding rock fig. 2. the following several simplifications have been considered for deriving the stiffness matrix of this element: • the body formed by the grouting material is considered as an axisymmetric thick-walled hollow cylinder, which, due to its shear deformation, transmits tension from the anchor rod into the surrounding rock. • both bolt materials (grouting material and the anchor rod) are considered with a linear elastic behaviour, and thus the relation between the stress and strain in the anchor rod and in the grouting material are described using hooke’s law. • in terms of the coordinates of nodes, the radius of the bolt is negligible in terms of the coordinates of nodes. this presumption naturally does not apply when creating the stiffness matrix. • the bolt considers only the existence of three types of deformation: . ε0 relative longitudinal deformation of the anchor rod caused by axial displacements of the nodes of the anchor rod, . γg shear deformation of grouting caused by different axial displacements of the nodes of anchor rods and the nodes connected with the surrounding rock, . γx transverse shear deformation of grouting caused by different radial displacements of the nodes connected with the surrounding rock. the relationship of the rod bolt strain in terms of nodal displacements (the b index determines the variables associated with the bolt (rod) and the g index determines the values belonging to cement grout): εb = bb ub (4) and the relationship of the grouting ring strain using nodal displacements εg = bg ∆ug (5) where u is the matrix of displacement and b the matrix of differential operators. physical equations for the linear elastic behaviour of rods and the grouting ring can be described using the above expressions as: σb = db εb σg = dg εg (6) where d is the relevant material stiffness matrix. by discretization using finite elements the equations of virtual work (it is assumed that the stress field σ is structurally possible and the field of displacements is kinematically allowed), we get expressions for the stiffness matrix: ke = ∫ btdb d(vol) = ∫ le 0 ∫ rh 0 ∫ 2π 0 btdb dϕdrdz (7) after the integration, we obtain the stiffness matrix of the element in the form given in fig. 3, where 44 vol. 10/2017 modelling rock mass improvement using rock bolts figure 1. virtual element for the rock with bolts. figure 2. scheme of a special bolt element: 1, 2 nodes connected with surrounding rock; 3, 4 nodes connected with the bolt rod. kb = eb · π · r2 b le (8) ks = gb · π · r2 b le (9) kg = π ·gg · le 3ln( rh rb ) (10) aydan’s element has been successfully implemented in scientific and commercial programmes. fig. 4 shows an example of the application of this element to the pmd system by d. runt [3]. 2.3. modelling using geotextile elements some authors in their publications describe the ability to model grouting bolts using geotextile elements e.g. m. šejnoha [4]. these are reinforcing elements which are continuously fixed in the earth massif. this element is, therefore, a system of two node rod elements connected in the places where the line of the geotextile intersects the edge of individual network elements see fig. 5. these elements can only be loaded by tensile forces, they do not have compressive strength and cannot transmit bending moments. they exhibit linear elastic behaviour (that is dependent on a specified compressive strength) and have limited tensile strength until the moment of failure. 2.4. modelling using internal forces in the rock mass modelling using rod elements is another possibility for describing bolts that transmit only axial forces. these elements have the ability to transfer compressive load, unlike the elements for geotextile modelling. it is also possible for this element to specify the input forces in the anchor (prestress) and not consider the prestress due to compressive load. according to some authors (e.g. [5]), the bolt root can be modelled as elements without compressive strength with contact elements. the cohesion of contact elements should be determined so that the total frictional force acting on a 1 m strip corresponds to the frictional force acting on the bolt (reducing cohesion by the ratio of the bolt area to the finite element area). for modelling bolts fixed along their own length, this model is unacceptable in underground engineering [6]. 2.5. modelling using internal forces in the rock mass the use of internal forces is one of the oldest methods of modelling anchors and rock bolts in fem. the principle of modelling consists in the insertion of internal forces into the rock mass at both sides of the rock bolt (head and root). this kind of plane modelling is only used for tensioned bolts or anchors. the inserted forces simulate the bracing area in the rock mass stabilized by rock bolts. however, this kind of modelling often leads to the plastification in the internal force location and to a situation where the calculation does not converge. 3. effect of installation time it is s quite difficult to make a sufficiently accurate model of the effect of rock bolts. we can usually only estimate the maximum possible effect. this is not only due to the established simplifications in different procedures, but the installation time of rock bolts also plays an important role (time delay due to the 45 jan pruška acta polytechnica ctu proceedings figure 3. the stiffness matrix of the element figure 4. rock behaviour in the stress σxx curve without rock bolts (left) and with rock bolts (right) figure 5. dividing geotextiles on rod elements application of shotcrete lining). this effect is very difficult to describe correctly in a numerical model. rock bolts are often part of primary lining and also help to improve the final deformation. therefore, we can only determine correctly the effects of the immediate installation of bolts or bolts installed to partially deformed lining. 4. conclusion this paper gives an overview of different approaches to rock bolts modelling using fem for tasks related to underground structures. from the above mentioned methods, a survey clearly shows that the main approximation of rock bolts in fem uses modified strength and deformation parameters in the rock bolt’s area or specially derived elements (quantifying the effect of bolting for the rock mass). also, fem is not suitable for modelling a discontinuous rock mass and, therefore, a direct impact of rock bolts on discontinuities; we can say that both of the above mentioned approaches (based on the theory of continuum mechanics) are quite suitable for describing the behaviour of rock bolts. subsequently, engineers can choose such bolt properties to reach a steady state of an underground structure and also optimize its design (based on the comparison of fem modelling of different options). 5. acknowledgement this article was written as part of a study within the project supported by the competence centres program of the technology agency of the czech republic (ta cr), no. te01020168. references [1] h. larsson, t. olofsson. bolt action in jointed rock. in rock bolting : theory and application in mining and underground construction : proceedings of the international symposium on rock bolting, abisko, 28 august 2 september 1983, pp. 33–46. balkema publishers, a.a. / taylor & francis the netherlands, 1984. godkänd; 1984; 20080926 (ysko). [2] ö. aydan. the stabilisation of rock engineering structures by rockbolts. nagoya: nagoya university, 1989. 46 vol. 10/2017 modelling rock mass improvement using rock bolts [3] d. runt, j. pruška, j. novotný. modelling of rock bolts using the finite element method. in isrm regional symposium eurock 2015. international society for rock mechanics, 2015. [4] m. šejnoha. finite element analysis in geotechnical design. saxe-coburg publications, kippen, stirling, scotland, 2015. [5] z. bittnar, j. šejnoha. numerické metody mechaniky 1. české vysoké učení technické v praze, 1992. [6] m. hilar. numerická analýza tektonicky porušeného horninového masivu s primární výstrojí při aplikaci nrtm. ph.d. thesis, české vysoké učení technické v praze, 2000. 47 acta polytechnica ctu proceedings 10:44–48, 2017 1 introduction 2 rock bolts modelling using fem 2.1 modelling of rock bolts using homogenization 2.2 modelling of rock bolts as discrete elements 2.3 modelling using geotextile elements 2.4 modelling using internal forces in the rock mass 2.5 modelling using internal forces in the rock mass 3 effect of installation time 4 conclusion 5 acknowledgement references acta polytechnica ctu proceedings doi:10.14311/app.2017.8.0020 acta polytechnica ctu proceedings 8:20–23, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app mechanical properties of cr-dlc layers prepared by hybrid laser technology petr písaříka,b,∗, miroslav jelíneka,b, jan remsaa,b, zdeněk toldec a faculty of biomedical engineering, czech technical university in prague, sitna sq. 3105, 272 01 kladno, czech republic b institute of physics of the czech of sciences, na slovance 2, 182 21 prague 8, czech republic c department of materials engineering, faculty of mechanical engineering, czech technical university in prague, karlovo namesti 13, 121 35 prague 2, czech republic ∗ corresponding author: petr.pisarik@fbmi.cvut.cz abstract. diamond like carbon (dlc) layers have excellent biological properties for use in medicine for coating implants, but poor adhesion to biomedical alloys (titanium alloys, chromium alloys and stainless steel). the adhesion can be improved by doping the dlc layer by chromium, as described in this article. chromium doped diamond like carbon layers (cr dlc) were deposited by hybrid deposition system using krf excimer laser (deposition diamond like carbon graphite target) and magnetron sputtering (deposition chromium chromium target). carbon and chromium contents were determined by wavelength dispersive x-ray spectroscopy. chromium content of cr dlc layers was 0, 1, 2, 4-5 and 15 17 at.%. the topology and roughness of layers were studied using atomic force microscopy. roughness of chromium doped dlc layers was measured on si substrates about 0.2-0.7 nm and on metallic substrates about 1-6 nm. mechanical properties were studied by nanoindentation. hardness and reduced young's modulus were reduced with rising the cr content. hardness and reduced young's modulus reached from 15.0 gpa to 31.2 gpa and from 172.7 to 271.5 gpa, respectively. films adhesion was determined by scratch test and reached 19 n for titanium substrates and for highest cr concentration. good adhesion to biomedical alloys and high dlc hardness will help to progress in the field of implantology. 1. introduction tissue grows around and into all forms of carbon [1–3]. diamond-like carbon (dlc) layers have potential applications in orthopaedics, cardiology, ophthalmology, nephrology, and other fields of medicine [1, 4–9]. dlc layers are ideal for coating stents, heart valves, because of its excellent haemocompatibility and reduced thrombus formation, and for joint implant protective films [10]. dlc have unique mechanical (high hardness = 1 − 80 gpa), tribological (low friction coefficient ≈ 0.01 − 0.7, high wear resistance), optical (transparency in ir and vis), topological (nanosmooth), and biological (chemical inertness, no cytotoxicity, good biocompatibility and haemocompatibility) properties [1, 11–13]. these properties can be modified and adapted for specific medical applications by using doping. dopants in dlc layers produce changes in hardness, coefficient of friction, resistance to wear, surface roughness, adhesion, and even biocompatibility and biological properties [13, 14]. the scheme of typical dopants and supposed change of dlc properties is in figure 1 [13]. the influence and properties of a lot of proposed elements was successfully tested and characterized till now. in our case, the doping of chromium was used to change the mechanical properties and increase the adhesion dlc layers to biomedical alloys. 2. experimental 2.1. depositions chromium doped diamond like carbon layers (crdlc) were deposited by hybrid deposition system consists of pulsed laser deposition (pld krf excimer laser) and magnetron sputtering (ms). pld technique was used for the deposition of dlc and ms technique for doping chromium. deposition parameters are summarized in table 1. figure 2 shows the schematic diagram of the deposition system used to prepare the cr-dlc film samples. silicon (100) wafers and biomedical alloy (ti-6al-4v) were used as substrates. ti-6al-4v substrate was polished before deposition (roughness was 7.7 ± 1.2 nm). 2.2. characterization chromium content of cr dlc layers was determined by a wavelength dispersive x-ray spectroscopy (wds jeol 840). more information can be found in [12]. adhesion macro scratch tester (revetest scratch tester csm co.) was used to determination of the adhesion [15]. scratch test parameters are summarized in table 2. an optical microscope was used to evaluate the critical force. hardness and reduced young's modulus nanohardness was measured on the nanotest system with 20 http://dx.doi.org/10.14311/app.2017.8.0020 http://ojs.cvut.cz/ojs/index.php/app vol. 8/2017 mechanical properties of cr-dlc layers figure 1. scheme of proposed doping elements of dlc [13]. figure 2. the scheme of hybrid deposition system: 1 substrate, 2 carbon target, 3 laser beam, 4 magnetron with cr target, 5 magnetron stopper, 6 rotation, 7 rf, 8 vacuum gauge, 9 tbm, 10 gas flow (ar). laser repetition rate laser energy density magnetron power wds cr content hardness reduced young's modulus [hz] [j·cm−2] [w] [at. %] [gpa] [gpa] cr-dlc-0 20 8 0 0 31.2 ± 1.4 271.5 ± 16.8 cr-dlc-1 40 8 40 1 24.8 ± 1.1 236.3 ± 11.4 cr-dlc-2 20 8 40 2 21.8 ± 0.8 217.7 ± 4.4 cr-dlc-3 10 8 40 4 5 17.5 ± 0.9 183.9 ± 9.5 cr-dlc-4 3 8 40 15 17 15.0 ± 0.6 172.7 ± 3.4 table 1. deposition parameters, chromium content and mechanical properties of dlc and cr doped dlc layers. indenter parameters diamond type, rockwell, radius: 200 µm normal load linearly ramped minimum 1 n and maximum 30 n scratch length 8 mm scratch speed 10 n·min−1 critical loads lc2 edge spallation critical loads lc3 spallation inside the groove table 2. scratch test parameters. 21 p. písařík, miroslav jelínek, j. remsa, z. tolde acta polytechnica ctu proceedings figure 3. afm scans of the surfaces. samples with various concentrations of chromium: afm of pure dlc (left), dlc with 15-17 at. % of cr (right). figure 4. hardness and reduced young's modulus of the dlc and cr-dlc films with various cr contents. a berkovich diamond tip. maximum indentation depth of the indenter was 10 % (about 60 nm), to minimize the effect of substrate on the resulting hardness. the presented values are averages of 20 measurements. hardness and reduced young's modulus was calculated according to [16]. 3. results and discussion cr dlc films were synthesized using hybrid system (magnetron sputtering and pulsed laser deposition) of carbon and chromium target. in dependence with deposition conditions the cr content moved from 1 at. % to ∼ 17 at. % (wds), and the thickness was 800 ± 100 nm on titanium substrate and 100 ± 30 nm on silicon substrate. afm showed that the layers were smooth, but with small amounts of random droplets see figure 3. roughness (ra) were calculated from 10×10 µm area (software nova p9) [15]. ra of our layers was measured on si substrates about 0.2-0.7 nm and on metallic substrates about 1-6 nm. adhesion diamond like carbon have poor adhesion to metal alloys [1]. baragetti [17] presented that diamond like carbon on aluminium alloy had critical load (lc3) about 3.5 n. two scratches were made in each layer and the adhesion was evaluated using a ccd micrograph. due to the substrate roughness caused by polishing, the character of load trace was not monotonous. this fact complicated the determination of critical load parameters. the first spallation presence was used as the critical load value. results of scratch tests measurement showed that the critical load (lc3) for the pure dlc films was about 14 n and for cr dlc films ranged from 15.3 n (1 at. %) to 19 n (15-17 at. %). the same trend was observed in [15]. the higher value of adhesion for pure dlc layers (compared to baragetti group) can be due to the application of the rf cleaning before the deposition and a further increase was reached by chromium doping. hardness and reduced young's modulus the applied maximum load for the film was observed at the depth of 60 nm. nanoindentation also makes it possible to specify the modulus of elasticity. the determination of the reduced young's modulus for the instrumentally performed hardness test is based on the inclusion of the elastic strain of the given ma22 vol. 8/2017 mechanical properties of cr-dlc layers terial and also of the testing indenter. the hardness and reduced young's modulus values for the diamondlike carbon film were determined to be ∼ 31.2 and ∼ 271.5 gpa, respectively see table 1 and figure 4. hardness of cr-dlc layers prepared by pld+ms decreased from 24.8 gpa (1 at. %) to 15.0 gpa (15-17 at. %), as the cr content increased, as well as reduced young's modulus of 236.3 gpa (1 at. %) to 172.7 gpa (15-17 at. %) see table 1 and figure 4. 4. conclusion this paper focuses on doped dlc films (cr-dlc films on silicon and titanium alloy). the layers were prepared using hybrid laser technology (pld+ms). the cr content moved from 1 at. % to ∼ 17 at. %. afm showed that the layers were smooth, but with small amounts of random droplets. with the cr content rise, both the hardness and young's modulus were reduced from 31.2 gpa to 15.0 gpa and 271.5 gpa to 172.7 gpa, respectively. scratch test showed that critical load lc3 rose with cr content and that the maximum critical load lc3 was 19 n. good adhesion on biomedical alloys and high hardness 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[17] s. baragetti, l. lusvarghi, g. bolelli, f. tordini. fatigue behaviour of 2011-t6 aluminium alloy coated with {pvd} wc/c, pa-cvd {dlc} and pe-cvd siox coatings. surface and coatings technology 203(20-21):3078 – 3087, 2009. doi:10.1016/j.surfcoat.2009.03.040. 23 http://dx.doi.org/10.1016/j.mseb.2010.01.010 http://dx.doi.org/10.1007/s00339-010-5912-9 http://dx.doi.org/10.1016/j.diamond.2005.08.025 http://dx.doi.org/10.1016/j.diamond.2005.12.006 http://dx.doi.org/10.1016/j.diamond.2008.04.011 http://dx.doi.org/10.1016/j.diamond.2006.12.009 http://dx.doi.org/10.1016/j.surfcoat.2005.07.077 http://dx.doi.org/10.1007/s00339-012-7216-8 http://dx.doi.org/10.1016/s0925-9635(03)00019-0 http://dx.doi.org/10.1016/s0927-796x(02)00005-0 http://dx.doi.org/10.1007/978-0-387-49891-1_12 http://dx.doi.org/10.1007/s00339-013-8206-1 http://dx.doi.org/10.1016/j.msec.2014.10.035 http://dx.doi.org/10.1557/jmr.1992.1564 http://dx.doi.org/10.1016/j.surfcoat.2009.03.040 acta polytechnica ctu proceedings 8:20–23, 2017 1 introduction 2 experimental 2.1 depositions 2.2 characterization 3 results and discussion 4 conclusion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.10.0001 acta polytechnica ctu proceedings 10:1–6, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app nontraditional support of the western portal of the tunnel považský chlmec jan faltýnek czech technical university in prague, faculty of civil engineering, thákurova 7, prague 6, czech republic correspondence: jan.faltynek@hochtief.cz abstract. the paper is focused on general description of support elements used on the western portal of the tunnel považský chlmec in slovakia, near the city of žilina. it presents basic aspects of the method of the shell structure. in this case the shell structure in combination with pile walls was used. you can also find here detailed description of geotechnical behaviour together with the setting up of the numerical model constructed in plaxis. conclusions of important points from the entire paper including results evaluation you can find at the end of the paper. keywords: tunnel, finite element method (fem), plaxis, shell structure, pile wall, anchor. 1. introduction two-tube tunnel považský chlmec with length of about 2.2 km forms the major part of technically very challenging section žilina (strážov) žilina (brodno) of future highway d3 in the slovak republic. the route forms the western bypass of the city of žilina. the excavation in the area with flysh evolution represents for the designer and also the contractor of the tunnel solving many difficult geotechnical problems. one of them is the technical solution of the construction pit of the western tunnel portal, which was key for compliance with the construction schedule because of the planned construction process. the competition for the contract was launched and construction is still in progress in design and build mode (db) specifying the conditions according to fidic yellow book. it allows the designer and contractor to optimize technical solutions, under the conditions specified in the tender documentation. limited areas of permanent works, tight deadlines of contractual milestones of construction and complicacy of geotechnical conditions in the area led the designer and contractor of the company hochtief cz a. s. [1] to change the concept of securing the stability of the construction pit of the western portal and following excavation beside the original draft from the previous step of project documentation. after considering all options, it was decided to use a method of the shell structure. 2. method of the shell structure method of the shell structure could be classified to the hybrid cover & cut methods that combine various aspects of the excavated and cut & cover underground structures. first part of a construction process is a cutting of a ground down to the level of the lower surface of the shell structure (figure 2 stage 2). that is concreted (figure 2 stage 3) and generally backfilled after curing. the material under the shell structure could be excavated at the same time with the landscaping of the backfilled surface (figure 2 stage 4). this is very positive in terms of time of construction process. there is a big difference from the classic milan method in the shape of the supporting structure, which is in this case vaulted. the vault behaviour of the structure is very positive from the structural point of view. the option to keep the cross section the same like in the excavated part of the tunnel is also advantageous. you can use the same formwork car. method of the shell structure is particularly used for tunnels that are carried shallowly, where can be problem during excavation with breaking the cover of a tunnel, or in landslide areas where the landslide could be in a portal construction pit activated. economically, this method leads to savings earthworks and difficult enumerable reduction of the risk of construction. 3. history of this method and its modifications method of the shell structure is in czech called literally “turtle method”. the term ‘turtle’ was created during the construction of the eastern portal of branisko tunnel (1996), in the slovak republic and its author is ing. ermín stehlik. in this case the shell structure was on one tunnel tube monolithic and on the other tube prefabricated. it is another point of interest of this tunnel. method of the shell structure is quite widespread abroad, for construction in and outside of the urban areas. in the czech republic, this method was first used on the railway section zábřeh krasíkov, tunnels malá huba and hněvkovský i. 3.1. shell structure found on plain ground a shallow tunnel, where the rock strength increases very quickly with the depth, is a typical example of 1 http://dx.doi.org/10.14311/app.2017.10.0001 http://ojs.cvut.cz/ojs/index.php/app jan faltýnek acta polytechnica ctu proceedings figure 1. section situation of the d3 motorway žilina (strážov) žilina (brodno). figure 2. the construction process of the basic method of the shell structure shell structure found on plain ground figure 3. the eastern portal of the tunnel branisko, left monolithic, right prefabricated shell structure (photo by ing. libor mařík [2]) this type of construction. this leads to the use of better quality rock mass as a support for the shell structure. it means that a shell structure rests only on the plain ground. this solution was used for example in tunnels hněvkovský i and schellenberg in germany. figure 4. the shell structure on the schellenberg tunnel (photo by ing. jiří zmítko) 3.2. shell structure additionally supported in worse geological conditions the base part of shell structure is additionally supported due to uneven deformation by columns of jet grouting, micropiles or by using sn rock bolts. this solution was used for example in sudoměřice tunnel and in bypass around 2 vol. 10/2017 nontraditional support of the tunnel považský chlmec the town of jihlava (i / 38), where the shell structure was concreted on low-formwork. another example is the use of this type of structure in the central construction pit of the tunnel povážský chlmec. there was the shell structure supported by micropile walls as well as in the case of the western portal of žilina tunnel. figure 5. the shell structure supported by micropiles in the central pit of the tunnel považský chlmec (photo by ing. libor mařík [2]) 3.3. shell structure with foundations fixed to sheeting construction in the case of very unpleasant geotechnical conditions it is necessary to secure the lateral sides of the tunnel over the entire height in another way milan or pile wall. the shell structure in this case is fixed into sheeting structure and form the support (strut) level of the vertical sheeting elements to ensure the safety of the construction pit. this complex and unique solution has been used in euerwang tunnel on high-speed line nuremberg-ingolstadt in germany and považský chlmec tunnel in the slovak republic on the western portal which technical solution is the main topic of this paper. figure 6. the fixed shell structure on the euerwang tunnel (photo by ing. jiří zmítko) 4. original way of securing the western portal and start of excavation the original way of securing the western portal by tender documentation (which was not obligatory) consisted of the slope stabilization of construction pit by layer of shotcrete with two concrete reinforcing meshes. layers of surface soil were secured by nailing. sn rock bolts were used in the lower parts where occurrence of disintegrated rock was supposed. prestressed stranded anchors passing through reinforced concrete walers were among the other elements ensuring the stability of the construction pit. in this way arranged construction pit the classic cut & cover tunnel should be constructed. initiation of the excavation was assumed under the protection of micropile roof piping. 5. new way of securing the western portal the contractor hochtief cz a. s. decided to change the concept of securing the construction pit after the thorough consultation with the designer at the stage of processing of tender documentation. the method of the shell structure combined with anchored large-diameter pile walls was used for securing the portal area. pile walls work as a construction pit sheeting and also as a protection of the sides of the tunnel during the subsequent excavation under the shell structure roofing. this change reduced volume of earthworks and activities with the necessary technological pauses, e.g. concreting of the reinforced walers, implementing multilevel anchors etc. the size of the territory affected by construction and the number of anchoring elements were reduced too. the length of cut & cover tunnel was shortened to one concreting block. the risk of losing stability of a high slope decreased. the important point was also the possibility of an earlier commencement of the excavation on the western portal. the faces of the excavation pit are stabilized by anchored steal sheet pile walls. (1.) excavation of shallow sloped construction pit at a gradient of 1:1.5 at the level of drilling of the large-diameter pilot walls; (2.) drilling and subsequent concreting of the reinforced concrete piles 0,8 m in diameter length of 16 m, 18 m and 19 m with an axial distance of 1 m; (3.) excavation on the first anchor level; (4.) aking concreate walers with dimensions of 0.7 x 0.8 m, making and activation of prestressed stranded anchors length of 16 m and 18 m drilled with axial distance of 2 m; (5.) excavation of the construction pit at the level of the bottom shape of the shell structure; 3 jan faltýnek acta polytechnica ctu proceedings figure 7. original way of securing the western portal (6.) creating a niche in every individual pile, which is used for connection of the reinforcement of the shell structure with the reinforcement of piles (in each pile was added additionally glued anchor); (7.) profiling of the base of foundation pit by plane concrete into its final form, laying separating foil and geotextile; (8.) reinforcing and concreting the shell structure block by block (thickness of the structure in the crown is 0.6 m, the arch span is 10.78 m with the rise of 3.53 m, final length on southern (right on the picture) tunnel tube 37.5 m and on northern (left on the picture) tube 50 m); (9.) excavation of top heading and bench of the tunnel (excavation with horizontal sequence, unlimited length advance thanks to good workability by tunnel bagger); (10.) additional supporting of the foundation of the shell structure and shaping the sides of the tunnel by shotcrete lateral beams; (11.) making of the backfill (the shell structure was filled up after the tunnel excavation because of the need to meet a milestone for the beginning of the excavation, another reason was structural, because of the shell structure which had to be filled after making the supporting lateral shotcrete beams). 6. geological conditions at the western portal the excavation is in the upper part realized in finegrained deluvial soil with the occurrence of fragments and rubble. they passed with increasing depth into the gravel-clay soil of fluvial terraced steps. the lower part of the construction pit was excavated in the zone variously weathered flysch formation (sandstones, mudstones, siltstones, conglomerates). 7. numerical model of securing the western portal the complexity of static calculations was based mainly on uncertainty about the actual behaviour of the structural elements (prestressed stranded anchors, large diameter pile walls, shell structure) and consideration of these ideas in the mathematical model. the most important thing for the creation of a numerical model is in this case the reliable and accurate interaction between the shell structure, sheeting wall and cooperating rock mass considering all phases of construction and the relevant load cases. the connection between the shell structure and the pile wall is capable of transmitting a certain inner forces. its real stiffness but depends primarily on the quality of the execution. during the processing of the project there were a large amount of computations, whose aim was to determine the effect of input variables. secondary lining under the shell structure was examined in detail in the last phase stage simulating end of life of the construction pit supporting system where backfill weight rests directly on the secondary lining. calculations were performed by finite element method in program plaxis. the dimensions of the solved area were chosen so that the results were not affected by the boundary conditions. the finite element mesh in areas of interest was refined. all rock and soil layers were considered as plane elements with the mohr-coulomb plasticity condition. the shell structure, pile wall, shotcrete supports and secondary lining were modelled as linear plane element. to the centreline of these structural plane elements was inserted so called “reference beam”, which has a considerably smaller bending and axial stiffness. it deforms simultaneously with the structure. thanks to it, there is no need to integrate internal forces from the stress in the individual sections. the interaction between structural elements and the rock mass as well as between the individual elements together was modelled using a specially tested contact interface element. the reached ground water level and ground water flow due to the excavation of the bench was also considered in the calculation. it was very important in the numerical model to take into account all necessary load cases. the weather load (mainly temperature) and shrinkage was modelled as prescribed volume strain of finite elements. 4 vol. 10/2017 nontraditional support of the tunnel považský chlmec figure 8. new way of securing the western portal surroundings of žilina is located in a seismic zone. this effect was taken into consideration into the model using quasi-static calculation. figure 9. scheme of a basic numerical model 8. results of numerical modelling the mathematical model confirmed the smooth feasibility of designed construction system. first the slope stability of the construction pit excavated at the level of pile walls was determined by the phi-c reduction method. with “reference beam” internal forces acting on the pile wall were obtained. the bearing capacity of stranded anchors was also evaluated. as mentioned above, the greatest influence on the interaction of the whole system has a connection between the shell structure and pile walls. connection height is about 1.5 m. it is very difficult to predict how a given node will behave. therefore, it is necessary to monitor and evaluate stress at this point in principal stresses. from the structural point of view, the decisive stage is the construction phase after the completion of the excavation under the shell structure. the positive impact of the backfill on the distribution of stresses on the shell structure and pile walls was also confirmed. figure 10. envelopes of internal forces on the pile wall from left to right (nmax = -695 kn, vmax = 550 kn, mmax = 900 knm) 9. conclusion if predicted and actual geological conditions should be compared, it could be said, that sufficient consensus has been reached. geotechnical monitoring of the shell structure consisted of determining the relative deformation by strain gauge sensors located in the major blocks in the top of the vault at both surfaces. it allowed to compare the results of a numerical model with reality. an interesting finding was that the shell structure on north and south tunnel tube behaves differently in reality. a comparison of the data after the excavation under the shell structure with the results of the monitoring are quite different. both northern and southern structures in the case of a numerical model behave similarly (the upper fibres of a cross section are in tension, lower are compressed). acceptable sim5 jan faltýnek acta polytechnica ctu proceedings figure 11. distribution of principal stresses after the excavation stage (left) and after the final stage (right) (compression red and tension blue colour) figure 12. shell structure on the western portal of the tunnel povážský chlmec ilarity is evident when comparing the southern shell structures. the results from the measurement on the north shell structure are not very close. that is also the same case for other construction stages. simplifications of the numerical model (material model of construction elements and surrounding soil and rock, sub-horizontal layers etc.) and the real behaviour of the structural elements (the value of the prestressing in the anchors, the real execution of the connection between structures) may be a possible cause. as you can see even the most complex mathematical model may not always accurately capture the geotechnical behaviour of the real structure. the shell structure fixed into the sheeting structure belongs to the most unique and less conventional design solutions. the designer and contractor despite it managed to design and build a structure without significant problems during construction. generally, it could be said, that the correct optimization of the solution of the western portal had contributed to reducing the risks during construction and speeded up the construction progress. at the time of writing this paper the construction is completed successfully, backfilled and supported by final lining of monolithic concrete. it allows the above mentioned recap. references [1] hochtief cz a.s. zds a rds tunelu povážský chlmec 2015-2016. [2] l. mařík. povážský chlmec tunnel on žilina (strážov) žilina (brodno) section of the d3 motorway from design to realisation. tunel 3:88 – 103, 2015. 6 acta polytechnica ctu proceedings 10:1–6, 2017 1 introduction 2 method of the shell structure 3 history of this method and its modifications 3.1 shell structure found on plain ground 3.2 shell structure additionally supported 3.3 shell structure with foundations fixed to sheeting construction 4 original way of securing the western portal and start of excavation 5 new way of securing the western portal 6 geological conditions at the western portal 7 numerical model of securing the western portal 8 results of numerical modelling 9 conclusion references 212 acta polytechnica ctu proceedings 2(1): 212–216, 2015 212 doi: 10.14311/app.2015.02.0212 detection of diatomic molecules in the dust forming nova v2676 oph m. nagashima1, a. arai1,2, t. kajikawa1, h. kawakita1, e. kitao1, t. arasaki1, g. taguchi1, y. ikeda1 1kyoto sangyo university, koyama astronomical observatory 2university of hyogo, nishi-harima astronomical observatory corresponding author: g0837714@gmail.com abstract novae are generally considered to be hot astronomical objects and show effective temperatures up to 10,000 k or higher at their visual maximum. but, it is theoretically predicted that the outer envelope of the nova outflow can become cool enough to form molecules that would be dissociated at high temperatures. we detected strong absorption bands of c2 and cn radicals in the optical spectrum of nova v2676 oph, a very slow nova with dust formation. this is the first report of the detection of c2 and the second one of cn in novae during outburst. although such simple molecules are predicted to form in the envelope of the outflow based on previous studies, there are few reports of their detection. in the case of v2676 oph, the presence of the molecular envelope is considered to be very transient, lasting several days only. keywords: cataclysmic variables classical novae optical spectroscopy ir individual: v2676 oph. 1 introduction dust formation in the outflow of a nova had been proposed by mclaughlin (1935) to explain the rapid drop in the visual light-curve of dq her in 1934. dust formation in fh ser had also been confirmed by infrared observations by geisel et al. (1970). dq her was the first nova in which molecular absorption bands of cn in optical wavelength had been identified. the formation of molecules as the precursor to dust grains in novae is considered important for understanding how dust grains form in the outflow of novae. in the case of dq her in 1934, strong cn absorption bands of both violet and red systems had been detected merely 2 days after the visual maximum, and these absorption bands were identified for only 1 week approximately (wilson & merrill, 1935; sanford, 1935; stoy & wyse 1935; antipova 1969; sneden & lambert, 1975). since the formation of simple molecules such as cn is considered an intermediate process in the formation of dust grains from the hot atomic gas in the outflow of a nova, molecular formation in the early phase of dq her might be associated with dust formation its later phase. although cn is the first molecule observed in a nova during outburst (in the case of dq her), there are no further reports about cn in other novae. whereas, carbon monoxide (co) emission in the early phase of novae has been observed by both photometric and spectroscopic observations. in particular, the first overtone band of co (∆v = 2) has been routinely detected in near-infrared spectra of several novae, as reviewed by evans & rawlings (2008). based on previous observations, the correlation between detection of co and dust formation is noticeable. however, hydrogen (h2) or other molecules have not detected in novae during the early phase of their outburst. here we report the detection of c2 and cn in optical spectra of the classical nova v2676 oph during the early phase of its outburst. this nova could be classified as a slow nova, and it showed a rapid drop in its visual light curves about 90 days after its discovery. this is the first report of the detection of c2 in novae during outburst and the second for cn. furthermore, co emission in the near-infrared had been detected in this nova (rudy et al., 2012). 2 observations nova v2676 oph (pnv j17260708-2551454) was discovered at ut 2012 mar 25.789 (t = 0 day) by h. nishimura (reported in the central bureau electronic telegram (cbet) 3072). after the discovery of the nova, we carried out spectroscopic observations with the low-dispersion spectrograph losa/f2 (shinnaka et al., 2013) mounted on the 1.3-m araki telescope at koyama astronomical observatory on ut 2012 mar 27. on the 212 http://dx.doi.org/10.14311/app.2015.02.0212 detection of diatomic molecules in the dust forming nova v2676 oph first night, we detected narrow balmer emission lines (both hα and hβ) and narrow fe ii emission lines on a highly reddened continuum that seemed to be due to interstellar extinction. the color excess e(b − v ) was estimated by using the balmer decrement and the color of the nova (b−v ); it was determined as 0.71±0.02 and 0.72±0.06, respectively. based on the p cygni profile of the hα emission, the expansion velocity was estimated to be ∼ 800 km/s. we concluded that the object was a fe ii-type classical nova in the early phase (arai & isogai, 2012). after the first observation of v2676 oph, we continued the observation of it routinely to assess its the spectroscopic evolution (nagahsima et al., 2014). 4500 5000 5500 6000 6500 7000 7500 n or m al iz ed s pe ct ru m wavelength [å] ∆v=+1 ∆v=0 ∆v=−1 c 2 ∆v=+5 ∆v=+4 ∆v=+3 cn hβ na i hα o i v2676 oph tx psc figure 1: comparison of the spectrum of v2676 oph obtained on apr 8 with that of a typical carbon star, tx psc. tick marks indicate telluric absorption lines. after the first spectroscopic observations on ut 2012 mar 27, the emission lines in the optical spectra became fainter relative to the continuum (on ut 2012 mar 28, apr 4 and 6), while the optical brightness was increasing slowly (the optical brightness changed gradually from 12 to 11 magnitudes in the v-band, see the american association of variable star observers (aavso) database, http:// http://www.aavso.org/lcg/). no emission lines could be observed (except hα emission with a p cygni profile), but many absorption lines of fe ii and neutral atoms such as na i (5890å) and o i (7773å) were detected clearly in the spectra obtained on apr 6 (t = 12 days). those absorption lines are indicative of lower ionization and the lower temperature conditions in the outflow of the nova. prominent c2 (swan) and cn (red system) absorption bands were detected on ut 2012 apr 8 (t = 14 days), as shown in figure 1. the obtained spectrum is similar to that of a carbon star. we also plotted the spectrum of tx psc (a well-known carbon star of spectral type n0;c6,2, with teff = 3030 k; lambert et al.,1986) for comparison. we also identified weak emission lines of hα, hβ, and fe ii. based on the substructure of the c2 swan band (∆v = -1) absorption, we could derive the isotopic ratio of carbon. figure 2 shows the spectrum of the nova, the modeled spectra of 12c12c, 12c13c, and 13c13c (with an excitation temperature of 4500k). the doppler shift of the nova spectrum has been corrected by using the relative velocity of the nova to the observer, estimated as 341±87 km/s (this is derived from the velocities for hα and hβ emission peaks). the wavelengths of sub-peaks in this band cannot be explained by 12c12c only. clearly 213 m. nagashima et al. 12c13c and 13c13c contribute to form the absorption. 0.75 0.8 0.85 0.9 0.95 1 1.05 1.1 5400 5450 5500 5550 5600 5650 5700 5750 n or m al iz ed fl ux wavelength [å] 13 13 c c 13 12 c c 12 12 c c apr. 08.7 figure 2: comparison between observed and modeled spectra of the c2 (∆v = -1) absorption band. the observed spectrum is shown by dashed line (the region influenced by the hg emission from the city-light, at ∼ 5460 å, has been removed). the modeled spectra for 13c13c, 12c13c and 12c12c are shown by the thin solid lines and the sum of those lines is shown by the thick solid line. for the modeled spectra, we assumed the rotational and vibrational temperatures of 4500 k and the isotopic ratio of 12c/13c = 4. the next observations were carried out on ut 2012 apr 16 (t = 22 days). in these observations, the c2 and cn absorption bands had already disappeared and strong balmer emission lines and fe ii lines were again prominent. at that time, the spectra were typical of fe ii-type classical novae. the other difference from the previous observations was the expansion velocity derived from hα, which had increased in comparison to that before molecular formation. this higher velocity is typical of the fe ii-type novae (williams 1992). thereafter, the spectra of this nova were not unusual for an fe ii-type nova, although we continued spectroscopic monitoring observations until ut 2012 may 26. the optical light curves showed a very slow decline after the visual maximum and a rapid drop (by about six magnitudes in the v-band) at around 90 days after the discovery (this nova can be classified as a ”slow” nova). the drop in the light curves may be caused by dust formation in the outflow of the nova. 3 results & discussion the equivalent widths of hα (and also of hβ) measured in our spectra were almost constant before and after the appearance of molecular absorption bands. however, optical light curves showed a small drop of ∼ 1 magnitude before and after molecular formation. figure 3 shows the optical and near infrared light curves taken from the database of the aavso and small and moderate aperture research telescope system (smarts), the color indices of (v − i) and the equivalent width of hα and hβ. for example, the c2 absorption could markedly affect band v-band magnitudes, while cn red absorption could also affect rand i-bands. this implies that extinction of the molecules in the outflow affected both continuum and emission lines from the nova. the molecular formation zone could be in the outer region of the outflow compared with regions emitting the continuum and/or emission lines in the nova. 1.2 1.4 1.6 1.8 2 v-i (aavso) v-i (smarts) -600 -500 -400 -300 -200 -100 0 0 10 20 30 40 50 60 70 80 90 100 110 120 hα hβ 5 10 15 20 25 v-mag. (aavso) v-mag. (smarts) i-mag. (aavso) i-mag. (smarts) k-mag. (smarts) figure 3: multi band light curve of v2676 oph (data from aavso and smarts), color indices (v −i) based on the aavso and smarts database, and equivalent widths of hα and hβ measured in our spectra. upper tick marks indicate days on which spectroscopic observations were performed. furthermore, molecular formation in v2676 oph is considered very rapid (within 2 days or less) and the existence of the molecular envelope was transient (it was present at most 9 days) at around the brightness maximum in optical. why was the appearance of both c2 and cn absorption bands so transient that they could be detected on apr 8 only? we considered that the outer region of the outflow became cool enough to form molecules, since the hard ultraviolet (uv) radiation from the pseudo-photosphere of the nova in the early phase was blanketed by an giron curtainh, and the iron ions could have absorbed uv radiation strongly (shore, 2008). this picture is consistent with the spectrum taken on apr 6, which was dominated by a continuum with absorption lines indicative of lower ionization conditions. the measurements of the color indices (v − i) obtained from the aavso and smarts database also showed a redder continuum for later periods after the discovery until the molecular bands appeared. this fact also supports the later lower color temperatures until molecular formation. however, as the envelope expanded and ejected materials rarefied (i.e., became more optically thin), hard uv radiation again increased in intensity. at this time, molecules would be destroyed 214 detection of diatomic molecules in the dust forming nova v2676 oph through photo-dissociation reactions caused by uv radiation. in support of this, the later spectra showed many emission lines from ionized species, such as fe ii. however, the molecular absorption bands may have disappeared due to some opacity effects. similar behavior in terms of cn formation was observed in dq her in 1934. the appearance of cn absorption bands immediately following the optical brightness maximum was transient, persisting for approximately 1 week only (sneden & lambert, 1975). the possible dust formation about 100 days after discovery was also similar to v2676 oph. theoretical studies of chemistry in the outflow of novae suggest that formation of even more complex molecules is possible (pontefract & rawlings, 2004; evans & rawlings, 2008). it has been demonstrated that a model atmosphere could reproduce both strong cn absorption bands in optical and the co emission band in the nearinfrared, as observed in some novae (hauschildt et al., 1994). although simple molecules might be destroyed by uv radiation, more complex molecules such as polycyclic aromatic hydrocarbons (pahs) (if they formed during the transient cool phase of the outer envelope), could survive and might act as nuclei for dust formation. indeed, pah emission was detected in this nova. we performed mid-infrared spectroscopic observation using a cooled mid-infrared camera and spectrometer (comics) mounted on the subaru telescope on ut 2013 june 20 (t = 452 days). the spectrum showed pah emission at 11.4 µm (and a hint of the emission line at 7.7 µm) on the smooth continuum that could be explained by amorphous carbon grains. 1 1.5 2 2.5 3 3.5 4 4.5 5 8 9 10 11 12 13 f lu x de ns ity [1 0-1 8 w /c m 2 /µ m ] wavelength [µm] pah figure 4: the mid-infrared spectrum of v2676 oph. references [1] mclaughlin, d.b. 1935, publ. aas, 8, 145. [2] geisel, s.l., kleinmann, d.e., low, f.j. 1970, astrophysical journal, 161, l101. doi:10.1086/180579 [3] wilson, o.c. & merrill, p.w., 1935, publications of the astronomical society of the pacific, 47, 53. [4] sanford, r.f. 1935, publications of the astronomical society of the pacific, 47, 209. [5] stoy, r.h. & wyse, a.b. 1935, publications of the astronomical society of the pacific, 47, 50. [6] antipova, l.i. 1969, soviet astronomy a.j., 13, 288. [7] sneden, c. & lambert, d. 1975, monthly notices of the royal astronomical society, 170, 533. doi:10.1093/mnras/170.3.533 [8] evans, a. & rawlings, j.m.c. 2008, in classical novae, 2nd edition. edited by m.f. bode and a. evans (cambridge astrophysics series, no. 43, cambridge: cambridge university press, 2008), p.308. [9] rudy, r. j., et al. 2012, electronic telegram no. 3103, central bureau for astronomical telegrams, international astronomical union (ed., green, d.). [10] nishimura, h. 2012, electronic telegram no. 3072, central bureau for astronomical telegrams, international astronomical union (ed., green, d.). [11] shinnaka, y., kawakita, h., kobayashi, h., naka, c., arai, a., arasaki, t, kitao, e., taguchi, g., ikeda, y. 2013, icarus, 222, 734. doi:10.1016/j.icarus.2012.08.001 [12] nagashima, m., et al. 2014, astrophysical journal letter, 780, 26 doi:10.1088/0004-637x/780/1/26 [13] arai, a. & isogai, m. 2012, electronic telegram no. 3072, central bureau for astronomical telegrams, international astronomical union (ed., green, d.). [14] lambert, d.l., gustafsson, b., eriksson, k., hinkle, k.h. 1986, astrophysical journal supplement series, 62, 373. doi:10.1086/191145 [15] williams, r.e. 1992, the astronomical journal, 104, 725. doi:10.1086/116268 [16] shore, s.n. 2008, in classical novae, 2nd edition. edited by m.f. bode and a. evans (cambridge astrophysics series, no. 43, cambridge: cambridge university press, 2008), p.194. [17] pontefract, m. & rawlings, j.m.c. 2004, monthly notices of the royal astronomical society, 347, 1294. doi:10.1111/j.1365-2966.2004.07330.x 215 http://dx.doi.org/10.1086/180579 http://dx.doi.org/10.1093/mnras/170.3.533 http://dx.doi.org/10.1016/j.icarus.2012.08.001 http://dx.doi.org/10.1088/0004-637x/780/1/26 http://dx.doi.org/10.1086/191145 http://dx.doi.org/10.1086/116268 http://dx.doi.org/10.1111/j.1365-2966.2004.07330.x m. nagashima et al. [18] hauschildt, p.h., starrfield, s., allard, f. 1994, in cool stars; stellar systems; and the sun; eighth cambridge workshop, astronomical society of the pacific conference series, vol. 64; proceedings of the 8th cambridge workshop (held in athens, georgia; october 11-14; 1993; san francisco: astronomical society of the pacific (asp); 1994; edited by jean-pierre caillault), p.705. 216 introduction observations results & discussion acta polytechnica ctu proceedings doi:10.14311/app.2015.1.0051 acta polytechnica ctu proceedings 2:51–56, 2015 © czech technical university in prague, 2015 available online at http://ojs.cvut.cz/ojs/index.php/app a case for domain-independent deterministic multiagent planning michal štolba department of computer science, faculty of electrical engineering, czech technical university in prague, karlovo nám. 13, 121 35 praha 2, czech republic correspondence: stolba@agents.fel.cvut.cz abstract. the notion of planning using multiple agents has been around since the very beginning of planning itself. it has been approached from various viewpoints especially in the multiagent systems community. recently, domain-independent multiagent planning has gained more attention also in the automated planning community. in this paper, we shortly present the current state of the art, question some aspects of the research field and discuss the rising challenges. keywords: planning, multi-agent planning. 1. introduction we could trace the first mention of multiagent planning back nearly as far as strips itself – in 1980 nillson published together with konolige a paper titled “multiple-agent planning systems” [1], in which they presented a high-level extension of strips [2] towards multiple agents. since then, the topic has been active mainly in the multiagent systems community. one of the most cited works on distributed and multiagent planning is [3], which describes basics of possible coordination schemes for planning agents. there was also a large amount of work dealing with another facets of the coordination area, but usually without deeper study of the plan synthesis part (e.g., gpgp [4]) or requiring additional domain-specific knowledge (e.g., talplanner [5]). multiagent planning also often relates to planning models described by decentralized pomdps (dec-pomdps) [6], similarly as pomdps are used in single agent planning under uncertainty. the point of view on multiagent planning from the multiagent community is extensively summarized in [7, 8]. in the planning community, extensions of the pddl language intended to support multiagent planning were introduced as multiagent planning language (mapl) in [9] and as multiagent pddl (ma-pddl) in [10], but none of the extensions gained wide popularity, probably because of their complexity. in 2008, a well accepted paper on multiagent planning was published by brafman and domshlak at the icaps conference [11], which finally ignited more interest in the topic. the paper formally introduced a minimalistic extension of strips (thus forming ma-strips) and have shown that the complexity of multiagent planning is not directly exponentially dependent on the number of agents, but rather on the tree-width of their interaction graph and a minimal number of interactions needed to solve the problem. such results suggested that at least for loosely coupled problems (where the tree-width is low), the approach may be beneficial. in the following years, several multiagent planners were proposed [12–19], either using directly the ma-strips formalism, or some ad-hoc, but very similar one. rather different approach was taken by crosby et al. in [20, 21], where the agent decomposition was based not on actions, but on a variables in finite domain representation, and was used in a centralized planner, significantly improving performance over (single agent) sota mainly in well decomposable domains. a dedicated workshop distributed and multiagent planning (dmap) also took place at the icaps’13 and icaps’14 conferences. 2. ma-strips ma-strips is the most commonly used formalism for domain-independent deterministic cooperative multiagent planning. the domain independence means that the input of the planner consists of description of available operators, predicates, functions etc. describing the general mechanics of the world as well as the particular instance of the world represented by ground initial state and the particular problem represented by the ground goal facts that need to be achieved. most commonly the input is described using pddl language, where the general part is termed “domain” and is described in a domain file and the particular initial and goal configurations are termed “problem” and are described in a problem file. in the multiagent setting, additional information is typically needed to determine what are agents and which actions belong to which agent (this is not part of the ma-strips formalism). deterministic in this case relates to the action model, where each action has deterministic effects, although the multiagent planning algorithm itself may be non-deterministic in the sense that for the same input it gives different output and runs for different time this is caused by the inherent nondeterminism of communication and distributed computation. 51 http://dx.doi.org/10.14311/app.2015.1.0051 http://ojs.cvut.cz/ojs/index.php/app michal štolba acta polytechnica ctu proceedings by cooperative multiagent planning we understand a setting where a group of agents is attempting to find a joint plan, where each agent uses its own actions in order to reach some joint (and possibly some private) goals. the agents typically need to coordinate their actions and to cooperate in order to do so, although each agent is planning for itself and the agents may have some private knowledge which they do not want to reveal to other agents. the ma-strips formalism is very much the same as the original strips, except that the actions are disjunctively split (or factored) among the agents, resulting in the following definition of the multiagent planning problem: definition 1. multiagent planning problem is a quadruple π = 〈l,a, s0, sg〉, where l is a set of propositions, a is a set of agents α1, . . . , α|a|, s0 is an initial state and sg is a set of goal states. an agent α = {a1, . . . , an} is represented by a set of actions it can perform. a state s ⊆ l is a set of atoms from a finite set of propositions l = {p1, . . . , pm} which hold in s. an action is a tuple a = 〈pre(a), add(a), del(a)〉, where a is a unique action label and pre(a), add(a), del(a) respectively denote the sets of preconditions, add effects and delete effects of a from l. in the set of propositions l can further be identified subsets of public propositions known to all agents and α-internal (a.k.a. α-private) propositions known only to a specific agent α. such separation of the propositions can be derived from the problem itself (as proposed in [11]) , where a proposition is public iff it is used by any two actions of different agents and it is internal to the agent α (α-internal) iff it is used only in actions of agent α. alternatively, what propositions are public or private can be a part of the problem definition (used in [16, 17]). how the actions are partitioned among agents is not a part of the ma-strips definition and is implementation dependent, in most planners, the agents are defined as objects in pddl and an action is assigned to an agent if the agent object is part of the grounded parameters of the action. similarly to the separation of the propositions, the actions of a single agent can be seen as either public or internal. an action a ∈ α is internal iff it uses only α-internal propositions in its preconditions and effects. otherwise, the action is public, which in fact means, that the action interacts with some other agent, or agents. following the strips formalism, a solution for the multiagent planning problem is a set of sequential plans (sequence of actions, one plan for each agent), where some of the actions of different agents may be performed in parallel, although in most implementations the resulting plan is sequential (i.e. there are no parallel actions). formally, the solution is defined as follows: definition 2. a solution to multiagent planning problem ∏ is a multiagent plan p =〈 pα1 , ..., pα|a| 〉 , where each pαi is a plan of agent αi, i.e. consisting of a sequence of actions in αi ∪ {noop}. a multiagent plan p is valid, iff (1.) for each α, β ∈ a, |pα| = |pβ |. the noop actions mean that the agent is idle in the respective timestep. (a) for each time-step tk where k ∈ 〈1, ..., |pα|〉, actions ai = pαi [tk] for all i ∈ 〈1, ..., |a|〉are not mutually exclusive. (b) all actions in time-step t1 are applicable in the initial state, for all time-steps tk where k ∈ 〈2, ..., |pα|〉, actions in tk are applicable in the state resulting from time-step tk−1 and the state resulting from time-step t|pα| is in the set of goal states sg. since all the plans are required to have the same length, the ma plan can be represented by a matrix, where each row consists of a plan for single agent and each column contains all actions in the respective time-step. it is clear that the ma-strips formalism is very simplistic and minimalistic extension and can be developed further to accommodate various aspects of the multiagent systems (i.e., finer separation of public and internal actions, as discussed for example in [22]). the philosophy of the formalism is to provide the smallest possible common ground and to enable the easiest possible migration of the planning algorithm to the multiagent setting. unlike in many multiagent systems, the mastrips formalism assumes the agents to be fully cooperative. from the multiagent perspective, this may seem as an oversimplification, but similarly to the simplicity of the ma-strips, we argue to first tackle the problems of the simplest possible multiagent extension – cooperative agents – and then gradually add complexities of the multiagent nature, such as selfish agents, negotiation and such. some attempts have already been taken, for example in [23, 24]. 3. is it any good? the first question that is asked after introduction of some new or nonstandard paradigm is – what is it good for? how does it help us? in this paper, we would like to ask such questions and try to come up with some answers. from the multiagent point of view, we can see significant benefits of introducing domainindependent planning into multiagent systems, namely reuse of the wide spectrum of planning systems and techniques from the area of classical planning. on the other hand, the drawback of ma-strips for the multiagent setting is that it requires cooperation among the agents. this can be mitigated in future by means such as mechanism design, as shown in [24]. 52 vol. 2/2015 a case for domain-independent deterministic multiagent planning in the following section, we will present some of the benefits we suggest that multiagent planning may bring to the area of planning in general. 3.1. improve scalability by decomposition although being largely improved in recent years, scalability is still an issue for domain-independent planning. multiagent planning can be seen as a method of factorization of the planning problems, which has been studied in works such as [25, 26]. it has been shown that factorization of the planning problem can be beneficial, especially in the problems, where it is possible to find large independent parts – loosely coupled problems. take for example the rovers domain with several rovers. the problem may be factored in such a way that the rovers do not need to coordinate, except for the last bit, where they use shared communication channel to communicate the result. in such a case, most of the planning can be done independently (even on different machines), however some coordination is needed here (it is not possible to simply run several classical planners in parallel). this is a case for multiagent planning. given a single agent problem (e.g. from the ipc benchmark set), it is not obvious what entities should be considered as agents and how the factorization should be done. in ma-strips, the first question is not answered, but the second one has some theoretical background. once the actions are assigned to agents, the factorization is based on the interactions among the agents’ actions, effectively meaning that it is based on the causal graphs of the problem (as in [11]), the factoring is one of the best known to date, as shown in [25]. still, how to best assign actions to agents is an open question. in the fmap planner [17, 27] formalism, the actions are assigned to agents by the domain designer, as is the separation of private and shared information. this gives the domain designer more freedom, but also more responsibility in that making more information public may increase the problem complexity (as the tree width of interaction graph rises) and making less information public may render the problem unsolvable (i.e. global solution may not exist). completely different approach to factorization was taken by crosby in [20, 21], where the factorization is automatic and based on the variables of a finite domain representation (fdr) of the planning problem. the method is, again, based on causal graph structures and tries to identify agents as sets of variables which are somehow self-contained and represent the agent’s internal state. variables which do not form an internal state of any agent are understood as environment and thus public variables. classification of actions is rather more complex than in ma-strips, but can be summarized as follows. actions, which interact only with the agent variables are assigned to the particular agent, other actions are left as public, which means that they can be used by any agent. this approach was not shown to increase scalability, but was shown to increase solution efficiency, especially in some domains. note, that crosby’s approach was implemented as a centralized, single-thread planner. various kinds of factoring, and understanding gained from the research of it, may be also used for other aspects of classical planning, such as search state pruning [28]. 3.2. multi-core / cluster computing planning on multi-core machines gained wide popularity and had a separate track at the ipc2011 competition. it is definitely beneficial to be able to scale the computation using multiple cores. but, if we want to scale the computation even further and use multiple machines, we are no longer able to use shared memory (as in parallel computation). in such case, approaches of distributed computing utilizing message passing need to take place, and multiagent planning aspires to be one of them (although obviously not the only one). in this scenario, multiagent planning represented by ma-strips can be seen as an equivalent for distributed planning with factorization fixed by the partitioning of actions to particular agents. such approach has been successfully tested against sota in multi-core planning in [14] as a parallel version of mad-a*, called map-a*. again, the question of best factorization arises here, with the crosby’s variable based factorization being another candidate, however never tested in a distributed system. 3.3. privacy in multiagent systems, privacy of the data is often one of the main concerns. in ma-strips-based multiagent planning, this requirement is not one of the top priorities – the privacy (or internality) of the propositions and actions is understood rather as a way of improving effectiveness of the computation by reducing the complexity – but nonetheless if required by the application, some degree of privacy of the data can be achieved. in practice, it may be somewhat harder not to reveal the structure of the private information and it may also reduce usability of some techniques, such as distributed heuristics, but it seems to be possible. one such approach was described in [22], but without implementation or experimental evaluation. 3.4. asynchronous computation distributed computation (and multiagent as well) is inherently asynchronous and non-deterministic. this brings several challenges and complexities that need to be tackled, but once solved, some of the insights may be beneficial to classical planning as well. as a representative example, we can take the computation of a global heuristic. a heuristic in multiagent planning can be computed locally, using only a projection of the planning problem to the propositions of the respective agent. a public 53 michal štolba acta polytechnica ctu proceedings action a ∈ α can be projected to agent β by removing all α-internal propositions from pre(a), add(a) and del(a), thus retaining only public propositions (and technically also β-internal propositions, but actions of agent α contain none). such heuristics were used for example in [14]. a different approach is to attempt to compute a global heuristic estimate without exposing the internal information to other agents. this can be achieved for example by requesting other agents for their estimates of the current state and the goal, or some sub-goals, as in [29, 30]. such global heuristic computation may involve nontrivial communication, resulting in an asynchronous computation of the heuristic estimate. to our knowledge, such a phenomenon has not been studied yet. it seems to be interesting also from the point of view of classical planning, because if successfully utilized, asynchronous computation of heuristics may be used to evaluate computationally intensive heuristics, to use external solvers for heuristic estimation, sensory input (in robotics), etc. also it is interesting to observe that the global heuristic is always equally or more informative than the projected heuristic, thus we have two heuristics, the first one is less informative, gives lower estimates, but is faster, the second one is more informative, gives higher estimates, but takes significantly longer to compute. if generalized, a sequence of gradually more precise, but costlier heuristics could be used to guide search (including blind search as the fastest one), which is an interesting research topic. also, as the costly distributed heuristic is computed partly by other agents, the time while waiting for the results may be used to do some more computation such as exploration using only the local heuristic. 3.5. applications ma-strips planning may bring domain independent planning to some (more or less) new application domains. as such we see the following: • multi-robotics: slowly but steadily, domainindependent planning is penetrating the robotic research, providing the robots with high-level reasoning. on the other hand, robotic research is being extended towards multi-robotic teams. multiagent planning seems to bridge those two advancements and in the future may enable multi-robotic teams to be controlled by a high-level distributed planning system. in such scenarios, each robot would have its own planning representation of the world, thus reducing the domain and problem size and keeping the local information (i.e., sensory data) local. communication will clearly be an issue, which may encourage research of multiagent planning techniques aiming not primarily on planning speed, but on the communication requirements (this may for example discourage the use of global heuristic estimates). • orchestration of internet services: since internet services are computer programs already described in (formal) programming languages their coordination and orchestration can straightforwardly profit from multiagent planning techniques. moreover services are usually described by interfaces resembling planning actions with preconditions on the input data and effect on the data. therefore if such actions have to be ordered in a suitable fashion, beginning with initial constraints on the data and with a goal form of the data, planning is an appropriate fit. additionally, the services can be distributed over the internet and the data processing tasks can vary in the sense of particular areas of focus (e.g., financial processing, logistics services, etc.). both of these challenges are covered by the domain-independent multiagent planning. a single agent planning applications of this kind were already covered for example in [31]. • coalition planning: in recent years, many military operations involve coalitions. coalition operations are in nature cooperative, but some information cannot be disclosed among the coalition partners. this can be generally modeled by multiagent systems and in particular by multiagent planning. such a scenario is not applicable only in military, but may find uses also in business cooperation and other areas, although some more detailed privaci concerns may be necessary as illustrated in [22]. 4. challenges in the following, we will present some of the outstanding challenges of domain-independent multiagent planning we are aware of. 4.1. comparison of planners up to the present day, we know of about a half dozen domain-independent multiagent planners [12–17] and more are in the development. the biggest issue in order to compare them is that although the underlying formalisms are mostly similar, the actual language used as input differs (it is pddl with some ad-hoc definition of agents and/or public propositions). some consensus on this matter needs to be settled. similarly to the common definition language, a widely accepted set of benchmarks is needed. in the recent works, the benchmarks were typically created by ad-hoc converting some suitable ipc domains, where the agent decomposition is natural, such as logistics or rovers. only few new – multiagent specific – domains were introduced, i.e., cooperative pathfinding. in the future, it would be interesting to come up with more such domains, drawing from real world and multiagent systems applications and also designed to test some specific properties and pitfalls of multiagent planning. naturally, the best venue for such efforts would be a dedicated ipc track. the metrics used for planner comparison are also challenging. all metrics used to compare classical 54 vol. 2/2015 a case for domain-independent deterministic multiagent planning planners still apply, but there are some additional ones, such as number of exchanged messages or the amount of communicated data. further metrics can be adopted from the research of other multiagent algorithms. moreover, the comparison of multiagent planners gains a new complexity in that a single problem can be partitioned in multiple ways, and each partitioning may be beneficial for different planners. similarly, the amount of agent interaction significantly influences performance of the planners some algorithms may be better suited for loosely coupled problems while other for tightly coupled problems. this should be also reflected in the potential analysis. 4.2. which planning paradigm is the best? in classical sequential domain-independent planning, the dominating planning paradigm seems to be heuristic forward-chaining search typically utilizing one or more highly informative heuristic estimators (used by planners as fastforward, fastdownward, lama and many more), although some other approaches (such as bidirectional search) has performed well in the last ipc competition. it is not clear, whether the same holds for multiagent planning (and for all metrics). again, the only way to reliably answer this question is to perform a rigorous comparison of the planners, such as in the ipc competition. currently the most frequent approaches to multiagent planning are distributed heuristic search [14, 29, 30], partial order planning [16, 17], and various other, such as plan reuse [12] or generate-and-test [18, 19]. 4.3. heuristics one interesting area of research are the heuristic estimator for multiagent planning. as mentioned in the section about asynchronous computation, the baseline solution for heuristic computation is to use a projection of the problem to the particular agent’s propositions. this approach was used in [13, 14]. another approach is to attempt to compute (or at least approximate) the global value as if the problem was not partitioned in order to obtain better heuristic guidance. to our knowledge, the only heuristics treated this way so far were the ff heuristic in [29] and [30] and a domain transition graph based heuristic in [17]. of course, in some cases, the communication needed to compute a global heuristic may be prohibitive, in such a situation, the local heuristic would have to suffice, or a clever combination of both would need to be devised. different challenge is to come up with a heuristic specific to the multiagent planning. such heuristic may not only lead the search towards the goal, but may also lead the search in a way minimizing some multiagent metric, such as the communication load. 4.4. privacy multiagent planning can be seen also from the perspective of privacy-preserving distributed computing, although it is not the main concern of most of the ma-strips based planners. this perspective raises many questions, some of them were already addressed in [22, 32], but a comprehensive analysis of possible privacy violations in ma-strips and ma-strips based planning algorithms has not been yet presented. even the question if a ma-strips based multiagent planner can be privacy preserving (and if so how strongly) is yet to be answered. 4.5. extending complexity analysis from the theoretical perspective, the original [11]’s complexity results can give a solid groundwork for future and more detailed studies of complexity of multiagent planning. we envision two main directions: (i) problem-specific and (ii) finer complexity classes. the problem-specific study could be inspired by works as [33], where particular planning domains are analyzed from perspective of computational complexity showing which problems are easy, even if planning in general is known to be computationally hard. the idea of study of finer complexity classes, is for example parametrized analysis of classical planning by [34]. additionally, these studies can be extended by communication complexity showing how much communication would be required to solve the problems. 5. final remarks domain independent planning is a field of research bridging two distinct topics of multiagent systems and domain independent planning. we see providing a common problem definition language and set of benchmarks in order to be able to determine the state of the art and compare it with newly emerging techniques 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[34] c. bäckström, y. chen, p. jonsson, et al. the complexity of planning revisited a parameterized analysis. in aaai. 2012. 56 http://dx.doi.org/10.1609/aimag.v22i3.1581 http://dx.doi.org/10.1613/jair.1497 http://dx.doi.org/10.3233/mgs-2009-0133 http://dx.doi.org/10.1145/1838206.1838379 http://dx.doi.org/10.5220/0002702601280134 http://dx.doi.org/10.3233/978-1-61499-098-7-762 http://dx.doi.org/10.5220/0004918701780189 http://dx.doi.org/10.1007/s10489-014-0540-2 http://dx.doi.org/10.3233/978-1-61499-098-7-624 acta polytechnica ctu proceedings 2:51–56, 2015 1 introduction 2 ma-strips 3 is it any good? 3.1 improve scalability by decomposition 3.2 multi-core / cluster computing 3.3 privacy 3.4 asynchronous computation 3.5 applications 4 challenges 4.1 comparison of planners 4.2 which planning paradigm is the best? 4.3 heuristics 4.4 privacy 4.5 extending complexity analysis 5 final remarks references acta polytechnica ctu proceedings doi:10.14311/app.2017.8.0027 acta polytechnica ctu proceedings 8:27–29, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app the current view on the use of reconstruction materials in dentistry radka vrbovaa,∗, pavel bradnaa, martin bartosa, lucie himmlovaa, tomas horazdovskyb a institute of dental medicine, first faculty of medicine, charles university and general university hospital in prague, prague, czech republic b department of physics, faculty of mechanical engineering, czech technical university in prague, prague, czech republic ∗ corresponding author: vrbova@vus.cz abstract. the hardest tissue in the human body is the enamel which covers the anatomical crowns of teeth. it must be resistant to mechanical stress and the chemical attack of many substances from food, drinks and products of the metabolism of bacteria present in the oral cavity. these low ph substances dissolve the mineral components of enamel, cause tooth demineralization, and lead to decay or erosion damage with the irreversible loss of dental hard tissues and the necessity of their reconstruction. the range of dental materials intended for dental tissue reconstruction is extensive. dental amalgam can be mechanically applied into the strongly stressed lateral segments of teeth. the use of amalgam is, however, in decline, with the possible health risks attributed to it, coupled with the need to extensively prepare tooth tissue promoting a shift towards using aesthetically and biologically favourable dental ceramic and polymeric materials instead. current developments also concentrate on these materials to reinforce this, with polymeric composite materials based on methacrylates with varying amounts of inorganic fillers at the forefront. these materials are distinguished by their good mechanical and aesthetic properties and wear resistance. however, polymerization shrinkage and a strong hydrophobic nature does not allow for their direct bonding to hard dental tissues. risks associated with the release of residual free monomers from the structure to the environment, which may cause health complications, mainly allergic reactions in sensitive individuals, have been monitored recently. further development in the field of composite materials aims to reduce or completely eliminate these negatives. keywords: hard dental tissues, tooth decay, erosion, dental materials. 1. introduction teeth are specific formations in the oral cavity which are mainly composed from hard tissues such as enamel, dentine and cementum. enamel covers the surface of anatomical crowns and is the hardest tissue in the human body due to the high content of mineral substances. the so-called prismatic structure is typical for enamel, with closely spaced prisms bound with interprismatic substance (fig. 1a). enamel prisms with a diameter of 4-8 µms are formed predominantly from hydroxyapatite nanocrystals. the interprismatic mass also contains proteins, except hydroxyapatite, which serve as a binder for the individual prisms. dentine is mineralized less than enamel, is softer, and contains about 20-30 vol. % of proteins and 20-30 vol. % of water, and is biologically active compared to enamel. typical structural elements are known as dentinal tubules, canals in the dentine where extensions of the odontoblasts exist alongside dentinal fluid (fig. 1b). figure 1. a) prismatic structure of enamel after phosphoric acid etching (cross-section); b) the surface of dentin with dentinal tubules after phosphoric acid etching (cross-section). (sem, jsm5500-lv, jeol, tokyo, japan). figure 2. a) 3d model of the damaged tooth by caries from micro-ct (skyscan 1272, bruker, belgium); b) the longitudinal cross section of a tooth with tooth decay in the enamel and dentin (optical microscope olympus, smz 2mt, japan). 27 http://dx.doi.org/10.14311/app.2017.8.0027 http://ojs.cvut.cz/ojs/index.php/app r. vrbova, p. bradna, m. bartos et al. acta polytechnica ctu proceedings figure 3. the surface of enamel exposed to drinks for 12 hours: a) intact enamel; b) coca-cola, ph 2.5; c) fanta, ph 2.8; d) sprite ph 2.7. (sem, jsm5500-lv, jeol, tokyo, japan). 2. the typical damages of hard dental tissues 2.1. tooth decay due to the effect of products of the metabolic conversions of cariogenic bacteria present in dental plaque, there is a local demineralization in the subsurface layers of enamel. if the process reaches the dentineenamel border, it will break the surface layers of the enamel and will lead to the formation of a cavity (fig. 2a, b). 2.2. erosion in the case of dental tissue erosion, the demineralization is of non-bacterial origin. it results from the attack of substances with high acidity and simple sugars content. from this point of view, so-called "soft drinks" are very aggressive with a low ph, containing e.g. phosphoric acid or citric acid (fig. 3 b, c, d). they cause the dissolution of enamel mineral components; reduce its surface hardness and resistance to abrasion or mechanical stress. the result of the above-mentioned conditions may be the loss of dental hard tissues with the necessity of their reconstruction, which is often complicated and costly. additionally, the lifetimes of reconstructions are always limited. 3. polymeric materials for the reconstruction of hard dental tissues the range of dental materials intended for the reconstruction of lost or damaged dental tissues, whether as a result of carious processes, extensive erosions or traumatic damages is very broad. the most frequently used are composites, whose matrix consists mainly of methacrylate polymers (e.g. bis-gma, tegdma, udma, bis-ema) and the fillers are ba, sr, zr ground glass with surfaces treated by silane coupling agents and amorphous sio2 added primarily for adjusting the thixotropic properties of materials and pigments. these are mainly light-cured materials containing photoinitiators of polymerization reaction, usually camphorquinone (2,3-bornandion), propanedione (1phenyl-1,2-propanedione) or lucirin tpo (biphenyl (2,4,6-trimetylbenzoyl-diphenylphosphine oxide), often in conjunction with tertiary amine co-initiators. figure 4. a) the adhesive material leaking into the dentinal tubules; b) damaged marginal seal between the filling material and enamel. (sem, jsm5500-lv, jeol, tokyo, japan). they must also contain inhibitors of the polymerization reaction. the hardening of materials occurs by radical polymerisation, when molecules of photoinitiators absorb photons of light from curing lamps forming free radicals, which initiate very fast polymerization reactions. mainly halogen or led curing lamps emitting light in the wavelength range 400 to 515 nms are currently used for curing of materials. it is very important that the spectrum of emitted light from the curing light must overlap the absorption spectrum of the photoinitiator present in material to ensure the best possible polymerization [1, 2]. composite materials are characterized by very good mechanical and aesthetic properties, and are indicated for lateral and front sections of the dental arches. however, these materials are hydrophobic and do not adhere to tooth structure comprising water. therefore, quality micromechanical binding provides adhesive systems that flow into the previously etched microrelief of dental tissue (fig. 4a). adhesive systems include hydrophilic monomers with the ability to wet moist surfaces and bond them with hydrophobic monomers which are chemically combined with a composite material after polymerization. the main disadvantage of these materials is their shrinkage due to polymerization. this may cause damage to the marginal seal, i.e. loss of contact between the dental tissue and the filling material (fig. 4b). the polymer materials also show a possible risk of residual free monomers releasing into the surrounding environment, which may give rise to health problems in susceptible individuals, especially to allergic reactions [3–6]. 28 vol. 8/2017 the current view on the use of reconstruction materials in dentistry 4. conclusion further development of polymer composites is driven by efforts to improve their mechanical and aesthetic properties, increase wear resistance, reduce polymerization shrinkage and achieve significant improvements in biocompatibility. acknowledgements this work was supported by grant prvouk p28/lf1/6 mšmt. references [1] p. bradna, l. comba, j. froněk, d. houšová. kam směřuje vývoj polymeračních lamp? česká stomatologie 110(3):61–68, 2010. [2] j. froněk. studium vlivu vlastností polymeračních lamp na vytvrzení kompozitních materiálů s různými fotoiniciačními systémy. master’s thesis. [3] m. syed, r. chopra, v. sachdev. allergic reactions to dental materials-a systematic review. journal of clinical and diagnostic research 9(10):ze04 – ze09, 2015. doi:10.7860/jcdr/2015/15640.6589. [4] i. stoeva, a. kisselova, m. zekova. allergic contact stomatitid from bisphenol-a-glycidyldimethacrylate during application of composite restorations. a case report. journal of imab annual proceeding (scientific papers) pp. 45 – 46, 2008. book 2. [5] s. gupta, p. saxena, v. pant, a. pant. release and toxicity of dental resin composite. toxicology international 19(3):225–234, 2012. doi:10.4103/0971-6580.103652. [6] m. goldberg. in vitro and in vivo studies on the toxicity of dental resin components: a review. clinical oral investigations 12(1):1–8, 2008. doi:10.1007/s00784-007-0162-8. 29 http://dx.doi.org/10.7860/jcdr/2015/15640.6589 http://dx.doi.org/10.4103/0971-6580.103652 http://dx.doi.org/10.1007/s00784-007-0162-8 acta polytechnica ctu proceedings 8:27–29, 2017 1 introduction 2 the typical damages of hard dental tissues 2.1 tooth decay 2.2 erosion 3 polymeric materials for the reconstruction of hard dental tissues 4 conclusion acknowledgements references 210 acta polytechnica ctu proceedings 1(1): 210–214, 2014 210 doi: 10.14311/app.2014.01.0210 electron acceleration in supernovae and millimeter perspectives keiichi maeda1,2 1department of astronomy, kyoto university, japan 2kavli institute for the physics and mathematics of the universe (wpi), university of tokyo, japan corresponding author: keiichi.maeda@kusastro.kyoto-u.ac.jp abstract supernovae launch a strong shock wave by the interaction of the expanding ejecta and surrounding circumstellar matter (csm). at the shock, electrons are accelerated to relativistic speed, creating observed synchrotron emissions in radio wavelengths. in this paper, i suggest that sne (i.e., ∼< 1 year since the explosion) provide a unique site to study the electron acceleration mechanism. i argue that the efficiency of the acceleration at the young sn shock is much lower than conventionally assumed, and that the electrons emitting in the cm wavelengths are not fully in the diffusive shock acceleration (dsa) regime. thus radio emissions from young sne record information on the yet-unresolved ‘injection’ mechanism. i also present perspectives of millimeter (mm) observations of sne – this will provide opportunities to uniquely determine the shock physics and the acceleration efficiency, to test the non-linear dsa mechanism and provide a characteristic electron energy scale with which the dsa start dominating the electron acceleration. keywords: acceleration of particles radiation mechanism: non-thermal supernovae: general. 1 introduction the most promising particle acceleration mechanisms require a strong shock wave, e.g., by the diffusive shock acceleration (dsa) mechanism where the particles acquire energy through repeated collisions between upand down-streams of a shock wave (fermi, 1949; blandford & ostriker, 1978; bell, 1978). supernova remnants (snrs) are believed to be the origin of cosmic rays at least up to ∼ 1015ev (e.g., bamba et al., 2003). there is one key issue in this picture for electrons – how the electrons are ‘pre-accelerated’. for the dsa mechanism to work efficiently, a particle must already have an enough kinetic energy. supernovae (sne), at the age of ∼< 1 year, also produce emissions which are believed to be originated by relativistic electrons, accelerated at a strong shock created by the expanding sn ejecta running into circumstellar matter (csm). radio emissions from sne are interpreted as the synchrotron emission, and x-rays from some sne have been suggested to be emitted through the inverse compton (ic) mechanism (e.g., chevalier & fransson, 2006 for a review). however, most of analyses on the non-thermal emissions from sne have been focusing on deriving the csm environment, rather than the acceleration mechanism (e.g., soderberg et al., 2012). in this paper, i argue that young sne provide a unique site to study the electron acceleration mechanism. i also suggest that millimeter (mm) observations, which are becoming feasible with new observatories like alma, can potentially provide essential information on this issue. 2 non-thermal emissions a situation around young sne related to the nonthermal emission is similar to that for snrs. energy transfer from the shock wave kinetic energy to relativistic particles and that to magnetic field are roughly described by equipartition (fransson et al., 1996). i adopt conventional notation – εe and εb describe constant fractions of the shock wave energy transferred to the relativistic electrons and the magnetic field, respectively. our arguments are based on modeling emissions from so-called striped envelope sne (se-sne; or sne iib/ib/ic) that are believed to be explosions of he or co stars (having lost at least the h envelope). in these sne, the radio emission is well described by synchrotron emissions with the synchrotron self-absorption (ssa) at low frequencies (see, e.g., chevalier & fransson, 2006). under some standard assumptions (björnsson & fransson, 2004; chevalier & fransson, 2006; maeda et al. 2012, 2013a), the synchrotron properties can be described by the following parameters: • p: power law index of spectral energy distribution of injected relativistic electrons. • m: power law index of shock evolution in time (r ∝ tm). 210 http://dx.doi.org/10.14311/app.2014.01.0210 electron acceleration in supernovae and millimeter perspectives table 1: characteristics of the synchrotron emission from young sne (lν ∝ ναtβ), for the adiabatic limit and for the synchrotron and ic cooling limits, respectively (maeda, 2013a). indices adiabatic syn. ic α 1−p 2 −p2 −p2 β (3m− 3) + 1−p 2 (3m− 3) + 2−p 2 (5m− 5) + 2−p 2 + δ α(p = 2) − 1 2 −1 −1 β(p = 2) (3m− 3)− 1 2 (3m− 3) (5m− 5) + δ α(p = 3) −1 − 3 2 − 3 2 β(p = 3) (3m− 3)− 1 (3m− 3)− 1 2 (5m− 5)− 1 2 + δ • δ: power law index of optical/nir sn emission in time (l ∝ tδ). • a∗: csm density scale (ρcsm ∝ a∗r −2; normalized as a∗ ∼ 1 for ṁ ∼ 10−5m�yr−1 with the mass loss wind velocity of 1, 000 km s−1). • εe: efficiency of the electron acceleration. • εb : efficiency of the magnetic field generation/amplification. note that the shock evolution (m) is mainly determined by the csm density distribution, e.g., by a self-similar solution (chevalier, 1982). table 1 shows expected synchrotron properties, lν ∝ ναtβ . from the observed properties (α, β) one can almost uniquely determine the power law indices (p, m, δ). there is a degeneracy in the other parameters (i.e., in the ‘scales’). properties of the ssa-synchrotron are described by two characteristic observables (peak date and luminosity), while these are described by the three model parameters (i.e., a∗, εe, εb). 3 efficiency of electron acceleration figure 1 shows how one can constrain the shock microphysics and csm density. an example is given for intensively observed nearby sn iib 2011dh. thanks to detailed models of the optical emission (bersten et al., 2012), the sn ejecta properties (mass and energy) have been strongly constrained – model a adopts the shock wave dynamics expected from the optical emission model. model b is shown for illustration, which assumes the dynamics so that εe ∼ 0.1, but this fails to explain the optical behavior. adopting model a, εe cannot be as large as ∼ 0.1 which has been conventionally assumed, since such a situation requires extremely large mass loss rate (a∗). then the expected thermal emission in x-rays would be much stronger than observed. indeed, from the x-ray strength, a∗ ∼< 30, thus εe ∼< 0.01 must apply. also, from the energy conservation, a∗ ∼< 2 is rejected (otherwise εb > 0.3). from these arguments, 0.005 ∼< εe ∼< 0.01 and εb ∼> 0.001 are obtained as robust constraints. this also indicates that α ≡ εe/εb < 10. 0.1 1 10 1e-3 0.01 0.1 model b model a b e e figure 1: εe and εb derived for sn 2011dh, as a function of a∗ (maeda, 2012). so, a strong constraint can be placed on εe. there is another independent argument against a large value of εe. figure 2 shows the models with small εe and large εe. large εe should produce a detectable cooling effect in radio properties, which was however not detected. this argument on the ic cooling effect should apply to sne in general. i note that sometimes a large value of εe is introduced/suggested to explain x-ray luminosities by ic up-scattered photons (e.g., chevalier & fransson, 2006), but indeed i suggest here that one has to check if such a situation is consistent with the radio (cm) properties. for example, for sn 2011dh α ∼> 30 (e.g., εe ∼< 0.3 and εb ∼ 0.01) has been suggested (e.g., soderberg et al., 2012), but as shown above this should produce a detectable change in the radio light curves that was not observed (maeda, 2012). applying the same constraint to a few other sne, it seems like that small εe is a generic feature in sne (maeda, 2013a). 211 keiichi maeda 10 100 0.1 1 10 (e) 25.0 ghz 10 100 0.1 1 10 (f) 36.0 ghz 10 100 0.1 1 10 (d) 16.0 ghz 10 100 0.1 1 10 (c) 8.4 ghz 10 100 0.1 1 10 (b) 4.9 ghz fl ux d en si ty (m jy ) day 10 100 0.1 1 10 (a) 1.4 ghz 10 100 0.1 1 10 (f) 36.0 ghz 10 100 0.1 1 10 (e) 25.0 ghz 10 100 0.1 1 10 (d) 16.0 ghz 10 100 0.1 1 10 (c) 8.4 ghz 10 100 0.1 1 10 (b) 4.9 ghz 10 100 0.1 1 10 (a) 1.4 ghz fl ux d en si ty (m jy ) figure 2: left: multi frequency radio light curves (red solid) as compared with those of sn 2011dh (maeda, 2012). the parameters are (a∗, εe, εb) = (4, 6×10−3, 5×10−2) (left; adopting model a) and (20, 0.26, 2.5×10−4) (right; model b). the synthetic light curves without the ic cooling are also shown (blue dashed). observational data are taken from soderberg et al. (2012). 4 injection and acceleration mechanisms since one can obtain both the spectral and temporal information for sne, there is essentially no degeneracy in deriving the electrons’ injected spectrum slope, p (tab. 1). one interesting issue is found from such analyses – p ∼ 3 is generally derived for young sne, unlike more evolved snrs (mostly p ∼ 2 − 2.4; e.g., bamba et al., 2003) and the standard dsa prediction in the test particle limit (p ∼ 2; e.g., ellison et al., 2000). a cause of the difference has not been clarified, and i propose that this is mainly due to totally different energies of the electrons emitting at cm wavelengths in young sne and more evolved snrs. the argument here is based on that of maeda (2013b). i note that a main difference between the synchrotron emission from sne and that from snrs is that the emitting electrons’ energy is quite different for given frequency (figure 3). typical magnetic field strength is b ∼ 1g for sne (e.g., chevalier & fransson, 2006) and 100µg for snrs (e.g., bamba, et al., 2003). this is consistent with the equipartition expectation (maeda, 2013b). at the observed frequency of ∼ 1 ghz, the emitting electrons’ energies are ∼ 50 mev and 5 gev in sne and snrs, respectively. one can estimate if these electrons satisfy an essential condition required for dsa, namely the electron’s mean free path is exceeding the shock wave width. this is satisfied by electrons with the energy ∼> 100 mev in sne and 10 mev in snrs. thus i suggest that the electrons emitting at ghz frequency are likely in the efficient dsa limit in snrs, while they cannot be efficiently accelerated by dsa in sne. 100 101 102 103 104 105 0.1 1 10 100 1000 dsa (sn) dsa (snr) alma vla /g h z figure 3: the relation between the electron’s energy and the synchrotron frequency, for b ∼ 1g typical of young sne (red-thick-solid) and ∼ 100µg typical of snrs (black-thin-solid). also shown is the minimum electron energy for the efficient dsa, adopting v ∼ 0.1c (sne; red-thick-dashed) and 0.01c (snrs; black-thindashed). the typical frequency coverage is shown by the shaded areas, for cm (‘vla’) and mm (‘alma’) observations . a unified scenario is proposed here – the steep energy spectrum of the electrons derived for young sne reflects the inefficient dsa acceleration, or in other word, the ‘injection’ spectrum. this scenario makes young sne interesting objects in studying the electron injec212 electron acceleration in supernovae and millimeter perspectives tion and acceleration mechanism, as one could directly probe the electron injection mechanism. 5 perspectives for mm observations i propose that observations of nearby young sne at mm wavelengths can potentially provide major advances in the issues discussed in this paper (see maeda, 2013b for details). on the acceleration efficiency, the ic cooling effect is more important at higher frequencies, and thus at mm wavelengths one should be able to see this effect to determine εe, or at least place much stronger upper limit than at cm wavelengths. alternatively, if εe is very small, then the synchrotron cooling becomes important, and the cooling frequency would enter into the mm wavelength. if it happens, it will provide direct estimate of b. in either case, there is a good chance to obtain additional information, and then we can solve the degeneracy between the shock physics and the csm environment (§2). another suggestion is on the electron injection. if the scenario suggested in §4 is correct, we should see the spectral flattening at high frequencies. this flattening could take place already at ∼ 100 mev (§4), then one should be able to detect this signature at mm wavelengths (fig. 3). if such a change in the electrons’ energy spectral slope is detected, this could provide direct evidence of the non-liner acceleration theory where the particles’ spectral slope is expected to become harder for higher energies (e.g., ellison et al., 2004). the energy scale for the possible transition will provide strong constraints on the acceleration theory. for nearby objects (up to ∼ 25mpc), such a signature should be detectable by alma (maeda, 2013b). 6 conclusions in this paper, i have suggested to study electron acceleration mechanisms at a strong shock wave by radio observations of nearby young sne. especially, several ideas have been presented regarding (1) the acceleration efficiency and (2) injection problem and non-linear acceleration toward the efficient dsa. the ideas include (a) to constrain the efficiency by combining radio and optical data, (b) to place an independent constraint on the efficiency by the ic cooling effect, and (c) to probe propertis of ‘injected’ electrons before entering into the efficient dsa regime. i also propose that these issues can be further advanced by mm observations. such observations are being planned – we have our too proposal of nearby sn follow-up observations by alma among the highest priority proposals in alma cycle 1, which is currently active (until early 2014). acknowledgement km thank franco giovannelli and the organizers of frascati workshop 2013 for creating the friendly and stimulating atmosphere. the work by km has been supported by wpi initiative, mext, japan, and by a grant-in-aid for scientific research for young scientists (23740141). references [1] bamba, a., et al.: 2003, apj, 589, 827 doi:10.1086/374687 [2] bell, a.r.: 1978, mnras, 182, 147 [3] bersten, m.c., et al.: 2012, apj, 757, 31 doi:10.1088/0004-637x/757/1/31 [4] blandford, r.d., ostriker, j.p.: 1978, apj, 221, l29 doi:10.1086/182658 [5] björnsson, c.-i., fransson. c.: 2004, apj, 605, 823 [6] chevalier, r.a.: 1982, apj, 258, 790 [7] chavalier, r.a., fransson, c.: 2006, apj, 651, 381 doi:10.1086/507606 [8] ellion, d.c., berezhko, e.g., baring, m.g.: 2000, apj, 540, 292 doi:10.1086/309324 [9] fermi, e.: 1949, phys. rev. 75, 1169 doi:10.1103/physrev.75.1169 [10] fransson, c., lundqvist, p., chevalier, r.a.: 1996, apj, 461, 993 doi:10.1086/177119 [11] maeda, k.: 2012, apj, 758, 81 [12] maeda, k.: 2013a, apj, 762, 14 [13] maeda, k.: 2013b, apj, 762, l24 [14] soderberg, a.m., et al.: 2012, apj, 752, 78 doi:10.1088/0004-637x/752/2/78 discussion sergio colafrancesco: ic losses are dominant w.r.t. synchrotron loses if the b-field is low. how this can match with the expectation that the ic losses are important in high b-field regions in snrs? what is a role of coulomb heating effects? keiichi maeda: on the ic cooling, i believe that we expect that in general the relative importance of the ic cooling is higher for lower b-field. note that i am 213 http://dx.doi.org/10.1086/374687 http://dx.doi.org/10.1088/0004-637x/757/1/31 http://dx.doi.org/10.1086/182658 http://dx.doi.org/10.1086/507606 http://dx.doi.org/10.1086/309324 http://dx.doi.org/10.1103/physrev.75.1169 http://dx.doi.org/10.1086/177119 http://dx.doi.org/10.1088/0004-637x/752/2/78 keiichi maeda talking about cooling, not heating/emission. here, the ic cooling rate is lic ∝ uphγ 2 and the synchrotron cooling rate is lsyn ∝ ubγ 2. then, for given observed frequency ν, if one increases b then one should decrease γ (to emit at ν), leading to lower lic. in this situation, lsyn can be large b/o the ub term. on the coulomb heating. so far i have been focusing on sne iib/ib/ic, which are believed to have relatively low density csm. i estimated the coulomb effect, and at ghz or higher frequencies, the coulomb heating is estimated to be negligible. 214 introduction non-thermal emissions efficiency of electron acceleration injection and acceleration mechanisms perspectives for mm observations conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.13.0055 acta polytechnica ctu proceedings 13:55–60, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app micro-mechanical performance of concrete used as recycled raw material in cementitious composite vladimír hrbeka,b,∗, veronika koudelkováa,b, zdeněk prošeka,c, pavel tesáreka a czech technical university in prague, faculty of civil engineering, thákurova 7, 166 29 prague 6, czech republic b institute of theoretical and applied mechanics as cr, v.v.i., prosecká 76, 190 00 prague 9, czech republic c university centre for energy efficient buildings of czech technical university in prague, třinecká 1024, 273 43 buštěhrad, czech republic ∗ corresponding author: vladimir.hrbek@fsv.cvut.cz abstract. the reduction of industrial pollution is recently one of main goals over all fields. in civil engineering, re-cycling of structural waste provides wide opportunity contributing this effort. this paper focus on re-use of concrete waste, which after further processing can be used in new constructions as partial supplement to the mixture. to investigate the impact of re-cycled concrete addition, it is necessary to determine mechanical and structural parameters of individual phases in the “raw” material. for this purpose, grid indentation and scanning electron microscopy with energy-dispersive x-ray spectroscopy (sem, edx) are combined to determine properties of concrete sample. keywords: re-cycled concrete, grid indentation, sem, edx, image analysis. 1. introduction the waste material accumulation became worldwide environmental and economical problem. development of new effective and thrifty methods for re-use of waste products lowers the number of waste deposits while saving natural sources and environment. for example, in 2012, the countries of european union produced over 2.5 billion tones of waste and managed to recycle barely 10% of this amount. in case of czech republic, over 23million tones of waste were produced and slightly over one-fifth recycled (statistics according to environmental data center on waste). one of main problems with incorporation of waste materials in civil engineering (especially in constructions) is mistrust of designers and developers toward recycled construction waste. despite lower price of these materials (compare to traditional raw materials), final cost can be paradoxically higher due to the transportation [1–3]. the solid phase of concrete is made of coarse and fine aggregate (65 to 70%) and cement paste. typically, when recycled, coarse aggregate (30 to 50% of raw material) is to be reused, which leaves majority of the concrete as secondary waste product [4]. complete recycling of concrete (concretely use of highspeed milling) can turn this waste into fine powder (fraction < 1mm) with potential usage as micro-filler (fine ground hydration products and fine aggregate) and partial cement substitute (non-hydrated clinker in cement paste). nevertheless, the processing itself is complicated and bears addition financial costs. beyond that, due to the lack of studies and short experience of civil engineering practice with such fine powdered material, the implementation of recycled secondary waste material is not possible on large scale. m. chen et al. [5] used the recycled concrete fine powder in their study as full substitute of pulverized limestone in asphalt mixture. the results of x-ray diffraction and scanning electron microscopy (sem) showed higher content of sio2, lower caco3 content and rougher partical surface in recycled concrete fine powder, compare to of pulverized limestone. when used as filler in asphalt mixture, the water sensitivity of samples reduced while mechanical properties in high temperatures and fatigue persistence increased. however, mechanical properties in low temperature slightly decreased. in case of cement based mixtures, recycled concrete fine powder serves much as a micro-filler, which acts as coarse aggregate on the mezoand micro-scale of the material. unfortunately, studies about recycled micro-fillers are not yet carried out, although the idea seems promising as replacement of current microfilling agents [6]. moreover, the potential of nonhydrated clinker present in the powder was so far vastly ignored. y. j. kim et al. [7] presented in his study features of cement paste modified by recycled concrete fine powder as a partial replacement for a binder. according to the results, workability in mixture’s fresh state decreased with increasing level of cement compensation and the hydration process was delayed up to 2 hours. in case where 45% of cement was replaced by recycled concrete fine powder, the mechanical com55 http://dx.doi.org/10.14311/app.2017.13.0055 http://ojs.cvut.cz/ojs/index.php/app v. hrbek, v. koudelková, z. prošek, p. tesárek acta polytechnica ctu proceedings pressive strength reduced to 30% while absorptivity gain reached almost 70%. the conclusion of this study proposed limitation of the replacement to 15%. m. lidmila a k. šeps [8–10] used in their studies pulverized concrete recycled from railway sleepers. the product of recycling showed low reactive potential very likely due to very fine milling of the concrete, i.e. unfolding of non-hydrated clinkers. as the level of non-hydrated clinker is low, the material is to be possibly used for strengthening of subsoil under railway structures [11]. other potential utilization, in small-scale, can be found in cementitous composite material. the knowledge of the material on the micro-scale is thus crucial to understand the composite’s behavior on higher scale levels. with such level of investigation, it is possible to develop up-scaled prediction of macro-mechanical properties, as well as optimize the efficiency of used fine powdered concrete recycle product. this study is focused on investigation of micro-mechanical and micro-structural performance of the in-put “raw” material, i.e. concrete sleepers intended for recycle. the output would serve as comparative analysis to further planed research of the recycled pulverized concrete. 2. material on of raw materials used for the recycled pulverized concrete are railway sleepers type pb2 and sb8 (used in this study, fig. 1a). it the first step of the recycling process, crude recycled concrete gravel with dimension 0–32mm (fig. 1b) arises from the kibble of the sleepers and the metallic parts and reinforcement is separated. after selection of finer concrete gravel (fraction 0–16mm, fig. 1c), the material is milled in two steps to the final product (recycled pulverized concrete, fraction 0–1mm). the fine milling of the material was delivered by company lavaris ltd. (procedure protected by patents act) using the high speed milling technique. for a purpose of the investigation, piece of crude concrete gravel (fig. 1b) was embedded in epoxy resin and let to harden for approx. 24 hours. a part of the specimen was than severed (approx. thickness 15mm) and silica-carbon papers and diamond suspensions were used for grinding and polishing of the specimen surface. this technique ensured adequate surface roughness of the sample for both indentation and sem investigation. the coordination mark was inscribe on the polished surface, serving as origin for further orientation. this enabled positioning of both investigation techniques in the very like area of the sample. 3. investigation procedure the investigation of the crude recycled concrete consisted of three main techniques, instrumental indentation, scanning electron microscopy combined with (a) . railway sleepers, type pb8. (b) . crude recycled concrete (0 32mm) (c) . “raw” recycled concrete (0 16mm) figure 1. products of concrete recycling procedure. electron probe microanalysis (sem epma) and back scattered electron micrographs (sem bse) image processing. as a result, combination of micromechanical properties, phases chemical composition and material structure enabled proper description of the material. 3.1. scanning electron microscopy the scanning electron microscopy (sem) investigation was performed in mira ii lmu (tescan corp., brno) on polished specimens coated with thin layer of carbon necessary to ensure proper conductivity of the surface. working distance of the microscope was set closely to 15 mm and accelerating voltage was set to 15 kv – to provide good signal. chemical composition (in weight percentage) of each phase characterized by the same level of grey scale was determined using epma based on the detection of the x-rays by energy dispersive x-ray detector (edx, bruker corp., berlin) on several point of each position. due to the time-demands of technique such as phase determination by epma, image analysis of sem bse micrographs was used to obtain phase volumetric representations in viewed field, i.e. material structure. the micrographs were acquired at different magnifications. the approximate area of indentation was investigated at first at the magnification 600× to gain adequate overview. than the area was scanned with higher magnification (above 1200×) for detailed study of indented positions in several images. the sem micrographs acquired with back scattered electron detector (bse) provide information about distribution (and chemical composition) of different phases due to different spectrum of the back scattering coefficient. 56 vol. 13/2017 re-cycled concrete 3.2. quasi-static nano-indentation the technique of nano-indentation (ti 7500 series, hysitron inc.) was selected for evaluation of microscale elastic properties of the material. its principal is based on dependency of probe propagation with respect to the recorded force. the force-displacement record is further further processed and the mechanical properties are calculated from the unloading part of the record. incorporated errors of the measurement, such as creep and visco-elasticity of measured phases, is avoided by appropriate test setup [12–18]. for purpose of this study, the load function kept for further described indentation similar, i.e. the “loading” and “unloading” segments lasted 5 seconds each with an in-between 60 seconds “holding” time segment. the measurement was performed in two major steps (level i and ii) to achieve efficient investigation of phases on different material levels. as an early step, a load-controlled quasi-static grid indentation was performed with an applied force of 10mn (almost maximum capacity of the transducer) to obtain route-identification of the material. the indents were each separated by 25 µm in 10 by 10 raster, which allowed both micro-mechanical evaluation of phases in large range and estimation of further used indentation depth. however, such setting does not meet the grid-indentation specifications of heterogeneous composite [19–22], particularly does not guarantee consistent half-space influenced by each indent. the first step (level i) was thus selected as displacement-driven quasi-static grid measurement with each indent driven into 150 nm depth in two positions. the grid was constructed of 21 by 21 indents pattern with 5µm spacing. the setting ensured equal indented half-space volume of material represented on the sample surface by circle with 6×indentation depth diameter [19]. the indentation covered space over the total investigated area (given by the grid dimensions 100 by 100 µm) was computed equal to 2.81% (ratio of efficiency). the second step (also displacement-driven with identical indentation depth level ii) was therefore designed for detailed investigation of selected position. the grid consisted of 25 by 25 indents separated by 2 µm and the efficiency equaled to 17.26%. the setting (especially location and size of the position) aimed for close evaluation of phases present in cement paste. 4. results interpretation the sem epma edx analysis of 41 material positions showed five main phases present in the investigated material, i.e. low-density and high-density calcium-silica-hydrate (ld c-s-h and hd c-s-h), calcium hydroxide (ch), non-hydrated clinker and aggregate – potassium and sodium feldspar and quartz (fig. 2). the phases average weight percentage of each element are summarized in tab. 1. moreover, 1.25mm by 1.25mm area, where level i indentation positions are expected, was sequentially figure 2. micrographs with identified material phases. scanned in bse mode with high resolution (5×5 sequence of 250µm wide images). the reconstruction of this area enabled exact linkage between indentation data material structure. the histograms of nano-indentation results, the indentation modulus in particular, were normalized in respect to the 0.1 of minimum value, as captured for all studied levels in fig. 3. the preliminary study of the material (fig. 3a) proved to insufficiently detail mechanical properties of all phases. (a) . reduced modulus histogram – preliminary study. (b) . reduced modulus histogram – level i. (c) . reduced modulus histogram – level ii. figure 3. histograms of indentation modulus this can be observed in comparison with level i 57 v. hrbek, v. koudelková, z. prošek, p. tesárek acta polytechnica ctu proceedings element quartz potassium sodium ld c-s-h hd c-s-h ch clinker feldspar feldspar ca 6.65 37.37 45.37 60.05 50.18 si 46.74 29.39 27.24 6.41 12.83 0.35 12.42 al 10.09 11.06 1.42 1.33 0.50 mg 0.35 0.71 0.32 0.40 na 0.87 8.09 0.11 0.24 k 14.01 0.52 0.33 0.35 0.52 s 2.24 0.81 0.16 cl 0.36 fe 1.21 1.05 1.13 0.48 o 53.26 45.63 46.45 50.56 36.95 37.99 35.50 table 1. average weight percentage of elements present in phases. of the study (fig. 3b). the results, in this case, are more likely to depict the material structure as the occurrence of reduced modulus around 40gpa is most frequent (see [23–26]). also, several peaks corresponding to number of phases identified by sem analysis can be found in the histogram. the level ii of the material was focused mostly on the investigation of cement paste, especially on csh and ch phase. again, fig. 3c confirms predominant representation of high-density calcium-silica-hydrate in the matrix. the overall results (fig. 4), as combination of both measured levels, gives detailed view of micromechanical performance of the material. the probability density function of measured indentation moduli was subsequently processed with spectral deconvolution in order to obtain gaussian distribution of expected phases. the mechanical properties of phases 1-5 in fig. 4 were thus determined as: phase 1= 19.17 ± 3.54gpa = ld c-s-h phase 2= 39.75 ± 5.98gpa = hd c-s-h phase 3= 58.59 ± 6.34gpa = calcium hydroxide phase 4= 79.78 ± 3.11gpa = presumably aggregate phase 5= 118.35 ± 16.85gpa = clinker figure 4. histogram of overall reduced modulus results. the results are consistent with previously published researches [23–32]. based on these results, maps of indentation moduli over the investigated positions (fig. 5 –6) were constructed with bordering conditions figure 5. contour map of preliminary results. figure 6. contour map of results on level ii. identical to limits in fig. 4. in addition, it was possible to link maps of indentation data to particular segments of sem bse micrographs (fig. 7). 58 vol. 13/2017 re-cycled concrete figure 7. contour maps of level i results linked to the sem bse micrograph. 5. conclusion the raw material (railway sleeper pb8) used after milling as recycled pulverized concrete in cementitious composites was in focus of this study. the micromechanical properties and material structure of this base material were investigated with combined methodology to predict performance when used as filler and cement replacement. the scanning electron microscopy methods (sem epma edx, bse) were used to determine chemical and structural composition of the material (unknown prior to the investigation). therefore, lowand high-density calcium-silica-hydrate (ld / hd c-s-h), calcium hydroxide (ch), three aggregate types and non-hydrated clinker were identified as main material phases. the nanoindentation technique over two main material levels enabled evaluation of the indentation modulus of these phases due to the spectral deconvolution of measured data. reverse reconstruction of indented areas with respect to deconvolution results let to interlink of indentation and bse diagrams. although the combined investigation provided sufficient results, more detail should be obtained in case of aggregate phases prior to modeling of the material. list of symbols f applied force [µn] hi indentation depth [nm] er reduced modulus [gpa] h hardness [gpa] hc contact depth [nm] acknowledgements the research is financially supported by czech technical university in prague – project sgs17/168/ohk1/3t/11 and by the czech science foundation research project 17-06771s. the support is gratefully appreciated. references [1] m. stibůrek. možnosti využití stavebních odpadů. beton tks 2:45–47, 2008. 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http://dx.doi.org/https://doi.org/10.1016/j.eml.2016.03.002 http://dx.doi.org/https://doi.org/10.1016/s0008-8846(03)00039-5 http://dx.doi.org/https://doi.org/10.1016/j.matchar.2007.05.018 http://dx.doi.org/https://doi.org/10.1016/j.cemconres.2008.09.002 http://dx.doi.org/https://doi.org/10.1016/j.cemconres.2010.09.001 http://dx.doi.org/https://doi.org/10.1007/s11340-010-9373-z http://dx.doi.org/https://doi.org/10.1016/s0008-8846(00)00505-6 acta polytechnica ctu proceedings 13:56–61, 2017 1 introduction 2 material 3 investigation procedure 3.1 scanning electron microscopy 3.2 quasi-static nano-indentation 4 results interpretation 5 conclusion list of symbols acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.12.0005 acta polytechnica ctu proceedings 12:5–9, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app model car transport system – modern its education tool karel bouchner∗, alina mashko department of vehicles, ctu in prague, horská 3, praha 2, 120 00, czech republic ∗ corresponding author: bouchkar@fd.cvut.cz abstract. the model car transport system is a laboratory intended for a practical development in the area of the motor traffic. it is also an important education tool for students’ hands-on training, enabling students to test the results of their own studies. the main part of the model car transportation network is a model in a ratio 1:87 (ho), based on component units of faller car system, e.g. cars, traffic lights, carriage way, parking spaces, stop sections, branch-off junctions, sensors and control sections. the model enables to simulate real traffic situations. it includes a motor traffic in a city, in a small village, on a carriageway between a city and a village including a railway crossing. the traffic infrastructure includes different kinds of intersections, such as t-junctions, a classic four-way crossroad and four-way traffic circle, with and without traffic lights control. another important part of the model is a segment of a highway which includes an elevated crossing with highway approaches and exits. keywords: model car transportation system (model), motor traffic, intelligent transport system (its), smart city. 1. introduction with a constant growth of people mobility, expansion of cities infrastructure, increase in traffic flow, traffic density in the cities, the efficient traffic management systems are rather crucial. telematic systems are being used for traffic monitoring and control. the road traffic is affected by a number of parameters such as weather conditions, infrastructure, human behavior, technical state of a vehicle etc. telematic systems are used in city planning, transport management, parking solutions, operation of logistics and municipal services, organization of urban space, implementation of sustainable energy sources. it can as well as be comprised under an umbrella term, the smart city initiative, and it is approached from the view of different disciplines including technical, economic, humanitarian, legal etc. [1]. traffic modeling is important in the process of traffic systems implementation. the preliminary system simulation and testing in laboratory conditions with implementation of real traffic data is safe and provides feasible results that can be used for timely corrections and improvement in traffic management schemes. there are many advantages of performing traffic studies in safe laboratory conditions. these include possibility of simulating the enforcement of services work in emergency situations, simulating dangerous human behavior in traffic with a high density, dangerous road sections or on high-speed roads, planning safer routes for dangerous goods transportation, efficient city traffic planning including city municipal transport, parking areas, better overview of city safety in general etc. rather crucial for smart city technologies is testing newly developed telematic systems on real traffic data which can be realized within the suggested model[2, 3]. the smart city solutions are to take into account the existing city architecture while dealing with efficient energy flows[4]. the mathematical (or general) models of such complex systems provided with the use of tools of virtual reality to the users are nowadays very popular and widely applied. however, the real interpretation of the models is still for many people straightforward for understanding and working with. the real models are not only convenient for demonstration and illustration purposes, but they are also especially convenient for education and training. the model car transport system described herein presents a laboratory with a physical model of infrastructure and is intended for research and analysis of road traffic monitoring and management and is realized at department of vehicle technology at faculty of transportation sciences at ctu in prague. a similar project has been realized for rail traffic model within the laboratory of transport technology[5] and is running at department of transport telematics of ctu, prague. 2. system overview the basis of the model car transportation network is a model in a ratio 1:87 (ho), based on component units of faller car system[6], e.g. vehicles, traffic lights, carriageway, parking spaces, stop sections, branch-off junctions, sensors and control sections (see figure 1[6]). the faller car system was initially designed to complement railway models. in our case it is used the other way around. the fundamental car model is 5 http://dx.doi.org/10.14311/app.2017.12.0005 http://ojs.cvut.cz/ojs/index.php/app karel bouchner, alina mashko acta polytechnica ctu proceedings figure 1. some components of the model. source: [6]. figure 2. city (left) and village (right) infrastructure. supplemented with a small railway that among other things includes two railway stations and a railway crossing. it enables simulation of real traffic situations on intraand extravilan communications with a level crossing with a rail road and a section of highway (see figures 2 through 5 for reference). see the general schematic representation of the whole model on figure 6. 2.1. technical description of the model road in the model is realized with the help of wooden plates. the technology that controls vehicles’ lateral movement is allocated within the road surface (wire rail) and under the surface. model vehicles are equipped with an electric motor, a steering apparatus, a rechargeable battery, an on/off switch on the bottom of the car to start it and a reed sensor that responds to magnet effect. permanent magnet tip is attached in a flexible way under the road so that an approaching vehicle with steering mechanism in front responds to wire magnetism which is keeping vehicles on track. 2.1.1. physical layer of the model infrastructure physical part of the model is represented by the road that is built up with the help of wooden plate elements figure 3. intravilan connection. figure 4. highway section with a trumpet-type interchange. fixed on foam plastic pieces of various constructions for modeling of different terrain levels. a wire rail is embedded into the wooden road along its length. control sections are placed under the road (see figures 7 through 9 for physical layer elements for reference). sensors are used for activation of functional elements, for example stop sections, parking spaces and branch-off junctions. they contain reed contact. sensors embedded in the road are activated by magnets on the vehicles when the vehicle goes over the sensor. the sensor gives precise feedback on the traffic control. this signal activates the control of a functional element. 2.2. traffic control • traffic node control – intersection the stop section (see figure 10) is needed to initiate vehicle full stop at road junctions (intersections and level intersections), bus stops, parking slots etc. it consists of an electromagnet embedded in the roadway. with power, its magnetic field will switch off the vehicle’s motor power via the reed sensor. for example, stop sections together with traffic lights and hw control section can control traffic on a classic four-way crossroad in a completely automated way (see figure 11). • traffic node control – navigation and routing the branch-off junction (see figure 12) is used for turning of vehicles to the right or left. when activated, the magnetic field of the branch-off junction diverts a vehicle onto a second, branching contact wire. this is done through the magnet on the vehicle’s steering slider. 6 vol. 12/2017 model car transport system figure 5. supermarket with parking. figure 6. general schematic representation of traffic real model. • parking control permanent magnet is also applied in case of longer stops such as parking (see figure 13). when the parking space is activated, an integrated electric coil briefly interferes with this magnetic field. this closes the reed sensor in the vehicle and supplies power to the motor. the vehicle starts moving. the traffic infrastructure includes different types of intersections including t-junctions, a classic fourway crossroad with traffic lights and a four-way traffic circle, bus stops etc. an important part of the model is a segment of a highway which includes an elevated crossing with highway entries and exits. the highway has two lanes in each direction. such an arrangement corresponds to common real construction of highways (according to standard [7], except for a few parts where accommodation was needed due to space constrains). the two-lane arrangement enables to simulate real traffic situations, e.g. when one vehicle enters the highway and the second one is approaching to the highway at the same time, or during overtaking of vehicles on the figure 7. road with metal wire, with control element. figure 8. physical part of road construction in different sections (left – four-way highway, right – elevated intersection) and model vehicles. highway. a disadvantage of the technology is that a movement of model vehicles does not fully correspond to a behavior of real vehicles. model vehicles move by a constant speed. the speed depends only on a status of a rechargeable battery. when the battery is fully charged the speed is the highest. during its discharging, the speed of model vehicle decreases. so far, model vehicles are neither able to start and stop smoothly, nor to vary their speed. in addition, now, their speed does not correspond to a type of real vehicles. 2.3. model operation and control there are three different ways to control the whole model: • manual control an operator activates the control of functional elements manually, using push buttons and switches. model vehicles move according to the operator’s immediate actions. • preset automatic control the functional elements are controlled by associated control sections. the operation of the control sections can be either fully automatic, depending only on their initial setting, or depending on their initial 7 karel bouchner, alina mashko acta polytechnica ctu proceedings figure 9. examples of three types of control sections (from left to right): parking space, stop section and branch-off junction – an alternative to faller elements. figure 10. stop section. source: [6]. setting in combination with signals from the associated sensors. model vehicles move according to their immediate status of functional elements controlled by the corresponding control section. operation of individual control sections is not synchronized. • program control the functional elements are controlled by an associated pc-standard module and expansion modules. the pc-standard module is connected to a pc with an appropriate sw application and interconnected with expansion modules. also sensors are connected to the modules. an operator creates on the pc programs of different traffic situations for the whole model, using the sw application. the sw application also utilizes signals from sensors for its activity. modules operate according to the running program. model vehicles move according to their immediate status of functional elements controlled via corresponding modules by the running program. figure 11. example of intersection control. source: [6]. figure 12. branch-off junction. source: [6]. 3. further perspective the current model shall be used as the basis platform for future smart systems implementation, programming based on real traffic data, or for simulation of real traffic and driver behavior. it brings several challenges for the development of software applications for intelligent transport systems, implementations of more traffic data collectors such as a camera or road section detectors and other traffic surveillance and control systems[8]. the system may serve for students’ training in a wide range of disciplines applied in transport studies and research, namely, traffic management and control, city planning and infrastructure design, software development, driver behavior and humanmachine interaction just to name a few. the current project has a goal to design a fully automatically operated system with simulation of vehicle-to-vehicle (v2v), infrastructure-to-vehicle (i2v or v2i) commu8 vol. 12/2017 model car transport system figure 13. parking space. source: [6]. nication in a way so that fully autonomous vehicles could drive in real conditions. the video-based data from the cameras that will be installed in the system will provide the traffic information for decisions to be taken by robot drivers of individual vehicles. the cameras are to be installed in the control sections and on the vehicles for strategic route planning as well as immediate reaction to the traffic in front, correspondingly. the front cameras can also be used for manual vehicle control with remote driver. thus, it is planned to simulate possible future scenarios of vehicle operation in smart cities[9]. 4. conclusion the model car transport system is one of important tools, assisting students of faculty of transportation science in their study. it facilitates understanding of matters of the intelligent transport system and the smart city. finally, it enables a comprehensive application of student theoretical knowledge in a wide range of transportation theory topics, in informatics, electronics, control theory. it is an appropriate tool for software and model hardware testing of various its applications and tools applicable in smart city projects. references [1] m. lom, o. přibyl, m. svítek. industry 4.0 as a part of smart cities. conference paper. smart cities symposium prague 2016. doi: 10.1109/scsp.2016.7501015. [2] l. galán-garcía, g. aguilera-venegas, p. rodrígues-cielos. an accelerated-time simulation for traffic flow in a smart city. journal of computational and applied mathematics. volume 270, november 2014, pages 557-563. [3] z. li, m. shahidehpour. deployment of cybersecurity for managing traffic efficiency and safety in smart cities. the electricity journal. volume 30, issue 4, may 2017, pages 52-61. [4] c. navarro, m. rca-riu, s. furió, m. estrada. designing new models for energy efficiency in urban freight transport for smart cities and its application to the spanish case. transportation research procedia. volume 12, 2016, pages 314-324. [5] laboratory of transport technics. czech technical university in prague, faculty of transportation sciences, department of transport telematics (16120), konviktská 20, prague 1, 110 00 czech republic, http://dsfd.fd.cvut.cz, 10.2.2017. [6] faller gmbh, gütenbach / schwarzwald. amtsgericht freiburg hrb610917, http://www.faller.de, 7.10.2016. [7] čsn 73 6101 projektování silnic a dálnic. praha: český normalizační institut, 2004. [8] m. a.-p.-taylor. intelligent transport systems. university of south australia, adelaide, http://www.emeraldinsight.com/doi/abs/10.1108/ 9781615832460-031, 10.2.2017. [9] conceptualizing smart city with dimensions of technology, people, and institutions. taewoo nam & theresa a. pardo, center for technology in government, university at albany, state university of new york, u.s., https: //www.ctg.albany.edu/publications/journals/dgo_ 2011_smartcity/dgo_2011_smartcity.pdf, 10.2.2017. 9 http://dsfd.fd.cvut.cz http://www.faller.de http://www.emeraldinsight.com/doi/abs/10.1108/9781615832460-031 http://www.emeraldinsight.com/doi/abs/10.1108/9781615832460-031 https://www.ctg.albany.edu/publications/journals/dgo_2011_smartcity/dgo_2011_smartcity.pdf https://www.ctg.albany.edu/publications/journals/dgo_2011_smartcity/dgo_2011_smartcity.pdf https://www.ctg.albany.edu/publications/journals/dgo_2011_smartcity/dgo_2011_smartcity.pdf acta polytechnica ctu proceedings 12:5–9, 2017 1 introduction 2 system overview 2.1 technical description of the model 2.1.1 physical layer of the model infrastructure 2.2 traffic control 2.3 model operation and control 3 further perspective 4 conclusion references 252 acta polytechnica ctu proceedings 2(1): 252–256, 2015 252 doi: 10.14311/app.2015.02.0252 the recurrent eclipsing nova u sco: a short review r. gonzález-riestra1 1xmm science operations centre, esac, madrid, spain corresponding author: rosario.gonzalez@sciops.esa.int abstract u scorpii is the recurrent nova with the shortest inter-outburst period, only ten years. the last active phase took place at the beginning of 2010, and it provided a large amount of data from both ground-based and space observatories. this paper reviews some of the more relevant recent findings and points out some, still unanswered, questions. keywords: recurrent novae uv x-rays individual: u sco. 1 introduction u scorpii is a recurrent nova that undergoes frequent outbursts. it is also an eclipsing binary (i=83 deg, thoroughgood et al. 2001), hence the geometrical parameters of the system are known with great accuracy. the orbital period is 1.23 days (schaefer 1990). ten outbursts of this system have been observed, the first one in 1863 (schaefer 2010). outbursts take place quite regularly, every ≈ 10 years. there are two long intervals of about 20 years during which no outbursts were observed (around 1927 and 1957), but very likely they were missed because the system was too close to the sun when they took place. the system is characterised by extremely short timescales: the recurrence time is only ten years, the shortest known in this type of objects, the system goes into outburst in a few hours, and decays in a few days, with t2=1.2 days and t3=2.6 days. in accordance with all this, very high velocities of the order of 104 km s−1 have been observed. all the above implies that the primary of the system is a high-mass white dwarf. the nature of the secondary star is still unclear, but it is very likely slightly evolved, k2 iv (anupama and dewangan 2000). there is a general agreement on the sizes and masses of both stars: r2 ≈2.4 r�, m2 ≈1.3 m�, m1 ≥1.37 m� (hachisu et al. 2000, thoroughgood et al. 2001). the size of the orbit is ≈ 6.7 r�, and the distance to the system has been estimated to be 12 kpc (schaefer 2010). 1.1 before 2010: uv data iue observed u sco during the first weeks of the 1979 outburst. the uv spectrum presented at the beginning low ionisation lines, and strong p-cygni profiles in the resonance lines. later on, there was an overall increase in the ionisation level, so that in the last observations figure 1: evolution of the ultraviolet spectra of u sco during active phases. spectra of days 4-16 were taken with iue during the 1979 outburst, while the last two were taken with hst-stis in 1999. 252 http://dx.doi.org/10.14311/app.2015.02.0252 the recurrent eclipsing nova u sco: a short review the strongest lines corresponded to he ii, n v, c iv, n iv, and possibly [mg v] (williams et al. 1981, barlow et al. 1981). it is worth noting that the he ii 1640 å line was always much narrower than the others. further uv observations were obtained with hststis during the first two months of the 1999 outburst, confirming the evolution observed before (fig. 1). the last spectra showed only high ionisation broad lines and a narrow he ii line. 1.2 before 2010: x-ray data u sco was known to be a strong x-ray emitter already before the 2010 outburst. the sax observation on day 19 of the 1999 outburst, when the system was detected as a supersoft source, is described by kahabka et al. (1999). these authors fitted a model atmosphere to the sax spectrum, finding a temperature of 9×105 k and a luminosity in the range 2-20×1037 erg s−1. they also found evidence for a weak harder component, and reported variations of the order of 50% during the observation. 2 the 2010 outburst by the beginning of the 21st century the recurrence time of u sco was well established, 10±2 years (schaefer 2005). the last outburst had taken place in 1999, and the date of the next one was predicted to be 2009.3±1. in very good agreement with this prediction, the outburst took place on january 28 2010 (2010.08). the time to rise to maximum brightness was only 9 hours. the optical light curve was very complex, with many different features: there was an early decline phase, a plateau, a second decline and a second plateau. and superimposed on all this, there were short-lived phenomena: flares, dips and the resumption of eclipses (see a detailed description in schaefer et al. 2011). 2.1 x-ray observations 2.1.1 swift the 2010 outburst of u sco was followed by all the x-ray missions, swift, suzaku, chandra and xmmnewton. particularly relevant is the monitoring carried out by swift since, apart from its own scientific value, it allowed to schedule efficiently target of opportunity observations with the other missions, as described below. swift observed u sco daily during two months. supersoft x-ray emission was detected around day 12, when the flux started to increase until reaching a maximum around day 31, to decrease slowly afterwards. the appearance of the supersoft emission roughly coincided with the first extended optical plateau, while the x-ray turn-off started at the time of the second optical decline (schaefer et al. 2010). 2.1.2 suzaku suzaku took three observations of u sco, but only the last one, on day 15, provided useful data, and a surprising result: the detection of a shallow x-ray eclipse (with a depth of ≈30%) in coincidence with the predicted time of the optical eclipse. from the duration of this eclipse, takei et al. (2013) estimated the size of the x-ray emitting region in 5 r�. 2.1.3 high resolution spectroscopy: chandra and xmm-newton a further x-ray observation was taken on day 18, this time with chandra letg. unfortunately, it was short, and taken out of eclipse, and therefore the suzaku result could not been confirmed. orio et al. (2013) claimed that the deep absorption lines seen in the letg spectrum (see top panel of fig. 2) are not p-cygni profiles, but just the superposition of blue-shifted absorptions from the white dwarf atmosphere (whose shift is due to a wind) and the emission lines from the ejecta. these authors derived a temperature of 7×105 k and a luminosity of 7×1036 erg s−1. this is to be compared with the sax estimations, with a much higher luminosity. it is not clear whether the 1999 outburst was intrinsically more luminous, or if the discrepancy is just due to the different atmosphere models used for both determinations. two more x-ray high resolution spectra were obtained with xmm-newton on days 23 and 35, the second one just after the x-ray peak. the xmm-rgs spectrum of the first observation showed similar emission lines as the chandra spectrum, but no absorptions. this was interpreted by orio et al. (2013) as an indication of the end of the wind phase of the white dwarf. the model atmosphere fits presented by these authors showed an increase in the temperature of the white dwarf from day 18 to day 35, at a a nearly constant x-ray luminosity. the emission lines in the day 23 spectrum can be explained by collisional ionisation, while the situation is more complex on day 35, requiring also the existence of a strong uv field. there are some unidentified lines, and others whose presence just cannot be explained. the three grating spectra are shown in left panel of fig. 2. the x-ray light curves also provided interesting information. the first xmm observation started at orbital phase 0.8, thus a clear x-ray eclipse was expected, but an irregular light curve was seen instead, with dips and flares. these dips are an indication of clumps of 253 r. gonzález-riestra material in the re-forming accretion disk (ness et al. 2012). on the contrary, on day 35 the eclipse is very well defined. it is worth to note that on this date the depth of the eclipse is 50%, showing that the x-ray source is very extended, likely a thomsom scattering corona (ness et al. 2012, orio et al. 2013). takei et al. (2013) interpreted the difference in the x-ray eclipses of days 15 and 35 as a shrinking of the x-ray emitting region, from 5 to 4 r�. the optical eclipse mapping done by schaefer et al. (2011) also indicates a shrinking of the optical source, from 4 r� on day 20 to 2.2 r� on day 50. after day 20, the source of the optical light changes, from spherically symmetric to disk-like, first with a bright rim, later brighter at the centre. xmm-newton obtained uv photometry simultaneously with the x-ray observations. on day 23 there was a very well defined uv eclipse, and the light curve was rather smooth, with some structures, as a flare that can be coincident with a similar feature in the x-ray light curve. the depth of the minima in both uv and x-ray light curves was similar (≈50%). the eclipse on day 35 is twice as deep in the uv than in x-rays, indicating a smaller emitting area (ness et al. 2012). figure 2: x-ray high resolution spectra (left panel) and light curves (right panel) of u sco during the 2010 outburst. from top to bottom, chandra letg data taken on day 18, and xmm-newton rgs spectra and epic light curves obtained on days 23 and 35. 2.2 optical spectroscopy also interesting to mention is the evolution of the optical spectra. mason et al. (2012) reported the appearance of narrow emission lines of h, he i and he ii on day 8. the radial velocity curve of these lines (that does not mach either of the two stars) indicate that they form in an accretion flow suggesting that the disk was already re-established. mason (2011) studied the abundance in the ejecta and found a high ne/o ratio, concluding that the white dwarf belongs to the o-ne-mg class, with the implications for the further evolution of the system. finally, in this outburst, forbidden emission lines have been observed for the first time, around day 46 (mason et al. 2012, dı́az et al. 2010). this result must be taken with caution, as it can be just a selection effect, since this outburst had a much better observational coverage than the previous ones. 2.3 the evolution of the outburst as shown in the previous sections, the last outburst of u scorpii has provided a large amount of data that have given us to a more clear view of the behaviour of the system. 254 the recurrent eclipsing nova u sco: a short review models show he disk was destroyed in the outburst (drake and orlando 2010). but only a few days later there were already evidences of accretion being re-established, e.g.: • appearance of narrow optical lines on day 8, • optical and x-ray eclipses on day 15, indicating the existence of a large emitting region ≈ 4-5 r�, • optical flickering and dips in the x-ray light curve on day 23. analysis of the optical light curve shows that by day 40 the disk was already fully re-established. table 1: summary of the evolution of the 2010 outburst of u scorpii day event 0 disk destroyed 8 he, hei and heii narrow emission lines 9-15 optical flares 12 supersoft phase 15 x-ray and optical eclipses 20 end of the white dwarf mass-loss 23 x-ray dips 24 flickering 30 rim-bright disk 40 optical dips 46 nebular spectrum 3 conclusions this system represents an unique opportunity to study the outburst mechanisms of recurrent novae, as it allows us to compare data obtained in several different cycles, with relatively similar instrumentation. despite of the large amount of available data, or possibly due to that, there are still many open issues. for instance, when going through the literature, the values of the mass of the envelope cover a range of 60, even for the same outburst. williams at al. (1981) and anupama and dewangan (2000) get the same value of 10−7 m� for the 1979 and the 1989 outbursts, respectively. on the other hand, takei et al. (2013) obtain 6×10−6 m� for the last outburst. also striking is the wide range of helium abundance values (n(he)/n(h)), as high as 4.5 (evans et al. 2001), but also as low 0.07 (maxwell et al. 2012). is there is a real difference in the mass ejected in the different outbursts? how can the values of the helium abundance be reconciled? obviously, the methods used to derive this quantities and the underlying assumptions are very different. a deep, uniform analysis of all existing data is necessary to find the reason for these discrepancies and to better understand the behaviour of the system. acknowledgement i warmly thank the organisers for their kind invitation to this meeting. references [1] anupama, g. and dewangan, g.: 2000, aj 119, 1359 [2] barlow, m., brodie, j., brunt, c. et al.: 1981, mnras 195, 61 [3] dı́az, m., williams, r., luna, g. et al.: 2010, aj 140, 1860 [4] drake, j. and orlando, s.: 2010: apj, 720, l195 doi:10.1088/2041-8205/720/2/l195 [5] evans, a., krautter, j., vanzi, l. and starrfield, s.: 2001, a&a 378, 132 [6] hachisu, i.; kato, m., kato, t. and matsumoro, k.: 2000, apj 534, l189 [7] kahabka, p., hartmann, h., parmar, a. and negueruela, i.: 1999. a&a 347, 43 [8] mason, e., 2011, a&a 532, l11 [9] mason, e., ederoclite, a., williams, r. et al.: 2012, a&a 544, 149 [10] maxwell, m., rushton, m., darnley, m. et al.: 2012, mnras 419, 1465 doi:10.1111/j.1365-2966.2011.19803.x [11] ness, j.-u., schaefer, b., dobrotka, a. et al.: 2012. apj 745, 43 doi:10.1088/0004-637x/745/1/43 [12] orio, m., behar, e., gallagher, j. et al.: 2013, mnras 429, 1342 doi:10.1093/mnras/sts421 [13] takei, d., drake, j., tsujimoto, m. et al.: 2013, apj 769, l4 doi:10.1088/2041-8205/769/1/l4 [14] schaefer, b.: 1990, apj 355, l39 [15] schaefer, b.: 2005, apj, 621, l53 doi:10.1086/429145 255 http://dx.doi.org/10.1088/2041-8205/720/2/l195 http://dx.doi.org/10.1111/j.1365-2966.2011.19803.x http://dx.doi.org/10.1088/0004-637x/745/1/43 http://dx.doi.org/10.1093/mnras/sts421 http://dx.doi.org/10.1088/2041-8205/769/1/l4 http://dx.doi.org/10.1086/429145 r. gonzález-riestra [16] schaefer, b.: 2010, apjs 197, 275 doi:10.1088/0067-0049/187/2/275 [17] schaefer, b., pagnotta, a., osborne, j. et al.: 2010, atel 2477 [18] schaefer, b., pagnotta, a., lacluyze, a. et al.: 2011, apj 742, 113 doi:10.1088/0004-637x/742/2/113 [19] thoroughgood, t., dhillon, v., littlefair, s. et al.: 2001, mnras 327, 1323 [20] williams, r., sparks, w. gallagher, j. et al.: 1981, apj 251, 221 256 http://dx.doi.org/10.1088/0067-0049/187/2/275 http://dx.doi.org/10.1088/0004-637x/742/2/113 introduction before 2010: uv data before 2010: x-ray data the 2010 outburst x-ray observations swift suzaku high resolution spectroscopy: chandra and xmm-newton optical spectroscopy the evolution of the outburst conclusions acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0019 acta polytechnica ctu proceedings 4:19–21, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app radiation degradation of pcbs in sediments: comparison between two methods ľubica darážováa,∗, andrea šagátováa,b, vladimír nečasa, marko fülöpb, bumsoo hanc a institute of nuclear and physical engineering, faculty of electrical engineering and information technology, slovak university of technology, ilkovičova 3, 812 19 bratislava, slovakia b university centre of electron accelerators, slovak medical university, ku kyselke 497, 911 06 trenčín, slovakia c eb tech co., ltd., daejeon 305-500, south korea ∗ corresponding author: lubica.darazova@stuba.sk abstract. polychlorinated biphenyls are toxic compounds which have accumulated in river sediments in eastern slovakia. bioaccumulation could cause even cancer. radiation degradation with electrons is new and perspective method to dechlorinate pcbs in sediment matrix. we tested the influence of two difference chemical pretreatments and electron irradiation on pcb contaminated sediments. keywords: pcbs, cuso4 · 5h2o, electron beam, irradiation, sediment. 1. introduction polychlorinated biphenyls (pcbs) were used as additives for lubricants, adhesives in transformers and capacitors. chemical and physical properties are following: inertness, resistance to heat, non-flammability and high dielectric constant. pcbs were produced all over the world, but the production was banned in 1998. in slovakia the producer of pcbs was the chemical company chemko strážske ltd. probably, a part of produced pcbs was released to the environment through the strážske channel. over the years the sediments in surrounding area of the chemical factory (the laborec river and the zemplínska šírava lake) were contaminated with pcbs. the contamination in strážske channel exceeds 400-times the limit, which is allowed in slovakia for the sediment matrix. behavior of pcbs in the soil is strongly dependent on the basic soil properties. great attention has been devoted to the pcbs problem in soil contamination in united kingdom, usa, canada, japan and sweden. in slovakia, the monitoring of pcbs was carried out, but specific solution has not been given [1, 2]. irradiation of pcbs with electron beam has not been used very often and it is new technology, which could provide non-combustion method for pcbs degradation in soil sediments. water is a product produced during radiolysis and it is also presented in soil samples contaminated by pcbs. the presence of oxygen during the irradiation process has negative effect to radiolytic dechlorination of pcbs contaminated sediments. soil matrice is rich of organic and anorganic compounds. the dechlorination yields of pcbs were reduced, due to the organic content of the soil, which could compete with required free radiacal reactions [3]. due to the hydrophobicity of pcb, organic-rich sediments could be easily solubilized in water with the use of organic co-solvent. during the radiolysis, hydroxyl radicals react with pcbs through the addition to the phenyl rings to produce various isomeric pcb radicals (arcl(oh)) [4]. 2. pcbs degradation with electron beam 2.1. simple pcbs irradiation with electron beam electrons interact at high energies predominantly by elastic scattering by bound electrons. the chemical changes in pcbs occur through secondary reactions of radiolytic species with pcbs (fig. 1). hydrogen atoms and hydroxyl radicals react with pcbs via addition to the phenyl rings, producing pcbs radicals. pcbs that remain in association with or within the sediment phase may undergo dechlorination by thermalized electrons [5, 6]. figure 1. mechanism of radiation dechlorination of pcbs [5]. 19 http://dx.doi.org/10.14311/ap.2016.4.0019 http://ojs.cvut.cz/ojs/index.php/app ľ. darážová, a. šagátová, v. nečas et al. acta polytechnica ctu proceedings 2.2. chemical pretreatment and electron irradiation of pcbs due to the fact that pcbs are hydrophobic compounds, it is required to use co-solvent. very often is used as co-solvent propan-2-ol, which assist with the dechlorination process of pcbs. it is essential to stabilize the formed aromatic radicals, that´s why it is need the compound which could easily donate hydrogen atoms, which could stabilize the aromatic cycle. such compounds are alcohols. trifan et al. [7] tested the influence of propan-2-ol, ethanol, thf and electron beam irradiation for pcbs destruction in transformer oils and solutions (fig. 2). the best results in terms of degree of dechlorination and convertion of pcbs into biphenyls were obtained when propan-2-ol was used. also, naoh or koh are needed for basic environment, which prevent the oxidation of cl– ions to cl2 [7]. figure 2. influence of the different solvent type on dechlorination of pcbs (dose of irradiation = 40 kgy, [pcbs] = 32.6 g dm−3, naoh = 1.5 g, temp. 65 ◦c, cb = conversion of pcb into biphenyl, dd = degree of dechlorination) [7]. 3. methodology our study was aimed to compare our method of chemical pretreatment and electron irradiation of samples to results obtained by colleagues from south korea, who chemically pretreated and irradiated the samples of soil contaminated by pcb from slovakia. they used lower energy of electrons, 2.5 mev. after irradiation at eb-tech to a dose of 400 kgy the total concentration of pcbs in soil samples decreased by more than 53 % (fig. 3). 3.1. chemical pretreatment and electron irradiation of pcbs in our experiment we used 5 mev electrons and chemical pretreatment: cuso4 · 5h2o and k2co3. 20 g of wet sediment was mixed with 2 g of k2co3, which provided stable ph ∼ 10 which is essential to keep cl– anions during reaction. our samples were rich figure 3. pcb concentration in soil sample as a function of dose irradiated by eb-tech vs. ucea trenčín. of water and water molecules are competitive compounds in the process of pcbs irradiation. due to this fact, 1 g of cuso4 · 5h2o, as a water scavenger, was added to the sample. samples were irradiated in the test tubes by electron accelerator with scanning beam uelr-5-1s at the university centre of electron accelerators (ucea) of the smu in trenčín. we applied doses: 100, 300, 500 and 700 kgy to chemical pretreated samples. determination of pcb in sediment was done at the department of toxic organic pollutants of the smu in bratislava. isotopedillution method by using of 13c-labeled standard solution was used. about 0.15 g of dried homogenized irradiated sediment was soxhlet extracted with toluene (8 hours). an 1/50 aliquot of the extract was applied on multi-layer silica column (44 % sulphuric acid/potassium hydroxide/silver nitrate on activated silica gel). the pcb extract was carefully concentrated and after dilution coupled with high-resolution mass spectrometry (hrgc). the initial total content of pcbs was intended to 1842.69 ng g−1. 4. results and discussion fig. 3 shows that with increasing dose, the total amount of pcb congeners is decreasing at our experiments. at dose 700 kgy the pcb degradation falls to 46 %. from the fig. 4, it is seen, that pcbs groups are decreasing with increasing dose, but also the increase occurs, when higher chlorinated pcbs are converting to lower ones. for environmental purposes, it is required to degrade pcb with higher efficiency. our methodology (ucea) was less efficient than the methodology of eb-tech, as we reached only 46 % decrease of total amount of pcbs at 700 kgy in comparison to their 53 % decrease at 400 kgy. it could be caused by energy of electrons and also by the chemical pretreatment method. for this purpose we are going to find better chemical pretreatment methodology in our future research. 20 vol. 4/2016 radiation degradation of pcbs in sediments figure 4. concentration of pcb groups in soil samples chemically pretreated by cuso4 · 5h2o and k2co3 as a function of increasing dose of electrons. acknowledgements the authors would like to thank for financial contribution to the research to the sut grant scheme for support of young researchers. references [1] i. danielovič, j. hecl, m. danilovič. soil contamination by pcbs on a regional scale: the case of strážske, slovakia. pol j environ stud 23(5):1547–1554, 2014. http://www.pjoes.com/pdf/23.5/pol.j. environ.stud.vol.23.no.5.1547-1554.pdf. [2] i. danielovič, j. hecl, r. mati. polychlórované bifenyly a ich obsah v životnom prostredí regiónu zemplín. informačná publikácia, košický samosprávny kraj, 2009. [3] a. singh, w. kremers. radiolytic dechlorination of polychlorinated biphenyls using alkaline 2-propanol solutions. radiation physics and chemistry 65:467–472, 2002. doi:10.1016/s0969-806x(02)00360-2. [4] d. c. schmelling, d. l. poster, m. chaychian, et al. degradation of polychlorinated biphenyls induced by ionizing radiation in aqueous micellar solutions. environmental science & technology 32(2):270–275, 1998. doi:10.1021/es9704601. [5] h. yuan, h. pan, j. shi, et al. kinetics and mechanisms of reactions for hydrated electron with chlorinated benzenes in aqueous solution. frontiers of environmental science & engineering 9(4):583–590, 2015. doi:10.1007/s11783-014-0691-8. [6] m. chaychian. radiation-induced dechlorination of pcbs and chlorinated pesticides and the destruction of the hazardous organic solvents in waste water. ph.d. thesis, university of maryland, 2007. [7] a. trifan, i. calinescu, d. martin. transformation of polychlorrinated biphenyls (pcbs) into non-hazardous products by electron beam treatment. rev roum chimie 60(10):1053–1055, 2009. 21 http://www.pjoes.com/pdf/23.5/pol.j.environ.stud.vol.23.no.5.1547-1554.pdf http://www.pjoes.com/pdf/23.5/pol.j.environ.stud.vol.23.no.5.1547-1554.pdf http://dx.doi.org/10.1016/s0969-806x(02)00360-2 http://dx.doi.org/10.1021/es9704601 http://dx.doi.org/10.1007/s11783-014-0691-8 acta polytechnica ctu proceedings 4:19–21, 2016 1 introduction 2 pcbs degradation with electron beam 2.1 simple pcbs irradiation with electron beam 2.2 chemical pretreatment and electron irradiation of pcbs 3 methodology 3.1 chemical pretreatment and electron irradiation of pcbs 4 results and discussion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.9.0019 acta polytechnica ctu proceedings 9:19–25, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app preparing of the chameleon coating by the ion jet deposition method jakub skocdopolea,∗, lucrezia aversab, martin golanc, antonin schenkd, giacomo baldib, irena kratochvilovac, ladislav kalvodaa, petr nozarb a department of solid state engineering, faculty of nuclear sciences and physical engineering, czech technical university in prague, prague, czech republic b istituto materiali per elettronica e magnetismo imem-cnr, trento, italy c institute of physics, cas in prague d department of physical electronics, faculty of nuclear sciences and physical engineering, czech technical university in prague, prague, czech republic ∗ corresponding author: jakub.skoc@gmail.com abstract. preparation of chameleon coatings using an ionized jet deposition (ijd) technique is reported in the present paper. ijd is a new flexible method for thin film deposition developed by noivion, srl. the chameleon coatings are thin films characterised by a distinct change of their tribological properties according to the external conditions. the deposited films of sic and tin materials were examined by the raman spectroscopy, sem and xps. the results of the raman spectroscopy have proved an amorphous structure of sic films. the data from xps on tin films have shown that the films are heavily oxidized, but also prove that the films are composed of tin and pure ti. the sem provided information about the size of grains and particles constituting the deposited films, which is important for tribological properties of the films. deposition of the chameleon coating is very complex problem and ijd could be ideal method for preparation of this coating. keywords: ion jet deposition, chameleon coating, raman spectroscopy, scanning electron microscope, x-ray photoelectron spectroscopy. 1. introduction chameleon coating is a multilayer film, which changes its tribological attributes according to the external conditions. the main attributes interesting from a point of view of possible industrial applications are the capability of the layer to withstand high mechanical loads without a fracture, high wear resistance and low friction coefficient of the film. ionized jet deposition is one of pvd (physical vapor deposition) methods for preparation and growth of thin films. it is based on generation and application of dense pulsed electron beam which interacts with selected target material and produces a plume of the target material. the thin layer of target material is grown by condensing the plasma plume on the appropriate substrate. the flexibility of the method stands in the set of independent parameters, variety of suitable materials for the deposition and in the possibility to use multiple ijd systems for the deposition of multilayers films. the independent parameters are distance between target and substrate, working gas, pressure during deposition, frequency of electron beam pulses and trigger voltage. all these parameters can be adjusted according to the desired deposition process outcome. the ijd technique permits to deposit both inorganic and organic materials on substrates which, again, could be of inorganic or organic nature because of low temperature of deposition plasma. it is also possible to deposit conducting and non-conducting/isolating materials and optically transparent materials. however, in order to deposit strongly isolating materials, it is necessary to add an auxiliary anode between ijd hollow cathode and target of the deposited material to electrically decouple the ijd system from the target. from these characteristics it seems to be reasonable to assume that the ijd method could be ideal technique for the chameleon coatings preparation. in this article we will focus on a part of the chameleon coatings, namely, hard metal carbides and nitrides. such deposited hard films are examined by raman spectroscopy, sem and xps and the results reported and discussed. 2. theory 2.1. ionized jet deposition the ijd working tool a pulsed energetic electron beam is generated in the ijd source. the main part of the ijd source is a hollow flight-through anode/cathode. an electron discharge trigger is attached to the anode/cathode and serves for the controlled "firing" of the main discharge and for the generation of the dense electron pulse directed towards the tar19 http://dx.doi.org/10.14311/app.2017.9.0019 http://ojs.cvut.cz/ojs/index.php/app jakub skocdopole, lucrezia aversa, martin golan et al. acta polytechnica ctu proceedings figure 1. example of an ijd source [8]. get. usually (but not necessarily), either a small channel spark or a pseudospark switch, or an electron and plasma source is connected to the main anode/cathode and used as the trigger (see figure 1). the main anode/cathode electrode has the form of a hollow cylinder with openings in both bases and oriented as follows: the base with the smaller opening towards the target and the base with the larger opening towards the substrate. the hollow cathode produces, owing to a hollow cathode effect, a dense bunch of energetic electrons [7], that leave the hollow cathode towards the target in the final stage of the process. the electrons of the bunch hitting the target surface interact with the atoms of the target transferring to them their kinetic energy and creating a plume of energetic and highly ionized target plasma. the plasma plume which is predominantly expanding in the direction perpendicular to the target surface faces the hollow cathode, enters the smaller opening in the cylinder base facing the target, expands (flies) through the hollow cylinder and leaves the hollow cathode through the larger opening base towards the substrate (therefore "flight-through cathode"). 2.2. chameleon coating it is often necessary to use a combination of different materials within one thin film layer to optimize its selected properties. for example, it is possible to combine an amorphous matrix from dlc (diamond like carbon) with small grains of hard/ultra-hard material (such as tungsten carbide) within it. the grains should have the diameter in tens of nm and distance between them in nm for the best mechanical properties. the diamond like matrix provides the high hardness and low friction of deposited thin film, while the grains of carbide prevent the film from brittle fracturing and, if required, ensure the abrasive properties of the film as e.g. in the case of cutting tools. unfortunately, the low friction of this film occurs only in humid environment, because the dlc under the friction converts to graphite. the graphite does not have good wear resistance however it could be compensated by the grains of hard material. graphite has low frictions coefficient only in humid environment. to provide low friction of the film in dry environment or in vacuum it is necessary to add another material e.g. mos2 which has a hexagonal structure similar to the graphite but is excellent lubricant for dry environment or vacuum. to provide the low friction the mos2 film has to present the hexagonal planes parallel to the friction force. fortunately, the mos2 material under friction has the tendency to orient its structure in such a way that it provides the lowest friction coefficient. such ability allows substantial reduction of the system friction coefficient in dry environment just by adding the mos2 material to the dlc matrix with carbide/nitrite particles incorporated. film composition of mos2/dlc/wc could be called chameleon because it adjusts its mechanical properties to the environment in which it is situated. in humid environment, the amorphous dlc provides low friction, the mos2 and wc are scratched from the film surface in form of a debris. in dry environment the low friction is provided by mos2, the graphitized dlc and wc are scratched from the surface [1] (figure 2). we assume that the ijd could be good choice for preparing such film. there are two options how the ijd could be used. first option uses two electron guns (ijds) with two seperated targets (each for one ijd). then the substrate must be placed in position where both plasma plumes overlap. the second option uses only one electron gun but needs rotary target holder. the rotary target holder provides opportunity 20 vol. 9/2017 preparing of the chameleon coating by the ion jet deposition method figure 2. principle of chameleon coating function [1]. name substrate film time [min] pressure [mbar] distance [mm] kuba7 silicon wafer tin 15 1.6 105 kuba9 stainless-steel tin 14 1.4 105 k2 aluminium alloy sic 30 0.6 180 table 1. deposition parameters. of deposition from multiple targets only with one electron gun (ijd). 3. experiment two types of hard material have been prepared trying to enhance the resistance of the deposited layer against fracturing, namely, the sic deposited on aluminium alloy and tin deposited on stainless steel and single crystalline silicon. all deposition events have been performed in ar atmosphere. the deposition time, process gas (ar) pressure during deposition and distance between the target and the substrate (see table 1) have been chosen as important process parameters to be adjusted for different deposited samples. the films have been analysed by raman spectroscopy, sem and xps. 4. results the thickness of films was not directly measured, but it was deduced from the xrd results and from the values obtaind for similar films, which was deposited with the same deposition parameters.the roughly estimated thickness value obtaind in such way amounted several microns. 4.1. raman spectroscopy the measurement was performed at room temperature using an excitation laser source with the wavelength of 488 nm. the exact positions of the peaks (bands) in the raman spectrum were found by using a function findpeaks in matlab r2008b. the raman spectrum of the sample k2 is shown in the figure 3: figure 3. raman spectrum of k2 sample. the measured raman band at 478 cm−1 (black arrow) is coresponding to si-si bond in amorphous phase and 1448 cm−1 (red arrow) is coresponding to c-c amourphous bond. the raman band at 829 cm−1 (green arrow) coresponds to si-c bond. the low intesity of si-c peak is not due to the number of the bonds, but it follows from the generally small raman transition probability. the bands at 1005 cm−1, 2283 cm−1 and 2889 cm−1 (blue arrows) link to the signals of si-h and c-h bonds [2]. the raman spectrum of the sample k7 and k9 is shown in figure 4. according to [3], the peaks for tin are found at 250; 330-360 and 560 cm−1 and are marked by blue arrows. observed peaks might be, perhaps, assigned to the presence of tin in the deposited layer, however, the intensity of the peaks is too weak to provide a decisive prove for tin compound existence. the peaks marked by black arrows correspond to monocrystalline silicon [6]. 21 jakub skocdopole, lucrezia aversa, martin golan et al. acta polytechnica ctu proceedings figure 4. raman spectra of samples k7 and k9. 4.1.1. discussion the raman bands, for all samples, exhibit some shifts in their position, when compared with literature [2] [3]. this fact could be caused by some small variations of the stoichiometry of deposited films. for supposed application it is necessary to obtain well-defined grains of sic or tin. unfortunately for this aim the thin films of sic are amorphous. in order to be able to grow the polycrystalline sic layers, it is necessary to heat the substrate during the deposition process, the treatment that was not performed during the present depositions. it is not possible to decide whether or not the thin films of tin are really composed of pure tin only. or consist of some mixture of metallic ti, tin and titanium oxide. all these materials exhibit rather similar raman spectra [4] and, taking in account the small intensity of the spectra obtained from present measurements it is impossible to conclude about the nature of grown material. 4.2. xrd the glancing angle xrd analysis was performed on θ / θ diffractometer x'pert operating in braggbrentano geometry with x-ray source λ (cokα )=0,179026 nm. the xrd patterns obtained with the sample k7 (figure 5) show only amorphous halo. the amorphous halo is indicative of two facts, firstly that the film is thick enough that only the diffraction signal coming from the film is registered, and secondly that the structure of the films is amourphous in its nature. the xrd patterns obtained with sample k9 (figure 6) show only presence of austenitic steel. the result indicates that the film is not thick enough to stop the diffraction signal from the substrate and that the structure of film is amorphous. 4.3. sem the sem image of sample k2 (figure 7) contains particles with size under 500 nm. the film background is homogenous despite of fact that on its surface are particles. sic is very hard material and was expected to consist of separated particles figure 5. xrd patterns obtained with sample k7 figure 6. xrd patterns obtained with sample k9 figure 7. sem micrograph of sample k2: sic layer on aluminium alloy substrate. the tin was deposited on the stainless steel and monocrystalline silicon substrates. in sem image of sample k7 (figure 8) shows particles with size under 150 nm. the film is very homogenous, in agreement with its amorphous nature confirmed by xrd. the sem image of sample k9 (figure 9) shows particles under 250 nm. the film is amourphous, as confirmed by xrd. the red lines indicate the differencies in the film structure due to existence of underlying grain boundaries present in the polycrystalline substrate. 22 vol. 9/2017 preparing of the chameleon coating by the ion jet deposition method figure 8. sem micrograph of sample k7: tin film on si single crystal substrate. figure 9. sem micrograph of sample k9: tin layer on stainless steel substrate. 4.3.1. discussion all samples exhibit some type of particles on their surface. the particles differ from each other mostly in their size. the size of particles is important for improvement of the mechanical properties. the particles should not be too large because in such case the cracks through the coating could propagate also through the particle and even not too small because the crack of the matrix may avoid the particle just by circling around it. the smallest particles are observed on the tin film deposited on single crystalline silicon. the ideal size of the particles is found to be between tens and hundreds of nanometers [1]. figure 10. xps spectra recorded with samples k7 and k9; pe = 50 ev. 4.4. x-ray photoelectron spectroscopy the xps analysis was performed using the x-ray source working at the mgkalpha energy 1253.6 ev and the wsw analyzer that can be operated at different pass energy (pe), in order to collect spectra with different resolutions. in particular, the following settings were used: 1.) pe = 50 ev to acquiring the wide range spectra used in identification of the main chemical species on the surface 2.) pe = 20 ev to acquire single peak spectra with an intermediate resolution ideal to perform a quantitative analysis and 3.) pe = 10 ev to obtain single peak spectra at high resolution. the recorded wide range spectra are shown in figure 10. in the ti-n samples, the main chemical species on the surfaces are those attended, i.e. titanium (ti2p), nitrogen (n1s), oxygen (o1s), silicon (si2p), carbon (c1s) from contaminants and boron (b1s) from the pbn sample holder. the corresponding auger electrons lines, that are always present in a typical xps spectrum, are marked, too. the o1s and c1s peaks appear quite intense, in particular compared to the n1s peak that is expected to be stronger, even taking into account its low photoemission cross section: this suggests that the films could be strongly oxidized. spectra at pe=20 ev give more indication on oxidation processes together with the quantitative evaluation of surface atomic percentages, that are collected in table 2. there is a significant amount of carbon that is present in k samples: the atomic percentages here reported take into account any contribution from the sample holder that has been properly subtracted from the c1s peak, thus the carbon percentage relies only on carbon inside or over the films. the ti2p peak is centered at a be of 459ev, the value that is typical of titanium in high oxidation state bonded to oxygen, and shows a long tail at lower bes, usually related to lower valence states. the lineshape analysis (through voigt functions, considering a shirley background) put in evidence up to three contributions to the peak: the main one (light blue peak) is at higher be and can be correlated to tio2, the second one, centered at 457.5 ev, is out of the typical region of tin (that is at even lower binding 23 jakub skocdopole, lucrezia aversa, martin golan et al. acta polytechnica ctu proceedings sample % ti2p % n1s % o1s % c1s % si2p kuba7 13.2 3.3 38.5 38.2 6.8 kuba9 7.2 1.2 24.3 67.3 table 2. chemical composition obtained from xps experiments for the k7 and k9 samples. figure 11. xps spectrum close to ti 2p line for k7 and k9 samples. figure 12. xps spectrum courses close to o1s line observed for the k7 and k9 samples. energy) and could be assigned to a mixed ti-o-n phase (oxynitrides), while the third one at 455.4 ev is the tin contribution. its intensity is low compared to the tio2 phase, suggesting that the tin layer is few nanometers deeper: the ti2p escape length in tio2 is 2.12 nm, thus the signal from the nitride layer comes from about 6-8nm below the surface. the o1s spectra for all samples show the presence of a main contribution at about 530-530.5 ev and a less intense feature at higher binding energy. the lineshape analysis, however, reveals a third contribution at around 532 ev. the most intense peak at low be can be assigned to metal oxides, i.e. titanium oxides, while the peak at higher be is typically assigned to oh groups at the surface. taking into account the indications given figure 13. xps spectra close to n1s line observed for the k7 and k9 samples; experimental values (the noisy courses) and the fit curves are shown. for more details see text. by ti2p spectra, we can assume that this component together with the other o peak can be related to oxynitrides species. this assumption can be confirmed by looking at the n1s spectra (figure 13). each nitrogen core level can be reproduced by the peak at low be ( 396-397 ev, in blue and purple) that is assigned to the nitride layer, plus one or two components at higher be that can be reasonably correlated to the oxynitrides already found in the o1s lineshape analysis. 4.4.1. discussion the measurement has been performed before the sic film has been prepared. thus only tin film is analyzed. it was expected that the measured data would originate mostly from the oxidation layer on the surface of the sample. this assumption was confirmed. the xps does not prove unambiguously that the film is composed of tin only. it seem reasonable to state that the xps proves that ti and n species are present in the film, however they could be combined in some mixture of ti, tin and ti-o-n (oxynitrides) phases. 5. conclusions both films are composed of particles created during the deposition process, the feature which is necessary for their role in the chameleon coating. the deposition of particles from these materials were successful, however further research should be performed to ensure the reliable particle size control. the thickness of films is found to be in units of micrometres. both 24 vol. 9/2017 preparing of the chameleon coating by the ion jet deposition method tin and sic films are amorphous, as proven by raman spectroscopy and xrd. further research steps towards the chameleon layer preparation should be the deposition of mos2 films and the incorporation of the mos2 into dlc matrix and their characterisation. acknowledgements the authors are indebted to ing. gianpiero tedeschi, ceo, noivion srl, for providing the deposition technology for samples preparation and to the institute of materials for electronics and magnetism, cnr, trento for its hospitality, especially to the institute director dr. salvatore iannotta, and to the trento unit head dr. roberto verucchi. this work was supported by the grant agency of the czech technical university in prague, grant no. sgs16/245/ohk4/3t/14. references [1] a. a. voevodin, j. s. zabinski. supertough wear-resistant coatings with ‘chameleon’ surface adaptation. thin solid films 370: 223-231, 2000. [2] y. inoue, s. nakashima, a. mitsuishi. raman spectra of amorphous sic. solide state communations 48(12): 1071-1075, 1983. [3] w. spengler, r. kaiser. raman scattering, superconductivity, and phonon density of states of stoichiometric and nonstoichimetric tin. physical review b 17(3): 1095-1101, 1978. [4] r. j. nemanich, c. c. tsai, g. a. n. connell. interference-enhanced raman scattering of very thin titanium and titanium oxide films. physical review letters 44(4): 273-276, 1980. [5] j.skocdopole. preparation of thin layers by ijd method and characterization of their physical-chemical properties.prague. bachelor thesis. czech technical university in prague, faculty of nuclear sciences and physical engineering, 2015. [6] j.skocdopole. construction of system for deposition of thin films by ijd method and trial deposition of chosen materials..prague. research thesis. czech technical university in prague, faculty of nuclear sciences and physical engineering, 2016. [7] s.o. leathem,et al. influence of the injection speeds on the discharge characteristics and minimization of delay time in a pseudospark discharge. the open plasma physics journal 3: 20-27, 2010. [8] p. nozar. ionized jet deposition technique, a new class of thin film deposition equipment, vacuum symposium coventry, 16 october 2014, the united kingdom [9] s.tricot, et al. dynamics of a pulsed-electron beam induced plasma: application to the growth of zinc oxide thin ïňąlms journal of physics d 41(17): 10pp., 2008 [10] m.a. raadu, j.j.rasmussen. dynamical aspects of electrostatic double layers astrophysics and space science 144: 43-71, 1988 [11] yu. d. korolev, et al. electron beams generated at different stages of the pseudospark discharge, the 27th international conference on phenomena in ionized gase, eindhoven, 18-22 july 2005, the netherlands 25 acta polytechnica ctu proceedings 9:1–7, 2017 1 introduction 2 theory 2.1 ionized jet deposition 2.2 chameleon coating 3 experiment 4 results 4.1 raman spectroscopy 4.1.1 discussion 4.2 xrd 4.3 sem 4.3.1 discussion 4.4 x-ray photoelectron spectroscopy 4.4.1 discussion 5 conclusions acknowledgements references 127 acta polytechnica ctu proceedings 1(1): 127–131, 2014 127 doi: 10.14311/app.2014.01.0127 multifrequency behaviour of the gamma-ray binary system psr b1259-63: modelling the fermi flare brian van soelen1, pieter j. meintjes1 1department of physics, university of the free state, bloemfontein 9300, south africa corresponding author: vansoelenb@ufs.ac.za abstract this paper presents a brief overview of the multifrequency properties of the gamma-ray binary system psr b1259-63 from radio to very high energy gamma-rays. a summary is also presented of the various models put forward to explain the fermi “flare” detected in 2011. initial results are presented of a new turbulence driven model to explain the gev observations. keywords: gamma-ray binaries individual: psr b1259-63. 1 introduction there are only a handful of known gamma-ray binary systems. of these, it is only in psr b1259-63 that the nature of the compact object is known due to the detection of pulsed radio emission (johnston et al., 1992a). the very high energy (vhe) nature of the source was confirmed by the h.e.s.s. telescope around the 2004 periastron passage (aharonian et al., 2005). the gammaray binary system consists of a 48 ms pulsar, in an eccentric (e = 0.87) 3.4 year orbit around a be star (e.g. johnston et al., 1992, 1994), with a spin-down luminosity of ė = 8.3 × 1035 erg s−1 (e.g. wang et al., 2004). recent spectroscopic observations have placed better constraints on the parameters of the optical companion, ls 2883, and the binary system (negueruela et al., 2011). in this paper, we present an overview of the multifrequency behaviour of psr b1259-63, and discuss some of the modelling undertaken to explain the large “flare” event detected by fermi after the previous periastron passage. 2 multifrequency observations in this section we summarize the multifrequency behaviour of the non-thermal emission originating from psr b1295-63, discussing the radio, x-ray, vhe gamma-ray and, finally, the gev gamma-ray observations. 2.1 radio behaviour psr b1259-63 was originally detected as a radio pulsar during a galactic plane survey undertaken with the 64 m parkes radio telescope (johnston et al., 1992b). observations around periastron showed that there was an increase (and variability) in the dispersion measurement of the pulsed signal and an eclipse of the pulsed signal between approximately 20 days before periastron to 20 days after (e.g. johnston et al., 1996, 1999, 2001). significantly, around periastron an unpulsed and variable radio emission was detected with a flux density of 10 − 30 mjy, higher than the flux of the pulsed signal (2 − 3 mjy). these observations are explained by the pulsar passing through and/or behind the circumstellar disc of the be star, and the formation of synchrotron emission in the pulsar wind nebula. more recently a large extended pulsar wind nebula has also been reported around periastron by moldón et al., (2011). 2.2 x-ray behaviour a non-thermal x-ray component has been detected from psr b1259-63 across the whole of the orbit, with early detections determining a luminosity of l ∼ 1034 erg s−1 around periastron (kaspi et al., 1995). combined asca, chandra, xmm -newton, bepposax, swift and suzaku observations covering the 1997 – 2010 periastron passages have shown a consistent x-ray light curve (see chernyakova et al., 2006, 2009, abdo et al., 2011, and references therein). these datasets have presented particular coverage focused on the disc crossing epochs. the observations show that the x-ray emission peaks within two narrow time bands most likely associated with the pulsar approaching the circumstellar disc. pavlov et al., (2011) also reported on an extended x-ray structure detected by chandra near apastron. the observations in the 0.5–8 kev en127 http://dx.doi.org/10.14311/app.2014.01.0127 brian van soelen, pieter j. meintjes ergy band showed an elongated structure (∼ 4′′) with a luminosity of ∼ 1032 erg s−1 (assuming a distance of 3 kpc). it is likely that this is associated with the pulsar wind nebula outflow. 2.3 vhe behaviour psr b1259-63 was detected for the first time at vhe with the h.e.s.s. telescope during the 2004 periastron passage (aharonian et al., 2005). the observations showed a variable light curve with an implied maximum flux a few days before and after periastron. the system has since been detected during 2007 (aharonian et al., 2009) and 2011 (abramowski et al., 2013), albeit with much less coverage. the h.e.s.s. observations appear to be consistent with the double peak structure observed at x-ray and radio wavelengths, but this conclusion is not definitive due to lower coverage during the pre-periastron approach of the pulsar. the spectrum of the vhe emission also appears to be consistent with a single power-law distribution, with no cut-off in the spectrum (see e.g. fig. 4 in abramowski et al., 2013). while the coverage over the last periastron passage was poor, the 2011 observations were coincident with the fermi “flare” discussed in the next section. unlike the fermi detection, the h.e.s.s. observations showed no significant change between the preand post-flare event, and morphologically the gev to tev energies are not consistent with a single power-law distribution (see fig. 5 in abramowski et al., 2013). 2.4 he behaviour due to the consistency of the radio, x-ray and vhe light curves, it was presumed (before 2010/2011) that fermi would observe similar behaviour. in fact, it was not actually clear whether the system would be detectable by fermi (e.g. chernyakova et al., 2009). the gamma-ray detection and rapid transient behaviour that were reported by fermi were completely unexpected. as reported by abdo et al. (2011), the system was relatively undetected before periastron, with a faint “brightening” phase which began around the point of the first disc crossing and lasted until ∼ 18 days after periastron. however, approximately 30 days after periastron, there was a rapid increase in the detected emission from the source showing an average flux of f (> 100mev) = (4.4±0.3stat±0.7sys)×10−10 erg cm−2 s−1, with a photon index of γ = (1.4±0.6stat±0.2sys) and a cutoff energy ec = (0.3±0.1stat±sys) gev. this “flare” was detected until > 60 days after periastron. significantly, radio, x-ray, and vhe observations showed no unusual or flaring events. most surprisingly, the daily binned light curve showed a peak luminosity of lγ ≈ 8 × 1035 erg s−1 (for isotropic emission at an assumed distance of 2.3 kpc), corresponding to ≈ 100 per cent of the spin-down power of the pulsar. the emission detected by fermi has proved difficult to reconcile with models of the system. in the next section we discuss some of the models pertaining to gev energies and the fermi flare. 3 modelling the fermi flare 3.1 effect of the infrared excess in anticipation of the fermi observations of psr b125963, van soelen & meintjes (2011), van soelen et al. (2012) and meintjes & van soelen (2012), considered the influence the infrared flux from the circumstellar disc of the be star would have on gamma-ray production. if the same population of electrons which produces the vhe emission through inverse compton scattering of the optical photons, scatters the infrared photons from the disc, it will produce emission in the gev energy range. first using an isotropic approximation (van soelen & meintjes, 2011) and then a full anisotropic approximation, which took into account the anisotropic inverse compton scattering as well as the changing flux from the circumstellar disc as measured from the pulsar’s position (van soelen et al., 2012), we showed that the scattering of the infrared photons would increased the flux at gev energies by a factor of 2. while it was thought that the large size of the circumstellar disc would result in it dominating near the disc crossing, we found that the low density of the disc mitigated this effect as the majority of the infrared emission occurred near the star and not far out in the disc. however, the flux was below what was detected by fermi. 3.2 cold pulsar wind khangulyan et al., (2012) proposed that the scattering of the cold pulsar wind (γ = 104) off photons from the circumstellar disc, after the second disc passage, could produce the observed fermi flare. the authors propose that the shock-front around the pulsar is confined within the disc, and after the pulsar leaves the circumstellar disc the opening of the shock structure will allow the inverse compton scattering of the cold pulsar wind to produce the flare. one problem presented by this model is the number of additional photons required to do this. the authors estimate that the additional photon distribution must have a luminosity of approximately 40 per cent of the stellar luminosity. this does not appear to be consistent with the observations obtained around periastron nor with the estimation of the available energy from shock-heating (van soelen et al., 2012). however, it must be cautioned that the reported observations were not undertaken at the same time as 128 multifrequency behaviour of the gamma-ray binary system psr b1259-63: modelling the fermi flare the fermi flare and new observations around the next periastron passage must be obtained, to obtain better constraints. 3.3 sph modelling a process of smooth particle hydrodynamic (sph) modelling of psr b1259-63 was undertaken by takata et al., (2012) to model the behaviour of the be star’s circumstellar disc around periastron. the simulations show that the disc should be considerably disrupted during the pulsar crossing. however, observations on 5 january 2011, approximately three weeks after periastron, showed that the mid-infrared flux was consistent with previous observations (see van soelen et al., 2012). this suggests that either the disc was not dramatically effected, or that there was a rapid recovery. in addition, the approximation of the emission light curve, while in agreement with the x-ray emission, was not in agreement with the gev light curve, as the simulations suggested that the maximum emission should occur before periastron (see figs. 3 and 5 in takata et al., 2012). 3.4 doppler boosting emission the most recent model which has been suggested is that the synchrotron emission is doppler boosting to gev energies to produce the observed flare. this was modelled in detail by kong et al. (2012). the authors consider two emission regions along the shock front: the first near the apex with a bulk lorentz factor of γ = 1 and the second along the shock tail which is mildly relativistic (γmax ≈ 2) and is beamed along the shock. these simulations are able to account for the fermi detection during the flare period, but are not so successful during the pre-periastron period – though it should be noted that the pre-periastron detections have a much lower significance. the light curve predictions also suggest only a single peaked emission around periastron for the gev energies, and a double peaked structure from the x-ray and vhe emission. however, the modelled light curves predict a higher flux for the gev and tev emission around periastron (see fig. 5 in kong et al., 2012), an effect which is not observed. 3.5 turbulence driven emission? thus far all models have presented unique problems in modelling the fermi flare. for this reason it is still necessary to consider alternative models. below we consider the possibility of a turbulence induced flare. hydrodynamical simulations of colliding wind systems have shown that kelvin-helmoltz instabilities develop along the dividing line between the pulsar and stellar winds (see e.g. bosch-ramon et al., 2012). if these instabilities form a turbulent medium, it may be possible for secondary particle acceleration to occur due to second-order fermi acceleration (see e.g. bosch-ramon & rieger 2012). it has been considered by a number of authors that under the effect of radiative cooling and second-order fermi acceleration, a maxwellian-like distribution will form (see e.g. schlickeiser 1985 for a discussion of firstand second-order acceleration with radiative cooling). such a secondary distribution of electrons may be responsible for producing the gev emission in psr b1259-63 if acceleration in the turbulent region occurs around the second disc crossing. as a first approximation we consider the modified maxwellian distribution suggested by stawarz & petrosian (2008), given by ne = n0γ 2 exp [ −1 a ( γ γeq )a] , (1) where a = 3 − q for dominant synchrotron/thomsonlimit inverse compton cooling, or a = 1.5− q for dominant klein-nishina inverse compton cooling. here q is the index of the turbulence power-law, and γeq is determined by equating the appropriate radiative cooling time to the acceleration time (see stawarz & petrosian, 2008, and reference therein, for details related to the acceleration). we calculate the best fit inverse compton emission for the electron distribution given by equation (1) for isotropic scattering (e.g. blumenthal & gould, 1970), with a blackbody distribution of photons (t? = 33 000 k). in this first approximation an isotropic radiation field has been assumed. the equilibrium energies required to fit the maxwellian distributions (equation 1) were found to be γeq = 1614.4 for the bohr approximation (q = 1), γeq = 656.30 for the hard-sphere approximation (q = 2), γeq = 1030.4 for the kolmogorov spectrum (q = 5/3) and γeq = 1196.7 for the kraichnan spectrum (q = 3/2). only a = 3 − q was considered. a constant factor was applied to match the flux level of the flare. the resulting fits are shown in fig. 1. the figure shows that the distribution produces a reasonable fit to the resulting fermi detection. initial considerations of the parameter space suggest that it may be possible to accelerated electrons to the appropriate energies around the period of periastron. a more detailed analysis is currently under-way. 129 brian van soelen, pieter j. meintjes -12 -11 -10 7 8 9 10 11 lo g ν f ν [e rg s -1 c m -2 ] log energy [ev] q=2 q=1 q=5/3 q=3/2 figure 1: inverse compton spectrum formed by a modified maxwellian electron distribution fitted to the post-periastron fermi flare detection. references [1] abdo, a.a., ackermann, m., ajello., m. et al.: 2011, apj, 736, l11 doi:10.1088/2041-8205/736/1/l11 [2] aharonian, f., et al. (h.e.s.s. collaboration): 2005, a&a, 442, 1 [3] aharonian, f., et al. (h.e.s.s. collaboration): 2009, a&a, 507, 389 [4] abramowski, a., et al. (h.e.s.s. collaboration): 2013, a&a, 551, a94 [5] blumenthal, g.r., gould, r.j.: 1970, reviews of modern physics, 42, 237 [6] bosch-ramon, v., rieger f.m.: 2012, in astroparticle, particle, space physics and detectors for physics applications proceedings of the 13th icatpp conference.. g. simone et al. (eds.), 219 [7] bosch-ramon, v., barkov, m.v., khangulyan, d., et al.: 2012, a&a, 544, 59 [8] chernyakova, m., neronov a., lutovinov a., et al.: 2006, mnras, 367, 1201 doi:10.1111/j.1365-2966.2005.10039.x [9] chernyakova, m., neronov, a., aharonian f., et al.: 2009, mnras, 397, 2123 doi:10.1111/j.1365-2966.2009.15116.x [10] johnston, s., manchester, r.n., lyne, a.g, et al.: 1992a, apj, 387, 37 [11] johnston, s., lyne, a.g, manchester, r.n., et al.: 1992b, mnras, 255, 401 [12] johnston, s., manchester, r.n., lyne, a.g, et al.: 1994, mnras, 268, 430 [13] johnston, s., manchester, r.n., lyne, a.g, et al.: 1996, mnras, 279, 1026 [14] johnston, s., manchester, r.n., mcconnel, d.: 1999, mnras, 302, 277 [15] johnston, s., wex, n., nicastro, l., et al.: 2001, mnras, 326, 643 [16] kaspi, v. m., tavani m., nagase f., et al.: 1995, apj, 453, 424 doi:10.1086/176403 [17] khangulyan, d., aharonian, f.a., bogovalov, s.v., et al.: 2012, apj, 752, l17 doi:10.1088/2041-8205/752/1/l17 [18] kong, s. w., cheng, k. s., huang, y. f.: 2012, apj, 753, 127 doi:10.1088/0004-637x/753/2/127 [19] meintjes, p.j., van soelen, b.: 2012, in multifrequency behaviour of high energy cosmic sources, f. giovannelli, l. sabau-graziati (eds.) mem. s.a.it., 83, 246 [20] moldón j., johnston s., ribó m., et al.: 2011, apj, 732, l10 [21] negueruela i., ribó m., herrero a., et al.: 2011, apj, 732, l11 [22] pavlov g. g., chang c., kargaltsev o.: 2011, apj, 730, 2 [23] schlickeiser, r.: 1985, a&a, 143, 431 [24] stawarz, l., petrosian, v.: 2008, 681, 1725 [25] takata, j., okazaki, a. t., nagataki, s. et al.: 2012, apj, 750, 70 [26] van soelen, b., meintjes, p.j.: 2011, mnras, 412, 1721 [27] van soelen, b., meintjes, p.j., odendaal, a., et al.: 2012, mnras, 426, 3135 [28] wang, n., johnston, s., manchester, r. n.: 2004, mnras, 351, 599 discussion carlotta pittori: in august 2010 agile reported the detection of gamma-ray activity above 100 mev from the psr b1259-63 region during the initial approach-to-periastron part of the orbit. fermi did not confirm this detection, but later in november reported faint gamma-ray emission before the big 2011 flare. are you aware of the agile detection and can the model explain a ∼ 100 mev emission just before the disk passage? 130 http://dx.doi.org/10.1088/2041-8205/736/1/l11 http://dx.doi.org/10.1111/j.1365-2966.2005.10039.x http://dx.doi.org/10.1111/j.1365-2966.2009.15116.x http://dx.doi.org/10.1086/176403 http://dx.doi.org/10.1088/2041-8205/752/1/l17 http://dx.doi.org/10.1088/0004-637x/753/2/127 multifrequency behaviour of the gamma-ray binary system psr b1259-63: modelling the fermi flare brian van soelen: yes i am aware of the reported agile detection, as well as the fermi follow-up analysis that did not detect emission. at this point i do not believe any model has completely accurately modelled the events that occurred around the previous periastron passage, including the reported detection by agile. 131 introduction multifrequency observations radio behaviour x-ray behaviour vhe behaviour he behaviour modelling the fermi flare effect of the infrared excess cold pulsar wind sph modelling doppler boosting emission turbulence driven emission? 26 acta polytechnica ctu proceedings 2(1): 26–32, 2015 26 doi: 10.14311/app.2015.02.0026 the space density of magnetic and non-magnetic cataclysmic variables, and implications for cv evolution m. l. pretorius 1department of physics, university of oxford, denys wilkinson building, keble road, oxford ox1 3rh, united kingdom 2previous address: school of physics and astronomy, university of southampton, highfield, southampton so17 1bj corresponding author: retha.pretorius@astro.ox.ac.uk abstract we present constraints on the space densities of non-magnetic and magnetic cataclysmic variables, and discuss some implications for models of the evolution of cvs. the high predicted non-magnetic cv space density is only consistent with observations if the majority of these systems are extremely faint in x-rays. the data cannot rule out the very simple model where long-period ips evolve into polars and account for the entire short-period polar population. the fraction of wds that are strongly magnetic is not significantly higher for cv primaries than for isolated wds. finally, the space density of ips is high enough to explain the bright, hard x-ray source population seen in the galactic centre. keywords: cataclysmic variables dwarf novae nova-likes intermediate polars polars x-rays. 1 introduction there are many remaining uncertainties in the theory of cataclysmic variable (cv) formation and evolution, as well as several serious discrepancies between predictions and the properties of the observed cv population (e.g. patterson 1998; pretorius, knigge & kolb 2007a; pretorius & knigge 2008a,b; knigge, baraffe & patterson 2011). in order to constrain evolution models, we require more precise observational constraints on the properties of the galactic cv populations. a fundamental parameter predicted by evolution theory, that should be more easily measured than most properties of the intrinsic cv population, is the space density, ρ. a few specific, important open questions concerning the formation and evolution of cvs are: (i) is the large predicted population of non-magnetic cvs at short orbital period consistent with the current observed cv sample? (ii) is there an evolutionary relationship between ips and polars? (iii) can the intrinsic fraction of mcvs be reconciled with the incidence of magnetic wds in the isolated wd population? (iv) do mcvs dominate the total galactic x-ray source populations above lx ∼ 1031 ergs−1? these questions can be addressed empirically, with reliable measurements of the space densities of the different populations of cvs. uncertainty in ρ measurements is in part caused by statistical errors, resulting from uncertain distances and small number statistics. however, the dominant source of uncertainty is most likely systematic errors caused by selection effects. fig. 1 shows some reported measurements (differing by several orders of magnitude for non-magnetic cvs). selection effects are most easily accounted for in samples with simple, well-defined selection criteria. in the absence of a useful volume-limited cv sample, a purely flux-limited sample is the most suitable for measuring ρ. whereas optical cv samples always include selection criteria based on, e.g., colour or variability, there are x-ray selected cv samples that are purely flux-limited. all active cvs show x-ray emission generated in the accretion flow. furthermore, mcvs are luminous x-ray sources, while the correlation between the ratio of optical to x-ray flux and the optical luminosity of non-magnetic cvs, implies that an x-ray flux limit does not introduce as strong a bias against shortperiod cvs as an optical flux limit (e.g. van teeseling et al. 1996). here we use 2 x-ray surveys, the rosat bright survey (rbs; e.g. schwope et al. 2002), and the rosat north ecliptic pole (nep) survey (e.g. henry et al. 2006) to construct x-ray flux-limited cv samples. we then provide robust observational constraints on the space densities of both magnetic and non-magnetic cvs, by carefully considering the uncertainties involved. 26 http://dx.doi.org/10.14311/app.2015.02.0026 the space density of magnetic and non-magnetic cataclysmic variables, and implications for cv evolution figure 1: some previously reported measurements of the space densities of different cv populations. we provide additional background on the questions listed above in section 2, present the measurements in section 3, discuss the implications of the results in section 4, and finally list the conclusions in section 5. 2 context 2.1 missing non-magnetic cvs it is not clear whether the present-day observed nonmagnetic cv population is inconsistent with theoretical expectations. population synthesis models predict that only ' 1 percent of all cvs are long-period systems (see e.g. kolb 1993). the the vast majority of cvs should therefore be intrinsically faint. pretorius et al. (2007a) and pretorius & knigge (2008b) used a specific model of kolb (1993), together with models of the outburst properties and seds of cvs, to show that, although observed cv samples are strongly biased against shortperiod systems, a currently undetected faint cv population cannot dominate the overall population to the extent predicted by this particular population synthesis model. knigge et al. (2011) used the properties of cv donor stars to conclude that the aml rate is lower above the gap and higher below the gap than predicted by the standard model. this leads to larger predicted factions of both period bouncers and long-period systems. whether this is consistent with observed cv samples is not yet known. that a large faint population of cvs exists is now clear from observations (gansicke et al. 2009; patterson 2011). however, whether observations have truly revealed a population as large as predicted remains to be seen. some predicted values of the non-magnetic cv space density are as high as 2 × 10−4 pc−3 (de kool 1992; kolb 1993); most observational estimates are much lower, but values ranging from ≤ 5×10−7pc−3 to ρ ∼ 10−4pc−3 have been reported. perhaps the most straight forward test of these predictions is to compare them to the measured space density of the galactic short-period, non-magnetic cv population. 2.2 evolutionary relationship between ips and polars in most regards, the formation and evolution of magnetic and non-magnetic cvs is believed to be similar. both types of cvs form via common envelope (ce) evolution, evolve initially from long to short porb as a result of angular momentum loss (aml), and eventually experience period bounce, when the thermal timescale of the donor becomes longer than the mass transfer time-scale. the main proposed difference between the evolution of mcvs and non-magnetic cvs actually affects only the polars, where magnetic braking (mb) is thought to be suppressed because of the very strong wd magnetic field (e.g. li & wickramasinghe 1998; townsley & gansicke 2009). the porb distributions of magnetic and non-magnetic cvs are broadly consistent with these ideas. considering polars and ips together, their porb distribution is very similar to that of non-magnetic cvs, showing a period gap in the range 2 hr<∼porb <∼ 3 hr, as well as a period minimum at around porb ' 80 min (see fig. 2). it has long been recognized that most ips are found above the period gap and most polars below (fig. 2)., which immediately suggests that ips may evolve into polars (e.g. chanmugam & ray 1984). physically this makes sense, since smaller orbital separation and lower ṁ (besides large magnetic field strength) favour synchronization. 27 m. l. pretorius figure 2: the orbital period distribution of all cvs (black), and mcvs (green). cumulative distributions are also shown for polars (red) and ips (blue). almost all ips are found at long porb, while most polars are short-porb systems. periods from ritter & kolb (2003). mb drives much higher mass-transfer rates above the period gap than gravitational radiation (gr) does below the gap; therefore, it is plausible that many accreting magnetic wds may only become synchronized after crossing the period gap. the main problem with this scenario is that the magnetic fields of the wds in ips (bip <∼ 10mg) are systematically weaker than those of the wds in polars (bpolar ∼ 10− 100mg). there are several possible solutions to this problem. perhaps the most simple (in terms of binary star evolution) is that the high accretion rates in ips partially “bury” the wd magnetic fields, so that the observationally inferred field strengths for these systems are systematically low (cumming 2002). it is also possible that the short-period polar population is dominated by systems born below the period gap. of course this does not explain why we observe so few short-period ips, although it may be that longperiod ips become unobservable once they reach short periods (see patterson 1994; wickramasinghe, wu & ferrario 1991). a way to investigate the relationship between ips and polars is to compare their respective space densities. for example, if all long-period ips evolve into short-period polars, and all short-period polars form out of of long-period ips, then their space densities should be proportional to the evolutionary time-scale associated with these two evolutionary phases. in this particular example, we would predict that ρpolar/ρip ' τgr/τmb >> 1. 2.3 intrinsic fraction of mcvs magnetic systems make up ' 20% of the known cv population (ritter & kolb 2003). taken at face value, this is a surprisingly high fraction, considering that the strong magnetic fields characteristic of ips and polars (b>∼ 106 g) are found in only ' 10% of isolated wds (e.g. kulebi et al. 2009). if these numbers really represent the intrinsic incidence of magnetism amongst cvs and single wds, the difference between them would have important implications, namely that either strong magnetic fields favour the production of cvs, or that some aspect of pre-cv evolution favours the production of strong magnetic fields (see e.g. tout et al. 2008). however, it is in reality not yet clear that magnetism is more common in cv primaries than in isolated wds. the main problem is that the observed fraction of magnetic systems amongst known cvs is almost certainly affected by serious selection biases. for example, since mcvs are known to be more luminous in x-rays than non-magnetic cvs, they are likely to be over-represented in x-ray-selected samples. conversely, polars, in particular, are relatively faint in the optical band (since they do not contain optically bright accretion disks), so they are likely to be under-represented in optically-selected samples. given that the overall cv sample is a highly heterogeneous mixture of x-ray, opticaland variability-selected sub-samples (which also typically lack clear flux limits), it is very difficult to know how the observed fraction of mcvs relates to the intrinsic fraction of magnetic wds in cvs. 28 the space density of magnetic and non-magnetic cataclysmic variables, and implications for cv evolution 2.4 galactic x-ray source populations several studies have attempted to determine the makeup and luminosity function of galactic x-ray source populations in different environments, including the milky way as a whole, the galactic centre, the galactic ridge, and globular clusters. remarkably, in all of these environments, mcvs have been proposed as the dominant population of x-ray sources above lx >∼ 1031ergs−1. in most of these studies, identifying the observed xray sources with distinct populations is very uncertain, since few of the sources have either optical counterparts or properties that allow for clear classification. the classification of observed sources rely mainly on x-ray luminosities and hardness, and statistical comparisons of observed and expected number counts. the local space densities of the relevant physical populations are likely the most important aspect of these comparisons. in effect, the relevant question is whether the extrapolation of the local space density to the environment being investigated can account for the number of sources observed there. in the case of mcvs, such extrapolations are difficult, mainly because the local space densities are quite poorly known. 3 calculating space densities 3.1 the flux-limited samples the rbs covers |b| > 30◦ to fx >∼ 10−12erg cm−2s−1, and includes 16 non-magnetic cvs, and 30 mcvs (6 ips and 24 polars). the nep covers 81 sq.deg. to fx >∼ 10−14. only 4 cvs where detected in the nep, all of them non-magnetic. the samples are presented in pretorius et al. (2007b), pretorius & knigge (2012), and pretorius et al. (2013). 3.2 the method we use the 1/vmax method (e.g. stobie et al. 1989) together with a monte carlo simulation designed to sample the full parameter space allowed by the data, as described in pretorius et al. (2007b) and pretorius & knigge (2012). we tested the method to verify that it gives reliable error estimates, and also considered various possible systematic biases (pretorius & knigge 2012; pretorius et al. 2013). 3.3 results 3.3.1 probability distribution functions the distributions of mid-plane ρ values, normalized to give probability distribution functions, from the simulations are shown in fig. 3. the best-estimate midplane space densities are 4+6 −2 × 10−6 pc−3 for nonmagnetic cvs, and 8+4 −2 × 10−7 pc−3 for mcvs. for the 2 classes of mcvs, we find 3+2 −1 × 10−7 pc−3 for ips and 5+3 −2 × 10−7 pc−3 for polars. 3.3.2 upper limits on ρ of undetected populations the ρ estimates assume that the detected populations are representative of the intrinsic populations, in that they contain at least 1 of the faintest systems present in the intrinsic populations. it is possible that even large populations of sources at the faint ends of the luminosity functions can go completely undetected in flux-limited surveys. we performed additional monte carlo simulations to place limits on the sizes of faint populations of cvs that could escape detection in the surveys we have used (see pretorius & knigge 2012; pretorius et al. 2013). fig. 4 shows the maximum allowed ρ as a function of lx , separately for possible undetected nonmagnetic, polar and ip populations. specifically, if ρn−m = 2×10−4 pc−3 (at the high end of the predicted range), we require that the majority of non-magnetic cvs have lx <∼ 4 × 1028 erg s−1. a population of undetected polars with a space density as high as 5× the measured ρpolar must have lx <∼ 1030 ergs−1. a hidden population of ips can only have ρ = 5 × ρip if it consists of systems with x-ray luminosities fainter than 5× 1030 ergs−1. 4 discussion 4.1 missing non-magnetic cvs we discuss our measured ρn−m, as well as the upper limit, in the context of the predicted (i) large total space density of non-magnetic cvs, and (ii) large predicted fraction of normal short-period cvs and period bouncers. population synthesis models predict that only a few percent of all cvs are above the period gap (kolb 1993 finds less than 1%, while knigge et al. 2011 predict 3%). although we find that long-period systems account for just over 50% of our total ρn−m, the data cannot rule out these theoretical predictions. for example, using the knigge et al. (2011) fraction of longperiod systems, and assuming that we have not significantly under-estimated the space density of longperiod cvs, the space density of short-period cvs is ' 2 × 10−6 pc−3(97/3) ' 6 × 10−5 pc−3. the upper limit on ρn−m from section 3.3.2 then implies that a short-period cv population of this size could escape detection in the two surveys, as long as these systems have lx <∼ 8 × 1028 erg s−1 (for the simple case of a hypothetical single-lx population of faint, undetected cvs). the predicted ρ = 2 × 10−4 pc−3 would require that most cvs have x-ray luminosities below lx = 4× 1028 erg s−1. 29 m. l. pretorius figure 3: the ρ distributions for non-magnetic cvs (left-hand panel) and mcvs (right-hand panel) resulting from our simulations. solid lines in both panels mark the modes, medians, and means of the distributions; dashed lines show 1-σ intervals. the probability distribution functions shown in the inset are for the whole mcv sample, polars alone (red), and ips alone (blue). reproduced from pretorius & knigge (2012) and pretorius, knigge & schwope (2013). figure 4: the upper limit on ρ as a function of x-ray luminosity for undetected populations of cvs. the left-hand panel is for non-magnetic cvs, and the right-hand panel for ips (blue) and polars (red). in the lefthand panel, the 2 upper, fine histograms show the corresponding results for the rbs (middle) and nep (top) surveys alone. note that the assumed x-ray spectra of non-magnetic cvs, polars, and ips are different, hence the different slopes. reproduced from pretorius & knigge (2012) and pretorius et al. (2013). 4.2 evolutionary relationship between ips and polars if one assumes that long-period ips are the only progenitors of short-period polars, and that all ips become polars after crossing the period gap, then the ratio of the space densities of long-porb ips and short-porb polars (ρip,lp and ρpolar,sp) will simply reflect the ratio of evolutionary time-scales. the observed logarithm of this ratio is log (ρpolar,sp/ρip,lp) = 0.32 ± 0.36. if the evolution of long-period ips is driven by mb, while that of short-period polars is driven by gr alone, the evolutionary time-scale of short-period polars should be >∼ 5× that of long-period ips (e.g. knigge et al. 2011). this is completely consistent with the ratio of the inferred space densities. in fact, at 2-σ, the uncertainties are large enough to allow both ratios exceeding 10 and ratios below one. this means that, with the best existing space density estimates for polars and ips, we cannot strongly constrain the evolutionary relationship between these two classes. nevertheless, it is interesting to note that the simplest possible model, in which short-period polars derive from long-period ips and all ips become polars, is not ruled out by their observed space densities. 30 the space density of magnetic and non-magnetic cataclysmic variables, and implications for cv evolution 4.3 intrinsic fraction of mcvs combining the space density estimates of magnetic and non-magnetic cvs to estimate the intrinsic fraction of mcvs, we find log(fmcv ) = −0.80+0.27 −0.36. this is consistent, within the considerable uncertainties, with the fraction of isolated wds that are strongly magnetic . furthermore, it is possible that the x-ray-selected cv sample is less complete for non-magnetic cvs than for mcvs. therefore, the incidence of magnetism is not obviously higher amongst cv primaries compared to isolated wds. 4.4 galactic x-ray source populations we consider if it is plausible that ips dominate x-ray source populations above lx ' 1031ergs−1, taking the galactic centre as an example. the deep chandra survey of muno et al. (2009) includes ' 9000 sources down to lx ' 1031 ergs−1, in an area of ' 10−3deg2. approximating the volume covered by the survey as a sphere of radius 150 pc, the space density of x-ray sources in the galactic centre is ρx,gc ∼ 6×10−4 pc−3, compared to the local ip space density of ρip ∼ 3 × 10−7 pc−3. the stellar space density in the galactic centre is ' 1600× higher than in the solar neighborhood. thus these densities are consistent, and we conclude that most of the x-ray sources seen in the galactic centre can indeed be explained as ips. 5 conclusions assumming that the cv samples from the rbs and nep surveys are representative of the intrinsic populations (in the sense that we detected at least one system at the faintest ends of the luminosity functions of those populations), we find ρn−m = 4+6 −2 × 10−6 pc−3 and ρmcv = 8+4 −2×10−7 pc−3 (ρpolar = 5+3 −2×10−7 pc−3 and ρip = 3+2 −1 × 10−7 pc−3). the data allow for more than half of non-magnetic cvs having 28.7 < log(lx/erg s−1) < 29.7, and being undetected. however, to reach ρn−m = 2 × 10−4 pc−3 (at the high end of the predicted range), the data requires that the majority of non-magnetic cvs have lx <∼ 4× 1028 erg s−1. the ratio of the space densities of short-period polars to long-period ips is consistent with the simple hypothesis that long-period ips evolve into short-period polars, giving rise to the entire short-period polar population. existing data cannot rule out that strongly magnetic wds have the same incidence amongst cvs as in the field. taking into account the difference in stellar density, the measured local space density of ips can account for the number of bright x-ray sources detected in the galactic centre. acknowledgement i thank the organizes for a successful meeting, and for inviting me to present this review. references [1] chanmugam g., ray a.: 1984, apj, 285, 252 [2] cumming a.: 2002, mnras, 333, 589 doi:10.1046/j.1365-8711.2002.05434.x [3] de kool m.: 1992, a&a, 261, 188 [4] gänsicke b. t., et al.: 2009, mnras, 397, 2170 doi:10.1111/j.1365-2966.2009.15126.x [5] henry j.p., et al.: 2006, apjs, 162, 304 doi:10.1086/498749 [6] knigge c.: 2006, mnras, 373, 484 doi:10.1111/j.1365-2966.2006.11096.x [7] knigge c., baraffe i., patterson j.: 2011, apjs, 194, 28 doi:10.1088/0067-0049/194/2/28 [8] kolb u.: 1993, a&a, 271, 149 [9] külebi b., et al.: 2009, a&a, 506, 1341 [10] li j., wickramasinghe d. t.: 1998, mnras, 300, 718 [11] muno m. p., et al.: 2009, apjs, 181, 110 [12] patterson j.: 1984, apjs, 54, 443 [13] patterson j.: 1994, pasp, 106, 209 [14] patterson j.: 1998, pasp, 110, 1132 [15] patterson j.: 2011, mnras, 411,2695 doi:10.1111/j.1365-2966.2010.17881.x [16] pretorius m. l., knigge c.: 2012, mnras, 419, 1442 doi:10.1111/j.1365-2966.2011.19801.x [17] pretorius m. l., knigge c.: 2008a, mnras, 385, 1471 [18] pretorius m. l., knigge c.: 2008b, mnras, 385, 1485 [19] pretorius m. l., knigge c., kolb u.: 2007a, mnras, 374, 1495 [20] pretorius, m. l., knigge, c., schwope, a. d.: 2013, mnras, 432, 570 doi:10.1093/mnras/stt499 [21] pretorius m. l., et al.: 2007b, mnras, 382, 1279 doi:10.1111/j.1365-2966.2007.12461.x 31 http://dx.doi.org/10.1046/j.1365-8711.2002.05434.x http://dx.doi.org/10.1111/j.1365-2966.2009.15126.x http://dx.doi.org/10.1086/498749 http://dx.doi.org/10.1111/j.1365-2966.2006.11096.x http://dx.doi.org/10.1088/0067-0049/194/2/28 http://dx.doi.org/10.1111/j.1365-2966.2010.17881.x http://dx.doi.org/10.1111/j.1365-2966.2011.19801.x http://dx.doi.org/10.1093/mnras/stt499 http://dx.doi.org/10.1111/j.1365-2966.2007.12461.x m. l. pretorius [22] ritter h., kolb u.: 2003, a&a, 404, 301 [23] schwope a.d., et al.: 2002, a&a, 396, 895 [24] tout c. a., et al.: 2008, mnras, 387, 897 doi:10.1111/j.1365-2966.2008.13291.x [25] townsley d. m., gänsicke b. t.: 2009, apj, 693, 1007 doi:10.1088/0004-637x/693/1/1007 [26] wickramasinghe d. t., wu k., ferrario l.: 1991, mnras, 249, 460 doi:10.1093/mnras/249.3.460 [27] warner b.: 1987, mnras, 227, 23 [28] van teeseling a., beuermann k., verbunt f.: 1996, a&a, 315, 467 32 http://dx.doi.org/10.1111/j.1365-2966.2008.13291.x http://dx.doi.org/10.1088/0004-637x/693/1/1007 http://dx.doi.org/10.1093/mnras/249.3.460 introduction context missing non-magnetic cvs evolutionary relationship between ips and polars intrinsic fraction of mcvs galactic x-ray source populations calculating space densities the flux-limited samples the method results probability distribution functions upper limits on of undetected populations discussion missing non-magnetic cvs evolutionary relationship between ips and polars intrinsic fraction of mcvs galactic x-ray source populations conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0038 acta polytechnica ctu proceedings 7:38–42, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app uhpc sandwich structures with composite coating under compressive load jan markowski∗, ludger lohaus institut für baustoffe, leibniz universität hannover, appelstraße 9a, 30167 hannover, germany ∗ corresponding author: j.markowski@baustoff.uni-hannover.de abstract. ultra-high-performance concrete (uhpc) sandwich structures with composite coating serve as multipurpose load-bearing elements. the uhpc’s extraordinary compressive strength is used in a multi-material construction element, while issues regarding the concrete’s brittle failure behaviour are properly addressed. a hollow section concrete core is covered by two steel tubes. the outer steel tube is wrapped in a composite material. by this design, uhpc is used in a materialand shape-optimised way with a low dead weight ratio[1] concerning the load-bearing capacity and stability[2]. the cross-section’s hollow shape optimises the construction’s buckling stability while saving self-weight. the composite coating on the column’s outside functions both as a layer increasing the construction’s durability and as a structural component increasing the maximum and the residual load capacity. investigations on the construction’s structural behaviour were performed. keywords: uhpc, sandwich structure, hollow tubular cross-section, composite materials, lightweight. 1. introduction the compressive strength of an ultra-highperformance concrete (uhpc) (fc) exceeds 130 n/mm2. concrete with compressive strengths of 200 n/mm2 can be unerringly produced. one of the challenges to face while working with uhpc is its brittle failure behaviour. since abrupt failure of building components is to be avoided, constructive solutions have to be found. this article addresses the design and mechanical system (see para.2.1) and the production (see para.2.3.2) of uhpc sandwich structures with composite coating, while the individual materials are described in para.2.2. the uhpc sandwich structures with composite coating exploit the concrete’s properties and provide ductile structure behaviour, as proven in experiments (see paragraph 2.3). a test set-up (see para.2.3.3) and results (see para.2.3.4) of axial compressive tests of specimens with and without composite coating are described. the results are discussed in para.2.3.4. 2. uhpc sandwich structures with composite coating as shown in figure 1, uhpc sandwich structures with composite coating consist of four layers of different materials. a hollow section uhpc core is covered by two concentrically arranged steel tubes which can be understood as lost framework and reinforcement of the uhpc core[3]. the outer steel tube is wrapped in a composite material layer. the composite layer fulfills different tasks: its fibres act as a structural component (as described in para.2.1) and its matrix protects the outer steel tube’s surface from corrosion. figure 1. uhpc sandwich structure with composite coating, cross-section. 2.1. mechanical system – conceptual approach uhpc sandwich structures with composite coating serve as multipurpose load-bearing elements, predominantly for compressive loads. axial loads are borne especially by the concrete’s cross-sectional area. the inner and outer steel tube are ideally not involved in the axial load-bearing (as far as the serviceability limit state is not exceeded), nor is the composite material layer. pure uhpc has the most favourable ratio of dead weight to compressive strength in comparison to steel. in order to increase the second moment of area and, thereby, the cross-section’s buckling resistance, a hollow cross-section design is chosen. despite the uhpc’s brittle failure behaviour, a ductile behaviour of the construction can be achieved by the interaction of the uhpc core and the construction’s other layers. after exceeding the ultimate limit 38 http://dx.doi.org/10.14311/app.2017.7.0038 http://ojs.cvut.cz/ojs/index.php/app vol. 7/2017 uhpc sandwich state, the construction is still able to bear further loads by the lateral supporting effects of the steel tubes and the composite layer. the composite material’s fibres are arranged in peripheral direction. consequently, no axial loads are borne by the composite material while buckling and detachment issues are avoided as confinement effects increase both the construction’s load-bearing capacities and its ductility. longitudinal strains of the columns under axial compression result in transverse strains. while the steel’s poisson’s ratio is larger than the concrete’s poisson’s ratio, peripheral tensile stresses occur in the concrete core. radial expansions can be converted into peripheral stresses by the composite material’s fibres, reducing the harmful tensile stresses inside the concrete core and, therefore, multiaxial compressive states of stress can be activated. due to these unidirectional properties of the composite material wrapping, the outer steel tube can be chosen with a relatively low thickness, resulting in further weight savings compared to conservative constructions. 2.2. materials 2.2.1. steel non-alloy quality steel, grade dc01, is used for the outer steel tube and conventional structural steel s235 is used for the inner steel tube. both materials have a characteristic yield stress (fy) of 235 n/mm2. 2.2.2. ultra-high performance concrete the concrete’s mix design and its basic material parameters are shown in table 1 and 2. component type kg/m3 cement cem i 52.5r hs/na 175 microsilica uncompacted 825 fine quartz powder 50/16 µm 200 sand 0.125/0.5 mm 975 water 185 superplasticizer polycarboxylate 28 w/c = 0.24 water to cement ratio w/b = 0.20 water to binder ratio table 1. the design of the concrete mix used. 2.2.3. composite material the carbon fibre reinforced plastic composite consists of • a unidirectional carbon band, which is aligned in the peripheral direction of the specimen (see fig. 2) and • a matrix of epoxy resins, which is predominantly used for rotor blades for wind turbines and shipbuilding. average density 2.323 kg/dm3 slumpflow (sf) (1) 900 mm compressive strength (2,3) 220.0 n/mm2 flexural strength(2,4) 13.3 n/mm2 (1) according to din en 12350-8[4] (2) after thermal treatment at 90 ◦c for 48 h, started 24 h after casting, cube 100 × 100 mm (3) according to din en 12390-3[5] (4) according to din en 196-1[6] table 2. the basic material parameters of the concrete used. carbon band material carbon fibre (ht) width 25.0 mm thickness 0.3 mm weight 350.0 g/m2 yarn count 400.0 tex matrix epoxy resin hexion epikote epoxy hardener hexion epikure heat-curing 12 h, 70 ◦c table 3. the composite material used. figure 2. unidirectional carbon fibre band 2.3. experimental research in order to demonstrate the composite material layer’s impact on the mechanical system, the maximum loadbearing capacities of specimens with fibre reinforced plastic composite coating (series b, two specimens) are compared to those of specimens without composite coating (series a, three specimens). 2.3.1. specimen geometry the specimen’s properties are shown in table 4. 2.3.2. production of the specimens in a first step, the steel tubes are aligned perfectly concentrically. afterwards, the concrete is placed by means of a tremie pipe (contractor method). after heat curing the concrete (see para.2.2.2), the composite material is applied onto specimen b in a hand lay-up process by means of a mounting fixture that allows rotation around the longitudinal axis. in a last step, the composite material is heat cured. a specimen of series b is shown in figure 3. 39 jan markowski, ludger lohaus acta polytechnica ctu proceedings series a: without composite layer inner steel tube: ∅outside = 133.0 mm ts, inner = 2.9 mm outer steel tube: ∅outside = 169.0 mm ts, outer = 1.0 mm concrete core: ∅mid−line = 155.0 mm tc = 19.2 mm length: l = 500 mm weight: m = 15.39 kg series b: with composite layer composite material: 8 layers of carbon band ≈ 3.0 mm (inc. matrix) weight: m = 16.64 kg in all dimensions as series a table 4. properties of the two series figure 3. specimen of series b 2.3.3. test set-up the experimental work focuses on the maximum loadbearing capacity and the ductility. the specimens are loaded in a displacement-controlled (load speed 0.25 mm/min) test by a hydraulic cylinder to failure and beyond. an integrated calotte levels possible tilting. normal force and displacement are measured. in order to introduce the load predominantly into the concrete core and to avoid cracks in the load introduction area, the specimens are grouted in a load introduction panel. the same concrete mix design as used for the specimen is used as grout material. figure 4 shows the test set-up containing the specimen, the load introduction panels, three inductive displacement transducers and protective equipment. 2.3.4. results table 5 shows the results for all specimens of series a and b. force–distance diagrams for two selected exfigure 4. experimental set-up figure 5. force–distance diagrams, two selected examples fn ,max fn , residual series a, specimen 1 1, 395 kn 554 kn series a, specimen 2 1, 389 kn 675 kn series a, specimen 3 1, 260 kn 684 kn series a average 1, 348 kn 638 kn series b, specimen 2 1, 774 kn 1, 610 kn series b, specimen 2 2, 073 kn 950 kn series b average 1, 924 kn 1, 280 kn table 5. results of the experimental research 40 vol. 7/2017 uhpc sandwich amples are presented in figure 5. positive fn -values represent compressive forces for means of presentation. figure 6 shows the two specimen after testing. the broken concrete core of the specimen shown causes a buckling formation on the outer steel tube. the inner steel tube (not shown in fig. 6) is also affected. the buckling appeared when the maximum load capacity of 1, 260 kn was reached. the specimen of series b shown appeared to be undamaged from the outside until a displacement of 10.0 mm is reached. at this point, only single sectors of the composite material failed to a limited extent. when the displacement reached 10.0 mm, a larger amount of fibres failed, causing an extensive detachment in the specimen’s middle section. under the composite layer, the outer steel tubes showed buckling formations that are comparable to those of specimen a. figure 6. series a specimen 3 (left) and series b specimen 1 (right) after testing 3. discussion as the results show, the maximum load-bearing capacity and the residual load-bearing capacity of uhpc sandwich structures can be increased by the addition of a composite layer. the ductility (in this context, the ratio of the residual force to the maximum force) is affected as well, but the results differ. while the ductility of specimen 1 of series b can be increased significantly (the residual force is at 90 % of the ultimate load), the residual force of specimen 2 is at 59 % of its ultimate load. it is still higher than the average ductility of the specimens of series a (47 %), but, in view of the large variation, the effect is negligible. it is assumed that different modes of failure are the reason for this variation. while the concrete core of specimen 1 fails first and is still supported laterally by the composite material, it is suggested that in the case of specimen 2, the fibres fail first and lead to a sudden drop in the load-bearing capacity (from 2, 073 to 950 kn) bearing capacity. table 6 shows a simple approach to estimate the construction’s load-bearing capacity. the composite layer is not taken into account because of its peripheral fibre orientation. cross-sectional area (specimen a and b) steel tubes: as = 1, 713 mm2 concrete core: ac = 7, 959 mm2 load-bearing shares (simple assumption): fn,s = as ∗ fy = 402.4 kn = 16.7 % ∗ fn,total fn,c = ac ∗ fc = 1, 750.9 kn = 81.3 % ∗ fn,total fn,total = fn,s + fn,c = 2, 153.3 kn load-bearing capacity (experimental results): specimen a: fn , average = 1, 348 kn specimen b: fn , average = 1, 924 kn table 6. maximum load-bearing capacity estimation, simple approach the construction’s maximum load-bearing capacity is overestimated by the simple approach. the reason for this could be • the load introduction by load introduction panels that exclude loads partially from the steel tubes; • effects caused by stability; or/and • imperfections (material and geometry). lindschulte proposes a more sophisticated estimation model (eq. 7-1[2]) for sandwich structures without composite coating: fn = ac ∗0.8∗fc +αs−1 ∗as,−1 ∗fy +αs+1 ∗as,+1 ∗fy (1) where is as,−1 = area of the inner steel tubes cross-section as,+1 = area of the outer steel tubes cross-section αs−1 = stability reduction factor concerning to χ(λ) according to eurocode 3, inner steel tube αs+1 = stability reduction factor concerning to χ(λ) according to eurocode 3, outer steel tube applying lindschulte’s model to the series’ geometry shown leads to fn = 1, 400 kn assuming a non-load-bearing role of the steel tubes. this estimation fits the experimental results of series a (fn,average = 1, 348 kn) well. the increase 41 jan markowski, ludger lohaus acta polytechnica ctu proceedings of the maximum load-bearing capacity of series b cannot be explained with this model. confinement effects as a result of the composite layer have to be considered as a reason for this. the composite material’s fibres bear tensile stresses in a peripheral direction, that are caused by transversal strains in a radial direction under axial compression. without these fibres, these radial strains lead to tensile stresses in the concrete-core. due to the confinement effect, all compressive stress states in the concrete core are reached, leading to a higher maximum loadbearing capacity. both specimen of series b also have a higher residual load-bearing capacity. this can be explained by the lateral supporting effect of the composite material. after the concrete is broken, it is kept in place by the inner steel tube and the outer steel tube, which is additionally supported by the composite material. 4. outlook uhpc sandwich structures with composite coating could be beneficially used, for example, in large frameworks of offshore megastructures[7]. in order to prove the concept, further investigations have to be performed. the following subjects require special attention: • the identification of different failure modes. • numerical simulations to prove the mechanical behaviour assumed. • further experimental research with different geometries in order to derive a model for the prediction of the maximal load and the residual load. • the component’s behaviour under pure bending and bending with normal force. • the component’s behaviour under cyclic load. • junctions and load introduction. list of symbols ε strain [–] ac concrete area [mm2] as steel area [mm2] fn maximum normal force [kn] fn,c normal force, concrete’s share [kn] fn,s normal force, steel tubes’ share [kn] fc concrete’s compressive strength [n mm−2] fy steel’s yield stress [n mm−2] u displacement [mm] w/c water to concrete ratio [–] w/b water to binder ratio [–] acknowledgements the research project is supported by the german research foundation (dfg) within the scope of priority programme 1542 "lightweight building with concrete". the authors would like to express their gratitude for the financial support. references [1] n. scholle, l. lohaus, n. lindschulte. weight-saving potential of hybrid tube structures. proceedings of hipermat 2016, 4th international symposium on ultra-high performance concrete and high performance construction materials 2016. [2] n. lindschulte. druckverhalten von rohren aus ultrahochfestem beton mit stahlblechummantelung. institut für baustoffe, leibniz universität hannover, appelstr. 9a, 30167 hannover, de, 1st edn., 2013. [3] n. scholle, l. lohaus. hybrid tubes: material-adapted construction with ultra-high performance concrete. iass2015 annual international symposium on future visions 2015. [4] din en 12350-8: testing fresh concrete part 8: self-compacting concrete slump-flow test; german version en 12350-8:2010. [5] din en 12390-3: testing hardened concrete part 3: compressive strength of test specimens; german version en 12390-3:2009. [6] din en 196-1: methods of testing cement part 1: determination of strength; german version en 196-1:2005. [7] n. scholle, l. lohaus. uhpc-steel hybrid tube components for application in offshore support structures. the annual international offshore and polar engineering conference (isope) 2016. 42 acta polytechnica ctu proceedings 7:38–42, 2017 1 introduction 2 uhpc sandwich structures with composite coating 2.1 mechanical system – conceptual approach 2.2 materials 2.2.1 steel 2.2.2 ultra-high performance concrete 2.2.3 composite material 2.3 experimental research 2.3.1 specimen geometry 2.3.2 production of the specimens 2.3.3 test set-up 2.3.4 results 3 discussion 4 outlook list of symbols acknowledgements references 316 acta polytechnica ctu proceedings 1(1): 316–319, 2014 316 doi: 10.14311/app.2014.01.0316 us astronomical photographic data archives: hidden treasures and importance for high-energy astrophysics rené hudec1,2, lukáš hudec2 1astronomical institute, academy of sciences of the czech republic, cz-25165 ondřejov, czech republic 2czech technical university in prague, faculty of electrical engineering, prague, czech republic corresponding author: rene.hudec@asu.cas.cz abstract we report here on an ongoing investigation of us astronomical plate archives and tests of the suitability of transportable scanning devices for in situ digitization of archival astronomical plates, with emphasis on application in high-energy astrophysics. keywords: astronomical data archives: astronomical photographic archives – spectroscopy: low-dispersion spectra – data mining. 1 introduction there are numerous important astronomical plate archives in the usa, including plate collections that are little known to the community and that have been little investigated in the past. within the framework of a czech-us collaborative project (msmt kontakt amvis me09027), we have recently analyzed some of them, obtaining test scans with the use of a portable digitizing device. digitization is a necessary step for an extended evaluation of the plate data using dedicated programs and powerful computers. several recently found large us negative archives are expected to play important role in high-energy astronomy. motivation for including this subject into multi– frequency studies of high energy sources is as follows. numerous he/vhe/uhe sources are also emitters of optical light, many of them are variable. the astronomical plate archives represent the only method how to study the behavior of the objects over very long (100 years or even more) time intervals (hudec, 1999 and 2012). in addition, huge monitoring times allows to detect and to study rare events such as flares. the databases allow to study prominent spectra and/or spectral changes as well (hudec et al., 2012). 2 the plate archives the us astronomical archival plate collections that we recently visited and investigated include those housed in the following 16 institutions: carnegie observatories pasadena, ca, lick observatory, ca yerkes observatory, wi, mt palomar observatory, ca, pari, rosman, nc (which has a collection of plates from many observatories), kpno tucson, az, cfht waimea, hi, ifa manoa, hi, usno flagstaff, az, usno washington, dc, steward observatory tucson, az, nmsu, las cruces, nm, rosemary hill observatory, university of florida, gainesville, fl and leander mccormick observatory, university of virginia, charlottesville, va, smithsonial archives washington, dc, and hazy space center, dulles, va. our estimate is that there are more than 2 million astronomical archival plates and/or negatives in these archives. there are however many us plate collections not included in our study (robbins and osborn, 2009). we performed a quality check and analyzed these plate archives with emphasis on their scientific, historical and cultural value, which we have found to be enormous. in addition to that, collaboration with several german institutes with astronomical plate archives started, with emphasis on digitization and investigation of relevant photographic collections. 3 transportable digitizing device most of the plate archives that we visited have no plate scanners and lack modern instrumentation in general. as our study includes plate digitization, it was necessary to find a solution. since we were going to travel from europe to the us by air, the obvious option was a transportable digitization device based on a digital camera with a high-quality lens and a stable tripod. this solution has the following advantages over other techniques: the device is easily transportable, and offers much faster scanning and higher repeatability than commercial flatbed scanners, because there are no mov316 http://dx.doi.org/10.14311/app.2014.01.0316 us astronomical photographic data archives: hidden treasures and importance for high-energy astrophysics ing scanner parts. the equipment that we used was as follows: camera: 21 mpx canon eos 5d mark ii, lenses: canon ef 24-70 f/2.8 l usm and canon 70200mm f4, a stable tripod, and a fomei lp-310 professional photographic light table. in last project year, a better custom-made light table based on highly homogeneous led illumination was used, and also a further improved camera (39 mpx) and lenses. the recorded images are then corrected for lens image distortions and for other effects, in order to store research-grade digital images. the achieved pixel size depends on the size of the plate, and fine pixel sizes of order of 25–30 microns or less can be typically obtained for small and medium sized plates (up to 16 cm x 16 cm or 18 cm x 24 cm) while for larger plates larger pixel sizes will be obtained (or, alternatively, the large plate may be covered by several shots to achieve smaller pixel sizes). examples of digitized 16 cm x 16 cm plates are illustrated in figs. 1 and 2 with relevant field recognition and star identification. figure 1: example of digitized bamberg southern sky patrol plate processed by astrometry.net tools: field recognition 4 general picture after visiting the us plate collections mentioned above, we offer a (subjective) list of the major problems found in these archives: (i) the list of us plate collections provided by dr. wayne osborn (robbins and osborn, 2009) was found to be incomplete. we have found valuable plate collections with plates from important telescopes that are not listed, e.g. the two hawaii plate collections in manoa (institute of astronomy) and in waimea (canada-france hawaii telescope cfht). some plate archives have been completely hidden, as their home institutes were in some extreme cases not even aware that they have plate stacks. (ii) in numerous collections, only a very rough estimate of the number of plates can be given, as no exact information about the total number of plates, etc., is available. usually, the real number of plates is higher than the previously available estimate. in general, it is very difficult to give the exact number of plates, due to lack of observation logs and inadequate organization of the plate archives. (iii) in many cases, there is no contact person responsible for the plate archive, and it is difficult to make contact. in some places, it is even difficult to get access. this situation very has a serious adverse effect on efforts to exploit these plate collections for scientific purposes. (iv) for some archives, no information is available, not even an approximate number of plates. in many archives, no plate logs are available; they have either been removed or are lost. the only available information is what is written on the plates or on the envelopes (in some cases, there is not even adequate information on the envelope). we guess that there were originally observation logs, but that these were later separated from the plates and archived in a different location. example: carnegie observatories pasadena (nearly 0.5 million plates), where the logs are probably located in the attic above the library, with difficult access. (v) damaged plates in some archives (mostly due to a partly-released or even complete released emulsion layer), probably due to improper storage (or changes in humidity/temperature over time). we point out however that even these plates can be restored using suitable chemical methods and procedures. (vi) lack of electronic records no lists of plates, the only information is on the plates and/or plate envelopes (vii) many of the archives that we visited suffer from inadequate funding, lack of devices, e.g. no scanners. (viii) we have revealed that many plates have been removed from their home: these plates are usually scattered in private homes and offices, or are being kept by observers (often abroad). numerous plates taken at us observatories have been found in european plate archives. nevertheless, we found highly valuable plates almost everywhere, and the quality of the plates (and hence their scientific potential) is mostly high or even very high, in comparison with the plates in european archives. this is true both for direct images and for spectral images (taken with an objective prism). in addition to stellar images, some of the archives that we visited also include extensive collections of solar images (e.g. carnegie observatories in pasadena) and/or planetary images (unique collection in las cruces). the storage conditions were found to vary from archive to archive, from proper temperature and humidity conditions, to less proper conditions. the main degradation sources found in the plate collections were high levels 317 rené hudec, lukáš hudec of humidity and probably also temperature variation, resulting in partial or complete release of the emulsion layer. the scientific use of the plate archives is negatively impacted by poor access to the plates at some places, and also by the fact that the plates have in most cases not yet been cataloged. figure 2: example of digitized bamberg southern sky patrol plate processed by astrometry.net tools: star identification/astrometry 5 two recently found large us archives with possible major impact on hea the two following databases found within our project are expected to play an especially important role in high-energy astronomy. baker super schmidt camera domed films with 55 degrees diameter fov, limiting magnitude up to 15, dense sampling 20 min, ∼ 110 000 negatives (fig. 5), ∼ 10 years coverage. the essential part of the archive is located at pari (pisgah astronomical research institute) in nc. baker-nunn camera networks negatives fov 30 x 5 degrees, limiting magnitude up to 16, very dense sampling ∼ few sec, more than 1 mil negatives, ∼20 years coverage (figs. 3 and 4). the part of the archive (21 boxes with ∼ 2000 film rolls) is located at smithsonian institution archive in washington, d.c. these data are suitable for wide-field studies, optical transient (ot) searches, and fast variability studies. there are up to 100 000 stars per 1 full frame. these data represent direct images suitable for photometry. however, one baker nunn kwajalein slit-less spectrograph camera for u.s. air force was designed to provide unique low–dispersive spectra. this baker nunn missal reentry tracking camera consisted of a three-element 20-inch entrance aperture corrector lens system. mounted on top of the corrector lens assembly was a multi-set of triangular prisms converting the incoming sky image into a spectrum image. figure 3: dismantling of the usaf baker–nunn camera at the evergreen aviation & space museum, mcminnville, oregon, united states figure 4: example of digitized film from sao baker– nunn camera the corrected spectral image is then projected down to a 31-inch f/1 spherical primary mirror. the focusing converging image was then reflected back up to a 4-inch x 6-inch x 0.6-inch thick mosaic of fiber-optics making film supporting focusing plate. the resulting database is expected to has applications in astronomy as well. 6 summary 16 us astronomical plate archives were visited within the amvis czech-us collaborative project. the quality of the plates and their scientific, historical and cultural value were investigated for possible inclusion in the us astronomical plate repository at pari, nc. some of these archives (e.g. baker super schmidt, baker–nunn, cfht waimea, ifa manoa) were un318 us astronomical photographic data archives: hidden treasures and importance for high-energy astrophysics known to the astronomical community before our study, and the two first mentioned are expected to play important role in high–energy astronomy because of their very wide–field and very fine time resolution. selected plates were digitized using a transportable scanning device. all the archives that we visited have plates that are scientifically valuable, and in many cases unique. the plates are however mostly hidden from the astronomical community, and the plates have not yet been catalogued. the total number of plates is higher than expected in many of the locations, the actual number of plates is unknown. as no catalogs exist, the real number of plates is very difficult to estimate, but for sure the places that we visited have more than 2 million photographic plates and/or negatives in their collections. we plan to continue these efforts, now with emphasis on german astronomical plate collections. figure 5: example of digitized film from sao baker super schmidt camera we plan to continue data mining and plate digitization in astronomical photographic plate/negative archives is as follows. (i) digitize the plate archives using a fast and transportable scanning device, as described above. this scanning method is fast and inexpensive. these are important considerations, as the archives are scattered and there are very large numbers of plates. (ii) create electronic catalogs. (iii) include these catalogs into search programs like wfpd, operated by our bulgarian colleagues (e.g. tsvetkov et al., 2005, and tsvetkov, 2009). acknowledgement the scientific part (investigation of long–term behaviour of high–energy sources) of the study is linked to the grant 13-33324s provided by the grant agency of the czech republic (gacr). the analyzes of astronomical plates are more recently supported by the gacr grant 13-39464j. references [1] hudec, r. et al., acta polytechnica, ibws2011 proceedings, 1(52), 2012. [2] hudec, r. astrophysics with astronomical plate archives, in exploring the cosmic frontier: astrophysical instruments for the 21st century. eso astrophysics symposia, european southern observatory series. edited by andrei p. lobanov, j. anton zensus, catherine cesarsky and phillip j. diamond. series editor: bruno leibundgut, eso. isbn 978-3-540-39755-7. published by springerverlag, berlin and heidelberg, germany, 2007, p.79 [3] hudec, r., an introduction to the world’s large plate archives, acta historica astronomiae, vol. 6, p. 28-40, 1999. [4] robbins, l.; osborn, w., preserving astronomy’s photographic legacy: current state and the future of north american astronomical plates. asp conference series, vol. 410, appendix b and c. edited by wayne osborn and lee robbins. san francisco: astronomical society of the pacific, 2009. 319 introduction the plate archives transportable digitizing device general picture two recently found large us archives with possible major impact on hea summary 66 acta polytechnica ctu proceedings 1(1): 66–70, 2014 66 doi: 10.14311/app.2014.01.0066 evolution of massive population iii stars sung-chul yoon1 1astronomy program, department of physics and astronomy, seoul national university, seoul, 151-742, republic of korea corresponding author: yoon@astro.snu.ac.kr abstract while the evolution of massive stars in the local universe is dominated by mass-loss, the evolution of massive population iii stars should be dominated by rotation. an important effect of rotation is rotationally-induced chemical mixing that can dramatically change the stellar structure and the nucleosynthesis. this has significant consequences in the predicted explosion types of population iii stars. keywords: stars: evolution stars: rotation stars: population iii supernovae gamma-ray bursts. 1 introduction formation of population iii (pop iii) stars marks the end of the so-called dark age in the early universe. these first stars are believed to be intrinsically massive (30 m� < m < 1000 m�), given that the primordial gas does not contain any efficient coolants in star-forming regions, and supposed to play a key role in the evolution of the early universe, in many aspects (see bromm 2013, for a recent review). neutral hydrogens and heliums are re-ionized by the first lights from these first generations of stars, and the primordial gas becomes polluted with heavy elements produced by both hydrostatic and explosive nucleosyntheses in them. although direct identification of them will be highly unlikely even with next generations of telescopes, their nature can be indirectly probed with observations of their explosions that may be luminous enough to be discovered in near future. observational studies on the surface abundances of extremely metal poor stars, which are believed to retain the nucleosynthesis signatures of pop iii stars, will also provide a good constraint on the evolution of pop iii stars. theoretical predictions that can confront future observations are indispensable for these efforts (e.g., marigo et al. 2001; heger & woosley 2002; umeda & nomoto 2003; heger & woosley 2010; kasen et al. 2011; limongi & chieffi 2012; dessart et al. 2013; whalen et al. 2013; tanaka et al. 2013). in this paper, i discuss the current understandings on the evolution of massive pop iii stars, focusing on the role of rotation in the stellar evolution (e.g., marigo et al. 2003; ekström et al. 2008; yoon et al. 2012). recent numerical studies indicate that massive pop iii stars would be born with surface rotation close to the critical value (e.g., stacy et al. 2011). 2 importance of rotation in our galaxy, stars having masses higher than about 30 m� usually undergo strong mass-loss during their evolution. this is because numerous metal lines in their atmospheres and the consequent high radiation pressure cause instabilities of various sorts at the stellar surfaces (see puls et al. 2008, for a recent review). the evolution of massive stars at high metallicity is therefore dominated by mass-loss. for instance, in the local universe, stars as massive as 120 m� at their birth would lose more than 100 m� throughout their lives, dying as 10 20 m� stars (e.g., meynet & maeder 2005). this also means that such massive stars would rapidly lose most of their initial angular momentum, rendering the effect of rotation minor or negligible in general. by contrast, it is believed that massive pop iii stars do not experience significant mass-loss because they are generally very stable (baraffe et al. 2001). in addition, lines by hydrogen and helium are too weak to drive radiation-driven winds (krticka & kubát, 2006). therefore, massive pop iii stars would retain a significant fraction of the initial angular momentum throughout their evolution. this has the following important consequence: while the evolution of very massive stars at high metallicity is dominated by mass-loss, the evolution of massive pop iii stars is dominated by rotation. an important effect of rotation is chemical mixing resulting from rotationally-induced hydrodynamic instabilities like eddington-sweet circulations that are driven by thermal imbalance inside rapidly rotating stars (e.g., maeder 2009). see brott et al. (2011b) for a 66 http://dx.doi.org/10.14311/app.2014.01.0066 evolution of massive population iii stars ! ! !" !" !"#$%&'()"&*+,"./0$,1%&&2'3"$"40-0"*5'()"&*+,"!"#$ #%&'($)*+)',) -"#$ #$% &' (%) *)+ %, -*.+/'(%)*)+%, !0/(%1",' 2,3"$%." 45"'6%("'+7' "88+6+",)$0' 9(*:"/'/%&,' /;"')%' )5"'6%("<",3"$%."' 6%;.$+,1= 65*%&'1"#071"&&%850 >%'6%("'9(*:+,1'90' )5"'6%("<",3"$%."' 6%;.$+,1= (98&"5,"-'8":0#0;' <2'#"+%+,"-'&,=0'>?@ #)(%,1'65"?+6*$'1(*/+",)'9")&"",' )5"'!<9;(,+,1'6%,3"6)+3"'6%("' *,/')5"'",3"$%." >%'65"?+6*$'1(*/+",)'9")&"",' )5"'!<9;(,+,1'6%,3"6)+3"'6%("' *,/')5"'",3"$%." figure 1: illustration for the bifurcation of massive star evolution according to their initial rotational velocity. slowly rotating massive stars develop the classical core-envelope structure such that they become red-supergiant stars during the post-main sequence phases. rapidly rotating massive stars, on the other hand, may undergo very rapid rotationally-induced chemical mixing to such an extent that quasi-chemical homogeneity can be maintained on the main sequence, if their initial metallicity is sufficiently low. in this case, stars are gradually transformed into helium stars at the end of the main sequence. see yoon & langer (2005), yoon et al. (2006), and woosley & heger (2006) for more details. recent dicussion on the observational tests and related uncertainties of the rotational mixing scenario. the hydrogen burning core is supplied with fresh hydrogenrich material from the envelope because of this mixing, resulting in a larger core size than in the corresponding case without rotation. the most extreme case is the socalled chemically homogeneous evolution (che), which is illustrated in fig. 2. with a sufficiently high rotational velocity (i.e., more than about 50% of the local keplerian value at the equatorial surface), the chemical mixing timescale by eddington-sweet circulations can be shorter than the nuclear burning time of hydrogen, so as to maintain quasi-chemical homogeneity in the star. because almost all the hydrogens in the star participate nuclear burning in this way, the star gradually becomes a massive helium star at the end of the main sequence. this is an important evolutionary channel to make massive he stars at low metallicity, while che may not play an important role at high metallicity because of rapid angular momentum loss via stellar winds (see yoon et al. 2006). this mode of evolution is also considered an important channel to produce long gamma-ray bursts from metal-poor massive stars (yoon & langer 2005; yoon et al. 2006; woosley & heger 2006). stars with the che evolve bluewards instead of evolving redwards on the hr diagram. the presence of such stars in the early universe would make significant impact on the history of reionization, because they produce more ionizing photons by several factors than stars that follow the normal evolution (yoon et al. 2012). this particular mode of stellar evolution also results in a significant diversity of pop iii star explosions, as discussed below. 3 explosions of massive population iii stars the theoretical predictions on the final fates of massive pop iii stars are given as the phase diagram in fig. 2. pop iii stars that develop the classical core-envelope structure would die as red or blue supergiant stars, and their final fates may not be much different from those 67 sung-chul yoon 10 20 35 60 100 160 250 500 0.0 0.2 0.4 0.6 0.8 final fates of rotating massive pop iii stars 10 20 35 60 100 160 250 mzams [msun] 0.0 0.2 0.4 0.6 0.8 v z a m s /v k forbidden region v zams=v crit sn iip (ns remnant) collapse to bh, or weak sn ii collapse to bh pisn (sn ii) p uls. p is n (s n ii) grb / hn (sn ibc) p uls. p is n g r b /h n (ibc) pisn (sn ibc) figure 2: final fates of massive pop iii stars for given initial masses and rotational velocities, predicted from the stellar evolution models by yoon et al. (2012). the rotational velocity on the zero-age main sequence is given in units of the keplerian value at the equatorial surface (i.e., vk = √ gm/r). we adopted the most up-to-date calibration for the rotationally-induced chemical mixing efficiency by brott et al. (2011a). the region for the chemically homogeneous evolution (che) is marked by yellow color, and the thick solid line gives the boundary between the che regime and the region for the normal evolution. different regions are marked by expected final outcomes: type ii supernovae (sn ii), collapse to black hole (bh), pulsational pair-instability supernovae (puls-pisn), pair-instability supernovae (pisn), long gamma-ray bursts (grb), hyper-novae (hn), type ib or ic supernovae (sn ibc). in the forbidden region, the equatorial surface velocity exceeds the critical velocity: vcrit = √ (gm/r)[1 − γ], where γ is the eddington factor at the stellar surface. this figure is taken from yoon et al. (2012). of non-rotating pop iii stars as predicted by heger & woosely (2002). but the limits of the initial masses for pulsational pair-instability and pair instability supernovae would move downwards for a higher initial rotational velocity, because rotational mixing tends to increase the he core masses. as explained above, in the che regime, pop iii stars would die as massive helium stars and therefore produce supernovae of type ib/c. conditions for long gamma-ray bursts can also be fulfilled in this regime for an initial mass range of 13 84 m�. while non-rotating pop iii stars would require initial masses of about 140 270 m� to produce a pair instability supernova, this mass range would decrease to about 84 190 m� in the che regime (see also chatzopoulos & wheeler 2012). another interesting prediction is that for intial masses of about 56 84 m�, a pulsational pair-instability supernova would be followed by a long gamma-ray bursts, only several years later. given that gamma-ray jets would interact with a very massive circumstellar matter in this case, extremely bright afterglow might be produced. our models also predict that the final masses of pop iii grb progenitors (∼ 10−70 m�) would be significantly more massive than those of grb progenitors in the local universe (∼ 10−20 m�; yoon et al. 2006). on the other hand, recently several authors argued for super-collapsar formation in very massive pop iii stars (m > 270 m�; mészáros & rees 2010; komissarov & barkov 2010; suwa & ioka 2011 ). however, our models show that very massive pop iii stars with initial masses larger than about 190 m� cannot retain enough angular momentum in the core to produce any rotation-powered event at their deaths. this is because such stars have a very large convective core that leads to efficient angular momentum transport from the innermost layers to the stellar surface, and because large eddington-factors of these stars facilitates mass and angular momentum loss via centrifugally driven massshedding. 68 evolution of massive population iii stars acknowledgement i am very grateful to norbert langer and alexandra dierks for their contribution to this work. references [1] baraffe, i., heger, a., & woosley, s.e., 2001, apj, 550, 890 doi:10.1086/319808 [2] bromm, v., rep. prog. phys., 2013, submitted. [3] brott, i., de mink, s.e., & cantiello, m. et al., 2011a, a&a, 530, 115 [4] brott, i., evans, c.j., & hunter, i. et al., 2011b, a&a, 530, 115 [5] chatzopoulos, e., & wheeler, j.c., 2012, apj, 760, 154 doi:10.1088/0004-637x/760/2/154 [6] dessart, l., waldman, r., livne, e., hillier, d.j., blindin, s., 2013, mnras, 428, 3227 doi:10.1093/mnras/sts269 [7] ekström, s., meynet, g., chiappini, c., hirschi, r., & maeder, a., 2008, a&a, 489, 685 [8] heger, a., & woosley, s.e., 2002, apj, 567, 532 doi:10.1086/338487 [9] heger, a., & woosley, s.e., 2010, apj, 724, 341 doi:10.1088/0004-637x/724/1/341 [10] kasen, d., woosley, s.e., & heger, a., 2011, apj, 734, 102 doi:10.1088/0004-637x/734/2/102 [11] komissarov, s.s., & barkov, m.v., 2010, mnras, 402, 25 doi:10.1111/j.1745-3933.2009.00792.x [12] krticka, j. & kubát, j., 2006, a&a, 446, 1039 [13] limongi, m., & chieffi, a., 2012, apjs, 199, 38 doi:10.1088/0067-0049/199/2/38 [14] maeder, a., 2009, physics, formation and evolution of rotating stars, astronomy and astrophysics labirary, springer [15] marigo, p., chiosi, c., & kudritzki, r.-p., 2003, a&a, 399, 617 [16] marigo, p., girardi, l., chiosi, c., & wood, p.r., 2001, a&a, 371, 152 [17] mészáros, p., & rees, m.j., 2010, apj, 715, 967 doi:10.1088/0004-637x/715/2/967 [18] meynet, g., & maeder, a., 2005, a&a, 429, 581 [19] puls, j., vink, j.s., & najarro, f., 2008, a&arv, 16, 209 [20] spruit, h., 2002, a&a, 381, 923 [21] stacy, a., bromm, v., & loeb, a., 2011, mnras, 413, 543 doi:10.1111/j.1365-2966.2010.18152.x [22] suijs, m.p.l., langer, n., poelarends, a.-j., yoon, s.-c., hger, a., & herwig, f., 2008, a&a, 481, 87 [23] suwa, y., & ioka, k., 2011, apj, 726, 107 doi:10.1088/0004-637x/726/2/107 [24] tanaka, m., moriya, t.j., & yoshida, n., 2013, arxiv:1306.3743 [25] umeda, h., & nomoto, k., 2003, nature, 422, 871 doi:10.1038/nature01571 [26] whalen, d. et al., 2013, apj, 762, 6 doi:10.1088/2041-8205/762/1/l6 [27] woosley, s.e., & heger, a., 2006, apj, 637, 914 doi:10.1086/498500 [28] yoon, s.-c., & langer, n., 2005, a&a, 443, 643 [29] yoon, s.-c., langer, n., & norman, c., 2006, a&a, 460, 199 [30] yoon, s.-c., dierks, a., & langer, n., 2012, a&a, 542, 113 discussion dorota rosinska: you have shown that evolution of low-metallicity massive stars strongly depends on rotation. such stars should rotate differentially. what laws of differential rotation you assume? how results depend on the degree of differential rotation (ωe/ωc; ωe is the angular velocity at the equatorial surface, and ωc the angular velocity at the center)? sung-chul yoon: stars always tend to rotate differentially because of the contraction of the core that results in spinning-up the central layers. the degree of differential rotation in a star is then determined by the efficiency of the angular momentum transport from the core to the envelope. i.e., we do not ”assume” the degree of differential rotation, but it is self-consistently calculated with a given prescription for the transport of angular momentum. in our models, we adopted the socalled talyer-spruit dynamo (spruit 2002) which leads to a very strong coupling between the core and the envelope, making a star rotate almost rigidly on the main sequence. stellar evolution models including the taylerspruit dynamo have proved to be consistent with observations, in terms of the predicted spin-rates of stellar 69 http://dx.doi.org/10.1086/319808 http://dx.doi.org/10.1088/0004-637x/760/2/154 http://dx.doi.org/10.1093/mnras/sts269 http://dx.doi.org/10.1086/338487 http://dx.doi.org/10.1088/0004-637x/724/1/341 http://dx.doi.org/10.1088/0004-637x/734/2/102 http://dx.doi.org/10.1111/j.1745-3933.2009.00792.x http://dx.doi.org/10.1088/0067-0049/199/2/38 http://dx.doi.org/10.1088/0004-637x/715/2/967 http://dx.doi.org/10.1111/j.1365-2966.2010.18152.x http://dx.doi.org/10.1088/0004-637x/726/2/107 http://dx.doi.org/10.1038/nature01571 http://dx.doi.org/10.1088/2041-8205/762/1/l6 http://dx.doi.org/10.1086/498500 sung-chul yoon remnants like white dwarfs and neutron stars (suijs et al. 2008). matteo guainazzi: which black hole spin distribution would you expect from your evolutionary scenario? sung-chul yoon: bimodal distribution. if a bh forms in the che regime, its kerr parameter will be close to 1. otherwise, bhs will not have any significant angular momentum, having a kerr parameter close to zero. 70 introduction importance of rotation explosions of massive population iii stars 259 acta polytechnica ctu proceedings 1(1): 259–264, 2014 259 doi: 10.14311/app.2014.01.0259 a review of astrophysical jets james h. beall1,2 1st. john’s college, annapolis, md 2space sciences division, naval research laboratory, washington, dc corresponding author: beall@sjc.edu abstract astrophysical jets are ubiquitous: this simple statement has become a commonplace over the last three decades and more as a result of observing campaigns using detectors sensitive from radio to gamma-ray energies. during this epoch, theoretical models of these sources have become more complex, moving from assumptions of isotropy that made analytic calculations possible, to fully anisotropic models of emission from the jets and their interactions with the interstellar and intra-cluster medium. such calculations are only possible because we have extensive computational resources. in addition, the degree of international cooperation required for observing campaigns of these sorts is remarkable, since the instruments include among others the very large array (vla), the very long baseline array (vlba), and entire constellations of satellite instruments, often working in concert. in this paper, i discuss some relevant observations from these efforts and the theoretical interpretations they have occasioned. keywords: astrophysical jets active galactic nuclei uhe cosmic rays quasars microquasars. 1 introduction extended linear structures, usually interpreted as astrophysical jets, are found in star-forming regions, in compact binaries, and of course in active galactic nuclei (agns), and galaxy clusters. gamma-ray bursts can be associated with astrophysical jets associated with stellar collapse where the jets is directed toward earth. we have become aware of considerable details of these results through decades of sustained observing campaigns. the results of these campaigns show similarities and significant differences in the data from some epochs of galactic microquasars, including grs 1915+105, the concurrent radio and x-ray data (beall et al., 1978) on centaurus a (ngc 5128), 3c120 (marscher (2006), and 3c454.3 as reported by bonning et al. (2009), to name a few. the bonning et al. analysis of the 3c454.3 data showed the first results from the fermi space telescope for the concurrent variability at optical, uv, ir, and γ-ray variability of that source. in combination with observations of microquasars and quasars from the mojave collaboration (see, e.g., lister et al., 2009), these observing campaigns provide an understanding of the time-dependent evolution of these sources at milliarcsecond resolutions (i.e., parsec for agns, and astronomical unit scales for microquasars). in blazar sources (see, e.g., ulrich et al. 1997, and marscher, 2006) there seems to be a confirmed connection of jets with accretion disks. in sources without large-scale linear structures (i.e., jets), as ulrich et al. (1997) note, the source variability could result from the complex interactions of the accretion disk with an x-ray emitting corona. but to the extent that ”small” jets are present in these sources, the disk-jet interaction must still be of paramount importance, since it provides a mechanism for carrying away energy from the disk. current theories (see e.g., hawley 2003 and bisnovatyi-kogan 2013 for a discussion of disk structure and jet-launch issues, respectively) suppose that the jet is formed and accelerated in the accretion disk. but even if this is true in all sources, it is still unclear whether or not astrophysical jets with shorter propagation lengths are essentially different in constitution from those that have much longer ranges, or whether the material through with the jet propagates determines the extent of the observational structures we call jets. at all events, the complexities of the jet-ambient medium interaction must have a great deal to do with the ultimate size of emitting region. this sort of argument has applications to both quasars and microquasars, especially if essentially similar physical processes occurs in all these objects (see, e.g., beall, 2003, and marscher, 2006). to some, it has become plausible that essentially the same physics is working over a broad range of temporal, spatial, and luminosity scales. hannikainen (2008) and chaty (2007) have discussed some of the emission characteristics of 259 http://dx.doi.org/10.14311/app.2014.01.0259 james h. beall microquasars, and paredes (2007) has considered the role of microquasars and agns as sources of high energy γ-ray emission. in fact, the early reports of the concurrent radio and x-ray variability of centaurus a can be plausibly interpreted as the launch of a jet from cen a’s central source into the complex structures in its core. additionally, these observations are remarkably similar to the observations of galactic microquasars and agns, including the observations from the fermi space telescope of concurrent γ-ray, ir, optical, and uv variability of 3c454.3 (bonning et al., 2009), and observations by madejski et al. (1997) for bl lac, among others. 2 concurrent variability of agn jet sources as an indication of jet launch or jet-cloud interactions i now turn to two such observations in this paper, the concurrent radio and x-ray variability of centaurus a (beall et al., 1978), and the gamma-ray, uv, and ir concurrent variability discussed by bonning et al., (2009) using the fermi lat and swift spacecraft. 2.1 radio and x-ray variability measurements of centaurus 1 (ngc 5128) the first detection of concurrent, multifrequency variability of an agn came from observations of centaurus a (beall et al., 1978, see figure 1 of that paper). beall et al. conducted the observing campaign of cen a at three different radio frequencies in conjunction with observations from two different x-ray instruments on the oso-8 spacecraft in the 2-6 kev and 100 kev xray ranges. these data were obtained over a period of a few weeks, with the stanford interferometer at 10.7 ghz obtaining the most data. beall et al. also used data from other epochs to construct a decade-long radio and x-ray light curve of the source. figure 1a of beall (2011) shows the radio data during the interval of the oso-8 x-ray observations, as well as the much longer timescale flaring behavior evident in the three different radio frequencies and at both low-energy (2-6 kev, see figure 1b of beall, 2011) and in high-energy (∼ 100 kev, see figure 1c of beall, 2011) x-rays. as noted by beall (2011), a perusal of figure 1a in that paper shows the that the radio data (represented as a “+” in that figure) generally rise during 1973 to reach a peak in mid-1974, then decline to a relative minimum in mid-1975, only to go through a second peak toward the end of 1975, and a subsequent decline toward the end of 1976. this pattern of behavior is also shown in the ∼ 30 ghz data and the ∼ 90 ghz data albeit with less coverage at the higher two radio frequencies. several points are worthy of note. first, as beall et al. (1978) show, the radio and x-ray light curves track one another. this result demonstrated the first report of concurrent radio and x-ray variability of an active galaxy. mushotzky et al. (1978), using the weekly 10.7 ghz data obtained by beall et al., (1978) demonstrate that the 10.7 ghz radio data track the 2-6 kev x-ray data on weekly time scales, also. the concurrent variability at radio and x-ray frequencies argues that the emitting region is the same for both the radio and xray light. this, as was noted by beall and rose (1980), can be used to set interesting limits on the parameters of the emitting region. in addition, the observations at the three radio frequencies (10.7 ghz, ∼ 30 ghz, and ∼ 90 ghz) clearly track one another throughout the interval whenever concurrent data are available. figure 1: fermi lat data (see, e.g., lott et al. 2013) showing the time history of the flaring from 3c454.3 (figure 1b), along with the bonning et al. (2009) data showing concurrent gamma-ray, ir, optical, and uv data (figure 1b). the time of the jet launch from the mojave ”movie” is illustrated by the arrow. the result, first reported here, shows radio flaring consistent with the bonning et al. data. a plausible hypothesis for the observations we have witnessed is that they arise from physical processes associated with the ”launch” of an astrophysical jet into the complex structures in the core of centaurus a. the timescale of the evolution from early 1973 through 1977 appears to be associated with the evolution of a larger structure over a more extended region. the observations are consistent with the interaction of the astrophysical jet with an interstellar cloud in the core of cen a. 260 a review of astrophysical jets it is clear from this discussion that a distinction needs to be made about which observational signatures are associated with the jet launch, the jet itself, and the ambient medium’s reaction to the jet. in considering such a scenario applied to microquasars, the observations of sco x-1 by fomalont, geldzahler, and bradshaw (2001), as discussed by beall et al. (2013) are extremely informative. 2.2 a jet launch coincident with the 3c454.3 multi-frequency flaring bonning et al. (2009) performed an analysis of the multi-wavelength data from the blazar, 3c454.3, using ir and optical observations from the smarts telescopes, optical, uv and x-ray data from the swift satellite, and public-release γ-ray data from the fermilat experiment. in that work, she demonstrated an excellent correlation between the ir, optical, uv and gamma-ray light curves, with a time lag of less than one day. urry (2011) noted that 3c454.3 can be a laboratory for multifrequency variability in blazars. while a more precise analysis of the data will be required to determine the characteristics of the emitting regions for the observed concurrent flaring at the different frequencies, the pattern of a correlation between low-energy and higher-energy variability is consistent with that observed for cen a, albeit with the proviso that the energetics of the radiating particles in 3c454.3 is considerably greater. a perusal of the data for 3c454.3 at milliarcsecond scales taken from the mojave vlba campaign during the bonning et al (2009) flare show that the timedependent flare occurs during launch of a new component of the jet that originates from the core. figure 2: figure 2: 3c454.3 shown at milliarcsecond scales for data taken from the mojave vlba campaign during the bonning et al (2009) flare. a perusal of the time-dependent flare clearly shows that the jet launch from the core of the agn is coincident with the double peaked flaring shown in the bonning et al. results. the pattern of variability reported by bonning et al., is consistent with the injection of relativistic particles into a region with relatively high particle and radiation densities (i.e., an interstellar cloud). the picture that emerges, therefore, is consistent with the observations of spatially and temporally resolved galactic microquasars and agn jets. it should not escape our notice that other epochs in the 3c454.3 data from mojave and fermi also show similar periods of injection of radio blobs that are associated with a double-peaked structure in the gamma-ray light. for the cen a data, and for data from 3c454.3, it is the concurrent variability that suggests that the radio to x-ray (in cen a’s case) and the ir, optical, and uv to γ-ray fluxes (in 3c454.3’s case) are created in the same region. this leads to the possibility of estimates of the source parameters that are obtained from models of these sources. vlbi observations of cores vs. jets (see, e.g., the study of bl lac by bach et al. 2006) show the structures of the core vs. jet as they change in frequency and time. it has thus become possible to separate and study the time variability of the jet and the core of agn at remarkably fine temporal and spatial scales. van der laan (1976) discussed the theoretical interpretation of cosmic radio data by assuming a source which contained uniform magnetic field, suffused with an isotropic distribution of relativistic electrons. the source, as it expanded, caused an evolution of the radio light curve at different frequencies. each of the curves in van der laan’s paper represents a factor of 2 difference in frequency, the vertical axis representing intensity of the radio flux and the horizontal axis representing an expansion timescale for the emitting region. van der laan’s calculations show a marked difference between the peaks at various frequencies. the data from cen a (as discussed more fully in beall (2008, 2010) are, therefore, not consistent with van der laan expansion (van der laan, 1976), since for van der laan expansion, we would expect the different frequencies to achieve their maxima at different times. also, the peak intensities should decline with increasing frequencies at least in the power-law portion of the spectrum. the most likely explanation for the changes in the spectrum of the cen a data at 100 kev (beall, et al., 1978) is that the emitting region suffered an injection of energetic electrons. that is, a jet-ambient-medium interaction dumped energetic particles into a putative ”blob,” or, equivalently, that there was a re-acceleration of the emitting electrons on a timescale short compared to the expansion time of the source. an analysis of the 3c120 results compared with the data from the galactic microquasar, sco x-1, under261 james h. beall taken by beall (2006) shows a similar radio evolution, with rapidly moving “bullets” interacting with slower moving, expanding blobs. it is highly likely that the elements of these sources that are consistent with van der laan expansion are the slower-moving, expanding blobs. i believe that the relativistically moving bullets, when they interact with these slower-moving blobs, are the genesis of the flaring that we see that seems like a re-acceleration of the emitting, relativistic particles. i note that a similar scenario could be operating in cen a and 3c454.3. this is not to say that the ”slower-moving blobs” are not themselves moving relativistically, since the bipolar lobes have significant enhancements in brightness due to relativistic doppler boosting for the blobs moving toward us. the true test of this hypothesis will require concurrent, multifrequency observations with resolutions sufficient to distinguish jet components from core emissions in galactic microquasars as well as for agn jets. one of the most remarkable sagas regarding the discovery of quasar-like activity in galactic sources comes from the decades long-investigation of sco x-1 by ed fomalont, barry geldzahler, and charlie bradshaw (fomalont, geldzahler, and bradshaw, et al. 2001). during their observations, an extended source changed relative position with respect to the primary object, disappeared, and then reappeared many times. we now know that they were observing a highly variable jet from a binary, neutron star system. the determinant observation was conducted using the very large array (vla) in socorro, new mexico and the vlba interferometer (see, e.g., beall, 2008) for a more complete discussion). the observations of the concurrent ir, optical, uv, and γ-ray variability of 3c454.3, and its associated jet launch in the mojave data, argue for a reinvestigation of these data sets in the near future. it is worthy of note that the milliarcsecond observations show a complex evolution of structure at parsec scales, including an apparently sharp change of directions associated with changes in the polarization of the radio light at that point in the jet’s evolution (see figure 2). furthermore, the multi-frequency flares reported by bonning et al. (2009) are consistent with the launch of another component of the astrophysical jet in the core region. regarding the acceleration region and the possible mechanisms for the collimation of the jets, a number of models have been proposed (see, e.g., kundt and gopal-krishna (2004), bisnovaty-kogan et al. (2002), romanova and lovelace (2009), and bisnovaty-kogan (2012) that might help explain the complexity present in these data. 3 concluding remarks the data discussed therein suggest a model for the jet structures in which beams or blobs of energetic plasmas propagate outward from the central engine to interact with the ambient medium in the source region. this ambient medium in many cases comes from prior ejecta from the central source, but can also come from clouds in the broad line region. the jet can apparently also excavate large regions, as is suggested by the complex structures in, for example, 3c120. the physical processes which can accelerate and entrain the ambient medium through which the jet propagates, have been discussed in detail in several venues (see, e.g., rose et al., 1984, 1987, beall, 1990, beall et al., 2003, and beall, 2010). in this paper, we have focused on the patterns of concurrent radio and x-ray variability for cen a, and on concurrent radio, gamma-ray, optical, ir, and uv variability for 3c454.3. the data can be interpreted as being associated with a jet-launch scenario for these sources, and this paper represents the first report of the association between a jet launch in the mojave data for 3c454.3 and its gamma-ray flare from fermi. in addition, jets from microquasars show similar patterns of variability to those of agns. these data require us to abandon our assumptions both of spherical symmetry and of single-zone productions in our models of these sources. acknowledgement the author gratefully acknowledges the support of the office of naval research for this research. this research has made use of data from the mojave database that is maintained by the mojave team (lister et al., 2009, aj, 137, 3718). the author gratefully acknowledges the data provided by the mojave team for this paper. references [1] the pierre auger collaboration, et al., 2007, science 318, 938. doi:10.1126/science.1151124 [2] bach, u., villata, m., raiteri, c. m., et al. 2006, ”structure a variability in the vlbi jet of bl lacertae during the webt campaigns (1995-2004),” a&a, 456, 105. 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[46] zanni, c., murante, g., bodo, g., massaglia, s., rossi, p., ferrari, a., 2005 astron. astrophys., 429, 399. discussion todor stanev do you expect an important role of magnetic reconnection in the particle acceleration in the jets? jim beall i do believe that magnetic reconnection plays an important part in particle acceleration, not only in the launch region, but also in the jet itself. if you recall the data i showed for 3c454.3, the region where the get seems to turn shows marked variations in brightness that seem to be associated both with the blobs from the jet traversing that region, and with the jet luminosity at the ”elbow.” in fact, it seems likely that the acceleration and collimation region of the jet in 3c454.3 extends many parsecs from the launch region. carlotta pittori can you say something about the southern jet of the crab nebula? as i actually showed at a previous vulcano workshop and promptly noticed by w. kundt, the jet orientation for x-ray images from chandra changed in the ten years from 20002010. how can this be explained? by kink instabilities? where does the field close in this system? jim beall this is only a conjecture, but if we look at the large distance where the jet in 3c454.3 changes direction, it appears that magnetic field structures can extend out to several parsecs and maintain their coherence, at least in agn sources. if the same is true in the crab, then the magnetic fields might be responsible for the changes in the jet orientation. wolfgang kundt can you tell me when and where geoff burbidge argued in favor of hadronic jets on the grounds of their stability? in my model with gopal, a pair-plasma jet is thought to be stable on the grounds of their exb drift, for example in new astronomy reviews, 2008, 52, pp 364-369. jim beall geoff burbidge’s article was published in astrophysical journal, 1956, 124, 416. that paper was in the main an argument that the energy supplied to the giant radio lobes must be of order 1060 ergs, and could only be delivered by hadronic jets. 264 introduction concurrent variability of agn jet sources as an indication of jet launch or jet-cloud interactions radio and x-ray variability measurements of centaurus 1 (ngc 5128) a jet launch coincident with the 3c454.3 multi-frequency flaring concluding remarks 200 acta polytechnica ctu proceedings 1(1): 200–204, 2014 200 doi: 10.14311/app.2014.01.0200 high-resolution x-ray spectroscopy of galactic supernova remnants satoru katsuda1, hiroshi tsunemi2 1riken (the institute of physical and chemical research), 2-1 hirosawa, wako, saitama 351-0198, japan 2department of earth and space science, graduate school of science, osaka university, 1-1 machikaneyama, toyonaka, osaka, 560-0043, japan corresponding author: katsuda@crab.riken.jp abstract high-resolution x-ray spectroscopy of galactic supernova remnants (snrs), based on grating spectrometers onboard xmm-newton and chandra, has been revealing a variety of new astrophysical phenomena. broadened oxygen lines for a northwestern compact knot in sn 1006 clearly show a high oxygen temperature of ∼300 kev. the high temperature together with a lower electron temperature (kte ∼ 1 kev) can be reasonably interpreted as temperature non-equilibration between electrons and oxygen behind a collisionless shock. an ejecta knot in the puppis a snr shows blueshifted line emission by ∼1500 km s−1. the line widths are fairly narrow in contrast to the sn 1006’s knot; an upper limit of 0.9 ev is obtained for o viii lyα, which translates to an oxygen temperature of kto < 30 kev. the low temperature suggests that the knot was heated by a reverse shock whose velocity is ∼4 times slower than that of a forward shock. anomalous intensity ratios in o vii heα lines, i.e., a stronger forbidden line than a resonance line, is found in a cloud-shock interaction region in puppis a. the line ratio can be best explained by the charge-exchange emission that should arise at interfaces between the cold/warm clouds and the hot plasma. there are several other targets for which we plan to analyze high-quality grating data prior to the operation of the soft x-ray spectrometer onboard astro-h. keywords: supernova remnants x-rays individuals: sn 1006, puppis a. 1 introduction there are many scientific motivations to perform highresolution x-ray spectroscopy of supernova remnants (snrs), since the x-ray emission is often dominated by thin thermal emission, namely line emission. for instance, accurate line widths allow us to measure the degree of temperature equilibration between electrons and ions as well as efficiency of particle acceleration. resolved fine structures of lines give us insight into emission processes. we can also reveal ejecta dynamics and measure abundances in unprecedented detail. current challenges are based on grating spectrometers onboard xmm-newton and chandra. both of the grating systems are slitless. therefore, while they work well for point-like sources or compact extended sources, they are generally not suitable for largely extended sources because off-axis emission along the dispersion direction is detected at wavelength positions shifted with respect to the on-axis source. most snrs in the large/small magellanic clouds are small enough for the gratings, and indeed over 10 papers have been published in literature (e.g., burrows et al. 2000; rasmussen et al. 2001; behar et al. 2001; van der heyden et al. 2001; 2002; 2003; flanagan et al. 2004; kosenko et al. 2008; 2011; broersen et al. 2011). a problem here is that we can not deduce spatial information, since the grating spectra are integrated for the entire snr. this causes serious ambiguities of interpretations. therefore, it is important to observe large galactic snrs for spatiallyresolved high-resolution spectroscopy. however, in this case, grating spectra suffer from spectral degradation due to the spatial extent of the source. the only solution to this dilemma is to focus on locally bright and compact features in large snrs. we here review a few successful examples of high-resolution spectroscopy of galactic snrs with the xmm-newton’s reflection grating spectrometer (rgs: den herder et al. 2001). the rgs has a large dispersion angle and is more suitable for extended sources than chandra’s grating spectrometer, although there are some nice results (lazendic et al. 2006; rutherford et al. 2013). 2 fast-moving knots in sn 1006 and puppis a a pioneering work employing the rgs to obtain highresolution spectra from galactic snrs was given by vink et al. (2003) who observed a northwestern (nw) knot in sn 1006 (see fig. 1 (a)). as shown in fig. 1 200 http://dx.doi.org/10.14311/app.2014.01.0200 high-resolution x-ray spectroscopy of galactic supernova remnants (b), the rgs spectrum showed several emission lines, including o vii heα forbidden and resonance, from the knot. by taking account of the degradation effect due to spatial extent, vink et al. (2003) found intrinsic broadening of o k-shell lines to be σ = 3.4 ± 0.5 ev. this value was later revised by the same group based on additional deep observations to σ = 2.4±0.3 ev (broersen et al. 2013). the amount of broadening corresponds to an oxygen temperature of 275+72 −63 kev, if attributed to thermal doppler broadening. on the other hand, the electron temperature is derived to be ∼1.35 kev, which is ∼200 times lower than the oxygen temperature. this temperature discrepancy is the evidence for temperature non-equilibration as is expected behind collisionless shocks; the ion temperatures (kti) immediately behind collisionless shocks are given by kti =3/16miv 2 sh, where mi is an elemental mass and vsh is a shock speed, so that the initial temperatures are proportional to particle masses. 18 19 20 21 22 23 0 0.5 1 c ou nt s s− 1 å − 1 wavelength (å) knot knot bek (a) sn 1006 (c) puppis a (b) (d) o viii ly α r f figure 1: (a) x-ray view of sn 1006 in 500–599 ev, taken from broersen et al. (2013). the rgs field of view is within the two lines. (b) rgs spectra zooming into o vii heα from the nw knot in sn 1006. the positions of the resonance (21.6å), the intercombination (21.8å), and the forbidden line (22.1å) are indicated. this figure is taken from broersen et al. (2013). (c) x-ray view of the puppis a snr in 0.5–5 kev. the rgs spectra taken from the two solid lines (hosting the knot) or dashed lines (hosting the bek) are shown in fig. 1 (d) and fig. 3, respectively. (d) rgs spectrum zooming into o k-shell lines from the ejecta knot in puppis a. in the model, the contribution from the knot is indicated as a blue line. rest-frame positions of the o viii lyα (18.9å) and the o vii heα lines are indicated as dashed lines. the blueshifts are clearly visible. along the same line, another interesting target is an ejecta knot in the northeast of the puppis a snr (see, fig. 1 (c)) whose southern portion is positionally coincident with an optical o-rich filament (the so-called ω filament which is not shown here: winkler & kirshner 1985). based on nondispersive x-ray ccds onboard xmm-newton (epic: turner et al. 2001, strüder et al. 2001), katsuda et al. (2008) noticed blueshifted k-shell lines from the knot. however, the poor energy resolution of the epic data (e/∆e ∼ 20) prevented them from conclusive arguments; the doppler velocity ranged from 1700+700 −800 km s−1 at the south of the knot, which agrees with the optical measurement of ∼1500 km s−1 (winkler & kirshner 1985), to 3400+1000 −800 km s−1 at the north of the knot. since the knot is bright and compact (∼5 times brighter than its surroundings and the size is smaller than ∼3′), the rgs is capable of yielding a highresolution spectrum at a level of e/∆e ∼ 150. thus, we performed a new xmm-newton observation, and ob201 satoru katsuda, hiroshi tsunemi tained a nice rgs spectrum as shown in fig. 1 (d). it exhibits prominent k-shell lines, including o vii heα and o viii lyα. the lines are clearly blueshifted by 1480±140±60 km s−1 (the first and second term errors are measurement and calibration uncertainties, respectively), which is fully consistent with optical measurements for the ω filament. it is also found that doppler velocities are uniform within the knot (katsuda et al. 2013b). in addition, the rgs spectra enabled us to measure line broadening to be σ < 0.9 ev at o viii lyα, indicating an upper limit of an oxygen temperature of 30 kev. interestingly, the temperature for puppis a’s knot is at least an order-of-magnitude lower than that for sn 1006’s knot, even though they are comparably fast moving. to interpret the dramatic difference in oxygen temperatures between sn 1006’s knot and puppis a’s knot, we investigate temperature equilibration through coulomb interactions behind collisionless shocks. in the calculation, we assume elemental abundances and the ionization timescales given in the literature (table 1 in broersen et al. 2013 for sn 1006 and table 2’s case-b in katsuda et al. 2013b for puppis a). also, since the degree of electron heating at collisionless shocks is not yet understood well, we examined various initial electronto-proton temperature ratios, te/tp = β, for each shock speed. in this way, we ran calculations for several shock speeds. figure 2 shows the best-representative models, where temperature curves are illustrated only for electrons (black) and oxygen (red). for comparison, we also show model curves with β = me/mp. we find that the data require fairly different shock speeds; a fast (∼3000 km s−1) shock for sn 1006 and a relatively slow (∼600 km s−1) shock for puppis a. also, the values of β are obtained to be ∼0.06 for sn 1006 and less than ∼0.5 for puppis a. these values roughly agree with an observational trend shown in van adelsberg et al. (2008). furthermore, the value for sn 1006 is consistent with a direct measurement from hα spectroscopy for the optical filament (β < 0.07: ghavamian et al. 2002). on the other hand, it is interesting to note that our best-estimated value of 0.06 is higher than a recent theoretical prediction, β = 0.023 for vsh > 1500 km s−1 (ohira & takahara 2008). we will revisit this issue in our future work. the inferred shock velocity for sn 1006 is roughy consistent with the proper motion of the shock ahead of the knot (winkler et al. 2003; katsuda et al. 2013a). therefore, a simple interpretation is that the knot was heated by a forward shock. however, we cannot rule out a possibility of reverse-shock heating. in fact, the knot shows an elevated si abundance, suggesting that it originates from the sn ejecta that should have been heated by a reverse shock. in this case, the (reverse) shock velocity should be higher than ∼5000 km s−1 (see, the discussion in katsuda et al. 2013b). such a fast shock requires an oxygen temperature of ∼800 kev. this is significantly higher than the x-ray measurement, thereby a significant fraction of the shock energy may go into cosmic-rays. if true, this suggests efficient cosmic-ray acceleration at the reverse shock. as for puppis a, the inferred shock velocity, ∼600 km s−1, is less than the shocked-gas velocity, ∼2000 km s−1, derived by the doppler velocity of ∼1500 km s−1 and the optical proper motion of ∼1250 km s−1 at a distance of 2.2 kpc (winkler et al. 1988). this is consistent with a picture that the ejecta knot was heated by a reverse shock rather than a forward shock, since the forward shock velocity should be ∼2700 km s−1 (= 4/3 × 2000 km s−1 according to the rankine-hugoniot relation). 109 1010 1011 1012 1 10 100 kt ( ke v ) net (cm−3s) oxygen electron vshock = 3000 km s−1 solid line: β = 0.06 dotted line: β = me/mp 109 1010 1011 1012 0.1 1 10 kt ( ke v ) net (cm−3s) oxygen electron vshock = 600 km s−1 solid line: β = 0.5 dotted line: β = me/mp sn 1006 puppis a figure 2: temperature histories for electrons (black) and oxygen (red) as a function of net. left and right panels are for the nw knot in sn 1006 and the ejecta knot in puppis a, respectively. 202 high-resolution x-ray spectroscopy of galactic supernova remnants 3 cloud-shock interaction regions in puppis a possible sites for high-resolution spectroscopy of galactic snrs are not only ejecta knots but also swept-up ism regions. in particular, cloud-shock interaction regions in the puppis a snr are promising, because they are bright and compact (e.g., hwang et al. 2005). so far, rgs spectra taken from the bright eastern knot (bek) and the northern knot were presented by katsuda et al. (2012). in fig. 3, we show one of the bek spectra focusing on the o vii heα lines, which was taken from the region within the dashed lines in fig. 1 (c). interestingly, we see a strong forbidden line with respect to the resonance line. this is inconsistent with any thermal emission models with reasonable plasma parameters (i.e., kte = 0.3–0.7 kev and net = 1010–5×1011 cm−3 s). after considering a few possibilities to reproduce the anomalous line ratio, katsuda et al. (2012) proposed that the charge-exchange emission, that arises at interfaces between the cold/warm clouds and the hot plasma, can best explain the data. this would support a long-standing expectation of chargeexchange x-ray emission in snrs. 21 21.5 22 22.5 0 0.5 1 c ou nt s s− 1 å − 1 wavelength (å) puppis a bek f i r figure 3: rgs spectrum zooming into o vii heα from the bek in puppis a. the positions of the resonance (21.6å), the intercombination (21.8å), and the forbidden line (22.1å) are indicated. 4 future prospects there are several nice rgs data sets of galactic snrs that are waiting for being analyzed. these include bright shells of rcw 86, an equatorial belt in g292.0+1.8, and a southwestern knot in the cygnus loop. in addition, it is worth while to search for other promising targets and observe them. we are planning to analyze the rgs data in the near future. the rgsbased study is a great pathfinder for the coming highresolution x-ray spectroscopy of snrs with the nondispersive soft x-ray spectrometer (mitsuda et al. 2010) onboard astro-h (takahashi et al. 2012). acknowledgement s.k. is supported by the special postdoctoral researchers program in riken. this work is partly supported by a grant-in-aid for scientific research by the ministry of education, culture, sports, science and technology (23-000004 and 24-8344). references [1] behar, e., et al. 2001, a&a, 365, l242 [2] broersen, s., et al. 2011, a&a, 535, 11 [3] broersen, s., et al. 2013, a&a, 552, 9 [4] burrows, d. n., et al. 2000, apj, 543, l149 doi:10.1086/317271 [5] den herder, j. w., et al. 2001, a&a, 365, l7 [6] flanagan, k. a., et al. 2004, apj, 605, 230 doi:10.1086/382145 [7] ghavamian, p., et al. 2002, apj, 572, 888 doi:10.1086/340437 [8] hwang, u., et al. 2005, apj, 635, 355 doi:10.1086/497298 [9] katsuda, s., et al. 2008, apj, 678, 297 doi:10.1086/586891 [10] katsuda, s., et al. 2012, apj, 756, 49 doi:10.1088/0004-637x/756/1/49 [11] katsuda, s., et al. 2013a, apj, 763, 85 doi:10.1088/0004-637x/763/2/85 [12] katsuda, s., et al. 2013b, apj, 768, 182 doi:10.1088/0004-637x/768/2/182 [13] kosenko, d., et al. 2008, a&a, 490, 223 [14] kosenko, d., et al. 2011, a&a, 532, 114 [15] lazendic, j. s., et al. 2006, apj, 651, 250 doi:10.1086/507481 [16] mitsuda, k., et al. 2010, spie, 7732, 773211 [17] ohira, y., & takahara, f. 2008, apj, 688, 320 doi:10.1086/592182 [18] rasmussen, a. p., et al. 2001, a&a, 365, l231 [19] rutherford, j., et al. 2013, apj, 769, 64 doi:10.1088/0004-637x/769/1/64 203 http://dx.doi.org/10.1086/317271 http://dx.doi.org/10.1086/382145 http://dx.doi.org/10.1086/340437 http://dx.doi.org/10.1086/497298 http://dx.doi.org/10.1086/586891 http://dx.doi.org/10.1088/0004-637x/756/1/49 http://dx.doi.org/10.1088/0004-637x/763/2/85 http://dx.doi.org/10.1088/0004-637x/768/2/182 http://dx.doi.org/10.1086/507481 http://dx.doi.org/10.1086/592182 http://dx.doi.org/10.1088/0004-637x/769/1/64 satoru katsuda, hiroshi tsunemi [20] strüder, l., et al. 2001, a&a, 365, l18 [21] takahashi, t., et al. 2012, spie, 8443, 84431z [22] turner, m. j. l., et al. 2001, a&a, 365, l27 [23] van adelsberg, m., et al. 2008, apj, 689, 1089 doi:10.1086/592680 [24] van der heyden, k. j., et al. 2001,a&a,365,l254 [25] van der heyden, k. j., et al. 2002,a&a,392,955 [26] van der heyden, k. j., et al. 2003,a&a,406,141 [27] vink, j., et al. 2003, apj, 587, l31 doi:10.1086/375125 [28] winkler,p.f. & kirshner,r.p. 1985,apj,299,981 [29] winkler, p. f., et al. 1988, iau colloq. 101: 65 [30] winkler, p. f., et al. 2003, apj, 585, 324 doi:10.1086/345985 204 http://dx.doi.org/10.1086/592680 http://dx.doi.org/10.1086/375125 http://dx.doi.org/10.1086/345985 introduction fast-moving knots in sn 1006 and puppis a cloud-shock interaction regions in puppis a future prospects acta polytechnica ctu proceedings doi:10.14311/app.2017.8.0005 acta polytechnica ctu proceedings 8:5–7, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app adhesion of biocompatible tinb coating tomas kolegara,∗, martin matouseka, monika vilemovab, vladimir starya a faculty of mechanical engineering, department of material engineering, czech technical university in prague, charles square 13, 121 35 prague, czech republic b institute of plasma physics as cr, v.v.i. ∗ corresponding author: tomas.kolegar@fs.cvut.cz abstract. preparation of a coating with a high quality requires good adhesion of the film to the substrate. the paper deals with the adhesion of biocompatible tinb coating with different base materials. several materials such as titanium cp grade 2, titanium alloys ti6al4v and stainless steel aisi 316l were measured. testing samples were made in the shape of small discs. those samples were coated with a tinb layer by using the pvd method (magnetron sputtering). onto the measured layer of tinb an assistant cylinder was stuck using a high strength epoxy adhesive e1100s. the sample with the assistant cylinder was fixed into a special fixture and the whole assembly underwent pull-off testing for adhesion. the main result of this experiment was determining the strength needed to peel the layer and morphology and size of the breakaway. as a result, we will be able to determine the best base material and conditions where the coating will be remain intact with the base material. keywords: pvd coating, adhesion, biocompatible materials, pull-off test, titanium, niobium. 1. introduction today's civilized society brings human kind many simplifications for numerous activities in every day life. due to this comfort more civilization illnesses appear, such as obesity, cancer, atherosclerosis, heart attack and of course musculoskeletal diseases including joints and tendons, but also chronic stress and sports injuries. high life expectancy on other hand causes faster aging of tissue and makes surgery of hip, shoulder and other joints necessary. one solution to help with this this health problem is the utilization of implants. nowadays, commonly used implants are made of lower quality material like stainless steel and these implants are coated with a high quality biocompatible material such as tinb and also other titanium alloys. the most important property of the coating is its adhesion to the base material. the main quality of the parameters for adhesion are the substrate structural properties, purity and surface condition at the time of coating formation, the value of the kinetic energy of falling atoms and ions to the surface, and also the forming a coating on the support surface and the other deposition parameters. according to g. rosenman, the minimum adhesion strength of biocompatible coating to the substrate is 15 mpa [1] and cells have better conditions for adhesion, growth and their establishment in the living body. the goal of this experiment is to verify if the coating is capable of withstanding the strain which can be found in the human body. each human body and conditions inside are very individual and results depend on many factors [2]. 2. materials and procedure for the experiment three base materials were used. titanium cp grade 2, ti6al4v and stainless steel aisi 316l. chemical composition of these materials is shown in table 1, 2 and 3 [3]. experimental samples (discs of diameter 14 mm and 4 mm thickness) were coated with tinb (61 wt % of ti and 39 wt % of nb). the pvd magnetron sputtering method was used [4]. final thickness of the coating was measured by calotest (csm, switzerland) and it was 2.4 ± 0.1 µm. the screw according to din 931 with a 10 mm metric thread was used as the assistant cylinder. these two parts were glued together with high strength epoxy adhesive e1100s with a minimum ultimate tensile strength 70 mpa. the glue was cured in a furnace for 1 hour at 140 ◦c. the pull-off test performed on the available samples was according to en iso 4624:2003 [5, 6]. table 4 presents the measured parameters of the experiment, especially the force when the tested sample was broken. ultimate tensile strength and the average value were measured. 3. results of the experiment (morphology and tensile strength) results of the experiments can be seen in figures 1, 2 and 3. note: the most suitable sample was chosen. black spot indicates detachment of coating. 5 http://dx.doi.org/10.14311/app.2017.8.0005 http://ojs.cvut.cz/ojs/index.php/app t. kolegar, m. matousek, m. vilemova, v. stary acta polytechnica ctu proceedings c n mn p s cr mo ni cu si fe 0.022 0.094 1.75 0.021 0.001 17.18 2.71 14.1 0.06 0.35 rest table 1. chemical composition of aisi 316l [wt %] c n o h fe al v ni mo other ti 0.08 0.03 0.25 0.0125 0.3 rest table 2. chemical composition of titanium cp grade 2 [wt %] figure 1. stainless steel aisi 316l. figure 2. titanium cp grade 2. 4. conclusions • average uts on fe-material was measured (22.48 mpa). . coating stayed on sample. • average uts on ti-material was measured (19.30 mpa). . coating was partially removed. • average uts on ti6al4v-material was measured (34.27 mpa). . large part of coating was removed. figure 3. titanium alloys ti6al4v. ultimate tensile strength of epoxy adhesive e1100s specified by manufacturer is 70 mpa. in the experiment, we achieve 34 mpa in the best result (ti6al4v) while all three testing materials should withstand more than 15 mpa which is the minimum adhesion strength according to g. rosenman [1]. each human body is very individual and we must be sure that implants withstand all the processes in the human body. high values of uts approaching the values set up by manufacturer are more than is required. generally, on a surface with high roughness the adhesion is also higher. further experiments will involve changing parameters of the surface roughness, combination of epoxy adhesion and film adhesion. an ultimate tensile strength of coating at least higher than 50 mpa should be achieved. list of symbols f force [n] ra roughness average [µm] uts ultimate tensile strength [mpa] acknowledgements this work was supported by project lo1207, program npu1, from the ministry of education, youth and sports of the czech republic and by czech science foundation project no. 15-01558s. 6 vol. 8/2017 adhesion of biocompatible tinb coating c n o h fe al v ni mo other ti 0.08 0.05 0.13 0.012 0.25 6.5 4.5 rest table 3. chemical composition of ti6al4v [wt %] sample f ra uts average uts stand. deviation [n] [µm] [mpa] [mpa] [mpa] aisi 316l 1 1540 0.06 ± 0.01 19.62 22.48 2.592 1950 24.84 3 1990 25.35 ti (cp2) 1 1040 13.25 19.30 4.942 1490 18.98 3 1990 25.35 ti6al4v 1 3160 40.25 34.27 4.902 2630 33.50 3 2220 28.28 table 4. table of measured parameters references [1] n. eliaz, o. ritman-hertz, d. aronov, et al. the effect of surface treatments on the adhesion of electrochemically deposited hydroxyapatite coating to titanium and on its interaction with cells and bacteria. journal of materials science: materials in medicine 22(7):1741–1752, 2011. 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[2] e. eisenbarth, d. velten, m. müller, et al. biocompatibility of β-stabilizing elements of titanium alloys. biomaterials 25(26):5705 – 5713, 2004. doi:http://doi.org/10.1016/j.biomaterials.2004.01.021. [3] s. guo, j. zhang, x. cheng, x. zhao. a metastable β-type ti-nb binary alloy with low modulus and high strength. journal of alloys and compounds 644:411 – 415, 2015. doi:http://doi.org/10.1016/j.jallcom.2015.05.071. [4] k.-t. k. chiang, r. wei. growth morphology and corrosion resistance of magnetron sputtered cr films. surface and coatings technology 206(7):1660 – 1665, 2011. doi:http://doi.org/10.1016/j.surfcoat.2011.09.020. [5] b. jönsson, s. hogmark. hardness measurements of thin films. thin solid films 114(3):257 – 269, 1984. doi:http://dx.doi.org/10.1016/0040-6090(84)90123-8. [6] x. dai, a. zhou, l. feng, et al. molybdenum thin films with low resistivity and superior adhesion deposited by radio-frequency magnetron sputtering at elevated temperature. thin solid films 567:64 – 71, 2014. doi:http://doi.org/10.1016/j.tsf.2014.07.043. 7 http://dx.doi.org/10.1007/s10856-011-4355-y http://dx.doi.org/http://doi.org/10.1016/j.biomaterials.2004.01.021 http://dx.doi.org/http://doi.org/10.1016/j.jallcom.2015.05.071 http://dx.doi.org/http://doi.org/10.1016/j.surfcoat.2011.09.020 http://dx.doi.org/http://dx.doi.org/10.1016/0040-6090(84)90123-8 http://dx.doi.org/http://doi.org/10.1016/j.tsf.2014.07.043 acta polytechnica ctu proceedings 8:5–7, 2017 1 introduction 2 materials and procedure 3 results of the experiment (morphology and tensile strength) 4 conclusions list of symbols acknowledgements references acta polytechnica ctu proceedings doi:10.14311/ap.2016.4.0073 acta polytechnica ctu proceedings 4:73–79, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app cfd simulation of upward subcooled boiling flow of freon r12 tomas romsy∗, pavel zacha faculty of mechanical engineering, czech technical university in prague, technická 4, prague 6, 166 07, czech republic ∗ corresponding author: tomas.romsy@fs.cvut.com abstract. subcooled flow boiling under forced convection occurs in many industrial applications to maximize heat removal from the heat source by the very high heat transfer coefficient. this work deals with cfd simulations of the subcooled flow boiling of refrigerant r12 solved by code ansys fluent r16. the main objective of this paper is verification of used numerical settings on relevant experiments performed at debora test facility. also comparisons with previously provided simulation on nri rez are presented. data outputs from this work are basis to subsequent calculations of steam-water mixture cooling of pb-li eutectic. keywords: cfd simulation, subcooled boiling, freon r12. 1. introduction subcooled flow boiling can solve a wide range of high power thermal challenges in the following areas: central processing unit (cpu) and computational application specific integrated circuits (asics) [1, 2], ultra-high brightness light emitting diodes (leds) and lasers sources [3], automotive power electronics [4], or avionics [5], where research findings have made possible the development of a new generation of cooling hardware, which promises order of magnitude increase in heat dissipation compared to today’s cutting edge cooling schemes. subcooled flow boiling is expected to realize the high heat flux cooling for electronic devices [6, 7], or for high heat flux cooling in microgravity [8]. subcooled flow boiling also plays a significant role in case of cooling of plasma facing component of thermonuclear reactors. the subcooled flow boiling is a high complex form of two-phase liquid flow in which the single-phase flow merges into the two-phase flow and back to the singlephase flow. a local appearance and disappearance of the two-phase flow allow the use of the latent heat of vaporization for a heat removal from the surface into the liquid without causing the boiling crisis. in comparison with a single-phase fluid it represents the efficient way to improve heat transfer from the wall to the flowing liquid. therefore, it provides an ability of the sufficient heat transfer at high heat fluxes. detailed investigation of this phenomenon can help for its better understanding to make wider improvement. one of the perspective application of subcooled flow boiling is so-called cold trap facility. this device serves for corrosion impurity separation from the metal eutectic (pb, pb-li), whereas the separation is carried out by the cooling of the eutectic down to the required temperature. this facility considered in centre of advanced nuclear technology project (canut) [10] provides sufficient heat removal from eutectic across the wall to the subcooled steam-water mixture (cooling loop) and subsequently to the tertiary water loop providing ultimate heat removal. part of the cold trap design is cooling concept which strongly depends on steam-water mixture behaviour. description of cooling loop behaviour is provided with the aid of computational fluid dynamics (cfd) code ansys fluent. verification of suitable numerical settings and computational methodology should be determined in the first step. selected experiments on the debora facility were used for this purpose. a detailed description of this device can be found in [11] and [9]. debora project at cea grenoble (french alternative energies and atomic energy commission) was focused on determination of subcooled boiling character by using refrigerant dichlorodifluoromethane (r12). provided experiment outputs contain especially void fraction, gas velocity, temperature of the fluid and the bubble size. because both freon r12 and water have relative physical similarity, we can use this freon for his lower operating parameters in comparison with water. this leads to a much simpler and safer measurements. the geometry of the debora facility is shown in figure 1. it is the vertical heated tube with inner diameter of 19.2 mm. freon is heated along the 3.5 m long part of pipe. the rest of 5 m long tube is unheated. it corresponds to 1 m of inlet section and 0.5 m of outlet section. a radial profile of the vapour volume fraction and its speed at the end of the heated part were measured by optical probe. additionally, the bubble size profiles were available for this area. axial wall temperatures were measured using thermocouples, but radial temperatures were not available [9]. cfd model was performed based on the debora facility parameters and the boundary conditions and standard numerical approaches were set according to the experiment conditions. the results from simula73 http://dx.doi.org/10.14311/ap.2016.4.0073 http://ojs.cvut.cz/ojs/index.php/app tomas romsy, pavel zacha acta polytechnica ctu proceedings figure 1. a) sketch of the debora test geometry [9] b) computational model sketch with detail of used grid. measured quantity p [mpa] v [m/s] qw [w/m2] tin [◦c] tsat [◦c] case 1 3.008 0.86 58 260 67.89 94.24 case 2 3.006 0.891 58 260 73.7 94.21 table 1. specified conditions of the chosen experimental cases. tions provided at nuclear research institute rez (nri rez) [12] are included in section 4 for better comparison. main purpose of this comparison are different approaches in calculation which lead to opportunity to compare them. while the previous simulation from nri rez was performed at ansys fluent r13, presented work was processed at ansys fluent r16. earlier release 13 missed necessary subcooling numerical models and these calculations were implemented by individual user defined functions (udf). however, starting from release 15, numerical models describing this phenomenon are implemented internally. the main output of this work is to determine selected parameters (pressure, velocity, temperatures) in the specified geometry position and compare them against the measured experimental data provided from debora test facility and against the previously calculated values from nri rez simulations. 2. model description simulation model is based on geometry of the debora experimental device. the 10° v-cutout, shown in figure 1, was considered due to the symmetry and to reduce the computational time. slightly rough hexahedral grid was tested in the first steps of the calculation. further enhancements were applied after obtaining better knowledge of the calculation behaviour on this grid. also much finer grid was tested. this grid was only the 10° v-cutout of tested geometry for computational time reduction due to a greater number of cells closer to the wall. however, there was a too small angle of the tip in the axis (centre of the tube) and therefore a smooth auxiliary wall had to be applied with tip neglecting. as the result, flow cross-section has been little changed, but hexahedral cells could be used for the whole geometry. the simulation results for this grid were similar to case with 45° v-cutout geometry. the 45° v-cutout grid has been selected for the final evaluation of the results, because no geometry adjustments are used there. also, it is not appropriate to use fine meshes with respect to numerical approach for the used boiling computational model, like accretion of bubbles near the wall etc. this final grid contains 90 000 hexahedral cells with their higher concentration in the wall vicinity, shown in figure 1. cells quality was evaluated for equi-size skew, which does not exceed value of 0.5 and by the aspect-ratio with the maximum of 10.3. two cases with different boundary conditions based on the debora experiments are considered. the first one – case 1 – has a much larger subcooled inlet state then the case 2, but the saturation conditions and heat flux are almost the same for both of them. the main specified conditions of these experiments are given by table 1 and setting of the boundary conditions in the simulation model corresponds with them. usage of these two experimental cases brings the opportunity to try if the simulation model can solve various ratio of boiling states; from subcooled up to almost boiling crisis – departure from nucleate boiling (dnb). the physical values setting for the freon r12 liquid and vapour is based on these conditions. therefore linear functions depending on the temperature were used for density, specific heat capacity, viscosity and thermal conductivity. these quantities were obtained from nist database [13]. 74 vol. 4/2016 cfd simulation of upward subcooled boiling flow of freon r12 setting of the model boundary conditions: • inlet: velocity inlet – the same speed for both phases turbulence intensity – estimated at 3 % • outlet: pressure outlet – 0 backflow volume fraction • heated wall: heat flux the measuring line was created on one symmetry wall directly at the interface between the heated and outlet non-heated section. this line contains 11 radially distributed evaluation points which were created to monitor calculated data. they are situated in the centre of each appropriate cell and their distribution is shown in the figure 2. radial distance in [m] . ........ . . figure 2. distribution of the evaluation points. 3. solver setting the solver setting is mainly supported by the documentation [12, 14–17]. time dependent solution has to be considered with time step set to 0.01 s for each calculated case. the realizable k−ε turbulence model with the non-equilibrium wall function has been chosen. this turbulence model is solved for each phase, but the wall function is calculated only for singlephase. the multiphase coupled model was used for the sequential solution of velocity and pressure fields and the least square cell-based method was set for gradients. all discretization schemes were set to 1st order, otherwise the simulation is very susceptible to the formation and disintegration of bubbles along the simulation domain. calculations were carried out on the sixteen intel xeon e5-2660 processors. the complete final calculation took about 8 hours of computer time for each case. setting of boiling in ansys fluent 16: multiphase eulerian – rpi boiling model this boiling model is appropriate to use for subcooled flow, where condition tsat − tbulk > 3 k is fulfilled. model does not calculate the vapour temperature, but it is fixed at the saturation temperature instead. as an alternative, non-equilibrium boiling model can be used with criterion tsat − tbulk ≤ 3 k, where the vapour temperature is included in the solution process. this condition could occur at the higher model levels, where the liquid can be already sufficiently heated close to saturation conditions. however, the rpi boiling model is considered for the next steps of this work. figure 3 shows scheme of the selected submodels for rpi boiling model. figure 3. scheme of the selected sub-models for rpi boiling model. the wall lubrication model (effect of virtual mass) was neglected, because of big impact to the solution grid fineness, which is not very desirable for the model. 4. calculation results the results of performed calculations are compared with data calculated by nri rez (ansys fluent r13) and measured values from the debora experiment given by [12]. the radial profiles of important monitored parameters for both calculated cases are described below. these profiles are obtained from measuring line, for contained evaluation points respectively. dispositional (orthographic) views are also given for contours of selected parameters in the computational area, see figure 12. if they had not been applied, the side view would have showed just the long and thin tube with nothing obvious to see in the 75 tomas romsy, pavel zacha acta polytechnica ctu proceedings computational domain. given the similarity of the boiling behaviour of both cases, only results for case 1 are listed. 4.1. radial temperature profiles unfortunately due to unavailable experimental data for radial temperature profiles, only the comparison with the results provided by nri rez is mentioned. for both calculated cases the evaluated radial profile has a similar course, as shown in figure 4 for case 1 and in figure 5 for case 2. . . . . . . . . . . . . . . . . . . . . . . figure 4. radial temperature profile, case 1. . . . . . . . . . . . . . . figure 5. radial temperature profile, case 2. only slight differences between the temperature values obtained by nri rez and calculation up to 0.78 ◦c in the fluid midstream and up to 1.36 ◦c near the wall for case 1 are seen. as regards the case 2, here is obvious difference between temperature profiles in the midstream. the nri rez results for case 2 are very close to saturation temperature almost across the whole radial profile, except the wall. the character of ctu calculation temperature profile has a decreasing character up to the axis – tube centre (little bit subcooled state). but near the axis the temperature difference does not exceed 0.58 ◦c. 4.2. radial void fraction profile radial profiles for void fraction with measured data and also nri rez results have been compared already. this is shown in figure 6 (case 1 ) and figure 7 (case 2 ). in case 1 is seen that all the data are in good agreement near the wall, but the curves have slightly different courses closer to axis – tube centre. in case of this work, such disagreement is probably caused by collecting of non-condensed secondary phase in the midstream and efforts of liquid go closer toward the wall. this can be seen from void fraction rendered along the calculated area in section 4.5, where the results evaluation along the model is described. figure 6. radial void fraction profile, case 1. figure 7. radial void fraction profile, case 2. 76 vol. 4/2016 cfd simulation of upward subcooled boiling flow of freon r12 the greater disagreement with other data is obvious for case 2. the ctu simulation model estimates almost abrupt increase of void fraction near the heated wall pretty well. but in the midstream the void fraction profile is lower than the others. this probably correlates with the results for temperature quite well. for the treatment of such disagreements it would be possible to try a different approach in model setting, or using of non-equilibrium boiling model for a future simulations respectively. 4.3. radial vapour velocity profile vapour velocity radial profile comparison for case 1 is illustrated in figure 8. it can be seen that the ctu and nri rez results have similar character, but compared with the measurement they have a higher drop of vapour velocity in the fluid midstream. this is probably caused by using of non-ideal single phase wall function. this will be the subject of further investigation in a future simulations. figure 8. radial vapour velocity profile, case 1. in case 2, see figure 9, it is well visible that curve of ctu calculation follows the measured data near the wall pretty well. on the other hand, the same problem as in the previous case occurs in the fluid midstream. figure 9. radial vapour velocity profile, case 2. 4.4. radial bubble diameter profile very important parameter in terms of subcooled boiling behaviour is diameter of vapour bubbles. for experiment measured data; the sauter mean diameter is defined as the diameter of a sphere, which has the same ratio of volume and surface area as the base particle (bubble) and the average diameter dg is the diameter of the bubble, which would have the equivalent two-phase flow with the same density of bubbles amount, the same density of interfacial area and the same diameter for all bubbles, see [12]. for case 1, the results are depicted in figure 10. here is evident that the bubble diameters along the radius have similar size and character as the measured data. it means that the bubbles are breaking up near the wall and their diameter is increasing in the centre of the stream. slighter difference in the fluid midstream probably corresponds with the above listed diagram for void fraction. also bubble diameter along the tube for this case is shown in figure 12. figure 10. radial bubble diameter profile, case 1. figure 11. radial bubble diameter profile, case 2. the results for case 2, shown in figure 11, are in very good agreement with experiment – dg and nri rez near the wall. whereas the bubble diameters in the midstream have little bit lower values compared with other data, they are still in very good agreement 77 tomas romsy, pavel zacha acta polytechnica ctu proceedings figure 12. axial liquid temperature, void fraction and bubble diameter, case 1. with experiment – dg, because it is seen, that the character of radial profile have nearly the same course. smaller values for bubbles are probably caused by lower temperature of fluid in the midstream, shown in figure 5. therefore, the question of using the non-equilibrium boiling model arises here. 4.5. axial results profiles figure 12 (case 1 ) due to similarity of the both cases of boiling behaviour mentioned above is presented for a better understanding, how the fluid behaves along the tube and where boiling occurs. there are orthographic views for the fluid temperature, void fraction and bubble diameters. there is visible, that all of these quantities correlate with each other. for example; the fluid temperature approximately in the middle of the model reaches the saturation condition near the wall and the void fraction begins to occur there. the higher level the fluid stream in tube reaches, the higher temperature in the midstream occurs. it also means, that the higher concentration of void fraction is there. on the profile of bubble diameters, it is shown how to bubbles reach the greater diameters in the higher levels of the tube and how they are trying to get into the centre of fluid stream. considering this view, it should be observed, that for setting of bubbles modelled by yao-morel model, the smallest possible value of the bubbles have to be set. for both cases this value was set to −105 m. 5. conclusion the main goal of this work was to try the possibility to utilize the newly implemented boiling models in cfd solver ansys fluent r16. the debora experiments were chosen for comparison with data received from these simulations. some of the earlier works, such as nri rez (fluent r13), were also tried to simulate boiling experiments by using older version of fluent cfd solver. however, suitable boiling models had to be supplied by user defined functions (udf) in this earlier version. for comparison, how the solver with newly implemented boiling models (fluent r16) stand up against the older version with udf’s, the evaluation of these data compared with ctu is described. two cases (case 1 and case 2 ) of debora experiments were chosen. only inlet conditions for fluid temperature are different in these two cases. it means that the first one is much more subcooled case then the second one. the comparison between measured data, calculations from nri rez and results of this work are in the high level of agreement. only few small differences occur. the vapour velocity disagreement of both calculations can be primarily caused 78 vol. 4/2016 cfd simulation of upward subcooled boiling flow of freon r12 by numerical approach, or by using of non-ideal single phase wall function respectively. also, for radial void fraction closer to axis the curve have slightly different course compared to experiment and nri rez. this disagreement is probably caused by collecting of non-condensed secondary phase in the midstream and effort of liquid go closer toward the wall. and also in case 2 the void fraction has the lower values in the fluid midstream. therefore the question of using the non-equilibrium boiling model arises here. it will be subject of further research, because it can treat the fact, that for case 2 the midstream fluid temperature could reache the values close to saturation conditions in the measured section. after evaluation of all the results we can say, that the cfd solver with newly implemented boiling models (fluent r16) can be successfully used for problems where the subcooled boiling occurs. but some minor deficiencies are still present. unfortunately due to very complicated and sensitive numerical model used for description of this boiling phenomenon, there are many degrees of freedom at the model settings. also variables that are tracked interact with each other and individual numerical approaches have limited validity. this leads to time-consuming study to solve these minor deficiencies and verifying all of the used hypotheses (and their interaction) by experiments. all the knowledge and experiences described above are currently being used for simulations of more complicated situation of subcooled boiling of water, which occurs for example in pb-li cold trap cooling system, and they are continuously being improved. list of symbols p pressure [mpa] v inlet liquid velocity [m/s] qw heat flux [w/m2] t temperature [°c] tin inlet liquid temperature [°c] tbulk bulk liquid temperature [°c] tsat saturation temperature [°c] % liquid density [kg/m3] cp specific heat capacity [kj/kg k] ν dynamic viscosity [pa s] λ thermal conductivity [w/m k] references [1] s. g. kandlikar. high flux heat removal with microchannels – a roadmap of challenges and opportunities. heat transfer engineering 26(8):5–14, 2005. doi:10.1080/01457630591003655. [2] n. khan, k. c. toh, d. pinjala. boiling heat transfer enhancement using micro-machined porous channels for electronics cooling. heat transfer engineering 29(4):366–374, 2008. doi:10.1080/01457630701825481. [3] a. bar-cohen, p. wang, e. rahim. thermal management of high heat flux nanoelectronic chips. microgravity science and technology 19(3):48–52, 2007. doi:10.1007/bf02915748. [4] f. ramstorfer, h. steiner, g. brenn, et al. subcooled boiling flow heat transfer from plain and enhanced surfaces in automotive applications. asme j heat transfer 130(1), 2008. doi:10.1115/1.2780178. [5] i. mudawar. assessment of high-heat-flux thermal management schemes. ieee transactions on components and packaging technologies 24(2):122–141, 2001. doi:10.1109/6144.926375. [6] j. l. parker, m. s. el-genk. enhanced saturation and subcooled boiling of fc-72 dielectric liquid. international journal of heat and mass transfer 48(18):3736–3752, 2005. doi:10.1016/j.ijheatmasstransfer.2005.03.011. [7] y. madhour, j. olivier, e. costa-patry, et al. flow boiling of r134a in a multi-microchannel heat sink with hotspot heaters for energy-efficient microelectronic cpu cooling applications. ieee transactions on components, packaging and manufacturing technology 1(6):873–883, 2011. doi:10.1109/tcpmt.2011.2123895. [8] k. suzuki, h. kawamura. microgravity experiments on boiling and applications: research activity of advanced high heat flux cooling technology for electronic devices in japan. annals of the new york academy of sciences 1027(1):182–195, 2004. doi:10.1196/annals.1324.017. [9] e. krepper, r. rzehak. cfd for subcooled flow boiling: simulation of debora experiments. nuclear engineering and design 241(9):3851–3866, 2011. doi:10.1016/j.nucengdes.2011.07.003. [10] o. frybort. background report – pb-li17 cold trap. nuclear research centre rez, 2014. [11] j. garnier, e. manon, g. cubizolles. local measurements on flow boiling of refrigerant 12 in a vertical tube. multiphase science and technology 13(1&2), 2001. doi:10.1615/multscientechn.v13.i1-2.10. [12] l. vyskočil. simulation of the subcooled boiling in fluent 13. nuclear research institute rez, 2011. [13] e.w. lemmon, m.o. mclinden, d.g. friend. thermophysical properties of fluid systems. in nist chemistry webbook, nist standard reference database number 69, p. linstrom, w. mallard (eds.). national institute of standards and technology. http://webbook.nist.gov. [14] t. romsy, p. zacha. cfd simulation of subcooled boiling, 2016. erin, the 8th international conference for young researchers and phd students, april 23–25, 2014, blansko, czech republic. [15] ansys, inc. fluent user’s guide, 2013. release 15.0. [16] ansys, inc. fluent theory guide, 2013. release 15.0. [17] ansys, inc. fluent multiphase 15.0 optional lecture 03 – wall boiling models: training materials, 2014. 79 http://dx.doi.org/10.1080/01457630591003655 http://dx.doi.org/10.1080/01457630701825481 http://dx.doi.org/10.1007/bf02915748 http://dx.doi.org/10.1115/1.2780178 http://dx.doi.org/10.1109/6144.926375 http://dx.doi.org/10.1016/j.ijheatmasstransfer.2005.03.011 http://dx.doi.org/10.1109/tcpmt.2011.2123895 http://dx.doi.org/10.1196/annals.1324.017 http://dx.doi.org/10.1016/j.nucengdes.2011.07.003 http://dx.doi.org/10.1615/multscientechn.v13.i1-2.10 http://webbook.nist.gov acta polytechnica ctu proceedings 4:73–79, 2016 1 introduction 2 model description 3 solver setting 4 calculation results 4.1 radial temperature profiles 4.2 radial void fraction profile 4.3 radial vapour velocity profile 4.4 radial bubble diameter profile 4.5 axial results profiles 5 conclusion list of symbols references acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0053 acta polytechnica ctu proceedings 7:53–57, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app righting of chinese mitten crabs (eriocheir sinensis) and their models tobias riphausa,∗, florian hoffmannb, susanna labischb a international degree course in biomimetics, city university of applied science bremen, germany b biomimetics-innovation-centre (b-i-c), city university of applied science bremen, germany ∗ corresponding author: t. riphaus via slabisch@bionik.hs-bremen.de abstract. the usage of unmanned underwater vehicles for marine tasks is continuously growing and bioinspired stabilizing systems shall help them to gain and keep a stable position during work. therefore the righting maneuver of e. sinensis has been studied. these crabs are able to perform a 180◦-rotation with an angular velocity of 4.30 s−1 when falling underwater from a supine starting position. high-speed particle image velocimetry has shown, that propulsive forces with a peak of 0.021 ± 0.001 n were produced by the hind legs to initiate and stop the rotation. in a numerical multibody simulation a constant force of 0.009 n acting for 0.2 s leads to the same rotation. in order to prove this mechanism, it was implemented into a robotic system. its mean density of 1.15 g/cm3 deviates not more than 4% from the biological and numerical models. it can complete a 180◦-turn within 1.03 ± 0.12 s with a rotational velocity of up to 4.25 s−1. keywords: biomimetics, righting maneuver, robot stabilization. 1. introduction since the first success of unmanned underwater vehicles (uuvs) their field of operation is constantly spreading. in spite of all the technology, the optimization of their stabilizing behavior is still a crucial topic in contemporary research. the reason why even modern uuvs are facing problems in holding stable positions, to carry out their tasks or turn around quickly once they have lost their preferred position, is the kind of drive that is mainly used. propeller and pump-jets are advantageous for high-speed locomotion, but too expensive for the use in a seldom occurring event. to gain new ideas for solving such problems more and more research groups are investigating biological models. first successful terrestrial applications are the amphibious robot robocrab by krummel et al., which adapts the skills of horseshoe crabs within the surf zone, or the four-wheeled autonomous robot by changsiu et al., which is capable of mid-air reorienting during free fall modeled on geckoes (hemidactylus platyurus) [1][2]. but the usage of biological models for improving aquatic robots is poorly documented. thus, the research group dfu of the department of biomimetics in bremen started investigations on different benthic marine animals. the aim was to search for a strategy that allows a quick turning or efficient reorientation manoeuvre which uses neither a propeller nor is driven by a permanent rotation. especially promising seemed the crustacean order decapoda. therefore the species eriocheir sinensis has been studied in terms of their mid-water righting behavior [3][4]. besides the morphological biomechanical analysis, also the necessary figure 1. individual of e. sinensis (a, [3] modified), its numerical model (b) [4] and the adapted robot o-typus (c) with an insight into its electronic devices (d) [5]. hydrodynamic forces have to be determined to show, that such a strategy is transferable to a technical application. 2. material and methods 2.1. eriocheir sinensis biological model in total 52 rotations of 10 individuals of e. sinensis were analysed. the rotations are differentiated in the kinematic approach with 39 analysed rotations (28/11, initialising/stopping rotation) and for the piv (particle image velocimetry) analysis with 13 analysed rotations (9/4, initialising/stopping rotation). 53 http://dx.doi.org/10.14311/app.2017.7.0053 http://ojs.cvut.cz/ojs/index.php/app t. riphaus, f. hoffmann, s. labisch acta polytechnica ctu proceedings 2.1.1. kinematic analysis to observe the natural righting behavior of e. sinensis (figure 1a), the crabs were held in a supine starting position at the height of 0.60 m within a freshwater tank with a ground area of 0.6 × 0.6 m and a high of 0.8 m and released by starting device. the body movement was high speed recorded (250 fps) to be able to manually track two points on the body and the tip of the 5th leg. furthermore falling speed, body angle and leg trajectories were plotted and the speed of the leg tip calculated. the leg induced force (fd) during the strike was calculated by fd = 1 2 ρ v2 c cd a (1) where ρ = water density, vc = leg centroid velocity, a = area of 5th legs and cd = drag coefficient from static force balance measurements. centroid velocity was calculated by: vc = vt lbc lbt (2) where vc = velocity of centroid, vt = velocity of leg tip, lbc = length leg base to leg centroid and lbt = length leg base to leg tip. lbt and lbc were experimental determined on 15 legs of 10 dead e. sinensis. centroid x/y coordinates were calculated with an integrated function of imagej from the leg area. the resulting factor for lbc / lbt was calculated as 0.44 ± 0.016. 2.1.2. piv measurements and force calculation the tank of the kinematic study was also used for the piv measurements. crabs were released by hand or the automated release fixture. the laser sheet was placed vertically in the middle of the tank illuminating a surface of approx. 0.3 x 0.3 m. flow was visualized by polyamid seeding particles (ø 57 µm, density: 1.03 g/cm3). images were taken by a high speed camera (photron apx-rs) at an interframing time of 3.75 ms (266 fps). crabs were released at different distances to the lasersheet depending on the leg length. we used falling sequences where the last leg was cutting the lasersheet at positions from 50 to 80% of the leg. by measuring the bound circulation forces around the leg the generated propulsion force was calculated by using the kutta-joukowski theorem. circulation γ was measured from the beginning to the end of the leg stroke in order to get a temporal resolution of the circulation. in pivlab [6] under matlab (the mathworks inc.) the piv images were analysed and the spanwise circulation (circulation around the spanwise axis) was derived by a loop integral of the tangent velocity: γ = ∮ svort vt dsvort = ∫ avort ωz davort (3) where svort = circular path around the vortex core, vt = tangential velocity, avort = area of the vortex core and ωz = spanwise vorticity. the vortex ring momentum calculation model was used to estimate an average propulsive force [7][8]. the average propulsive force of the leg stroke was herewith calculated by f = 2 γ ρ ν b (4) where γ = circulation, ρ = fluid density, ν = fluid velocity and b = leg length. the force results were multiplied by two, to get the force of both legs. 2.2. simulated model for the numerical simulation of the physical behavior the software adams (rel. 2013.1) was used. it allows to describe the limb movement as a motion of mechanically joint rigid bodies, builds the relevant differential equations of motion and solves them numerically. basis for the multi-body-analysis is experimental gained data of an individual crab showing the dimensions, the mass, the density and the center of mass (com) of each limb. all body-parts are connected with rigid joints. in order to simulate the correct falling speed in water the gravity was reduced to 1.09 m/s2. during movement the crabs hold their front legs close to the carapax and stretching out only the hind legs. therefore the main body can easily be simplified to a cylinder. with a diameter of 6.00 cm and a height of 2.75 cm for carapax and front legs such a cylinder will have an average density of 1.12 g/cm3 which leads to a mass of 87 g. this data fits the measured crab very well. the hind leg pair is modelled with the merus/ischium, the propodus/carpus and the dactylus in their measured length and density. the parts of the leg are conical so that the com of these parts matches also (figure 1b). the acting forces are applied on the joint between dactylus and propodus with a constant value for a given duration (thick arrows in fig 1b). 2.3. o-typus technical model 2.3.1. setup to confirm whether the observed mechanism is correctly understood, the basic model is implemented in the purpose-built robot o-typus (figure 1c+d) [5]. its chassis is congruent with the carapace of an individual of e. sinensis and scaled 2:1, to house drive units and the sensor system. the actuating elements consist of two waterproof hk15328d servo motors (max torque: 12,8 kg.cm) with a 6v external power supply (2250 ma). their control is based on the pwm-signals from an arduino uno. the position tracking is enabled by the mpu6050 accelerometer. the real time operation sends the current yaw-/ pitch-/ roll-angles (ypr) to the arduino uno to log the data (~27 hz). 54 vol. 7/2017 righting of chinese mitten crabs (eriocheir sinensis) and their models figure 2. a. stereotypical turning maneuvers observed for e. sinensis after a virtually moment-free start ([9], modified). ∆t = 0.2 s. b. positions of body axis, right 5th leg and com for one individual (e. s.). origin of ordinates on caudal end of carapace at starting point. ∆t = 0.02 s (0.1 s for body axis). 2.3.2. experiments the performed tests are adapted by the setup of the experiments carried out in section 2.1.1. therefore, the robot starts in a supine position at the top of the tank. to initialize the turning, the two legs will strike simultaneously. the appropriate kinematic parameters were determined by an iteratively change of the striking angle θ at the maximum angular striking velocity ω of 4.76 s−1. the acting forces were kinematically analyzed by equation 1. 3. results falling e. sinensis show a body rotation along the transversal axis during free fall (see figure 2a). the rotation is initiated directly after release by one stroke cycle of the 5th leg pair followed by a passive phase and stopped again with the 5th leg pair by a counterstrike. the turn is completed in 0.76 ± 0.15 s which leads to a mean angular velocity of ω = 4.3 s−1. in figure 2b the trace of one individual turning maneuver is given in sagittal view. besides the reorientation of the body axis the trajectory of the 5th leg tip is given to show the efficient strike and counterstrike. the moving location of the com testifies the complex interaction of the acting forces. 3.1. force calculation of 5th leg pair by kinematic approach and piv forces which are induced by moving the hind leg pair in phase 2a (see figure 3b) have a maximum at 33% of the stroke with a mean force of 0.018 ± 0.004 n and a maximum peak of 0.023 ± 0.002 n. the total momentum during phase 2a is 0.0036 ns. for phase 3a the maximum is at 35% of leg stroke with a mean force 0.015 ± 0.003 n and a maximum peak of 0.018 ± 0.002 n. figure 3. results from experiment and multibodysimulation for a: body angle and b: induced forces. experimental forces are mean values of the force calculations. body angle of experimental data (blue rhomb), n=8 and multibody-simulation (red line) are showing the same trend in time and angle. the calculated forces are 1.5 to 2 times higher (piv: 2a n=9, 3a n=3, kinematic: 2a n=28, 3a n=11) than the forces used in the simulation. the piv data shows that propulsive forces were produced by the hind legs to initiate and stop the rotation. peak forces to initiate the rotation (45% of stroke cycle) of 0.021 n (± 0.001 n) (n=9) lead to a total momentum of 0.0021 ns. 3.2. simulation the simulation shows that a constant force of 0.0045 n acting on each hind leg respectively for 0.2 s leads to a successful rotation within time. this means that the total momentum of 0.0018 ns causes a constant angular velocity of 3.99 s−1 in the middle part of the turning maneuver, part 2b in figure 3. 3.3. technical model the experiments confirmed the assumption, that a stroke with two legs is sufficient for a 180◦-turn (see figure 4b). the correspondent kinematic parameters are θ = 2.44 and ω = 4.76 s−1. the complete turn was herewith possible within 1.00 ± 0.12 s (n = 6). an exemplary run is shown in figure 4b. the turn is divisible into the same five phases like e. sinensis. during the initializing (1) the chassis is descending in a supine position( till i/ 2). the striking phase (2a) includes the active leg movement and thereby the acceleration (i-ii/ 2-3). the following gliding phase (2b) describes the passive turning based on inertia (ii-iii/ 55 t. riphaus, f. hoffmann, s. labisch acta polytechnica ctu proceedings figure 4. turning movement of o-typus. b. observed turning behavior with five characteristic phases (initializing pi=̂1, striking ps=̂2a, gliding pg=̂2b, counterstriking pc=̂3a, descending pd=̂3b); ø∆t = 0,36 s. a. course of the body axis and trajectory of the left leg’s tip. leg positions at the end of pi (i), end of ps (ii) and the target position (iii) in grey. iv shows the maximal overwinding; ∆t = 0,2 s (0,1 s during passive turning (ii-iii)). c. angle of attack (green) and angular velocity (red) of three runs. 3-5). when the horizontal target position is reached, the counterstriking phase (3a) starts with a counter movement of the legs, to stop the rotation (iii-iv/ 5-6). thereafter the chassis descends (3b) in a stable up-right position. additionally figure 4a shows the trajectory of one striking leg. point i poses the initiation of the stroke, point ii the end of the stroke, point iii the end of the 180◦-turn and thereby the initiation of the counterstrike and point iv the eventual slight overwinding. the graphs of figure 4c are describing the shifting of the angle of attack and its angular velocity. the same phases can be located here. the stroke starts at 2000 ms and leads over from phase 1 to 2a. the maximal angular velocity of 4.06 s−1 is reached at the end of 2a. subsequently ω starts decreasing within phase 2b. after approximately 1150 ms the turn is completed and results in phase 3a, which prevents overwinding. afterwards the body descends stable with minor wobbling. the force which is induced by the moving leg pair in phase 2a has a mean value of 0.0175 n. this propulsive force is acting over 0.51 s, which results in a total generated momentum of 0.00898 ns. figure 5. comparison of characteristic turning phases of (a) e. sinensis, (b) o-typus and (c) the simulated model. phases: 1 (yellow), 2a (blue), 2b (green), 3a (orange) and 3b (grey). 4. conclusions 4.1. comparison of e. sinensis with its models a qualitative comparison of the righting behavior of e. sinensis with the turning characteristics of the adapted robot and the multibody simulation is shown in figure 5. o-typus shows like the biological model a complete rotation after a single stroke. its rotation could be divided into the exact same phases like e. sinensis. the correspondence can be seen by comparing the phases. the duration of some phases are partially varying. a considerable difference between a and b can be seen within phase 2b. according to this, the larger o-typus needs significantly more time to complete the passive turn. a full comparison of the designed and measured parameters is shown in table 1. while the numerical model could be simulated in the original scale, the robot had to be enlarged to fit all devices. however the mean density was adapted. the measured propulsive forces of e. sinensis deviate among the two methods. while the piv data corresponds closely to the values gained by the simulation, the kinematic approach matches nicely with the acting forces on o-typus. due to the considerable bigger dimensions of o-typus, the total momentum to generate a similar turn is about 3 times of e. sinensis value. herewith o-typus reaches a mean angular velocity of 3.93 ± 0.30 s−1, which deviates no more than 8.6% of its model. 4.2. transferability to aquatic robots as the motivation for this study showed, there is a desperate need in new stabilizing systems for technical aquatic applications. the observed and tested righting behavior of e. sinensis revealed a high efficiency and therefor a potential approach to solve the problem. in order to verify, whether this new stabilizing system is an optimization compared to current methods, further 56 vol. 7/2017 righting of chinese mitten crabs (eriocheir sinensis) and their models parameter e. sinensis simulation robot kinematic piv scaling 100% 100% 200% mass [g] 88.65 87 220 mean density [g/cm3] 1.12 1.12 1.15 mean force [n] 0.018 0.011 0.009 0.0175 ± 0.004 ± 0.003 momentum [ns] 0.0036 0.0021 0.0018 0.00898 mean angular vel. [s−1] 4.30 3.99 3.93 ± 0.30 table 1. summary of relevant parameters regarding the turning of e. sinensis, its numerical model and its technical application. values of the measured force are mean values during the striking phase 2a. the angular velocity is the averaged value of the whole turn. figure 6. smart-e. modern thruster-driven auv, which is declared to be highly efficient [10]. studies have to be carried out. thus, two different efficiencies have to be compared. on one hand, the power consumption has to be evaluated. at the current state of research no statement is possible, as there is no data about robotic devices, driven by thruster, available to compare it with. it would be worth to use an existing modern robot like the auv smart-e [10], to compare the two mechanisms at the same chassis. on the other hand, time efficiency has to be considered. most remotely operated vehicles are featuring slow turning capabilities. unfortunately non published the specific turning kinematics. however, the maximum angular velocity of 4.25 s−1 reached by otypus is considerably (visually) higher than of most found thruster-driven devices. acknowledgements special thanks are referring to the department of biomimetics in bremen, which made these studies possible. references [1] g. krummel, k. n. kaipa, s. k. gupta. a horseshoe crab inspired surf zone robot with righting capabilities. in proc. of the asme 2014 int. design eng. tech. conf. & comput. and inform. in eng. conf. 2014. doi:10.1115/detc2014-34679. [2] e. chang-siu, t. libby, m. tomizuka, r. j. full. a lizard-inspired active tail enables rapid maneuvers and dynamic stabilization in a terrestrial robot. ieee/rsj int conf of intelligent robots and syst 2011. doi:10.1109/iros.2011.6094658. [3] p. bausch, f. hoffmann, a. b. kesel. im freien fall unter wasser lagestabilisierung bei wollhandkrabben. eine experimentelle analyse. in bionik: patente aus der natur (ed. a.b. kesel und d. zehren). 155-161, bionik-innovations-centrum, bremen, 2015. [4] f. hoffmann, s. labisch, r. sonntag, et al. analysis of underwater righting reflex of the chinese mitten crab (eriocheir sinensis) using piv and numerical multibody simulation. in proceedings of the annual main meeting of the society for experimental biology, prag, [a 11.68]. 2015. [5] t. riphaus, s. labisch. konstruktion des biologisch inspirierten roboters o-typus zur implementierung und untersuchung des stabilisationsverhaltens von decapoden. in proceedings of the 7. ieee germany student conference, magdeburg. 2016. [6] w. thielicke, e. j. stamhuis. pivlab towards userfriendly, affordable and accurate digital particle image velocimetry in matlab., 2014. j.openres.softw.,2,. doi:http://doi.org/10.5334/jors.bl. [7] j. m. v. rayner. a new approach to animal flight mechanics. j exp biol 80:17–54, 1979. [8] g. r. spedding, j. m. v. rayner, c. j. pennycuick. momentum and energy in the wake of a pigeon (columba livia) in slow flight. j exp biol 111:81–102, 1984. [9] p. bausch, p. berger, f. hoffmann, a. b. kesel. how to land on your legs underwater righting reflexes in crabs and crayfish. in proceedings of the annual main meeting of the society for experimental biology, prag, [a 11.67]. 2015. [10] b. meyer, k. ehler, c. osterloh, e. maehle. an autonomous omnidirectional underwater robot. journal of behavioral robotics pp. 204–210, 2013. 57 http://dx.doi.org/10.1115/detc2014-34679 http://dx.doi.org/10.1109/iros.2011.6094658 j. open res. softw., 2,. http://dx.doi.org/http://doi.org/10.5334/jors.bl acta polytechnica ctu proceedings 7:53–57, 2017 1 introduction 2 material and methods 2.1 eriocheir sinensis biological model 2.1.1 kinematic analysis 2.1.2 piv measurements and force calculation 2.2 simulated model 2.3 o-typus technical model 2.3.1 setup 2.3.2 experiments 3 results 3.1 force calculation of 5th leg pair by kinematic approach and piv 3.2 simulation 3.3 technical model 4 conclusions 4.1 comparison of e. sinensis with its models 4.2 transferability to aquatic robots acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2016.3.0047 acta polytechnica ctu proceedings 3:47–50, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app structural and mechanical characterization of deformed polymer using confocal raman microscopy and dsc birgit neitzel∗, florian aschermayer, milan kracalik, sabine hild johannes kepler university linz, institute of polymer science, altenberger straße 69 4040 linz, austria ∗ corresponding author: birgit.neitzel@jku.at abstract. polymers have various interesting properties, which depend largely on their inner structure. one way to influence the macroscopic behaviour is the deformation of the polymer chains, which effects the change in microstructure. for analyzing the microstructure of non-deformed and deformed polymer materials, raman spectroscopy as well as differential scanning calorimetry (dsc) were used. in the present study we compare the results for crystallinity measurements of deformed polymers using both methods in order to characterize the differences in micro-structure due to deformation. the study is ongoing, and we present the results of the first tests. keywords: raman spectroscopy, dsc, deformed polymers, crystallinity. 1. introduction deformed polymers are used in a wide range of applications because of their advanced mechanical properties. especially, materials with high strength gained increasing importance. in order to obtain high strength materials with tailored properties, the morphology can be controlled by varying process conditions. nevertheless, there is still a lack of knowledge in the correlation between mechanical properties, processing conditions and polymer morphology. the microscopic structure is claimed as a crucial factor, which determines the mechanical properties. furthermore, mechanical performance is influenced by the crystallinity and chain orientation of a polymer. therefore, characterization of these parameters is important for developing new tailored polymeric materials. wide angle x-ray diffractometry or differential scanning calorimetry (dsc) are common methods to determine the overall crystallinity of polymers. besides, also spectroscopic techniques such as raman spectroscopy [1–4] have shown to be suitable techniques to observe process-induced changes in crystallinity [5] and chain orientation [3]. raman spectroscopy uses polarized laser light to scan the surface of a sample. when changing the polarization angle of the filter, the intensities of certain structure-related peaks in the raman spectrum change as well, which allows conclusions on the polymer morphology. the degree of orientation can be determined from these peaks via a material specific orientation function fcz, such as equation (1) for pp [3]: fcz = 0.134 · ∑ i973∑ i998 − 0.182 (1) see [3] it reveals if the polymer chains are randomly distributed (fcz = 0), in deformation direction (fcz > 0) or perpendicular to it (fcz < 0). as fcz depends on the polarization filter’s orientation, the differences in multiple spectra must be considered when determining its value. crystallinity α is supposed to be independent of the filter’s orientation. its equation sums up peaks of multiple spectra to determine its value. αraman = ∑ i809∑ i809 + ∑ i841 (2) see [5] directed force is applied to the samples, this direction is designated mod (machine orientation direction). for each sample two raman spectra were recorded. the first with polarisation set to 0 degrees, emitting laser light perpendicular to the mod. the second spectrum is taken with the laser aligned parallel (i.e. 90 degrees) to the direction of the applied force. we took 40000 measurements of one sample per mod to see if mod-dependent peaks in the spectra can be identified. the relative intensities were determined by integration of raman bands. the crystallinity was then calculated via equation (2) from the sum-spectra of both measurement series, parallel and perpendicular to the deformation direction. the second method we used, was dsc. from dsc curves, first the enthalpy of the sample can be calculated and from these results the crystallinity as well. one goal of this study is to compare the crystallinity values, obtained from both methods, because each technique is best suited for different surface textures. if a sample has a very smooth surface, then confocal raman microscopy can be used; for more irregular surfaces, measuring with dsc is more suitable. to characterize the polymer sample also on a macro-structure level, mechanical tests are ongoing. 47 http://dx.doi.org/10.14311/app.2016.3.0047 http://ojs.cvut.cz/ojs/index.php/app b. neitzel, f. aschermayer, m. kracalik, s. hild acta polytechnica ctu proceedings the mechanical investigation focuses on tensile testing. with this method, tensile strength and fracture behaviour can be analysed. furthermore, hardness tests could give us important data to build up the comprehensive material overview of the polymer samples in microand macro structure scales. 2. experimental in this current study, raman measurements were done with a confocal raman microscope (alpha300r, witec gmbh, ulm, germany). for the measurements, polarized laser light of 532 nm and 16 mw power was used. a polarization direction of 0° or 90° was applied. the graphical analysis has been performed using an objective with 20x magnification. with this equipment and these settings, polypropylene (pp) samples with different degrees of deformation in one direction were analyzed. furthermore, polyethylene terephthalate (pet) samples were investigated. the second method in this study was dsc using the instrument perkin elmer, dsc 8000, usa . both, heating rate and cooling rate were set at 10 k/min. the pp samples were heated from 25°c to 250°c, and the pet samples from 25°c to 300°c. the crystallinity was calculated from the first heating curve, to detect the influence, caused by the deformation. 3. results and discussion 3.1. crystallinity determined by confocal raman microscopy in the case of pp, the peaks at 809 cm−1 and 841 cm−1 provide information about the crystallinity, whereas the peaks at 973 cm−1 and 998 cm−1 are important for determining the chain orientation. these peaks change their orientation depending on the polarization of the laser light. all results were calculated via integration of the peak areas (see figure 1). figure 1. material specific (pp) peaks for crystallinity and chain-orientation calculation. in figure 2, the crystallinity distribution of a nondeformed (figure 2a), deformed pp (figure 2b), and highly deformed pp (figure 2c) can be seen. the deformed sample has a higher degree of crystallinity compared to the non-deformed sample. thus, the random distribution of the polymer chains, in the nondeformed sample changed to a well-ordered structure in the highly deformed pp-sample. (a) . non-deformed pp (b) . deformed pp (c) . highly deformed pp figure 2. crystallinity α calculated from raman spectra. confocal raman microscopy can be a powerful tool for structural analysis of further polymeric materials, but in this case it is necessary to find material specific structure relevant peaks. two peaks could be interesting for the second investigated material, pet: 998 cm−1 and 1096 cm−1. [6] furthermore, material specific formulas for crystallinity and orientation are required. 3.2. crystallinity obtained by dsc a big advantage of differential dsc is that samples can be produced very easily and in the same way for every polymer. also the crystallinity can be calculated with the same equation. so far, pet has been analysed as a second polymeric material. in figure 3, the crystallinity, calculated from dsc measurements, can be seen. these first measurements show, that crystallinity increases with high deformation. in a next step, these results will be compared to the crystallinities, determined via confocal raman microscopy. macrostructure will be characterized via tensile test. the aim is to find a relationship between the microand 48 vol. 3/2016 structural and mechanical characterization of deformed polymer figure 3. crystallinity of pet samples, measured via dsc; (a) amorphous, (b) deformed and (c) highly deformed pet. macro-structure behaviour of different polymeric materials. 3.3. comparison of crystallinity calculated by confocal raman microscopy and dsc using both methods, dsc and raman spectroscopy, it was found that the crystallinity α (figure 4) increases with higher deformation, but they have different increase rates. figure 4. crystallinity α calculated from raman spectra and dsc measurements for a non-deformed, b deformed and c highly deformed polypropylene (pp). the highest crystallinity and best correlation between both measuring methods was observed in the most deformed polypropylene c. it was furthermore observed that deformation of pp causes changes in its microstructure. 3.4. orientation distribution obtained by confocal raman microscopy figure 5 shows that the orientation function for the polymer chains, determined via confocal raman microscopy, increases with higher deformation. the polymer chains realign under stress by positioning themselves parallel to each other, resulting in a restructured polymer. this effect was also observed for the crystallinity, which also increases. a denotes non-deformed pp without orientation, b deformed polymer with weak orientation and c highly deformed pp with a strong chain-orientation along the deformation direction, 0° perpendicular, 90° parallel to mod. figure 5. orientation function calculated from raman spectra and dsc measurements for a nondeformed, b deformed and c highly deformed polypropylene (pp). (a) . parallel to mod, nondeformed (b) . perpendicular to mod, nondeformed (c) . parallel to mod, deformed (d) . perpendicular to mod, deformed (e) . parallel to mod, highly deformed (f) . perpendicular to mod, highly deformed figure 6. orientation distribution of pp samples calculated from confocal raman spectra figure 6 shows the orientation distribution of the pp-samples at different mods and degrees of deformation. the scanned area was 200 µm× 200 µm. it can be seen that the deformation changes the chain orientation from a random distribution to a well-defined periodic arrangement for both laser polarizations. the random distribution of the chains in non-deformed pp changes to an uniform distribution in highly deformed pp. 49 b. neitzel, f. aschermayer, m. kracalik, s. hild acta polytechnica ctu proceedings 4. summary with the two selected methods, dsc and raman spectroscopy, crystallinities were calculated. it was shown that the crystallinity and orientation of the chains increase with the deformation of the polymer. the effect of increasing crystallinity caused by deformation was shown for both polymeric materials, pp and pet. 5. outlook in the current study, pp as one important polymeric material, was analyzed and the results show that confocal raman microscopy and differential scanning calorimetry are powerful tools for the characterization of the inner structure. because of the different chemical behavior of different polymers, it is necessary to find useful structure peaks and mathematical formulations for crystallinity and orientation. finding solutions for other polymer, like pet, will be a subject of future work. in addition, relationships between mechanical properties and the polymer morphology/structure on a microand macro-scale are currently under investigation. acknowledgements robert führicht for latex typesetting. references [1] j. martin, m. ponçot, p. bourson, et al. study of the crystalline phase orientation in uniaxially stretched polypropylene by raman spectroscopy: validation and use of a time-resolved measurement method. polymer engineering & science 51(8):1607–1616, 2011. doi:10.1002/pen.21944. [2] m. fernandez, j. merino, m. gobernado-mitre, j. pastor. molecular and lamellar orientation of α-and β-transcrystalline layers in polypropylene composites by polarized confocal micro-raman spectroscopy: raman imaging by static point illumination. applied spectroscopy 54(8):1105–1113, 2000. [3] j. rodríguez-cabello, j. merino, l. quintanilla, j. pastor. deformation-induced conformational changes in stretched samples of amorphous poly (ethylene terephthalate). journal of applied polymer science 62(11):1953–1964, 1996. [4] j. rodríguez-cabello, j. merino, t. jawhari, j. pastor. rheo-optical raman study of chain deformation in uniaxially stretched bulk isotactic polypropylene. journal of raman spectroscopy 27(6):463–467, 1996. [5] a. s. nielsen, d. batchelder, r. pyrz. estimation of crystallinity of isotactic polypropylene using raman spectroscopy. polymer 43(9):2671–2676, 2002. [6] s. yang, s. michielsen. orientation distribution functions obtained via polarized raman spectroscopy of poly (ethylene terephthalate) fibers. macromolecules 36(17):6484–6492, 2003. doi:10.1021/ma034486q. 50 http://dx.doi.org/10.1002/pen.21944 http://dx.doi.org/10.1021/ma034486q acta polytechnica ctu proceedings 3:47–50, 2016 1 introduction 2 experimental 3 results and discussion 3.1 crystallinity determined by confocal raman microscopy 3.2 crystallinity obtained by dsc 3.3 comparison of crystallinity calculated by confocal raman microscopy and dsc 3.4 orientation distribution obtained by confocal raman microscopy 4 summary 5 outlook acknowledgements references 181 acta polytechnica ctu proceedings 1(1): 181–188, 2014 181 doi: 10.14311/app.2014.01.0181 magnetorotational explosions of core-collapse supernovae gennady s. bisnovatyi-kogan1, sergey g. moiseenko2, nikolay v. ardeljan3 1space research institute, profsoyuznaya str. 84/32, moscow 117997, russia, and national research nuclear university ”mephi”, kashirskoye shosse, 31, moscow 115409, russia 2space research institute, profsoyuznaya str. 84/32, moscow 117997, russia 3department of computational mathematics and cybernetics, moscow state university, vorobjevy gory, moscow b-234, russia corresponding author: gkogan@iki.rssi.ru abstract core-collapse supernovae are accompanied by formation of neutron stars. the gravitation energy is transformed into the energy of the explosion, observed as sn ii, sn ib,c type supernovae. we present results of 2-d mhd simulations, where the source of energy is rotation, and magnetic field serves as a ”transition belt” for the transformation of the rotation energy into the energy of the explosion. the toroidal part of the magnetic energy initially grows linearly with time due to differential rotation. when the twisted toroidal component strongly exceeds the poloidal field, magneto-rotational instability develops, leading to a drastic acceleration in the growth of magnetic energy. finally, a fast mhd shock is formed, producing a supernova explosion. mildly collimated jet is produced for dipole-like type of the initial field. at very high initial magnetic field no mri development was found. keywords: core-collapse supernova magnetorotational mechanism numerical modeling. 1 introduction supernova is one of the most powerful explosion in the universe which releases about 1051 erg both in radiation and kinetic energies. sne explode at the end of evolution of massive stars, with initial mass larger than ∼ 8m�. a thermonuclear explosion of c-o degenerate core with total disruption of the star takes place in sn ia, what happens when initial mass of the star does not exceed ∼ 12m�, when electrons are degenerate in the carbon-oxygen core . for larger initial masses the evolution proceeds until the formation of the iron core, and the star collapses due to a loss of a hydrodynamic stability. during the core collapse and formation of a neutron star, gravitational energy release ∼ 6 · 1053 erg, is carried away by neutrino. the first mechanism suggested in [15] for the explanation of the explosion in a corecollapse sn was connected with a neutrino deposition. the huge energy flux carried by neutrino heats the infalling outer layers, reverse the direction of motion, and leads to formation of the shock wave, producing explosions of sn ii, sn ib,c types. later more accurate calculations revealed that the energy of such explosion is not enough for the explanation of observations. many modifications of the neutrino model have been calculated during years, but the problem is not yet clear. the review of the problem may be found in the book [8]. in recent simulations (see details in [23]) we have found that for extremely strong initial magnetic field h0 = 1012g a prompt supernova explosion occurs, and collimated jet is formed in agreement with [28]. for case when the initial magnetic field is weaker h0 = 109g we have identified, after the linear growth of the poloidal magnetic field due to differential rotation, the exponential field growth due to the magnetorotational instability of tayler type [30]. we call the combination of differential rotation with the tayler type mri instability, as magneto-differential-rotation instability (mdri). the ejection due to the explosion is only weakly collimated, while [28] had obtained a strong collimation in this variant also. in these simulations we considered a uniform magnetic field along the rotational axis, as the initial field configuration, similar to [28]. 2 magnetorotational mechanism of explosion in magnetorotational explosion (mre) the transformation of the rotational energy of the neutron star into explosion energy takes place by means of the magnetic field [7]). neutron stars are rotating, and have magnetic fields up to 1013 gs, and even more. often one or two-side ejections are visible. that indicate to nonspherical form of the sne explosions. in differentially 181 http://dx.doi.org/10.14311/app.2014.01.0181 gennady s. bisnovatyi-kogan, sergey g. moiseenko, nikolay v. ardeljan rotating new born neutron stars radial magnetic field is twisted, and magnetic pressure becomes very high, producing mhd shock by which the rotational energy is transformed to the explosion energy. calculations of mre have been done in [12], using one-dimensional nonstationary equations of magnetic hydrodynamics, for the case of cylindrical symmetry. the energy source is supposed to be the rotational energy of the system (the neutron star, and surrounding envelope). the calculations show that the envelope splits up during the dynamical evolution of the system, the main part of the envelope joins the neutron star and becomes uniformly rotating with it, and the outer part of the envelope expands with large velocity, carrying out a considerable part of rotational energy and rotational momentum. mre has an efficiency about 10% of the rotational energy, the ejected mass is ≈ 0.1 of the star mass, explosion energy ≈ 1051 erg. ejected mass and explosion energy depend weekly on the parameter α = emag/egrav at initial moment. explosion time depends on α as texpl ∼ 1√ α . small α is difficult for numerical calculations with explicit numerical schemes because of the courant restriction on the time step, hard system of equations, where α determines a hardness. 3 2-d calculations the numerical method used in simulations is based on the implicit operator-difference, completely conservative scheme on a lagrangian triangular grid of variable structure, with grid reconstruction (fig.1). the implicitness of the applied numerical scheme allows for large time-steps. it is important to use the implicit scheme in the presence of two strongly different time-scales: the small one due to huge sound velocity in the central parts of the star, and the big one determining the evolution of the magnetic field. the method applied here was developed and its stability was investigated in the papers of [5], [6], [1]. the scheme is fully conservative, what includes conservation of mass, momentum and total energy, and correct transitions between different types of energies. it was tested thoroughly with different tests by [2]. in the calculations of magnetorotational corecollapse supernova performed by [3], magnetohydrodynamic (mhd) equations with self-gravitation, and infinite conductivity have been solved using the numerical scheme as described above. the problem has an axial symmetry ( ∂ ∂φ = 0), and the symmetry to the equatorial plane (z=0). initial toroidal current jφ was taken at the initial moment (time started now from the stationary rotating neutron star) producing hr, hz according to biot-savart law b = 1 c ∫ v j×r r3 dv . initial magnetic field of quadrupole-like symmetry is obtained at opposite directions of the current in both hemispheres. neutrino cooling was calculated using a variant of a fluxlimited method, [3]. figure 1: example of the triangular grid magnetic field is amplified due to twisting by the differential rotation, and subsequent development of the magnetorotational instability. the field distribution for initial quadrupole-like magnetic field with α = 10−6, at the moment of the maximal energy of the toroidal magnetic field is represented in fig.1. the maximal value of bφ = 2.5·1016 gs was obtained in the calculations. the magnetic field at the surface of the neutron star after the explosion is b = 4 ·1012 gs. time dependence during the explosion of rotational, gravitational, internal, and kinetic poloidal energies is given in figs.3. almost all gravitational energy, transforming into heat during the collapse, is carried away by weakly interacting neutrino. the total energy ejected in the kinetic form is ∼ 0.6 · 1051 erg, and the total ejected mass is equal to ∼ 0.14m�. figure 2: toroidal magnetic field distribution at the moment of its maximal energy for the initial quadrupole field . 182 magnetorotational explosions of core-collapse supernovae time, s 0 0.1 0.2 1 2 3 4 erot[1051 ergs] ekinpol[1051 ergs] figure 3: time dependence of rotational, kinetic poloidal, and magnetic energies during explosion for a dipole -like field, from [22]. the simulations were done for the initial poloidal magnetic field of quadrupole [3] and of dipole [22] types of symmetry. before the collapse the ratios between the rotational and gravitational, and between the internal and gravitational energies of the star had been chosen as: erot egrav = 0.0057, eint egrav = 0.727. the initial magnetic field was ”turned on” after the collapse stage. the ratio between the initial magnetic and gravitational energies was chosen as 10−6. the initial poloidal magnetic field in the center, at start of the evolution of the toroidal field was ∼ 3.2× 1013g. time, s e je ct ed m as s/ m su n 0 0.1 0.2 0.30.00 0.04 0.08 0.12 figure 4: time dependence of the ejected mass during the magnetorotational explosion with initial dipole magnetic field, from [22]. the magnetic field works as a piston for the originated mhd shock. the time dependence of the ejected mass and energy is given in figs. 4, 5. during the magnetorotational explosion ∼ 0.14 m� of the mass and ∼ 0.6 · 1051ergs (∼ 10% of the rotational energy) are ejected. the simulation of the mr supernova explosion for various initial core masses and rotational energies was done by [11]. the initial core mass was varied from 1.2m� to 1.7m�, the initial specific rotational energy erot/mcore, was varied from 0.19 × 1019 to 0.4 × 1019 erg/g. the explosive energy increases with the mass of the core, and the initial rotational energy. the energy released in mr explosion, (0.5−2.6)×1051 erg, is sufficient to explain supernova with collapsing cores, types ii and ib. the energies of type ic supernovae could be higher. time, s e je ct ed e n er g y [1 051 er gs ] 0.2 0.3 0.1 0.2 0.3 0.4 0.5 0.6 figure 5: time dependence of the ejected energy during the magnetorotational explosion with initial dipole magnetic field, from [22]. 4 magnetorotational instability magnetorotational instability (mri) leads to exponential growth of magnetic fields. different types of mri have been studied by [31], [27]. mri starts to develop when the ratio of the toroidal to poloidal magnetic energies is becoming large. in 1-d calculations mri is absent because of a restricted degree of freedom, and time of mr explosion is increasing with α as texpl ∼ 1√ α , α = emag0 egrav0 . due to development of mri the time of mr explosion depends on α much weaker. the mr explosion happens when the magnetic energy is becoming comparable to the internal energy, at least in some parts of the star. while the starting magnetic energy linearly depends on α, and mri leads to exponential growth of the magnetic energy, the total time of mre in 2-d is growing logarithmically with decreasing of α, texpl ∼ − logα. these dependencies are seen clearly from 1-d ([12]) and 2-d calculations ([3], [22]) giving the following explosion times texpl (in arbitrary units): α = 0.01, texpl = 10, α = 10−12, texpl = 106 in 1d, and α = 10−6, texpl ∼ 6, α = 10−12, texpl ∼ 12 in 2-d. the dependence of the explosion time is shown 183 gennady s. bisnovatyi-kogan, sergey g. moiseenko, nikolay v. ardeljan in graphs for the quadrupole ([21]), and dipole ([22]) configurations of the magnetic field. the qualitative picture of the mri in 2d, and the example of the analytical toy model with an exponential growth of the magnetic field, have been presented by [3], [22]. 5 jet formation in mre jet formation in mre happens when the initial magnetic field is of a dipole-like structure. 2-d calculations with the initial dipole-like magnetic field gave almost the same values of the energy of explosion ∼ 0.5 · 1051 , and ejected mass ≈ 0.14m�, but the outburst was slightly collimated along the rotational axis [22], see fig.6 and fig.7. r, km z, km 0 2000 4000 6000 0 1000 2000 3000 4000 5000 6000 7000 0 500 10000 200 400 600 800 1000 figure 6: time evolution of the velocity field (outflow) for the time moment t = 0.075s, from [22] 0 500 10000 200 400 600 800 1000 r, km z, km 0 2000 4000 6000 0 1000 2000 3000 4000 5000 6000 7000 figure 7: time evolution of the velocity field (outflow) for the time moment, t = 0.25s, from [22]. simulations of the mr supernova have been made with equation of state suggested in [25]. a comparison of our results for the initially uniform magnetic field, using a lagrangian scheme, with the results in [28] and [29], using an eulerian scheme for the same initial and boundary conditions, shows good agreement for a strong initial field (h0 = 1012g), while for a weaker field (h0 = 109g) we get mildly collimated jet-like explosion; see also [13]. details of the results of these simulations will be published elsewhere ([23]). mri is developed in the case of a weaker initial magnetic field, and it is not present in the calculations with stronger field, see fig.8 and fig.12. we have made simulations for the initial magnetic fields h0 = 109, 1012g. the ratio of the initial rotational energy to the absolute value of the gravitational energy was taken erot0/egrav0 = 1%, 2%. when the initial magnetic field is moderate (h0 = 109 g) and erot0/egrav0 = 1% mdri develops what means exponential growth of all components of the magnetic field (fig.8). figure 8: developed mdri due to convection and mri/tayler instability at t = 267ms for the case h0 = 109g, erot0/egrav0 = 1% (contour plot the toroidal magnetic field, arrow lines force lines of the poloidal magnetic field). at fig.9 the lagrangian triangular grid and the ratio of the toroidal magnetic energy to the poloidal one (etor/epol) is represented for the case h0 = 109 g, and erot0/egrav0 = 1%. the toroidal magnetic energy dominates over the poloidal one in the significant part of the region where new neutron star is forming. the mdri is well-resolved on our triangular grid. in the case (h0 = 1012 g) and erot0/egrav0 = 1% there is no regions of domination of etor over epol. the fig.10 represents a time evolution of rotational, magnetic poloidal and toroidal energies for mr explo184 magnetorotational explosions of core-collapse supernovae sion when h0 = 109g. the fig.11 is the same data plot as the fig.10 but zoomed and the vertical axis is in logarithmic scale. the straight dash-dotted line at the fig.11 shows the exponential growth of the toroidal and poloidal magnetic energies with the time due to the mdri. the rotational energy has two maxima. the first contraction is accompanied by the strong growth of the rotational energy due to angular momentum conservation, maximum of which coincides with the first maximum of the density. the first contraction, and the subsequent bounce, happens when the magnetic field is growing slowly, and the angular momentum losses from the stellar core are small. development of the magnetorotational instability leads to a rapid growth of the magnetic field, large angular momentum flux from the core, what stops the expansion, and leads to the second contraction phase. in this case the contraction is not transforms into expansion, because of the rapid decrease of the rotational energy due to strong angular momentum flux outside from the core. r,cm z ,c m 0 5e+060 2e+06 4e+06 6e+06 eetor/eepol 1000 800 600 500 200 100 10 1 time= 0.265sec figure 9: the lagrangian triangular grid and the ratio of the toroidal magnetic energy etor to the poloidal magnetic energy epol, etor epol at t = 265ms for the case h0 = 109g, erot0/egrav0 = 1%. the energy of the poloidal magnetic field grows due to the contraction until the time t ≈ 0.225 sec. then it slightly decreases because of the formation of the bounce shock, and its motion outwards. the toroidal magnetic energy grows as quadratic function because of wrapping of the magnetic force lines (toroidal component of the magnetic field grows linearly). starting from t ≈ 0.3 sec both the poloidal and toroidal magnetic energies begin to grow exponentially due to mdri. at t ≈ 0.36 sec both magnetic energies comes to saturation. the mhd shock wave develops what leads to the mr explosion. the mr explosion develops in all directions without formation of a collimated flow. the mr explosion for an extremely high initial magnetic field (h0 = 1012 g) is developing in a qualitatively different way. the initial magnetic field is so strong that it grows strongly during the first contraction, and the explosion happens before the development of mdri happens (fig.12). at the fig.13 the time evolution of the rotational, poloidal magnetic and toroidal magnetic energies are represented. the rotational energy has one extremum at t ≈ 0.32 sec corresponds to the maximal contraction, accompanied by a corresponding growth of of the toroidal and poloidal magnetic energies. the poloidal magnetic field grows due to the contraction, the toroidal magnetic field appears due to the differential rotation and is amplified both due to the differential rotation and the contraction of the core. the strong initial magnetic field leads to a rapid loss of the angular momentum from the core already during the contraction phase. the centrifugal force becomes unimportant, and the first contraction is not followed by any bounce, leaving behind a dense slowly rotating neutron star core. we have got here a prompt explosion. the force lines of the magnetic field play the role of ’rails’. the matter moves along the force lines. the magnetic pressure dominates a the periphery of the core. the mr explosion develops mainly along the axis of rotation, and the collimated flow (protojet) is formed. the mr explosion results in the collimated jet. the degree of jet collimation is approximately the same as in [28]. for the case when erot0/egrav0 = 1% and h0 = 109 g the mr supernova explosion energy is ∼ 4× 1050 erg, for the h0 = 1012 g the mr supernova explosion energy reaches the value of ∼ 8 × 1050erg. the explosion energy resulted in the simulations by lagrangian method are close to those ones found in the simulations made by eulerian scheme [28] (excluding the case of b0 = 1012g and erot0/|egrav0| = 1/%). 6 asymmetry of the explosion it is known from the observations that the shapes of core collapse supernovae are different. from our simulations it follows that mr supernova explosion arises after development of the mri. the development of the mri is a stochastic process and hence the resulting shape of the supernova can vary. we may conclude that mr supernova explosion mechanism can lead to different shape of the supernova. it is important to point out that mr mechanism of supernova explosion leads always to asymmetrical outbursts. the simulations of the mr supernova explosions described here are restricted by the symmetry to the equa185 gennady s. bisnovatyi-kogan, sergey g. moiseenko, nikolay v. ardeljan torial plane. while in reality this symmetry can be violated due to the mri, simultaneous presence of the initial dipole and quadrupole -like magnetic field ([33]) and initial toroidal magnetic field ([10]). the violation of the symmetry could lead to the kick effect and formation of rapidly moving radio pulsars. a kick velocity, along the rotational axis, formed due to magnetohydrodynamic processes in presence of the asymmetry of the magnetic field, by estimations [9] does not exceed 300km/sec. figure 10: time evolution of rotational energy erot (solid line), magnetic poloidal energy emagpol (dashed line) and magnetic toroidal energy emagtor (dashdotted line) for the case h0 = 109g, erot0/egrav0 = 1%. when rotational and magnetic axes do not coincide the whole picture of the explosion process is three dimensional. nevertheless, the magnetic field twisting happens always around the rotational axis, so we may expect the kick velocity of the neutron star be strongly correlated with its spin direction. during the phase of mre explosion the regular component of magnetic field may exceed temporally 1016 g [3], [22], when the neutrino cross-section depends on the magnetic field strength. the level of the anisotropy of the magnetic field relative to the plain perpendicular to the rotational axis [20] may be of the order of 50%, leading to strong anisotropy of the neutrino flux. the kick velocity due to the anisotropy of the neutrino flux may reach several thousands km/c [9], explaining appearance of the most rapidly moving radio pulsars [32]. simultaneously, because of the stochastic nature of mri, the level of the anisotropy should be strongly variable, leading to a large spreading in the the neutron star velocities. this prediction of mr explosion differs from the models with a powerful neutrino convection, where arbitrary direction of the kick velocity is expected ([14],[17]). it was claimed in [16], that proto-neutron star (pns) convection was found to be a secondary feature of the corecollapse phenomenon, rather than a decisive ingredient for a successful explosion. figure 11: zoomed time evolution of rotational energy erot (solid line), magnetic poloidal energy emagpol (dashed line) and magnetic toroidal energy emagtor (dash-dotted line) for the case h0 = 109g, erot0/egrav0 = 1%. straight dash-dotted line shows exponential growth of the toroidal and poloidal magnetic energies. analysis of observations of pulsars shows that rotation and velocity vectors of pulsars are aligned, as is predicted by the mr supernova mechanism. this alignment was first found in [26], and was confirmed with reliability, increasing with time, in the papers [18],[19],[24]. the alignment of the vectors can be violated in the case when the supernova explodes in a binary system. 7 conclusions in mre the efficiency of transformation of rotational energy into the energy of explosion is ∼ 10%. mri strongly accelerates mre, at lower values of the initial magnetic fields. jet formation is possible for dipolelike topology of the field. mre energy is not sensitive to the details of the equation of state, model of the neutrino transfer, and to the choice of the numerical scheme. the observed alignment of the rotation and velocity vectors of pulsars follows directly from the mre supernova model. 186 magnetorotational explosions of core-collapse supernovae r,cm z ,c m 0 1e+06 2e+060.0e+00 5.0e+05 1.0e+06 1.5e+06 2.0e+06 time= 0.328sec figure 12: absence of mdri at t = 328ms for the case h0 = 1012g, erot0/egrav0 = 1% (contour plot the toroidal magnetic field, arrow lines force lines of the poloidal magnetic field). 0.1 0.15 0.2 0.25 0.3 0.35 time, sec e rot e magpol e magtor 10 8 6 4 2 e n e rg y x 1 0 5 0 , e rg figure 13: time evolution of rotational energy erot (solid line), magnetic poloidal energy emagpol (dashed line) and magnetic toroidal energy emagtor (dashdotted line) for the case h0 = 1012g, erot0/egrav0 = 1%. acknowledgement the work of sgm and gsbk was supported partially by rfbr grant 11-02-00602, grant for leading scientific schools nsh-5440.2012.2 and 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[28] takiwaki, t., kotake, k., nagataki, s., & sato, k. 2004, apj, 616, 1086 doi:10.1086/424993 [29] takiwaki, t., kotake, k., & sato, k. 2009, apj, 691, 1360 doi:10.1088/0004-637x/691/2/1360 [30] tayler, r. 1973, mnras, 161, 365 [31] velikhov, e.p. 1959, j. exper. theor. phys., 36, 1398 [32] vlemmings, w.h.t., et al. 2005, mem. sai, 2005, 76, 531 (astro-ph/0509025) [33] wang, j. c. l., sulkanen, m. e., lovelace, r. v. e., 1992, apj, 390, 46 188 http://dx.doi.org/10.1086/589759 http://dx.doi.org/10.1111/j.1365-2966.2006.10517.x http://dx.doi.org/10.1111/j.1365-2966.2012.21083.x http://dx.doi.org/10.1086/424993 http://dx.doi.org/10.1088/0004-637x/691/2/1360 introduction magnetorotational mechanism of explosion 2-d calculations magnetorotational instability jet formation in mre asymmetry of the explosion conclusions 282 acta polytechnica ctu proceedings 2(1): 282–285, 2015 282 doi: 10.14311/app.2015.02.0282 diagnostic of the symbiotic stars environment by thomson, raman and rayleigh scattering processes m. sekeráš1, a. skopal1 1astronomical institute of the slovak academy of sciences, 059 60 tatranská lomnica, slovakia corresponding author: msekeras@ta3.sk abstract symbiotic stars are long-period interacting binaries consisting of a cool giant as the donor star and a white dwarf as the acretor. due to acretion of the material from the giant’s stellar wind, the white dwarf becomes very hot and luminous. the circumstellar material partially ionized by the hot star, represents an ideal medium for processes of scattering. to investigate the symbiotic nebula we modeled the wide wings of the resonance lines ovi λ1032å, λ1038å and heii λ1640å emission line in the spectrum of ag dra, broadened by thomson scattering. on the other hand, raman and rayleigh scattering arise in the neutral part of the circumstellar matter around the giant and provide a powerful tool to probe e.g. the ionization structure of the symbiotic systems and distribution of the neutral hydrogen atoms in the giant’s wind. keywords: symbiotic stars spectroscopy. 1 introduction symbiotic stars are interacting binary systems consisting of a cool giant and a hot compact star most probably a white dwarf. typical orbital periods are between 1 and 3 years, but can be significantly larger. a small part of the material lost by the giant in the form of a stellar wind is accreted by the compact star. this process generates a very hot (th ∼ 105 k) and luminous (lh ∼ 102 − 104 l�) source of radiation, which then ionizes a fraction of the neutral wind from the giant, giving rise to nebular emission in the so-called symbiotic nebula. we distinguish two stages of symbiotic systems. a quiescent phase, when the hot star releases its energy with constant rate and spectral energy distribution, and active phase, when the symbiotic system significantly changes its radiation and brightens up by a few magnitudes in the optical. the partially ionized circumbinary environment represents an ideal medium for scattering processes. in particular we measure effects of the raman and rayleigh scattering of the hot star radiation on neutral atoms of hydrogen and the thomson scattering on free non-relativistic electrons. fig. 1 shows a sketch of simplified ionization structure of symbiotic stars with location of scattering processes in their environment. in this contribution we present the effects of these three types of scattering processes observed in the spectra of symbiotic stars and their possible applications. thomson scattering raman scattering & rayleigh white dwarf red giant ) h ii region (symbiotic nebula h i region figure 1: simplified ionization structure of a symbiotic star. while the radiation from emission region in a vicinity of the white dwarf is thomson scattered in ionized part of the circumstellar environment, in the neutral part it can be raman or rayleigh scattered. 2 thomson scattering the scattering of photons on free low-energy electrons (hν << mec 2) has a very small cross section σt = 6.652 × 10−25cm2 and is wavelength independent. within the symbiotic nebula this scattering will attenuate the cores of emission lines redistributing the scattered part of the line into its wings. the wings be282 http://dx.doi.org/10.14311/app.2015.02.0282 diagnostic of the symbiotic stars environment by thomson, raman and rayleigh scattering processes come very broad, because of a large thermal motions of free electrons, and due to the small value of σt , they will be faint. nevertheless the densest portions of symbiotic nebula with high electron concentration (ne ∼ 108 − 1012cm−3) together with the extremely intense emission lines of highly ionized elements formed in the vicinity of the hot star (e.g. ovi λ1032å, λ1038å) allow us to observe these broad wings. figure 2: a model (solid line) of the observed (dotted line) profile of the ovi λ1032, λ1038å emission lines as a result of thomson scattering in the spectra of ag dra during active and quiescent phase. to model the broad faint wings of the line profile, we adopted the theoretical line profile used already by castor et al. (1970). we applied modeling to the resonance dublet ovi λ1032å, λ1038å and heii λ1640å emission line in the (far-)uv spectra of symbiotic star ag dra. we determined the mean electron optical depth, τe, and electron temperature, te, of the symbiotic nebula during different levels of activity (fig. 2). during quiescent phases the mean value of τe = 0.056 ± 0.006 and te = 19 200 ± 2300 k. on the other hand during active phases τe = 0.64±0.11 and te = 32 300±2000 k (see sekeráš & skopal, 2012 in detail). during the active phases the hot star significantly enhances its stellar wind. this is supported by the broadening of the hα wings (skopal, 2006) as well as by the x-ray/uv flux anticorrelation observed in ag dra during active and quiescent phases (skopal et al., 2009). the material of the wind is ionized by the luminous hot star, which enhances radiation from the symbiotic nebula, which dominates the spectral region u. this produces a significant supplement of free electrons into the nebula. because τe depends on the electron concentration along the line of sight throughout the symbiotic nebula in direction to the hot star, its increase during the active phase indeed indicates the presence of an enhanced mass loss from the white dwarf (fig. 3). 8 9 10 11 0.1 0.3 0.5 0.7 0.9 1.1 1.3 u m ag ni tu de τe figure 3: during the transition from the quiescent phase (u∼11; bottom left) to the active phase (u∼8; top right), the ionized enhanced stellar wind from white dwarf represent a new source of free electrons into the nebula, which increases the electron optical depth τe. 3 raman scattering unlike the thomson scattering on free electrons, which acts in the ionized part of the red giant’s wind (symbiotic nebula), raman scattering arises within its neutral part around the giant. the raman scattering on neutral atoms of hydrogen represents the most pronounced effect. it is a process when a photon excites the atom from its ground state to an intermediate state, which is immediately stabilized by a transition to a different lower main energy level, resulting in emitting a photon of a different frequency. we can observe several raman emission features originated from scattered photons of intense emission lines, such as heii λ6545å (e.g. lee et al., 2003), cii λ7023å, λ7054å (schild & schmid, 1996), heii λ4851å (van groningen, 1993), etc. however the most conspicuous example of raman scattering are broad emission lines at λ6825å and λ7082å (e.g. schmid et al., 1989) (see fig. 4). these are the characteristic features in the spectrum of about half of symbiotic stars. they are result of scattering of resonance dublet of ovi λ1032å, λ1038å in the far-uv on neutral hydrogen atoms. their nature was confirmed by near-simultaneous uv and optical observations and spectropolarimetry (e.g. schild & schmid, 1996, birriel et al., 2000). the raman scattered lines often show a multi-peaked structure, even when the parental ovi emission line is single-peaked. to explain the line profile differences between the ovi lines and their raman scattered counterparts, schmid et al. (1999) suggest doppler shifts introduced in the raman scattering process and non-isotropic ovi line emission. moreover, the evolution of raman lines during quiescent and active phases can reveal the ionization structure around the hot star (e.g. skopal et. al., 2006, fig. 4 here). one of the main characteristic feature of the ramanscattered lines is the broadening according to the 283 m. sekeráš, a. skopal parental uv line. the wavelength λ0 of raman scattered radiation is associated with the wavelength λi of the incident uv radiation, which leads to the broadening of the raman emission lines by factor of λ0/λi. for example the raman emission at 6545å is broadened according to the parental heii λ1025å line by a factor of ≈ 6.4. as raman scattering is a dipol process we can observe strong polarization of the broad emission lines λ6825å and λ7082å. the amount and orientation of the polarization are expected to change periodically due to the orbital motion. this fact can be helpful to provide information concerning the orbital parameters, such as binary period, orientation and inclination of the orbital plane (e.g. schild & schmid, 1996, harries & howarth, 1996). 0 1 2 fl ux [ 10 -1 2 e rg c m -2 s -1 a -1 ] fuse: 05/07/2002 ϕ = 0.95 optical: 07/08/2002 ϕ = 0.99 o vi λ1032/500 raman λ6825 0 1 2 fuse: 22/10/2002 ϕ = 0.09 optical: 02/02/2003 ϕ = 0.23 o vi λ1032/150 raman λ6825 0 1 2 -200 -100 0 100 200 radial velocity [km/s] fuse: 04/08/2003 ϕ = 0.47 optical: 31/07/2003 ϕ = 0.47 o vi λ1032/400 raman λ6825 figure 4: comparison of the ovi λ1032å line profiles with their raman scattered counterparts along the outburst in symbiotic star z and (adopted from skopal et al., 2006). in addition to polarimetric measurements, the scattering geometry can be estimated by the raman scattering efficiency. it is defined as the ratio of the number of raman scattered photons to the number of emitted far-uv photons. this parameter strongly depends on the size of the neutral scattering region as ’seen’ by the original photons and thus also on the mass loss rate from the cool giant in symbiotic stars (e.g. lee et al., 2003). 4 rayleigh scattering in the case of rayleigh scattering, a photon excites an atom from its ground state to an intermediate state, which is immediately stabilized by a transition to a true bound state and this is followed by immediate reemission of a photon of the same wavelength. thus when the far-uv radiation from/around the hot star goes through the neutral part of the giant’s wind, it can be rayleigh scattered on the neutral hydrogen atoms. effect of this type of scattering is well observed in the form of strong attenuation of the continuum around hydrogen lines of the lyman series. the presence of rayleigh scattering was observed in the spectra of symbiotic stars with a high orbital inclination at/around the position of the inferior conjunction of the giant (e.g. eg and, vogel, 1991). figure 5 demonstrates this case for eg and. 1 3 5 7 9 3.1 3.2 3.3 3.4 3.5 3.6 fl ux [ 10 -1 3 e rg c m -2 s -1 a -1 ] log wavelength [a] eg and 13/01/1983 ϕ=0.95 figure 5: strong attenuation of the far-uv continuum by rayleigh scattering process (gray area) in the spectrum of eg and, close to the inferior conjunction of the giant. the cross section for raman scattering depends strongly on wavelength with λ−4, which is well demonstrated by monte carlo simulations by schmid (1995), and increases sharply toward lyman resonance transitions. therefore it is easily observable in far-uv spectrum (1200 å 1400 å) and not distinguishable in the optical. in optically thick environment the photon may undergo many rayleigh scatterings until it is raman scattered and escape the neutral region. rayleigh scattering arises in the neutral wind around the giant. if we consider the simplified steady284 diagnostic of the symbiotic stars environment by thomson, raman and rayleigh scattering processes state ionization model of the symbiotic star (see fig. 1), where the hi zone is approximately cone-shaped with the giant at its top (seaquist et al., 1984), it is obvious that the effect of rayleigh scattering will depend on the ionization structure, the inclination of the orbital plane and the orbital phase. it is therefore most easily measurable in eclipsing systems as periodic changes in the far-uv radiation. through the rayleigh scattering we can measure the neutral hydrogen column density in the line of sight as a function of the orbital phase, with typical values of 1020 − 1024cm−2. in this way, it is possible to explore the density and distribution of the neutral hydrogen and thus also the velocity structure in outer atmosphere of a red giant (e.g. vogel, 1991, pereira et al., 1999). 5 conclusions the nature of the environment around the symbiotic stars, with a fully ionized and also the neutral part of the circumstellar matter, allow us to investigate symbiotics through the effects of scattering processes. thomson scattering on free electrons can diagnose the symbiotic nebula by determining the mean electron optical depth, τe, and electron temperature, te. while the nebula is directly connected with the changes of the hot star properties, the effects of thomson scattering can provide some information also about the symbiotic nebula during the quiescent and active phase. raman and rayleigh scattering on neutral hydrogen atoms arises in the neutral part of the giant’s wind. they are observed in a form of broad emission features and an attenuation of the far uv continuum, respectively. these processes are useful to examine the ionization structure of the symbiotic systems, kinematics of the scattering and emitting region, the structure and density distribution of the neutral hydrogen in the giant’s wind and thus its mass loss rate. because the environment, where these scattering processes arises, is a result of the interaction between the giant and the white dwarf, they can provide also information about orbital parameters and physical properties of the two stars independently of other approaches. acknowledgement the research was supported by a vega grant of the slovak academy of sciences no. 2/0002/13. references [1] birriel, j. j., et al.: 2000, apj 545, 1020. doi:10.1086/317851 [2] castor, j.i., smith, l.f., van blerkom, d.: 1970, apj 159, 1119. doi:10.1086/150393 [3] harries, t. j., howarth, i. d.: 1996, a&a 310, 235. [4] lee, hee-won., et al.: 2003, apj 598, 553. doi:10.1086/378886 [5] pereira, c. b., et al.: 1999, a&a 344, 607. [6] schild, h., schmid, h.m.: 1996, a&a 310, 221. [7] schmid, h. m., et al.: 1989, a&a 211, l31. [8] schmid, h. m., et al.: 1999, a&a 348, 950. [9] seaquist, e. r., taylor, a. r., button, s.: 1984, apj 284, 202. doi:10.1086/162399 [10] sekeráš, m., skopal, a..: 2012, mnras 427, 979. doi:10.1111/j.1365-2966.2012.21991.x [11] skopal, a.: 2006, a&a 457, 1003. [12] skopal, a., et al.: 2006, a&a 453, 279. [13] skopal, a., et al.: 2009, a&a 507, 1531. [14] van groningen, e.: 1993, mnras 264, 975. [15] vogel, m.: 1991, a&a 249, 173. 285 http://dx.doi.org/10.1086/317851 http://dx.doi.org/10.1086/150393 http://dx.doi.org/10.1086/378886 http://dx.doi.org/10.1086/162399 http://dx.doi.org/10.1111/j.1365-2966.2012.21991.x introduction thomson scattering raman scattering rayleigh scattering conclusions 188 acta polytechnica ctu proceedings 2(1): 188–191, 2015 188 doi: 10.14311/app.2015.02.0188 swsex stars, old novae, and the evolution of cataclysmic variables l. schmidtobreick1, c. tappert2 1european southern observatory, casilla 19001, santiago 19, chile 2departamento de f́ısica y astronomı́a, universidad de valparáıso, avda. gran bretaña 1112, valparáıso, chile corresponding author: lschmidt@eso.org abstract the population of cataclysmic variables with orbital periods right above the period gap are dominated by systems with extremely high mass transfer rates, the so-called sw sextantis stars. on the other hand, some old novae in this period range which are expected to show high mass transfer rate instead show photometric and/or spectroscopic resemblance to low mass transfer systems like dwarf novae. we discuss them as candidates for so-called hibernating systems, cvs that changed their mass transfer behaviour due to a previously experienced nova outburst. this paper is designed to provide input for further research and discussion as the results as such are still very preliminary. keywords: cataclysmic variables dwarf novae novae sw sextantis stars. 1 introduction in the following we briefly review our current knowledge on the populations of old novae and sw sextantis stars especially in the context of the evolution of cataclysmic variable stars (cvs). 1.1 evolution of cvs in general, the evolution of stable interactive binaries is driven by angular momentum loss which as such determines the mass transfer rate. the loss of angular momentum as a source for stable mass transfer implicates that the general evolutionary direction for cvs is from longer to shorter orbital periods. according to the standard model of cv evolution, the main source of angular momentum loss for cvs with orbital periods porb > 3 h is magnetic braking. due to the continuous mass transfer, the secondary is pushed out of thermal equilibrium and becomes bloated. at a period of about 3 h, i.e. at the upper edge of the period gap, the secondary becomes fully convective, magnetic braking ceases and only the much weaker braking through the emission of gravitational radiation continues. therefore, the mass transfer is greatly diminished which allows the secondary star to relax into a state of thermal equilibrium and to contract to a volume corresponding to its mass. it thus loses contact with its roche lobe and mass transfer stops completely. the angular momentum loss via gravitational radiation shrinks the orbit of the now detached and therefore hardly detectable binary until the secondary star fills its roche lobe again at an orbital period of about 2 h, i.e. at the lower edge of the gap and the binary continues as a low mass transfer cv below the gap. for an extensive review of the current understanding of cv evolution, see knigge et al.̃(2011). 1.2 swsex stars this sub-class was originally defined by thorstensen et al. (1991). incorporating eclipsing nova-like stars with single-peaked emission lines, high velocity line wings, strong he ii emission but no polarisation, and transient absorption features at orbital phases around φ = 0.5. the radial velocity curves show an offset of 0.2 cycle with respect to the phase defined by the eclipse. today, sw sex stars are considered novalike stars with an extremely high mass transfer rate (see e.g. rodŕıguez-gil et al. 2007a,b). this is supported by the high temperatures found for the white dwarfs in these systems (townsley & gänsicke, 2009). while sw sex stars used to be considered as rare and strange objects with unusual behaviour, it has been shown in the last years that they in fact represent the dominant cv population in the orbital period range between about three and four hours (schmidtobreick et al., 2012). from a sample of cvs that was purely seleceted to have an orbital period between three and four hours, they find that the percentage of sw sex stars in this range must exceed 85%. according to the standard model, all long period cvs have to evolve through this period range before entering the gap and will thus share the sw sex characteristics 188 http://dx.doi.org/10.14311/app.2015.02.0188 sw sex stars, old novae, and the evolution of cataclysmic variables during that time. this makes the sw sex phenomenon a phase in the secular evolution of cvs (schmidtobreick et al. in preparation). 1.3 old novae classical novae are cvs that experience a thermonuclear runaway on the surface of the white dwarf where the accreted material has reached a critical mass. in this process, the binary is not destroyed and mass transfer is usually re-established within a few months. it is therefore safe to assume that nova explosions are recurrent events and part of the evolution of every cv with a sufficiently high mass transfer rate to accumulate the necessary material on the white dwarf surface within its lifetime. inbetween the nova events, the behaviour of the cv depends on properties like orbital period, mass-transfer rate, and magnetic field of the white dwarf that also determine its subtype. in addition, the hibernation model predicts changes of the mass transfer rate in the evolution of the preand postnova: after an initial phase of high mass transfer rate – due to the secondary star being driven strongly out of thermal equilibrium via irradiation from the eruptionheated white dwarf – which increases the distance between the two stars, the binary should descend into a long state of low mass transfer once the white dwarf cooled down and the secondary is allowed to relax more towards thermal equilibrium. (shara et al., 1986; prialnik & shara, 1986). some potential evidence for hibernation has been presented in the form of old nova shells around cvs that have previously been known as low mass transfer systems, i.e. z cam (shara et al., 2007) and at cnc (shara et al., 2012). however this interpretation is not exclusive, as the presence of nova shells around dwarf novae could also indicate that all types of cv (including dwarf novae) can experience a nova explosion during their lifetime without necessarily undergoing cyclic changes of the mass transfer rate. 2 what can we learn combining our knowledge from old novae and swsex stars? several years ago, we conducted a project investigating old novae which had experienced large outburst amplitudes (schmidtobreick et al., 2003; 2005). the idea behind this was that since the absolute magnitude of a nova explosion depends mainly on the mass of the white dwarf (livio, 1992) it thus differs only slightly for different systems. thus, novae with large outburst amplitudes are likely to be intrinsically faint cvs and therefore candidates for low mass transfer rate systems. two systems of our sample, v842 cen and xx tau, show spectroscopic properties that, compared to other old novae, indicate a rather low mass transfer rate. the spectra present comparatively strong balmer emission lines from hα bluewards down to h11. a weak heii emission line is present at 469 nm and indicates a hot component in the system, but at the same time the presence and strength of the hei series is evidence for a significant amount of cooler material. we note that most old novae do not share these characteristics (e.g., ringwald et al. 1996, tappert et al. 2012, 2014). for xx tau, preliminary analysis of long-term photometric monitoring covering a range of 150 d furthermore shows a probable dwarf-nova like outburst with an amplitude of ∼0.8 mag and a duration of ∼10 d (tappert, private communication), which represents additional evidence for a comparatively low mass transfer rate. the approach by tappert et al. (2012) to re-discover lost old novae revealed two more such candidates from spectroscopy: v2109 oph and v728 sco. in particular v728 sco which has also been observed photometrically can be considered a low mass transfer system as it also shows frequent stunted dwarf novae outbursts (tappert et al., 2013a). for three of these low mass transfer old novae, i.e. v842 cen, v728 sco, and xx tau, at least rough values for the orbital period could be established (woudt et al., 2009; luna et al., 2012; tappert et al., 2013a; rodŕıguez-gil & torres, 2005) and they all fall into the range of sw sex stars, i.e. between 3 and 4 hours. on the one hand, this period range is thus dominated by high mass transfer cvs. on the other hand, also the majority of old novae have high mass transfer rates. in fact, the period distribution of old novae shows a distinctive peak in the 2.8-5 h period range, while few novae are found in the period bins that are dominated by dwarf novae (e.g., tappert et al. 2013b, schmidtobreick & tappert 2014). thus, the indicated low mass transfer nature of v842 cen, v728 sco and xx tau is somewhat surprising. for the sake of completeness, we point out that other low mass transfer novae are known. for example, the system v446 her (porb = 4.97 h, thorstensen & talor, 2000) shows frequent ”stunted” dwarf-nova like outbursts (honeycutt et al. 1998). however, we here restrict our discussion to systems with orbital periods in the 3-4 h range. when thinking about a reason why several old novae would appear as low mass transfer systems even though some of them are even situated in the sw sex regime, hibernation comes naturally to mind. it seems an attractive explanation that these cvs have indeed been sw sex stars which due to the nova explosion in the recent past were pushed into a low state and thus experience low mass transfer rates at the moment. in 189 l. schmidtobreick, c. tappert this context we point out that v728 sco in outburst presents a triangular eclipse shape that is typical for sw sex stars (tappert et al., this volume). 3 conclusions and future work cvs with orbital periods between 3 and 4 hours are in general sw sex stars and as such experience high masstransfer rates. however, we find evidence for three old novae with orbital periods in this range that should be of sw sex type but are instead low mass transfer systems. we tentatively conclude that the mass transfer of these systems was changed by the nova eruption, similar to what is proposed in the hibernation scenario. whether the mass transfer in these systems will completely cease or just remain on a low level before rising up again remains to be investigated. to better understand the recent mass transfer history and to thus shed light on the evolutionary state of these systems, it would be important to measure the dynamical masses and the temperatures of the two components in order to determine the binary solution. for this, it is valuable to have a system like v728 sco in the sample which as eclipsing binary offers more opportunities to determine the binary parameters. to test the idea that the low mass transfer novae in the sw sex regime are affected by hibernation, it will be essential to check for the few existing dwarf novae in the sw sex range whether they have experienced a nova eruption in the past. we thus started an observational project to look for nova shells around these objects. other possible candidates for hibernating cv could be found among the so-called pre-cvs, white-dwarf/mainsequence binary which are detached systems. examples for such candidates are ltt 560 (tappert et al., 2011) and qs vir (drake et al., 2014, and references therein) which both have orbital periods in the sw sex range and show evidence of accretion. if indeed a significant number of these low mass transfer systems in the sw sex regime can be shown to have experienced a nova outburst in the past, this would not only be strong evidence for the hibernation scenario but at the same time also prove the evolutionary significance of the sw sex stars as it would yield a natural explanation for the few remaining cvs in the 3-4 h period range that do not follow the sw sex behaviour. acknowledgement this research was supported by fondecyt regular grant 1120338 (ct). we gratefully acknowledge the use of the simbad database, operated at cds, strasbourg, france, and of nasa’s astrophysics data system bibliographic services. we thank an anonymous referee for valuable comments. references [1] knigge c., baraffe i., patterson j., 2011, apjs 194, 28 doi:10.1088/0067-0049/194/2/28 [2] drake j. j., garraffo c., takei d, gänsicke b., 2014, mnras 437, 3842 doi:10.1093/mnras/stt2186 [3] honeycutt r. k., robertson j. w., turner g. w., henden a. a., 1998, apj 495, 933 doi:10.1086/305299 [4] livio, m. 1992, in vina del mar workshop on cataclysmic variable stars, edited by n. vogt, asp conf. ser. 29, 4. [5] luna g. j. m., diaz m. p., brickhouse n. s., moraes m., 2012, mnras, 423, l75. doi:10.1111/j.1745-3933.2012.01260.x [6] prialnik, d., & shara, m. m. 1986, apj, 311, 172. doi:10.1086/164763 [7] ringwald f. a., naylor t., mukai k., 1996, mnras 281, 192 doi:10.1093/mnras/281.1.192 [8] rodŕıguez-gil p., schmidtobreick l., gänsicke b. t., 2007a, mnras 374, 1359 doi:10.1111/j.1365-2966.2006.11245.x [9] rodŕıguez-gil p., gänsicke b. t., hagen h.-j. et al., 2007b, mnras 377, 1747 doi:10.1111/j.1365-2966.2007.11743.x [10] rodŕıguez-gil p., torres m. a. p., 2005, a&a, 431, 289 [11] schmidtobreick l., tappert c., saviane i., 2003a, mnras 342, 145 doi:10.1046/j.1365-8711.2003.06523.x [12] schmidtobreick l., tappert c., bianchini a., mennickent r. e. 2003b, a&a, 410, 943. [13] schmidtobreick l., tappert c., bianchini a., mennickent r. e., 2005, a&a, 432, 199. [14] schmidtobreick l., rodŕıguez-gil p., gänsicke b. t., 2012, mem. s.a.it. vol. 83, 610 [15] schmidtobreick l., tappert c., 2014, stella novae: future and past decades. woudt & ribeiro (eds), asp in press [16] shara, m. m., livio, m., moffat, a. f. j., & orio, m. 1986, apj 311, 163 190 http://dx.doi.org/10.1088/0067-0049/194/2/28 http://dx.doi.org/10.1093/mnras/stt2186 http://dx.doi.org/10.1086/305299 http://dx.doi.org/10.1111/j.1745-3933.2012.01260.x http://dx.doi.org/10.1086/164763 http://dx.doi.org/10.1093/mnras/281.1.192 http://dx.doi.org/10.1111/j.1365-2966.2006.11245.x http://dx.doi.org/10.1111/j.1365-2966.2007.11743.x http://dx.doi.org/10.1046/j.1365-8711.2003.06523.x sw sex stars, old novae, and the evolution of cataclysmic variables [17] shara m. m., martin c. d., seibert m., rich r. m., salim s., reitzel d., schiminovich d., deliyannis c. p., sarrazine a. r., kulkarni s. r., ofek e. o., brosch n., lépine s., zurek d., de marco o., jacoby g., 2007, nature 446, 159 [18] shara m. m., mizusawa t., wehinger p., zurek d., martin c. d., neill j. d., forster k., seibert m., 2012, apj 758, 121. [19] tappert c., gänsicke b. t., schmidtobreick l., ribeiro t., 2011, a&a 532, 129 [20] tappert c., ederoclite a., mennickent r. e., schmidtobreick l., vogt n. 2012, mnras, 423, 2476. [21] tappert c., vogt n., schmidtobreick l., ederoclite a., vanderbeke j., 2013a, mnras 431, 92 [22] tappert c., schmidtobreick l., vogt n., ederoclite, a., 2013b, mnras 436, 2412 [23] tappert c., vogt n., della valle m., schmidtobreick l., ederoclite a., 2014, mnras in press [24] thorstensen j. r., taylor c. j., 2000, mnras 312, 629 [25] thorstensen j. r., ringwald f. a., wade r. a., schmidt g. d., norsworthy j. e., 1991, aj 102, 272 [26] townsley d. m., gänsicke b. t., 2009, apj 693, 1007 [27] woudt, p. a., warner, b., osborne, j., page, k. 2009, mnras, 395, 2177. discussion vitaly neustroev: you claim that some old novae have a very small mass transfer rate. does it mean that these stars should show dn-type outbursts? linda schmidtobreick: yes, indeed. and some stars do show such outbursts. we don’t yet have a lot of data but we have observed several outbursts for v728 sco. 191 introduction evolution of cvs swsex stars old novae what can we learn combining our knowledge from old novae and swsex stars? conclusions and future work acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0012 acta polytechnica ctu proceedings 7:12–17, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app microscopic features of cement paste modified by fine perlite vladimír hrbeka,∗, veronika koudelkováb, pavel padevěta, petr šašekb a czech technical university, thakurova 6, prague 6, czech republic b institute of theoretical and applied mechanics as cr, v.v.i., prosecka 76, prague 9, czech republic ∗ corresponding author: vladimir.hrbek@fsv.cvut.cz abstract. the use of waste material and replacement of binder element in cementitious composites is in focus of material development. perlite in the construction industry is usually used in form of lightweight aggregate enhancing the insulating performance of concrete. this paper focuses on integration of fine perlite into the cement matrix and possible replacement of the cement binder in the composition of the material. the macromechanical performance of the modified paste is tested on specimens with 5, 10, 15 and 20 % fine perlite substitution and pure cement sample. to distinguish the effect of the perlite on the microstructural level, pure cement material and specimen containing 10 % of fine perlite are investigated by the electron microscopy. furthermore, the mechanical properties of individual phases are examined and compared on same samples by instrumented indentation. the presented results enabled estimation of fine perlite impact on the macro and microscopic performance of the material. keywords: perlite, sem, nanoindentation, mechanical properties. 1. introduction reduction of energy consumption and co2 emissions production is the important challenge in the concrete industry at the present time, thus the focus on the utilization of different waste material partly replacing cement binder plays the key role in the field of research [1]. among supplementary materials perlite represents an expanded natural material produced through loosing water during heating of source material hydrous volcanic glass. most frequently is perlite with its porous structure used as a filler in the lightweight concretes. moreover, it also improves concrete insulation properties and fire resistance. processing of the crude natural volcanic material and the production of perlite lead into creation of perlite fines currently considered as the waste material [2]. the quality of concrete containing fine perlite is possible to asses from micro as well as from macro aspects. the most important phenomenon observable on the microscale is pozzolanic activity of perlite fines since creation of chemical bond between perlite particles and surrounding binder is crucial in developing proper mechanical properties of the cementitious mixture. the second important parameter is the total volume of fine perlite in cement which influences the mechanical behavior of cement composite. yu et. al [3] determined the most effective perlite content equal to 15 % since it significantly improved the compressive strength of concrete (about 16 mpa higher than in the case of concrete without perlite fines addition). similar results obtained rózycka and pichór [4] during testing of perlite waste addition effect on the properties of autoclaved aerated concrete. the compressive strength didn´t significantly changed up to 30 % of volume addition of perlite waste particles. on the contrary oktay et. al [5] determined that the highest compressive strength showed the concrete specimens with no addition of expanded perlite. the results mentioned above [3–5] confirms the importance of chemical availability of perlite particles resulting in creation of interface between perlite and surrounding binder. hence, this paper is aimed at the investigation of macroscopic and microscopic mechanical properties of cementitious paste containing different volume (5, 10, 15 and 20 %) of crushed fine perlite particles. the results of macroscopic testing determined samples for microscopical evaluation, where specimen with 10 % substitution of perlite is compared to pure cement paste. the microstructure is observed implementing the scanning electron microscope (sem), which enables defining different chemical phases and their interfaces in the material. the micromechanical properties of individual phases are determined from histograms of the results provided by instrumented indentation. 2. materials and methods the macroscopic specimens were prepared from ordinary portland cement cem i 42.5r mixture with water to cement ratio 0.35. the composition according to declaration of fine perlite producer is summarized in table 1. the specimens were placed in 40× 40× 160mm forms, cast out 24 hours after mixing and stored until 28 days of total age in water 12 http://dx.doi.org/10.14311/app.2017.7.0012 http://ojs.cvut.cz/ojs/index.php/app vol. 7/2017 to prevent the carbonation. the sets of specimens are denoted as modcem x.xx, where x.xx stands for the fine perlite percentage substitution and specimen modcem 0.00 served as reference sample (pure cement paste). the residues from macroscopic testing were embedded in epoxy resin and used for microscopic investigation. the samples were sectioned by diamond cut-off wheel and the surface grinded and polished using silica-carbon papers (grid roughness p1200, p2400 and p4000 according to european p-grade system) and the 3 µm diamond suspension. chemical content granulometry sio2 min 66 % > 0.2 mm max 10 % al2o3 max 18 % > 0.1 mm min 50 % fe2o3 max 3 % < 0.1 mm max 50 % cao + mgo max 6 % na2o + k2o max 8 % table 1. composition of used fine perlite. 2.1. macromechanical testing to determine macromechanical properties i.e. bending strength and compressive strength, 6 macroscopic specimens (40× 40× 160mm dimensions) were tested from each type of cement mixture. tensile stresscapacity was determined from load-controlled threepoint bending test with support spacing of 100 mm (l) from the equation 1, where ft is maximum applied force causing bending moment, b and h are dimensions of sample cross-section. σt = 3 2 ftl bh2 (1) compressive strength of samples was determined by load-controlled compression test with pressure pad area of 40×40mm and calculated according the equation 2, where fc is maximum applied compressive force and a is the pressure pad area (40× 40 mm). σc = fc a (2) figure 1. macroscopic tests setting – three-point bending (left), compression (right). 2.2. sem sem investigation was performed in mira ii lmu (tescan corp., brno) on polished specimens coated with thin layer of carbon necessary to ensure proper conductivity of the surface. working distance of the microscope was set closely to 15 mm and accelerating voltage was set to 15 kv to provide good signal. the micrographs were acquired at different magnifications. each specimen was investigated at first at the magnification 600× to gain good overview and than at higher magnifications (above 1200×) for better study of different phases in detail. sem micrographs acquired with back scattered electron detector (bse) provide information about distribution and chemical composition of different phases since back scattering coefficient strongly depends on the atomic number z. 2.3. nanoindentation to determine micromechanical properties, instrumented grid indentation using nanoindenter ti 750 serie (hysitron inc.) was performed on the polished specimens with high surface quality. in this technique mechanical properties are calculated from the unloading part of the force-displacement dependency diagram. one of the most important parameter which can be directly calculated is hardness h defined as pressure the maximum force (pmax) under the contact area of the tip (ac). h = pmax ac (3) the reduced (effective) elastic modulus (er) of measured volume of the material follows from the relationship between the unloading stiffness (s) and contact area with respect to the probe geometry (β) [6]. er = √ π 2β s√ ac (4) a grid indentation of 10× 10 pattern with equally spaced indents (30 µm separation) was used in order to cover sufficient area containing all material phases. the load-controlled protocol of indentation consisted of loading holding unloading parts lasting 5 25 5 seconds respectively and reaching maximum applied force of 2.5 mn. to obtain proper statistical set of measured data, four grid indentations were performed on different places of each sample. mechanical properties of individual phases in the heterogeneous cement paste can be obtained from the histograms with equally spaced bins of the examined property by statistical deconvolution [7, 8]. in this paper, we assess the properties of individual phases based on difference between histograms of indentation results of modified cement paste (modcem 0.10) and referential specimen (modcem 0.00). 13 v. hrbek, v. koudelková, p. padevět, p. šašek acta polytechnica ctu proceedings 3. results 3.1. three-point bending, compression the results of macromechanical testing (table 2) correspond with results presented by oktay et. al [5], i.e. referential pure cement samples reach the highest values of compressive (81.89± 9.68 mpa) and tensilestress capacity (1.50 ± 0.83 mpa). mod/ref value present deviation of specimen mechanical property from referential sample. at this preliminary stage of research, perlite modification of cement paste with similar macromechanical performance was in focus. according to table 2, specimens containing 10% of fine perlite substitution (modcem 0.10) exhibit lowest decrease of both compressive and tensile-stress capacity (about 8% and 4% respectively). this led to selection of modcem 10 sample for microscopic investigation of the material. compressive strength specimen σc [mpa] denotion mean stat.dev. mod/ref modcem 0.00 81.89 9.68 1.00 modcem 0.05 64.01 13.28 0.78 modcem 0.10 76.04 10.84 0.93 modcem 0.15 64.69 5.42 0.79 modcem 0.20 70.80 11.32 0.87 tensile strength specimen σt [mpa] denotion mean stat.dev. mod/ref modcem 0.00 1.50 0.83 1.00 modcem 0.05 1.36 0.63 0.91 modcem 0.10 1.45 0.52 0.97 modcem 0.15 1.57 0.34 1.05 modcem 0.20 1.56 0.30 1.04 table 2. macromechanical test results. 3.2. sem investigation the sem equipped with energy dispersive x-ray detector (edx) enables to distinguish different phases in the studied cementitious materials (modcem 0.00, modcem 0.10). based on the bse micrographs and epma (electron probe microanalysis using edx) was possible to determine five phases clinker, csh gels, portlandite (calcium hydroxide ch), pores and perlite particles (see in the figure 2). clinkers in the gray-scaled bse micrographs represent the most intensive particles because of their dense structure and high iron and calcium content. around clinker particles is possible to determine darker well defined area called high density calcium-silica-hydrate gel (hd-csh) as a result of progressive slow hydration of non-hydrated clinker cores. the hd-csh gel represent the first one modification of csh, the second one is low density csh gel (ld-csh) with more opened porous structure. figure 2. bse micrograph showing microstructure of cement paste with perlite addition. the size of perlite was variable from approximately 200 µm of undamaged whole particles to perlite fines i.e. internal lamella of perlite with various size. the interface between undamaged perlite particles and surrounding cement matrix was sharp and didn’t show in most cases any chemical reaction detectable at microscale in the sem (figure 4). nevertheless, according to literature perlite fines are considered as good pozzolanic material [3]. in our investigation chemical reaction between crushed internal lamella and cement was observed in the specimen modcem 0.10. the evident structural disintegration coupled with decreasing content of si in affected perlite lamella is demonstrated in the figure 3. figure 4. bse micrograph showing microstructure of cement paste with perlite addition. 14 vol. 7/2017 figure 3. sem – eds of integrated perlite fines – si content decrease and detail of lamella integration. the decreasing tendency of si content can be also presented on epma with edx analysis results of perlite lamella and cement matrix boundary. figure show positions of testing and table describes weight percentage containment (wpc) of individual elements in each position of interest. position 4 with si containment 10.55% of weight correspond to csh phases and position 8 (si wpc 16.31%) to pure perlite [9]. figure 5. epma – edx of perlite lamella and cement. pos 8 7 6 5 4 ca 9.80 27.61 23.49 23.25 23.91 si 16.31 15.38 13.96 11.39 10.55 al 3.11 2.88 3.34 2.27 4.22 mg 0.05 0.06 0.23 0.19 0.21 k 4.09 1.75 4.29 4.65 5.28 na 0.76 1.26 1.12 0.80 0.73 s 0.30 0.40 0.36 0.71 0.42 fe 1.17 0.51 0.86 0.82 1.22 o 64.42 50.15 55.85 55.91 53.47 table 3. epma – edx chemical elements analysis (weight percentage containment in %). 3.3. instrumented indentation the previously described phases of the material (ld csh, hd csh, ch and clinker) and their mechanical properties (reduced modulus) can be observed in the indentation histogram. the ld csh forms a significant peak close to 30 gpa, which is consistent with previous research (21.7 ± 2.2 gpa [7, 8, 10]). measured indentation modulus of the hd csh phase is close to 40 gpa (occurrence of peaks in range 35 to 50 gpa) and the ch reaches up to 60 gpa, according to the figure 6. more accurately, using statistical deconvolution, reduced modulus estimation reach 27.34± 2.56 for ld csh phase, 39.29± 4.11 gpa for hd csh phase and 61.54± 4.30 gpa for ch phase. compare to phase reduced modulus measured on samples with w/c ratio 0.5 (29.4± 2.4 gpa), hd csh phase reaches peak of indentation modulus naturally higher due to lower w/c ratio. the clinker phase is not in focus of this study due to its high stiffness and interference with other “low stiffness” phases, which misrepresent the result of indentation (collected data above 90 gpa are therefore excluded). figure 6. modcem 0.00 – reduced modulus histogram. figure7 represents the indentation data measured on specimen modcem 0.10. significant peaks of the cementitious matrix are slightly shifted to lower values due to the interaction of fine perlite residues to the composite structure and formation of “low stiffness" phase. the formation is not yet known to authors and will be subjected to further investigation. the 15 v. hrbek, v. koudelková, p. padevět, p. šašek acta polytechnica ctu proceedings individual phases of the cement form the peaks around 25 gpa for ld csh phase, 33 gpa for hd csh and 49 gpa in case of ch phase. the young’s modulus of expanded perlite is assumed to be equal 20 gpa [11, 12], which correspond to the peak found in the histogram. there is very significant peak formed around 10 gpa, which the authors have not been able to identify yet. the lower indentation modulus of all phases in modified cement paste also explains the decrease of macroscopic performance of the composite. figure 7. modcem 0.10 – reduced modulus histogram. 4. conclusions cementitious composite with substitution of fine perlite was investigated on macro and microscopical level. the macro mechanical testing of specimens showed slight decrease of material strength for all cases of cement replacement. the lowest decrease was observed on modcem 0.10, which was thus tested on microscopical level. the investigation of microstructure with sem proved the interaction of fine perlite lamella with cement matrix and integration of whole perlite particles. the instrumented indentation enabled to identify impact of cement paste modification due to comparison of referential data and reduced modulus of phases in specimen modcem 0.10. more detailed interaction of fine perlite and cement composite will be further researched. list of symbols σt bending strength [mpa] ft maximum applied force causing bending moment [n] b specimen cross section width [m] h specimen cross section height [m] σc compressive strength [mpa] fc maximum applied compressive force [n] a pressure pad area [m−2] l spacing of supports [m] h hardness [gpa] pmax maximum force [pa] ac contact area under the tip [nm−2] er reduced elastic modulus [gpa] β probe geometry constant [–] s stiffness [nm−1] acknowledgements the research has been supported by czech science foundation (project no. p105/12/g059). references [1] paris j.m., roessler j.g., ferraro c.c., deford h.d., townsend t.g., a review of waste products utilized as supplement to portland cement in concrete. j clean product 121:1 – 18, 2016. doi: 10.1016/j.jclepro.2016.02.013 [2] kotwica l., pichór w., nocún-wczelik w., study of pozzolanic action of ground waste expanded perlite by means of thermal methods. j therm anal calor 123:607 – 613, 2016. doi: 10.1007/s10973-015-4910-8 [3] yu l.h., ou h., lee l.l., investigation on pozzolanic effect of perlite powder in concrete. cem con res 33:73 – 76, 2003. doi: 10.1016/s0008-8846(02)00924-9 [4] rózycka a., pichór w., effect of perlite waste addition on the properties of autoclaved aerated concrete. const built mat 120:65 – 71, 2016. doi: 10.1016/j.conbuildmat.2016.05.019 [5] oktay h., yumrutas r., akpolat a., mechanical and thermophysical properties of lightweight aggregate concretes. const built mat 96:217 – 225, 2015. doi: 10.1016/j.conbuildmat.2015.08.015 [6] oliver w.c., pharr g.m., measurement of hardness and elastic modulus by instrumented indentation: advances in understanding and refinements to methodology. j mat res 19:3 – 20, 2004. doi: 10.1557/jmr.2004.0002 [7] constantinides g., chandran k.r., ulm f.j., vliet k.v., grid indentation analysis of composite microstructure and mechanics: principles and validation. mat sci eng a 430:189 – 202, 2006. doi: 10.1016/j.msea.2006.05.125 [8] němeček j., vondřejc j., králík v., micromechanical analysis of heterogeneous structural materials. cem con com 36:85 – 92, 2013. doi: 10.1016/j.cemconcomp.2012.06.015 [9] kabra s., katara s., rani a., characterization and study of turkish perlite. inter j innovative res sci, eng and techno 2:4319 – 4326, 2013. issn: 2319-8753 [10] velez k., maximilien s., damidot d., fantozzi g., sorrentino f., instrumented determination by nanoindentation of elastic modulus and hardness of pure constituents of portland cement clinker. cem con res 31:555 – 561, 2001. doi: 10.1016/s0008-8846(00)00505-6 [11] sengul o.,azizi s.,karaosmanoglu f.,ali m., effect of expanded perlite on the mechanical properties and thermal conductivity of lightweight concrete. energy build 43:671 – 676, 2011. doi: 10.1016/j.enbuild.2010.11.008 [12] abidi s., joliff y.,favotto c., impact of perlite, vermiculite and cement on the young modulus of a plaster composite material: experimental, analytical and numerical approaches. compos. b 92:281 – 36, 2016. doi: 10.1016/j.compositesb.2016.02.034 16 acta polytechnica ctu proceedings 7:12–16, 2017 1 introduction 2 materials and methods 2.1 macromechanical testing 2.2 sem 2.3 nanoindentation 3 results 3.1 three-point bending, compression 3.2 sem investigation 3.3 instrumented indentation 4 conclusions list of symbols acknowledgements references 331 acta polytechnica ctu proceedings 2(1): 331–333, 2015 331 doi: 10.14311/app.2015.02.0331 the golden age of cataclysmic variables and related objects ii concluding address f. giovannelli1 1inaf istituto di astrofisica e planetologia spaziali, area di ricerca di tor vergata, via fosso del cavaliere, 100 i00177 roma, italy corresponding author: franco.giovannelli@iaps.inaf.it abstract before to conclude officially this workshop — far from me the idea to attempt some concluding remarks already dealt at the meeting with various burning by joseph patterson, mariko kato, dmitry bisikalo, and rené hudec —, i would like to comment few highlights coming out from our fruitful week of discussions about the golden age of cataclysmic variables and related objects ii, without any pretension of completeness. keywords: cataclysmic variables and related objects photonic astrophysics. undoubtedly the advent of spacecrafts gave a strong impulse to astronomy; starting roughly from middle 1970ies almost all the electromagnetic spectrum was continuously surveyed by the many space experiments. the cataclysmic variables (cvs) historically were the first systems for triggering the studies of the accretion disk around white dwarfs (wds) starting from the 1960’s with the schools of warsaw (poland) and cambridge (uk). however, they lost rapidly their primeval importance because of the advent of the first x-ray space experiments that, with their limited sensitivity, were mostly detecting x-ray binary systems (xrbs) that showed x-ray emissions abundantly over the thresholds of their detectors. this thanks to the presence of neutron stars or black holes as companions of the optical low–mass or high–mass stars. the x-ray emission of cvs is about 2–3 orders of magnitude lower than that of xrbs. thus the bulk of cvs observations was coming for long time from optical and uv regions, and sometimes from ir and seldom from radio bands. in the last decade results coming from the new generation satellites, especially in the hard x–ray and γ– ray regions, renewed the interest of scientific community about cvs. this, together with the new developments in searching for the progenitors of type ia supernovae was the main reason for an new explosion of interest about cvs. during this week of a deep discussion about cvs and related objects, mostly through the physical processes occurring inside those systems, has shown the most powerful way for a better and faster development of our knowledge of the cataclysmic processes, rather usual in the universe. among the many experimental and theoretical results discussed during this workshop, i would like to remark one important old idea developed by vladimir lipunov in 1980’s, that, in my opinion, will stress the future of cvs physics. figure 1: lipunov’s diagram for gravimagneti rotators calculated for 1 m� white dwarf. the positions of the polars am her and ae aqr, and the intermediate polars dq her, ei uma, and ss cyg are marked (after lipunov, 1987). this is the physical description of cvs as gravimagnetic rotators (lipunov, 1982, 1987). in this way the behaviour of cvs is completely determined by the spin period of the wd and the gravimagnetic parameter y = ṁ/µ2, where ṁ is the mass accretion rate onto 331 http://dx.doi.org/10.14311/app.2015.02.0331 f. giovannelli the gravimagnetic rotator having mass m, and µ is its magnetic moment. this is valid also for all the compact objects, like neutron stars and black holes. in this way, the behavior of cvs is completely independent of the optical phenomena which until now have been those which prevailed in cataloging such systems in different classes. figure 1 shows a part of lipunov’s diagram where polars (pcvs), intermediate polars (ipcvs) and non–magnetic cvs (nmcvs) are situated. as discussed by giovannelli & sabau-graziati (this workshop), it appears evident that the most suitable approach for studying cvs from a physical point of view is to consider them as gravimagnetic rotators. the detection of several sw sex systems having orbital periods inside the so-called ’period gap’ opens a new interesting problem about the continuity in the evolution of cvs. are the ipcvs and pcvs smoothly connected via the sw sex-like systems placed just in between? in order to fully understand the emission properties and evolution of cvs, the mass–transfer process needs to be clearly understood, especially magnetic mass transfer, as well as the properties of magnetic viscosity in the accretion discs around compact objects. consequently, the investigation on the magnetic field intensities in wds appears crucial in understanding the evolution of cvs systems, by which it is possible to generate classical novae (e.g., isern et al., 1997) and type-ia supernovae (e.g., isern et al., 1993). in those catastrophic processes the production of light and heavy elements, and then the knowledge of their abundances provides strong direct inputs for cosmological models and cosmic ray generation problems. after this workshop it appears evident, once more, the importance of multifrequency astrophysics. however, there are many problems in performing simultaneous multifrequency, multisite, multiinstrument, multiplatform and multienergy measurements due to: i) objective technological difficulties; ii) sharing common scientific objectives; iii) problems of scheduling and budgets; iv) politic management of science. during this fruitful workshop, we hope to have demonstrated once more the “vulcano theorem” enunciated in 1984 in my concluding address: it is possible to develop science seriously even if smiling. but, as you probably suspected, this workshop has been organized under ”peaceful surroundings”. therefore, i would like to mention and to support tolstoy’s philosophy. ”think again”, was written by tolstoy in 1904, at the beginning of the russian-japanese war. the human conditions described by tolstoy in the war are ”like spiders in a glass”. this is a pamphlet that is not only against carnage...: ”again the suffering that benefits nobody, again the lies, and again the universal process of stupidity, the turning of men into beasts...” ...but that is also against the racism and the hypocrisy of the educated: ”scholars ... deal extensively with the laws of the migration of peoples, the relationship between the white and the yellow race, between buddhism and christianity, and according to their deductions and considerations justify the killing of men ...”. ... it shows unequivocally the tolstoyan base of gandhi’s non-violence doctrine: ”i cannot act in any other way than god requires of me, and therefore, as a man, i cannot take part in any war, neither directly nor through a third party, nor by giving orders, nor by cooperating in any form, nor by encouraging doing it: i cannot, i will not and i will not do it.” and finally, i would like to conclude with few wonderful words of dr daisaku ikeda (2001) – president of the soka gakkai international (sgi) – reported in the booklet for today and tomorrow the thought of 30th may: “the one who has many friends has greater opportunities for growth. in this way, one both makes society a better place, and lives happier and more satisfied. in all cases, human relations, the inter-personal interaction and communication are of vital importance. we must establish and nurture friendship and contacts with many people, both in our environment, and in society in general. in this manner our life will open up and will flourish”. we could go back to early childhood when we were as the ”little prince”. one sees clearly only with the heart. what is essential is invisible to the eye. (from ”the little prince” by antoine de saint exupéry). acknowledgement it is my pleasure to thank: the scientific organizing committee (dmitry bisikalo, massimo della valle, rené hudec, lola sabaugraziati, giora shaviv, paula szkody); the informatic operator (francesco reale alias figaro, the factotum) for helping in informatics and solving all related problems during the preparation and development of the workshop and in palermo, at the registration desk; 332 the golden age of cataclysmic variables and related objects ii concluding address the executive secretary daniela giovannini, who smoothed all the inconveniences occurred at the registration desk with professionalism and moreover with her nice smile. daniela giovannini (biologist) said goodbye to everybody and left in hurry tuesday afternoon because of the start of an important experiment in her institute (cnr/ibcn) about “treatment with a new generation of adjuvant to enhance the human immune response against the major infections”; the directors of the inaf-istituto di astrofisica e planetologia spaziali, roma, italy; intadepartamento de cargas utiles y ciencias del espacio, madrid, spain; ras-institute of astronomy, moscow, russia; inaf-osservatorio astronomico di capodimente, napoli, italy; ascr/astronomical institute, ondřejov & czech technical university, prague, czech republic; technion-department of physics, haifa, israel; department of astronomy, university of washington, seattle, wa, usa; the actresses lisa colosimo and flavia giovannelli; the violinist alessandro perpich and pianist valentina usai; the staff of the splendid hotel la torre. on behalf of the soc and loc, i am pleased to thank all participants and especially the speakers for their active contributions in rendering this workshop updated with their talks, alive with their discussions, and friendly with their attitudes. a special thank to the three colleagues and friends (joseph patterson, dmitry bisikalo, mariko kato, and rené hudec) who kindly accepted the not easy task of making the concluding remarks of the workshop. finally, on behalf of all participants, i would like to express my warm tanks to the chef, mr daniele inzerillo, who prepared for us a large number of delicacies. i hope to meet all of you once again during our next palermo workshop. references [1] giovannelli, f., sabau-graziati, l.: 2015, this volume. [2] ikeda, d.: 2001, for today and tomorrow the thought of 30th may, edizioni esperia. [3] isern, j., hernanz, m., garćıa-berro, e.: 1993, in white dwarfs: advances in observation and theory, m.a. barstow (ed.), kluwer academic publ., dordrecht, holland, nato asi ser., c403, 139. [4] isern, j., hernanz, m., abia, c., josé, j.: 1997, in frontier objects in astrophysics and particle physics, f. giovannelli & g. mannocchi (eds.), italian physical society, editrice compositori, bologna, italy, 57, 113. [5] lipunov, v.m.: 1982, ap&ss, 85, 451-457. doi:10.1007/bf00653467 [6] lipunov, v.m.: 1987, ap&ss, 132, 1-51. doi:10.1007/bf00637779 333 http://dx.doi.org/10.1007/bf00653467 http://dx.doi.org/10.1007/bf00637779 acta polytechnica ctu proceedings doi:10.14311/app.2015.1.0001 acta polytechnica ctu proceedings 2:1–7, 2015 © czech technical university in prague, 2015 available online at http://ojs.cvut.cz/ojs/index.php/app reinforced encoding for planning as sat tomáš balyo∗, roman barták, otakar trunda department of theoretical computer science and mathematical logic, faculty of mathematics and physics, charles university, malostranske namesti 2/25, praha 1, czech republic ∗ corresponding author: biotomas@gmail.com abstract. solving planning problems via translation to satisfiability (sat) is one of the most successful approaches to automated planning. we propose a new encoding scheme, called reinforced encoding, which encodes a planning problem represented in the sas+ formalism into sat. the reinforced encoding is a combination of the transition-based sase encoding with the classical propositional encoding. in our experiments we compare our new encoding to other known sas+ based encodings. the results indicate, that he reinforced encoding performs well on the benchmark problems of the 2011 international planning competition and can outperform all the other known encodings for several domains. keywords: planning, satisfiability, encoding. 1. introduction planning is the problem of finding a sequence of actions – a plan, that transforms the world from an initial state to a state that satisfies some goal conditions. the world is fully-observable, deterministic and static (only the agent we make the plan for changes the world). the number of possible states of the world as well as the number of possible actions is finite, though possibly very large. we will assume that the actions are instantaneous (take a constant time) and therefore we only need to deal with their sequencing. actions have preconditions, which specify in which states of the world they can be applied, as well as effects, which dictate how the world will be changed after the action is executed. one of the most successful approaches to planning is encoding the planning problem into a series of satisfiability (sat) formulas and then using a sat solver to solve them. the method was first introduced by kautz and selman [1] and is still very popular and competitive. this is partly due to the power of sat solvers, which are getting more efficient year by year. since then many new improvements have been made to the method, such as new compact and efficient encodings [2–5], better ways of scheduling the sat solvers [3] or modifying the sat solver’s heuristics to be more suitable for solving planning problems [6]. in this paper we present a new encoding scheme. it is inspired by the sase transition-based encoding [2], which was the first sat encoding based on the sas+ planning formalism. the motivation for our work is to make the sase encoding more robust by incorporating the strengths of older encoding schemes. we will prove the correctness of our encoding and compute an upper bound on the size of the encoded formula. in the experimental section of the paper we compare our new encoding to other sas+ encodings on benchmark problems from the 2011 international planning competition (ipc) [7]. 2. preliminaries in this section we give the basic definitions of satisfiability, and planning with parallel plans. 2.1. satisfiability a boolean variable is a variable with two possible values true and false. a literal of a boolean variable x is either x or ¬x (positive or negative literal). a clause is a disjunction (or) of literals. a clause with only one literal is called a unit clause and with two literals a binary clause. an implication of the form x ⇒ (y1 ∨ · · · ∨ yk) is equivalent to the clause (¬x∨y1∨· · ·∨yk). a conjunctive normal form (cnf) formula is a conjunction (and) of clauses. a truth assignment φ of a formula f assigns a truth value to its variables. the assignment φ satisfies a positive (negative) literal if it assigns the value true (false) to its variable and φ satisfies a clause if it satisfies any of its literals. finally, φ satisfies a cnf formula if it satisfies all of its clauses. a formula f is said to be satisfiable if there is a truth assignment φ that satisfies f . such an assignment is called a satisfying assignment. the satisfiability problem (sat) is to find a satisfying assignment of a given cnf formula or determine that it is unsatisfiable. 2.2. planning in the introduction we briefly described what planning is, in this section we give the formal definitions. we will use the multivalued sas+ formalism [8] instead of the classical strips formalism [9] based on propositional logic. a planning task π in the sas+ formalism is defined as a tuple π = {x,o, si , sg} where • x = {x1, . . . , xn} is a set of multivalued variables with finite domains dom(xi). 1 http://dx.doi.org/10.14311/app.2015.1.0001 http://ojs.cvut.cz/ojs/index.php/app t. balyo, r. barták, o. trunda acta polytechnica ctu proceedings • o is a set of actions (or operators). each action a ∈ o is a tuple (pre(a), eff(a)) where pre(a) is the set of preconditions of a and eff(a) is the set of effects of a. both preconditions and effects are of the form xi = v where v ∈ dom(xi). • a state is a set of assignments to the state variables. each state variable has exactly one value assigned from its respective domain. we denote by s the set of all states. si ∈ s is the initial state. sg is a partial assignment of the state variables (not all variables have assigned values) and a state s ∈ s is a goal state if sg ⊆ s. an action a is applicable in the given state s if pre(a) ⊆ s. by s′ = apply(a, s) we denote the state after executing the action a in the state s, where a is applicable in s. all the assignments in s′ are the same as in s except for the assignments in eff(a) which replace the corresponding (same variable) assignments in s. if p = [a1 . . . ak] is a sequence of actions, then apply(p, s) = apply(ak, apply(ak−1 . . . apply(a2, apply(a1, s)) . . . )). a sequential plan p of length k for a given planning task π is a sequence of k actions p such that sg ⊆ apply(p, si). 2.3. parallel plans a parallel plan p with makespan k for a given planning task π is a sequence of sets of actions (called parallel steps) p = [a1, . . . , ak] such that e(a1)⊕· · ·⊕e(ak) is a sequential plan for π, where e is an ordering function, which transforms a set of actions ai into a sequence of actions e(ai) and ⊕ denotes the concatenation of sequences. let us denote by sj the world state in between the parallel steps aj and aj+1, which is obtained by applying the sequence e(aj) on sj−1, i.e., sj = apply(e(aj), sj−1) (except for s0 = si). in this paper we will use the ∀-step parallel planning semantics [10], which requires that each action a ∈ aj is applicable in the state sj , the effects of all actions are applied in sj+1 and all possible orderings e of the sets aj make valid sequential plans (hence the name ∀-step semantics). to ensure, that each ordering of the sets of actions in a parallel plan leads to a valid sequential plan, it is sufficient to check that the actions in each set are pairwise independent [3]. we say that two actions a1 and a2 are independent if they do not share common variables, i.e., scope(a1) ∩ scope(a2) = ∅, where scope(a) ⊆ x is a set of all state variables that appear in pre(a) and eff(a). note, that the pairwise independence of actions is a sufficient but not a necessary condition for the parallel steps in a ∀-step semantics plan, as the following example demonstrates. example 1. let a1 and a2 be two actions such that pre(a1) = pre(a2) = {x = 1}, eff(a1) = {y = 2}, and eff(a2) = {z = 2}. clearly, a1 and a2 are not sp1 planningassat (π) sp2 k := 0 sp3 repeat sp4 k := k + 1 sp5 f := encodetaskwithmakespan(π, k) sp6 until issatisfiable(f ) sp7 p := extractplan(getsatassignment(f )) sp8 return p figure 1. pseudo-code of the basic planning as satisfiability algorithm. independent (they share the variable x), however, they can be ordered arbitrarily to achieve the same changes between two given states. the pairwise independence of actions in each step of a parallel plan also implies that they can be executed in parallel (at the same time). 3. finding plans using sat the basic idea of solving planning as sat is the following [1]. we construct (by encoding the planning task) a series of sat formulas f1, f2, . . . such that fi is satisfiable if there is a parallel plan of makespan ≤ i. then we solve them one by one starting from f1 until we reach the first satisfiable formula fk. from the satisfying assignment of fk we can extract a plan of makespan k. the pseudo-code of this algorithm is presented in figure 1 the method was first introduced by kautz and selman [1] and is still very popular and competitive. this is partly due to the power of sat solvers, which are getting more efficient year by year. since then many new improvements have been made to the method, such as new compact and efficient encodings [2–5], better ways of scheduling the sat solvers [3] or modifying the sat solver’s heuristics to be more suitable for solving planning problems [6]. clever ways of solver scheduling [3] can significantly improve the performance of the planning algorithm at the cost of possibly longer-makespan plans. nevertheless, we will use the basic one-by-one scheduling since we are interested only in comparing the properties of encodings, i.e., the construction of the formulas. in the following section we will describe how a formula encoding a planning task can be constructed using our new reinforced encoding. 4. reinforced encoding our goal is (given a planning task π = {x,o, si , sg} and an integer k) to construct a cnf formula fk such that fk is satisfiable only if there is a parallel plan of at most k steps for π. we also want to construct fk in a way, that in the case it is satisfiable, we can easily extract a plan from its satisfying assignment. before we describe the formula, we need to introduce the notion of transitions [2]. 2 vol. 2/2015 reinforced encoding for planning as sat a transition represents a change of a state variable x ∈ x from one value to another from its domain dom(x) or from an arbitrary value to a specific value. there are the following three kinds of transitions. • an active transition changes the value of the variable x from d to e such that d 6= e, {d, e} ⊆ dom(x), it is denoted by δx: d→e. an action a has an active transition δx: d→e if (x = d) ∈ pre(a) and (x = e) ∈ eff(a). • a prevailing transition conserves the value of the variable x (if it was d, then it remains d, d ∈ dom(x)), it is denoted by δx: d→d. an action a has a prevailing transition δx: d→d if (x = d) ∈ pre(a) and there is no assignment related to x in eff(a). • a mechanical transition changes the value of the variable x from any value to the value d (d ∈ dom(x)), it is denoted by δx: ∗→d. an action a has a mechanical transition δx: ∗→d if (x = d) ∈ eff(a) and there is no assignment related to x in pre(a). example 2. the action a with preconditions pre(a) = {x = 1, y = 3} and effects eff(a) = {y = 1, z = 2} has one active transition (δy: 3→1), one prevailing transition (δx: 1→1), and one mechanical transition (δz: ∗→2). the transition set of an action a is the set of all transitions that a has, it is denoted by ∆a. by ∆p we will mean the set of all possible prevailing transitions of a planning task, i.e., ∆p = {δx: d→d | x ∈ x, d ∈ dom(x)}. the set of all transitions ∆ is the union of all the prevailing transitions and the transition sets of all the actions ∆ = ∆p ∪ {∆a | a ∈ o}. by ∆x ⊆ ∆ where x ∈ x we will denote the set of all transitions related to the variable x. the constructed formula fk will have the following three kinds of boolean variables. • action variables ati indicating whether the i-th action is used in the t-th step. we will have one such variable for each action from the description of the planning task and for each of the k parallel steps. • assignment variables btx=v indicating whether the value of the variable x is equal to v in the end of the t-th step (after applying the actions of the t-th step). we will have one such boolean variable for each state variable x ∈ x and each value v ∈ dom(x) for each of the k parallel steps. • transition variables ctδ (or ctx: d→e where δ = δx: d→e) indicating whether the transition δ occurred during the t-th step. we will have one such variable for each δ ∈ ∆ for each of the k parallel steps. now we are ready to define the clauses contained in fk. the following set of binary clauses will enforce, that at most one value is assigned to each state variable x ∈ x. (¬btx=vi ∨ ¬btx=vj ) ∀x ∈ x, vi 6= vj , {vi, vj} ⊆ dom(x), ∀t ∈ {1, . . . , k} (1) the following three kinds of clauses connect the assignment variables with the transition variables. the first set of clauses ensures that each transition δx: d→e (including prevailing transitions δx: e→e and mechanical transitions δx: ∗→e) implies that x = e at the end of each step. (¬ctδx: d→e ∨ btx=e) ∀δx: d→e ∈ ∆,∀t ∈ {1, . . . , k} (2) similarly, we need to add clauses for each transition δx: d→e (except for mechanical transitions) to enforce that x = d holds at the end of the previous step, except for the first step, where we explicitly disable all the transitions that are not compatible with the initial state (using the clauses from equation 8). (¬ctδx: d→e ∨ bt−1 x=d) ∀δx: d→e ∈ ∆, d 6= ∗,∀t ∈ {2, . . . , k} (3) the third kind of clauses is needed to guarantee, that if a variable x has the value v then there is a transition which changes the value of x to v. (¬btx=v ∨ ctδ1 ∨ · · · ∨ ctδm ) ∀x ∈ x, v ∈ dom(x),δ1, . . . , δm transform x to v, ∀t ∈ {1, . . . , k} (4) next we describe the clauses that connect the action variables with the transition variables. if an action a is selected, then all the transitions in its transition set ∆a must be selected as well. this implication is expressed via the following clauses. (¬at ∨ ctδ) ∀a ∈ o,∀δ ∈ ∆a,∀t ∈ {1, . . . , k} (5) also we need to make sure, that transitions (except for prevailing transitions) cannot happen without actions that have them in their transition sets. the following set of clauses will ensure this. (¬ctδ ∨ ats1 ∨ · · · ∨ atsm ) ∀δ ∈ (∆ \∆p), support(δ) = {s1, . . . , sm}, ∀t ∈ {1, . . . , k} (6) by support(δ) we mean the set of indices of actions that have δ in their transition set, i.e., support(δ) = {i | ai ∈ o; δ ∈ ∆ai }. next we need to deal with the interfering actions inside a parallel step. as discussed earlier, it is sufficient to ensure, that only pair-wise independent actions are together in each parallel step. we will achieve this by disabling all pairs of non-independent (interfering) actions. to extrude interfering actions from the parallel 3 t. balyo, r. barták, o. trunda acta polytechnica ctu proceedings steps we will add binary clauses for all the interfering action pairs. (¬ati ∨ ¬atj) ∀ai, aj ∈ o, ai, aj not independent, ∀t ∈ {1, . . . , k} there might be a plenty of interfering action pairs producing a lot of clauses. but if we look carefully at the clauses we have already described, we can see, that most of the interfering actions cannot occur together anyway as we will show via the following notion of compatible actions. two sets of conditions (assignments) are compatible if they assign the same values to the variables they share. two actions a1 and a2 are compatible if the preconditions of a1 are compatible with the preconditions of a2 and also the effects of a1 are compatible with the effects of a2. due to the clauses that enforce, that actions imply their transitions (5) and their connection to assignment variables (2 and 3) together with the clauses that forbid a state variable to have more than one value 1, actions that are not compatible cannot be in a parallel step together. therefore it is enough to suppress compatible interfering action pairs. (¬ati ∨ ¬atj) ∀ai, aj ∈ o, ai, aj compatible and not independent, ∀t ∈ {1, . . . , k} (7) lastly, we add the clauses that enforce the initial state to hold in the beginning and the goal conditions to be satisfied in the end. as for the initial state, we will disable all the transitions that are not compatible with the initial state, i.e., if a variable x has the value d in the initial state, then all the transitions that change x from a value other than d are disabled by using a unit clause. note, that mechanical transitions are always compatible with the initial state (or any other state) and therefore no mechanical transition is disabled. (¬c1 δx: d→e ) ∀δx: d→e ∈ ∆, (x = d) /∈ si (8) to encode the goal conditions we will use unit clauses with assignment variables. fore each goal condition (x = v) ∈ sg we will have a unit clause (bkx=v) which forces the value of x to be v after the last parallel step. (bkx=v) ∀(x = v) ∈ sg (9) the formula fk for the reinforced encoding is a conjunction of the clauses defined in equations 1, 2, 3, 4, 5, 6, 7, 8, and 9. a ∀-step parallel plan can be extracted from any satisfying assignment of fk in the following way. let φ be a satisfying assignment of fk. pφ is a sequence of action sets such that its t-th set contains those actions ai ∈ o for which φ(ati) = true. 4.1. correctness in this subsection the prove the correctness of our encoding, i.e., the following proposition. proposition 1. if the formula fk obtained using the reinforced encoding of the planning task π is satisfied by a truth assignment φ then pφ is a valid ∀-step parallel plan of makespan k for the planning task π. proof. the requirements for the action sets given by the ∀-step semantics are clearly satisfied: • the preconditions of actions in each parallel step are satisfied due to 2, 3, and 5 • the effects are propagated also due to 2, 3, and 5 • the actions can be ordered arbitrarily thanks to 7 it remains to prove that psφ = [e(a1)⊕· · ·⊕e(ak)] is a valid (sequential) plan for π, where ⊕ denotes the concatenation of sequences and e is an arbitrary ordering of an action set. let us observe, that the transitions of the state variables are consistent at each step, i.e., exactly one transition is allowed for each state variable (due to 2, 3, and 1) and a non-prevailing transition cannot happen without an action that has it (thanks to 6). prevailing transitions do not have to be supported by any actions since they are used to preserve the values of the variables that are not changed in the given step by any actions. furthermore, all the transitions between two neighboring parallel steps must be compatible due to 2, 3, 4 and 1. note, that it may happen, that a variable x has no value assigned in the end of a step t (all the btx=v, v ∈ dom(x) are false) and no transition related to the variable is selected (all the ctδ, δ ∈ ∆x are false). however, this can only occur for variables that are not used in the goal conditions or by actions that appear in the t-th step or later. since the action variables imply the proper transition variables thanks to 5, the actions must be applicable if their action variable is true and also the transition connected to the action must happen. thanks to 8 only transitions compatible with the initial state can happen in the first step and because of 2 and 9 only transitions that change the variables to their goal values are allowed in the last step. this fact together with the consistency of the transitions during all the k steps implies the validity of psφ for the planning task π. the reversed implication, which is that if pφ is a valid ∀-step parallel plan of makespan k, then φ satisfies fk, does not hold. this is because pφ may contain a non-independent pair of actions in one of its steps and still be a valid ∀-step plan (see example 1). such a pair of actions would make one of the clauses of type 7 unsatisfied. 4 vol. 2/2015 reinforced encoding for planning as sat 4.2. size of the encoded formula the size of the formulas will of course depend on the parameters of the planning task being encoded. we will use the following quantitative properties of a planning task π = (x,o, si , sg) to compute the upper bounds. • n the number of actions (n = |o|). • v the number of state variables (v = |x|). • d the maximum domain size of any state variable (d = maxx∈x{|dom(x)|}). • p the maximum number of preconditions or effects an action has (p = maxa∈o{|pre(a)|, | eff(a)|}) typically, the number of actions is much higher than the other parameters. from these values we can compute the following upper bounds related to the planning task. • the number of assignments is at most vd. • the number of transitions is at most v(d2 +d) since there are at most d(d− 1) active, d prevailing, and d mechanical transitions for each variable. from these bounds it is apparent, that fk (a formula for makespan k) has at most kn action variables, kvd assignment variables, and kv(d2 + d) transition variables. therefore the total number of boolean variables in fk is k(n+ vd(d+ 2)). now let us compute an upper bound on the number of clauses in fk. we will count separately the number of unit clauses (clauses with one literal), binary clauses (clauses with two literals), and horn clauses (clauses with at most one positive literal). the formula fk obtained by the reinforced encoding is the conjunction of the clauses defined in equations 1, 2, 3, 4, 5, 6, 7, 8, and 9 • there are at most kvd2 clauses of the type 1 – one for each step and variable and two different values from its domain. these clauses are binary and horn. • there are at most kv(d2 + d) clauses of the both type 2 and type 3 – one for each step and transition. these clauses are binary and horn. • there are at most kvd clauses of the type 4 – one for each step and assignment. • there are at most 2knp clauses of the type 5 – one for each step, action and each of its transitions (there are at most 2p transitions connected to each action). these clauses are binary and horn. • there are at most kv(d2 + d) clauses of the type 6 – one for each step and transition. • there are at most kn2 clauses of the type 7 – one for each step, and each pair of compatible interfering actions (at most each pair of actions). these clauses are binary and horn. • there are at most v(d2 + d) clauses of type 8 – one for each transition that is not compatible with the initial state (at most all the transitions). these are unit clauses. • there are at most v clauses of the type 9 – one for each goal condition. these clauses are unit. in total we have k(n2 +2np+4vd2 +4vd)+vd2 +vd+v clauses, from which vd2 + vd+ v are unit clauses and k(n2 + 2np+ 3vd2 + 2vd) are both binary and horn clauses. 5. experimental evaluation to evaluate the performance of our new reinforced encoding, we compared it with three other sas+ based encodings of planning as sat. we ran experiments with a 30 minutes time limit using the following four encodings. • reinforced encoding (reinf). a java implementation of our new reinforced encoding as described in the previous section. • direct encoding (dir). we implemented a simple encoding based on the historically first encoding of planning as sat [1]. we adapted it for the sas+ formalism. this encoding is similar to our reinforced encoding but uses only action and assignment variables. • sase encoding (sase). our java implementation1 of the transition-based sase encoding [2]. this encoding uses only action and transition variables. • r2∃-step encoding (r2∃). the original java implementation of the r2∃-step encoding [5]. this encoding differs from the previous three encoding significantly since it uses a different parallel planning semantics. the r2∃-step encoding allows more actions inside the parallel steps, therefore it often finds plans with much lower makespans. lower makespan indicates that fewer sat solver calls are required to find a plan, however, it does not say anything about its length, i.e., the total number of actions it contains. 5.1. experimental setting to compare the performance of the encodings we created a simple script, which iteratively constructed and solved the formulas for time steps 1, 2, . . . until a satisfiable formula was reached (see figure 1). for each encoding we used the same sat solver – lingeling[11] (version ats). the time limit was 30 minutes for the sat solving part, i.e., the total time the sat solver could spend solving the formulas f1, f2, . . . for each problem instance was 30 minutes. the time required for the generation of f1, f2, . . . is usually negligible compared to the time required to solve them and therefore we will ignore it. hence the overall planning time could exceed the given time limit for a problem instance. 1the original sase implementation cannot be used since it does not support the format of the latest benchmark problems 5 t. balyo, r. barták, o. trunda acta polytechnica ctu proceedings domain dir sase reinf r2∃ barman 4 4 4 8 elevators 20 20 20 20 floortile 16 11 18 18 nomystery 20 10 20 6 openstacks 0 0 0 15 parcprinter 20 20 20 20 parking 0 0 0 0 pegsol 10 6 10 19 scanalyzer 14 12 15 9 sokoban 2 2 2 2 tidybot 2 2 2 2 transport 16 17 18 13 visitall 12 9 10 20 woodworking 20 20 20 20 total 156 133 159 172 table 1. the number of problems (out of 20) in each domain that the encodings solved within the time limit (30 minutes for sat solving). the experiments were run on a computer with intel i7 920 cpu @ 2.67 ghz processor and 6 gb of memory. the benchmark problems of the ipc are organized into domains. each domain contains 20 problems and there are 14 domains which results in a total of 280 problems. the benchmark problems are provided in the pddl format, however, the encodings require input in the sas+ format. we used helmert’s translation tool, which is a part of the fast downward planning system [12], to obtain the sas+ files from the pddl files. the translation is very fast requiring only a few seconds for all domains. 5.2. experimental results the number of solved instances in presented in table 1. looking at the results from the perspective of the domains, we can observe, that the elevators, parcprinter, and woodworking domains are entirely solved by every encoding. on the other hand, the parking domain is so difficult that not even a single problem is solved by any of the encodings. the openstacks domain is very difficult for all but the r2∃-step encoding. the sokoban and tidybot domains are also very hard for all of the encodings, only two of the twenty problems are solved by each encoding. if we compare the encodings, we can observe that the r2∃-step encoding has the highest total number of solved instances followed by our new reinforced encoding. as for the individual domains, the r2∃-step encoding solves strictly more problems than the other encodings in four cases. the reinforced encoding achieves this for three domains, while the direct and sase encoding cannot outperform the other encoddomain dir sase reinf r2∃ barman 121 121 121 84 elevators 190 190 190 85 floortile 302 181 344 169 nomystery 347 119 347 30 openstacks 93 parcprinter 261 261 261 30 parking pegsol 222 131 222 158 scanalyzer 83 61 95 17 sokoban 60 60 60 27 tidybot 14 15 15 6 transport 221 242 262 55 visitall 223 110 146 34 woodworking 68 68 68 33 table 2. the sum of makespans of the plans found within the time limit for each domain. lower makespan means fewer sat solver calls, it does not indicate better plan quality. domains with the same number of solved problems for each encoding are highlighted. ings in any of the domains. the reinforced encoding solves the same number of problems as any other encoding in seven cases. except for the visitall domain, the reinforced encoding is never worse than the direct or sase encoding. looking at the makespans of found plans displayed in table 2 we can observe that the makespans for the r2∃-step plans are indeed significantly lower than the makespans of plans found by the other three encodings. as expected, in the cases when the direct, sase, and reinforced encodings solve all the problems (or solve the same problems) their total makespans are identical. this is due to the fact that these three encodings use the same ∀-step parallel planning semantics. the times required to solve the problems are presented in table 3. if we look at the results for the domains, where each encoding solved the same number of problems, i.e., the highlighted domains, we can notice, that except for the parcprinter and sokoban problems, the runtime of the r2∃-step encoding is much higher than the runtime of the other methods. if we also look at table 2, which contains the total makespan of the found plans, we can deduce, that lower makespan, i.e., fewer sat calls does not necessarily mean faster planning, especially not in the case of the easy domains. nevertheless, for the domains, where r2∃-step significantly outperformed the other methods – openstacks, pegsol, and visitall, the makespans are much lower than the makespans of the other methods, despite the fact, that they solved fewer problems. 6 vol. 2/2015 reinforced encoding for planning as sat domain dir sase reinf r2∃ barman 2041.44 1549.31 1680.53 2999.30 elevators 33.96 55.72 38.10 288.29 floortile 7327.15 2083.57 1206.18 1380.63 nomystery 3798.45 1377.23 1894.65 1927.40 openstacks 2679.68 parcprinter 10.07 28.25 12.15 4.24 parking pegsol 3796.11 2096.72 4971.97 830.72 scanalyzer 1401.21 831.80 1435.19 1118.89 sokoban 592.03 1337.87 857.04 550.18 tidybot 75.68 74.02 118.09 480.85 transport 1404.23 3554.90 3203.62 7418.01 visitall 2380.76 683.25 726.53 14.24 woodworking 2.57 2.04 3.84 138.61 table 3. the time in seconds required to solve all the problems that were solved within the time limit. the presented time is the sum of times the sat solver alone required, formula generation time is not included. domains with the same number of solved problems for each encoding are highlighted. 6. conclusion in this paper we have introduced a new encoding of a planning problem represented in the sas+ formalism into sat. our new encoding performs well on the benchmark problems of the 2011 international planning competition. it can strictly outperform all the other evaluated sas+ encodings in three domains and solve the same number of problems as any other encoding for seven domains out of fourteen. on the remaining four domains our encoding is outperformed by the r2∃-step encoding which uses a different parallel planning semantics. as for future work, we believe that the reinforced encoding can be improved by decreasing the number of its clauses by using a more compact way of encoding of the action interference constraints. acknowledgements the research is supported by the czech science foundation under the contract p103/10/1287 and by the grant agency of 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[12] m. helmert. the fast downward planning system. journal of artificial intelligence research (jair) 26:191–246, 2006. doi:10.1613/jair.1705. 7 http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.35.9443 http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.35.9443 http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.182.9561 http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.182.9561 http://dx.doi.org/10.1016/j.artint.2006.08.002 http://aaai.org/ocs/index.php/icaps/icaps09/paper/view/732 http://aaai.org/ocs/index.php/icaps/icaps09/paper/view/732 http://dx.doi.org/10.1109/ictai.2013.131 http://dx.doi.org/10.1016/j.artint.2012.08.001 http://dx.doi.org/10.1016/j.artint.2015.01.004 http://dx.doi.org/10.1111/j.1467-8640.1995.tb00052.x http://dx.doi.org/10.1016/0004-3702(71)90010-5 http://dx.doi.org/10.1016/s0004-3702(96)00047-1 http://fmv.jku.at/lingeling/ http://dx.doi.org/10.1613/jair.1705 acta polytechnica ctu proceedings 2:1–7, 2015 1 introduction 2 preliminaries 2.1 satisfiability 2.2 planning 2.3 parallel plans 3 finding plans using sat 4 reinforced encoding 4.1 correctness 4.2 size of the encoded formula 5 experimental evaluation 5.1 experimental setting 5.2 experimental results 6 conclusion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2016.5.0051 acta polytechnica ctu proceedings 5:51–58, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app criticallity of transportation infrastructure in czech republic jan procházka∗, dana procházková czech technical university in prague, faculty of transportation sciences, praha, czech republic ∗ corresponding author: prochazka@fd.cvut.cz abstract. the paper deals with transportation infrastructure criticality because this quantity determines the state capability to overcome the critical conditions and to ensure the inhabitants survival. the criticality rates for individual types of transportation infrastructure and for the entire transportation infrastructure are determined by data from experts from the areas: transportation; transportation management in the territory; supply chains; public administration; and the integrated rescue system. the experts assessed 14 factors, which have been often used in the developed world countries, from the view of human security and development. the result values and their interpretations were determined by using the multiatribute utility theory. keywords: transportation infrastructure, system of systems, interdependences, criticality, interoperability, serviceability, human survival, state stability. 1. introduction transportation infrastructure belongs to the basic systems that make up the critical infrastructure in the european union, in developed countries and also in the czech republic. we understand the system of transportation in accordance with the current knowledge as a system of systems, i.e. the set of several overlapping systems. the most important property in such type of system is the interoperability of partial systems that depends on interdependences [1]. the interdependences are the cause of different emergent phenomena and cascade failures that cause that the transportation infrastructure does not fulfil its function, i.e. the serviceability of territory at normal, abnormal and critical conditions if it is threatened the human survival and state stability. therefore, it is necessary to manage the transportation infrastructure by the way so infrastructure criticality is acceptable [1]. the subject of this work is to assess the criticality of the transportation infrastructure in the czech republic on the basis of the integral safety concept, which aims are security and development of the territory concerned and its inhabitants. the concept used is based on the knowledge of the reality of the dynamic development of the human system and it considers that human system conditions are normal, abnormal and critical. the capability to overcome the critical conditions, ensuring the survival of humans and to have capability to stabilize the situation we consider crucial, and therefore, we use the degrees of criticality, which are aimed at assessing the aspects associated with the given properties. for the assessment of the criticality we use criteria used in developed countries, multi-objective approach and data from experts whose qualification is certified according to the criteria used in the european union [1]. 2. current knowledge on transportation infrastructure the transportation system, which provides transportation of humans and goods, includes all modes of transportation, which, under the coordination of individual transportation systems work together and create a logistical network [2]. transportation logistics network is currently becoming a very important area of business activities, and not just in a regional and national scale, but also in international relations. the transportation network can be combined with energy as one of the foundations of the economic prosperity of states and organizations. transportation systems for their activities require a considerable amount of funds, namely in investment, operational and administrative domains, which typically create autonomous sub-sectors, the activity of which is mutually coordinated. the characteristic feature of those technological units is their capability to own separate activity, and therefore, they are often considered as closed units, which is projected to the safety concept, and at risk management it is used the simplest approach, i.e. the procedures for a closed system, in which the sources of the risk are only the technical problems and the human factor [2]. infrastructure of transportation network is currently mostly owned by the public sector; however, its development is largely determined by the requirements of private sector. simultaneously it constitutes an important element of the economy and of the citizens living way. transportation network has considerable international political influence, as it allows the international cooperation of individual states and tourism, which contributes to the integration of citizens. the transportation system is built from the separate parts that make up certain units that provide certain 51 http://dx.doi.org/10.14311/app.2016.5.0051 http://ojs.cvut.cz/ojs/index.php/app jan procházka, dana procházková acta polytechnica ctu proceedings circuit activities separately. in the serviceability of territory (creating the space for human lives, i.e. the human system), however, the units are together overlapped, i.e. they create a system of systems [2] [3] [4]. the ground of each unit is a specific type of transportation vehicles, accompanied by complex of operational and administrative procedures. the characteristic feature of these technological units is their specialized capability to separate operation, i.e. the autonomy. the capability to separate operation, however, it is only apparent, the sub units are bound by the rules of their transport logistics, which not only coordinates their activities, but also makes it economically more profitable because it reduces operating costs. on the other hand, however, it is the source of internal dependencies "interdependences" [2] [5]. safety of transportation networks in the past was provided only by a simple guarding. the guarding was mostly limited to surveillance, which should prevent the mostly property-related offences, such e.g. theft of the goods transported, pertinently endangering the personal safety of transported passengers. on the basis of current knowledge, it is the aim of the safety management of the transportation system, which consists of objects and infrastructures, ensuring the security and development of both, the transportation system and transportation system vicinity, because it is the only way how to ensure the safe human system. on the basis of current knowledge, this means that we have to apply the tools of the disciplines that provide safety management of complex systems [1] [2] [5]; i.e. the multi criterial approach based on expert assessment of the possible variants that describe the behaviour of systems of systems designated by different behaviour of individual subsystems [4]. 3. transportation system of the czech republic in the czech republic a transportation network is in essence created from the following areas: railway transport system; road transport system; air transport; and water transport. the main activities of the business in the transport are passenger and freight transport. ensuring the rational operation requires considerable resources – labour, capital, information, as in a modern industrialized society, it is common that the interconnection and operation of transportation networks and the provision of transport services is an important part of near all other activities. for example, the provision of transport services in the major cities is done by public transportation, which is based on mostly coordinated cooperation of road and rail transport, sometimes supplemented by underground transportation; it is basically so called integrated transportation system. in the last few decades, the transportation infrastructure has become a major target of terrorist attacks. in particular, it clearly reflected in the air transport, in which they terrorists originally focused only on the kidnappings, and the destruction of the aircraft in flight [5]. after the attacks of 11 september, 2001 on the trade centre in new york, it turned out that the aircraft may change in the gun with the devastating consequences of the disastrous. from historical practice it is known that natural disasters (in our condition floods, storms, earthquakes and landslides) often caused considerable and practically difficult to quantify damages to parts of the rail and road transport of technological system and the environment. therefore, it can be concluded that transportation systems are particularly vulnerable to attacks and natural disasters. they are very favourite target of the activities of terrorists who by attack on any of transportation systems can cause considerable damage to property and infrastructure devices. it is necessary to recognize that the indirect impacts of attacks and their consequences can even endanger the stability of the economics of the industry, or even the state. from the above analysis it follows that it is necessary to devote to the issue of the destruction of the infrastructure of transportation systems special attention, to define particularly sensitive parts and to search for ways how to reduce the danger of the destruction of important parts, which can cause the interruption of the activity of transportation systems, and by such way to prevent the economic destabilization not only of the relevant business units, but also to other bodies in the industrial areas. if we want to manage the transportation system safety with the aim of ensuring its security and development, so we need to know the priority aspects, on which the achievement of objectives depend and on that we need to focus the attention, i.e. the measures and activities [1] [5]. from the same source it follows that the critical spots in the technological system (object, the infrastructure, plant, facility, territory) are the places where the basic technological processes are under way and for which there are in force specific provisions for the safety under normal, abnormal and critical conditions (e.g. single-level crossing of the railways and roads in the village). table 1 gives the important parts of the transportation system, separated for four of its parts according to criteria of governmental decree no. 2000 col. [6]. 4. method for determining the transportation infrastructure criticality according to the detailed discussion given in [1] [5] the criticality of item means that item has simultaneouslygreat importance and great vulnerability. it means that we work with conflict criteria at the solution of problem. therefore, we use the strategy defined by the keeny and raiffa [7] defined by the mathematical statement "the higher, the worse, i.e. the higher criticality in our case". as it has been already said above, the transportation system as a whole and its basic subsystems are 52 vol. 5/2016 criticallity of transportation infrastructure in czech republic rail transport road transport air transport water transport linear constructions tracked rail network, the electrification network of railways, railway security network the full road network the system of interconnected airports the waterways objects the railway station buildings for traffic management, expedition of passengers and redeployment of goods, the depots of vehicles, railway workrooms, railway bridges, railway tunnels, track divisionmaintenance rail network objects and networks for security techniques, railway workrooms for servicing the locomotives of all kinds and fleet, the power stations of power supply to rail network, fuel stations road bridges, road tunnels, stocks of fuels for road transport purposes, objects for the management of road traffic, gas fuel stations for road vehicles, objects for the management of emergency situations in road network airport runways for takeoff and landing, a network of runways, lighting, passing ways, aircraft stands, buildings for service stations for air transport, buildings for normal preflight preparationinput and general examination, air traffic control objectsairport, regional, the radar station for air traffic control, radar stations for meteorology, computing centre of the airport, the equipment for operational information sharing for regional service, facilities for the sharing of operational information for the management of the activities of the airport, centre for intervention in emergency traffic incidents (accidents...), gas stations and fuel warehouse ports with the devices, the locks, docks, hydrometeorology stations, objects for maintenance of vessels, fuel stations fittings rail vehicleslocomotives and cars, equipment of the rail stations and the tracked rail network, device for controlling the places on the crossing the road and rail transport, the equipment for operational information sharing within the operation of the rail system, facilities for the supply of fuel for vehicles the equipment for operational information sharing with the road network, equipment of centres with technique for solving incidents, buses, freight cars, personal cars aircrafts ships table 1. important parts of transport system 53 jan procházka, dana procházková acta polytechnica ctu proceedings systems of systems, i.e. it goes on several mutually penetrating systems of different nature (technical, organizational, financial, human resources, and legal), and therefore, the criticality assessment cannot be performed from a single indicator, but it is necessary to use a multicriterial approach and information from experts [4]. in accordance with the procedures that are used in the usa, australia, canada etc. [8] [9] [10] [11] [12] [13] there were used the following factors important to the criticality of transportation infrastructure: • a rate of capability of defence, • a rate of vulnerability to attack, • a rate of threat to the health and lives of humans, • a rate of accidents impact on the environment • a rate of cost of exchange or repair, • a rate of exchange time or repair time, • a rate of importance for ensuring the life-saving or emergency functions in the territory, • a rate of importance for ensuring the functions of administration and local government, • a rate of importance for ensuring the functions of army and police, • a rate of redundancy or replacement services, • a rate of importance for ensuring the communication functions, • a rate of impact of frontage failure on the economy of region (state), • a rate of importance of operability, • a rate of importance in the field of symbolic, cultural, etc. with the facts in the documentation of the czech republic transportation system [14] and with the data from 5 experts, selected according to the criteria of the eu given in [1], from the areas: transportation; transportation management in the territory; supply chains; public administration; and the integrated rescue system, there wereobtained verbal assessments of the factors mentioned above. since the main human objective is the human safety and the human development [3], for which the safe transportation infrastructure is vital, the criticality of the transportation infrastructure is understood from the perspective targeted on the human survival. therefore, the verbal assessment was transferred with the help of five experts participating in the panel discussion into the numerical scale that is analogue to the scale using in the risk assessment in the čsn standards [1] – allocate number of points is the following: (1.) if factor does not contribute to the criticality of the transport system (the expected damages are less than 5%), (2.) if factor contributes little to the criticality of the transport system (damages are expected at an interval of 5-25%), (3.) if factor contributes intermediately to the criticality of the transport system (the expected damages are in the interval 25-45%), (4.) if factor contributes significantly to the criticality of the transport system (the expected damages are in the interval of 45-70%), (5.) if factor contributes very significantly to the criticality of the transport system (the expected damages are in the interval of 70-95%), (6.) if factor significantly contributes most significantly to the criticality of the transport system (the expected damage is greater than 95%). the resulting evaluation of criticality for each partial system provided that we give equal weight to all factors, can have the values 0 to 70 and for the entire system having 4 subsystems, provided that their equivalence the criticality values are between 0 and 280. if we again apply approach used in the čsn standards [1], we get the data given in table 2. 5. results – the criticality rates for transport infrastructure the verbal assessments of factors for rail transport, obtained from the experts are the following: (1.) rate of capability of defence – defence of the railway is difficult due to the considerable complexity of rail system. at the attack of terrorists on main parts or at natural disaster there may originate extensive damages that stop the operation of a large part of the system. the human factor and organizational accident can also cause considerable damages. (2.) rate of vulnerability to attack – vulnerability of the railway is significant because some parts of it can be quite simply destroyed extensively (railway stations complexes, bridges, tunnels, etc.). (3.) rate of threat to the health and lives of humans – the health and lives of passengers are threatened by practically in all the accidents of the rail system. (4.) rate of impact of railway accidents on the environment – railway accidents can have significant impacts on the environment, in particular in the transport of fuels, chemicals and other raw materials. removal of contamination of environment is the most difficult and expensive. (5.) rate of cost of exchange or repair – elimination of damages caused by the destruction of the track system can be mostly done without the big cost. expensive there are large constructions repairs of faulty bridges and tunnels. repair or restoration of the destroyed railway vehicles is often expensive. 54 vol. 5/2016 criticallity of transportation infrastructure in czech republic criticality rate score the percentage of the total value individual transport systems entire transport system the extremely high more than 95% more than 66.5 more than 266 very high 70 95% 49 66.5 196 266 high 45 70% 31.5 49 126 196 medium 25 45% 17.5 31.5 70 126 very small 5 25% 3.5 17.5 14 70 insignificant / negligible less than 5% less than 3.5 less than 14 table 2. value scale used for determining the criticality rate (6.) rate of exchange time or repair time – repair of tracks is quite fast. large construction repairs of bridges and tunnels require a longer period of time. (7.) rate of importance for ensuring the life-saving or emergency functions in the territory – in emergency situations the railway is very important and often essential for the provision of emergency activities. (8.) rate of importance for ensuring the functions of administration and local government – for the provision of administrative and self-government the railway is important, but its services for the activities in most cases can be replaced by other means of transport. (9.) rate of importance for ensuring the functions of army and police – to the needs of the army and the police the railroad is necessary. (10.) rate of redundancy or replacement services – backup at the railway is quite high (multiple lines), particularly in the transport of basic industrial raw materials, food, and fuel in larger quantities. very important it is container shipping service linking the various transport systems and container transport requires its own technology. in particular, the important role has container transport in international traffic, which of course, requires the construction of investment-intensive terminals, which can be a sensitive target for terrorists. (11.) rate of importance for ensuring the communication functions – in emergency case, the communication network of railway can be used because it is independent. (12.) rate of impact of frontage failure on the economy of region (state) – disturbed rail traffic system adversely affects the smooth running of the regional or national economy and causes considerable economic losses. (13.) rate of importance of operability – railway operability is very important on both, the national and the international scales. (14.) rate of importance in the field of symbolic, cultural, etc. – .-the level and status of the railway transport system is testimony to the cultural and technical level of the state. the verbal assessments of factors for road transport, obtained from the experts are the following: (1.) rate of capability of defence – protection of the road network is complex because even if the disruption of the custom paths can be quite easily and quickly repair, sensitive parts such as bridges and tunnels it is necessary against terrorist attacks and natural disasters especially consistently to protect, because their damage or destruction often requires a long-term repair, mostly investment-intensive. the human factor and organizational accident can also cause considerable damages. (2.) rate of vulnerability to attack – vulnerability of road network is particularly determined by sensitive parts of system, such as bridges, tunnels, etc. (3.) rate of threat to the health and lives of humans health and lives are threatened by accidents during the operation, the number of which can be in the effective management of road traffic minimised. (4.) rate of impact of road accidents on the environment road transport heavily polluting environment by gases that vehicles emit into the atmosphere. when accidents of vehicles, environmental pollution is caused in particular by spilling fuel and possibly also by transported goods that is spread in nature. (5.) rate of cost of exchange or repair – except the costly repairs of sensitive network places – bridges tunnels etc. it is possible to perform repairs of damages of road network fairly cheaply and in a short time. (6.) rate of exchange time or repair time – outside the repairs of bridges, tunnels and other expensive parts it is possible to perform the repairs of network in a relatively short time. (7.) rate of importance for ensuring the life-saving or emergency functions in the territory – the serviceability of roads is very important, in the case of an emergency it can be solved by the finding a replacement path that avoids the damaged parts. (8.) rate of importance for ensuring the functions of administration and local government – road transport is very necessary. 55 jan procházka, dana procházková acta polytechnica ctu proceedings (9.) rate of importance for ensuring the functions of army and police – road transport is fundamentally necessary. (10.) rate of redundancy or replacement services – there are, in principle, to allow mutual logistic redundancy compensation of individual transport systems. (11.) rate of importance for ensuring the communication functions – communication function can be partially replaced by road transport. (12.) rate of impact of frontage failure on the economy of region (state) – the status and level of road system quality has a significant influence on the economy. (13.) rate of importance of operability – operability of the road system is very important and fundamentally affects all activities in the region and state. (14.) rate of importance in the field of symbolic, cultural, etc. – the level of road transport and the road system is indicative of the level of the state and its tradition. the verbal assessments of factors for air transport, obtained from the experts are the following: (1.) rate of capability of defence – defence of air transport is very exacting and difficult, because the air transport system is currently the most complex of all transport systems. the accidents in aviation occur from reasons, the technical reasons and the meteorological reasons. however, the air transport is also a hot target for terrorists. the human factor and organizational accident can also cause considerable damages. (2.) rate of vulnerability to attack – the vulnerability is high. preparation of the aircraft for operation is very challenging. therefore, the flight and technical staff is carefully selected and trained. defence against terrorist attacks is performed while the intensely, but not always successfully. (3.) rate of threat to the health and lives of humans – in air accidents it is occurred injury and death of crew and passengers. therefore, the prevention of accidents in the aviation service is very important. (4.) rate of impact of road accidents on the environment – air accidents are almost always accompanied by considerable local damage to the environment, but mostly they are hitting a small part of the territory. (5.) rate of cost of exchange or repair – replacement of the damaged aircraft technique is almost always very costly financially and time often challenging. repairs require a considerable supply of spare parts and the repair work of specialists. the repair needs to be carried out at the manufacturers or authorised service companies. (6.) rate of exchange time or repair time – the time length of the repair is different according to the nature of the fault. (7.) rate of importance for ensuring the life – saving or emergency functions in the territory – aviation equipment has a significant position and it is almost necessary in response to real crisis situations of all kinds. (8.) rate of importance for ensuring the functions of administration and local government – it is important only conditionally. (9.) rate of importance for ensuring the functions of army and police – it is very necessary. (10.) rate of redundancy or replacement services – air transport has a conditional redundancy that from its independence on surface networks enables to solve specific tasks. (11.) rate of importance for ensuring the communication functions – in some exceptional cases, air transport is the only viable solution. (12.) rate of impact of frontage failure on the economy of region (state) – air transport is of great importance for the economy, because outside of its own air traffic it is driving article of industry. (13.) rate of importance of operability – it is very important. (14.) rate of importance in the field of symbolic, cultural, etc. – air transport in the czech republic has a significant position in the world. the aviation industry of the czech republic has a long tradition, the products have been exported into all world. the verbal assessments of factors for water transport, obtained from the experts are the following: (1.) rate of capability of defence – with regard to the limited scope of the network of waterways in the czech republic this transport system can be probably successfully protected. the human factor and organizational accident can also cause damages. (2.) rate of vulnerability to attack – the vulnerability of the network of waterways, in particular, determines the sensitive parts – locks, weirs, etc., that ensure the navigability of the waterways. (3.) rate of threat to the health and lives of humans – the health and lives of the residents and workers in the transport sector are threatened to the extent that is usual in other sectors of industry. (4.) rate of impact of road accidents on the environment – in particular the pollution of waterways by fuels, which adversely affects the environment and the biosphere in the water and on the banks of streams. (5.) rate of cost of exchange or repair – ship accident are not common, there is not usually a large extent of the damages. 56 vol. 5/2016 criticallity of transportation infrastructure in czech republic factor rail transport road transport air transport water transport entire transport 1 5 4 5 2 16 2 5 4 5 3 17 3 4 3 4 3 14 4 4 3 3 2 12 5 4 3 5 2 14 6 3 2 4 3 12 7 5 5 4 1 15 8 3 3 2 2 10 9 5 5 5 2 17 10 3 2 3 1 9 11 3 2 3 1 9 12 5 4 4 4 17 13 4 4 4 2 14 14 3 2 3 2 10 all factors 56 46 54 30 186 table 3. rates of criticality of the transportation infrastructure in the czech republic (6.) rate of exchange time or repair time – the ship drives are mostly repairs in the port, where the repair can be done in a short time. repair of damage to the ship’s body can usually only be performed in the dock, which prolongs the time of repair. (7.) rate of importance for ensuring the life-saving or emergency functions in the territory – it is needed only for the rescue work of a certain character. (8.) rate of importance for ensuring the functions of administration and local government – small. (9.) rate of importance for ensuring the functions of army and police – it is significant only in special cases. (10.) rate of redundancy or replacement services – water transport can be replaced by the rail or road transport. (11.) rate of importance for ensuring the communication functions – small. (12.) rate of impact of frontage failure on the economy of region (state) – water transport by its low expenses positively affects the transport of raw materials and objects of large dimensions. (13.) rate of importance of operability – smaller, only to a limited extent. (14.) rate of importance in the field of symbolic, cultural, etc. – water transport has probably the longest tradition and by this reason it is one of the symbols of the country. the criticality rates determined by the methodological procedure described above are in table 3. table 3 shows that the greatest criticality has rail transport, which is followed by air transport, road transport and water transport. according to the chosen concept, the chosen scale and evaluation provided by the experts the criticality rates of both, the rail transport and the air transport are very high, the criticality rate of road traffic is high and the criticality rate of water transport is medium, and the criticality rate of whole transport system is high. from table 3 it is clear that to the size of criticality rate mostly contributes the vulnerability to attacks, little capability of protection (the protection of long linear networks in the territory is always a big problem), the importance for ensuring the functions of the army and the police, a big impact of transport failure on the economy of region (state), and the big importance for ensuring the emergency and rescue functions in the territory. 6. proposals for transport infrastructure safety improve from the above analysis of transportation systems criticality it follows that the transport domain is one of the most important areas of economic and social item in the state. to its high criticality it contributes that in recent decades this fact was discovered by population groups in different states, which are not satisfied with the current state establishment in the home countries, they create their own political ideology, which most strongly criticizes the current political establishment of the state in which they live and they try to their views and goals in life violently to enforce by illegal way and as onerous procedure for the enforcement of their ideology, they consider terrorism. terrorism currently has a global form, so its international character leads to the need for protection against attacks. in the reference case, the facts: the great importance of transport systems, the high vulnerability of transport systems, and also the fact that part of the transportation systems can be used as an offensive weapon with great destructive potential, as shown by the attacks of 11 september 2001 in new york. it is, therefore, necessary to develop countermeasures for reducing the eventuality of attack on transportation systems and to avert the devastating impacts on the functioning the state and on the lives of citizens. in conjunction with the results of the project the focus of the european union [15], it is necessary to consider that not only terrorism, but also a natural disasters, organizational accidents and corruption associated with the areas of control often to cause the extensive damages on the transportation systems. preparation and production of protective measures requires substantial investment, and therefore, it is necessary to coordinate investment and to combine possible measures for protection of transportation systems against possible damages caused by disasters [16] and terrorist activities, as required by the principles of strategic management [3]. 57 jan procházka, dana procházková acta polytechnica ctu proceedings due to the fact that neither terrorism nor natural disasters cannot be averted, the main goal of our activities are mitigating measures at occurrence of disasters in order to reduce the losses of human lives and minimize damages [1] [3]. because of the importance of transportation systems is considerable, it is very urgently to implement the measures and activities that will allow the critical infrastructure elements of transportation systems effectively protect against the activities of international terrorism and other disasters. it is necessary to carry out measures that reduce the vulnerability, ensure a rapid response to the failure of critical elements, and ensure the continuity of critical elements, and on the quick recovery of the other important elements. it is necessary to: • to estimate the vulnerability of functional elements of transportation system in the context of the assessment of transportation system objects such as bridges, tunnels, roads, highways, airports and waterways, • to provide for the most vulnerable part of the infrastructures, the failure of which can cause the most economic damages in infrastructure up to make impossible the transport activity, • to create scenarios of the impacts of major disasters and possible attacks, and on the basis of scenarios of impacts to determine the rapid-response procedures and the procedures for ensuring the transportation services as much as possible, • to improve measures and activities in the areas of planning, with the aim of improving the protection against possible disasters and terrorist attacks on the transportation system, and not only from the point of view of individual systems, but in the logistics context to link measures and to increase the safety of the entire system taken in as a system of systems, • to provide for measures that reduce the option of attack on transportation infrastructures and improve the detection of attacks on transportation infrastructure, • to estimate the amount of investment and labour costs, which will require the implementation of mitigation measures in case of failure of transportation infrastructures and to propose a procedure for their application, • to perform the analysis and to design the transportation infrastructure network protection against damages, which may arise as a result of possible disasters and to perform the estimation of operational inability origin as a result of their putting out of operation of functional elements or their parts, • to reduce the frequency of interruptions of transportation systems operation as a result of a failure that cannot be reliably in advance revealed during the regular inspections. 7. conclusions the above facts show that it is urgent to pay increased attention to safety issues of transportation systems. it needs to be processed as a separate concept of transportation system safety, so the concept of critical infrastructure safety, as it shows the work [17]. from the professional point of view, it is necessary to include into safety issues solution a systemic approach, which enables us to support the technological development of transportation systems, to consider the needs of people and transportation serviceability, the environmental protection and to reduce economic damages. it is necessary to define by the expert way the issues that are necessary to solve, and to process the relevant studies in the meaning of the above recommended procedure. references [1] d. procházková. základy řízení bezpečnosti kritické infrastruktury, 2013. isbn 978-80-01-05245-7. [2] d. procházková. bezpečnost kritické infrastruktury, 2012. isbn 978-80-01-05103-0. [3] d. procházková. strategické řízení bezpečnosti území a organizace, 2011. isbn 978-80-01-04844-3. [4] d. procházková. analýza a řízení rizik, 2011. isbn 978-80-01-04841-2. [5] d. procházková. safety of complex technological facilities, 2015. isbn 978-3-659-74632-1, id: 200303845. [6] czech republic, czech code. [7] r. l. keeny, h. raiffa. decision analysis with multiple conflicting objectives, 1976. [8] ema. critical infrastructure emergency risk management and assurance [online], 2003. www.ema.gov.au. [9] fema. promoting critical infrastructure protection by emergency managers and first responders [online], 2005. www.usfa.fema.gov. [10] saic. a guide to highway vulnerability assessment for critical asset identification and protection, 2002. national cooperative highway research program project 20-07/task 151b. [11] s. (sandia national laboratories). vital area identification, 2005. albuquerque. [12] us. the national strategy for the physical protection of critical infrastructures and key assets, 2000. [13] us. guide for critical infrastructure protection, 2005. [14] ministerstvo dopravy čr [online]. http://www.mdcr.cz. [15] eu. focus project [online], 2012. http://www.focusproject.eu/documents/14976/ -5d763378-1198-4dc9-86ffc46959712f8a. [16] fema. guide for all-hazard emergency operations planning, 1996. [17] us. us critical infrastructure conception, 2001. 58 www.ema.gov.au www.usfa.fema.gov http://www.mdcr.cz http://www.focusproject.eu /documents /14976/-5d763378-1198-4dc9-86ffc46959712f8a http://www.focusproject.eu /documents /14976/-5d763378-1198-4dc9-86ffc46959712f8a acta polytechnica ctu proceedings 5:51–58, 2016 1 introduction 2 current knowledge on transportation infrastructure 3 transportation system of the czech republic 4 method for determining the transportation infrastructure criticality 5 results – the criticality rates for transport infrastructure 6 proposals for transport infrastructure safety improve 7 conclusions references 199 acta polytechnica ctu proceedings 2(1): 199–204, 2015 199 doi: 10.14311/app.2015.02.0199 a new review of old novae a. pagnotta1 1american museum of natural history corresponding author: pagnotta@amnh.org abstract novae are certainly very exciting at the time of their eruptions, and there is much work left to be done in understanding all of the details of that part of their existence, but there is also much to be learned by looking at the systems decades, centuries, and even millennia after their peak. i give a brief overview of some of the history and motivation behind studying old novae and long-term nova evolution, and then focus on the state of the field today. exciting new results are finally starting to shed some light on the secular behavior of post-nova systems, although as is often the case in astronomy, the observations are at times conflicting. as is always the case, we need more observations and better theoretical frameworks to truly understand the situation. keywords: novae dwarf novae cataclysmic variables photometry. 1 introduction novae have been observed at least as far back as 134 b.c. (fontanille 2007), and we continue to observe them and their kin—recurrent novae (rne), dwarf novae (dne), and the rest of the cataclysmic variables (cvs)—to this day. just after discovery, near peak, and for the few weeks following peak, they are quite exciting and tend to receive a good amount of observational coverage from both amateur and professional astronomers. a month or two after peak, however, the number of observations decreases sharply, due to various reasons including limited telescope time and short attention spans among astronomers who understandably want to move on to the next exciting object. because of this, the long-term, secular behavior of novae is poorly understood. in this conference review, i examine what little we know about novae in the decades, centuries, and millennia following their eruptions and describe efforts to remedy this lack of knowledge and understand how novae fit into the broader context of cv evolution in particular and binary evolution in general. 2 the first decades a classical nova (cn) occurs in a cv when enough accreted gas accumulates on the surface of the white dwarf (wd) that a critical temperature/pressure is reached and a thermonuclear runaway is ignited, causing a dramatic brightening of the system, which we see as a nova. immediately after a nova eruption, two effects compete to affect the brightness of the system. these effects were quantified into the hibernation model originally proposed by shara et al. (1986) to explain the low observed space-density of novae. although more recent surveys seem to show that the low numbers of observed novae at the time may have been due to observational limitations and biases, (e.g. gänsicke et al. 2009), the physical effects described by the hibernation model remain valid and should be investigated. there are two potent effects we must consider. first, the mass ejection during the nova eruption leads to an increase in the angular separation between the accreting wd and its companion star. this leads to a decrease in the accretion rate and therefore the brightness of the star, since the observed brightness is due predominantly to the accretion luminosity. the second effect is that the thermonuclear runaway on the surface of the wd greatly increases its temperature; the hot wd then irradiates the companion star. the companion in turn puffs up, overflows its roche lobe more than it was previously doing, and the accretion rate increases, causing the system to get brighter. so the two main observable consequences following a nova eruption act in opposite directions and potentially cancel each other out. the question is which effect dominates, and why. collazzi et al. (2009) and schaefer & collazzi (2010) obtained the preand post-eruption magnitudes of a sample of 25 classical and 6 recurrent novae using a combination of published literature magnitudes, archival plates, and amateur observations. defining ∆m as the average difference between the preand post-eruption magnitude values for a given system, mpre − mpost, they found ∆mavg = +0.16 mag and 199 http://dx.doi.org/10.14311/app.2015.02.0199 a. pagnotta ∆mmed = +0.13 mag, with σ = 0.42 mag for the 25 cne with their 25 observed eruptions. adding in the 6 rne, for a total of 44 eruptions, they found ∆mavg = +0.03 mag and ∆mmed = +0.03 mag, with σ = 0.43 mag. both results are consistent with ∆m = 0, implying that the increase and decrease in the accretion rate after an eruption do in fact cancel each other out in most systems. a textbook example of this is qz aurigae, nova aurigae 1964, the preand post-eruption light curve of which can be seen in figure 1. qz aur has a ∆mavg ≈ 0.03 mag, essentially equal to zero. figure 1: qz aurigae, nova aurigae 1964, is a textbook example of the findings of collazzi et al. (2009), who showed that for nearly all novae, the preand posteruption magnitudes are identical, and that on average ∆m = mpre −mpost across all nova eruptions is consistent with 0. figure reproduced with permission from collazzi et al. (2009). there are of course a few systems that do not follow the trend. christened the v1500 cyg stars by schaefer & collazzi (2010) after their prototype system, these stars show large positive ∆m values years-to-decades after their eruptions have ended, i.e. they return to a quiescence that is brighter than their pre-eruption quiescence value. there are eight systems that fall in this category, with ∆m values ranging from 3.01 to > 4.96. the underlying physical mechanism causing this phenomenon is not well understood but it has been postulated that all of the systems are magnetic, either polars or intermediate polars. the magnetic field funnels the accreting material onto a small portion of the wd surface, leading to sustained nuclear burning, which irradiates the companion for a much longer time period than after a normal nova eruption and again causes an increase in the accretion rate and correspondingly the brightness of the system. this theory addresses the basics of the observations, but needs more thorough computational work to confirm its validity. neeley & schaefer (private communication) examined seven old novae that had a large number of magnitudes in the literature covering the decades since their eruptions. taking all seven together, they found an average decline of 1.4 mags per century, in line with the hibernation model, which predicts an average decline of 1 mag per century. johnson et al. (2013) examined one of the systems, v603 aquilae (nova aquilae 1918) in much greater detail and found an overall decline in brightness of 0.44 ± 0.04 mags per century since 1938, again as expected from the hibernation model. the light curve for v603 aql showing this decline can be seen in figure 2. this average behavior, however, hides the unusual behavior of a few systems among the more vanilla ones, including novae that appear to have undergone state changes, as well as at least one system (q cygni) that is getting brighter on a secular timescale (schaefer, private communication). figure 2: this yearly binned light curve for v603 aquilae (nova aquilae 1918) clearly shows a secular fading in both b− and v -band, as predicted by the hibernation model. the calculated decline rate for v603 aql is 0.44± 0.04 mags per century. figure reproduced with permission from johnson et al. 2013. the variety of behaviors seen when looking at even just a small number of systems indicates that a full survey is necessary to understand what is actually happening to post-nova cvs. i am embarking on a project to examine a much larger sample of post-nova systems in an attempt to obtain complete statistics on what novae do in the decades and centuries following their eruptions. i am working to combine historical magnitudes from archival plates and the published literature with a modern magnitude survey of all galactic novae. the bulk of the plate magnitudes will come from the collection of the harvard college observatory, which has ∼500,000 plates dating back to the 1890s and ranging from b=14 to b=18 in limiting magnitude. although at this point, much of the work done using the harvard plates must be completed by hand, the observatory has 200 a new review of old novae embarked on a scanning project known as dasch (digital access to a sky century at harvard) led by josh grindlay. eventually, the entire plate collection will be scanned and available digitally, which should provide an efficient way to study the long-term behavior of many systems, including novae. figure 3: this finder chart for v906 ophiuchi (nova ophiuchi 1952) from the online version of the catalog and atlas of cataclysmic variables (downes et al. 2001), showing the location of the nova eruption. there are at least three stars equally near the middle of the identifying circle, any of which could be the quiescent counterpart of the nova, or the actual counterpart could be a fainter star that is not easily detected in this relatively shallow image. there are many nova systems with finder charts as (un)clear as this one, which necessitates photometric and spectroscopic follow-up to identify the proper counterpart before any information can be obtained about its secular brightness history. one big challenge in this endeavor is identifying the quiescent counterpart of the nova eruption. although the eruptions are bright and, after detection, easy to identify, once the systems have faded, it becomes much more difficult. the positions and finder charts given for novae are often unclear, with multiple stars, or none at all, visible at the marked location, an example of which can be seen in figure 3, which shows the v906 ophiuchi finder chart given in the online version of the downes et al. (2001) catalog and atlas of cataclysmic variables. deep, multi-color images of the fields are required first, to identify blue stars which are more likely to be cvs. if in fact hibernation is correct and most novae spend their decades post-eruption fading in brightness, the practice of identifying the counterparts is more challenging, because they are fainter than they were before the eruption, and will continue to fade. when imaging is not enough to identify post-eruption nova counterparts, spectroscopy is required as well. the team of tappert, schmidtobreick, ederoclite, and vogt is currently in the middle of a dedicated effort to identify the counterparts of old novae using a combination of photometry and spectroscopy. tappert, schmidtobreick, and ederoclite also have papers in this proceedings, so i will leave the details of their work to them. figure 4: the expected cycle of a cv both pre-and post-nova eruption according to the hibernation model. before and after the nova, the system would be classified as a nova-like cv, with a high accretion rate but no known eruptions. as the accretion rate falls off post-eruption, the system transitions through a series of other types of cvs, from nova to nova-like to dwarfnova (perhaps multiple types of dwarf novae), before eventually settling into a state of hibernation in which the accretion essentially goes to zero. after a long period of time during which only gravitational radiation is actively moving the stars close together again, the companion once again overflows its roche lobe, accretion restarts at a low level, and the system moves up the left side of the figure, returning to dwarf nova and then nova-like states before likely undergoing another classical nova eruption tens of thousands of years after the first. 3 the centuries to millennia following eruption in addition to the long-term fading of a post-nova system, another prediction of the hibernation model is that a system should undergo state changes, passing through various other types of cvs on its way into and out of hibernation (shara et al. 1986). it is expected to be a cycle such as that depicted in figure 4, in which a 201 a. pagnotta system changes state as the accretion rate changes. immediately post-eruption, the system should appear as a nova-like variable, eventually transitioning to a dwarf nova, and then finally going into hibernation proper when the accretion essentially stops. after a time period that could be on the order of thousands of years, gravitational radiation will grind down the system, return it to contact, and restart the accretion, propelling the system back through the cycle from dwarf nova to nova-like and eventually back to another nova eruption. this is another testable prediction of the hibernation theory. figure 5: three images of the classical nova shell surrounding the dwarf nova z camelopardalis; from left to right they are in far-uv (1516 å) and near-uv (2267 å) from galex and in [nii] from the kpno 4m telescope. shell expansion has not yet been detected, but an upper limit of 0.17” per year, corresponding to a velocity no greater than 138 km s−1 has been placed on the expansion of the shell by shara et al. 2012b. the nova eruption of z cam is quite possibly associated with a guest star recorded by chinese astronomers in 77 b.c. (johansson 2007). figure reproduced with permission from shara et al. 2012b. at this time, we have regular post-eruption observations of novae going only approximately one century past their eruptions, for old novae with good coverage on the harvard plates. there are two systems in which both classical and dwarf nova eruptions have been observed. gk persei (nova persei 1901) was the first system in which this behavior was observed, when dwarf nova eruptions began approximately 50 years after the cn eruption. the second system is v1017 sagittarii, which was considered to be recurrent for many years, but upon closer examination it was realized that v1017 sgr had a dn eruption first, in 1901, followed by a cn eruption in 1919, followed by future dn eruptions, starting back up again in 1973 (webbink et al. 1987). this state change occurs on a much faster timescale than predicted by the hibernation model. the century of data from harvard is an excellent resource, but is not, however, the limit of how far forward—or backward, depending on your perspective—we can look. thus far there are two systems currently known to be dwarf novae around which very old nova shells have been discovered. the first was z cam, originally discovered by shara et al. (2007), and followed up with better observations of the shell published in shara et al. 2012b; figure 5 shows three of those images, the nearand far-uv images from galex (1516 å and 2267 å, respectively), and the [nii] optical emission image taken at the kitt peak 4-m telescope. shell expansion has been undetectable thus far, with an upper limit of 0.17” per year, corresponding to an expansion velocity no greater than 138 km s−1. it is likely that the nova eruption that caused the shell was recorded as a guest star by chinese astronomers in 77 b.c. (johansson 2007). 1’ fuv nuv[nii] figure 6: three images of the classical nova shell surrounding the current dwarf nova at cancri; from left to right they are in [nii] from the kpno 4m telescope, far-uv (1516 å) and near-uv (2267 å) from galex. at cancri is the second dwarf nova, after z cam, which has had a classical nova shell detected around it. figure reproduced with permission from shara et al. 2012c. the second dwarf nova to have a shell is at cancri, shown in figure 6 in the same three bands as the z cam image. additionally, at cancri’s shell has knots, as seen more clearly in the hα + [nii] image in figure 7. the knots are likely caused by the same rayleigh-taylor instabilities that cause the knots in gk per (shara et al. 2012a) and t pyx (shara et al. 1997, schaefer et al. 2010, toraskar et al. 2013). most recently, patterson et al. (2013) have pointed to the star bk lyncis as a third system that has changed state. pre-2005, bk lyn appeared to be a normal nova-like star, with a wd accreting at a relatively high rate, but nothing else special about the system. starting in 2005, however, and very well defined by 2011 and 2012, bk lyn transitioned into being an er umatype dwarf nova. (for more details about bk lyn and the contributions of the excellent observers of the center for backyard astrophysics to this discovery, see joe patterson’s proceedings paper from this meeting.) bk lyn is possibly associated with a nova recorded in 101 a.d., and therefore it took approximately 2000 years for it to make its transition, as opposed to just a few decades for gk per and v1017 sgr. this is loosely theorized to be due to the large difference in the orbital periods of the systems, with bk lyn being quite short (107.97 minutes; patterson et al. 2013) and gk 202 a new review of old novae per and v1017 sgr having long orbital periods (1.997 days and 5.780 days, respectively; pagnotta & schaefer 2013), but the effect is still not well understood and needs a more solid theoretical grounding. figure 7: this hα + [nii] image of the classical nova shell around at cancri clearly shows the knots present. the knots are likely caused by rayleigh-taylor instabilities and are similar to those seen in gk per (shara et al. 2012a) and t pyx (shara et al. 1997, schaefer et al. 2010, toraskar et al. 2013) figure reproduced with permission from shara et al. 2012c 4 conclusion with even just a small sample of post-eruption novae for which the long-term behavior has been studied, we see a wide variety of behaviors. some novae fade, as predicted by the hibernation model; others brighten, in direct opposition to the theory. some appear to stay at the same magnitude for many decades following their eruption; perhaps they will continue in this fashion, or perhaps a change will set in many years later. a number of systems have been seen to change states, from novae to dwarf novae, on time scales varying from approximately 50 years to approximately 2000 years. taken all together, the lesson from this review is that the longterm behavior of post-eruption novae is poorly understood, and most certainly in need of more study, both observationally and theoretically. references [1] collazzi, a. c., schaefer, b. e., xiao, l., pagnotta, a., kroll, p., löchel, k., & henden, a. a.: 2009, aj, 138, 1846 [2] downes, r. a., webbink, r. f. shara, m. m., ritter, h, kolb, u., & duerbeck, h. w.: 2001, pasp, 113, 764 doi:10.1086/320802 [3] fontanille, j.-p.: 2007, jrasc, 101, 11 [4] gänsicke, b. t., et al.: 2009, mnras, 397, 2170 doi:10.1111/j.1365-2966.2009.15126.x [5] johansson, g. h. i.: 2007, nature, 448, 251 doi:10.1038/448251d [6] johnson, c. b., schaefer, b. e., kroll, p., & henden, a.: 2014, apjlett, 780, 25 doi:10.1088/0004-637x/780/1/25 [7] pagnotta, a., & schaefer, b. e.: 2014, apj, 788, 164 doi:10.1088/0004-637x/788/2/164 [8] patterson, j., et al.: 2013, mnras, 434, 1902 doi:10.1093/mnras/stt1085 [9] schaefer, b. e. & collazzi, a. c.: 2010, aj, 139, 1831 [10] schaefer, b. e., pagnotta, a., & shara, m. m.: 2010, apj, 708, 381 doi:10.1088/0004-637x/708/1/381 [11] shara, m. m., livio, m., moffat, a. f. j., & orio, m.: 1986, apj, 311, 163 doi:10.1086/164762 [12] shara, m. m., zurek, d. r., williams, r. e., prialnik, d., gilmozzi, r., & moffat, a. f. j.: 1997, aj, 114, 258 [13] shara, m. m., et al.: 2007, nature, 7132, 159 [14] shara, m. m., et al.: 2012a, aj, 143, 143 [15] shara, m. m., et al.: 2012b, apj, 756, 107 [16] shara, m. m., et al.: 2012c, apj, 758, 121 [17] toraskar, j., mac low, m.-m., shara, m. m., zurek, d. r.: 2013, apj, 768, 48 [18] webbink, r. f., livio, m., truran, j. w., & orio, m.: 1987, apj, 314, 653 discussion ed sion: q cyg may not be so odd. we found that nova oph 1848 (v841 oph) and di lac (nova lac 1910) are also accreting at a high rate and probably getting brighter. ashley pagnotta: very interesting, and a great example of why we need a large-scale survey of novae to see what’s normal and what’s not. thank you for pointing out those two systems. jan-uwe ness: very encouraging results from historical plates. in addition to the harvard plates, smaller historical observatories such as hamburg may 203 http://dx.doi.org/10.1086/320802 http://dx.doi.org/10.1111/j.1365-2966.2009.15126.x http://dx.doi.org/10.1038/448251d http://dx.doi.org/10.1088/0004-637x/780/1/25 http://dx.doi.org/10.1088/0004-637x/788/2/164 http://dx.doi.org/10.1093/mnras/stt1085 http://dx.doi.org/10.1088/0004-637x/708/1/381 http://dx.doi.org/10.1086/164762 a. pagnotta have scanned plates that could fill more gaps. marina orio and rene hudec made similar comments about smaller observatories including asiago and bamburg. rene hudec also commented on his presentlyactive project to document what exists in current plate archives and help facilities get their collections scanned into a digitally-accessible form. 204 introduction the first decades the centuries to millennia following eruption conclusion 108 acta polytechnica ctu proceedings 1(1): 108–112, 2014 108 doi: 10.14311/app.2014.01.0108 mass accretion processes in young stellar objects: role of intense flaring activity salvatore orlando1, fabio reale2,1, giovanni peres2,1, andrea mignone3 1inaf osservatorio astronomico di palermo, piazza del parlamento 1, 90134, palermo, italy 2dip. di fisica e chimica, università degli studi di palermo, piazza del parlamento, 1, 90134, palermo, italy 3dip. di fisica generale, università degli studi di torino, via pietro giuria 1, 10125, torino, italy corresponding author: orlando@astropa.inaf.it abstract according to the magnetospheric accretion scenario, young low-mass stars are surrounded by circumstellar disks which they interact with through accretion of mass. the accretion builds up the star to its final mass and is also believed to power the mass outflows, which may in turn have a significant role in removing the excess angular momentum from the star-disk system. although the process of mass accretion is a critical aspect of star formation, some of its mechanisms are still to be fully understood. on the other hand, strong flaring activity is a common feature of young stellar objects (ysos). in the sun, such events give rise to perturbations of the interplanetary medium. similar but more energetic phenomena occur in ysos and may influence the circumstellar environment. in fact, a recent study has shown that an intense flaring activity close to the disk may strongly perturb the stability of circumstellar disks, thus inducing mass accretion episodes (orlando et al. 2011). here we review the main results obtained in the field and the future perspectives. keywords: accretion, accretion disks mhd stars: circumstellar matter stars: flare stars: pre-main-sequence x-rays: stars. 1 introduction observations in the x-ray band reveal that low-mass pre-main-sequence stars are strong sources with x-ray luminosities 3−4 orders of magnitude greater than that of the present-day sun. the source of this high-energy radiation is plasma with temperatures of 1 − 100 mk in the stellar outer atmospheres (coronae), heated by magnetic activity analogous to the solar one but higher by factors up to 106. such a magnetic activity manifests through very different phenomena that may occur in several places of the stellar atmosphere and circumstellar environment. the young star interacts with its disk in a complex fashion, with accretion and ejection of collimated outflows. strong magnetic fields are believed to connect the star with a keplerian circumstellar disk, funneling accretion onto limited portions of the stellar surface (e.g. hartmann 1998) where shocks are produced by the impact of the accretion streams (e.g. orlando et al. 2010). x-ray flares are violent manifestations of the stellar magnetic activity and are triggered by an impulsive energy input from coronal magnetic fields. x-ray observations in the last decades have shown that flares in young stellar objects (ysos) have amplitudes much larger than solar analogues and occur much more frequently. examples of these flares are those collected by the chandra satellite in the orion star-formation region (coup enterprise; favata et al. 2005). in the sun, such energetic events are often associated to coronal mass ejections and give rise to perturbation effects of the interplanetary medium, broadly known as space weather effects. similar phenomena are expected to occur in young stars, and may affect the circumstellar environment. for instance, favata et al. (2005) analyzed the most energetic flares observed by coup and found that these flares might be hosted in magnetic loops extending several stellar radii, much larger than ever observed in older stars. since the central star is surrounded by a circumstellar disk accreting material onto the star, it is natural to ask whether strong flaring activity involves the disk and even perturbs its stability, possibly affecting the mass accretion to the star. at the present time, in fact, it is unclear where these flares occur. the differential rotation of the disk together with the interaction of the disk with the magnetosphere may cause magnetic reconnection close to the disk’s surface, triggering large-scale flares there. in this case, the flares may perturb the stability of the circumstellar disk causing, in particular, a strong local overpressure. the pressure gradient force might be able to 108 http://dx.doi.org/10.14311/app.2014.01.0108 mass accretion processes in young stellar objects: role of intense flaring activity push disk’s matter out of the equatorial plane into funnel streams, thus providing a mechanism to drive mass accretion that differs from that, commonly invoked in the literature, based on the disk viscosity (romanova et al. 2002). bright flares close to circumstellar disks may therefore have important implications for a number of issues such as the transfer of angular momentum and mass between the star and the disk, the powering of outflows, and the ionization of circumstellar disks. recently, we have investigated the idea that an intense flare close to an accretion disk may perturb the stability of the disk and trigger mass accretion onto the star (orlando et al. 2011). in this paper we review our findings and present preliminary results of a study investigating the effects of a storm of small-to-medium flares on the stability of accretion disks (orlando et al. 2014). in sect. 2 we describe the mhd model; in sect. 3 we present the results; in sect. 4 we draw our conclusions. 2 the mhd model the model describes a classical t tauri star (ctts) of mass m∗ = 0.8m� and radius r∗ = 2r� located at the origin of a 3d spherical coordinate system (see orlando et al. 2011 for a detailed description). we adopted the initial conditions introduced by romanova et al. (2002). in particular, we assumed the rotation period of the star to be 9.2 days as representative of cttss. the initial unperturbed stellar atmosphere is approximately in equilibrium and consists of three components: the stellar magnetosphere, the extended stellar corona, and the keplerian disk. initially, the magnetosphere is assumed to be force-free, with dipole topology and magnetic moment aligned with the rotation axis of the star. the magnetic moment is chosen in order to have a magnetic field strength of the order of 1 kg at the stellar surface. the isothermal disk is cold, dense and rotates with angular velocity close to the keplerian value; its rotation axis (coincident with the rotation axis of the star) is aligned with the magnetic moment. the disk is initially truncated by the stellar magnetosphere at the radius rd where the ram pressure of the disk is equal to the magnetic pressure; for the adopted parameters, rd = 2.86r∗ and the co-rotation radius is located at rco = 9.2r∗. the corona is initially isothermal with temperature t = 4 mk and at low density. the system is described by the time-dependent mhd equations of mass, momentum, and energy conservation in a 3d spherical coordinate system, extended with gravitational force, viscosity of the keplerian disk, thermal conduction (including the effects of heat flux saturation), coronal heating (via a phenomenological term), and radiative losses from optically thin plasma (see orlando et al. 2011 for more details). the phenomenological heating is prescribed as a component, describing the stationary coronal heating, plus a transient component, triggering the flares. the calculations were performed using pluto (mignone et al. 2007), a modular, godunov-type code for astrophysical plasmas. 3 results as a first application of the model, we have investigated the effects of a single bright flare on the stability of the disk (orlando et al. 2011). the initial heat pulse triggering the flare is released at a distance of 5r∗, namely in a region comprised between the truncation and corotation radii, and it is supposed to be indicative of a likely area of magnetic reconnection. heat pulses occurring closer to the inner disk edge are expected to produce analogous perturbations on the disk dynamics. we followed the evolution of the star-disk system for ≈ 2 days. after the heat pulse has been released, an mhd shock wave develops above the disk and propagates away from the protostar. the heat deposition determines a local increase of temperature and pressure. disk material is heated and expands with a strong evaporation front which is channeled along the magnetic field lines towards the central star. after ∼ 1 hour a hot loop forms linking the disk with the star (see upper panel in fig. 1). the loop has an effective maximum temperature of ≈ 100 mk (at the peak of emission measure) and a length of ≈ 1012 cm; these values are in good agreement with those inferred from the analysis of the brightest flares observed by coup (favata et al. 2005). the overheating of the disk surface makes a significant amount of material expand and be ejected in the magnetosphere. a small fraction of this material fills the loop whose density increases from 108 cm−3 to 1010 cm−3. on the other hand, most of the expanding disk material is not confined by the magnetic field and is ejected away from the star, carrying away mass and angular momentum. during the evolution of the hot loop, an overpressure wave develops where the heat pulse has been injected. this overpressure travels through the disk and reaches the opposite boundary after ≈ 5 hours. there the pressure gradient force drives the material out of the disk and channels it into a funnel flow. then the gravitational force accelerates the escaped material toward the central star where the stream impacts ≈ 25 hours after the injection of the heat pulse. the accretion flow persists until the end of the simulation (t = 48 h). the lower panel in fig. 1 shows a cutaway view of the stardisk system after the impact of the stream onto the stellar surface. we found that the dynamics and physical characteristics of the accretion stream triggered by the flare closely recall those of streams driven by the accumulation of mass at the disk truncation radius under 109 salvatore orlando et al. the effect of the viscosity and pushed out of the equatorial plane because of the growing pressure gradient there (e.g. romanova et al. 2002). figure 1: effects of a single bright flare on the stability of the circumstellar disk. cutaway views of the star-disk system showing the mass density of the disk (yellow-green) at t = 2.0 hours (upper panel) and at t = 45 hours (lower panel) since the injection of the heat pulse. the upper panel also over-plots the threedimensional volume rendering of the plasma temperature (mk), showing the flaring loop (in red) linking the inner part of the disk with the star. the lower panel shows the accretion stream triggered by the flare in the side of the disk opposite to the flaring loop. selected magnetic field lines are overplotted in red. from the simulation, we derived also the mass accretion rate and found ṁ > 2.5 × 10−10 m� yr−1. we compared this rate with those inferred from optical observations of cttss (herczeg & hillenbrand 2008; curran et al. 2011) and found a good agreement. we concluded that a bright flare as those frequently detected in ysos (e.g. coup observations) can be an efficient mechanism to trigger accretion onto the protostar itself with accretion rates on the same order of those commonly measured in cttss. as a follow-up of the previous study, we explored in more details the possibility that significant mass accretion in young stars can be triggered by a storm of small-to-medium flares (as those frequently observed) occurring on the accretion disk (orlando et al. 2014). to this end, we performed a 3d mhd simulation analogous to that described in orlando et al. (2011) but considering a storm of flares distributed randomly in proximity of the disk surface instead of a single bright flare. we found that each simulated flare follows an evolution similar to that of the single bright flare described in orlando et al. (2011). the main difference is that, now, interactions between next flares may occur. figure 2 shows cutaway views of the star-disk system after ≈ 26 hours. during the system evolution, the flares build up an extended corona linking the star with the disk. at the same time, the disk is strongly perturbed by the flares and, after ≈ 20 hours, several funnel streams develop, accreting substantial mass onto the star (see lower panel in fig. 2). the streams persist until the end of the simulation and last for a time longer than the typical interval between flares. the simulated mass accretion rate is 10−10 < ṁ < 10−9 m�yr−1, again in good agreement with the values inferred from optical observations of cttss (herczeg & hillenbrand 2008; curran et al. 2011). 4 conclusions we investigated the effects of an intense flaring activity on the stability of a circumstellar disk surrounding a magnetized ctts. to this end, we developed a 3d mhd model including, for the first time, all key physical processes, most notably the thermal conduction and the radiative losses from optically thin plasma. as a first step, we analyzed the perturbation induced by a single bright flare occurring in proximity of the disk (orlando et al. 2011). then, we investigated the effects of a storm of small-to-medium flares distributed randomly close to the disk (orlando et al. 2014). our findings lead to the following conclusions: (a) flares occurring close to the circumstellar disk can trigger substantial and persistent accretion flows, similar to those caused by the disk viscosity; (b) an intense flaring activity close to the disk builds up an extended corona linking the star to the disk. in the case of a single bright flare occurring close to the disk, the simulations suggest that mass accretion events associated with x-ray flares should be observed. however, correlation between uv/optical accretion tracers and x-ray flux is rarely seen (stassun et 110 mass accretion processes in young stellar objects: role of intense flaring activity al. 2006). on the other hand, such a correlation is not prediced by simulations describing a continuous flaring activity close to the disk (orlando et al. 2014). in this case, the streams are triggered by the first flares at the beginning of the simulation and then are continuously powered by the following ones. at regime, therefore, no clear correlation between uv/optical accretion tracers and x-ray flux is foreseen. in the light of the above findings, we suggest that the flaring activity common to ysos may turn out to be important in the exchange of angular momentum and mass between the circumstellar disk and the central protostar. figure 2: effects of a storm of flares on the disk stability. cutaway views of the star-disk system showing the mass density of the disk (blue) at t = 26 hours. the panels over-plot the three-dimensional volume rendering of the plasma temperature (in mk), showing the flaring loops (in red) linking the inner part of the disk with the star. the upper panel shows the star-disk system observed edge-on, whereas the lower panel shows the system observed pole-on. selected magnetic field lines are overplotted in the upper panel. acknowledgement we thank the referee for constructive and helpful criticism. pluto is developed at the turin astronomical observatory in collaboration with the department of general physics of the turin university. we acknowledge the cineca award n. hp10a4zcv5,2012 for the availability of high performance computing resources and support. references [1] curran, r.l., argiroffi, c., sacco, g.g., orlando, s., peres, g., reale, f., maggio, a.: 2011, a&a 526, a104 [2] favata, f., flaccomio, e., reale, f., micela, g., sciortino, s., shang, h., stassun, k.g., feigelson, e.d.: 2005, apjs 160, 469 doi:10.1086/432542 [3] hartmann l.: 1998, accretion processes in star formation. new york: cambridge university press; cambridge astrophysics series; 32 [4] herczeg, g.j., hillenbrand, l.a.: 2008, apj 681, 594 doi:10.1086/586728 [5] mignone, a., bodo, g., massaglia, s., matsakos, t., tesileanu, o., zanni, c., ferrari, a.: 2007, apjs 170, 228 doi:10.1086/513316 [6] orlando, s., sacco, g.g., argiroffi, c., reale, f., peres, g., maggio, a.: 2010, a&a 510, a71 [7] orlando, s., reale, f., peres, g., mignone, a.: 2011, mnras 415, 3380. [8] orlando, s., reale, f., peres, g., mignone, a.: 2014, in preparation [9] romanova, m.m., ustyugova, g.v., koldoba, a.v., lovelace, r.v.e.: 2002, apj 578, 420 doi:10.1086/342464 [10] stassun, k.g., van den berg, m., feigelson, e., flaccomio, e.: 2006, apj 649, 914 doi:10.1086/506422 discussion matteo guainazzi: what kind of x-ray variability does your model predict? is it observed in the coup sources? salvatore orlando: the x-ray variability depends on the rate of flares triggered. in the simulation with a single flare, we observe the fast rise and subsequent slow decay of x-ray emission characteristic of flares. in the simulation with a storm of flares, we observe a background emission due to the many small flares evolving simultaneousluy with superimposed local peaks due to the brightest flares. the x-ray variability found is consistent with that of ysos observed by coup. 111 http://dx.doi.org/10.1086/432542 http://dx.doi.org/10.1086/586728 http://dx.doi.org/10.1086/513316 http://dx.doi.org/10.1086/342464 http://dx.doi.org/10.1086/506422 salvatore orlando et al. david buckley: do you believe that your magnetospheric disk interaction models could be extrapolated to intermediate polar class of cvs, where accretion occurs from disrupted disc onto a magnetic white dwarf? salvatore orlando: our model can be extrapolated (with appropriate scaling) to systems in which mass accretion occurs from a circumstellar disk, if relativistic effects can be neglected. 112 introduction the mhd model results conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.12.0099 acta polytechnica ctu proceedings 12:99–103, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app artificial neural network for models of human operator martin růžek czech institute of informatics, robotics and cybernetics (ciirc), czech technical university in prague, zikova 4, 166 36 prague 6, czech republic correspondence: martin.ruzek@cvut.cz abstract. this paper presents a new approach to mental functions modeling with the use of artificial neural networks. the artificial neural networks seems to be a promising method for the modeling of a human operator because the architecture of the ann is directly inspired by the biological neuron. on the other hand, the classical paradigms of artificial neural networks are not suitable because they simplify too much the real processes in biological neural network. the search for a compromise between the complexity of biological neural network and the practical feasibility of the artificial network led to a new learning algorithm. this algorithm is based on the classical multilayered neural network; however, the learning rule is different. the neurons are updating their parameters in a way that is similar to real biological processes. the basic idea is that the neurons are competing for resources and the criterion to decide which neuron will survive is the usefulness of the neuron to the whole neural network. the neuron is not using "teacher" or any kind of superior system, the neuron receives only the information that is present in the biological system. the learning process can be seen as searching of some equilibrium point that is equal to a state with maximal importance of the neuron for the neural network. this position can change if the environment changes. the name of this type of learning, the homeostatic artificial neural network, originates from this idea, as it is similar to the process of homeostasis known in any living cell. the simulation results suggest that this type of learning can be useful also in other tasks of artificial learning and recognition. keywords: neural network, artificial neuron, learning algorithm, mental model. 1. introduction for many practical applications it would be useful to have a model of a human operator, as for example in transport engineering where the human operator plays a principal role. unfortunately, the human factor causes also most of the accidents; therefore it would be helpful to understand the processes in the human brain. due to the complex nature of the human brain it is however very difficult to model and predict its behavior. he need to dispose of the model of a human operator, as the most complex part of many transport systems, stays behind this research. the transport and traffic simulations are on high level, but the principal component of any transport system – the human factor – is still quite unexplored. the main obstacles are the lack of knowledge about the mental processes and the differences between the typical artificial intelligence approaches and the biological neural networks. the artificial neural networks (ann) seems to be a promising method for these models because the architecture of the ann is directly inspired by the biological neuron and also because it is data driven method. the classical paradigms of artificial neural networks are however not suitable for direct use because they simplify too much the real processes in biological neural network, but it is possible to update the learning algorithm so that it corresponds more frankly to the biological reality. the neural networks have already been used in several projects aimed at mental models. one of them is the blue brain project[1, 2] with the goal to simulate the whole brain. this model should be so detailed that every cell is depicted on a molecular level. according to the authors, processes like consciousness, creativity, emotions or aggression will emerge. another research aimed at the models of human mind is the darpa synapse project with opposite attitude. the idea behind this research is to create a neural network with architecture similar to biological neural network, however with strongly simplified neurons[3]. the expectation is not to model mental processes, but to use the principles of biological neural network to improve the computer architecture. the way of information processing in the computer architecture is different from biological networks. in brain, the memory and computation are distributed; there is no central processor or memory. the expectation of synapse project is to understand the advantages of this architecture and to use them in formation of novel computer architecture. with respect to both above mentioned researches, the target of this paper is to find such an equilibrium point where the model of the neuron is still faithful enough so that it can model the strong processes and 99 http://dx.doi.org/10.14311/app.2017.12.0099 http://ojs.cvut.cz/ojs/index.php/app martin růžek acta polytechnica ctu proceedings yet be simple enough to be practically realizable. 2. new solution – homeostatical neural network the need for a compromise between the complexity of biological neural network and the practical feasibility of the artificial network led to a proposal of new learning algorithm. the idea is based on the classical multilayered neural network (mlp), the difference is in the learning process. the neurons are updating their parameters in a way that is similar to the real biological processes. the basic idea is that the neurons are in competition for resources and the survival criterion is the usefulness of the neuron to the whole neural network. the neurons are not using any "teacher" or other kind of superior system, they have the same information as the biological neuron. the learning process can be seen as searching of some equilibrium position which represents a state where the importance of the neuron for the neural network is maximal. this position can change in time if the environment changes. the name of this type of learning, the homeostatic artificial neural network, is derived from the similarity of this idea to the process of homeostasis that is known from biology. the proposed neural network is based on the idea of mcculloch-pitts neuron: y = φf n∑ i=0 xiwi (1) where f is the transfer function. the sigmoid transfer function was used: f(x) = 2 (1 + e−α∗x)− 1 (2) as the similarity to biological neuron was the basic requirement, the back propagation algorithm is not a solution because a higher structure (or teacher) is used to train the neuron. in the so called homeostatic neuron, the unit is using its proper forward connection to improve its function. the ’axon’ in this model has two functions – the first one is the transmission of the output to higher layer (as in back propagation), the second is the transmission of the utility information from higher layer to the lower one. the idea of this type of training is that the neuron improves its relative importance in the network, in other words, it is trying to maximize the part of its output signal that is accepted by other neurons. this idea corresponds to the biological reality because the information transmitted by the axon has the form of energy (and is inseparable from energy). therefore, the neuron knows which part of its output energy was accepted by other neurons. the process of learning can be described by the following algorithm: first, the neuron computes its output with its initial random weight. then the neurons in the higher layer set their weights according to their level of contentment with the reference neuron. in the next step, the neuron changes its weights accordingly. several possibilities of the weight change are described later in this paper. then the new output is computed. the neurons in the higher layer read the output and re-calculate their inputs weights. the reference neuron then decides which setting was better. this algorithm has several variants, all of them are using at least 2 successive values of the level of acceptance. this implies that the neuron must be equipped with a memory. the process of learning is on figure 1. from the point of view of the reference neuron the learning is described by the following algorithm: (1.) random initial weights (2.) output with initial weights for the first input (3.) neurons in higher layer (output neurons) compute the utility of the reference neuron and set their input weights accordingly. if they are satisfied with the output of the reference neuron, they increase their weights, otherwise they decrease them. there are several ways how to compute the utility, some of them are described in eq. 3 6. (4.) the reference neuron changes one (or more) of its input weights (5.) the reference neuron repeats the forward phase with the same data but with changed weight (6.) the output neurons compute the utility (as in step 3) (7.) the reference neuron evaluates the change in the step 4 – if it improves the utility, it will keep it, otherwise it will change the weights in the opposite direction (8.) neuron repeats steps 2 to 7 with all the connections and all the inputs. 3. criterions for optimization several methods can be used for the calculation the importance of the neuron. the basic difference among them is the number of output neurons for which the reference neuron is ’working’. the first extreme is a neuron that is optimizing its function for all output neurons. this neuron is ’reading’ all output weights without taking any particular weight into consideration. the opposite extreme is neuron that works only for one neuron in the higher layer; in other words is optimizing its function to improve its utility for this particular neuron. apart from these options, many other compromise criterions can be defined. 100 vol. 12/2017 artificial neural network for models of human operator figure 1. wide figure[4, 5]. 101 martin růžek acta polytechnica ctu proceedings this first idea corresponds to a neuron that is finding such a weight vector ∧ = w1, w2, ..., wn for which the sum of the absolute values of the output weights is maximal. this idea corresponds firmly to the biological reality because the neuron has only one axon and therefore it can only be aware of the total amount of the signal that is accepted by other neurons, not of the particular weights. in the case of the artificial neuron we also expect negative weights; therefore the neuron sums the absolute or square values. the utility q is: q = n∑ j=1 |woj | (3) respectively: q = n∑ j=1 (woj )2 (4) eq. 4 puts stress on great values and reduces the importance of the small ones. this may be in certain cases advantage for the learning but does not correspond to the biological reality. 4. searching the one neuron maximum – the second extreme the other type of training is based on the presumption that the neuron is increasing its importance to only one neuron in the higher layer, therefore it maximizes the function: q = max|woj |; j ∈ [0, 1, ...n] (5) the problem is that if max|wo| = 1, no further improvement is possible and the training stops. in a real situation, we expect networks with many neurons where this value will be reached very soon and then the learning stops. this is not the desired behavior; therefore in that case there should be used an additional condition that ensures the continuation of the training. the solution of this problem is to use a compromise that takes into consideration more than one output neuron but not all of them. this can be done by optimization of some given number of maximal output weights: u = max(|wo|) +max(wo −max(wo)) + ...; (6) where w = {w0, ..., wn−1}. 5. variants of homeostatical neural network apart from the above mentioned variant, several other options must be defined. first of all, the question of the weight range arises at least three options. the most biologically plausible is to limit the weights to interval between 0 and 1. that means that the weights cannot change the polarity of the signal and no gain of the output energy is allowed. this option is the most biologically plausible as the axon, synapse and dendrites are mostly working only as transmitters of the signal. on the other hand, some operation with the signal may be done also on the level of the axon dendrit transmission, for example the inhibitory weights can reduce the neuron potential. this leads to the second idea, to limit the weights to interval 〈−1; 1〉. the last option is not to limit the weights at all, that means the signal can be multiplied by any real number. this is the least biologically plausible method; on the other hand it will bring the highest computational power. the other question is how to choose the weights that should be updated. the first option that comes to mind is to update the weight that has the greatest influence on the result; that means the most sensitive weight. this will lead to highest increase of the utility of the neuron in the next step, however it may not be the best option from the global point of view. making the step always in the direction of the highest gradient may lead to falling into local extreme. also, to find the most sensitive weight consumes a lot of computational power. alternative option is to choose the updated weight randomly or in given order. these two options lead to similar results. it is also possible to imagine the combination of these algorithms, for example by using several steps to update of the most sensitive weights which may be followed by randomly chosen weights. because of the complex nature of the neural networks, it is not possible to say which method is the best for arbitrary data. 6. problems of the idea of homeostatical learning the described idea has two principal limitations. the first one is the learning of the highest layer. the idea of a learning algorithm is that neurons in certain layers are updating their weights according to the higher layer. this can be used for all layers except for the highest as it does not have any output neuron. the solution for practical simulation and testing is that the highest layer was not trained by the homeostatic learning algorithm, but by the back propagation. this is of course is an alteration of the original idea, but for the sake of the practical realization it is the easiest way how to program the homeostatic learning for the rest of the network. in the case of practical application, for example in robot, this problem will be solvable in a natural way because the network will be part of a closed loop. the second problem is the delay question. the reference neuron is updating its input weights accord102 vol. 12/2017 artificial neural network for models of human operator ing to its output weights, but in each neural cell the output calculation takes some time., meanwhile the inputs are changing this means that the forward information will not ’meet’ the information about the utility in the same time. this problem has two solutions. the first is to set the dynamics of inputs to a lower level, so that the speed of information processing in the whole system is significantly higher than the changes of the input signals. the other possibility is to equip the neurons with a memory that stores the previous inputs so that it is possible to recall them when the information about the utility reaches the neuron. 7. conclusions in this paper, the idea of a new learning algorithm for neural networks is presented. this algorithm can cope with some disadvantages that the classical neural networks paradigms have. the proposed algorithm has several variants; from the point of view of the optimization criterion it is optimization for all input weights vs. optimization for only one input weights, and many compromising solutions. from the point of view of the weight update, the possible variants are the update of the weight with the highest sensitivity to the change, of randomly chosen weight of consequently chosen weight. from the point of view of the weight range, it is possible to define weights as positive numbers smaller than 1, as either positive or a negative number in absolute value smaller than 1, or as real numbers. every variant has its pros and cons. due to the high number of variants which is even multiplied by the amount of data (for neural networks as for data driven method it is important which data is fed into the network. the same network can work well with one data and wrongly with another) it is difficult to decide which variants is the most promising. larger testing is needed to understand the quality of the methods. despite the fact that the initial tests showed that the signal prediction task is better fulfilled by back propagation algorithm, the homeostatic neural network seems as a promising method for modeling on mental processes. of course it is not possible to create a model of the complete consciousness, but it is possible to concentrate on some specific region. transport engineering brings many possible applications as the human factor is the most important part in many transport systems. several processes may be modeled and predicted by the use of this network. typical example is a car driver, who is often making decisions with a lack of information and with the use of prior data. it is difficult to understand the factors that make for example the decision whether to cross the crossroads if the traffic light is orange and will become red in a short period of time. in such situations some drivers react differently even if the conditions are the same. the analytical way to explain such states is quite complex, but it is possible to collect enough data (either from real traffic or from a simulator) to predict this type of decisions. the neural network is a good tool to process this data. once the network is trained for certain tasks in a driver’s decision making processes, it can be used for the investigation of other decisions and behavioral predictions. this can help to explain and avoid danger situations caused by aggressiveness, fatigue, emotions and others. references [1] m. růžek, t. brandejský. model of biological ann based on homeostatic neurons. in 12th wseas international conference on neural networks (nn’11), isbn 978-960-474-292-9, athens 2011, pp. 66 69. [2] m. růžek. artificial neural network inspired by homeostasis in biological networks. in proceedings of 17th international conference on soft computing (mendel 2011), isbn 978-80-214-4302-0, pp. 232 235. [3] m. růžek. artificial neural networks for models of driver’s brain functions. in 20th anniversary of the faculty of transportation sciences, czech technical university in prague – selected papers, čvut v praze, 2013, isbn 978-80-01-05320-1, pp. 207 211. [4] m. růžek. modeling of eeg signal with homeostatic neural network. in nostradamus 2013: prediction, modeling and analysis of complex systems, ostrava 2013, isbn 978-3-319-00541-6 pp. 175 180. [5] m. růžek, t. brandejský. model of homeostatic artificial neuron. in neural networks, fuzzy systems & evolutionary computing, isbn 978-960-474-195-3, athens 2010, pp. 145 148. 103 acta polytechnica ctu proceedings 12:99–103, 2017 1 introduction 2 new solution – homeostatical neural network 3 criterions for optimization 4 searching the one neuron maximum – the second extreme 5 variants of homeostatical neural network 6 problems of the idea of homeostatical learning 7 conclusions references 323 acta polytechnica ctu proceedings 2(1): 323–324, 2015 323 doi: 10.14311/app.2015.02.0323 concluding remarks d. v. bisikalo1 1institute of astronomy ras, moscow, russia corresponding author: bisikalo@inasan.ru keywords: cataclysmic variables. there are four persons making the concluding remarks of the conference, so i restricted myself by the 1-st part when we discussed the cvs. i am pleased to note that the scientific level of our meeting has been quite high. i have heard all 46 talks on cvs and only one has not been new for me, my own ”magnetic cvs behaviour: a review”. i would like to stress the very good organization of the conference program, which, in particular, appeared as a balanced number of reviews and contributed talks. i was really impressed by the review talks made by franco giovannelli & lola sabau-graziati, hans ritter & ulrich kolb, joseph patterson, margaretha pretorius, pietro parisi, christian knigge, edward sion, paula szkody, klaus reinsch, and solen balman. all these talks contain the absolutely comprehensive material available today on the discussed problems. i do not reproduce their content, since all of them can be found in this book of proceedings, but i want to note that any researcher, studying cvs, independently on the age and scientific status, will find them useful. nonetheless i would like to focus on one of the important problems addressed in the talks. this is the problem raised by hans ritter. we all know that during the last 30 years the rkcat (undoubtedly, the most known catalogue of cvs and related objects) has been annually supplemented at a rate of approximately 9% a year. however, in his talk, hans ritter has drawn our attention to two important points: 1) servicing the data base is now practically a full-time job, 2) he will not be able to provide this service any longer. at this point a natural question for the entire binary community arises, who will continue with rkcat and in what form?”. happily the authors of this catalogue still intensively work and we have time to solve this problem. but, of course, we all should think about it. the contributed talks have been well prepared and delivered, and the reader may see it when reading the papers in the book of proceedings. like for the reviews i will not retell the content of even the most interesting talks, but i will try to pick out general tendencies that came out after analysis of the contributions. besides, i will highlight the results that might be useful for a broader community of researchers, studying objects and problems other than cvs. the first point, i would like to mention, is grand astronomical progress in south africa. its scientists have presented 7 talks, some of which delivered by very young persons, and all of them have excited an intense interest of the audience. undoubtedly, this burst of activity is concerned with the development and launch of the salt. and, in spite of the fact that david buckley still regards the obtained results as an appetizer, they obviously have become the main course in various fields of astrophysics. the presented talks revealed that theoretical studies and interpretations (both in the number of delivered talks and excited interest) noticeably dominate over observations. indeed we have heard wonderful analytical and numerical contributions that not only explain available observational data both from the space and ground-based instruments but also possess the great potential for the predictions, analysis and generalization of upcoming data. i do not want to focus on a particular work since i hope that the reader will first get familiar with the original papers but not these concluding remarks however, i must emphasize noticeable progress in observational methods. this has become my discovery that by using quite simple modifications one can significantly improve the quality of doppler tomography (see the papers of e. kotze, m. uemura, s. zharikov, s. potter, d. kononov) observational works have mostly followed a conservative way of data accumulation, which, undoubtedly, is the most important part of any research and the basics of scientific progress. at the same time we have got some surprises: .odendaal has told us that cal83 is a new candidate to ae aqr-like system; j. v. hernandez santisteban et al. have confirmed the detection of a sub-stellar donor star in a cv; d. chochol et al. have reported the superoutburst observations of a possible new helium-rich dwarf nova 2013 in hercules. the next important aspect in the development of observations is concerned with the effective usage of surveys (see, e.g., the wonderful paper of p. szkody about cvs from sdss and the paper of p. cartera about cvns in 323 http://dx.doi.org/10.14311/app.2015.02.0323 d. v. bisikalo sdss) and data from space telescopes (see e.g. the papers of p. parisi, s. balman, m. kotze, v. suleimanov, a. semena). resuming my concluding remarks i would like to stress that the conference was not only interesting, but also useful. i thank the organizers of the conference not only for the nice time, spent in the marvelous place, but also for the opportunity to discuss all the results in the friendly atmosphere. as i found when talking with many participants, we all are interested in the continuation of this series of meetings and in making this conference recurrent. franco giovannelli & lola sabau-graziati and their team are the main engine of the conference and i hope that they will continue this hard job, the organization of cvs conferences. 324 acta polytechnica ctu proceedings doi:10.14311/app.2017.11.0091 acta polytechnica ctu proceedings 11:91–96, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app measurement methods of internal stress in continuous welded rail petr vnenk∗, bohumil culek department of transport structures, faculty of transport engineering, university of pardubice, studentska 95, pardubice, czech republic ∗ corresponding author: petr.vnenk@student.upce.cz abstract. this paper deals with the problem of internal rail stress estimation. it is based on a detailed research of contemporary situation in the field, presents basic outlines of the problem and sums up the major research areas and their possible applications in the current state of railway infrastructure management. the directions are divided into four categories in the paper: displacement methods, rail shifting methods, methods based on acoustoelastic effect and methods based on magnetoelastic effect. particular methods, both scientific and industrial, are presented in their section respectively. every method that is presented within the scope of this paper is briefly described and its advantages and disadvantages are mentioned. in the end, potential of application of some of the presented methods in the practical use is discussed. keywords: rail, stress, measurement, cwr, temperature. 1. introduction continuous welded rail, abbreviated as cwr, is a part of railway superstructure that has been under continuous development since its beginnings in the first half of the twentieth century. the implementation of continuous welded rail caused a major qualitative improvement in the railway transport. one of the biggest challenges of this improvement was the mitigation of the thermal stress effect. at the moment of welding, there is a certain stress state which equals a temperature called "neutral temperature". the neutral temperature is characterized by the attribute that when a welded rail reaches the neutral temperature, the rail is free from thermal stress. when the rail temperature is higher than the neutral temperature, compressive stress in rail emerges. at extreme temperatures, the compressive stress induced in the rail can cause railway track buckling, also known as "sun kink". on the contrary, when the rail temperature is lower than the neutral temperature, tensile stress in rail emerges. at extreme temperatures, the tensile stress induced in the rail can cause the rail to be pulled apart. the thermal stress in the continuous welded rail is expressed as σ = −α · ∆t · e (1) where α = 12 · 10−6k−1 (2) and e = 210 · 109pa (3) in the czech republic, the permitted welding temperature for rails ranges from 17 °c to 23 °c [1]. considering the minimum rail temperature at -30 °c and the maximum rail temperature at 60 °c (for rails situated in the sunny locations and thus heated), the difference between the extreme temperature and the neutral temperature can reach as many as 53 °c [2]. assuming such conditions, the thermal stress in continuous welded rail is σ = 133.56 · 106pa (4) this stress as such is not high enough to cause failure of continuous welded rail. however, there are other contributing factors, too. the thermal stress is cyclic, repeating in both daily and yearly cycles. trains cause further heavy dynamic loading which is cyclic, too. all these loadings are countable. it appears, however, that the neutral temperature is not constant over a period of time. based on the location of the rail, it seems the neutral temperature is shifting. this shift of the neutral temperature can reach even several degrees of celsius. this difference has to be added to the ∆t parameter, eventually increasing the thermal rail stress. combinations of the above mentioned stresses and their cyclic character have adverse influence on continuous welded rails. unlike the other items, it is very difficult to predict the shift of the neutral temperature. this article presents contemporary findings in 91 http://dx.doi.org/10.14311/app.2017.11.0091 http://ojs.cvut.cz/ojs/index.php/app petr vnenk, bohumil culek acta polytechnica ctu proceedings this area and suggests possible solutions to the evaluation of the thermal stress in rail with the influence of the neutral temperature shift. 2. displacement methods displacement methods of cwr stress measurement work on the simple mechanical assumption of change of a relative distance between two points of material, rail in this case. in newton’s mechanics, relatively stiff rail behaves according to hook’s law if unfastened. however, even the fastening systems ensure only a certain level of rigidity and, provided the axial force in rail is strong enough, a relative displacement can be observed even at fastened rail sections. as of now, some solutions using displacement are available as presented below. 2.1. research of the gdansk university of technology this research was carried out in the mid-seventies at the gdansk university of technology, poland. a displacement sensor with accuracy of 0.001mm has been applied for a measurement on a 200mm long rail section. next to the cwr measurement spot, a reference rail section has been placed. this reference rail section has been set free to lengthen and shorten. it was able to observe soon that the stress varies over different sections of the rail even if the temperature of the rail was the same at measured locations. it is believed that this effect is caused by slip of rail in the fastening points. such a slip can be derived by several sources like tangential forces of traffic, but also by exposure of some parts of rail to sun and location of some parts of rail to completely shady place. such a different exposure to sun results in different daily mean temperature and, subsequently, to a stress gradient in the rail. this revealing is a good asset of the measurement. the method itself, however, is not suitable for commercial use as it is very costly, time demanding and requires a reference rail to be placed at the measurement spot. nevertheless, it can well serve as a reference method for calibration of other methods [3]. 2.2. the calibrated length of rail method this method, which has supposedly been applied in china since 1982, consists of length comparison of a freely placed 50m long steel strip with a selected rail section originally of the same length. the principle of this method, however, appears to be the same like in the research of the gdansk university of technology, only modified for a bigger span. author’s daring claim that this method is the only one in the world without "fatal" shortcomings and can be operated widely does not match the state of the research in this area after the publication date, because much of research has been emerging in this field [4]. 2.3. measurement with bi-directional fbg strain sensors one of the most recent papers covering this topic, from 2015, presents a method of displacement measurement in a rail web in longitudinal and vertical direction using optic fbg sensors. in general, this measurement resembles strain gauge measurement. however, the advantage of fbg sensors is the possibility to measure even temperature, apart from mere strain. moreover, it is characterized by its longer durability in relation to strain gauge sensors. provided the sensor is attached to the rail web prior to cwr installation (i.e. at rail neutral temperature or known rail tension), it keeps measuring the deformation as long as the sensor works. this can be theoretically reached using strain gauges only, although the durability appears as an important factor here. [5]. 2.4. vortok measure and detect another option to measure displacement can be reached by using the measure and detect sensor produced by vortok ltd. company. simple sensor that is able to measure variety of parameters is made ready to be screwed into a drilled hole in a rail web. the manufacturer does not share any detailed information of what principles this device uses. it looks, however, like a piezoelectric sensor with accessories that is incorporated into a screw-in dowel. this robust shape most probably predicts a displacement method with a long durability. a disadvantage of this method is a necessity of calibration. after calibration is made, either by fastening of the device on a stress-free rail or by using another calibration method, the value of internal stress in rail can be obtained in a stable manner. the options to set up automatic data transmission via email or wi-fi even from a moving train make this sensor a user-friendly device [6]. 3. rail shifting methods rail shifting methods of cwr stress measurement use the principle of bending stiffness dependence on axial tension in rail. provided the rail is in tension, the higher force is necessary to be applied to laterally shift the rail the higher the axial force in the rail is. apparently, these methods are viable only when the rail is in tension, otherwise failure by buckling may appear. 3.1. verse method this method has been presented by vortok ltd. company from the united kingdom. in the first place, the rail shall be released from all fastenings in the length of 30m. afterwards, the central part of the unfastened section of the rail shall be lifted into a certain height. the force that is applied to move the rail is related to the axial force in the rail. wide use of this method is restricted by some disadvantages. the most obvious one is the limitation to tensile stress in the measured rail. the operator needs 92 vol. 11/2017 measurement methods of internal stress in cwr to be sure that there is a tensile stress as problems with re-installation of the rail into the original position could occur, leave apart the danger of operator’s injury or material damage. another disadvantage is the need to unfasten the rail in the length of 30m. this operation requires additional time and subsequently prolongs track closure. moreover, in case the measured section is situated in radius, re-installation of the rail can be difficult, too, as the condition of tensile stress in rail is inevitable. even though the disadvantages are important, this method appears to be one of the most widely spread to measure the cwr stress nowadays. the manufacturer produces their own device for rail lifting and stress measurement. light aluminium design of this device enables easy transport, manipulation and operation [7]. 3.2. use of tamping machine in a paper published in 2009, scientists at gdansk university of technology look into a possibility to use tamping machine for stress measurement in cwr. tamping machine is capable to shift rails in both vertical and horizontal direction when adjusting railway track geometry. the goal of this research was to use this movement to estimate the stress in cwr. the principle of this measurement is similar like at the verse method, including the disadvantages. however, the disturbing signal produced by the operation of tamping machine turned out to be too high and the attempts to get some cwr stress data were unsuccessful [8]. 4. methods based on acoustoelastic effect the acoustoelastic effect is a physical effect of change of sound velocity based on change of mechanical stress in elastic continuum. for measurements, ultrasound is used. the definition, however, can cover vibration, as mechanical waves, too. in such a case, vibrometer is used as a measurement tool. it is always necessary to execute a calibration measurement on the site with known temperature and mechanical stress as the sound velocity in rail is not dependent only on mechanical stress, but on steel microstructure, too. this calibration measurement can be performed either prior to cwr installation, or once the cwr is installed. however, in the latter only when the rail is cut, unfastened and welded again. as a consequence, similar disadvantage like at displacement methods emerges, which means the need to start the measurement at the neutral temperature. the advantage, on the contrary, is in possible high durability of ultrasound sensors and their attachment to measurement place. 4.1. j. szelazek measurement j. szelazek has worked out two ultrasound measurement procedures in the nineties of the twentieth century. in the first procedure, ultrasound signal is emitted vertically from the top of rail head to the bottom of rail foot where it reflects off and moves back to the receiver, which can be the same device as the emitter. the second procedure uses separate emitter and receiver and those are placed to the side of rail head horizontally next to each other. the signal moves through the rail head lengthwise, in this case. the first procedure showed as inapplicable, as the signal dispersed due to uneven rail head profile. the major cause of this unevenness is the rail head wear. placing the signal receiver to the bottom of rail foot did not improved the results and, moreover, the signal path was reduced to one half. the second procedure appeared more promising, but even at this measurement, disturbances appeared and the results were influenced by strong dispersion [9]. 4.2. research of the university of florence in 2007, italian scientists worked out the second procedure of j. szelazek. this procedure has been tested for 2 years and appears viable. however, it shares all the common disadvantages of ultrasound methods and the necessity to perform calibration measurement in situ [10]. 4.3. measurement of stresses using the polarization of rayleigh surface waves two us researches work with measurement of polarization of rayleigh surface waves. measurement of dependence of the rayleigh surface waves polarization on change of mechanical rail stress turned out not just to be more robust than measurement of dependence of the rayleigh surface waves velocity on change of mechanical rail stress, but also to be easier to detect. michael d. a. junge’s work deals with general measurement of mechanical stress in material based on rayleigh surface waves [11]. stefan hurlebaus’ report deals with application of this procedure on rail stress research. on page 42, the author presents that the polarization of rayleigh surface waves is dependent on the value of axial force in rail and that a further research is recommended [12]. 4.4. vibration measurement two publications, a diploma thesis and a research report, deal with vibration measurement of the internal rail stress. both of them are outputs of one research. the results of the rail stress determination from wave lengths of vibrating sensor seem well in laboratory conditions when a steel bar or a new rail is used. in case of worn rail, and this is very important for practical application, it is possible to get certain results, but these results are not that clear like in the previous cases. when performing a field measurement, the results of measurement on worn rail are much worse. 93 petr vnenk, bohumil culek acta polytechnica ctu proceedings as of yet, this method is inapplicable. in case it is possible to diminish the problems, this method can have a good perspective [13, 14]. 5. methods based on magnetoelastic effect the magnetoelastic effect is inverse magnetostrictive effect. it is presented as a change of magnetic susceptibility in relation to change of mechanical stress in material. the magnetoelastic effect is also known as the villari effect. 5.1. measurement of magnetic hysteresis in the nineties, d. utrata tested the possibility of application of the magnetoelastic effect on the rail stress measurement. he measured the dependence of coercivity and remanence of the magnetic field in rail on different surface conditions, like scaled rail surface, or milled rail surface. however, the comparison of the obtained data has shown various results based on the input type of rail. surprisingly, the only data that match were on the milled running surface and scaled base underside. d. utrata assumes, in the end, that either a calibration measurement or a new approach to data interpretation has to be delivered in order to make this method applicable. a. wegner needed 400 calibration sensors to run a measurement of 3 meters long rail using the hysteresis method, which does not contribute to viability of this method [14, 15]. 5.2. measurement of magnetic barkhausen effect japanese scientists tsuchima and enokinozo have studied the reaction of the barkhausen noise on mechanical stress in steel plate. it is possible to get some relation from the graphs of the mutual dependence. however, the authors found it difficult to estimate the influence of time and get a value of the mechanical stress. additionally, they suggest application of the chaos theory to get a better interpretation of the results [16]. measurement using the barkhausen noise together with measurement of magnetic permeability is used by elektro-thermit gmbh & co. kg. company to determine the internal rail stress. their method requires calibration on a rail test sample. their product has been awarded a certificate of the railway infrastructure manager of denmark, banedanmark. on the contrary, the manufacturer appears not interested in sale of their product and only offers to perform a measurement in the required section by themselves [3, 17]. 5.3. metal magnetic memory measurement collective of authors from the university of nanjing have carried out an experiment of measuring the effect called metal magnetic memory on a steel test sample. figure 1. dhp(y)/dx for applied tensile stress on a steel sample [18]; see the linear dependence in the elastic region. contrary to the barkhausen noise, this effect does not require external magnetization of the sample. the effect is activated anywhere in the natural magnetic field of the earth. when the loading increases, the rotation of the weiss magnetic domains in metals raises the value of the magnetic flux around the central point and this increases the gradient of the magnetic flux which is in elastic region linearly dependent on the stress in the sample. graph of the linear dependence of the magnetic flux gradient on the mechanical stress in a steel sample as measured by wang, et. al. [18] is presented in figure 1. the linear dependence in the elastic region is completely sufficient, because rail geometry deformation emerges earlier than plastic deformation in the axial direction of the rail [18]. 6. discussion every presented method has its limitation. displacement methods can be related to widely spread strain gauge measurement. this has been used in many industrial application; in this case, however, the biggest problem seems to be the necessity to measure an absolute value of stress, not a relative one, which is the common purpose of strain gauge measurement in general. rail shifting methods, especially the verse method, seem to be one of the most reliable at this time. the reliability is underpinned by its simplicity. however, more extensive use of this method is very limited through many disadvantages it inevitably drags along. movement of a rail is a complicated operation, which needs expensive tools and is very time demanding. re-installation of the rail requires verification that the rail is in good condition after the measurement and safety of operation on the track is kept. additionally, performing such a measurement in radius is much more complicated and performing such a measurement when the rail is under a compressive stress is excluded. considering the compressive stress 94 vol. 11/2017 measurement methods of internal stress in cwr in rail is usually during the day, the limitations of use of this method are vast. methods based on the acoustoelastic and magnetoelastic effect have the potential to become viable in the non-destructive rail stress measurements. as of yet, however, the problems of getting clear values of stress were not mitigated and residual stresses, difficult conditions of field measurement, or even various conditions of the rail itself (wear, rust, etc.) prevented the research to reach a satisfactory solution. 6.1. further research orientation out of the contemporary possibilities, there are some ways to be worked out in order to either get satisfactory results or to discover serious obstacles that hinder their application. (1.) application of the metal magnetic memory method on internal rail stress measurement seem like a research that has not been done yet. as mentioned in section 5, this method does not require external magnetization [18] and this is a great asset for possible further application. if the measurement of the gradient of magnetic flux in rail results in a similar dependence as shown in figure 1, the potential of applicability of this method would be great [18]. (2.) vibration measurement, or modal analysis could also offer an approach to obtain data of internal stress in cwr. however, damping caused by rail fastenings could have too high influence on the results. as presented in section 4, the vibration analysis performed by the team of the university of illinois at urbana-champaign did not produce any applicable results even after they released some fastenings, which is a procedure that is disadvantageous as such [13, 14]. (3.) provided the stress could be evaluated from a surface layer of rail only, i. e. there was a mutual relation between surface stress and stress in the core of the rail, another possible method emerges. method of dependence between passive layers formation in electrolyte and mechanical stress in the surface layers has been shown in an experiment of stainless steel in a normal sulphuric acid bath [19]. (4.) another option is to work out the measurement of stresses using the polarization of rayleigh surface waves. the papers presented in section 4 suggest a further research can have a potential to find out a viable solution [11, 12]. (5.) finally, if strain gauge is able to measure a quasi static load change in a long term, a statistical evaluation of measurements could provide a range of data that could be sufficient for prediction of neutral temperature level and subsequently stress level in rail. if such a research is biased towards a certain limited location, an applicable methodology can be a reasonable output. 7. conclusions many attempts to measure the neutral temperature or stress in continuous welded rail have been undertaken. displacement and rail shifting methods like vortok measure and detect or verse have been finalized in an applicable product and offered on market. these methods come out of mechanical solutions. however, these methods suffer from many limitations and requirements of special conditions that are necessary to be created in order to use the methods. later in time, non-destructive methods based on the acoustoelastic or magnetoelastic effects have been tested. as of yet, none of them reached the level of being reliable enough to compete with the above mentioned ones. nevertheless, there are some promising results and further research in this area, as described in section 6, could prove viability of some of them. provided strain gauges are capable of measuring quasi static load in a long term and a thorough strain gauge measurement is done, the value of stress in a continuous welded rail could be estimated on a certain geographical area even from statistical data measured by strain gauges. finally, the possible solution can lurk in another method of stress evaluation in a continuum, a method which is not yet known to the authors of this paper. acknowledgements the work was created in connection with the scientific research project of the university of pardubice no. sgs_2017_009. the authors are grateful for the support. references [1] sprava zeleznicni dopravni cesty, s.o. szdc s 3/2 bezstykova kolej, 2013. kapitola iii, cast a, bod 110. [2] sprava zeleznicni dopravni cesty, s.o. szdc s 3 dil iv zeleznicni svrsek. kolejnice ve zneni zmen c. 1 a 2, 2014. kapitola iv, bod 43. [3] w. koc, et. al. okreslanie wartosci sil podluznych w szynach toru bezstykowego. problemy kolejnictwa 163, 2014. [4] l. xing-han. the "calibrated length of rail" method for measuring rail temperature stress. arema proceedings of the 2000 annual conference 2000. [5] p. wang, et. al. longitudinal force measurement in continuous welded rail with bi-directional fbg strain sensors. smart materials and structures 25, 2015. [6] vortok, ltd. vortok measure and detect, 2012. vortok, [2016-06-07], http://www.vortok.com/rail-stress-management/ vortok-measure-and-detect-2. [7] vortok, ltd. verse, 2012. vortok, [2016-05-31], http: //www.vortok.com/rail-stress-management/verse. [8] w. koc, a. wilk. investigations of methods to measure longitudinal forces in continuous welded rail tracks using the tamping machine. journal of rail and rapid transit 223(1), 2009. 95 http://www.vortok.com/rail-stress-management/vortok-measure-and-detect-2 http://www.vortok.com/rail-stress-management/vortok-measure-and-detect-2 http://www.vortok.com/rail-stress-management/verse http://www.vortok.com/rail-stress-management/verse petr vnenk, bohumil culek acta polytechnica ctu proceedings [9] j. szelazek. monitoring of thermal stresses in continuously welded rails with ultrasonic technique, 1998. ndtnet, 1. june 1998, [2016-05-30], http://www. ndt.net/article/dresd97/szelazek/szelazek.htm. [10] d. vangi, a. virga. a practical application of ultrasonic thermal stress monitoring in continuous welded rail. experimental mechanics 47, 2007. [11] m. d. a. junge. measurement of applied stresses using the polarization of rayleigh surface waves, 2003. atlanta, georgia, school of civil and environmental engineering, institute of technology. [12] s. hurlebaus. determination of longitudinal stress in rails, 2011. college station, texas, transportation research board of the national academies. [13] r. weaver. vibration measurement of rail stress, 2006. champaign, illinois, transportation research board of the national academies. [14] m. j. koob. the development of a vibration technique for estimation of neutral temperature in continuously welded railroad rail, 2005. champaign, illinois, university of illinois at urbana-champaign. [15] d. utrata, a. strom, m. negley. stress measurement in railroad rail using ultrasonic and magnetic technique. review of progress in quantitative nondestructive evaluation 14, 1995. [16] y. tsuchida, m. enokinozo. stress evaluation by chaotic characteristics of barkhausen noise. review of quantitative nondestructive evaluation 22, 2003. [17] a. wegner. stress-free temperature monitoring using different measuring technologies – experiences and assessment. proceedings of 10th international heavy haul association conference 2013. [18] p. wang, et. al. stress measurement using magnetic barkhausen noise and metal magnetic memory testing. 17th world conference on nondestructive testing 2008. [19] f. navai. effects of tensile and compressive stresses on the passive layers formed on a type 302 stainless steel in a normal sulphuric acid bath. journal of materials science 30, 1995. 96 http://www.ndt.net/article/dresd97/szelazek/szelazek.htm http://www.ndt.net/article/dresd97/szelazek/szelazek.htm acta polytechnica ctu proceedings 11:91–96, 2017 1 introduction 2 displacement methods 2.1 research of the gdansk university of technology 2.2 the calibrated length of rail method 2.3 measurement with bi-directional fbg strain sensors 2.4 vortok measure and detect 3 rail shifting methods 3.1 verse method 3.2 use of tamping machine 4 methods based on acoustoelastic effect 4.1 j. szelazek measurement 4.2 research of the university of florence 4.3 measurement of stresses using the polarization of rayleigh surface waves 4.4 vibration measurement 5 methods based on magnetoelastic effect 5.1 measurement of magnetic hysteresis 5.2 measurement of magnetic barkhausen effect 5.3 metal magnetic memory measurement 6 discussion 6.1 further research orientation 7 conclusions acknowledgements references 66 acta polytechnica ctu proceedings 2(1): 66–70, 2015 66 doi: 10.14311/app.2015.02.0066 multifrequency behaviour of polars k. reinsch1 1georg-august-universität göttingen, institut für astrophysik, friedrich-hund-platz 1, 37077 göttingen, germany corresponding author: reinsch@astro.physik.uni-goettingen.de abstract cataclysmic variables emit over a wide range of the electromagnetic spectrum. in this paper i will review observations of polars in relevant passbands obtained during the last decade and will discuss their diagnostical potential to access the physics of the main components within the binary systems. this will include a discussion of intrinsic source variability and the quest for simultaneous multi-frequency observations. keywords: cataclysmic variables polars optical spectroscopy photometry ir uv x-rays. 1 introduction in the standard model of magnetic cataclysmic variables a polar is described as a semi-detached binary in which matter from a roche-lobe filling late-type mainsequence star is coupled outside the circularization radius to the field lines of a highly-magnetic white dwarf and channeled onto small accretion region(s) in the vicinity of the magnetic pole(s). the system components can be observationally disentangled – at least to some degree – by their characteristic emission in different wavelength regimes (see fig. 1). the contribution of the binary components to the spectral energy distribution of the system will be discussed individually and in the context of multi-frequency observations. the basic understanding of polars has not much changed since the comprehensive review by warner (1995). i will, therefore, concentrate on recent observational findings which led to a more detailed understanding of the physical processes involved. figure 1: schematic view of a polar and main emission regions (iris traulsen, adapted from marc garlick). 66 http://dx.doi.org/10.14311/app.2015.02.0066 multifrequency behaviour of polars 2 binary components and spectral energy distribution 2.1 secondaries in polars secondaries in polars emit most of their light in the red and near ir. but even in these bands their luminosity is generally outshone by other components within the binary. the secondaries are, therefore, best studied when the system happens to be in a low state of accretion or during eclipses of the accretion region and the white dwarf. optical and near-ir studies have revealed that their spectra are consistent with normal late-type dwarfs (or brown dwarfs). contrary to similar studies of non-magnetic systems, no significant abundance anomalies have been found from near-ir spectroscopy of the secondaries in polars. this provides evidence that magnetic and non-magnetic systems might take different evolutionary paths (harrison et al., 2005). spectroscopy during the eclipse of the primary combined with phase-resolved near-ir photometry of polars can be used to determine the spectral type and the brightness of the secondary, as has been shown e.g. for the long-period polar v1309 ori (reinsch at al., 2006). using calibrations of the surface brightness of m-dwarfs (e.g. beuermann 2000), from the brightness of the secondary an accurate distance of the system can be derived. 2.2 circumbinary dust disk mid-infrared observations of the short-period polar ef eri with the infrared spectrograph (irs) on the spitzer space telescope have revealed the presence of emission in the 3–14 µm wavelength range which exceeds the combined spectral energy distribution of the white dwarf, the l5-type brown dwarf secondary, and cyclotron radiation from the b ≈ 13 mg white dwarf magnetic field. hoard et al. (2007) concluded that the spectrum longward of ∼ 5 µm is dominated by emission from a circumbinary dust disk. in a later paper, however, harrison et al. (2013) argue based on combined ground-based, spitzer, wise, and herschel observation of the two polars am her and ef eri that their midinfrared excess can be fully explained by optically thin emission from the lowest cyclotron harmonics (n ≤ 3). 2.3 stellar activity of the secondary from long-term observations of polars it is well known that most systems alternate between low and high states and sometimes also intermediate states of accretion. the best studied system is am her with a record of 33 years of optical observations by the american association of variable star observers (aavso, http://www.aavso.org/). due to the absence of an accretion disk in polars such changes must reflect the immediate response of the system on variations of the mass-transfer rate. stellar activity of the donor star has been proposed as a possible mechanism to induce such variations (e.g. hessman et al., 2000). in a recent analysis of shortand long-term brightness variations of five polars, periodic variations were indicated which could result from magnetic cycles in the secondary stars (kalomeni, 2012). kafka et al. (2010) present another piece of evidence for stellar activity from phase-resolved high-resolution spectroscopy of polars in low states. they interprete two bright satellites of the central low-velocity component in the hα doppler map of bl hyi as prominencelike magnetic loops kept in place by magnetic field interactions between the white dwarf and the donor star. howell et al. (2006) have monitored the long-term variation of the hα equivalent width of ef eri during its extended low state and attribute the observed behaviour to chromospheric activity of the secondary. in addition they identify magnetic field interaction between the two stars as a probable mechanism that would concentrate stellar activity on the white dwarf facing hemisphere of the secondary. 2.4 coupling region partially ionized matter released from the secondary over the l1 point is assumed to follow initially a freefalling trajectory. at the magnetospheric radius of the white dwarf the ram pressure of the infalling gas is balanced by the magnetic pressure and the accretion stream couples to the magnetic field of the white dwarf. observationally little information is available on the processes occurring in this coupling region. xmm-newton observations of v1309 ori show a prolonged ingress of the soft x-ray light curve with xray emission being visible beyond the geometrical occultation of the white dwarf. schwarz et al. (2005) have suggested plasma heated by shocks in the coupling region as a possible origin of the x-ray emission seen during eclipse. 2.5 accretion curtain beyond the coupling region accretion becomes magnetically controlled and the initially narrow ballistic stream is diverted off the orbital plane and forms a broad curtain-like structure through which matter is channeled into the vicinity of the magnetic poles of the white dwarf. the accretion stream and curtain are characterized by an optical and uv emission-line spectrum comprising strong lines of neutral hydrogen and of ionized helium. using relatively simple geometrical assumptions indirect imaging techniques, like doppler 67 k. reinsch tomography, roche tomography, accretion stream mapping, and eclipse mapping, have been well established to confine the geometrical parameters of different parts of the accretion stream (e.g. schwope et al., 2004). 2.6 white dwarf white dwarfs in polars have typical temperatures in the range 10,000–15,000 k. their photospheric emission has been well studied in the uv and far-uv spectra of polars in low states of accretion. based on a far-uv spectroscopic survey with hst/ stis, araujo-betancor et al. (2005) found that at any given orbital period white dwarfs in magnetic cvs are colder than those in non magnetic cvs with the differences in effective temperatures being largest for systems above the period gap. as a possible explanation they suggest that magnetic braking in polars might be reduced. the magnetic field structure of several white dwarfs in polars has been studied in detail using phase-resolved circular spectropolarimetry and zeeman tomography (e.g. beuermann et al., 2007 and references therein). in most cases the field structure departs significantly from that of a dipole field and higher order multipoles are required to adequately describe the observed zeeman spectra. accreting material is flowing preferentially along field lines reaching far out towards the ballistic part of the stream. depending on field geometry and accretion rate, this leads to one or more accretion regions on the white dwarf. 2.7 accretion region in the standard scenario actual accretion onto magnetic white dwarfs occurs in a comparably small region of some 0.1% of the white dwarf surface. infalling matter forms an accretion column with a shock front at some height above the white dwarf where the supersonic gas of the accretion stream is decelerated to a subsonic settling flow. the shock height and the depression of the post-shock flow below the photosphere depends on the magnetic field strength, the mass of the white dwarf, and the specific accretion rate. the structure of the accretion column has been studied theoretically. the emergent spectra have been calculated by radiationhydrodynamical models as a function of mass-flow rate and field strength (e.g. fischer & beuermann, 2001; beuermann, 2004). at low mass-flow rates, the shock stands above the atmosphere and bremsstrahlung radiation is the main cooling process. for larger accretion rates the emission is hidden behind the column density and reprocessed as soft x-rays. irradiation is the principle cause for a large heated accretion cap extending far beyond the impact region of the accreted material. calculations with a standard lte stellar atmosphere code including an angledependent external radiation source have demonstrated that much of the reprocessed light appears in far uv and not at soft x-rays (könig et al., 2006). observationally the temperature distribution in the accretion spot could be demonstrated by the analysis of the chandra letg spectrum of am her. this data provide enough photons to show that the soft x-ray component cannot be fitted by a single temperature model (beuermann et al., 2012). at high mass-transfer rates sufficiently dense blobs can penetrate to large optical depths in the white-dwarf atmosphere submerging the shock below the photosphere. the most extreme example of this “blobby accretion” case has been observed in v1309 ori. its soft x-ray light curve obtained with xmm-newton shows x-ray emission occuring in flares of typically 10 s time scale. this corresponds to a length scale of 4 × 109 cm for the infalling filaments (schwarz et al., 2005). short-term spectral variability at x-ray wavelengths could be studied in the rosat pspc high state observation of am her which contains 1.3 million counts. significant variability on time scales down to 200 ms could be detected. correlated spectral and count-rate variations are seen in flares on time scales down to 1 s, demonstrating the heating and cooling associated with individual accretion events (beuermann et al., 2008). some polars are even bright enough that x-ray emission line spectroscopy is feasible with current instruments. the high-diagnostics potential of such observations has been demonstrated e.g. by girich et al. (2007), mauche et al. (2003), mauche et al. (2009). 3 variability of spectral energy distribution several polars have been studied at different epochs yielding that their optical, uv, and x-ray fluxes can vary by more than an order of magnitude. as an example, fig. 2 shows the integrated energy flux νfν from the infrared to the hard x-ray regime of the polar rx j1007.5-2017 collected with various instruments between 1992 and 2001. the left panel shows spectrophotometry of 1992, 1997, and 2000 (black curves), supplemented by the 2mass j, h, and k-band fluxes of 1999 (red filled squares) and the visual and ultraviolet fluxes measured with the optical monitor on board of xmm-newton simultaneous to the 2001 x-ray observation (red filled circles). the green curve represents the adjusted flux distribution of the dm3 star lhs58 which is expected to match the spectral type of the donor star and to be the main contribution to the 1997 low-state spectrum. 68 multifrequency behaviour of polars figure 2: spectral energy distribution of the polar rx j1007.5-2017 at different epochs (from: thomas et al. 2012) the right panel shows the incident spectra for the 2001 xmm pn observation (red filled circles) and the 1992 rosat pspc observation (open circles). the dashed curve illustrates the “source spectrum” corrected for interstellar absorption (thomas et al., 2012). 4 conclusions x-ray and optical surveys, like the rosat all-sky survey and the sloan digital sky survey, let to the discovery of a large number of new polars during the recent two decades increasing the sample size to 135 polars with known orbital periods (ritter & kolb 2003; 2013). in addition, sensitivity and instrumental capabilities at all wavelengths have been significantly enhanced. taking both together, polars provide an important lab to quantitatively understand individual systems and physical processes of matter under extreme conditions. in this sense, we are indeed currently in a “golden age” of research on polars. there are still several fundamental questions remaining open. among these are: do we fully understand the evolution of polars? what drives accretionrate variations? do polars with fields as high as in single white dwarfs exist? what is the origin of the magnetic field in polars? what exactly happens in the coupling region? multi-frequency observations are a powerful tool to improve our understanding of polars in future. due to large variations of the accretion rate on different time scales simultaneous coverage at different wavelengths is mandatory. acknowledgement i thank the many people who contributed to increase our knowledge on polars over the last decade, and kindly acknowledge fruitful and long-lasting collaborations with klaus beuermann, vadim burwitz, essam el-kholy, fabian euchner, boris gänsicke, yonggi kim, axel schwope, robert schwarz, hans-christoph thomas, iris traulsen, and fred walter which led to several papers i have referred to in this contribution. references [1] araujo-betancor, s., gänsicke, b.t., long, k.s., beuermann, k., de martino, d., sion, e.m., szkody, p., 2005, apj 622, 589 doi:10.1086/427914 [2] beuermann, k., 2000, new astr. rev. 44, 93 doi:10.1016/s1387-6473(00)00020-8 [3] beuermann, k., 2004, aspc 315, 187 [4] beuermann, k., el kholy, e., reinsch, k., 2008, a&a 481, 771 [5] beuermann, k., euchner, f., reinsch, k., gänsicke, b.t., 2007, a&a 463, 647 [6] beuermann, k., burwitz, v., reinsch, k., 2012, a&a 543a, 41 [7] fischer, a., beuermann, k., 2001, a&a 373, 211; 69 http://dx.doi.org/10.1086/427914 http://dx.doi.org/10.1016/s1387-6473(00)00020-8 k. reinsch [8] girich, v., rana, v.r., singh, k.p., 2007, apj 658, 525 [9] harrison, t.e., howell, s.b., szkody, p., cordova, f.a., 2005, apj 632, l123 doi:10.1086/498067 [10] harrison, t.e., hamilton, r.t., tappert, c., hoffman, d.i., campbell, r.k., 2013, aj 145, 19. [11] hessman, f., gänsicke, b., mattei, j., 2000, a&a 361, 952 [12] hoard, d.w., howell, s.b., brinkworth, c.s., ciardi, d.r., wachter, s., 2007, apj 671, 734. doi:10.1086/522694 [13] howell, s.b., walter, f.m., harrison, t.e., huber, m.e., becker, r.h., white, r.l., 2006, apj 652, 709 doi:10.1086/507603 [14] kafka, s., tappert, c., ribeiro, t., honeycutt, r.k., hoard, d.w., saar, s., 2010, apj 721, 1714 doi:10.1088/0004-637x/721/2/1714 [15] könig, m., beuermann, k., gänsicke, b., 2006, a&a 449, 1129 [16] mauche, c.w., liedahl, d.a., fournier, k.b., 2003, apj 588, l101 doi:10.1086/375684 [17] mauche, c.w., 2009, apj 706, 130 doi:10.1088/0004-637x/706/1/130 [18] reinsch, k., kim, y., beuermann, k., 2006, a&a 457, 1043 [19] ritter, h., kolb, u., 2003, a&a 404, 301 (update rkcat7.20, 2013) [20] schwarz, r., reinsch, k., beuermann, k., burwitz, v., 2005, a&a 442,271 [21] schwope, a., staude, a., vogel, j., schwarz, r., 2004, an, 325, 197 [22] thomas, h.-c., beuermann, k., reinsch, k., schwope, a.d., burwitz, v., 2012, a&a 546, a104 [23] warner, b., 1995, cataclysmic variable stars, cambridge university press discussion david buckley: would you care to comment on the fact that a certain fraction of polars have no directly (observed) determined magnetic fields (e.g. from either detection of cyclotron features or spectropolarimetry) and have been suggested to be low-field systems. klaus reinsch: the magnetic field of polars must be strong enough that spin and orbital motion of the white dwarf will be synchronized. direct measurements of magnetic fields in polars require the systems to be in a suitable state that either cylcotron or zeeman features can be detected. therefore, there are still many polars lacking field determinations. augustin skopal: how does the sed look like with the unabsorbed supersoft x-rays and dereddened far-uv fluxes? does your unabsorbed x-ray model fit the far-uv fluxes? klaus reinsch: the “source spectrum” of the x-ray components corrected for interstellar absorption is included as the dashed curve in fig. 2. it is two orders of magnitude below the observed flux in the uv. raymundo baptista: you showed doppler tomograms of hα emission from am her in low state by kafka et al. (2010), with side emission apparently from l4 and l5 regions. an alternative explanation for that is zeeman-doppler spliting produced by the magnetic field of the donor star, of the order of a few kg. klaus reinsch: yes, i agree. linda schmidtobreick’s comment: you showed the prominences detected by stella kafka in am her. we detected the same structure in the low state of bb dor which is a non-magnetic vy scl system. so we think it unlikely that the magnetic field of the wd has an influence on this structure and it should rather be explained by a combination of the magnetic field of the secondary plus the roche potential. klaus reinsch: this is indeed interesting to note. in the final remarks of their paper kafka et al. (2010) state that prominence-like structures are likely present in disk cvs above the period gap as well. but their stability and evolution with time is expected to be different. 70 http://dx.doi.org/10.1086/498067 http://dx.doi.org/10.1086/522694 http://dx.doi.org/10.1086/507603 http://dx.doi.org/10.1088/0004-637x/721/2/1714 http://dx.doi.org/10.1086/375684 http://dx.doi.org/10.1088/0004-637x/706/1/130 introduction binary components and spectral energy distribution secondaries in polars circumbinary dust disk stellar activity of the secondary coupling region accretion curtain white dwarf accretion region variability of spectral energy distribution conclusions 60 acta polytechnica ctu proceedings 2(1): 60–65, 2015 60 doi: 10.14311/app.2015.02.0060 on the influence of magnetic field on accretion processes in cvs d. v. bisikalo1, a. g. zhilkin1 1institute of astronomy ras, moscow, russia corresponding author: bisikalo@inasan.ru abstract we consider the influence of such parameters as the value of the proper magnetic field ba and the spin-rotation velocity of the white dwarf on accretion processes in cvs. the results of 3d mhd simulations have shown that the accretion rate is a non-monotonic function of ba: with growing ba it raises in the intermediate polars and decreases in the polars. the maximal accretion rate occurs in the systems, transiting from the stage of intermediate polars to polars; it’s value reaches ∼60% of the initially set mass transfer rate. we have also shown that the acretion rate decreases with the growing spin-rotation velocity of the white dwarf. keywords: cataclysmic variables intermediate polars polars accretion mhd simulations. 1 introduction two main classes of cvs where magnetic field significantly influences accretion processes are the intermediate polars and polars [1]. these are semi-detached binary systems, consisting of a low-mass late type star (donor-star) and a white dwarf (accretor). in the polars, white dwarfs possess strong magnetic fields (ba ≈ 107–108 g on the surface). observations show that no accretion disks form in polars. instead, the material, issuing from the l1 point, forms a collimated stream, that flows onto one of the magnetic poles of the accretor along magnetic field lines[1, 2]. in the intermediate polars, white dwarfs possess relatively weak magnetic fields (ba ≈ 104–106 g on the surface). these systems occupy an intermediate stage between the polars and non-magnetic cvs. we should note that in these systems the spin-rotation periods of the primaries may be significantly shorter than the orbital periods [3]. in our previous works [4, 5] we, by means of 3d mhd simulations, studied the flow structure of the intermediate polars and polars, having various surface magnetic fields of the accretors ba, ranging from 105 to 108 g. this allowed us to investigate conditions of accretion disk formation and to find a criterion, separating two types of the flow, corresponding to the intermediate polars and polars. besides, in [5] we also investigated how the spin-rotation velocity of the accretor influences the mhd flow structure in the system.in this paper we summarize the results of our previous research and show how the accretion rate varies, depending on two parameters as the magnetic induction on the surface of the white dwarf and its spin-rotation velocity. 2 what happens with the flow structure if ba grows to investigate how the value of the accretor’s surface magnetic field influences mhd flow structure in a close binary system we have conducted 7 computational runs with various ba: 105 g (model 1); 5 × 105 g (model 2); 106 g (model 3); 5 × 106 g (model 4); 107 g (model 5); 5 × 107 g (model 6); and 108 g (model 7). we suppose that the accretor’s magnetic field is of dipole type and the axis of the field is inclined with respect to the accretor’s rotation axis by θ = 30◦. for the computations we used our method of investigations of mass transfer processes in semi-detached binary systems where the accretors possess strong magnetic fields [4, 5]. the method is based on the idea that plasma dynamics is determined by the relatively slow average motion of plasma against a background of which very rapid mhd waves propagate. the equations, describing the slow motion of plasma, are derived via a procedure of averaging over the rapidly propagating pulsations. strong external magnetic field in this approach plays a role of an effective liquid interacting with plasma. in the equation of motion the mean electromagnetic force is analogous to the friction force working in multi-component plasma. in our numerical model we take into account processes of the magnetic field diffusion caused by the currents’ dissipation in turbulent vortices and magnetic buoyancy. besides, when averaging the induction equation over the rapidly propagating mhd waves we introduce an additional source of magnetic field dissipation (wave dissipation). in order to see how namely the magnetic induction influences the solution we fix all the other param60 http://dx.doi.org/10.14311/app.2015.02.0060 on the influence of magnetic field on accretion processes in cvs eters. the computations have been conducted for a close binary system, having parameters of the ss cygni (see [6]). the donor-star (red dwarf) in this system has the mass md = 0.56m� and the effective temperature of 4000 k. the accretor (white dwarf) has the mass ma = 0.97m� and the temperature of 37000 k. the orbital period of the system is porb = 6.6 hours and its binary separation is a = 2.05r�. we have supposed that the accretion disk forms in the system for the first time so the accretor’s spin-rotation is synchronous, i.e. pspin = porb. the influence of the accretor’s spinrotation on a formed accretion disk is considered in the next section. the obtained solutions can be divided into two groups. the first group contains models 1, 2, and 3 with relatively weak magnetic fields where accretion disks form. these models correspond to the intermediate polars. in the models of the second group (models 4–7) magnetic fields are strong and there are no accretion disks formed. these models represent the polars. the typical flow structure in the intermediate polars is shown in fig. 1, where we plotted an iso-surface of density logarithm lgρ = −4.5 (in units of ρ(l1)) obtained in the model 1 (ba = 105 g). in figure we also show the magnetic flow lines originating on the accretor’s surface, accretor’s rotation axis (thin straight line) and magnetic axis (bold inclined line). we note that all the gas dynamic structures found in our previous studies [7, 8, 5], including the accretion disk and shock waves exist in the obtained solution. near the accretor the magnetosphere forms and material is accreted via funnel flows. with growing magnetic field the outer radius of the disk significantly decreases. the efficiency of the magnetic breaking and angular momentum transfer increases. the region of the magnetosphere becomes significantly larger. finally, when ba = 106 g (model 3, fig. 2) the accretion disk almost degenerates. the material makes only 1–2 cycles before falling onto the accretor. to describe this flow structure a term ”spiralodisk” is more appropriate, since the velocity distribution in this structure strongly differs from the keplerian. the outer radius of this ”spiralo-disk” is approximately 0.1a and the inner radius is determined by the size of the magnetosphere. a significant part of the ”spiralo-disk” is accretion funnel flows. we can state that this solution is an ultimate case of the intermediate polars. to determine a criterion, separating the intermediate polars and polars let us consider behavior of the gas stream, issuing from the l1 point into the roche lobe of the accretor. taking into account that the gas in the stream moves with supersonic velocity we can consider its behavior using the ballistic approach and omitting the effects of pressure and magnetic field [9, 10]. figure 1: 3d flow structure for the model 1 with ba = 105 g. iso-surface of density (lgρ = −4.5 in units of ρ(l1)) and magnetic field lines are shown. the accretor’s rotation axis is shown by the thin straight line, magnetic axis — by the bold inclined line. figure 2: the same as in fig. 1 for the model 3 with ba = 106 g. figure 3: the same as in fig. 1 for the model 5 with ba = 107 g. 61 d. v. bisikalo, a. g. zhilkin 9 ,1 0 y ea r a m m e & , g a b 9 , 1 0 y ea r m m e & , g a b ,% a m m & & , g a b 9 ,1 0 y ea r a m m e & orb spinp p figure 4: the dependence of the accretion rate ṁa on value of the magnetic field ba (left row) in absolute values (top panel) and in % from the mass transfer rate ṁ (bottom panel). the vertical lines limit the specific amplitudes of the accretion rate variations. in the upper-right panel we show the mass transfer rate as a function of the value of magnetic field. in the lower-right panel we show the mass transfer rate as a function of the accretor’s spin velocity in the model with ba = 105 g. analysis of the trajectories [11] shows that the stream comes very close to the accretor’s surface at a distance rmin. if rmin is larger than the radius of the magnetosphere rm the magnetic field does not strongly influence the motion of material. the stream rounds the star and intersects itself at a certain point. the further evolution of this flow results in the formation of an accretion disk in the system. if rmin is smaller than rm then the magnetic field starts to strongly influence the stream at a certain part of its trajectory. the action of electromagnetic forces in this region slows the stream down and causes loss of the angular momentum. as a result the stream can not round the star and form an accretion disk. thus, the boundary between the intermediate polars (with accretion disks) and polars (no accretion disks) is determined by the relation rm = rmin. if we calculate both the radii using the parameters of the ss cygni we see that this relation is satisfied at ba ≈ 106 g separating the two regimes of the flow. we should note that this estimate of magnetic field induction, separating the intermediate polars and polars, is more or less general for cvs, since the value of q there varies insignificantly. the typical flow structure in the polars is shown in fig. 3, where, like in figures 1 and 2, we plotted an iso-surface of density logarithm lgρ = −4.5 (in units of ρ(l1)) for the model 4 (107 g). in the models 4–7 no accretion disks form and material is accreted via funnel flows. in the models 4 and 5 the stream, starting at l1 point, splits into two flows when approaching the accretor’s surface. then the first flows falls onto the northern magnetic pole of the accretor, the second — onto the southern. with growing magnetic field the difference between the two poles becomes more obvious. in the model 6, for example, only one accretion flow occurs that then ends up at the southern pole. in the model 7 the magnetic field is so strong that it almost entirely controls the flow structure in the roche lobe of the accretor. the field captures material in the immediate vicinity of the inner lagrangian point and, splitting 62 on the influence of magnetic field on accretion processes in cvs it into two flows — more powerful southern and weaker northern, — transports it onto the accretor’s surface along the field lines. let us now consider how the described variations of the flow structure influence the accretion rate. in the upper-left panel of fig. 4 we plot the computed accretion rate ṁa as a function of ba. the vertical lines show specific values of the accretion rate variations. the main feature of this function is that it is non-monotonic. for the values ba < 106 g the accretion rate increases with increasing magnetic field and the amplitude of its variations decreases. at the point ba = 106 g the accretion rate approaches its maximal value. this can be explained by the fact that in the solutions with accretion disks the accretion rate is controlled by processes of angular momentum transfer. the growing magnetic field in intermediate polars makes magnetic breaking more effective and, hence, increases ṁa. after the point of maximum the accretion rate starts to decrease while ba continues to grow. as we have shown above starting at the point ba = 106 g no accretion disk forms in the system and the material is accreted via funnel flows. in this case the accretion rate is determined by the throughput of the stream. when the magnetic field grows the width of the stream decreases and the accretion rate falls. dependence of the accretion efficiency ṁa/ṁ on the induction of magnetic field is shown in the lower-left panel of fig. 4. with growing ba this value increases monotonically. in a transit range of magnetic field values (near ba ≈ 106 g) this dependence has an inflection point. the lowest effectiveness of accretion (30–40%) is approached for intermediate polars with weak magnetic fields. this may be explained by the fact that their disks are large and a portion of material may leave the accretor’s roche lobe and form a common envelope of the binary system [12]. in the polars (with strong magnetic fields) almost all the material, flowing from the l1 point onto the accretor, is accumulated and ”enclosed” in the stream. thus, in such systems the effectiveness of accretion reaches almost 100%. the non-monotonic shape of the ṁa(ba) curve, obtained in our calculations, does not contradict the monotonic character of the dependence of the accretion effectiveness on ba. the point is that the mass transfer rate ṁ also depends on the value of magnetic field. this dependence is shown in the upper-right diagram of fig. 4. in figure one can see that with growing ba the value of ṁ monotonically decreases. in a range of weak fields (ba < 106 g, intermediate polars) this decrease is almost invisible. however in strong fields (ba > 106 g, polars) the value of the mass transfer rate sharply drops (by almost an order of magnitude). this behavior may be explained by the fact that the strong magnetic field of the accretor generates extra-pressure in the vicinity of the l1 point, which prevents the outflow of the material from the donor’s envelope. thus, with growing ba the throughput of the accretion stream decreases. 3 influence of the asynchronous rotation of the white dwarf on the accretion rate the influence of the accretor’s spin-rotation on mhd flow structure in cvs can be characterized by a relation between the radius of the magnetosphere rm and the co-rotation radius rc that is a distance at which the velocity of rotation of the field lines is equal to the rotation velocity of material in the accretion disk. if the accretor rotates relatively slow (rc > rm) then the rotation velocity of the field lines at the boundary of the magnetosphere is lower than the keplerian. so the material, captured by the magnetic field can freely fall onto the accretor’s surface. this regime may be called the ”accretor” regime. when the accretor’s rotation is fast enough (rc < rm) a centrifugal barrier occurs at the boundary of the magnetosphere. this barrier prevents material from free falling onto the surface. this regime we may call the ”propeller”. in systems of ae aqr type the rotation of the white dwarf is so fast that no accretion disk can form. thus, for this regime we can use a term ”super-propeller” [5]. to investigate how the asynchronous rotation of the accretor influences the flow structure in a close binary system we conducted four runs of 3d numerical simulations for the period relation of pspin/porb: 0.1 (”accretor”); 0.033 (”equilibrium rotation”); 0.01 (”propeller”); and 0.001 (”super-propeller”) [5]. to preserve the generality we again use the parameters of the ss cygni. in all the runs the magnetic induction was set equal to 105 g and the magnetic axis is inclined by θ = 30◦. in the models ”accretor” and ”equilibrium rotation” the flow structure is analogous to the model 1, considered in previous section. in the ”propeller” regime, in the inner regions of the disk a magnetospheric cavity forms. its radius is 0.05–0.1a. at the boundary of this cavity the kelvin–helmholtz instability develops. since there is almost no material in the cavity, the accretion rate in the ”propeller” model is close to zero. on the other hand the mass transfer continues and the mass of the disk grows. in the systems with an appropriate combination of parameters (disk mass, value of magnetic field and rotation velocity) the material at the boundary of the cavity at a certain moment can push the magnetosphere down and initiate a short period of accretion. after the exceptional mass has been removed the system returns into the ”propeller” regime. in the ”super-propeller” regime the material, issuing from the inner lagrangian point, is captured by the 63 d. v. bisikalo, a. g. zhilkin rapidly rotating accretor’s magnetosphere, acquires additional angular momentum and gets ejected out of the accretor’s roche lobe. the accretion rate in this case is almost zero. in the lower-right panel of fig. 4 we show dependence of the accretion rate on the parameter porb/pspin that characterizes the spin velocity of the accretor. the data shown are for the case of ba = 105 g. in figure one can see that with the growing accretor’s spin velocity the accretion rate decreases. if the white dwarf rotates relatively slow, which corresponds to the ”accretor” regime, the accretion rate decrease is not significant in comparison with the case of synchronous rotation. however, when the spin velocity overcomes an equilibrium value the system enters the ”¡propeller” regime and the accretion rate sharply drops. in fact, in the ”propeller” and ”super-propeller” regimes the accretion rate is determined by the accretion of material from the common envelope but not of the material, issuing from the inner lagrangian point. 4 conclusions using the results of 3d numerical mhd simulations, we have considered the influence of the magnetic field value ba and the spin-rotation velocity of the white dwarf on accretion processes in cvs. analyzing the results of seven computational runs for models with ba equal to 105 g, 5 × 105 g, 106 g, 5 × 106 g, 107 g, 5 × 107 g and 108 g, we have found that the accretion rate ṁa is a non-monotonic function of ba. in the intermediate polars the growing ba makes the magnetic breaking more effective and, hence, increases ṁa. in the polars, where the accretion rate is determined by the throughput of the funnel flow the accretion rate decreases with growing ba. the maximal value of the accretion rate occurs in the systems at a stage of transit between the intermediate polars and polars. this value is ∼60% of the initially set mass transfer rate. we should note that unlike the absolute value of ṁa the accretion efficiency ṁa/ṁ monotonically increases with the increasing induction of magnetic field. in the polars it approaches the value of almost 100%. this is because the mass transfer rate decreases with growing ba, since strong magnetic field prevents the inflow of material into the accretor’s roche lobe through the inner lagrangian point. analyzing the results of four computational runs of 3d mhd simulations with various values of the period ratio (pspin/porb = 0.1, 0.033, 0.01 0.001) and fixed ba = 105 g we found that the accretion rate decreases with the increasing spin-rotation velocity. it is interesting to note that even in a system, living in the ”propeller” regime, the average accretion rate may be not equal to zero if the combination of such parameters as the disk mass, value of magnetic field and rotation velocity can cause quasi-periodic accretion bursts (falling of the portion of the disk mass onto the accreting star). acknowledgement this work was supported by the basic research program of the presidium of the russian academy of sciences, the russian foundation for basic research research (projects 11-02-00076, 12-02-00047, 13-02-00077, 13-02-00939), the federal targeted program ”science and science education for innovation in russia 2009– 2013”. references [1] warner, b. : 1995, cataclysmic variable stars, cambridge university press, cambridge. doi:10.1017/cbo9780511586491 [2] campbell, c.g. : 1997, magnetohydrodynamics in binary stars, kluwer acad., dordrecht. [3] norton, a.j., , wynn, j.a., somerscales, r.v. : 2004, apj 614, 349. doi:10.1086/423333 [4] zhilkin, a.g., bisikalo, d.v. : 2010, astron. rep. 54, 1063. [5] zhilkin, a.g., bisikalo, d.v., boyarchuk, a.a. : 2012, phys. usp. 55, 115. [6] giovannelli, f., gaudenzi, s., rossi, c., piccioni, a. p.j. : 1983, acta astronomica 33, 319. [7] zhilkin, a.g., bisikalo, d.v. : 2009, astron. rep. 53, 436. [8] zhilkin, a.g., bisikalo, d.v. : 2010, advances in space research 45, 437. doi:10.1016/j.asr.2009.09.006 [9] boyarchuk, a.a., et al. : 2002, mass transfer in close binary stars, taylor & francis, london. [10] fridman, a.m., bisikalo, d.v. : 2008, phys. usp. 51, 551. [11] lubow, s.h., shu, f.h. : 1975, apj 198, 383. doi:10.1086/153614 [12] sytov, a.yu., et al. : 2007, astron. rep. 51, 836. doi:10.1134/s1063772907100083 64 http://dx.doi.org/10.1017/cbo9780511586491 http://dx.doi.org/10.1086/423333 http://dx.doi.org/10.1016/j.asr.2009.09.006 http://dx.doi.org/10.1086/153614 http://dx.doi.org/10.1134/s1063772907100083 on the influence of magnetic field on accretion processes in cvs discussion christian knigge: you seemed to use ss cyg as a prototype of dn intermediate polar, out what is the empirical evidence for this? dmitry bisikalo: we just used ss cyg as a dn illustrative example. the parameters of the ss cyg (components masses, radii, separation, etc.) are quite typical for intermediate polars, so we can consider these numerical results as a good illustration of the flow structure in the intermediate polars. giora shaviv: if i saw right, you do not have radiative transfer, only local energy sinks. how it works when the disk is optically thick? dmitry bisikalo:yes, this approach is strictly applicable for optically thin disks. if you consider optically thick disks it is necessary to add the radiative transfer in some form to the model, and we are working on this. fortunately, we can use the assumption of optically thin disks for a significant sample of cvs. 65 introduction what happens with the flow structure if ba grows influence of the asynchronous rotation of the white dwarf on the accretion rate conclusions acta polytechnica ctu proceedings doi:10.14311/app.2016.5.0026 acta polytechnica ctu proceedings 5:26–28, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app traffic management system in terms of data exchange dušan kamenický czech technical university in prague, faculty of transportation sciences, department of transport telematics, konviktská 20, prague, czech republic correspondence: kamendus@fd.cvut.cz abstract. prediction of train running and it support of conflict resolution decision for an efficient use of the existing railway infrastructure is needed. to meet these requirements standardized interfaces between infrastructure managers and railway undertakings and infrastructure description are indispensable. keywords: technical specification for interoperability, infrastructure description, traffic planning, dispatching, train controlling, telematics applications, railml, railtopomodel. 1. introduction with the increasing demand for freight and passenger transport railway subjects aims on increasing the capacity by a reduction of delays and improved traffic fluidity. to meet these requirements modern traffic management systems are implemented. they are based on a prediction of train running and automatic conflict resolution. standardized interfaces shall ensure the needs of the railway undertakings, infrastructure managements and customers of different european countries in traffic planning, dispatching and train control. directive 2008/57/ec of the european parliament and of the council of 17 june 2008 on the interoperability of the rail system within the community defines in annex ii infrastructure, energy, control-command and signaling and rolling stock as structural subsystems of the rail system, and traffic operation and management, telematics applications for passenger and freight services as a functional subsystem of the rail system. specifications are drafted by the european railway agency and adopted in a decision by the european commission, to ensure the interoperability of trans-european rail system. the paper describes data exchange with focus on the operational management. 2. architecture of management process railway management process can be divided into three basic layers: traffic planning, dispatching and train controlling. traffic planning can be characterized as conceptual planning, strategic network development, service planning and infrastructure planning in long term, timetabling in short term. timetabling is a process concerning transport demand by customer and path requests and allocation by railway undertakings and infrastructure managers [1]. traffic planning is influenced by transport demands, infrastructure parameters, rolling stocks parameters and path fees. traffic planning shall define rules, like priorities of the train and competence between railway undertakings and infrastructure managers. the aim of dispatching is at close approximation to scheduled state, from which railway system has been deflected by external influences. it support is necessary in dispatcher decision processes [2]. quality and timeliness of information is necessary condition the dispatcher could correctly decide the intervention, which leads to fulfillment of the planned timetable. infrastructure manager dispatcher is responsible for changing train sequences to minimalize deviations from the timetable. railway undertaking dispatcher is responsible for skipping a commercial stop, breaking a connection, providing rolling stock and staff. major incidents forcing those decisions like rolling stock or infrastructural failures with a following adaptation of the timetable require a close communication between infrastructure manager and railway undertaking. train controlling is process train route setting, shunting route managing and setting, infrastructure elements controlling to ensure railway safety. routine processes can be performed by automatic train route setting system. automatic train control system, which is designed to eliminate human error, can be supplemented by automatic train operation system or driver advisory system. a train movement is adjusted to achieve defined points of infrastructure in defined time slot and therefore to reduce energy consumption and increase the capacity at a time. 3. standardized interfaces technical parameters of infrastructure elements, like line layout, track parameters, switches and crossings, 26 http://dx.doi.org/10.14311/app.2016.5.0026 http://ojs.cvut.cz/ojs/index.php/app vol. 5/2016 traffic management system in terms of data exchange platforms etc. are defined by 1299/2014/eu "technical specifications for relating to the infrastructure subsystem of the rail system in the european union" [3]. with exception of the requirements for infrastructure register, infrastructure description, methodology of representation or the storage of infrastructure data are not defined. infrastructure register is defined by 2014/880/eu "specifications of the register of railway infrastructure" [4]. this specification concerns data about the infrastructure structural subsystem the energy structural subsystem, and the trackside control-command and signaling subsystem. railway network shall be subdivided into sections of line and operation points. section of line means the part of line between adjacent operational points and may consist of several tracks. operational point means any location for train service operations, where train services may begin and end or change route and where passenger or freight services may be provided [5]. the structural subsystems specific requirements that interoperable railway lines and rolling stock must meet and many of these requirements must be stored in the infrastructure registers and the register of rolling stock. comparing those registers should make it clear which lines accept which rail vehicles. telematics applications for passenger and freight services subsystem equipment are defined by 2006/62/es "technical specification for interoperability relating to the telematics applications for freight subsystem of the trans-european conventional rail system" (tsi taf) [6] and 2011/454/es "technical specification for interoperability relating to the subsystem telematics applications for passenger services of the transeuropean rail system" (tsi tap) [7]. the specifications relating to telematics applications define architecture of information system and interfaces among subjects: infrastructure manager, railway undertaking and customer. processes and data exchanges to allocating of train path and monitoring train movement are defined. fundamental processes are: • train path request – path departure point, path departure time, path destination point, command and control system including on-board radio equipment, train weight and length, braking system and braking performance, maximum speed, rid numbers relating to any dangerous goods, information concerning exceptional gauging etc., • train composition message – for the preparation of the train, railway undertaking must have access to the infrastructure restriction notice, to technical wagon data (rolling stock reference database), to the dangerous goods reference file and to current updated information status on the wagons (the wagon and intermodal unit operation database), • train ready – message must be sent to indicating, that train is ready for departure, • train running information and train running forecast. interface between telematics applications and subsystem "control-command and signaling" is not specified, although interlocking equipment need data on the parameters of the trains. interface between telematics applications and subsystem "infrastructure" is given with the train path data definition and via the infrastructure restriction notice database. interface between telematics applications and subsystem "rolling stocks" is only given via the rolling stock reference database. the procedures enabling a coherent operation of various structural subsystems during both normal and degraded operation are defined by 2015/995/eu "technical specification for interoperability relating to the operational and traffic management subsystem of the rail system in the european union" [8]. from the viewpoint of the data exchange, relevant is requirement of route book and timetables. the development of the route book is the responsibility of ru and should be prepared in the language of the railway undertaking. however, the format of the route book is not specified. each train must be identified by a train running number. the train running number is given by the infrastructure manager when allocating a train path. the train running number format is defined in commission decision 2012/88/eu. interfaces among different railway it applications weren’t specified. the railml.org initiative was founded in 2002 in order to create an interface to enable heterogeneous railway applications to communicate with each other [9]. the result has been the development of the railway markup language railmlwhich delivers a universally applicable data exchange format. the railml standard has been developed by infrastructure managers, railway undertakings, software and consulting firms and academic institutions from number of countries. the railml specification contains subschemas for four main areas: infrastructure, timetable, rolling stock and interlocking. railml can be seen as a direct use case of the railtopomodel. the railtopomodel is a logical object model to standardize the representation of railway infrastructurerelated data [10]. on the other side, railtopomodel will become international railway standard (irs) in spring 2016, compiled by uic, the largest railway organization worldwide. sncf réseau has worked since 2011 to develop its global model for railways business objects, ariane model, based on the same principles as railtopomodel. ariane model now covers the description of all functional objects and properties of the network, at track and lines levels, including topology, referencing and topography, routes description and signaling. on 2016-2017 catenary and power supply network, and finalization of rolling stock will be added. 27 dušan kamenický acta polytechnica ctu proceedings 4. coclusion technical specification for interoperability defines technical requirements of infrastructure, energy and rolling stocks parameters and control-command and signaling system to enable interoperable vehicle driving on interoperable infrastructure. necessary data exchange relating to path allocation and operation and management processes relating to ensure safety are defined in function subsystems. however, data exchange relating to dispatching is not standardized. infrastructure description, specified in infrastructure register, is not sufficient for prediction of train running. data exchange relating to train parameters, like traction characteristics, and timetable requirements is not specified. infrastructure managers and railway undertakings interface ensuring dynamic data exchange relating to breaking a connection is not defined in technical specification for interoperability. railml seems to become effective tool for data exchange supporting prediction of train running and conflict resolution decision among others. references [1] birgit jaekel, thomas albrecht. operational railway management as part of an integrated railway management process, 2014. euro žel, žilina. [2] d. kamenický. optimalizační algoritmy pro systémy řízení a zabezpečení železniční dopravy, studie k disertační práci, 2015. čvut v praze, fakulta dopravní, praha. [3] 1299/2014/eu ”technical specifications for relating to the infrastructure subsystem of the rail system in the european union”. [4] 2014/880/eu ”specifications of the register of railway infrastructure”. [5] j. barnet. rail infrastructure informational description, master thesis, 2011. ctu in prague, faculty of transportation sciences, prague. [6] 2006/62/es ”technical specification for interoperability relating to the telematics applications for freight subsystem of the trans-european conventional rail system”. [7] 2011/454/es ”technical specification for interoperability relating to the subsystem telematics applications for passenger services of the trans-european rail system”. [8] 2015/995/eu ”technical specification for interoperability relating to the operational and traffic management subsystem of the rail system in the european union”. [9] railml website [online]. [2016-01-25], http://www.railml.org/en/. [10] railtopomodel website [online]. [2016-01-25], http://www.railtopomodel.org/en/. 28 http://www.railml.org/en/ http://www.railtopomodel.org/en/ acta polytechnica ctu proceedings 5:26–28, 2016 1 introduction 2 architecture of management process 3 standardized interfaces 4 coclusion references untitled vol. 5/2016 scientific student conference interoperability of railway transport iricon 2016 may 4, 2016 prague, czech republic organised by: faculty of transportation sciences czech technical university in prague sponsored by: internal grant agency ctu svk 46/16/f6 guest editors: jitka jírová (faculty of transportation sciences, czech technical university in prague) jitka řezníčková (faculty of transportation sciences, czech technical university in prague) local organizing comittee: vít fábera tomáš brandejský jitka jírová dušan kamenický petr koutecký jitka řezníčková jan zelenka scientific comittee: tomáš brandejský (faculty of transportation sciences, czech technical university in prague) pavel hrubeš (faculty of transportation sciences, czech technical university in prague) josef jíra (faculty of transportation sciences, czech technical university in prague) zdeněk kaufmann (tp iži — technology platform, interoperability of railway infrastructure) martin leso (faculty of transportation sciences, czech technical university in prague) jiří masopust (faculty of electrical engineering, university of west bohemia) petr nachtigall (jan perner transport faculty, university of pardubice) otto plášek (faculty of civil engineering, brno university of technology) jindřich sadil (faculty of transportation sciences, czech technical university in prague) richard svoboda (brno university of technology, faculty of civil engineering) jaroslav vašátko (railway research institute, j.s.c., prague) martina vitteková (faculty of transportation sciences, czech technical university in prague) iii acta polytechnica ctu proceedings book title: scientific student conference interoperability of railway transport — iricon 2016. series title: acta polytechnica ctu proceedings. volume: 5. date of issue: october 15, 2016. published by: czech technical university in prague, zikova 4, 166 36 praha 6 – dejvice, czech republic. ič: 68407700. editorial office: ctu — central library, technická 6, 160 80 praha 6, czech republic. acta@cvut.cz . head of the editorial board: zbyněk škvor (ctu in prague, czech republic). editor-in-chief: iva adlerová (ctu in prague, czech republic). editorial board: robin arthur healey (rectorate of ctu in prague, dept. of external affairs, ctu in prague, czech republic), taťána jarošíková (faculty of biomedical engineering, dept. of natural sciences, ctu in prague, czech republic), milan jirásek (faculty of civil engineering, dept. of mechanics, ctu in prague, czech republic), jitka jírová (faculty of transportation sciences, dept. of mechanics and materials, ctu in prague, czech republic), petr jizba (faculty of nuclear sciences and physical engineering, dept. of physics, ctu in prague, czech republic), pavel kalina (faculty of architecture, dept. of theory and history of architecture, ctu in prague, czech republic), zuzana masáková (faculty of nuclear sciences and physical engineering, dept. of mathematics, ctu in prague, czech republic), jan píchal (faculty of electrical engineering, dept. of physics, ctu in prague, czech republic), miroslav sýkora (klokner institute, dept. of structural reliability, ctu in prague, czech republic), radek šulc (faculty of mechanical engineering, dept. of process engineering, ctu in prague, czech republic). graphic design and typesetting: tomáš hejda (faculty of chemical engineering, dept. of mathematics, university of chemistry and technology prague), jan řezníček (faculty of information technology, ctu in prague, czech republic), j. jílek (ctu in prague, czech republic). available on-line at http://ojs.cvut.cz/ojs/index.php/app each article is assigned a digital object identifier doi:10.14311/app.2016.5.〈4-digit article page number〉 issn 2336-5382 isbn 978-80-01-06022-3 (1st edition) © czech technical university in prague, 2016. reprinting is allowed only with the agreement of the editorial office and with citation of source. iv vol. 5/2016 preface the papers of the scientific student conference interoperability of railway transport – iricon 2016 are concerning new results coming from the project interoperability of railway infrastructure competence network (iricon) which was coordinated by technical university in brno in collaboration with the technological platform "interoperability of railway infrastructure" and was closed in 2015. the project was supported by the operational programme of the ministry of education, youth and sports – education for competitiveness under the priority axis – tertiary education, research and development. the aim of the project was to improve the quality of human resources for research and development and improve training of target groups, consist of students and young professionals in the field of interoperability of railway infrastructure. necessity of the project was supported by the research interests of students and academic staff of technical universities and research institutes. the project enables to involve young experts in advisory groups for members of the governing organs of the european network interoperability, which was established for the preparation and implementation of the interoperability of the european rail system. the project has set up expert groups called the mirror groups, which reflect the activities of the trans-european rail networks in the areas of: (i) infrastructure, (ii) management and safety, (iii) international railway research board, (iv) energy, (v) system solutions and (vi) research. preparing members of the target groups took the form of: (i) traineeships for young researchers at foreign universities or at european institutes aimed in railway interoperability (ii) organizing workshops and training sessions with the participation of domestic and foreign experts, (iii) participation in international conferences on railway transport, (iv) fellowships at leading foreign railway sites, (v) workshops aimed at exchanging the latest information about news in railway transport and (vi) additional training focused on project management in the field of railway research. besides the aforementioned activities there was created portfolio of complementary activities for the target groups aimed at transfer of technology and improving knowledge in the field of control and legislation in the field of research and development and for evaluation of scientific results. the aim of our conference is to exchange knowledge and connections of scientific and technical potential of universities, research and design institutes together with professional potential of construction and manufacturing companies to promote innovation in rail services in accordance with the requirements of technical specifications for interoperability trans-european rail system in subsystems of infrastructure, energy and management and safety. an important aim of the conference is also to contribute to higher education and professional qualifications of future graduates master and doctoral studies, which will enable them to participate on the management, coordination and other activities in the area of interoperability of the european rail system. otto plášek for the scientific comittee v 303 acta polytechnica ctu proceedings 1(1): 303–306, 2014 303 doi: 10.14311/app.2014.01.0303 atmosphere-space interactions monitor (asim): state of the art pere blay1, lola sabau-graziati2, vı́ctor reglero1, paul h. connell1, juana m. rodrigo1, juan m. macián1, josé t. biosca1, chris eyles1 1ipl, university of valencia, valencia, spain 2inta, madrid, spain corresponding author: pere.blay@uv.es abstract atmosphere-space interactions monitor (asim) mission is an esa payload which will be installed in the columbus module of the international space station (iss). asim is optimized to the observation and monitoring of luminescent phenomena in the upper atmosphere, the so called transient luminous event (tles) and terrestrial gamma ray flashes (tgfs). both tles and tgfs have been discovered recently (past two decades) and opened a new field of research in high energetic phenomena in the atmosphere. we will review the capabilities of asim and how it will help researchers to gain deeper knowledge of tgfs, tles, their inter-relationship and how they are linked to severe thunderstorms and the phenomena of lightning. keywords: space instrumentation atmosphere physics thunderstorms lightning high energy radiation. 1 introduction an increasing number of luminous phenomena related to lightning and severe thunderstorms have been discovered in the last decades. on the one hand, the transient luminous events (tles) are luminous phenomena produced at the stratosphere and mesosphere. tles studies were pushed forward with the advent of high speed cameras (capable of several tens of frames per second, see, e.g. franz et al. 1990). more recently, with very high speed cameras (thousands of frames per second, see for example cummer et al. 2006) these events have been very well characterized in terms of evolution and fine structure. on the other hand terrestrial gammaray flashes (tgfs) are very bright high energy atmospheric emissions (x-ray and γ-ray) and were discovered by astrophysical missions in orbit. according to their appearance, tles are classified mainly as blue jets, red sprites or elves. while blue jets and red sprites are directly linked to lightning and are due to air breakdown, elves are generated by electromagnetic pulses which produce ionization at around 90 km of altitude. elves have a typical lifetime of ∼1 millisecond. red sprites are generated at the mesosphere (55-80 km) and last from a few milliseconds to tens of milliseconds. blue jets are upward propagating jets of light from the cloud tops up to ∼37 km, with a velocity of ∼100 km/s and last for a few tens of a second. an schematic cartoon of these phenomena can be seen in fig. 1. with regards to tgfs, first reported detections by the batse team were published by fishman et al. (1994). tgfs are bright outburst of gamma-ray radiation produced in the atmosphere and which can be seen from space-based instruments. tgfs are thought to be produced by bremsstrahlung emission from energetic runaway electrons accelerated by electric fields on top of thunderclouds. the possible connection of tgfs to electron avalanches produced by cosmic-rays in the atmosphere, or a combination of both the cosmic-ray induced electron avalanches and the electrical discharges during lightning, is also a possibility under discussion. tgfs last typically a few hundreds of microseconds and have been observed from 40 kev up to 80 mev. for an up to date review see dwyer et al. 2012. several astrophysical high energy missions, other than batse, have detected tgfs: rhessi (designed to observe high energy emissions from the sun), fermi and agile (both dedicated to the observations of gamma-ray bursts in the universe). fermi team has even performed dedicated observations of the earth atmosphere and designed specific software and data analysis techniques in order to characterize the tgf emission. agile has been specially productive in the field of tgf detection and characterization in the 400 kev30 mev energy range. the agile team has released its own tgf catalogue available online1 (marisaldi et al. 2013). this new filed of atmospheric physics has gained 1http://www.asdc.asi.it/mcaltgfcat 303 http://dx.doi.org/10.14311/app.2014.01.0303 pere blay et al. an increasing attention from atmosphere physicist and high energy astrophysicists, and is being considered seriously by space agencies as a tool to understand atmospheric phenomena related to cloud formation, severe thunderstorms and lightning, and climate changes. in the wake of this new scientific field of research, the atmosphere-space interactions monitor (asim) was conceived as one of the first space missions dedicated and designed specifically for the observation and analysis of tgfs and tles. asim is an esa mission with contributions from spain, denmark, norway, france, italy and poland. figure 1: schematic view of tles associated to the lightning phenomena. 2 the asim mission asim was conceived as a monitoring mission with imaging and spectroscopic capabilities, with the goal to locate tgfs and tles and provide empirical data which will help to understand the nature of these emissions and the possible links between them. although tles are known to be related to lightning in severe thunderstorms, the relationship of tgfs with both of them is up to now only an hypothesis. there is some evidence that points to the relationship between tgfs and lightning, but a clear understanding is still lacking (oostgaard 2013). asim will be located at the nadir looking columbus external payload facility (cepf) on the columbus module of the international space station. asim will continuously monitor the earth atmosphere from an iss altitude of around 400 km. at a global scale, there are approximately 40 lightning flashes per second, as estimated from data taken by the optical transient detector (otd, christian et al. 1996) and lightning imaging sensor (lis, christian et al. 1999), and they are related to changes in the chemistry of the nox molecules in the atmosphere (very determinant for the ozone generation) and are thought of being of great interest for climate change studies (see for example reeve and toumi 2006, and price and rind 2012). for this reason, the observation and monitoring of lightning and related phenomenology has become of great interest for the scientific community. asim will also address this questions and provide for the first time strictly simultaneous optical and high energy data of the phenomenology related to severe thunderstorms. asim science goals will focus on understanding the physics behind tles and tgfs, get a deeper knowledge on how they are related to lightening, and understand their impact on atmospheric processes and possible links to climate determining factors. other science related to high-altitude cloud formation, cloud electrification, nox production, meteors, auroras, etc. will also be in the scope of the mission. 3 the asim instruments the asim payload will consist of two main instruments, the modular x and gamma-ray sensor (mxgs) and the modular multi-spectral imaging array (mmia). fig. 2 shows the location of the instruments on the cepa (columbus external payload adapter) which will be attached to the columbus nadir cepf. figure 2: schematic view of the mxgs and mmia instruments in the cepa. mxgs is a coded mask imaging instrument with two detector layers: one with imaging capabilities (led, low energy detector), operating in the 15−400 kev energy range, and a second layer (hed, high energy detector) sensitive to higher energy photons (200 kev−20 mev), but without imaging capabilities. the optimal 304 atmosphere-space interactions monitor (asim): state of the art energy resolution (10% at 60 kev for the led and 15% at 662 kev for the hed), the good angular location accuracy (0.7◦ for point sources and 2◦ for diffuse sources), and a time resolution bellow 5µs, make from mxgs an ideal instrument to locate tgfs and characterize their emission in terms of duration, shape of the light-curve and their spectral behavior. mxgs will have a field of view of 80◦×80◦, which at zero response becomes 147◦×147◦, i.e., the size of the earth disc as seen from the iss. table 1 summarizes the mxgs capabilities and in fig. 3 a mxgs model is depicted. table 1: summary of mxgs capabilities. led hed collecting area 1024 cm2 900 cm2 energy range 15−400 kev 200 kev−20 mev energy resolution 10% at 60 kev 15% at 662 kev time resolution ≤5 µs ≤5 µs location accuracy 0.7 (point src.) (degrees) 2 (diffuse) fov 80◦×80◦ † †147◦×147◦ at zero response mxgs may be the very first instrument locating tgfs with an error circle of ∼15 km radius, solving for the first time the ambiguities in the tgf association with lightning activity. mxgs will also be capable to observe for the very first time the tgf spectra in a very wide energy range, from 15 kev up to 20 mev. mxgs is also the very first coded mask imaging instrument specially designed to observe high energy atmospheric phenomena. figure 3: schematic view of the mxgs instrument. mmia will consist of 3 photometers and two imaging cameras. the 3 photometers are working in the wavelengths 337 nm, 180−230 nm, 777.4 nm, and the cameras are optimized to work at 337 nm and 777.4 nm, covering altogether from the near uv up to the near ir. the time resolution is 83 ms for the cameras and 0.01−0.1 s for the photometers. the cameras will have an spatial resolution between 0.4 and 0.5 km and both the photometers and the cameras have the same field of view, namely, 61.4◦. mmia will provide invaluable data on the optical emission (as opposed to the high energy emission) from severe thunderstorms. table 2 summarizes the capabilities of mmia and in fig. 4 a model of the instrument is depicted. figure 4: schematic view of the mmia instrument. table 2: summary of mmia capabilities. cameras photometers fov (nadir) 61.4◦ 61.4◦ num. of pixels 1024×1024 −− pixel resolution 0.4−0.5 −− (nadir) (km) time resolution (ms) 83 0.01−0.1 spectral bands 337/5 337/5 (center/width) 777.4/5 777.5/≤5 (nm) 205/50 mxgs and mmia will both work together in their triggering mode, and will be able to send their triggering information to each other. fig. 5 depicts a schematic view of the instruments capabilities and their interconnected cross-triggering system. they will offer the first strictly simultaneous observation of luminous emissions associated to thunderstorm activity. 305 pere blay et al. figure 5: schematic view of the mmia and mxgs configurations, depicting the instruments capabilities and the interconnected cross-triggering. 4 mission status asim mission was approved by esa during 2005. now (2013) the critical design review (cdr) is on going and the manufacturing is expected to start along 2013. the flight model should be ready by the end of 2014 and the launch of the mission is expected by mid-2015. the nominal operational life of the mission is 2 years, with possible extensions. 5 conclusions asim will help the scientific community to solve some of the problems related to tle and tgf formation, a quite recent new filed of atmospheric physics which has been also called high energy atmosphere physics (see dwyer et al. 2012). the capabilities of its instruments and the wavelength coverage will allow the location tgfs with high accuracy and disentangle their links to tles, thunderstorms and lightning. acknowledgement pere blay acknowledges funding from the spanish ministerio de economia y competitividad through project aya-2011-29936-c05. references [1] christian h.j., driscoll k., goodman s.j., blakeslee r.j., mach d., and buechler d. 1996, proc. 10th int. conf. on atmospheric electricity, osaka, japan, icae, 368371 [2] christian h.j., blakeslee r.j., goodman s.j., et al. 1999, proc. 11th int. conf. on atmospheric electricity, guntersville, al, international commission on atmospheric electricity, 746749 [3] cummer, s. a., n. jaugey, j. li, w. a. lyons, t. e. nelson, and e. a. gerken 2006, geophys. res. lett., 33, l04104 doi:10.1029/2005gl024969 [4] dwyer j.r., smith d.m., and cummer s.a. 2012, space sci rev, 173, 133 doi:10.1007/s11214-012-9894-0 [5] fishman g.j., bhat p.n., mallozzi r. et al. 1994, science, 264, 1313 doi:10.1126/science.264.5163.1313 [6] franz r.c., nemzak r.j., and winkler j.r. 1990, science, 249, 4851, 1990 [7] m. marisaldi, f. fuschino1, m. tavani et al. 2013, j. geophys. res. space physics, http://dx.doi.org/10.1002/2013ja019301 [8] n. ostgaard, t. gjesteland, b. e. carlson, a. b. collier, s. a. cummer, g. lu and h. j. christian 2013, geophys. res. lett.,vol. 40, 1-4 doi:10.1029/2012gl054022 306 http://dx.doi.org/10.1029/2005gl024969 http://dx.doi.org/10.1007/s11214-012-9894-0 http://dx.doi.org/10.1126/science.264.5163.1313 http://dx.doi.org/10.1029/2012gl054022 introduction the asim mission the asim instruments mission status conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.11.0043 acta polytechnica ctu proceedings 11:43–48, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app netgraph – an efficient tool for periodic timetabling and capacity planning zdeněk michl∗, michal drábek, rudolf vávra department of logistics and management of transport, faculty of transportation sciences, ctu in prague, czech republic ∗ corresponding author: michlzde@fd.cvut.cz abstract. a netgraph is a graphical representation of a periodic timetable concept for given spatial or modal scope. it adds a third dimension to the network plan – time. despite no strictly prescribed rules, a common practice notation has been settled over time. the authors propose an extension of a netgraph for planning of periodic railway capacity and operation, including related notation rules. keywords: edge, netgraph, node, notation, periodic timetable, periodic capacity. 1. introduction a netgraph, also called interval graphic, is a graphical representation of a periodic (interval) timetable concept of public transport lines in a designated geographical or political territory, for a transport segment or a production unit. it displays at first traffic and transport coherence of the individual lines in transfer nodes and their service function on the territory (number of stops). netgraph was made up of a combination of a network plan, as usually used in urban and local public transport, and a timetable, as used in railway timetabling. while the former reproduces the course of the lines and partially the intervals in the entire network, the latter shows in detail the scheduled traffic on a part of the network (mostly a single railway line). the netgraph adds a third dimension to the two-dimensional network plan – time schedule. thus, in a netgraph, periodic timetable with small to medium intervals in an area can be clearly illustrated. there are no strictly prescribed rules for creation of netgraphs, but over time a common practice notation has been settled. since the level of detail, the purpose of creation and highlighted properties in netgraphs varies, it is always necessary to provide a legend of line (edge) types and colours and time notation used in it. a netgraph may be created as an output of a specialised transport planning software package as german fbs – fahrplanbearbeitungssystem (fbs/iplan) [1], swiss viriato [2] and others, enabling an overview of the constructed lines and connections at a glance for comparison. a basic netgraph can even be constructed using a spreadsheet office suite or another graphic tool. a netgraph consists of following elements: • nodes, including their names, • edges, including the timetable notation for each public transport line and number of stops, • technological processes, • a legend. further, the authors propose an extension of a netgraph for planning of periodic railway capacity and operation. for such purpose, it is necessary to establish rules for notation of passing through defined station at a certain time, for alternative routing of a train path, for a train path for one direction only, and for crossing of the opposite trains on a single-track line. a proposal of related rules is presented and discussed consequently. 2. common practice in netgraph notation there emerged two main producers of netgraphs – irfp. e. k. (institut für regional-und fernverkehrsplanung), and sma und partner ag. both companies provide timetabling software tools. their rules for netgraph notation are mostly equal, except some differences (e.g. as in figure 9 by sma and as in figure 10 by irfp). both companies publish on their websites a short introduction into purpose and notation of a netgraph. irfp uses a term "interval graphic", sma uses "netgraph". the authors of this paper have decided for the term "netgraph" for the sake of brevity. irfp notes that a netgraph displays at least • geographical offer : (public transport) "line network and line management, main railway stations, operated access points per line • temporal offer : interval frequence per line as well as offer density on certain lines through overlap, arrival and departure times of the clocked lines in main railway and intermediate stations, determining of lines and transition periods in the stations • qualitative offer : long-distance traffic and local transport services with regard to the lines, single products or train categories if applicable train operation company, number of train changing per relation" [3] 43 http://dx.doi.org/10.14311/app.2017.11.0043 http://ojs.cvut.cz/ojs/index.php/app z. michl, m. drábek, r. vávra acta polytechnica ctu proceedings sma stresses that "a single line represents each service (and the corresponding journey in the reverse direction) connecting the stations it passes through on its trip, with the arrival and departure times for each station indicated. the repeating aspect of the timetable means that a whole repeating family of trains can be covered by one line on the diagram. the connection times between services at a station can be seen at a glance, giving a powerful method for improving the coordination between services." [4] the notation rules represented below generally come out from both above mentioned netgraph providers. besides fbs/iplan and viriato, some other timetabling software tools, e.g. railsys [5], optitakt [6] and takt [7] can produce netgraphs as well. 2.1. nodes nodes of a netgraph represent important places of a transport network from the passenger’s (user’s) point of view. each node must be named (in full or using an abbreviation – for the recommended place for descriptor see figure 1). optionally, a minimum transfer (connection) time in a node in minutes may be added to the description. node importance category, frequency of service and other attributes may be displayed using different borderline and filling types and colours. a netgraph node depicts a timetable and network node, which is: • station of origin or destination of at least one public transport line (or a part of its services), • transfer (interchange) station to other public transport lines and transport systems, even if they are not included in the netgraph • stations, where splitting or joining of trains or lines or other technology operation regularly takes place, • other important places in the network, such as regional or tariff borders, crossing of trains etc., according to the purpose of creation of the netgraph. 2.2. edges a netgraph edge represents a public transport line (or its branches and joint sections) from the passenger’s point of view. edges of lines passing more nodes are connected through the node boxes. important edge attributes are line style and colour, which depicts the service function and interval of the public transport line. 2.3. edge colour colours are usually used (according to the purpose of creation of the netgraph) for: • transport segment of the line (e.g. train category), • operation periods (e.g. lines operating only on working days, during peak hours etc.). figure 1. a node of a netgraph including name descriptor and the minimum transfer time (5 min). • different transport modes (each mode in another colour), • different train operating companies, public transport authorities etc., where applicable, • in exceptional cases individual lines can be distinguished by the line colour. there is no single correct way to colorize the lines. the selected scheme therefore has always to be explained in the legend next to the netgraph. yet there are common conventions. the authors recommend getting inspired from corresponding use cases. 2.4. edge line style a line style of the edge distinguishes the interval between services of the line. line style can even show public transport lines operated without a fixed interval. generally, one solid line represents one service per period (usually one hour). by convention, the line styles as shown in figure 2 are used. different line styles are used e.g. in urban public transport systems. in each case, the line styles used in a netgraph should always be explained in the legend. 2.5. timetable notation edges representing public transport lines with periodic timetable are complemented with time labels. they indicate periodic arrival and departure times to and from each node, noted only in minutes. the descriptors are usually on the side of travel direction from the edge – on the right in most cases, on the left e.g. for swiss railways. the descriptor closer to a node shows the arrival time, the one further from the node then the departure time respectively, as shown in figure 3. both lines (black and red) operate every hour between a and c. trains of the black line leave a every hour at minute 31 for c. they arrive to b in minute 44 and leave in minute 45, while arriving to c in minute 59. in the opposite direction the trains leave c every hour at minute 1, call at b between minutes 15 and 16 and reach a in minute 29. trains of the red line leaves a every hour at minute 4, does not call at b and arrive to c at minute 27. in the opposite direction the trains of the red line leave c every hour in minute 33, do not call at b and reach a in minute 56. if trains of a public transport line 44 vol. 11/2017 netgraph figure 2. line style usage convention according to the service interval. do not call at the node, the time descriptor is usually omitted also (see the red line at node b in figure 3). in some cases of netgraphs for timetabling or railway capacity planning purpose, it may also be useful to indicate the passage time as departure times. it is then useful to distinguish the nodes where the train calls with dots in the colour of the respective line at intersections of the edge and node borders (see figure 4). this is also useful for lines with fixed stops but non-periodic timetable, where minute descriptors are omitted. in the case of two-hours-interval the descriptor must also indicate the parity of the hour of operation (even or odd). by convention, the minute-descriptor of an even hour is descripted by normal font and that of an odd hour in italics, see figure 5. the public transport line is operated every two hours between a and c. for c it leaves a every even hour at minute 40, arrives at b every odd hour in minute 14, calls until minute 16 and arrives at c every odd hour in minute 59. in the opposite direction, it leaves c every even hour at minute 01, calls at b every even hour in minutes 44 to 46 and reaches a every odd hour in minute 20. alternative resolution of even and odd hours is also possible, e.g. by underscoring the minute descriptor for an odd hour. in the case of public transport lines operated every timetable period (60 minutes), there is no need to distinguish between odd and even hours, see both lines in figure 4. for public transport lines operated more than once a timetable period (with notation as in figure 2), only one minute-descriptor for all trains of the line within a period is provided, other service times of the period are omitted – see figure 6. the public transport line is operated twice an hour (every 30 minutes) between nodes a and c. for c it leaves a every hour in minute 03 and 33, arrives at b every hour in minute 29 and 59, calls there until minute 30 and 00 and arrives at c every hour in minute 58 and 28. in the opposite direction, it leaves c every hour in minute 02 and 32, calls at b every hour in minutes 30 and 00 to 31 and 01 and reaches a every hour in minute 57 and 27. descriptors for the opposite direction are calculated symmetrically along the main timetable axis (as complements to 60 or another timetable period). 2.6. number of serviced stops intermediate stops of a public transport line are shown on the edge between nodes. either each serviced stop is indicated with a solid dot (see figure 7) or grouped in an empty circle with number of grouped stops next to it or in it (see figures 8 and 9). 2.7. branching of a public transport line branching (some trains continue from a node in other direction than the others) is indicated in the node with two connections between the edges, see figure 10. trains arrive from b to a every hour in minute 29. they continue every odd hour in minute 32 for d, and every even hour in minute 32 for c. the situation is similar in the opposite direction. the line style shows the doubled service interval of the branches. 2.8. splitting and joining of trains (units) in this case, each train splits into two parts, and each part continues to a different destination, see figure 11. trains from b arrive in a every hour in minute 28 and split in two parts, one leaving for d every hour in minute 32, the other one continuing to c every hour in minute 35. the situation is similar in the opposite direction. the form of linking of edges in a node can also indicate a u-turn of trains of the public transport line. 3. proposed additional rules for netgraph creation and discussion thereof 3.1. different service routing in each direction in some cases, a route of a public transport line contains sections, where services operate in one direction only. such sections are distinguished with arrows. time descriptors are displayed in particular direction only. in figure 12, the line is from a to f routed through nodes b, c and e, and in the opposite direction through nodes e, d and b. 3.2. alternative routing of freight train paths lindner and von redern [8] found that it was necessary to let periodic time windows ("canals") free for freight 45 z. michl, m. drábek, r. vávra acta polytechnica ctu proceedings figure 3. example of timetable descriptors. figure 4. extended timetable descriptors example. serviced nodes are distinguished with dots of respective colour of the line. figure 5. extended timetable descriptors example – 2h interval with odd hour distinguished. figure 6. extended timetable descriptors example – 30 min interval. figure 7. three serviced intermediate stops between nodes a and b, each one indicated separately with a solid dot. 46 vol. 11/2017 netgraph figure 8. five intermediate stops between nodes a and b, the number of grouped stops is indicated with a numeric descriptor next to an empty circle. figure 9. five intermediate stops between nodes a and b, the number of grouped stops is indicated with a numeric descriptor in an empty circle. trains. these should be wide enough for required number of freight train paths per hour. these time windows should be preferably connected in nodes (if needed, among more than two railway lines to enable use by freight trains with various origin/destination stations). in the case of insufficient capacity, the authors proposed reviewing the structure of passenger transport offer. this idea was further worked up by drábek [9], who proposed a concept of network-bound periodic freight train paths with possible alternative routing in node station. this concept is, to a certain extent, an analogy to integrated periodic timetable (ipt) in passenger transport. ipt is a network-wide, periodic offer of services and transfer connections between them. the concept of network-bound periodic freight train paths is a network-wide periodic offer of capacity that meets various requirements of freight train operating companies. unified period and unified (zero) symmetry are maintained in this concept as well. alternative routing through nodes represents an analogy to transfer connection in ipt. this alternative routing is illustrated in figure 13. the train paths from b through a are routed alternatively in the direction of c and d. a freight train can pass through node a (without stop) in minute 32, either in direction c or d. in the opposite direction, a freight train can pass through node a in minute 31, either from direction c or d. 3.3. train crossing on a single-track line for planning of periodic capacity of single-track lines, a key information is in which stations the trains in opposite directions periodically cross (meet) each other – at present day, or in a certain planning time horizon. in the case of ipt, a unified axis (minute) of symmetry is kept, and the crossing happens (at least approximately) in symmetry time. in europe, a convention on zero symmetry is kept. due to mathematical prefigure 10. branching of a public transport line into two directions. figure 11. splitting and joining of trains (units). conditions of ipt, two groups of nodes with symmetry time always occur – for instance, for 60 min interval, zero symmetry means one group of nodes (stations) with symmetry time in minute 00, and another group of nodes with symmetry time in minute 30. necessity of displaying time descriptors in such symmetrical crossing stations depends on level of detail for the capacity planning. for timetabling purposes, the descriptors are necessary for information about (real or required) scheduled running time between neighbouring symmetry nodes. for conceptual planning, name of the node station may be sufficient, as such symmetrical crossing stations change only after implementation of a new ipt-stage (shortening of travel times). figure 14 shows, beyond a "common" netgraph, depiction of periodic crossing of fast train in station katovice. as this crossing is not connected with a commercial stop and the netgraph serves for conceptual level of detail only, time descriptors for katovice are omitted. 3.4. discussion besides timetable concept elaboration and presentation, netgraphs can be used for railway capacity planning as well. the authors further propose additional rules to address various aspects of railway capacity planning. in many cases, the meaning of an edge, displayed in a netgraph, shifts from periodic service to periodic capacity, which may (fully or partially), or may not, be really used by a train (service). 47 z. michl, m. drábek, r. vávra acta polytechnica ctu proceedings figure 12. operation of a public transport line in a certain direction only. figure 13. alternative routing of freight trains (alternative train paths – from a either to c or d). figure 14. example of descriptor of a crossing station (zero symmetry) [10]. 4. conclusions a netgraph is a very useful tool not only for public transport (mostly railway) timetable conceptual planning. for periodic railway capacity planning (either periodic passenger service with half interval during the peak hours, or periodic capacity for freight trains, even with alternative routing). netgraph cannot replace classical timetabling tools, but can enable an easy and rapid overview for network capacity planning. for codification of necessary descriptors of symmetrical periodic crossing in terms of group of symmetry nodes, all-day or peak only incidence and planning horizon, further research is needed. references [1] irfp e.k. institut für regional-und fernverkehrsplanung. our product: the timetable construction system fbs [online]. [cit. 2017-03-24] "http://irfp.de/our-product-fbs.html". [2] s. und partner ag: viriato, zlr. the versatile timetable system [online]. [cit. 2017-03-23] "http://www.sma-partner.com/en/solutions/viriatoand-zlr/overview". [3] irfp e.k. institut für regional-und fernverkehrsplanung. timetable creation [online]. [cit. 2017-03-23] "http://irfp.de/timetable-creation.html". [4] s. und partner ag: viriato, zlr. netgraph. focussing on service [online]. [cit. 2017-03-23] "http://www.sma-partner.com/en/solutions/viriatoand-zlr/functionality/netgraph". [5] r. m. c. gmbh. railsys [online]. [cit. 2017-03-17] "http://www.rmcon.de/railsys-en/". [6] w. h. et al. optitakt [online]. [cit. 2017-03-24] "http://www.optitakt.de/". [7] c. o. t. f. s. u dresden. timetabling [online]. [cit. 2017-03-23] "https://tudresden.de/bu/verkehr/ila/vkstrl/forschung/ forschungsfelder/fahrplanung?set_language=en". [8] h.-r. lindner, h. von redern. güterzüge im taktfahrplan – möglichkeiten und grenzen. die bundesbahn 10/1989. [9] m. drábek. periodic freight train paths in network. doctoral thesis, 2014. "http://takt.fd.cvut.cz/cargo/drabek_thesis.pdf". [10] m. drábek. netgraphs of regional railway public service in chosen czech regions. ctu in prague, undated. unpublished. 48 acta polytechnica ctu proceedings 11:43–48, 2017 1 introduction 2 common practice in netgraph notation 2.1 nodes 2.2 edges 2.3 edge colour 2.4 edge line style 2.5 timetable notation 2.6 number of serviced stops 2.7 branching of a public transport line 2.8 splitting and joining of trains (units) 3 proposed additional rules for netgraph creation and discussion thereof 3.1 different service routing in each direction 3.2 alternative routing of freight train paths 3.3 train crossing on a single-track line 3.4 discussion 4 conclusions references 251 acta polytechnica ctu proceedings 1(1): 251–254, 2014 251 doi: 10.14311/app.2014.01.0251 testing f (r)-theories by binary pulsars mariafelicia de laurentis1,2, ivan de martino2,3 1dipartimento di scienze fisiche, università di napoli ”federico ii” 2infn sez. di napoli compl. univ. di monte s. angelo, edificio g, via cinthia, i-80126 napoli, italy 3departamento de fisica teorica, universidad de salamanca, 37008 salamanca, spain corresponding author: felicia@na.infn.it abstract using the post-keplerian parameters to obtain, in the minkowskian limit we obtain constraints on f(r)-theories of gravity from the first time derivative of the orbital period of a sample of binary stars. in the approximation in which the theory is taylor expandable, we can estimate the parameters of an an analytic f(r)-theory, and fulfilling the gap between the general relativity prediction and the one cames from observation, we show that the theory is not ruled out. keywords: gravitation binary pulsar systems f(r)-theories gravitational waves. 1 introduction astrophysical systems like neutron stars (ns), coalescing binary systems, black holes (bhs), and white dwarfs (wds), are the most promising to study the gravitational waves (gws) emision. indeed, studying the binary system b1913+16, known as the hulsetaylor binary pulsar, the first time derivative of the orbital period was measured to be different from zero [13, 18], as predicted by general relativity (gr) when gravitational radiation is emitted. this measurements was confirmed by study in other relativistic binary systems. the agreement between gr and the observation is at the order of ∼ 1%. however, using the extended theories of gravity (etg) it should be possibile to explain the observational results as shown in [10, 12] where, starting from a class of analytic f(r)-theories it is possible evaluate the first time derivative of the orbital period and compare it with the data. this approach permit both to test the etgs both to explain the gap between observation and the theoretical prediction. this paper was organized as follow: in sec. 1 we calculate the quadrupole emission for an analytic f(r)-lagrangian using the weak-field limit; in sec 2 we compare the theoretical prediction with the observed data. finally in sec 3 we give our conclusions and remarks. 2 the first time derivative of the orbital period in the f(r)-theories the simplest extension to gr is the f(r)-gravity, in which, the lagrangian is an arbitrary function of ricci scalar [2]. starting from the field equations in f(r)gravity (for details see [2, 16, 4, 5]) f ′(r)rµν − f(r) 2 gµν − f ′(r);µν + +gµν�gf ′(r) = x 2 tµν , (1) 3�f ′(r) + f ′(r)r− 2f(r) = x 2 t , (2) where tµν = −2√ −g δ( √ −glm) δgµν is the energy momentum tensor of matter (t is the trace), x = 16πg c4 is the coupling, f ′(r) = df(r) dr , �g = ;σ ;σ, and � = ,σ ,σ. it is possibile, in the minkowskian approximation of an analytic f(r)-lagrangian1, f(r) = ∑ n fn(r0) n! (r−r0)n ' ' f0 + f ′0r+ f ′′0 2 r2 + ... (3) to compute the quadrupole emission due to gws [10, 11]. furthermore, it is possible calculate the energy 1for convenience we will use f instead of f(r). all considerations are developed here in metric formalism. from now on we assume physical units g = c = 1. 251 http://dx.doi.org/10.14311/app.2014.01.0251 mariafelicia de laurentis, ivan de martino momentum tensor of gravitational field in f(r)-gravity that assumes the following form tλα = f ′0k λkα ( ḣρσḣρσ ) ︸ ︷︷ ︸ gr − 1 2 f ′′0 δ λ α ( kρkσḧ ρσ )2 ︸ ︷︷ ︸ f(r) . (4) to be more precise, the first term, depending on the choice of the constant f ′0, is the standard gr term, the second is the f(r) contribution. it is worth noticing that the order of derivative is increased of two degrees consistently to the fact that f(r)-gravity is of fourthorder in the metric approach [10]. in this contest, we can write the total average flux of energy due to the gws integrating over all possible directions as 〈 de dt 〉 ︸ ︷︷ ︸ (total) = g 60 〈 f ′0 (... q ij ... qij ) ︸ ︷︷ ︸ gr − f ′′0 (.... q ij .... q ij ) ︸ ︷︷ ︸ f(r) 〉 , (5) where we point out that for f ′′0 → 0 and f ′0 → 4 3 , the previous equation becomes 〈 de dt 〉 ︸ ︷︷ ︸ (gr) = g 45 〈... q ij ... qij 〉 , (6) that is the prediction of gr [14, 17]. in order to evaluate the above expressions for the flux it is necessary to form explicit expressions for 〈... q ij ... qij 〉 and〈.... q ij .... q ij 〉 for the system under consideration. for our purposes we consider a binary pulsar system. if we assume a keplerian motion of the stars in the binary system, wherewe mp is the pulsar mass, mc the companion mass, and µ = mcmp mc +mp is the reduced mass, it is possible to compute the time average of the radiated power computing the first time derivative of the orbital period [11] ṗb = − 3 20 ( t 2π )− 5 3 µg 5 3 (mc +mp) 2 3 c5(1− ε2) 7 2 × × [ f ′0 ( 37ε4 + 292ε2 + 96 ) − f ′′0 π 2t−1 2(1 + ε2)3 × × ( 891ε8 + 28016ε6 + 43520ε2 + 3072 )] , (7) where ε is the orbital eccentricity and t is the orbital period of the binary. 3 methodology and data analysis knowing exactly the lagrangian that describes the system, we can predict the orbital period decay, however,we want understand how well the relativistic binary systems can fix bounds on f(r) parameters using eq. (7), and getting an estimation of the second derivative of the lagrangian with respect to ricci scalar, f ′′0 . we use the following prescription, the difference between the first derivative of the binary observed period variation (ṫbobs ± δ) and the theorethical one obtained by gr, ∆ṫb = ṫbobs − ṫgr, is fulfilled imposing that: ṫbobs − ṫgr − f ′′0 ṫbf(r) = 0, (8) ṫbobs ± δ − ṫgr − f ′′0±δ ṫbf(r) = 0, (9) where δ is the experimental error, that we propagate on the ṫbobs , into an uncertainty on f ′′0±δ . in this way, the extra contribution to the loss of energy due to the emission of gws radiation in the etgs regime can provide to fill the difference between theory and observations. we select a sample of observed relativistic binary pulsars (see their references reported in tab. 1 of [11]) for which we compute the correction ṫbf(r) , the difference ∆ṫgr between ṫbobs and ṫgr (equal to the correction −f ′′0 ṫbf(r) ), the corresponding f ′′0 solution of (8), the interval centered on f ′′0 and finally, the interval centered on f ′′0 and computed from the difference: f ′′0+δ −f ′′0−δ 2 , all results are reported in tab. 1. in fig. 1 we show, for sake of convenience, in logarithmic scale, the absolute values of f ′′0 reported in tab.1 versus the ratio ṫbobs ṫgr . there are six binaries in tables, for which the etgs are not ruled out 0.04 ≤ f ′′0 ≤ 38, getting 0.5 ≤ ṫbobs ṫgr ≤ 1.5. for those systems the difference between ṫgr and ṫbobs can be explained adding an extra contribution that comes out from the f(r)-thoery. instead for most of binaries we have f ′′0 values that can surely rule out the theory, since taking account of the weak field assumption we obtain 38 ≤ f ′′0 ≤ 4 × 107. from this last values to the first ones, there is a jump of about four up to five order of magnitude on f ′′0 . the origin of these strong discrepancies, perhaps, is due to the extreme assumption we made, to justify the difference between the observed ṫbobs and the predicted ṫgr using the etgs. 252 testing f(r)-theories by binary pulsars table 1: upper limits of f ′′0 correction to ṫgr of binary relativistic pulsars assuming that all the loss of energy is caused by gravitational wave emission. we reported the j-name of the system,the difference ∆ṫgr between ṫbobs and ṫgr equal to the correction −f ′′0 ṫbf(r) , the correction ṫbf(r) , the corresponding f ′′0 solution of (8), the interval centered on f ′′0 and computed from the difference f ′′0+δ −f ′′0−δ 2 ,where f ′′0±δ ,are the corresponding solutions of ( 8) taking account of the experimental errors ±δ on the observed orbital period variation ṫbobs . name ∆ṫgr ṫbf(r) f ′′0 ±∆f ′′0 j2129+1210c -2.17e-14 6.01e-13 3.61e-02 8.32e-02 j1915+1606 -2.04e-14 2.10e-13 9.74e-02 4.77e-03 j0737-3039a -4.23e-15 1.86e-14 2.28e-01 9.15e-02 j1141-6545 -1.65e-14 3.88e-15 4.25e+00 6.44e+00 j1537+1155 5.39e-14 1.42e-15 -3.79e+01 7.03e-02 j1738+0333 -1.56e-15 1.06e-16 -1.47e+01 2.92e+01 j0751+1807 1.41e-13 8.98e-16 -15.7e+01 1.002e+01 j0024-7204j -5.22e-13 3.13e-16 1.67e+03 4.15e+02 j1701-3006b -5.03e-12 8.81e-16 5.71e+03 7.04e+01 j2051-0827 -1.55e-11 4.77e-16 3.24e+04 1.68e+03 j1909-3744 -5.47e-13 2.62e-18 2.09e+05 1.14e+04 j1518+4904 2.41e-13 3.42e-19 -7.05e+05 6.43e+03 j1959+2048 1.47e-11 1.07e-17 -1.38e+06 7.51e+04 j2145-0750 4.01e-13 1.00e-19 -4.00e+06 2.99e+06 j0437-4715 1.59e-13 1.04e-19 -1.57e+06 2.73e+06 j0045-7319 3.02e-07 1.11e-16 2.74e+9 8.13e+07 j2019+2425 -3.00e-11 1.11e-22 2.71e+11 5.41e+11 j1623-2631 4.00e-10 2.02e-23 -1.98e+13 2.97e+13 4 discussion and remarks in this paper, we develop expressions for quadrupole gravitational radiation in f(r)-gravity theory using the weak field technique and apply these results, which are applicable in general, to a sample of a binary pulsars, though their orbits are eccentric. here, we seen that, where the gr theory is not enough to explain the gap between the data and the theoretical estimation of the orbital decay, there is the possibility to extend the gr theory with a generic f(r)theory to cover the gap. according to eq. (7),we have selected a sample of relativistic binary systems for which the first derivative of the orbital period is observed, we have computed the theoretical quadrupole radiation rate, and finally we have compared it to binary system observations. from tab. 1, it is seen that the first five systems have masses determined in a manner quite reliable, while for the remaining sample, masses are estimated by requiring that the mass of the pulsar is 1.4m� and, assuming for the orbital inclination one of the usual statistical values (i = 60◦ or i = 90◦ ), and from here comes then the estimate of the mass of the companion star. so a primary cause of major discrepancies, not only for the etgs, but also for the gr theory, between the variation of the observed orbital period and the predicted effect of emission of gravitational waves, could be a mistake in the estimation of the masses of the system. in addition, other causes may be attributable to the evolutionary state of the system, which, for instance, if it does not consist of two neutron stars may transfer mass from companion to the neutron star. in our sample, there are only five double ns that can be used to test gr and etgs. taking into account of the strong hypothesis we made, the etg correction to ṫgr can also include the galactic acceleration term correction ([7], [8]). here, we give a preliminary result about the energy loss from binary systems and we show that, when the nature of the binary systems can exclude energy losses due to trade or loss of matter, then, we can explain the gap between the first time derivative of the observed orbital period and the theoretical one predicted by gr, using an analytical f(r)-theory of gravity. 253 mariafelicia de laurentis, ivan de martino 10 0 10 5 10 10 10 15 10 −4 10 −2 10 0 10 2 10 4 10 6 10 8 10 10 f ′′0 ṫ b o bs ṫ g r ṫbobs ṫgr = 1.5 ṫbobs ṫgr = 0.5 f ′′ 0 = +0.04 f ′′ 0 = 38 psrj1537+1155 psrj1738+0333 f ′′ 0 = 14.71 psrj2129+1210c figure 1: in figure there are shown, for sake of convenience, in logaritmic scale, the absolute values of f ′′0 reported in tab. 1 versus the ratio ṫbobs ṫgr . we must note that for five binaries the etgs we are probing is not ruled out 0.04 ≤ f ′′0 ≤≈ 38, for those systems the difference between ṫgr and ṫbobs is tiny, indeed we get 0.5 ≤ ṫbobs ṫgr ≤ 1.5. instead for most of binaries we have f ′′0 values that can surely rule out the theory, since taking account of the weak field assumption we obtain 38 ≤ f ′′0 ≤ 4× 107. from this last values to the first ones, there is a jump of about four up to five order of magnitude on f ′′0 . references [1] bogdanos c., capozziello s., de laurentis m., nesseris s., 2010, astrop. phys. , 34, 236. doi:10.1016/j.astropartphys.2010.08.001 [2] capozziello s., de laurentis m., 2011, physics reports 509, 167. doi:10.1016/j.physrep.2011.09.003 [3] capozziello s., corda c., de laurentis m., 2008 phys. lett. b 669, 255-259 . doi:10.1016/j.physletb.2008.10.001 [4] capozziello s., francaviglia m., 2008, gen. rel. grav. 40,357. doi:10.1007/s10714-007-0551-y [5] capozziello s., de laurentis m., faraoni v., 2009 ,the open astr. jour , 2, 1874. 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[15] maggiore m., 2007, gravitational wawes: theory and experiments, oxford univ. press, oxford. doi:10.1093/acprof:oso/9780198570745.001.0001 [16] nojiri s., odintsov s.d., 2011, physics reports 505, 59. doi:10.1016/j.physrep.2011.04.001 [17] weinberg s., 1972 ,”gravitation and cosmology”, john wiley & sons, inc., new york. [18] weisberg j.m., nice d.j. and taylor j.h., 2010, apj, 722,1030-1034. doi:10.1088/0004-637x/722/2/1030 [19] will c.m, 1993, ”theory and experiment in gravitational physics” cambridge university press, uk. doi:10.1017/cbo9780511564246 254 http://dx.doi.org/10.1016/j.astropartphys.2010.08.001 http://dx.doi.org/10.1016/j.physrep.2011.09.003 http://dx.doi.org/10.1016/j.physletb.2008.10.001 http://dx.doi.org/10.1007/s10714-007-0551-y http://dx.doi.org/10.1103/physrevd.58.042001 http://dx.doi.org/10.1016/j.astropartphys.2011.08.006 http://dx.doi.org/10.1093/mnras/stt216 http://dx.doi.org/10.1111/j.1365-2966.2012.21253.x http://dx.doi.org/10.1093/acprof:oso/9780198570745.001.0001 http://dx.doi.org/10.1016/j.physrep.2011.04.001 http://dx.doi.org/10.1088/0004-637x/722/2/1030 http://dx.doi.org/10.1017/cbo9780511564246 introduction the first time derivative of the orbital period in the f(r)-theories methodology and data analysis discussion and remarks acta polytechnica ctu proceedings doi:10.14311/app.2016.3.0025 acta polytechnica ctu proceedings 3:25–29, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app experimental validation of cumulative surface location error for turning processes adam k. kiss∗, daniel bachrathy budapest university of technology and economics, department of applied mechanics, 1111 budapest, muegyetem rkp. 5., hungary ∗ corresponding author: kiss_a@mm.bme.hu abstract. the aim of this study is to create a mechanical model which is suitable to investigate the surface quality in turning processes, based on the cumulative surface location error (csle), which describes the series of the consecutive surface location errors (sle) in roughing operations. in the established model, the investigated csle depends on the currently and the previously resulted sle by means of the variation of the width of cut. the phenomenon of the system can be described as an implicit discrete map. the stationary surface location error and its bifurcations were analysed and flip-type bifurcation was observed for csle. experimental verification of the theoretical results was carried out. keywords: surface quality, surface location error, implicit map, flip bifurcation. 1. introduction in the industry for production and manufacturing, turning is a widely used method. however, high material removal rate often cannot be accomplished in practice due to the instability of the cutting process. this machining process induces harmful vibrations which are responsible for unacceptable surface quality [1]. the phenomenon is the self-excited vibration, the so-called chatter vibration which comes from loss of stability of the periodic vibration due to the surface regeneration effect [2]. this effect can be modelled with delayed differential equations (dde) [3]. the so-called stability chart [4] presents the chatterfree (stable) parameter domain which is usually illustrated along the parameters of the spindle speed and the depth of cut, calculated by numerical methods [5, 6]. the most productive parameter regions are located between the pockets of the the so-called lobes [7], where large cutting force can occur due to the high depth of cut ratio which leads substantial surface location error (sle). the stability chart is usually used at the roughing processes. due to the fact, that sle is relevant at finishing operations [8], its effect is usually neglected in the model of roughing operations, but despite this, it can has significant impact on the surface quality in case of consecutive immersions which is typical for roughing operation. we introduce a new type of surface error calculation which considers the effect of the series of sles during several consecutive immersion. the oversize of a workpiece is removed with several consecutive immersions in roughing machining process. at every immersion, the machined surface differs from the desired one due to the sle. the actual offset error slei modifies the subsequent immersion. this modified immersion generates different cutting force figure 1. sdof turning dynamical model. which leads another, modified offset error slei+1. during this process, the sle can be accumulated and leads a new surface quality parameter denoted by the cumulative surface location error (csle) [9, 10]. the evaluation of the series of sles values and its stability problems are investigated in turning operations on a single-degree-of-freedom (sdof) mechanical model. 2. evolution of cumulative surface location error the constructed mechanical model and the main steps of the sle computation are summarised as follows. 2.1. mechanical model in the mechanical model, the workpiece is considered as a rigid body and the cutting tool is considered as single-degree-of-freedom (sdof) model, as shown in figure 1. in the figure, some technological parameters which correspond to the material removal rate and 25 http://dx.doi.org/10.14311/app.2016.3.0025 http://ojs.cvut.cz/ojs/index.php/app adam k. kiss, daniel bachrathy acta polytechnica ctu proceedings figure 2. evolution of the surface location error (sle) in consecutive immersions. figure 3. schematic representation of map. the main mechanical parameters are represented. w is the width of the chip, h is the chip thickness or the feed per revolution, vf is the feed movement, ω is the spindle speed, f is the cutting force generated from the material removal process, s is the stiffness of the tool-holder and sle is the surface location error which is the distance between the machined and desired surface. the contour of the surface is defined by the position of the turning insert. in other words, the sle is the static displacement error of the turning insert which is generated by the f constant cutting force. in this model, the so-called surface regeneration effect of the machining process is not considered. this effect would lead to time dependent cutting force function, which may result stability problems, described in details in [11]. in this study, only the static displacement is analysed, hence exclusively the stationer component of the chip thickness is used. note, that in case of the surface regenerative models, the tool is considered to be flexible in the direction of the feed velocity [12], but, in our case it is flexible perpendiculat to the feed velocity. 2.2. calculation of csle the model considers the evolution of the width of the chip as follows: in roughing operation the desired width of cut w0 is modified by the actual slei and the subsequent slei+1 (see figure 2): wi+1 ( slei, slei+1 ) = w0 + slei − slei+1. (1) in the stationary position the spring force is equal to the cutting force: s · slei+1 = fi+1, (2) so the subsequent surface error can be calculated as: slei+1 = 1 s f ( wi+1 ( slei, slei+1 )) . (3) the above implicit discrete map describes how one sle develops into another sle over of a subsequent immersion. the sle values follow each other one by one. these series of the sles can converge to a fix point (see figure 3 ; where 45 degree line represents points where slei=slei+1 ) which is denoted by csle. this solution is obtained by two different methods. one of them is a numeric iteration of the map and the other one is a numerically calculated roots of the analytical function defined by eq.(3), made by multi-dimensional bisection method [13]. the characteristic of the map is highly dependent on the applied cutting force model. some typical approximations of the cutting force as the linear, the threequarter rule [14] and the cubic polinomial rule [15] were investigated. 2.3. stability analysis of csle the stability of the investigated system is determined based on the derivative of eq. 3 with respect to w width of cut at the fix points [16]. fold type bifurcation occurs, when the derivative is greater than 1, which leads to stabiliy loss of the csle and also could lead to bistable region. another case, when the derivative is smaller than -1, this situation corresponds to the period doubling or flip-type bifurcation. after some mathematical transformation, it can be proved that only the flip-type bifurcation can occure for this model. it happens when the derivative is equals to −s/2. for a realistic environment, the s stiffness is positive and the derivative of the turning force function is also positive for the usual turning force models, therefore the mechanical model is stable. but, there can exist some special cases, when the cutting force in the function of the width of cut turn out to negative sign (and its derivative is also negative) in real machining environment, not only in mathematical sense. for instance, in our experimental measurement (see in details in the following subsection), the resultant cutting force was negative due to the edge geometry of the applied insert. fold or saddle node bifurcation point cannot be obtained for physical meaningful parameters [10]. 26 vol. 3/2016 cumulative surface location error for turning processes figure 4. the softened tool mount and the fabricated strain gauges. 1st strain gauge 2nd strain gauge 3rd strain gauge 4th strain gauge def. calib. coeff.[ deformation strain value ] = [ mm µm/m ] -1.56·104 1.06·104 0.75·104 -0.57·104 force calib. coeff.[ force strain value ] = [ n µm/m ] -8.64·106 6.76·106 4.56·106 -3.38·106 stiffness[ force calib. coeff. deformation calib. coeff. ] = [ n mm ] 533.22 636.71 614.07 593.43 averaged stiffness[ n mm ] 599.36 table 1. calibration coefficients and the calculated stiffness. figure 5. experimental setup. 3. experimental validation experimental verification of the theoretical results was carried out in a 2 axes universal turning machine center. the development of the resulted offset error along the direction of the width of the chip (sle) was investigated on a given workpiece during five consecutive immersions, as shown in figure 5. for better measurement conditions, a softened tool holder figure 6. measured sign (blue) and averaged values (red lines) of force calibration. was used which results higher offset error. the tool holder is described in details in [17]. the generated cutting force and the deformation were measured by means of strain gauges installed on the softened tool holder (see figure 4). according to the strain gauges, the measurement instrument had to be calibrated for force and for deformation measurement. the force calibration was carried out as the artificial deformations and forces were generated meanwhile the signals from the strain gauges were recorded (see figure 6). the calibration coefficients (presented in table 1) were determined from the averaged measured data by applying linear regression by means of ordinary least squares approach. the calculated stiffness: s ∼= 600 n/mm. we carried out a series of measurements using different turning process parameters. in a single test, 5 consecutive cuts were performed with fixed cutting 27 adam k. kiss, daniel bachrathy acta polytechnica ctu proceedings figure 7. calculated csle function and the measured displacements (blue stars denote the converged solutions; colored stars denote the period doubling characteristics). figure 8. measured period doubling characteristics; parameters: w = 4 [mm], h0 = 0.2 [mm]. parameters to investigate the development of sle series. the measured cutting force was negative due to the applied insert. the reason of this phenomenon may come from geometrical setup, the edge geometry and the shape of the inserts. a fitting method was applied based on the measured averaged cutting forces to determine the specific cutting coefficients of the widely used polynomial cutting force function [15]. the material of the workpiece was almgsi0.5 aluminium alloy. the csle is calculated numerically from eq.( 3) for the fitted specific cutting coefficients and it is compared to the measured values. for the computed csle, flip-type bifurcation is occurred at certain parameter points at h0 = 0.17 [mm] and 0.23 [mm] (see figure 7) where the stable solution becomes unstable and creates a periodic-2 solution. between these parameter points, the series of the meeasured sle values do not converge to a certain value, but they alternate around 2 values (see figure 8). however, the amplitude of the measured alternating (bifurcating) displacement error has much smaller amplitude than the calculated one. the source of this large error could be the small number of consecutive cuts in the measurements, while the theoretical amplitude refers to the steady state amplitude after an infinite number of cuts. 4. conclusions in the present study, we show a new type of stability problem, which can occur during roughing process. this csle-stability problem leads to an unpredictable final surface location error, which can affect the finishing operation substantially. an experimental verification of the theoretical results was carried out in a softened machine tool environment, where a correlation was found between the measured and the computed values. in most of the cases, the series of csle values of one roughing test converged to certain value, showing also good correlation with the computed csles. in the predicted parameter range of period-2 solutions, the series of the measured deformations shows alternating characteristic. we can state, that the predicted phenomenon is validated by measurements. list of symbols sle surface location error [mm] csle cumulative surface location error [mm] w width of cut [mm] w0 pre-set width of cut [mm] h feed per revolution [mm/rev] h0 pre-set feed per revolution [mm/rev] v f feed movement [mm/s] ω spindle speed [ rpm] f cutting force [n] s stiffness of the tool-holder [n/mm] acknowledgements this paper was supported by the hungarian scientific research fund otka pd-112983 and the janos bolyai research scholarship of the hungarian academy of sciences. references [1] s. a. tobias. machine tool vibration. blackie and son, ltd, london 1965. [2] j. tobias, l. spacek. self-excited vibrations on machine tools, 1954. [3] g. stepan. retarded dynamical systems: stability and characteristic functions. longman scientific and technical 1989. [4] y. altintas, e. budak. analytical prediction of stability lobes in milling. cirp annals manufacturing technology 44(1):357–362, 1995. [5] t. insperger, g. stepan. semi-discretization for time-delay systems. springer, applied mathematical sciences 2011. [6] d. bachrathy, g. stepan. improved prediction of stability lobes with extended multi frequency solution. cirp annals manufacturing technology 62(1):411–414, 1995. [7] m. j. reith, g. stepan. optimization of material removal rate for orthogonal cutting with vibration limits. periodica polytechnica-mechanical engineering 56(2):91–97, 2012. doi:10.3311/pp.me.2012-2.03. 28 http://dx.doi.org/10.3311/pp.me.2012-2.03 vol. 3/2016 cumulative surface location error for turning processes [8] w. a. kline, r. e. devor, i. a. shareef. the prediction of surface accuracy in end milling. asme journal of engineering for industry 104(3):272–278, 2009. [9] a. kiss, d. bachrathy. explicit model of cumulative surface location error for milling processes. 12th hungarian conference on theoretical and applied mechanics 2015. [10] a. kiss. cumulative surface location error for cutting processes. msc thesis, bme, department of applied mechanics 2014. [11] r. szalai, g. stepan. lobes and lenses in the stability chart of interrupted turning. journal of computational and nonlinear dynamics 1(3):205–212, 2006. [12] t. insperger, d. a. w. barton, g. stepan. criticality of hopf bifurcation in state-dependent delay model of turning processes. international journal of non-linear mechanics 43(2):140–149, 2013. doi:10.1016/j.ijnonlinmec.2007.11.002. [13] d. bachrathy, g. stepan. bisection method in higher dimensions and the efficiency number. periodica polytechnica-mechanical engineering 56(2):81–86, 2012. [14] o. kienzle. spezifische schnittkrafte bei der metallbearbeitung. werkstattstechnik und maschinenbau 47(1):224–225, 1957. [15] h. shi, s. tobias. theory of finite-amplitude machine-tool instability. international journal of machine tools and manufacture 24(21):45–69, 1984. [16] j. t. sandefur. discrete dynamical systems : theory and applications 1990. [17] m. j. reith, d. bachrathy, g. stepan. stability properties and optimization of multi-cutter turning operations. asme, international design engineering technical conferences and computers and information in engineering conference: detc2013: portland, usa, oregon 2013. doi:10.1115/detc2013-12347. 29 http://dx.doi.org/10.1016/j.ijnonlinmec.2007.11.002 http://dx.doi.org/10.1115/detc2013-12347 acta polytechnica ctu proceedings 3:25–29, 2016 1 introduction 2 evolution of cumulative surface location error 2.1 mechanical model 2.2 calculation of csle 2.3 stability analysis of csle 3 experimental validation 4 conclusions list of symbols acknowledgements references 189 acta polytechnica ctu proceedings 1(1): 189–193, 2014 189 doi: 10.14311/app.2014.01.0189 are supernovae responsible for the gamma ray spectrum from the galactic center? todor stanev1 1bartol research foundation and department of physics and astronomy, university of delaware, u.s.a. corresponding author: stanev@bartol.udel.edu abstract we discuss the supernova remnants distribution as a function of the galactic longitude and compare their positions to that of the detected tev gamma ray sources. a large fraction of these sources either coincide or a close by known supernova remnants. if we look within 10o of the galactic center most identified sources are combinations of supernova remnants with giant molecular clouds. the diffuse gamma ray flux from the direction of the galactic center is much smaller. keywords: supernova remnants cosmic rays acceleration tev gamma rays. 1 introduction i will start this write-up the same way as i started the talk: with the answer to the question, which is i do not know. what i will write about is what we know about different types of supernova remnants (snr) from which tev γ rays are detected and what theoretical research says about the way these γ rays are produced in them. the main reason we are interested in supernova remnants is they are supposed to be the sources of galactic cosmic rays, which are accelerated at the supernova shocks. the outer regions of the expanding supernovae initially move with high velocity, approximately 0.1c. the expansion velocity is supersonic and a shock is formed in front of the remnant. the shock collects the interstellar matter that it meets during the expansion. once the shock radius is close to 1 pc, when the remnant is about 1,000 years old, the amount of the swept-up material becomes too much and the remnants velocity decreases. this is the time when cosmic rays are accelerated at the shock front. the magnetic field at the shock front is significantly higher than that of the interstellar medium and only a small fraction o(few %) of the kinetic energy of the remnant can supply all galactic cosmic rays (ginzburg & syrovatskii, 1964). 2 supernova remnants the latest supernova remnant catalog that i am familiar with is that of d.a. green (green 2009). it contains 274 supernova remnants studied in radio and gives their location, power at 1 ghz, and spectral indexes. ten of these snr have longitude less than 10o from the galactic center. all of them are closer than 1.5o from the galactic plane. the directions of all 274 these supernova remnants are shown in fig. 1 where the ones from supernovae after 1,000 ad (and the galactic center) are indicated. one can easily see that most of the remnants are very close to the galactic plane and a few are more than 5o away from it. one can also see that the supernova remnants density is much higher in the inner 60o of the galaxy. figure 1: locations of the supernova remnants in d.a. green catalog. the question if these snr are the sources of cosmic rays and of high energy γ-rays becomes very reasonable. to approach this question we will have a look at the galactic sources of high energy γ-rays, the tevcat of the university of chicago (http://tevcat.uchicago.edu). this catalog contains 145 gamma ray sources that have been discovered by the atmospheric cherenkov gamma ray telescopes. these devices consist of several mirror telescopes that observe the cherenkov light emitted by the cascade developing after the high energy gamma rays interact with atmosphere. the shape of the image of the cascade is enough to differentiate between atmospheric γ-ray cascades and cascades from the interactions of cosmic ray 189 http://dx.doi.org/10.14311/app.2014.01.0189 todor stanev protons and nuclei in the atmosphere. when the cascade is observed by more than one telescope the angular resolution is a small fraction of a degree. the threshold energy for these devices depends on the size of the mirrors and is often of o(100 gev). the three major tev gamma ray atmospheric telescopes are, in order of their completion, hess (hinton et al, 2004), veritas (hanna et al., 2008), and magic (boria tridon et al., 2010). hess and veritas have each four 12 m. telescopes and magic has two 17 m. telescopes. the average detection threshold for 12 m. telescopes is between 100 and 200 gev while the 17 m. telescopes can come down to 60 gev. tevcat has identified 64 galactic sources listed by different types in table 1. table 1: galactic tev gamma ray sources pulsar wind nebulae 31 shell supernova remnants 12 x-ray binaries 3 gamma ray binaries 1 massive stars 3 snr/molecular clouds 8 globular clusters 1 unidentified 5 it is not obvious that the different distribution of the tev gamma ray sources within 10o of the galactic center is important. out of the ten sources four are snr with close by molecular cloud, three are unidentified (which includes the galactic center and the galactic center ridge), one is pulsar wind nebula. there is also one shell snr and one globular cluster. since all of these objects are at the approximately the same distance from us we expect the gamma ray fluxes from them to correspond to the overall luminosity of the sources. the number of the detected gamma rays will also correspond to the threshold energy for detection. the exact threshold energy for detection by the tev air cherenkov telescopes depends on the size of the telescope mirrors and on the positions of the source and the telescope. to demonstrate this we show in fig. 2 the galactic plane and the sources in equatorial coordinates. the telescopes are sensitive to source elevation down to 30o but the lower the source is the higher the energy threshold. the hess telescope is in namibia at 23 degrees south, veritas is in arizona, u.s.a. at 31 degrees north, and magic is at 29 degrees north. all of them can observe most of the galactic plane, but the location of hess is the best one for observations of the galactic center. this is the reason it was constructed in namibia. figure 2: the vicinity of the galactic plane and the galactic sources of tev gamma rays in equatorial coordinates. figure 3 shows the galactic sources of tev gamma rays (circles) overlayed on the supernova remnants. the sources from the first fermi/lat catalog (abdo et al (2010)) are shown with triangles. if we had a look at the later fermi/lat catalogs we would find many more galactic sources the coincide with supernova remnants. one should not forget that fermi/lat is sensitive to γrays of energy 0.1 to 100 gev and the average spectral slope of the gamma ray sources is about 2.5. this means that are 30,000 more gamma rays above 100 mev than are gamma rays above 100 gev. this number varies, of course, from source to source depending on the spectral index of the source. figure 3: the position of the galactic tev gamma ray sources (circles) are overlayed on top of the supernova remnants from the green’s catalog. the triangles show the the fermi/lat gamma ray sources from its first catalog (abdo et al (2010)). 2.1 pulsar wind nebulae pulsar wind nebulae are formed by the highly relativistic mhd winds expelled by the rotating neutron stars. such objects can accelerate all kinds of charged particles, from electrons to heavy nuclei if there is a proper injection mechanism close to the neutron star. the best studied pwn is that of the crab. the gamma ray fluxes from different sources are often given in crab units that describe the ratio of their emission to that of the crab. its gamma ray energy spectrum is best described by the synchrotron self compton model that is based only on electron acceleration. electrons emitted by the source suffer from synchrotron energy loss to photons. these photons than go through inverse compton interactions 190 are supernovae responsible for the gamma ray spectrum from the galactic center? with the accelerated electrons that pushes them to tev energies. it is not expected that such sources can produce very high energy gamma rays when the inverse compton cross section decreases in the klein-nishina regime. the studies of most tev pulsar wind nebulae, however, agree better with leptonic models than with cosmic ray interaction models. the same is true for many other tev gamma ray sources such as geminga and vela x. 2.2 shell supernova remnants shell supernova remnants sources are the typical supernova remnants as we imagine them. the shock wave from supernova explosion heats up the interstellar material as it propagates through it. when we observe such a remnants we see mostly its outer edge that is brighter than the inside of the remnant. in optical astronomy this effect is called limb brightening. the observations also indicate higher magnetic fields at the limbs of the remnants. a very good introduction to the processes in the remnant is given in (reynolds, 1998) where the author deals only with electron acceleration. the acceleration of protons and heavier nuclei is discussed by (caprioli, amato & blasi, 2010). in order to understand the limb brightening one has to assume that there is electron acceleration at the edge of the remnants where the electrons have synchrotron energy loss in the higher magnetic field. the shell supernova tev gamma ray sources in tevcat include ic443, sn1006, cassiopeiaã, and tycho. 2.3 snr/molecular clouds this type of sources includes supernova remnants that have massive molecular clouds nearby. very often the tev gamma ray sources do not point at the center of the remnant, rather at the molecular cloud itself or at the side of the remnant that is close to the cloud. figure 4: positions of the molecular clouds and the number of tev gamma rays observed by the hess experiment (aharonian et al, 2006). most of these sources were first observed by the hess experiment and carry its name. an extremely interesting analysis was performed by hess after its observation of the galactic center ridge (aharonian et al, 2006). this analysis is illustrated in fig. 4. hess saw that the number of tev gamma rays coming from the vicinity of the galactic center has gaps, i.e. there would be hundreds of gamma rays coming from certain direction, then almost no gamma rays, then again hundreds of gamma rays. the exact directions of the locations that produced hundreds of gamma rays coincided with the positions of several giant molecular clouds containing 2-4×107 m�. at the 8.5 kpc distance of the galactic center 0.2o longitudinal difference corresponds to a distance of 30 pc. the analysis concluded with the idea that cosmic rays were accelerated in the galactic center (maybe at sagittarius a east) many years ago and started diffusing away from it. when they diffuse into one of the huge molecular clouds they interact with the matter there, generate neutral mesons that decay into gamma rays. these cosmic rays were able to diffuse at distances up to 100 pc but have not yet reached the molecular cloud at a distance of 200 pc. this leads to an estimate of the time of the supernova remnant acceleration episode of 104 years ago. an acceleration episode could be similar to the movement of a small molecular cloud to the black hole sgr a∗ in the galactic center that is being observed now (gillesen et al, 2013). the absorption of large amount of matter by the black hole can easily create a shock and thus accelerate cosmic rays for a relatively short time. there are now analyses of different gamma ray sources that require the existence of molecular clouds nearby. a very interesting one is that of (torres, rodriguez marrero & decea del pozo, 2010) of the supernova remnant ic443. the gamma ray emission of this source is known from the 1990’s when it was detected by egret. it was observed by the tev cherenkov telescopes magic and veritas at a slightly different (0.4o) direction. the direction of the same source from agile and fermi/lat are consistent with this of egret. the authors of this analysis identify two (or maybe three) different sources: ic443 as seen by the tev telescopes and a molecular cloud in front of it that is observed in the gev energy range. it is also possible that another, relatively small molecular cloud also emits gamma rays. the existence of different sources solves the problem with the different spectral indices in the gev and the tev gamma ray emission. 3 other possible ideas an old paper (berezinsky et al, 1993) looks at the possibility that there would be a strong diffuse radiation from the central region of the galaxy. the paper uses a matter density study (bloemen, 1989) that determined that 191 todor stanev the matter density in the inner 300 pc of the galactic plane within b < |2|o is 38 nucleons cm−3. the matter density strongly decreases to reach less than 1 per cm3 at distances greater than 6 kpc. assuming that the matter distribution in the galaxy is symmetric (which it is not) the paper used the data of bloemen to calculate the column density in different directions. the highest column density for latitude less than 2o around the galactic center reached 8×1022 cm−2. using this mapping the paper provides the ratio between the γray flux and cosmic ray flux as a function of the galactic longitude. in the vicinity of the galactic center and for energies less than 10 tev this ratio is still less than 10−4. it is easy the explain that: a column density of 8×1022 cm−2 is slightly more than 0.1 g/cm2 when the proton interaction length is about 50 g/cm2. this means that only 0.6% of the galactic cosmic rays interact and generate gamma rays that we will see coming from the direction of the galactic center. in all other directions the diffuse gamma ray flux is smaller. i refer to this paper because it attempted to calculate in an easy way the diffuse gamma ray flux. the contemporary attempts to do this are much more sophisticated and involve measurements and subtraction of all known gamma ray sources. the fermi bubbles were discovered in this way (su, slatyer & finkbeiner, 2010). the bubbles cover an area much larger than the galactic center region and are still discussions of the origin of the gamma ray emission from them. one example of the fermi/lat studies of the diffuse gamma ray radiation in the galaxy is in (ackermann et al, 2012) where the small and large scale anisotropy is studied and the existence of unknown gamma rays sources is discussed. in other papers the diffuse radiation is searched for for possible dark matter signatures. 4 discussion and conclusions the gamma ray energy spectra from the detected gamma ray sources are very often compared to leptonic and hadronic models models of gamma ray production. some of the sources, typically the pulsar wind nebulae, fit better the leptonic models, where electrons accelerated at the source have inverse compton collisions with synchrotron photons emitted by the same electrons in propagation of the magnetic fields around the source. even if these so called ssc models fit much better the gamma ray emission in a wide energy range, there are still problems that are hard to solve. the main problem (for me) is that it is difficult to imagine a mechanism that only injects electrons and not charged nuclei in the acceleration site. one possible answer is that both electrons and cosmic rays are accelerated but the matter density around the source is very low and the cosmic rays do not interact to produce neutral mesons and gamma rays. electrons, on the other hand, emit synchrotron radiation in their propagation in magnetic fields and these low energy photons are the target for inverse compton interactions. there are, of course, several sources that fit better the hadronic interaction models and this is true for more of the combinations of supernova remnants and molecular clouds. the proof of π0 origin of the gamma rays in a source is the decrease of the flux at energies lower than 70 mev, one half of the π0 mass. this however does not happen if there is a significant contribution to the gamma ray flux from bremsstrahlung. this is one of the reasons that for most of the gamma ray sources the hadronic origin is suspected, but not proven. the suspicion is usually because of the existence of large matter density around or in front of the source. figure 5: the neutrino flux that corresponds to the gamma ray flux of ic 443. no neutrinos attributed to this sources have been observed yet. the only way we can be certain that the gamma ray generating process is hadronic is if we observe also neutrinos from the same object. gamma ray and neutrino productions are closely related as shown in eq. 1 that gives the shape of the gamma ray and neutrino fluxes as a function of the same astrophysical parameters. dnγ(ν) deγ(ν) = dncr decr fa σinel mn [ρr]cν 2znπ0(π±) γ + 1 (1) the term fa accounts for the differences between proton-proton and nuclei interactions and the term cν , that is less than 1, accounts for the different kinematics 192 are supernovae responsible for the gamma ray spectrum from the galactic center? of gamma ray and neutrino production. the gamma ray flux is higher than that of neutrinos. the big problem is the tiny neutrino interaction cross section that requires huge detectors similar to the 1 km3 icecube detector at the south pole. in some cases the low neutrino cross section is an advantage as all neutrinos generated by a source will not be absorbed and will be visible by the neutrino telescopes. acknowledgement this work is supported in part by the us department of energy contract ud-fg02-91er40626. references [1] abdo, a.a. et al. (fermi/lat collaboration): 2010, ap.j. suppl. 188, 429. doi:10.1088/0004-637x/715/1/429 [2] aharonian, f. et al. (hess collaboration): 2006, nature, 439, 695. doi:10.1038/nature04467 [3] ackermann, m (fermi/lat collaboration(: 2012, phys. rev. d85:109901; arxiv:1202.2856 [4] berezinsky, v.s., gaisser, t.k., halzen, f., & stanev, t.:1993, astropart. phys. 1, 281. doi:10.1016/0927-6505(93)90014-5 [5] bloemen, h.:1989, ann. rev. astron. astrophys. 27, 469. doi:10.1146/annurev.aa.27.090189.002345 [6] boria tridon, d. et al. (magic collaboration):2010, nim a623, 437. [7] caprioli, d., amato, e. & blasi:2010, p.:astropart. phys., 33, 160. [8] gillesen, s. et al.:2013, arxiv:1306.1374 [9] ginzburg, v.l. & syrovatskii, s.i.:1964, the origin of cosmic rays (pergamon press, oxford). [10] green, d.a.:2009, bull. astr. soc. india, 37, 45. astro-ph:0905.3699v2 [11] hanna, d. et al. (veritas collaboration):2008, nim a588, 26. [12] hinton, j.a. et al. (hess collaboration):2004, new astr. rev. 48, 331. doi:10.1016/j.newar.2003.12.004 [13] reynolds, s.p.:1998, apj 493, 375. [14] su m., slatyer t. r.& finkbeiner d. p.:2010, apj, 724, 1044. doi:10.1088/0004-637x/724/2/1044 [15] torres, d., rodriguez marrero, a.y. & de cea del pozo, e.:2010, mnras, 408, 1257. doi:10.1111/j.1365-2966.2010.17205.x discussion carlotta pittori: is there any possible correlation between your viewgraph of the galactic center with the idea of an episode of cosmic ray acceleration 106 years ago and the 511 kev integral map shown by ubertini? todor stanev: as piero ubertini said himself it is a matter of electron and positron density in the annihilation site. there is, of course, also the problem of their diffusion. how far these particles would go away from the acceleration site in a million years and how big the annihilation area would be? the hess analysis of the galactic ridge discusses the diffusion in a location where we expect very irregular and strong magnetic fields and thus fast diffusion. 193 http://dx.doi.org/10.1088/0004-637x/715/1/429 http://dx.doi.org/10.1038/nature04467 http://dx.doi.org/10.1016/0927-6505(93)90014-5 http://dx.doi.org/10.1146/annurev.aa.27.090189.002345 http://dx.doi.org/10.1016/j.newar.2003.12.004 http://dx.doi.org/10.1088/0004-637x/724/2/1044 http://dx.doi.org/10.1111/j.1365-2966.2010.17205.x introduction supernova remnants pulsar wind nebulae shell supernova remnants snr/molecular clouds other possible ideas discussion and conclusions 49 acta polytechnica ctu proceedings 1(1): 49–55, 2014 49 doi: 10.14311/app.2014.01.0049 planck 2013 cosmology results: a review josé alberto rubiño-mart́ın1,2 on behalf of the planck collaboration 1instituto de astrofisica de canarias, e-38200 la laguna, tenerife, spain 2departamento de astrofisica, universidad de la laguna, e-38206 la laguna, tenerife, spain corresponding author: jalberto@iac.es abstract this talk presents an overview of the cosmological results derived from the first 15.5 months of observations of the esa’s planck mission. these cosmological results are mainly based on the planck measurements of the cosmic microwave background (cmb) temperature and lensing-potential power spectra, although we also briefly discuss other aspects of the planck data, as the statistical characterization of the reconstructed cmb maps, or the constraints on cosmological parameters using the number counts of galaxy clusters detected by means of the sunyaev-zeldovich effect in the planck maps. all these results are described in detail in a series of papers released by esa and the planck collaboration in march 2013. keywords: cosmology: observations cosmic microwave background cosmological parameters galaxy clusters. 1 introduction planck1 (tauber et al., 2010; planck collaboration i, 2011) is the third generation space mission to measure the anisotropy of the cosmic microwave background (cmb). it observes the sky in nine frequency bands covering 30–857 ghz with high sensitivity and angular resolution from 31’ to 5’. the low frequency instrument (lfi; mandolesi et al., 2010; bersanelli et al., 2010; mennella et al., 2011) covers the 30, 44, and 70 ghz bands with amplifiers cooled to 20 k. the high frequency instrument (hfi; lamarre et al., 2010; planck hfi core team, 2011a) covers the 100, 143, 217, 353, 545, and 857 ghz bands with bolometers cooled to 0.1 k. polarisation is measured in all but the highest two bands (leahy et al., 2010; rosset et al., 2010). a combination of radiative cooling and three mechanical coolers produces the temperatures needed for the detectors and optics (planck collaboration ii, 2011). two data processing centres (dpcs) check and calibrate the data and make maps of the sky (planck hfi core team 2011b; zacchei et al., 2011). planck ’s sensitivity, angular resolution, and frequency coverage make it a powerful instrument not only for cosmology, but also for galactic and extra-galactic astrophysics. this talk focuses on the main cosmology results based on planck ’s second data release, which covers data acquired in the period 12 august 2009 to 27 november 2010, and will be quoted here as nominal mission maps. all these results and the associated data products are described in a series of papers released in march 2013 (planck collaboration i–xxix, 2013). because the analysis of the polarization data is not yet as mature as the analysis of the temperature data, the planck polarization results are not included in this release. 2 overview of planck 2013 cosmology results the main goal of the planck mission is to determine with great precision the key cosmological parameters describing our universe, using the information encoded in the cmb anisotropies on intermediate and small angular scales over the whole sky (tauber et al., 2010; planck collaboration i, 2013). the data processing pipelines and beam calibrations employed by the lfi and hfi dpcs to create and characterize the nine full-sky maps based on the first 15.5 months of operations are described in planck collaboration ii–ix (2013). these nine maps (see table 1) allow robust reconstruction of the primordial cmb temperature fluctuations over nearly the full sky, as well as new constraints on galactic foregrounds, including thermal dust and line emission from molecular carbon monoxide (planck collaboration xii 2013). four different component separation methods were optimized to produce 1 planck (http://www.esa.int/planck) is a project of the european space agency (esa) with instruments provided by two scientific consortia funded by esa member states (in particular the lead countries france and italy), with contributions from nasa (usa) and telescope reflectors provided by a collaboration between esa and a scientific consortium led and funded by denmark. 49 http://dx.doi.org/10.14311/app.2014.01.0049 josé alberto rubiño-mart́ın a cmb map based on the planck maps alone, i.e., without the addition of any other external data. figure 1 shows the map produced by the smica method. 2.1 the planck cmb likelihood and the angular power spectrum a complete statistical description of the two-point correlation function of the cmb temperature fluctuations measured by planck which accounts for all known relevant uncertainties, is encoded in the planck likelihood (planck collaboration xv 2013). we follow a hybrid approach to construct this likelihood, using a exact approach at large scales (` < 50), and a pseudo-c` approach at small scales (` > 50). this function can be used to derive our estimate of the cmb angular power spectrum (see figure 2), which constitutes an extremely precise measurement over three decades in multipole range, allowing to see seven acoustic peaks. in this plot, our main source of error at ` ≤ 1500 is due to cosmic variance. the measurements are in excellent agreement with previous experiments (wmap, act, spt). we have validated our likelihood through an extensive list of consistency tests, assessing the impact of residual foreground and instrumental uncertainties on the final results. although the polarization data are not released, we have checked that the best-fit λcdm cosmology is in excellent agreement with preliminary planck ee and te polarisation spectra. table 1: planck performance parameters determined from flight data (planck collaboration i 2013). channel νcenter fwhm noise sensitivity [ghz] [arcmin] [µkrj s 1/2] 30 ghz 28.4 33.16 145.4 40 ghz 44.1 28.09 164.8 70 ghz 70.4 13.08 133.9 100 ghz 100 9.59 31.52 143 ghz 143 7.18 10.38 217 ghz 217 4.87 7.45 353 ghz 353 4.70 5.52 545 ghz 545 4.73 2.66 857 ghz 857 4.51 1.33 2.2 lensing by large scale structure on small (arcminute) angular scales, the cmb anisotropies are perturbed by gravitational lensing, primarily sourced by the large scale structure of the universe at relatively high redshifts (peaking at z ∼ 2). planck provides a 25σ detection of this effect (planck collaboration xvii, 2013), allowing also a lensing potential reconstruction at the map level on almost the full sky. the power spectrum of this lensing potential map is used to construct a “lensing” likelihood, which is included in our cosmological analyses. the inclusion of the planck lensing reconstruction can break degeneracies inherent in the temperature data alone, especially the geometric degeneracy in nonflat models, thus providing a strong constraint on spatial curvature without the need of including polarization data. 2.3 cosmological parameters: base model the planck measurements of the cmb temperature and lensing-potential power spectra are well described by the standard spatially-flat six parameter λcdm model with adiabatic scalar perturbations (planck collaboration xvi, 2013). the computed values of the six key parameters within this model are summarized in table 2, together with the values obtained for some derived parameters, as ωλ, ωm, σ8 or the hubble constant h0. the most remarkable result is that, for this cosmology, we find a low value of the hubble constant, which is in tension with recent direct measurements of h0, but is in excellent agreement with constraints from baryon acoustic oscillation surveys (see planck collaboration xvi (2013) for a detailed discussion). we also find a higher value of the matter density, as compared to previous measurements. 2.4 cosmological parameters: beyond the base model multiple one-parameter extensions to the base (sixparameter) model have been discussed in planck collaboration xvi (2013). however, the main result is that there is no compelling evidence for any of these extensions. for example, including curvature, we find that the universe is consistent with spatial flatness to subpercent level precision (ωtot = 1.0010± 0.0065, at 95%, using planck +lensing+wp+highl+bao). there is no evidence for additional neutrino-like relativistic particles beyond the three families of neutrinos in the standard model. using bao and cmb data, we find neff = 3.30 ± 0.27 for the effective number of relativistic degrees of freedom, in excellent agreement with the standard value of 3.046, and an upper limit of 0.23 ev for the sum of neutrino masses. in addition, we find no evidence for dynamical dark energy; using bao and cmb data, the dark energy equation of state parameter 50 planck 2013 cosmology results: a review is constrained to be w = −1.13+0.13 −0.10. finally, deviations from the simplest inflationary scenario are discussed in planck collaboration xvi and xxii (2013), including tests of specific inflationary models, isocurvature modes, and broken scaleinvariance. as a main result, planck rules out exact scale invariance (ns = 1) at high significance. the deviation of the scalar spectral index from unity is insensitive to the addition of tensor modes and to changes in the matter content of the universe. we find a 95% upper limit of r < 0.11 on the tensor-to-scalar ratio (see figure 3), which allows us to constrain a number of inflationary models. figure 1: the smica method estimates the cmb over about 97% of the sky, with the remaining area replaced with a constrained gaussian realization. figure taken from planck collaboration i (2013). figure 2: cmb temperature angular power spectrum from planck. the shaded area represents cosmic variance. the solid line corresponds to the best-fit six-parameter λcdm model quoted in the text. figure taken from planck collaboration i (2013). 51 josé alberto rubiño-mart́ın table 2: cosmological parameter values for the six-parameter base λcdm model. column 2 give the results for the planck temperature and lensing potential power spectra, while column 3 adds the information from wmap polarization (wp) at low multipoles (` ≤ 23), and other small scale cmb experiments (highl). see planck collaboration xvi 2013 for details. the last four rows are derived parameters. planck + lensing + wp + highl ωbh 2 0.02217 ± 0.00033 0.02218 ± 0.00026 ωch 2 0.1186 ± 0.0031 0.1186 ± 0.0022 100θmc 1.04141 ± 0.00067 1.04144 ± 0.00061 τ 0.089 ± 0.032 0.090+0.013 −0.014 ns 0.9635 ± 0.0094 0.9614 ± 0.0063 ln(1010as) 3.085 ± 0.057 3.087 ± 0.024 ωλ 0.693 ± 0.019 0.693 ± 0.013 ωm 0.307 ± 0.019 0.307 ± 0.013 h0 67.9 ± 1.5 67.9 ± 1.0 σ8 0.823 ± 0.018 0.8233 ± 0.0097 figure 3: marginalized joint 68% and 95% confidence level regions for ns and r from planck in combination with other data sets, compared to the theoretical predictions of some inflationary models. taken from planck collaboration xxii (2013). 2.5 gaussianity and statistical isotropy the statistical isotropy and the gaussian nature of the planck cmb maps has been rigorously examined in several papers (planck collaboration xxiii–xxvi, 2013). as a main result, there is no detection of primordial non gaussianity, obtaining the following values for the primordial local, equilateral and orthogonal bispectrum amplitudes: f local nl = 2.7 ± 5.8, f equil nl = −42 ± 75, and fortho nl = −25 ± 39 (all at 68% confidence level). the integrated sachs-wolfe-lensing bispectrum signal is detected at 2–3 sigma level. the planck data also provides stringent new constraints on cosmic strings and other defects (planck collaboration xxv 2013). alternative geometries and non-trivial topologies have also been analyzed (planck collaboration xxvi 2013). deviations from isotropy have been found in planck 52 planck 2013 cosmology results: a review cmb maps, essentially confirming all the low-angle cmb anomalies previously seen in wmap data at similar levels of significance (about 3σ): the low quadrupole amplitude; the quadrupole-octupole alignment; the hemispherical asymmetry; and the “cold spot”. finally, planck notes a further low-angle discrepancy, related to the deficit of power in the angular power spectrum in the multipole range 20 ≤ ` ≤ 40, which could be connected with some of the previous features (e.g. the hemispherical asymmetry or the low observed variance). 2.6 galaxy clusters planck maps can also be used to detect and study galaxy clusters by means of their sunyaev-zeldovich (sz) effect (sunyaev & zeldovich, 1972). early planck results on clusters were published in planck collaboration viii-xii (2011). in march 2013, we have released the planck catalogue of sz sources (psz1) based on the nominal mission maps (planck collaboration xxix 2013). psz1 contains 1227 entries, out of which 861 are confirmed galaxy clusters, and it constitutes the largest all-sky cluster catalogue to date (see figure 4). in planck collaboration xx (2013), we present constraints on cosmological parameters using the number counts (n(z)) for a well-defined and 100% reliable subsample of 189 galaxy clusters from psz1. using a xray calibrated mass-sz flux relation, and assuming a 20% bias between the x-ray determined mass and the true mass of a cluster, we derive constraints on the matter power spectrum amplitude and the matter density parameter, obtaining σ8(ωm/0.27)0.3 = 0.78±0.01, with one-dimensional ranges σ8 = 0.77 ± 0.02 and ωm = 0.29 ± 0.02. these results are in excellent agreement with the cosmological constraints from the angular power spectrum of the thermal sz emission. in planck collaboration xxi (2013), we construct the first all-sky maps of the thermal sz emission, and compare their power spectrum to theoretical models, finding σ8(ωm/0.27)0.3 = 0.784 ± 0.016. however, these results favour somewhat low values of σ8 and ωm as compared to the cmb based analysis (see table 2). this tension can be eliminated by relaxing the assumption on the mass bias between x-ray and true mass up to 45%, although such a high value is difficult to reconcile with the known observed properties of galaxy clusters. there is another interesting possibility to reconcile these values, which consists in allowing for a component of massive neutrinos with a total mass (for the sum of the three species) of the order to ∑ mν ≈ 0.22 ev (see marulli et al. 2011 for a review of how cosmological observations can be affected by the inclusion of neutrino masses). these possibilities will be further investigated in future releases. figure 4: distribution of the 1227 planck sz clusters and candidates across the sky, shown in mollweide projection in galactic coordinates. the masked regions in black color (point-sources, magellanic clouds and galactic emission) cover a total area of 16.3%, and are not used by the sz cluster-finder algorithms. taken from planck collaboration xxix (2013). 3 conclusions the main conclusions of the planck 2013 release are: • the planck data are in remarkable agreement with a flat six-parameter λcdm model; • we detect with high significance lensing of the cmb by intervening matter, providing evidence for dark energy from the cmb alone; • the best-fit model contains a weaker cosmological constant (∼ 69%), and more cold dark matter (∼ 26%) than previously estimated; and we firmly establish a deviation from scale invariance for primordial matter perturbations; • we find a low value of the hubble constant, in tension with other astrophysical measurements; • there is no compelling evidence for extensions of the base model; • we find no evidence for significant deviations from gaussianity in the statistics of cmb anisotropies; however, we confirm the anomalies at large angular scales first detected by wmap and find a deficit of power at low-multipoles with respect to our best-fit model. • the planck sz cluster measurements are in tension with the cmb results; although this conclusion is limited by our knowledge of the observablemass relations, it might provide hints for physics in the neutrino sector. 53 josé alberto rubiño-mart́ın the next (2014) release of planck data, which will include the full-mission maps and the polarization information, will provide a significant improvement in data quality and the level of systematic error control, helping in answering these open questions. acknowledgement the development of planck has been supported by: esa; cnes and cnrs/insu-in2p3-inp (france); asi, cnr, and inaf (italy); nasa and doe (usa); stfc and uksa (uk); csic, micinn, ja and res (spain); tekes, aof and csc (finland); dlr and mpg (germany); csa (canada); dtu space (denmark); ser/sso (switzerland); rcn (norway); sfi (ireland); fct/mctes (portugal); and prace (eu). a description of the planck collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck. jar-m is grateful to the organizers of the frascati workshop 2013 for the invitation to present these results. jar-m acknowledges support from the project aya2010-21766-c03-02 of the spanish ministry of science and innovation (micinn). references [1] bersanelli, m., mandolesi, n., butler, r. c., et al. 2010, a&a, 520, a4 [2] mandolesi, n., bersanelli, m., butler, r. c., et al. 2010, a&a, 520, a3 [3] mennella et al. 2011, a&a, 536, a3 [4] lamarre, j., puget, j., ade, p. a. r., et al. 2010, a&a, 520, a9 [5] leahy, j. p., bersanelli, m., d’arcangelo, o., et al. 2010, a&a, 520, a8 [6] marulli, f. et al. 2011, mnras, 418, 346 [7] planck collaboration i. 2011, a&a, 536, a1 [8] planck collaboration ii. 2011, a&a, 536, a2 [9] planck collaboration viii. 2011, a&a, 536, a8 [10] planck collaboration ix. 2011, a&a, 536, a9 [11] planck collaboration x. 2011, a&a, 536, a10 [12] planck collaboration xi. 2011, a&a, 536, a11 [13] planck collaboration xii. 2011, a&a, 536, a12 [14] planck hfi core team. 2011a, a&a, 536, a4 [15] planck hfi core team. 2011b, a&a, 536, a6 [16] planck collaboration i. 2013, a&a submitted [17] planck collaboration ii. 2013, a&a submitted [18] planck collaboration iii. 2013, a&a submitted [19] planck collaboration iv. 2013, a&a submitted [20] planck collaboration v. 2013, a&a submitted [21] planck collaboration vi. 2013, a&a submitted [22] planck collaboration vii. 2013, a&a submitted [23] planck collaboration viii. 2013, a&a subm. [24] planck collaboration ix. 2013, a&a submitted [25] planck collaboration x. 2013, a&a submitted [26] planck collaboration xii. 2013, a&a submitted [27] planck collaboration xiii. 2013, a&a subm. [28] planck collaboration xiv. 2013, a&a subm. [29] planck collaboration xv. 2013, a&a submitted [30] planck collaboration xvi. 2013, a&a subm. [31] planck collaboration xvii. 2013, a&a subm. [32] planck collaboration xviii. 2013, a&a subm. [33] planck collaboration xix. 2013, a&a subm. [34] planck collaboration xx. 2013, a&a submitted [35] planck collaboration xxi. 2013, a&a subm. [36] planck collaboration xxii. 2013, a&a subm. [37] planck collaboration xxiii. 2013, a&a subm. [38] planck collaboration xxiv. 2013, a&a subm. [39] planck collaboration xxv. 2013, a&a subm. [40] planck collaboration xxvi. 2013, a&a subm. [41] planck collaboration xxix. 2013, a&a subm. [42] rosset, c. et al. 2010, a&a, 520, a13 [43] sunyaev, r. a. & zeldovich, y. b. 1972, comments on astrophysics and space physics, 4, 173 [44] tauber, j. a. et al. 2010, a&a, 520, a1 [45] zacchei et al. 2011, a&a, 536, a5 54 planck 2013 cosmology results: a review discussion marco regis: can the large scale anomalies be due to galactic foregrounds ? jose alberto rubiño-martin: we have performed a large number of tests using the four cmb maps produced by the different component separation algorithms, and the consistency of the results strongly favors a cosmological origin for the anomalies. in addition, the agreement between planck and wmap rules out a possible explanation based on systematic effects. 55 introduction overview of planck 2013 cosmology results the planck cmb likelihood and the angular power spectrum lensing by large scale structure cosmological parameters: base model cosmological parameters: beyond the base model gaussianity and statistical isotropy galaxy clusters conclusions acta polytechnica ctu proceedings doi:10.14311/app.2016.3.0039 acta polytechnica ctu proceedings 3:39–42, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app database finliv – focus on staircase method maxim lutovinov∗, jan papuga, milan růžička faculty of mechanical engineering of czech technical university in prague, technická 4, prague, czech republic ∗ corresponding author: maxim.lutovinov@fs.cvut.cz abstract. this paper introduces finliv database focused on gathering, manipulating and providing experimental static and fatigue data. one of its new features is the ability to include also fatigue tests realized by the staircase method. keywords: fatigue, database, staircase method, fatigue limit. 1. introduction finliv is a database intended to gather the information about static and stressand strain-controlled fatigue experiments and also about parameters of various static and fatigue material models derived from such data. it was developed to resolve the problems of researchers in a lack of quality data, their frequent second-hand use, and the way the data items are selected for various benchmark tests. by now, finliv has a large set of tools for entering and processing data. one of the newest tools is the staircase method [1] that automatically evaluates data from stress-controlled experiments and provides the fatigue limit as a result. 2. finliv finliv is represented by two parts, which closely cooperate, but which also can be used as standalone applications. the first part serves for entering data, while the second part serves for listing them. the second part is implemented as a web database and can be found at www.fadoff.cz/page/finliv. it allows the user to have permanent access to the raw experimental data or to the final regression curves retrieved from them. in the web part there are no tools to process the data, it simply retrieves and lists them on a request in a raw or processed form. the first part, finliv.vba [2], was built as an ms excel application written in visual basic for applications, and its main purpose is to enter experimental data and to process them. data processing is necessary in order to e.g. perform regression analysis or to prepare automated input for fatigue solvers, if a particular experimental data set has to be used within a benchmark of a particular calculation method. the ms excel platform was chosen because of its prevalence among engineers, and because it is substantially cheaper than matlab. the application can be accessed from any computer which has ms excel installed. the main interface of finliv.vba is represented by "form" sheet (see the part of the input interface in figure 1). it consists of a group of tables, combo boxes and buttons. data input is realized by filling in the salmon colored cells and by choosing options from the combo boxes. in the first non-empty column there are designations that correspond to the input parameters. the same designations are used in the datasheets (figure 2), where the material data are stored. the datasheets are placed in the same workbook as the “form” sheet, and their structure is quite simple: in the second column there are designations that represent the entered parameters, while the other columns contain information on individual curves of the particular data set. finliv works with data from static experiments and stressand strain-controlled fatigue experiments. since each type of experiments uses a different set of parameters, the “form” sheet changes its structure to accommodate the selected type. in addition to entering data, finliv.vba can also process data. with the help of the application the user can easily perform regression analyses of experimental data and obtain corresponding regression parameters. for strain-life data there are two types of a regression analysis. the first one is carried out in a conventional way, which is represented by linear regression using the least square method. the second method performs non-linear regression according to the 3-d method [3]. the 3-d method is based on the assumption that one value of the total strain amplitude corresponds to only one stress amplitude and to a single number of cycles. if this assumption is valid a curve can be drawn in a 3-dimensional space which besides formulation of the total characteristics depicts also plastic and elastic strain. unfortunately, implementing such a non-linear 3-d regression in excel is problematic, therefore it was decided to carry out the regression analyses in an external matlab application. to prepare an input file for that application the user should click "input for regression" button. to load the resulting parameters of the regression analysis to finliv, the user should click "get regression data" button and choose the output file created by the matlab application. for stress-life data, there are also two types of a regression analysis, but unlike the case of strain-life 39 http://dx.doi.org/10.14311/app.2016.3.0039 http://ojs.cvut.cz/ojs/index.php/app m. lutovinov, j. papuga, m. růžička acta polytechnica ctu proceedings figure 1. "form" sheet of finliv with sample data. figure 2. a datasheet of finliv with sample data. data both types of the regression are carried out in the excel environment. regression analyses of s-n data as well as a visual display of obtained e-n curves are available in another workbook that is generated automatically from finliv. individual sheets in that workbook correspond to the data sets that were selected for processing. at each page of such data there are two plots of regression curves. in the case of strain-life data, there are two manson-coffin curves, constructed on the basis of parameters obtained from conventional regression analyses and 3-d analyses. in the case of stress-life data, the first regression curve is represented by the basquin relation and another one by kohout-vechet relation. for s-n data, a new tool is also available in the same workbook the staircase method, which is described below. 2.1. staircase method the staircase method is a standardized method [1] for carrying out and evaluating experiments in order to determine the fatigue limit related to a given number of cycles. the essence of the method is to increase or decrease the load amplitude of a new test specimen by a constant pre-selected value based on the response of the previous specimen, i.e. whether a failure occurred during the previous experiment. for evaluation, the staircase method uses a special table (figure 3) constructed according to the standard iso 3800 [1]. the rows of the table represent stress levels and the columns represent the order of the experiments. a symbol “o” is entered into the appropriate cell when a failure doesn’t occur, and a symbol “x” in the opposite case. if the essence of the method has been respected, then the symbols “x” and “o” are arranged in the table into the sequence that 40 vol. 3/2016 database finliv – focus on staircase method figure 3. process of generating the output table according to the staircase method in finliv. looks like stairs. in case of a suitable choice of the first stress level and a step size between individual levels, the stress levels after several experiments (about 10 experiments) will oscillate around a certain value – the fatigue limit. the fatigue limit and the corresponding standard deviation can be then calculated with the help of the equations given by the standard [1], which uses values from the left part of the table (figure 3, columns 3 to 8). the fatigue limit labeled as sig_50 in figure 3 is calculated according to: sig_50 = σao + ∆σall( a c + x) (1) here, σao is the lowest load amplitude level at which the first non-failed specimen appears, given that the total sum of the non-failed specimens is less than the total sum of the failed specimens. in the opposite case, the load level corresponding to the first failed specimen should be input. the standard doesn’t specify how to proceed in the case when the total sums of the failed and non-failed specimens are equal. the observations show that in such case the result will be the same regardless of whether failed or non-failed specimens are selected as the reference type. the algorithm implemented in finliv in cases like that calculates the fatigue limit in two steps, with the failed and non-failed specimens as the reference type and then chooses the lowest fatigue limit. the parameter ∆σall is the step size between individual load levels. a and c are sums of the values in the columns z*f and f. the parameter x is equal to +0.5 when the number of the non-failed specimens is lower than the number of the failed specimens, or -0,5 in the opposite case. it is worth noting that the method can be applied to the load levels represented by stress as well as to the levels represented by forces. the result is then the fatigue limit or the force corresponding to the fatigue limit. the parameter s(sig) is a standard deviation of the distribution and is calculated according to: s(sig) = 1.62∆σall( ce −a2 c2 + 0.029) (2) where e is the sum of values in the column zˆ2*f. the staircase method was extended in finliv, and the application analyzes whether the data are suitable for being processed by the staircase method at all. thanks to that, the method can also be used on data that were obtained from experiments initially unintended to be processed by the staircase method. if the data are suitable for the method, finliv automatically draws an output table (figure 3). the algorithm that analyzes data from the selected load levels assembles various combinations that differ 41 m. lutovinov, j. papuga, m. růžička acta polytechnica ctu proceedings in the step size between levels and/or by the number of levels. then individual combinations are checked according to the criteria that say whether individual sets of load levels and corresponding sets of specimen states (failure, non-failure) are suitable for evaluation by the staircase method. these criteria are derived from the essence of the method. for example, one of the criteria says that if the number of the non-failed specimens at the highest load level is more than one, then such set of load levels and specimen states is not suitable for the staircase method. according to the method, the appearance of a non-failed specimen leads to increasing the value of load amplitude. if the experiment with such specimen is not the last one, then the next experiment should be carried out at a higher level of load amplitude, which means that the level of load amplitude corresponding to the non-failed specimen in question is not the highest level in the particular set of experiments. in the other case, if the experiment at the highest load level with non-failed is the last one, then at the same level there cannot be other non-failed specimens. after selected data are checked by the criteria, finliv provides the user the list of possible combinations of load levels and corresponding steps to choose from (figure 3). the combinations are ordered by the number of included specimens. for each combination there are also listed corresponding step sizes and calculated fatigue limits. while selecting a combination it is important to check the ratio of the fatigue limit and the step size. the smaller is the ratio, the more accurate the estimate should be. the drawback of the implemented check is that it works only with load levels and can’t take into account the possibility of individual specimens being removed from evaluation in order to assemble a suitable combination of the load levels and specimen states. 3. summary the paper refers to finliv database for storing, listing and manipulating experimental static and fatigue data. it describes its newest feature, which is the ability to process data by the staircase method. acknowledgements the authors thank for the support of their research by sgs14/181/ohk2/3t/12 ctu grant. references [1] iso 3800:1993(e). threaded fasteners axial load fatigue testing test methods and evaluation of results. switzerland: international organization for standardization, 1993. [2] j. papuga, m. lutovinov. help for finliv.vba excel database [ver. c], fme ctu in prague & evektor, spol. s.r.o., prague 2014. [3] a. nieslony, c. dsoki, h. kaufmann, p. krug. new method for evaluation of the manson–coffin–basquin and ramberg–osgood equations with respect to compatibility. international journal of fatigue 30(1011):1967–1977, 2008. doi:10.1016/j.ijfatigue.2008.01.012. 42 http://dx.doi.org/10.1016/j.ijfatigue.2008.01.012 acta polytechnica ctu proceedings 3:39–42, 2016 1 introduction 2 finliv 2.1 staircase method 3 summary acknowledgements references 255 acta polytechnica ctu proceedings 1(1): 255–258, 2014 255 doi: 10.14311/app.2014.01.0255 probing gravitational theories with eccentric eclipsing detached binary stars leopoldo milano1,2, rosario de rosa1,2, mariafelicia de laurentis1,2, fabio garufi1,2 1dipartimento di fisica universita’ federico ii di napoli complesso universitario di monte s. angelo, via cinthia, i 80125, napoli, italy 2sezione infn di napoli,complesso universitario di monte s. angelo, via i 80125, napoli, italy corresponding author: milano@na.infn.it abstract in this paper, we compare the effects of different theories of gravitation on the apsidal motion of eccentric eclipsing detached binary stars. the comparison is performed by using the formalism of the post-newtonian parametrization to calculate the theoretical advance at periastron and compare it to the observed one, after having considered the effects of the structure and rotation of the involved stars. a variance analysis on the results of this comparison shows that no significant difference can be found due to the effect of the different theories under test with respect to the standard general relativity (gr). it will be possible to observe differences, as we would expect, by checking the observed period variation on a much larger lapse of time. keywords: relativity gravitation eclipsing binaries apsidal motion. 1 introduction the problem of the motion of two bodies under their mutual gravitational attraction and the study of binary stellar systems has always been the ideal test bed for the theories of gravitation. several authors in the last decades dedicated a lot of work in analyzing, both on the theoretical and the experimental point of wiew, the phenomenon of the periastron precession in binary systems to test various gravitational theories [1, 2] as well as to find correction to the newtonian and general relativistic behaviour of the systems due to stellar form factors, spin, tides and other phenomena [3]. the classical effect of general relativity (gr) on the apsidal motion rate at periastron is well known since long time and described by levi-civita in a famous paper in 1937 [4, 5]. another possible formulation of the problem, that allows also to test other gravitational theories besides gr, is the use of parametrized post newtonian (ppn) formalism [6, 7]. using this formalism, the different gravitational theories can be compared side by side on the basis of a set of post-newtonian (pn) parameters: the masses, the system major semiaxis and the eccentricity. thus, using a sample of eccentric eclipsing detached binary (eedb) systems, for which masses and orbital parameters are known with sufficient precision, it is possible to compare the apsidal motion rate at periastron ω̇th, as expected in the different theories with the observations in order to verify whether the observations can select one theory or another. the choice of this class of stellar objects to test the theories is dictated by the circumstance that the both orbital and the structural parameters can be precisely determined by observation of the eclypses (the only alea being the orbit plane observation angle), and that in close stellar orbits, the gravitational field is supposed to be strong, thus enhancing eventual effects of deviations from the classical theory. there are so many aspects of binary star evolution and angular momentum exchange (see, e.g., [8]) that any attempt to dig out from these other effects the subtleties of gr could seem futile, nonetheless, we consider useful to ascertain whether from the observation of many binary systems, some statistical information about the prevalence of one or another theory of gravitation can be extracted and to ground the bases of a method that can be used when other more significant data will be available. 2 advance at periastron the idea of considering relativistic gravitational tests in terms of a metric expansion is originally based on a work by shiff [9] who expanded the single body metric in terms of the ratio between the geometrized mass mg = gm/c2 and the distance r: g00 = 1− 2α mg r + 2β (mg r )2 255 http://dx.doi.org/10.14311/app.2014.01.0255 leopoldo milano et al. g0k = 0 gik = − ( 1 + 2γ mg r ) δik i, k = 1, 2, 3 (1) four new parameters α′, α′′, α′′′, ∆ were then introduced to account for relative velocities and accelerations. for general relativity all the parameters are equal to 1 and the advance at periastron can be verified to reproduce the ”classical” formula by levi civita [4]. we conveniently modified the ’classical’ formula by introducing a factor (kth) to take into account the dependance on the theory dependent pn terms in order to test the different relativistic theories. [10]: ω̇rel = 1.8167× 10−4kth (m p ) 2 3 c2(1− e2) (2) where: kth = αth(8∆th − αth + 2α ′′ th − α ′′′ th − γth − α ′ th) 2 (3) the pn parameters, are calculated for the different gravitational theories , i.e. the general relativity (’classical’ term), the nordvedt, the brans-dicke theories and the so called f(r) theories that take into account higher order terms of the ricci scalar r, giving a general expression for the relativistic term ω̇rel, that contributes to the advance at periastron. using for the different theories the appropriate values of αth, α ′ th, α ′′ th, α ′′′ th,∆th and γth the numerical values of kth can be obtained [10]: kth =  kgr = 3→ (general −relativity) kbd = 19 7 → (brans−dicke) knd = 11 4 → (nordvedt) kf(r) = 13 4 → (f(r)) (4) 3 comparison with experimental data to test the effects of deviations from the gr, we choose to study binary stellar systems with small radius orbits, so that the gravitational field is strong enough to evidence these deviations, if any. among the various binary stars catalogues available in literature, we choose a sample of eccentric eclipsing detached binary stars such that the period, the eccentricity, the masses of the components, and, possibly, the observed internal structure function are known with a good precision as e.g. [11]. for these systems the passage at periastron precedes in a way that is precisely predictable from the gravitational theory, once given the stellar parameters such as masses, radius of the components, and orbital parameters. to compare the global rate of theoretical apsidal motion in a binary system with the measured one we must take into account the individual contributions of each component due to tidal and rotational distortions, and the general relativistic term ω̇th, where the index th indicates the theory under test (e.g. ωgr for general relativity). assuming that rotation of both components of an eclipsing binary system is perpendicular to the orbital plane, the apsidal motion rate, ω̇ is given by the following simple relation [12]: ω̇obs = ω̇cl + ω̇rel (5) where ω̇cl is the classical newtonian term and ω̇rel is the relativistic contribution of eq. 2 and eq. 4. the dependance of ω̇cl on the binary system parameters is expressed through the internal second-order constants (isc): k̄2th = c21k21th + c22k22th c21 + c22 (6) k̄2obs = ω̇cl c21 + c22 (7) where the parameters c2i are related to the masses and the orbital eccentricity of the binary system. it must be noticed that the individual isc’s k2,i cannot be obtained from the observations although they can be interpolated from evolutionary codes like those used in [13, 14]. so we can evaluate a mean model dependent k̄2th and a mean observation dependent k̄2obs, and compare them to test the evolution stellar models from the observations of apsidal motion. taking into account that k̄2obs is generally smaller than k̄2th (this means that the evolution models predict stellar cores less dense than those found by observed data), remembering eq. 2 and eq. 5 we see that ω̇cl will vary according to ω̇th. in this way we can test the different relativistic theories of gravitation by verifying whether the agreement of the model dependent mean isc, with those coming from observations is significantly improved by using the different ω̇th relativistic terms. in fig. 1 we show the trend of the apsidal motion rate ω̇gr vs ω̇gr,bd,nd,f(r). it results: ω̇bd ∼= 0.92ω̇gr, ω̇nd ∼= 0.90ω̇gr, ω̇f(r) ∼= 1.10ω̇gr. obviously the numerical coefficients are the ratios kth kgr (see eq. 4). it is interesting to note that the f(r) theory gives a relativistic contribution that is slightly higher than gr,bd and nd. moreover, gr is ≈ the mean between f(r) and bd and nd theories. it is also evident that there is no significant difference among the theories under test within the errors. in fig. 2 we show the trend of observed ω̇obs vs ω̇rel for different relativistic terms (th ≡ gr,bd,nd, f(r)). the red line is the trend of ω̇rel = ω̇obs. it is evident that, apart 256 probing gravitational theories with eccentric eclipsing detached binary stars from a few systems, the relativistic term is always less than the observed one. 0 0.5 1 1.5 2 2.5 3 3.5 x 10 −3 0 0.5 1 1.5 2 2.5 3 3.5 x 10 −3 dω/dtgr d ω /d t g r ,b d ,n d ,f( r ) dω/dt gr dω/dt bd dω/dt nd dω/dt f(r) figure 1: ω̇gr vs ω̇gr,bd,nd,f(r) for the different relativistic theories (gr,bd,nd,f(r)): ω̇gr = ω̇gr, ω̇bd ∼= 0.92ω̇gr, ω̇nd ∼= 0.90ω̇gr, ω̇f(r) ∼= 1.10ω̇gr fig. 3 shows the isc’s comparison: log(k̄2obsth ) vs log(k̄2stellarmodel) are shown for different relativistic terms. the blue line is the trend of log(k̄2stellarmodel) = log(k̄2obsth ). it is evident that, apart from a few systems, log(k̄2stellarmodel) is always greater than the observed one. so the stellar core densities derived from the observations is higher than those coming from stellar model prevision. −0.02 0 0.02 0.04 0.06 0.08 0.1 0.12 0 0.5 1 1.5 2 2.5 3 3.5 x 10 −3 dω obs /dt dω re l/d t dω rel /dt=dω obs /dt figure 2: observed ω̇obs vs ω̇rel for different relativistic terms (th ≡ gr,bd,nd, f(r)). the red line is the trend of ω̇rel = ω̇obs. it is evident that apart from some systems the relativistic term is always less than the observed one. 4 discussion and conclusion using data coming from apsidal motion rate of eedb we compared the variation of the relativistic term of the apsidal motion rate due to different theories of gravitation, that accordingly produces variation of classical newtonian term (see eq. 5). the results of this comparison was that we could not find any significant difference due to the effect of the different theories under test with respect to the standard general relativity. since the advance at periastron accumulates, the trend and the amount of this motion can be better determined by the observation of more orbits (or a larger fraction of orbit). longer observations also improve the determination of isc’s; thus, it would be possible, perhaps, to observe more significant differences, by checking the period variation on a much larger lapse of time and verifying the assumptions of syncronous orbital and rotation motion of the binary star components. a lot of observing work are producing new and more accurate data and step by step it is getting a better agreement between theory and observations. −4.5 −4 −3.5 −3 −2.5 −2 −1.5 −1 −2.6 −2.4 −2.2 −2 −1.8 −1.6 log k2obs th lo g k2 s te lla r m od el hp aur bm mon hh car v1765 cyg δ ori ι ori log k2 obs th =log k2 stellar model figure 3: internal second order structure constants (isc) log(k̄2obsth ) vs log(k̄2stellarmodel) for different relativistic terms (th ≡ gr,bd,nd, f(r)). the blue line is the trend of log(k̄2stellarmodel) = log(k̄2obsth ). it is evident that apart from some systems log(k̄2stellarmodel) is always greater than the observed one. so the stellar core according to the observations is more dense than the stellar model prevision. acknowledgement this work was supported by infn grant 2011.the authors gratefully acknowledge the referee prof. todor stanev for his useful suggestions. references [1] breen b., 1973, j. phys. a: math., nucl. gen., 6, 150. 257 leopoldo milano et al. [2] l. lin-sen, 2010, astrophys. space sci., 327, 59. doi:10.1007/s10509-010-0267-4 [3] giménez a., claret a., 2010, astron. and astroph. 519, a57. [4] levi civita t., 1937, amer. j. of math., 59, 225. doi:10.2307/2371404 [5] giménez a., 1985, astroph. j., 297, 405. doi:10.1086/163539 [6] thorne k.s., will c.m., 1971, astrophys. j., 163, 595. doi:10.1086/150803 [7] nordtvedt k., 1969, phys. rev., 180, 1293. doi:10.1103/physrev.180.1293 [8] biermann, p., et al. 1985, astrophys. j., 293, 303 [9] schiff l.i. , 1967, relativity theory and astrophysics vol 1, ed j ehlers 1967 (philadelphia: american mathematical society) [10] m. de laurentis,r. de rosa,f. garufi & l. milano,2012,mnras, 424, 2371-2379 [11] bulut i., demircan o., 2007, mon. not. r. astron. soc. 378, 179. [12] kopal z., dynamics of close binary systems. reidel,dordrecht (1978) [13] claret a., giménez a., 1992, astron. and astroph. suppl. 96, 255. [14] claret, a. 2004, a&a, 424, 919 doi:10.1111/j.1365-2966.2007.11756.x discussion jim beall: what systems would give a proper test? leopoldo milano: the systems that give a proper test are about eleven. carlotta pittori: do you think that it could be useful to study in more datail the outliers? which kind of obsevations could help to constrain the theory? leopoldo milano: many group of astronomers are doing new observations on the outliers with the aim of improving the knowledge on the rotations velocities and other parameters that can be the cause of the failure of the simple model that is generally adopted. 258 http://dx.doi.org/10.1007/s10509-010-0267-4 http://dx.doi.org/10.2307/2371404 http://dx.doi.org/10.1086/163539 http://dx.doi.org/10.1086/150803 http://dx.doi.org/10.1103/physrev.180.1293 http://dx.doi.org/10.1111/j.1365-2966.2007.11756.x introduction advance at periastron comparison with experimental data discussion and conclusion acta polytechnica ctu proceedings doi:10.14311/app.2016.5.0044 acta polytechnica ctu proceedings 5:44–46, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app railway infrastructure capacity management for ad hoc trains on the sždc network petr nachtigall∗, martin škárek dopravní fakulta jana pernera, univerzita pardubice, studentská 95, 532 10 pardubice ∗ corresponding author: petr.nachtigall@upce.cz abstract. the paper describes basic principles of ad hoc routes assignment. each carrier has its own interface called information system kadr with sždc for capacity requests management. the paper describes all steps which must be done before train departure keywords: informition system, carrier, ad hoc train, railway infrastructure capacaty. 1. introduction for last couple of years is growing volume of request from railway operators to infrastructure manager (sždc) for so called ad hoc trains [1]. these trains are operated out of the regular construction of the timetable. to make this agenda easier, there was developed an information system called isoř kadr. the effects of the implementation of this system were in much faster and streamline assignment of the ad hoc routes. faster is as well the distribution of the time table to all supporting information systems. among the most important systems which are linked with kadr belong isoř (information system for operative control), compost (train composition) and aport (preparedness and composition of the train). during autumn 2015 kadr stopped being just a planning program, but it was implemented into the basic operation of the traffic. via kadr are constructed deflecting routes by traffic incidents and by traffic situation which requires that the train is going on different than basic route. the sždc has also competency to set the request instead of the carrier and assign the route and the capacity in one step. 2. basic information about kadr information system kadr has two main parts. there is a web part and a desktop part. the access rights for both parts of the system are restricted by roles in the system. there are five basic roles: • carrier – in this role are open up all functions for carriers. this role is available only as a web part, • billing – in this role you can use all functions of the program, • oss – one stop shop – construction of the route, • da – dispatcher – construction of the route, • tnack restrictions – construction of the time table by track restriction (available only in desktop part). each user must be authorized before entering the kadr software. for authorization there is used the logserver. on the logserver are saved all types of roles and for each role are assigned users. after successful authorization the logserver returns back the role (or more roles) for the user. the system automatically starts the interface with functions and data for user’s role [2]. 3. web part of the application the web part of kadr is available anywhere on public internet at the website of the infrastructure manager (http://provoz.szdc.cz/kadr). this part is used mainly by carriers pro submitting of their new requests for assignment of the capacity, for activation and deactivation of trains, for statistics and so on. on the figure 1 is a basic screen of the web part for the carrier after log in. the basic screen has some bookmarks with groups of functions: • requests/djř (day time table) – on this bookmark are all routes of the carrier (including routes from the year time table). each row is one train and carrier can see their basic information and the application status. at the end of each row are icons for work with each request. • activation – this bookmark is for changing of the train status. the carrier can activate the train (train will be really operated), deactivate the train (carrier doesn’t use the capacity that day or period), put together some routes and submit a request for re-activation of the detached train. • train preparation – carrier can set the analysis of the train and preparation of the train for the departure. both information are absolutely necessary for train operation. • restrictions – link for domin (database of infrastructure restrictions) application, where can be find actual track restrictions and other incidents. • carriers – the list of carriers is in register of the infrastructure manager (sždc). this list is in the system called kafr (catalogue of carriers). each carrier can find here basic information about other carriers as well as contacts for responsible people. 44 http://dx.doi.org/10.14311/app.2016.5.0044 http://ojs.cvut.cz/ojs/index.php/app vol. 5/2016 railway infrastructure capacity managment for ad hoc trains figure 1. basic screen of the web part [2]. • numbered lists – there is an overview of all available numberings, such as: . numbered list of engines – information from the information system revoz (register of engines) – basic information about engines and special vehicles. . services – there is a numbered list of services, which are offered by infrastructure manager for ad hoc routes. . operations – numbered list of acts, this can be requested by a carrier. . products – numbered list of products, this can be assigned to a request. • archive – archive of data from previous time tables. • statistics – carrier has to available 4 types of statistics: . charges for capacity assignment – carrier can see financial costs for capacity assignment for any period. . set of capacity requests – list of all capacity requests. requests can be filtered or exported according to various parameters. . set of time tables – list of all assigned requests. requests can be filtered or exported according to various parameters. . day set of time tables – day list of all route of trains. trains can be filtered or exported according to various parameters. probably the most important feature of the web part of kadr is for the carrier submitting of the application. the carrier must fill in step-by-step the following information: • schedule – carrier must choose days for which he submits the request. there are three types of requests. type c – less than 3 working days (the train departs less than 3 days from the request). type b – more than 3 working days (the train departs 4 of more days after the request). this distribution is for easier preferences by capacity assignment. • route of the request – carrier finds his requested route on the map. • basic information about a train – carrier must fill in all mandatory data such as: train engines, weight, length, used type of the brake, category and type of the train. • extending data – here are stated other train parameters, transport of dangerous goods, special load, military transport, services on the train. after completing the entire information carrier is allowed to forward the application to the interfaces of the infrastructure manager. next possibility for submit of the request is via data communication, when carrier has its own software which is compatible with kadr. the data interface is in the format of tsi taf. this requires bidirectional communication between kadr and carrier’s information system. this interface shall be in defined format tsi taf with annexes. nowadays is valid version 5.17 and during this year will be implemented new version 2.1. the web part of the application is for the infrastructure manager very similar to the carrier’s web part. the infrastructure manager doesn’t use this part very often, because most of his usually used functions are in the desktop part. 4. desktop part of the application the desktop part of kadr is available only for infrastructure manager. the installation is executed 45 petr nachtigall, martin škárek acta polytechnica ctu proceedings figure 2. desktop part of the application [2]. through the web part. the work with the desktop part is possible only from the sždc intranet. the infrastructure manager is setting up the time table of ad hoc trains in this part of the application. here can be also authorized the carrier’s request for the ad hoc trains or prepare the aids of the time table like dispatch or tabular time table. the basic screen of the desktop part after authorization is at the figure 2. 5. conclusions the information system kadr becomes during its existence one of the most important planning tool for basic operation of the railway transport. without its existence isn’t nowadays possible ride of any train, because kadr secures activation and deactivation of trains and information system isoř on request of kadr establish the route into all other information systems. the sždc offers to all carriers the web part of kadr for free. each carrier pays only charges and fees for capacity assignment and using of railway infrastructure according to the czech law [3]. references [1] document of infrastructare manager "prohlášení o dráze celostátní u regionální". [2] internal materials of the company oltis group a.s. [3] law nr. 266/1994 sb., o dráhách. 46 acta polytechnica ctu proceedings 5:44–46, 2016 1 introduction 2 basic information about kadr 3 web part of the application 4 desktop part of the application 5 conclusions references 217 acta polytechnica ctu proceedings 2(1): 217–221, 2015 217 doi: 10.14311/app.2015.02.0217 the slow nova v1280 sco: a short review h. naito1 1graduate school of science, nagoya university, furo-cho, chikusa-ku, nagoya 464-8602 corresponding author: naito@phi.phys.nagoya-u.ac.jp abstract we summarize the results of the extremely slow nova v1280 sco and discuss the approach using discrete multiple blueshifted absorption lines, such as metastable he i* and na i d, detected in our high-resolution spectra. keywords: cataclysmic variables classical novae optical spectroscopy photometry individual: v1280 sco. 1 introduction a nova occurs in a binary system consisting of a white dwarf (wd) and a normal star. the correlation between the wd mass and the decline rate of the light curve is widely accepted (e.g. hachisu and kato 2006), and the nova which occurs on low mass wd tends to decline in brightness at a slow rate and shows slow ionization evolution of its ejacta. a slow nova provides us a good opportunity to perform detailed observation over a long duration. in this review, we summarize the results of the extremely slow nova v1280 sco and discuss the approach using discrete multiple blue-shifted absorption lines, such as metastable he i* and na i d, detected in our high-resolution spectra. 2 summary of v1280 sco 2.1 initial observations v1280 sco was independently discovered by two japanese amateur astronomers (y. nakamura and y. sakurai) at the position of r.a. = 16h57m41s.0, decl. = −32◦20’ 36”.4 (equinox 2000.0) on 2007 february 4 at ninth visual magnitude (yamaoka et al. 2007). it was identified as a classical nova by naito and narusawa (2007) from a low resolution spectrum obtained on february 5.87 (one day after the discovery). it reached the maximum brightness of v = 3.78 mag on february 16, which was 11.3 days after its discovery (munari et al. 2007). the amplitude (a), the magnitude difference between pre-outburst and maximum brightness, is 15 mag or larger because das et al. (2008) noted that no star was visible down to b and r magnitudes of 20.3 and 19.3, respectively, at the position on pre-discovery plates. the notable point is that v1280 sco showed a remarkable formation of dust in its very early phase (das et al. 2007). this dust formation was directly detected using eso’s very large telescope interferometer (vlti) by chesneau et al. (2008) and this result was published as the eso press release (eso0822: http://www.eso.org/public/news/eso0822/). 2.2 infrared observation das et al. (2007) observed the nova in the nir region on 2007 march 4.95, and found that the continuum in the 1.08-2.35 µm region had risen sharply, indicating dust formation in the nova ejecta. das et al. (2008) suggested that the dust was in clumps from nir studies of v1280 sco. puetter et al. (2007) reported spectroscopic observations in the visual-nir regions carried out in 2007 may, and found that the nova was in a very low-excitation state showing strong c i lines and no discernible he i emission. 2.3 high spatial resolution observation high spatial resolution monitoring of the dust formation event was performed using the vlti during the first four months following the discovery, indicating that the dusty shell expanded regularly (chesneau et al. 2008). chesneau et al. (2012) revealed the presence of a dusty hourglass-shaped bipolar nebula around v1280 sco based on mid-infrared imaging observations taken in 2010 and 2011 using the vlt spectrometer and imager for the mid-infrared (visir). 2.4 high quality photometric observation hounsell et al. (2010) published the data set of v1280 sco observed by the solar mass ejection imager (smei) on board the coriolis satellite. thanks to high quality and high time resolution, they revealed that there had been three major but short episodes of brightening near 217 http://dx.doi.org/10.14311/app.2015.02.0217 h. naito maximum light (before 2007 february 20), which had not been detected by any ground-based telescopes. 2.5 distance and wd mass parameters (distance and wd mass) of v1280 published in the literature are controversial (see table 1). hounsell et al. (2010) estimated the distance to be 630 ± 100 pc by measuring the condensation time of dust grains, assuming that the condensation temperature of the dust was 1200 k and the ejection velocity was about 600 km s−1. they also noted that wd mass of 0.6 m� is likely to be an upper limit. on the other hand, chesneau et al. (2008) derived the distance of 1.6 ± 0.4 kpc from direct observations of the size of the expanding shell with velocity of ∼500 km s−1. the discrepancy between these two estimations of distance is over a factor of two, which could result from the complexity in the physical conditions (temperature and velocity) of the dust shell. das et al. (2008) estimated the distance to be 1.25 kpc using the maximum magnitude versus rate of decline (mmrd) relation, and inferred that the higher mass end (1-1.25 m�) may be supported when the amplitude a and the expansion velocity values observed inv1280 sco were taken into account. 3 our results in this section, our results of v1280 sco are summarized. especially we focus on multiple absorption lines detected in high-resolution spectra (see sadakane et al. 2010, naito et al. 2012, naito et al. 2013 for details). photometric and spectroscopic observations have been conducted from february 2007 to july 2013 over table 1: parameters of v1280 sco in the literatures distance [kpc] wd mass [m�] reference 0.63 ± 0.10 < 0.6 hounsell et al. 2010 1.6 ± 0.4 — chesneau et al. 2008 1.25 1.0-1.25 das et al. 2008 1.1 ± 0.5 < ∼0.6 naito et al. 2012 0 2 4 6 8 10 12 14 16 18 0 500 1000 1500 2000 2500 m a g n it u d e s days since maximum v723 cas (vis) -2.8 mag. v1280 sco (v) nebular phase v1280 sco v723 cas figure 1: comparison of light curve and nebular phase between slow novae v1280 sco and v723 cas. light curve of v723 cas is collected from aavso database (http://www.aavso.org) and is shifted by −2.8 mag. v723 cas entered the nebular phase about 18 months after maximum (iijima 2006), while v1280 sco took about 50 months (about three times longer than v723 cas) to enter the nebular phase (naito et al. 2012). 218 the slow nova v1280 sco: a short review six years. photometry in b, v , rc, ic, and y band was carried out with a 0.51-m reflector at osaka kyoiku university. low-resolution spectroscopy (r∼1000) was carried out mainly with 2.0-m nayuta telescope at nishi-harima astronomical observatory and highresolution spectroscopy (r∼60000) was carried out with 8.2-m subaru telescope. according to iijima 2006, v723 cas had been the slowest nova, spending a long time to enter the nebular phase. to compare the evolution between v1280 sco and v723 cas, the light curves and the nebular phases of them are shown in figure 1. v723 cas declines in brightness at very slow rate gradually, while v1280 sco keeps its brightness (v∼10) for 2000 days. v723 cas entered the nebular phase, defined by the appearance of both [o iii] 4959 and 5007, about 18 months after maximum (iijima 2006), while v1280 sco took about 50 months (about three times longer than v723 cas) to enter the nebular phase (naito et al. 2012). considering that v723 cas had the longest transitional time to enter the nebular phase, we conclude that v1280 sco is going through the slowest spectral evolution among known classical novae. hachisu and kato (2004) estimated the mass of v723 cas to be 0.59 m� by fitting their theoretical light curve. our results suggest that the mass of a wd in v1280 sco system might be 0.6 m� or lower by comparing evolution rates between v1280 sco and v723 cas. 0 1 2 3 4 5 5870 5875 5880 5885 5890 5895 5900 in te n s it y + c o n s t. wavelength [ ]å 2009 jun. 16 2010 jul. 1 2011 aug. 6 na d1(is)na d2(is)na d1na d2 2013 jul. 1he i figure 2: multiple high velocity absorption lines associated with na i d1 and d2. we found discrete multiple blue-shifted na i d lines, ranging from −650 to −900 km s−1, on high-resolution spectra (figure 2). some components weakened significantly from 2009 to 2011 and almost all lines disappeared in 2013. similar absorption lines associated with ca ii h and k and metastable he i* 3188 and 3889 are shown on our spectra. metastable he i* 3889 absorption lines were detected for the first time in 2011 (four years after the maximum light) and have been shown until 2013 (figure 3). this is the first detection of he i* absorption lines in the ejected (circumstellar) gas around novae (naito et al. 2013). we suggest that the complex evolutions of multiple absorption lines are due to combined changes in physical conditions, such as the density, recombination and ionization rate. survival time of these absorption lines in v1280 sco is an order of years, which is much longer than those observed among fast novae (an order of weeks or months; williams and mason 2010). this can be related to the fact that the ionization evolution of v1280 sco is very slow. the behavior associated with he i* in 2011 can be understood that the number of ultraviolet photons had increased significantly to produce singly-ionized helium as the central photosphere shrinks to become hotter, and the disappearance of na i d lines low excitation lines in 2013 can be caused by an additional increase in the number of ultraviolet photons. 0 1 2 3 4 5 3820 3830 3840 3850 3860 3870 3880 3890 3900 in te n s it y + c o n s t. wavelength [ ]å 2009 jun. 16 2011 aug. 6 2012 mar. 20 2013 jul. 1 h e i * 3 8 8 9 h i 3 8 3 5 h i 3 8 3 5 ( h 9 ) h i 3 8 8 9 ( h 8 ) s i ii 3 8 5 6 s i ii 3 8 6 3 f e i i 3 8 2 5 s i ii 3 8 5 4 figure 3: multiple high velocity absorption lines associated with he i* 3889. 4 discussion and conclusions as described in the previous section, metastable he i* absorption lines could survive longer than low excita219 h. naito tion lines, such as na i d and ca ii h and k. this means that metastable he i* absorption lines are more likely to be detected than low excitation lines in the late phase. moreover metastable he i* lines are often used to derive physical parameters of nebulosity because the processes of transition are well understood. these characteristics of metastable he i* lines have advantage in measuring helium composition and the mass of the ejected material, and in studying nova shell structures. using metastable he i* lines in v1280 sco, we show that the ejected shell consists of numerous clumpy gas which cover a significant part of the continuum emitting radiation region as figure 4 (naito et al. 2013). we postulate that this approach is very useful to research nova shell. we reveal that v1280 sco is the extremely slow nova and is available for high-resolution spectroscopic observation for long periods. we attempt to obtain new results of v1280 sco by follow-up observations. free-free emission region clumpy gas photosphere { observer figure 4: schematic of ejected shell producing absorption lines of metastable he i* (see naito et al. 2013 for details). acknowledgement i thank dr. akito tajitsu, prof. kozo sadakane and dr. akira arai for longstanding observations and valuable discussion. i also thank prof. iijima for his useful comments. references [1] chesneau, o., et al.: 2008, a&a 487, 223. [2] chesneau, o., et al.: 2012, a&a 545, a63. [3] das, r. k., et al.: 2007, cbet 866, 1. [4] das, r. k., et al.: 2008, mnras 391, 1874. doi:10.1111/j.1365-2966.2008.13998.x [5] hachisu, i., kato, m.: 2004, apj 612, l57. doi:10.1086/424595 [6] hachisu, i., kato, m.: 2006, apjs 167, 59. doi:10.1086/508063 [7] hounsell, r., et al.: 2010, apj 724, 480. doi:10.1088/0004-637x/724/1/480 [8] iijima, t.: 2006, a&a 451, 563. [9] munari, u., et al.: 2007, cbet 852, 1. [10] naito, h., narusawa, s.: 2007, iau circ. 8803, 2. [11] naito, h., et al.: 2012, a&a 543, a86. [12] naito, h., et al.: 2013, pasj 65, 37. [13] puetter, r. c., et al.: 2007, iau circ. 8845, 1. [14] sadakane, k., et al.: 2010, pasj 62, l5. [15] williams, r., mason, e.: 2010, ap&ss 327, 207. doi:10.1007/s10509-010-0318-x [16] yamaoka, h., et al.: 2007, iau circ. 8803, 1. 220 http://dx.doi.org/10.1111/j.1365-2966.2008.13998.x http://dx.doi.org/10.1086/424595 http://dx.doi.org/10.1086/508063 http://dx.doi.org/10.1088/0004-637x/724/1/480 http://dx.doi.org/10.1007/s10509-010-0318-x the slow nova v1280 sco: a short review discussion alessandro ederoclite: how long after the explosion do you see the emergence of the he i* lines? hiroyuki naito: our latest spectrum taken in july 2013, shows the emergence of the he i* lines which indicates that these lines have appeared until at least 6.5 years after maximum. 221 introduction summary of v1280 sco initial observations infrared observation high spatial resolution observation high quality photometric observation distance and wd mass our results discussion and conclusions 231 acta polytechnica ctu proceedings 1(1): 231–234, 2014 231 doi: 10.14311/app.2014.01.0231 data analysis of globular cluster harris catalogue in view of the king models and their dynamical evolution. i. theoretical model marco merafina1, daniele vitantoni1 1department of physics, university of rome la sapienza, piazzale aldo moro 2, i-00185 rome, italy corresponding author: marco.merafina@roma1.infn.it abstract we discuss the possibility to analyze the problem of gravothermal catastrophe in a new way, by obtaining thermodynamical equations to apply to a selfgravitating system. by using the king distribution function in the framework of statistical mechanics we treat the globular clusters evolution as a sequence of quasi-equilibrium thermodynamical states. keywords: globular clusters gravothermal catastrophe king models thermodynamical stability. 1 introduction globular clusters (gcs) are stellar systems with masses within the interval 104 − 106 m�, containing a number of stars of the order of 105. they are considered as nearly spherical systems due to their low values of eccentricity e; at least 50% of gcs have e < 0.1 and there are no clusters with e > 0.2. the core radius rc, namely the radial coordinate at which the brightness becomes one half of the corresponding value at the center of the system, is almost 10 pc, whereas the tidal radius rt, which is the biggest spatial extension of the cluster allowed by the external tidal field, is typically around 50 pc. for their symmetry and age, there is the possibility to test the evolution of a gcs studying a classical single mass king model (king, 1966) in relation to thermodynamical instability phenomena. in fact, in the analysis of the evolution of gcs, stellar encounters strongly contribute in phase space mixing of stellar orbits. in this scenario, thermodynamics plays a centrale role in the gravitational equilibrium and stability of these clusters, being the average binary relaxation time shorter than their old absolute age which ranges between 10 to 13 gyr. this means that fokker-planck approximation, which takes into account the nature of collisions in globular clusters, can determine the distribution function relevant for obtaining the equilibrium configurations of these systems, whereas the tidal effects due to the presence of galactic gravitational potential are responsible of the confination of the cluster. on the other hand, the observations of the luminosity profiles of different gcs (king, 1962) show similar curves depending only on different values of the star concentration, giving the possibility to fit them by an empirical law and suggesting a unique distribution function for the whole sample of clusters (king, 1966). this effect can be described as a change of the main parameters of the cluster during the dynamical evolution (horwitz & katz, 1977), which maintains the form of the distribution like in a sort of reversible trasformation of a gas in thermodynamic equilibrium, also in accordance to numerical simulations existing in literature which result in keeping unchanged the distribution of velocities of stars for a wide range of values of the concentration during the time evolution driven by the fokker-planck equation. therefore, the evolution of globular clusters can be studied by considering small thermodynamic transformations which keep constant the functional form of the velocity distribution of stars like in the framework of boltzmann statistical mechanics. it is important to note that while the equilibrium is given by the form of the distribution which depends on the fokker-planck equation and consider the real nature of collisions, thermodynamics plays a role in the tidal effects acting on the confination of the system, due to a two competitive phenomena: one given by stellar encounters which tend to refresh the tail of high velocities in the distribution and one due to evaporation of stars which prevents the formation of it, maintaining the system in a sort of thermodynamical equilibrium with the same distribution function even if in presence of a cutoff in the velocity of the stars. 2 the effective potential the king df characterizing the energy distribution of stars with the same mass m in a model that describes 231 http://dx.doi.org/10.14311/app.2014.01.0231 marco merafina, daniele vitantoni a spherically symmetric system with isotropic velocity distribution may be written as f(ε) = b [ e−(ε+mϕ)/kθ − e−(ψ+mϕ)/kθ ] for ε ≤ ψ , f(ε) = 0 for ε > ψ . (1) here ψ = m (ϕr − ϕ) is the energy cutoff, corresponding to the maximum kinetic energy that a star can have at a given radial coordinate r, while ϕ is the gravitational potential. this energy is sufficient to reach the border of the equilibrium configuration r = r, being also the difference between the value of the gravitational potential at the edge of configuration and the same quantity evaluated at a generic distance r from the center. the quantity θ is the thermodynamic temperature of the system while b is a constant of normalization. the behavior of equilibrium solutions for king models has been also analyzed by merafina & ruffini (1989) by solving the poisson equilibrium equation in newtonian regime. we can see the presence of a maximum value of the total mass m at increasing values of the central gravitational potential w0, which denotes the arising of a sort of thermodynamic instability at w0 = 1.35 (fig.1). figure 1: mass in function of w0 for families of solutions at different values of the velocity dispersion (merafina & ruffini, 1989). over this value, we can think the system can evolve towards the loss of thermodynamical equilibrium (gravothermal catastrophe), in accordance to the expected evolution of lynden-bell & wood (1968). in order to consider thermodynamic transformations in the framework of statistical mechanics, it is possible to describe the king df like a maxwell-boltzmann one by introducing an effective potential. in this way the evolution of the king models can be treated as a succession of quasi-equilibrium stages by a thermodynamic theory formally equivalent to the classical one. then, the expression of the effective potential is given by φ = −kθ ln [ 1− e(ε−ψ)/kθ ] (2) and the distribution function can be expressed as f = be−h/kθ , (3) where h = ε + mϕ + φ is the single particle hamiltonian of the system which includes also the gravitational energy of the single star. the effective potential is a screen potential which restricts the phase space of the available velocities for the stars and takes into account the effect of the tidal forces on the system. in this way, the kinetic temperature t connected with the average velocity of the stars, depending on the radial coordinate r, becomes distinguished from the thermodynamic temperature θ, constant all over the equilibrium configuration. from the modified boltzmann df of eq.3, we can deduce the generalized thermodynamical quantities, as the energy u , the thermodynamical pressure π and the entropy s, related to a shell with radial coordinate r. we get n = av ∫ ψ 0 f √ ε dε , (4) u = av ∫ ψ 0 fh √ ε dε , (5) π = 1 3 a ∫ ψ 0 fε3/2 dh dε dε , (6) s = kav ∫ ψ 0 f(1− ln f) √ ε dε , (7) where we have replaced the costant b with a, being b = aeα/kθ and now f = ae(α−h)/kθ, while α = µ + mϕ is the chemical potential in presence of the gravitational potential ϕ. in this way we can rewrite the first law of thermodynamics and obtain a new form for the eulero expression, that include the extensive and intensive quantities. we can get also an equation of state formally equivalent to classical one which involves the thermodynamical quantities, valid for a shell with radial coordinate r. we have du = θds −πdv + αdn +n〈dh〉 , (8) u = θs −πv + αn , (9) πv = nkθ (10) 232 data analysis of globular cluster harris catalogue... part i and, for kinetic quantities like temperature t and pressure p , pv = nkt . (11) finally, by integrating the expression of u containing the single particle hamiltonian h (eq.5) all over the configuration, we can find an additional term eeff in the expression of the total energy etot of the system, called effective energy etot = ekin + egr + eeff , (12) where ekin and egr are the total kinetic energy and the total gravitational energy, respectively. the partecipation of the effective potential in the total energy corresponds to the account of the tidal potential which determines a finite radius of the cluster. moreover, eq.5 defines the energy of the test shell but, for calculating egr, we need to use the expression egr = 1 2 ∫ r 0 ρϕ dv . (13) 2.1 the gravothermal catastrophe thermodynamical instability of a selfgravitating spherical system was first studied by lynden-bell & wood (1968), by considering an isothermal sphere (core) confined in a spherical box. using the classical form of the virial theorem, including a boundary term due to spatial truncation of the density prophile, it is possible, for that system, to calculate the critical value of the central gravitational potential w0 = 6.55 after that thermodynamical instability, known as gravothermal catastrophe, onsets. it is important to note that such instability takes place only in presence of an external thermal bath exchanging heat with the core and driving the system towards the dynamical collapse. with the introduction of the effective potential, we can repeat this analysis for king models and get another critical value for the central gravitational potential w0 = 6.9, which differs from the one obtained by katz (1980) w0 = 7.4, due to the additional term in the total energy etot (see eq.12). the most interesting results concern the profile of specific heat for different values of w0 (see merafina et al., in preparation). by analyzing the behavior of the specific heat all over the configuration, we found different results. the expression of the specific heat cv = (dq/dθ)v arises from eq.8, being constant n and v , by using the expression dq = du −n〈dh〉 . (14) • for w0 < 1.35, we have equilibrium configurations with positive heat capacity all over the system. there are not existing conditions for an evolution of the system towards the critical value corresponding to the onset of the gravothermal catastrophe (w0 = 6.9). further, this particular value (w0 = 1.35) corresponds to one concerning the first maximum mass we found among the equilibrium solutions (see fig.1). • for w0 > 1.35, the system shows an external halo with negative heat capacity and an internal core with a positive value. the system can evolve by increasing the value of w0 until reaching the critical value in which the gravothermal instability onsets. these evolution can take place without the necessity of the presence of an external thermal bath, differently from the previously requested condition in the lynden bell & wood model. results showing the specific heat profiles in function of the radial coordinate for different values of w0 are summarized in fig.2. 0.00 0.25 0.50 0.75 1.00 -0.6 -0.4 -0.2 0.0 0.2 0.4 0.6 0.8 c v/ n k r/r figure 2: behaviour of the specific heat in function of the radial coordinate for different values of w0. 2.2 preliminar observational evidences the stability of the king models was analyzed in detail by katz in 1980, with the same investigation carried out by lynden-bell & wood for the isothermal sphere. katz introduced a new parameterk, which corresponds essentially to the ratio between the escape velocity and the dispersion velocity, both calculated at the center of the cluster. this parameter is directly connected with w0. calculations performed by katz showed that models become thermodynamically unstable over the value k = 8.1 (w0 = 7.4). but, analyzing the sample of data coming from peterson & king (1975) and peterson (1976), katz highlighted an unexplainable gap between the expected value of the sample, k = 7.8 equivalent 233 marco merafina, daniele vitantoni to w0 = 6.9, and the one corresponding to the onset of gravothermal instability, resulting at w0 = 7.4 (see fig.3). figure 3: distribution of galactic gcs at different values of k (katz, 1980). we indeed expect that gcs had enough time to undergo the gravothermal catastrophe and, therefore, the distribution of gcs in terms of k or w0 should peak exactly in correspondence to the critical value. in fact, the primeval gaussian distribution, approaching the critical value during the evolution, deforms in a non-symmetric gaussian curve due to the effect of gravothermal catastrophe which progressively subtracts the collapsed gcs with values of w0 larger than the critical value. for these reasons, the resulting distribution must present a maximum which corresponds to the critical value. it is remarkable to note that, with the introduction of the effective potential in the study of the thermodynamical instability, we obtain a critical value, w0 = 6.9, that bridges this gap and corresponds exactly to the expected value of the sample. this correspondence becomes much more evident by considering the sample of harris (1996) with 127 clusters (if we exclude the pcc ones), as well becomes more evident the non-symmetric form of the distribution. on the other hand, by making a z-test in order to verify the statistical significance of the gap between the stability limit w0 = 7.4 expected by katz and the peak value of the distribution at w0 = 6.9, it can be shown that these two values are not compatible within a confidence level of 95%. 3 conclusions • the additional (positive) contribution of the effective potential on the total energy, considering also the virial condition 2ekin +egr = 0, implies that etot = −ekin + eeff . this enables us to construct models in which the core has a positive heat capacity, allowing to assume the possibility of a survival of the system from the gravothermal cathastrophe which could explain the existence of post core-collapsed objects (pcc). • the model is selfconsistent and admits regions with positive and negative heat capacity which can exchange energy and produce gravothermal instability, without the necessity to assume an external bath as in the lynden-bell & wood model. • we obtain a new critical value for the onset of gravothermal instability by the presence of the effective potential. this value coincides with the value of k (or, equivalently, to w0) corresponding to the peak of the gcs distribution, removing the unexplainable difference outlined by katz. this is an observational evidence of the effects due to the presence of the effective potential, confirmed in the analysis of data of more than 150 gcs contained in the last version of catalogue recently published by harris in 2010 (see also harris, 1996). finally, it may be useful to consider some unsolved problems and perspectives in order to develop the analysis of thermodynamical instabilities of gcs. • the model is not a multimass one and does not take into account the effects in the formation of binary stars. at moment this is a preliminary model which has to be improved. • the new possibility of measuring transverse velocities of the stars in gcs opens important perspectives on the knowledge of the distribution of the star orbits and their eccentricity, in order to better develop n-body simulations in supporting the validity of the model. references [1] cohn, h.: 1980, apj, 242, 765. doi:10.1086/158511 [2] harris, w.e.: 1996, aj, 112, 1487. [3] horwitz, g., katz, j.: 1977, apj, 211, 226. doi:10.1086/154924 [4] katz, j.: 1980, mnras, 190, 497. doi:10.1093/mnras/190.3.497 [5] king, i.: 1962, aj, 67, 471. [6] king, i.: 1966, aj, 71, 64. [7] lynden bell, d., wood, r.: 1968, mnras, 138, 495. doi:10.1093/mnras/138.4.495 [8] merafina, m., ruffini, r.: 1989, a& a 221, 4. [9] merafina, m., fragione, g., piscicchia k.: in preparation. [10] peterson, c.j.: 1976, aj, 81, 617. [11] peterson, c.j., king, i.: 1975, aj, 80, 427. 234 http://dx.doi.org/10.1086/158511 http://dx.doi.org/10.1086/154924 http://dx.doi.org/10.1093/mnras/190.3.497 http://dx.doi.org/10.1093/mnras/138.4.495 introduction the effective potential the gravothermal catastrophe preliminar observational evidences conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.12.0038 acta polytechnica ctu proceedings 12:38–41, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app analysis of stored data help to propose and generate new tracks václav jirkovský czech technical university in prague, faculty of transportation sciences, department of vehicle technology. konviktská 20, 110 00 prague correspondence: vaclav.jirkovsky@volny.cz abstract. during experiments on vehicle simulators a large amount of data is stored. on these data, it is possible to trace some similarities in the behavior of drivers in certain areas or when performing the same task. we can assume that if the driver performs a certain type of experiment, his behavior exhibits certain traits. these elements of common behavior can be used to create virtual track for experiments. which elements and how they can be used is described in this article. the algorithm for automatic creation of virtual track based on type of experiment is provided. it will help us to define the purpose of measurement and the track could be generated automatically. keywords: vehicle simulator, measurement, virtual track. 1. introduction conducting of experiments is one of the most important things related to the operation of driving simulators at the faculty of transportation sciences. there are many types of them. they are focused on investigating the driver behavior in fatique[1–3], testing systems for predicting microsleeps[4], humanmachine interaction[5], interaction with surrounding traffic[6, 7] and many more. during their performing the data are collected, which are mostly of a technical nature, and on the other hand, they give us information about the state of the monitored driver. all information about a vehicle, terrain and environment belong the first category. the data collected on a driver's body such as heart beat, eeg, eye view direction, blink rate etc. belong to the second category[8]. after the data evaluation we are able to describe a driver's behavior in particular states of experiment and determine a crisis situations or areas. hierarchical structure of measured data is shown on fig.1 figure 1. hierarchical structure of measured data 2. measured data analysis if the amount of the measured data is sufficiently large, we are able to detect with help of mathematical tools how the drivers react to a given event, incentive or transport situation. we can find out if their reactions are different or identical. it is possible, based on the analysis and using of appropriate tools, to predict the behavior of drivers on virtual tracks if these tracks are only modeled or created without performing of experiments with data collection[9]. on the basis of structure and character of the track, it is possible to determine the place and the moment when the driver will have to solve the crisis situation. but the opposite procedure will be applied. it means to design and construct a virtual track according to the requirements of the type of crisis. on thus obtained results we can create new scenarios with a specific focus. for example the results of the analysis shows that while operating the radio in rugged terrain, a large percentage of drivers do not hold the vehicle on an ideal path and run off the road. it's evident that the equally segmented track is suitable for testing similar devices. based on these derived addiction it is possible to design and construct virtual tracks with greater efficiency. it will also allow it to specialize in one specific purpose. the figure no.2 shows the experimental track. the yellow marks show the places where the value of deviation from the ideal track overlaps 1.5 m. this value indicates that the car doesn't stay in the correct road lane and crosses the middle line to the opposite road lane. this can cause a serious traffic situation with possibility of frontal collision. the chart shows that the deviation from the ideal track is caused by splitting the focus of the driver between the driving and the device manipulation. for more detailed evaluation we can divide the tasks into easy and difficult. an easy task can be done by one 38 http://dx.doi.org/10.14311/app.2017.12.0038 http://ojs.cvut.cz/ojs/index.php/app vol. 12/2017 analysis of stored data help to propose and generate new tracks figure 2. experimental track or two clicks (touch). difficult task needs more time to finish. 3. identifying common elements of behavior during data analysis i've found out that the common behavior patterns could be observed for most types of experiments. with a very high probability we can assume that if the driver performs the measurements under the same conditions as the previous driver, his behavior will show the same elements. by examining the experiments i received the following connection: • assistive devices ragged track • research on driver fatigue monotonous, minimally curved track with minimal distractions • research driver's responsiveness to sound stimuli monotonous track • research driver's responsiveness to obstacles in riding complex traffic situations, poor visibility • driving precision special testing polygon (slalom, braking precision, ride along a line etc.) • overtaking research track with poor clarity (bend, curl, heavy traffic) individual connections determine the characteristics. with their help, i set up a knowledge base. that gives us an idea of which features driver's behavior occur in different types of experiments. that will tell us what behavior we expect on a particular experiment, but in the opposite case it will help us, when examining on the basis of activity to determine the shape of table 1. experimental characteristics the track. characteristics of each experiment can be found in the following table. experiment properties c om pl ex tr ac k r ec om m en de d ve lo ci ty su rr ou nd in g tr affi c li gh t tr affi c h ea vy tr affi c g oo d vi sib ili ty c or ru ga te d tr ac k o bj ec ts reaction speed on sound effects no no yes no no reaction speed on road obstacles yes yes no yes no yes the accuracy of the ride yes no no no driver's fatigue no 90130 km/h no yes no no assistance devices handling yes 50 km/h no overtaking yes yes no yes no yes 4. proposal track by type of experiment a knowledge base is essential for the design of the track, which i described in the last chapter. to create the track i proposed algorithm, which is described below. the entire process can be divided into several steps: • the user determines variables, which aims to examine • distinguishing features are loaded from knowledge base • the track is automatically proposed based on those distinguishing features • the result is a polyline characterizing the road axis in space first the user enters input data. it is primarily a type of experiment. the next steps of propose are fully automatic and the user cannot affect them. based on input values the distinguishing features are obtained from the knowledge base. it means maximal velocity, curvature, longitudinal profile etc. these go to input of an algorithm as a specific values (arcs with radius from 100m to 350m, narrow lines of length from 200m to 1000m etc.). based on the input data the algorithm proposes the whole track. geometric properties of individual building elements comply with standard csn 73 6101. the result is a polyline that determines the 39 václav jirkovský acta polytechnica ctu proceedings points of the track. it can be subsequently imported into other software where it's finalized[10]. 5. the algorithm for automatic generation of experimental tracks the automatic generation of a track is as old as the game industry itself. the limitation of existing platforms did not allow the distribution of a large predefined content. ad-hoc algorithmic procedures were widely used to generate game content on-the-fly. it was called procedural content generation. now, when the distribution of games is not limited by memory space, the automatic generation of the content is still used mainly to reduce design costs. the principle of automatic generation of the track is based on evolutionary computation to evolve track for a simple two-dimensional car racing game[11]. the basic idea is to connect individual segments (lines, arcs) so that they don't cross the other parts. and they gradually point to beginning. the connection of the parts is strictly defined. for example between each line and arc must be placed a spiral. the segment properties are based on the rules mentioned above. additional parameters slope can be added to extend into 3d space to make virtual track more realistic[12]. 6. pseudo-code as described in section four, the type of track is dependent on the type of experiment. it means each track consists of segments with a specific property. the track properties are set at the beginning of the algorithm. in the next step the random segment is randomly selected from the segment list. the list consists of narrow lines of different length and arcs of different length and radius. the end point of the previous segment is the start point of a next segment. the algorithm takes into account the crossing of the segments. if the actual segment crosses the track it is not placed and other segment is chosen. in some cases the algorithm doesn't offer the closed track, therefore, it must be done manually. to reduce the occurrence of these cases, the number of right-handed arcs is bigger than the number of left=handed arcs. once the track has been built, it needs to be smoothen. in this step the spirals are placed between a line and an arc to provide a fluent transition. (1.) var property = settrackproperty() (2.) track=null (3.) object=choose random object from list (4.) object.properties=random(property) (5.) end_point=object.endpoint() (6.) start_point=object.startpoint() (7.) track.insert(object) (8.) do while (start_point != point) (9.) object2=choose random object from list (10.) object2.properties=random(property) (11.) object2.start_point=end_point (12.) point=object2.endpoint() (13.) if(collision(track, object2) == false and suitableposition(object2, start_point) == true) (14.) track.insert(object2) (15.) calculate parts connection (16.) if(distance(start_point, point) < minimal_distance) (17.) break (18.) else (19.) point=end_point (20.) loop (21.) connect point and start_point (22.) track.smooth() 7. conclusions the measurements on a vehicle simulator and data analysis confirmed that the use of assistance and media devices can directly cause a dangerous behavior of the driver. those devices should be designed to reduce driver's attention and thereby minimize dangerous situations on the road. thorough tests could help us to determine which devices are suitable for using in a car and which are not. the analysis also showed that there are connections between driver's behavior and track's properties and conditions of the measurement. the connections define rules that can be used during creating of the new tracks. in the future we will be able to define purpose of measurement and the track will be generated automatically. the described algorithm for creating a track is one of many possible. it's easy to understand and fulfills the purpose. a number of track were generated during testing. many of the tracks were useful and usable as a basis of a new created track. their use is one of the steps to improve the quality of experiments on vehicle simulators. references [1] p. bouchner, r. pieknik, s. novotny, et al. fatigue of car drivers – detection and classification based on the experiments on car simulators. 2006, wseas transactions on systems, 5 (12), pp. 2789-2794. [2] p. bouchner. a complex analysis of the driver behavior from simulated driving focused on fatigue detection classification. 2006, wseas transactions on systems, 5 (1), pp. 84-91. [3] p.bouchner, m.hajny, s.novotny, et al. car simulation and virtual environments for investigation of driver behavior. 2005, neural network world, 15 (2), pp. 149-163. 40 vol. 12/2017 analysis of stored data help to propose and generate new tracks [4] p. spurny, j. andrs, p. bouchner, et al. testing a system for predicting microsleep. 2016 lekar a technika, 46 (2), pp. 51-54. [5] p. bouchner, s. novotny. system with driving simulation device for hmi measurements. 2005, wseas transactions on systems, 4 (7), pp. 1058-1063. [6] m. matowicki, o. pribyl, p. bouchner. pragmatic overview of surrounding traffic implementation into driving simulator. elektro 2016 – 11th international conference, proceedings, art. no. 7512111, pp. 423-428. [7] h. klee. microscopic car modeling for intelligent traffic and scenario generation in the ucf driving simulator. [8] p. bouchner. driving simulators for hmi research. phd. thesis, ctu. [9] r. pieknik. the methodology of creating scenario roads of driving simulator for different types of experiments. conference of driver-car interaction and interface 2009. [10] a. orlicky. automatic generation of road infrastructure in 3d for vehicle simulators. diploma thesis, prague 2016. [11] j. togelius, r. de nardi, s. lucas. making racing fun through player modeling and track evolution. [12] d. loicono, l. caramone, p. lanzi. automatic track generation for high-end racing games using evolutionary computation. 41 acta polytechnica ctu proceedings 12:38–41, 2017 1 introduction 2 measured data analysis 3 identifying common elements of behavior 4 proposal track by type of experiment 5 the algorithm for automatic generation of experimental tracks 6 pseudo-code 7 conclusions references 56 acta polytechnica ctu proceedings 1(1): 56–65, 2014 56 doi: 10.14311/app.2014.01.0056 multi-frequency study of the sz effect in cosmic structures sergio colafrancesco1 1university of the witwatersrand, johannesburg (south africa) corresponding author: sergio colafrancesco. email: sergio.colafrancesco@wits.ac.za abstract the sunyaev-zel’dovich effect (sze) is a relevant probe for cosmology and astrophysics. a multi-frequency approach to study the sze in cosmic structures turns out to be crucial in the use of this probe for astrophysics and cosmology. astrophysical and cosmological applications to galaxy clusters, galaxies, radiogalaxies and large-scale structures are discussed. future directions for the study of the sze and its polarization are finally outlined. keywords: cosmology cmb dark matter dark energy cosmic magnetism cosmic structures: galaxy clusters, galaxies, radio galaxies. 1 introduction galaxy clusters, the largest gravitationally bound structures in the universe, are the representative systems of the distribution of lss in the universe. the description of these cosmic structures is continuously enriching of physical details regarding their matter and field content. dark matter (dm) is the dominant form of matter that creates the potential wells of cosmic structures, from those on the largest scales down to galactic and sub-galactic scales. if we consistently take into account the fundamental nature of dm particles, we are inevitably bound to consider the effects of their annihilation or decay on the structure and evolution of the dm clumps [13]. baryonic material collected in the dm potential wells of lss is likely heated and shocked by large–scale shock waves found in cosmological simulations (see, e.g, [53]) which produce a complex distribution of mach numbers. the presence of shock waves with relatively high mach numbers naively suggest that fermi-like acceleration might take place in lss thereby accelerating cosmic rays (crs) that can be efficiently confined mainly in galaxy clusters [8], while they can diffuse out of galactic and sub-galactic structures [8, 9]. radio observations and magneto-hydrodinamic (mhd) simulations also suggest that magnetic fields are associated to the distribution of baryonic material collected in lss potential wells. the seed magnetic field is likely amplified and made turbulent by the coupling of gravitational collapse and mhd processes during the formation of galaxy clusters. evidence for wide-scale and turbulent intra-cluster magnetic field is indicated by the diffuse radio synchrotron emission found in many clusters (with typical values b ∼ 0.1 − 2 µg), by radio relics in dynamically active clusters (with typical values b ∼ 0.2 − 5 µg) and by faraday rotation measurements of background and embedded polarized radio sources (with typical values b ∼ 1− 50 µg [27]. very massive dm clumps that collapse at high redshifts (z ∼ 6−7) often contain the most massive black holes (bhs) at their centers [35]. the agn descendants of these ancient supermassive bhs (smbhs) are found to be part of the massive galaxies located at the centers of the most massive galaxy clusters we observe at the present epoch, like, e.g., cena, m87/virgo, perseus, a262, a4059, with their radio lobes penetrating the icm for tens or hundreds of kpcs. it is often observed that the radio jets/lobes end up in approximately spherical bubbles of relativistic plasma (likely containing relativistic or mildly-relativistic plasmas) that appear as cavities in the x-ray images of galaxy clusters [3] with dimensions ranging from a few kpcs (as in perseus) to ∼ 100 kpc. the combination of high-resolution radio and x-ray images indicates that the relativistic plasma found inside the x-ray cavities is connected with the jet/lobe structure of the central agn and with the history of the ejection events and mechanisms from the central agn. the cluster cores which host such non-thermal phenomena (bhs, cavities, magnetic fields) are found to be systematically cooler than the outer regions of the clusters with the inner temperature setting at a value ∼ 1 3 − 1 2 of the outer temperature, usually consistent with the virial expectation. it seems that a heating agent of nongravitational and non-thermal nature – with a heating rate that is able to accomodate itself to the cooling rate 56 http://dx.doi.org/10.14311/app.2014.01.0056 multi-frequency study of the sz effect in cosmic structures of the intra-cluster plasma – is present in the cluster’s cool core so as to maintain it in a quasi-stationary, warm configuration [16]. the previous evidence indicates that galaxy clusters are the largest storage rooms for cosmic material (galaxies, dm, hot thermal baryonic plasma, non-thermal and relativistic plasma, bhs, magnetic fields, crs). in this sense they can be considered as the largest multidisciplinary laboratories in the universe where one can efficiently study some of the most interesting aspects of the astrophysics of lss: the nature of dm, the origin and distribution of crs, the impact of magnetic fields on lss, the impact of bhs on lss, the interplay between thermal and non-thermal phenomena in lss. two ways can be identified to proceed in this study: i) a multi-technique, single-purpose approach that require to integrate the analysis of various observations performed in various frequency bands; ii) a singletechnique, multipurpose approach that is able to provide detailed physical information based on a single observational technique. we will discuss, in the following, some of the results obtainable through the last approach by using the physical information contained into the sze. 2 the physics of the sz effect the sze is produced by the inverse compton scattering (ics) of cmb photons off the electrons confined in the atmospheres of cosmic structures. manifestations of the sze include: i) spectral distortions of the cmb due to up-scattering of cmb photons induced by high-e electrons (thermal, non-thermal and relativistic sze); ii) spectral distortion of the cmb due to a bulk motion of the electronic plasma w.r.t. the hubble flow (kinematic sze); iii) polarization of the cmb due to dynamical and plasma effects (sze polarization). the sz effect. the spectral distortion of the cmb spectrum observable in the direction of a galaxy cluster writes [56, 2, 6] as ∆i(x) = 2 (ktcmb)3 (hc)2 y g(x) , (1) where ∆i(x) = i(x) − i0(x), i(x) is the up-scattered cmb spectrum in the direction of the cluster and i0(x) is the unscattered cmb spectrum in the direction of a sky area contiguous to the cluster. here x ≡ hν/ktcmb , h is the planck constant, k is the boltzmann constant, tcmb = 2.726 k is the cmb temperature today and ν is the observing frequency. the comptonization parameter y is y = σt mec2 ∫ ped` (2) in terms of the pressure pe contributed by the electronic population. here σt is the thomson cross section, me the electron mass, and c the speed of light. the spectral function g(x) of the sze is g(x) = mec 2 〈εe〉 { 1 τe [∫ +∞ −∞ i0(xe−s)p (s)ds− i0(x) ]} (3) [6] in terms of the photon redistribution function p (s) and of i0(x) = i0(x)/[2(ktcmb)3/(hc)2] = x3/(ex − 1) . (4) the quantity 〈εe〉 ≡ σt τe ∫ ped` = ∫ ∞ 0 dpfe(p) 1 3 pv(p)mec , (5) where fe(p) is the normalized electron momentum distribution function, is the average energy of the electron plasma [6]. the optical depth along the line of sight ` of the electron population with number density ne is τe = σt ∫ d`ne . (6) the photon redistribution function p (s), with s = ln(ν′/ν) in terms of the cmb photon frequency increase factor ν′/ν, can be calculated by repeated convolution of the single-scattering redistribution function, p1(s) = ∫ dpfe(p)ps(s; p), where ps(s; p) depends on the physics of inverse compton scattering. the previous description is relativistically covariant and general enough to be applied to both thermal and nonthermal plasma, as well as to a combination of the two (see [6, 17, 38] for details). kinematic sz effect. the velocity (or kinematic) sze (hereafter ksze) arises if the plasma causing the thermal, or non-thermal, sze is moving relative to the hubble flow. in the reference frame of the scattering particle the cmb radiation appears anisotropic, and the effect of the ics is to re-isotropize the radiation slightly. back in the rest frame of the observer the radiation field is no longer isotropic, but shows a structure towards the scattering atmosphere with amplitude ∝ τevt/c, where vt is the component of the peculiar velocity of the scattering atmosphere along the line of sight [55, 51]. the brightness change of the cmb due to the ksze is given by ∆i i = −τeβt xex ex − 1 (7) with βt ≡ vt c [55, 40]. a general relativistic description of the ksze has been given in the framework of the general boltzmann equation [29] and in the relativistic covariant formalism [38]. sz effect polarization. the ics process yields naturally a polarized upscattered radiation field. the polarization π of the sze arises from various dynamical 57 sergio colafrancesco and plasma effects [54, 22, 32, 1]: galaxy clusters transverse motion (πk ∝ β2 t τ in the rayleigh-jeans, rj, regime), transverse motions of plasma within the cluster (πv ∝ βtτ 2 in the rj regime) and multiple scattering between electrons and cmb photons within the cluster (πth ∝ θτ2 in the rj regime for the thermal sze with θ = kte/mec 2). a general, covariant, relativistic derivation of the sze polarization for thermal, non-thermal and relativistic plasma can be derived [22] and generalizes the non-relativistic derivation [54] in a way similar to the general derivation of the sze [6] previously discussed. 3 astrophysical and cosmological impact studying the sze in the atmospheres of various cosmic provides many insights on their energetics, pressure and dynamical structure. the combination of sze with other emission mechanisms related to the same particle distribution (i.e., synchrotron, high-e ics and bremsstrahlung emission) provides further information on the radiation, matter and magnetic fields that are co-spatial with the electrons producing the sze. these properties of the sze concern various cosmic structures, from galaxy clusters to radiogalaxy lobes, from galaxy halos to supercluster. the redshift-independent nature of the sze allows to use it as a powerful cosmological probe yielding constraints on the evolution of cluster abundance, cosmological parameters, the dark energy equation of state, the homogeneity of the universe, the properties of cosmological magnetic fields [14]. observations aimed at these challenges must however exploit the whole physical information contained in the spectral and spatial features of the sze. 3.1 simple sze astrophysics the sze has been searched in galaxy clusters since it was originally proposed [55, 56] using various techniques (see [14] for a recent review). ground-based sze experiments (e.g., spt, act, apex, ami, gbt, among others) provided excellent results in terms of imaging and blind search surveys with their low frequency, multiple-band observations, but they do not have neither true spectroscopic capabilities nor a wide frequency band, and they are not sensitive to the high-ν range ( ∼> 400 ghz) of the sze signals, which is crucial to exploit the astrophysical information contained in the sze (see fig. 1, [14]). ground-based instruments widely improved the source statistics (crucial to obtain cosmological information using the sze) and the angular resolution of sze images (crucial to disentangle the extended sze signal from point-source contamination), but add little to the physical specification of the detected sze sources, and therefore they need x-ray and optical follow-up to fully characterize the physical parameters derived from sze observations. figure 1: thermal sze spectrum of galaxy clusters with different plasma temperatures (as indicated) and the same value of the optical depth. the low-ν part (ν ∼< 220 ghz) of the spectrum depends mostly on the total compton parameter y ∝ ∫ d`ptot with no strong spectral dependence on the temperature. the high-ν part of the spectrum (at ∼> 300 ghz) shows a strong spectral dependence from the plasma temperature [17]. typical frequency bands where the sze is observed from the ground are shown as blue-cyan bands, while the region accessible from space observations is shown by the gray shaded area. 3.2 the road to astrophysics the planck satellite allowed for the first time to access a wide frequency range in the study of the sze. planck early sze science observations yielded 189 sze sources with s/n > 6 which provides the first sze measure for ∼ 80 % of the known galaxy clusters, and 20 additional new clusters (see arnaud at this meeting). this is the largest sample so far of sze detected clusters. planck detected sze clusters are followed-up with a multi-frequency observation program in the x-rays, sze, optical bands to obtain confirmation, redshift estimation and estimates of the global physical parameters. these results show that the sze selection is a very powerful method for the detection of new distant and very massive clusters. planck also unveiled a population of dynamically perturbed clusters at z ∼> 0.3, 58 multi-frequency study of the sz effect in cosmic structures possibly underrepresented in x-ray surveys. the information collected so far strengthen our overall view of the icm properties and mass content in galaxy clusters. most of these results are discussed in the early and intermediate papers [41, 42, 43, 45, 46, 47] and more analyses are still coming. the use of planck sze results also allowed to extend the sample of radio halo clusters with combined radio, sze and x-ray data [23]. the correlation ysz−lx probes the existence of a substantial amount of non-thermal pressure in clusters that also requires a correlation x ∝ l−0.96x between the nonthermal to thermal pressure ratiox = pnon−th/pth and the cluster x-ray luminosity lx [23]. the nature of the non-thermal electron population could be only probed with additional high-ν spectroscopic studies. the herschel satellite (co-eval with planck) has been able to observe the sze in a few pointed clusters with the spire instrument equipped with an fts spectrometer working in the frequency range ∼ 600 − 1200 ghz. the possibility to have sensitive spectroscopic measurements in these high-frequency bands opens the way to the deep astrophysical exploitation of the sze. as an example, the additional data points on the sze spectrum of the bullet cluster observed with herschelspire [60] allowed to establish a number of properties for the thermal and non-thermal plasma superposition in the atmosphere of this strong merging cluster (see, e.g. [18, 48, 49]. a consequence of such superposition is that cluster temperature distribution has a high value of of the temperature standard deviation σt , as in the case of the bullet cluster where it is found σt = 10.6 ± 3.8 kev [50]. this result shows that the temperature distribution in the bullet cluster is strongly inhomogeneous along the line of sight and provides a new method for studying galaxy clusters in depth. these studies have been possible because the access to the very high-ν part of the sze spectrum contains detailed information on the relativistic effect on the single thermal plasma and on the presence of additional plasmas of either thermal or non-thermal nature (see discussion in [18, 21]. planck and herschel observations of the sze opened a rich field of investigation that will fully blossom in the next years with the full exploitation of spatiallyresolved spectroscopic sze observations. in the following we discuss some of the astrophysical and cosmological studies that will be possible with a spectropolarimetric study of the sze. 4 astrophysical impact studying the sze in various cosmic atmospheres provides many insights on their energetics, pressure and dynamical structure. the combination of sze with other emission mechanisms related to the same particle distribution (i.e., synchrotron, high-e ics emission, bremsstrahlung emission) provides further information on the radiation, matter and magnetic fields that are co-spatial with the electrons producing the sze in various cosmic structures. 4.0.1 galaxy clusters precise observations of the sze at mm and sub-mm wavelengths are crucial for unveiling the detailed structure of cluster atmospheres, their temperature distribution, and the possible presence of suprathermal and/or nonthermal plasma because the high-frequency part (i.e. at ν ∼> 350 ghz or x ∼> 6) of the sze spectrum is more sensitive to the relativistic effects of the electron momentum distribution [6, 10, 17]. this is even more so for galaxy clusters with a complex plasma distribution as found for powerful merging clusters, like the exemplary case offered by the bullet cluster (1es0657-56) [18]. powerful merging events in galaxy clusters can, in fact, produce an additional high-t plasma distribution (if the electron acceleration time scale at the merging shocks is longer than their equilibration time scale [57]), or an additional nonthermal population (produced either in a merging process with a very short acceleration time scale or by secondary electrons produced by p-p collisions, after the high-e protons have been accelerated by the merging and accumulate in the cluster region on long time scales [58]). the quasi-stationary case provided by the competition between particle thermalization and stochastic acceleration and momentum diffusion [26] can develop a subrelativistic electron distribution tail and can produce suprathermal regions in the cluster atmosphere. a quantitative estimate of the temperature inhomogeneity (stratification) along the line of sight is possible using sze data only providing a measure the temperature standard deviation of the cluster plasma along the line of sight. we found that the bullet cluster has a temperature standard deviation of 10.6±3.8 kev [50]. this result (obtained for the first time with sze measurements) shows that the temperature distribution in the bullet cluster is strongly inhomogeneous and provides a new method for studying galaxy clusters in depth. study of the multifrequency (from ∼ 30 to ∼ 850 ghz) sze signal observed in the bullet cluster shows, in fact, the presence of a thermal plasma at ∼ 13.9 kev coexisting with a second plasma component, either at higher temperature (≈ 25 kev) or, more preferably, of a nonthermal origin [18] (see fig.2). additional observations of the bullet cluster at ν ∼ 400 ghz with a precision ∼< 1% of the expected signal will be able to further distinguish between the two cases of non-thermal powerlaw or suprathermal tail [18]. sze observations over a wide frequency range, and especially with high sensitivity in the high-ν range, can 59 sergio colafrancesco also add relevant information on the electron distribution function (df) in the icm, a subject that even though relevant for a proper analysis of the sze has not been addressed in details so far. the relativistic kinetic theory, on which the df derivation is based, is still a subject of numerous debates (see discussion in [48]). sze observations can separate the sze spectrum caused by a departure from the diffusive approximation based on the kompaneets approach [31] from those which are due to using a relativistic correct df instead of a maxwell-boltzman df (see fig.3) and therefore set constraints to the actual electron df [48]. this analysis is best fulfilled in hot massive clusters because the sze intensity change due to using a relativistic correct df instead of a maxwell-boltzman df are much larger in hot clusters due to the fact that relativistic sze corrections scale as ∝ t 5/2. a method used to derive the df of electrons using sze multi-frequency observations of massive hot clusters [48] makes use of fourier analysis representation of the approximate electron df whose parameters are best fitted using observations in the (optimal) frequency channels at 375, 600, 700, 857 ghz. figure 2: the sze spectrum at the bullet cluster center modeled with a thermal plus nonthermal plasma: thermal plasma with kt = 13.9 kev and τ = 1.1×10−2 (dot-dashed); nonthermal plasma with p1 = 1, s = 2.7 and τ = 2.3 × 10−4 (dotted); total sze produced by the sum of the two plasmas (solid). a morphological analysis of the sze observed at various frequencies adds relevant information to assess the pressure and energy density structure of cluster atmospheres. morphological sze differences are particularly evident for clusters undergoing violent mergers that create large inhomogeneities of the electron df. sze intensity maps of merging clusters obtained from hydrodynamical simulations show that the morphology of the sze intensity maps observable with laboca (at 345 ghz) and herschel-spire (at 857 ghz) are rather different [49] (see fig.4). for a bullet-like cluster, the sze intensity map at 857 ghz has a spatial feature caused by the presence of the cold bullet-like substructure seen also in the x-ray surface brightness map. however, this cold substructure is not present in the sze intensity map at 345 ghz. this is a consequence of the relativistic effects of the sze and shows that observations of the sze intensity maps at very high frequencies can reveal complex pressure substructures within the atmospheres of massive galaxy clusters. this result shows that the analysis of the sze signal at 857 ghz, correlated with lower-ν observations offers a promising method for unveiling high-t regions in massive merging clusters using available experiments like, e.g laboca and herschel-spire. figure 3: the sze intensity spectra for a massive cluster with a temperature of kte = 15.3 kev for juttner (solid) and maxwell-boltzman (dashed) dfs. the non-relativistic sze spectrum (solid) is also shown for comparison. figure from [48] in more relaxed clusters spectroscopic measurements of the sze over a wide frequency band allow to derive precise information on the temperature distribution and on the cool-core nature independently of x-ray priors [17] and hence reconstruct the full set of cluster physical parameters [25]. spectro-polarimetry measurement of the sze are able to add further information on the transverse plasma motions within the cluster and on the pressure substructure of the plasma. sze polarization signals in galaxy clusters are quite low and typically below mjy (or ≈ µk) level even for high-t clusters [14] but it is interesting to note that the sze polarization in cluster has quite different spectra w.r.t. the intensity sze spectrum, a property that requires to use spectropolarimetry to fully disentangle the physical information contained in the sze. combining intensity and polarization observations of the sze can uncover unique 60 multi-frequency study of the sz effect in cosmic structures details of the 3d (projected and along the line of sight) velocity structure of the icm, of its 3d pressure structure and of the influence of a structured magnetic field in the stratification of the icm, and therefore provides a full tomography of cluster atmospheres. analogously, the combination of the intensity and polarization observations of the kinematic sze (and its frequency dependence) can yield crucial information on the 3d distribution of the cosmological velocity field traced by galaxy clusters. specifically, the ratio ∆ith/πth yields direct information on the plasma optical depth τ , and the ratio ∆ith/πv on the combination τ ·βt, thus allowing to use intensity and polarization sze measurements to fully disentangle the pressure and velocity structure of the cluster atmospheres. sze polarization measurements are quite difficult to obtain with present-day experiments and they are also at the limit of next generation experiments. however, stacking analysis of even small samples (order of ∼ 20) of hot and dense galaxy clusters would allow to determine statistically the polarization signals of the thermal sze for clusters with kt > 10 kev and τ > 0.03 in the optimal frequency range ≈ 90− 250 ghz. figure 4: from top to bottom. the sze signal to noise ratio map for the cluster 1e0657-558 at 345 ghz smoothed to the resolution of laboca and at 857 ghz smoothed to the resolution of herschel-spire. figures from [49]. 4.0.2 cluster cavities the atmospheres of galaxy clusters often show the presence of bubbles filled with high-e particles and magnetic field that are sites of bright radio emission and produce cavities in their x-ray emission distribution. cavities with diameters ranging from a few to a few hundreds of kpc have been observed by chandra in the x-ray emission maps of several galaxy clusters and groups [3, 34]. while the properties of these cavities and of the relativistic plasma they contain is usually studied by combining x-ray and radio observations, an alternative and efficient strategy is to study the consequences of the sze produced by the high-energy electrons filling the cavities [7, 39] whose amplitude, spectral and spatial features depend on the overall pressure and energetics of the relativistic plasma in the cavities. as an example, the overall sze observable along the line of sight (los) through a cluster containing cavities (see fig.5 for the case of the cluster ms0735.6+7421) is the combination of the non-thermal sze produced by the cavity and of the thermal sze produced by the surrounding icm. due to the different ν-dependence of the thermal and non-thermal sze, the non-thermal sze from a cluster cavity shows up uncontaminated at frequencies ν ≈ 220 ghz: at this frequency, in fact, the overall sze from the cluster reveals only the ics of the electrons residing in the cavities without the presence of the intense thermal sze dominating at lower and higher frequencies. the cavity’s sze becomes dominant again at very high-ν (x ∼> 14 or ν ∼> 800 ghz) where the nonthermal electrons dominate the overall ics emission (see fig.5). the cavity’s sze is more spatially concentrated than the overall cluster sze because it is only emerging from the cavity regions: this fact allows to study the overall energetics and pressure structure of the cavity’s high-e particle population and the b-field structure in combination with x-rays and radio images. the observation of the crossover of the non-thermal sze from the cavities (which depends on the value of emin(p1) or, equivalently, on the value pcavity) provides a way to determine the total pressure and hence the nature of the electron population within the cavity [7], an evidence which adds crucial, complementary information to the x-ray and radio analysis. if cluster cavities contain a high-t (∼ 109 − 1010 k) plasma, the sze flux from cocoons in the central part of a distant elliptical and a nearby galaxy cluster are of the same order. for a high-t plasma, the cocoon’s sze spectrum is rather flat at high-ν resembling the shape of the non-thermal sze from cavities. in this high-t plasma model, however, no strong radio emission at ν ∼> 1 ghz (as instead observed) is expected from the cocoon, unless the cocoon’s b-field is very high b ∼> 103µg. 4.0.3 radiogalaxy lobes studies of (giant) radio-galaxy (rg) lobes (see, e.g., [28, 30, 24, 4]) have shown that these extended structures contain relativistic electrons that are currently available to produce both low-ν synchrotron radio emission and ics of the cmb (as well as other radiation background) photons. as a consequence, an sze from the lobes of rgs is inevitably expected [11]. such nonthermal, relativistic sze has a specific spectral shape that depends on the shape and energy extent of the spectrum of the electrons residing in rg lobes. the 61 sergio colafrancesco sze emission from rg lobes is expected to be co-spatial with the relative ics x-ray emission [11] and its spectral properties are related to those of the relative ics x-ray emission. in fact, the spectral slope of the ics x-ray emission αx = (α− 1)/2 (where fics ∼ e−αx ) can be used to set the electron energy spectral slope α (where ne ∼ e−α) necessary to compute the sze spectrum, and to check its consistency with the synchrotron radio spectral index αr = (α − 1)/2 (where fsynch. ∼ e−αr ), that is expected to have the same value [11, 19]. figure 5: top. the geometry of the cavities in the cluster ms0735.6+7421. bottom. the sze spectrum has been computed at a projected radius of ≈ 125 kpc from the cluster center where the los passes through the center of northern cavity. the thermal sze (blue), the non-thermal sze from the cavity (black) and the total sze (red) are shown. the non-thermal sze is normalized to the cavity pressure p = 6 · 10−11 erg cm−3, and is shown for various values of p1. figure from [7] the sze in rg lobes has not been detected yet: only loose upper limits have been so far derived on the sze from these sources (see [2, 59]). a detection of the sze from rg lobes can provide a determination of the total energy density and pressure of the electron population in the lobes [11] allowing to determine the value of emin once the slope of the electron spectrum is determined from radio and/or x-ray observations. sze measurements provide a much more accurate estimates of the electron pressure/energy density than with other technique like ics x-ray emission or synchrotron radio emission, since the former can only provide an estimate of the electron energetics in the high-energy part of the electron spectrum, and the latter is sensitive to the degenerate combination of the electron spectrum and of the magnetic field in the radio lobes. the combination of sze observations (that depend on the electron distribution and on the known cmb radiation field) and the radio observations (which depend on the combination of the electron distribution and of the magnetic field distribution) provides an unbiased estimate of the overall b-field in the lobe by using the ratio fradio/fsze ≈ eb/ecmb , that is more reliable than that obtained from the combination of ics x-ray (or gamma-ray) and radio emission [19]. the spatially resolved study of the sze and synchrotron emission in rg lobes also provide indication on the radial behaviour of both the leptonic pressure and of the magnetic field from the inner parts to the boundaries of the lobes. study of the pressure evolution in rg lobes can provide crucial indications on the transition from radio lobe environments to the atmospheres of giant cavities observed in cluster atmospheres, which seem naturally related to the penetration of rg jets/lobes into the icm (see fig.5). a substantial sze polarization is also expected in rg lobes due to both coherent transverse motions of the plasma along the jet/lobe direction and to the electron pressure substructures induced by e.g. plasma inhomogeneities and magnetic field turbulence. the transverse velocity-induced polarization is πv ∝ τrel(βtτrel), and the multiple scattering induced polarization is πτ ∝ τrelprel where prel is the pressure of the relativistic electron distribution. observations of the sze and its polarization in rg lobes can yield, therefore, direct information on electrons τrel and βt in the rg lobe. 4.0.4 galaxies hot gas trapped in a dm halo can produce a sze. a typical galaxy halo might hence show an integrated thermal sze at the level of ∼< 0.5 mjy arcmin−2 from a plasma with t ∼ 106 k and density ne ∼ 10−3cm−3 extended for ∼ 50 kpc in the inter-stellar medium. a measurement of galaxy halo sze would provide direct information on the mass, spatial distribution and thermodynamic state of the plasma in a low-mass galactic halo, and could place important constraints on current models of galaxy formation. detecting such an extended, low-amplitude signal will be challenging, but possible with sensitive all-sky sze maps. an sze is also expected from galaxy outflows swept by galaxy (hyper-)winds. a thermal sze is expected to arise from the shocked bubble plasma in a galaxy wind described by a simple, spherical blast wave model [52]. 62 multi-frequency study of the sz effect in cosmic structures however, such simple recipe for the sze from galaxy winds is to be modified by the presence of cosmic rays and magnetic field in the expanding wind leading on one side to a more complex sze spectrum, and on the other side to an amplification of the overall sze at high frequencies, thus increasing the detection probability. sze observations from galaxy winds will be possible with high-sensitivity and high-resolution telescopes like alma and ska.     figure 6: top. thermal sze spectrum (continuous line in bottom panel), compared to the atmospheric transmission of a dry, cold, atmosphere (top panel, pwv= 0.5 mm), and to spectra of the nonthermal sze (dotted line), of cmb anisotropy and kinematic sze (dashed line), and of dust anisotropy (dotdashed line). the parameters of the different spectra are for τth = 5 × 10−3, te = 8.5 kev, ∆tcmb = 22µk, τnon−th = 10−4, α = −2.7, p1 = 1.4 mev/c, ∆id(150ghz) = 600 jy. the frequency coverage of different experiments [25] is shown as dotted horizontal lines, labelled with the experimental configuration number. bottom. simulated data sets for the spectroscopic configurations ec5 (differential cold fts on a l2-orbit satellite, with cold telescope). 5 cosmology and fundamental physics the redshift-independent nature of the sze allow to use this effect as a powerful cosmological probe [14] by using both the redshift evolution of cluster abundance and direct probes of cosmological parameters. the recent planck results however indicate a tension at ∼ 3σ level on the value of σ8 vs. ωm comparing sze counts and cmb results that might be mitigated by other cosmological effects like, e.g., a more complex cluster bias dependence, the existence of massive neutrinos with ∑ mν ∼ 0.2 ev (see rubino-martin in these proceedings) or by addressing more in details the complex astrophysics issues still pertaining cluster formation and evolution. this last possibility requires to have new high-quality sze cluster samples studied with full spectra-polarimetric capabilities and in the high-ν range of the sze spectra where the astrophysical effects are more evident. fig.6 shows the frequency coverage requirements for a full spectroscopic sze mission and the outcomes of a simulated thermal sze spectrum from a kte = 8.5 kev cluster [25]. the sensitivity and spectro-polarimetry power of such an experimental configuration (ec5) will allow to address fundamental questions in cosmology and fundamental astrophysics with the sze, in addition to standard cosmological probes [14]. a wide discussion on the cosmological relevance of the sze for probing the concordance cosmological scenario, the search for the nature of dm, cosmological magnetic fields and cosmological velocity fields can be found in [14]. here we discuss the additional application of the spectro-polarimetric observations of the sze to measure the cmb multiplies and test the assumption of the homogeneity of the universe. high-sensitivity observations of the (thermal and kinematic) sze and its polarization can be used to test the homogeneity of our universe through probes of the copernican principle (cp) [33, 23]. in fact, large variations of the thermal sze induced by cmb photons that have temperature significantly different from the blackbody temperature we observe directly, and that arrive at galaxy cluster from points inside our light cone, could indicate a violation of the cp and homogeneity. analogously, large variations of the cmb dipole measured by the cluster ksze could also indicate a violation of the cp and homogeneity. the sze polarization contains more refined information on the cmb temperature and thus it can also provide a powerful probe of cp and homogeneity. thus, observations of large sze and of its polarization w.r.t. to the expectations of the sze produced from a pure blackbody cmb spectrum might provide indications of a non-flrw universe. the combination of an ec5 experiment with radio observations of the low-ν part of the sze spectrum can also be used to probe even more fundamental aspects of astrophysics, like the fundamental properties of the photon. measurements of the sze with sensitivity of order of < 0.1 jy, in the range ∼ 10 − 50 ghz, can set very stringent constraints on the photon decay time [20]. this frequency band is also the one less affected by other sources of astrophysical contamination, and it will be best explored with the advent of the high63 sergio colafrancesco sensitivity ska telescope. at higher frequencies (i.e., ∼ 120 − 180 and ∼ 200 − 300 ghz), there are other spectral windows where the sze method is again competitive if not advantageous in this respect. the necessary sensitivity in the high-ν range can be achieved with the next coming millimetron space mission [14], whose ec5-like configuration is also advantageous in disentangling other astrophysical sources of contamination (e.g., sources of non-thermal sze and/or special distortions of the sze due to multiple-temperature regions) that could contaminate these measurements. figure 7: difference between the standard thermal sze calculated for a2163 in 2–45 ghz range and integrated in a 1 arcmin2 area and the one modified for values e∗ = 5×10−9 ev (solid line), 3×10−9 ev (dash 3 dots), 2 × 10−9 ev (dot-dashed), and 1 × 10−9 ev (dashed). the sensitivity achievable with ska in ∼ 30 hours (red thick solid line) and in ∼ 260 hours (blue thick long-dashed line) are shown [20] 6 future directions the impact of sze observation for astrophysical and cosmological application is steadily increasing since the advent of dedicated experiments and large-scale surveys in the mm and sub-mm frequency range. the quality and the spatial resolution of sze images is reaching the level of arcsecs and the spectral coverage in systematically extending in the sub-mm region where highest spatial resolutions can be achieved with a wide spectral coverage able to decipher the physical details of the electron distribution in the atmosphere of cosmic structures. new paths of theoretical investigations are underway and concern both the detailed study of the ics mechanism and the impact of the various plasma structure and fields in cosmic structures. the possibility to perform precise measurements of the various sze signals and to extract the relevant astrophysical information depends crucially on the capability to have spatially-resolved spectral (and polarization) observations of sze sources over a wide ν band, from radio to sub-mm. in particular, the important condition for such study is to have a wide-band continuum spectroscopy (polarimetry) and especially a good spectral coverage and sensitivity in the high-ν band, where most of the astrophysical effects reveals more clearly. spatially resolved spectroscopic and polarimetric observations of the sze in the frequency range from ∼ 100 ghz to ∼ 1 thz, complemented by analogous observations in the radio band ∼ 1 − 30 ghz, are the key to improve our understanding of the structure of cosmic atmospheres through analysis of the intensity and polarized sze signal, and will allow to use this technique to probe the fundamental properties of the universe. acknowledgement s.c. acknowledges support by the south african 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http://dx.doi.org/10.1146/annurev.aa.18.090180.002541 http://dx.doi.org/10.1086/498227 http://dx.doi.org/10.1086/591723 introduction the physics of the sz effect astrophysical and cosmological impact simple sze astrophysics the road to astrophysics astrophysical impact galaxy clusters cluster cavities radiogalaxy lobes galaxies cosmology and fundamental physics future directions acta polytechnica ctu proceedings doi:10.14311/app.2017.7.0022 acta polytechnica ctu proceedings 7:22–28, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app validation and implementation of failure parameters in integrated simulations for short fibre reinforced polypropylene anna kalteisa,∗, martin reitera, michael jerabekb, zoltán majora a institute of polymer product engineering, johannes kepler universität linz, altenberger straße 69, linz, austria, 4040 b borealis polyolefine gmbh, st.-peter-straße 25, 4021 linz ∗ corresponding author: anna.kalteis@jku.at abstract. nowadays short fibre reinforced polymers are often used in load carrying structural parts. compared to continuous fibre reinforced polymers they exhibit a more complex morphology. hence the determination of the strength is a difficult but important task. therefore this was the objective of this research. the strength of short fibre reinforced polymers was numerically determined for low-speed to high-speed strain rates for specimens with different fibre orientations. for the failure modelling the micromechanical approach “first pseudo grain failure” in digimat was used. the parameters for the material and failure description were determined with the reverse engineering method. integrated finite element simulations were performed to validate the material and failure models by tensile and bending tests with different specimens. the comparison of the results of the experiments and simulations showed low deviation. keywords: integrated simulation, short fibre reinforced polymer, failure prediction, first pseudo grain failure, reverse engineering. 1. introduction the prediction of the stiffness of a fibre reinforced material is not a difficult task anymore because there is appropriate software available. one is the software digimat mf. there only few input parameters are needed to calculate the stiffness [1]. however the prediction of the strength of a material especially for short fibre reinforced polymers is not trivial. to perform simulations is very common nowadays, therefore in this research the strength of short glass fibre reinforced polypropylene is determined by integrated finite element simulations. there are many different approaches how to predict the strength of a discontinuous fibre reinforced polymer. for example there is an analytical model where the strength of fibre reinforced composites can be calculated without any numerical software [2]. furthermore there are several continuum mechanics based models [3], [4], [5], [6], [7], [8], [9] and micromechanics based models [10], [11], [12], [13]. in the paper also a micromechanics based model is used namely the “first pseudo grain failure”(fpgf) model [1]. a short description is given in section 4 of this paper. the investigated material is a short glass fibre reinforced polypropylene. the glass fibre content is 32 w%. because of the short fibre reinforcement the fibre distribution and orientation in the different specimens have to be investigated. the fibre orientations were determined by the computer tomographic method. the raw data from the computer tomographic measurements of the fibre orientation were provided by fh-oö (wels, austria). therefore a description of the ct-measurements is not given here but in [14]. the experimental data were provided by borealis polyolefine gmbh (linz, austria). standardized tensile (iso 527) and bending tests (iso 178) were performed with the corresponding strain rate and specimen. specimens with different complexity of fibre distribution and orientation were used. specimens with a uniform fibre distribution and orientation (ud multi tool) are used for the reverse engineering. for the validation specimens with a more complex fibre distribution and orientation are used. a description of the used specimens is given in section 2. the modelling of the material behaviour is an other part of this paper. elastic-plastic (low-speed strain rates) and elastic-viscoplastic (low-speed and highspeed strain rates) material models are generated. the needed material parameters are reverse engineered based on experimental data of tensile tests. in section 4 the determination of an appropriate failure criterion is described. because the polymer is reinforced with short fibres classical failure criteria (e.g. tsai-hill) cannot be simply used because they are just valid for continuous fibre reinforced composites [1]. hence as already mentioned above the “first pseudo grain failure” (fpgf) model has to be used. the failure parameters are determined with the method of reverse engineering with data of tensile tests. the results of the material and failure modelling are validated with tensile tests with specimens with different fibre distribution and orientation as the reverse engineered ones. further validation follows by per22 http://dx.doi.org/10.14311/app.2017.7.0022 http://ojs.cvut.cz/ojs/index.php/app vol. 7/2017 forming bending tests. the appearing difficulties in the simulation of the bending test have to be solved and are described in section 5.3. the validation of the material and failure model is done for low-speed and high-speed strain rates. in this paper only the results for the low-speed strain rates are discussed. 2. specimens as already mentioned different types of specimens are used for the experiments and simulations. an overview of the used specimens is given in fig. 1. figure 1. overview of different specimens. different specimens are used because of their different complexity of fibre orientation. the ud-multitool was designed by borealis polyolefine gmbh (linz, austria). the specimens, which can be milled out of the tool have a highly uniform fibre distribution. the specimens 0◦, 45◦ and 90◦ are relevant for this paper. because of the uniform fibre distribution these specimens are used for the reverse engineering of the material and failure parameters. for the validation of the material and failure models the iso-mps specimen and the plate specimens are used. the plate specimens were milled out of a plate at different positions and under the angles 0◦, 45◦ and 90◦. these specimens do not show a uniform fibre orientation through the thickness as the ud-multitool specimens. 3. material modelling for the material modelling the software digimat mf 6.0.1 is used. for the glass fibre a linear elastic, isotropic material model is chosen. therefore only the elastic modulus and the poisson’s ratio have to be defined. for the elastic modulus and poisson’s ratio the following values are used: e = 72000 mpa, ν = 0.2 the aspect ratio (ar) of the fibres is set to 35 [15]. an elastic-plastic (ep) and also an elastic-viscoplastic (evp) material model are generated for the matrix. the ep and evp material models for the matrix need more input parameters than an elastic one. the j2plasticity model is chosen (eq. 1). for the hardening the exponential and linear law is used (eq. 2). where r(p) is the hardening stress, p is the accumulated plastic strain, k is the linear hardening modulus, r∞ is the hardening modulus,m is the hardening exponent [1]. σeq = √ j2(σ) (1) r(p) = kp+r∞[1 − exp(−mp)] (2) for the elastic-viscoplastic model some additional parameters for considering the viscoplasticity have to be determined. a law for the accumulated plastic strain rate ṗ has to be chosen. in this paper the current yield norton law is chosen (eq. 3). there the ṗ is dependent on the initial yield stress σy, the viscoplastic stress f , the hardening stress r(p), the viscoplastic coefficient η and the viscoplastic exponent m. ṗ = σy η ( f σy +r(p) )m (3) a detailed description is given in [1]. the above described parameters are reverse engineered with the software digimat mx 6.0.1. with this procedure the parameters for an artificial matrix are generated. they are artificial because the real behaviour of the matrix (e.g. micro-cracking) and the influence of the fibre on the matrix (e.g. fibre-matrix debonding) are inherently considered. these influences cannot be modelled by using the parameters for the neat matrix material [16]. in the reverse engineering procedure experimental stress-strain curves are needed where the microstructure (fibre orientation) is known. the parameters of the matrix are fitted to the experimental curves in an iterative optimization process [1]. the results of the material modelling for the ep and evp material models for different strain rates are summarized in table 1 and table 2. 4. failure modelling the intralaminar failure criteria, which are available in digimat are only valid for a lamina layer with unidirectional aligned fibres [1]. they can be non-interactive, interactive or failure mode based [17]. the failure criterion, which is used is tsai-hill 3d transversely isotropic (stress based, interactive). this failure criterion assumes that the strength in tension and compression is identical and the material is isotropic in the 2-3 plane [1]. direction 2 and 3 are the directions transverse to the fibre orientation (direction 1). for the description of the failure criterion three input parameters have to be defined: 23 a. kalteis, m. reiter, m. jerabek, z. major acta polytechnica ctu proceedings strain rate [s−1] 10−4 10−3 10−2 young’s modulus [mpa] 1800 1800 1800 poisson’s ratio [-] 0.42 0.42 0.42 yield stress [mpa] 4 4 4 hardening modulus [mpa] 10.3 13.3 14.2 hardening exponent [-] 154.5 208.2 188.3 linear hardening modulus [mpa] 22.6 19.3 32.2 table 1. reverse engineered elastic-plastic material parameters for low-speed strain rates. strain rate [s−1] low-speed (10−4, 10−3, 10−2) high-speed (0.1, 1, 14) young’s modulus [mpa] 1800 1800 poisson’s ratio [-] 0.42 0.42 yield stress [mpa] 3 4 hardening modulus [mpa] 12 9 hardening exponent [-] 145 85 linear hardening modulus [mpa] 22 60 viscoplastic coefficient [mpa*s] 51 71 viscoplastic exponent [-] 4 6 plastic strain multiplier [-] 1.5 1.9 table 2. reverse engineered elastic-viscoplastic material parameters for low-speed and high-speed strain rates. • axial tensile strength x (tensile strength in fibre direction) • in-plane tensile strength y (transverse tensile strength) • transverse shear strength s the failure criterion is defined as follows [1]: fa(σ) = σ2 11 x2 − σ11(σ22 + σ33) x2 + σ2 22 + σ2 33 y 2 +( 1 x2 − 2 y 2 ) σ22σ33 + σ2 12 + σ2 13 s2 +( 4 y 2 − 1 x2 ) σ2 23 (4) because a short fibre reinforced polymer with nonperfectly oriented fibres is used and not a lamina layer with perfectly aligned fibres the “first pseudo-grain failure” (fpgf) method has to be used. with this method the failure criteria for laminates can also be used for composites with complex fibre orientation distributions because the short fibres are divided into regions with uniform fibre orientations [1]. this is illustrated in fig. 2. the strength values are reverse engineered based on the ep material model. also here the data of the tensile tests of specimens of the ud multi tool are used. in fig. 3 the strength parameters of the failure figure 2. illustration of the first pseudo-grain failure method [16]. modelling for different strain rates are illustrated. it can be seen that the higher the strain rate the higher the strength is. 5. integrative simulation 5.1. interface digimat cae for the validation of the material model integrative digimat-abaqus fem simulations are performed. for these simulations an interface is needed. thus the software digimat cae 6.0.1 is used. with this software the material properties are calculated depending on the fibre orientation either before or during the simulation. this depends on which so24 vol. 7/2017 figure 3. illustration of strength parameters for different strain rates. lution is chosen in digimat cae. in the following the solutions are described [1]: • micro solution: the material properties are calculated at every iteration and not kept constant. as a result the simulation takes very long. • hybrid solution: the material properties are precomputed before the simulation. this enables that the simulation is sped up. with this method so called hybrid parameters are computed during the generation of the material input file. integrative simulations (tensile test) with the two different solution methods are performed. the results show that there is nearly no difference between micro and hybrid solution (fig. 4). the hybrid solution is chosen for the further simulations because of the lower computation time. figure 4. comparison of hybrid and micro solution method. 5.2. simulation model of tensile test as the specimens show a fibre orientation distribution through the thickness this distribution has to be discretised for the simulation model. the discretised distribution can be modelled with a layer build-up of the specimen (fig. 5). the layers can be modelled by partitioning the specimen through the thickness and assigning a material model with a specific fibre orientation to every partition. the number of layers can vary. the higher the number of layers the more accurate the fibre distribution is described. furthermore the higher the number of layers is the higher the computation time because more different material models have to be assigned. for the tensile tests a 4 layer model is used. therefore for the simulation of a tensile test a 4 layer model with the hybrid solution method is used. in this simulation model no problems occur. figure 5. simulation model with 4 layers. 5.3. simulation model of bending test because there are no problems in the simulation model of the tensile test these settings are also applied for the bending tests. therefore a bending test with a 4 layer model and with the hybrid solution method is modelled. in contrast to the tensile test simulation model, the bending simulation model shows various complications by using exactly the same simulation approach. therefore the settings of the simulation model of a tensile test cannot be directly transferred to the simulation model of the bending test. the simulation model of the bending test has to be modified. the problems in the simulation model of the bending test (hybrid solution, 4 layers) and the belonging solutions are explained in table 3. figure 6. specimen with global fibre orientation. the soft contact, which is used is a normal behaviour with exponential law between the master and slave surface. this contact is implemented in abaqus. two parameters (clearance and pressure) have to be defined. with this contact the pressure of the stamp 25 a. kalteis, m. reiter, m. jerabek, z. major acta polytechnica ctu proceedings problem solution 1 fibre orientation does not rotate with specimen applying global fibre orientation (fig. 6) 2 elements break under pressure soft contact between specimen and stamp (fig. 7) 3 “kink” in curve (fig. 8) 10 layer model instead of 4 layer model 4 considering of different behaviour under compression [18] adjustment of hardening modulus for the upper 5 layers (fig. 9) 5 no valid hybrid parameters could be determined for some layers using micro solution 6 specimen breaks at a too low stress adjustment of failure parameters table 3. description of the problem and the corresponding solution for the bending simulation model. figure 7. illustration of position of applied soft contact. figure 8. illustration of kink in curve. figure 9. adjustment of material behaviour under compression; a) illustration of layers for the adjustment; b) red curve: stress-strain curve without adjustment, green curve: stress-strain curve with adjustment. is distributed over a larger area of the specimen [19]. therefore the stress concentrations on the specimen are lowered and as a result the specimen does not break under pressure anymore. the parameters are investigated by performing simulations of a bending test to find the most appropriate ones to solve the problem that the elements break under pressure. the reason for using a 10 layer model for the bending test is that the stress differences in the 10 layer model are lower than in a 4 layer model. this is because in the 10 layer model there is a smoother transition between the different fibre orientations. therefore the “kink” in the curve vanishes. unlike in the simulation model of the tensile test in the simulation model of the bending test the hybrid solution cannot be used. the reason for this is that in some layers no valid hybrid parameters could be determined by the software. therefore the micro solution has to be chosen. the failure parameters are reverse engineered for the ep material model. but for the bending tests the evp material model is used in order to consider the strain rate dependency. therefore the reverse engineered failure parameters may not fit as well for the evp material model as for the ep material model. as a result the parameters are fitted as it is described in section 6.2. 6. results 6.1. results of tensile test fig. 10 shows the result of the tensile test for a lowspeed strain rate. the material model is the elasticplastic one with strain rate of 10−3s−1. as the strain rate for the simulation is implemented in the elasticplastic material model also for the low-speed strain rates the dynamic explicit solver can be used to speed up the simulation. also an uncoupled simulation was performed in digimat mf. a difference in the failure stress between the simulations performed in abaqus 6.14 (integrative simulation) and digimat mf can be seen. 26 vol. 7/2017 figure 10. comparison of stress-strain curves of experiment, simulation performed in digimat mf 6.0.1 and simulation performed in abaqus 6.14. the reason for this is that the specimen shows a stress concentration in the region of the shoulder (fig. 11). figure 11. illustration of location of stress concentrations; a) specimen before failure, b) failed specimen. the notch effect at the specimen typically does not appear in reality. in reality the iso-mps specimen should break in the middle. in the simulation this cannot be realized in any specimen. because the simulation model itself cannot be modified to consider the notch effect, the failure parameters have to be fitted. therefore the parameters are fitted in this way that the notch effect can be considered. this fitting is performed by lowering the strain rate dependency by a power of 10. this means that the failure parameters for the strain rate of 10−2 s−1 are used for the elasticplastic material model for the strain rate of 10−3 s−1. in the following figure the results of the experiment and the simulation with the fitted failure parameters are shown. figure 12. comparison of stress-strain curves of experiment and simulation performed in abaqus 6.14 with fitted failure parameters. 6.2. results of bending test the bending test simulations are performed with the elastic-viscoplastic low-speed material model. because of the viscoplastic behaviour the strain rate has to be defined in abaqus. the static solver is used. in the following the result of the bending test for a specimen with misaligned fibres with the not fitted failure parameters is shown (fig. 13). as it can be seen the specimen breaks at a lower force than the experiment. one reason for this is described in section 5.3. figure 13. comparison of force/thicknessdisplacement curves of experiment and simulation. therefore the in-plane tensile and the transverse shear failure parameters are fitted. the axial tensile strength is kept constant because it has the most influence on layers with fibres, which are nearly perfectly aligned. in table 4 the previous and the fitted parameters are listed for the two different parameters. the difference between the previous and the fitted value is not very big. nevertheless these little increased values have a huge influence on the global result, which is illustrated in fig. 14. strength parameter previous value fitted value in-plane tensile strength 22.83mpa 25.32mpa transverse shear strength 13.38mpa 13.60mpa table 4. previous and fitted strength parameters. figure 14. comparison of force/thicknessdisplacement curves of experiment and simulation with fitted strength parameters. 27 a. kalteis, m. reiter, m. jerabek, z. major acta polytechnica ctu proceedings 7. conclusion with the knowledge of the specimen’s fibre orientation simulations can be set up, where this fibre orientation is considered. material and failure modelling was done for specimens with different fibre orientations and for low-speed to high-speed strain rates. it was shown that it is possible to determine failure in tensile and bending tests with low deviation (fig 15). figure 15. illustration of the deviation between failure force in the experiment and in the simulation. many influences have to be considered in a bending test (e.g. applying a global fibre orientation). little different values of failure strength parameters have a huge influence on the failure strength of the specimen. acknowledgements i would like to thank dr. michael jerabek for the possibility to do this research in cooperation with borealis polyolefine gmbh. references [1] digimat documentation 6.0.1. 2015. 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[19] abaqus analysis user’s guide, 6.14. 2014. 28 acta polytechnica ctu proceedings 7:22–28, 2017 1 introduction 2 specimens 3 material modelling 4 failure modelling 5 integrative simulation 5.1 interface digimat cae 5.2 simulation model of tensile test 5.3 simulation model of bending test 6 results 6.1 results of tensile test 6.2 results of bending test 7 conclusion acknowledgements references 55 acta polytechnica ctu proceedings 2(1): 55–59, 2015 55 doi: 10.14311/app.2015.02.0055 cataclysmic variables from sdss: a review and a look forward to lsst p. szkody1 1department of astronomy, university of washington, usa corresponding author: szkody@astro.washington.edu abstract the past and current projects of the sloan digital sky survey are reviewed in the context of applicability and results for cataclysmic variables. ongoing and future time domain surveys that will have impact on the field are also briefly discussed. keywords: cataclysmic variables dwarf novae intermediate polars polars optical photometry spectroscopy. 1 introduction cataclysmic variables (cvs) have been discovered in a variety of ways, with the largest numbers of new systems coming from survey work. the mode of operation and the limiting magnitude of each survey determines the different types of cvs that are discovered. the palomar-green survey (green et al. 1986) used blue color to find objects that were brighter than 16th magnitude, hence it found many bright novalike systems. x-ray surveys such as rosat (voges et al. 1999) identified those systems with high x-ray flux, hence many polars and intermediate polars were found. the hamburg survey (hagen et al. 1995) searched for emission line objects down to about 18th magntitude, finding sw sex stars, intermediate polars and long period dwarf novae. the sloan digital sky survey (sdss) used both photometry (to 22nd magnitude) and spectroscopy (to 19th magnitude) to identify all types of cvs, especially those with low accretion rates and orbital periods below the gap (szkody et al. 2011). current and future surveys are concentrating on variability as a means of identification and as a result are turning up many dwarf novae. the combination of all of these results will ultimately end in a better understanding of the total space density of all types of cvs. 2 sdss the sdss project (york et al. 2000) began taking data in 2000 and has continued to the present time, undergoing changing modes of operation and target selection. the past results on cvs from this survey, as well as current and future plans are summarized below. 2.1 sdss i,ii legacy survey sdss i started with a goal to photometrically survey the entire north galactic cap, as well as obtain spectra of a selected subset of objects within what is termed the legacy survey. in addition to the north cap, a 2.5 degree wide stripe centered on the celestial equator (stripe 82) was also included (see figure 1). the initial plan for completion in 5 years was extended (sdss ii) in order to finish the original footprint so the legacy encompassed the years 2000-2008 and the final entire database was released as data release 7 (dr7; www.sdss.org/dr7/). this database includes imaging data of 230 million objects, using 54 second integrations in 5 filters (ugriz). based on the colors obtained, targets (primarily quasars and galaxies) were selected by a variety of groups, within restrictions of fiber spacing, brightness limits, etc. for 1 hour integration spectra with wavelength coverage from 3800-9200å at a resolution of about 2000. plug plates were than drilled and threaded to accomodate 640 fibers resulting in 1.37 million spectra in dr7, including 225 thousand stars. since the sources receiving spectra were determined by color, and cvs have a broad range of colors (szkody et al. 2003), the main source of cv spectra turned out to be objects taken from quasar loci, which span a broad range of colors outside the main sequence footprint. the resulting computer and eye searches of all the legacy spectra for balmer lines turned up 285 cvs which included 30 polars, 6 ips and 9 systems containing pulsating white dwars. a list of these sources can be found in szkody et al. (2011) as well as on the web with links to the spectra (http://www.astro.washington.edu/users/szkody/cvs/). from 2000-2011 extensive followup on more than 300 55 http://dx.doi.org/10.14311/app.2015.02.0055 p. szkody nights was conducted on this list by many observers using apo, la palma, usno, steward, mdm, mmt observatories. as a result of this work, 151 orbital periods were determined that allowed specific classification of these objects and how they fit into population models. gänsicke et al. (2009) used 126 of the periods known at that time to reach major conclusions that enforced the magnetic braking model and confirmed the population synthesis predictions of howell et al. (2001): i.e. the majority of the disk accreting systems exist below the period gap and a period spike appears at the minimum period. the sdss results showed that the discrepancies in the past were primarily due to selection effects that favored the discovery of bright, long period systems, while sdss was able to uncover the larger population of faint sources. however, the percentages under the gap are slightly less and the period spike occurs at a slightly longer period than predicted so adjustments to the angular momentum losses are needed (knigge 2011). the fainter magntitude limit reached by sdss also revealed large numbers of accreting pulsators and low accretion rate polars (larps). of the 16 known accreting pulsators, 9 were found in the legacy survey. all of these showed broad balmer absorption lines surrounding the emission, providing a clear optical signature of the white dwarf. followup optical and uv results on the set of accreting pulsators has led to three major results. the first is that the instability strip is much wider than h atmosphere pulsating white dwarfs (zz ceti) (szkody et al. 2010). arras et al. (2006) attribute this to the existence of a he instability strip as well as hydrogen. because many of the accreting white dwarfs in this wide instability strip are observed not to pulsate, followup long term observations were conducted. this led to the second result that objects can stop pulsating, usually after an outburst, but sometimes when no outburst has occurred! e.g. sdss0745+45 (eq lyn, mukadam et al. 2013). third, in followup observations with hst, it was discovered that the pulsation that was present after outburst in v455 and appeared in the emission lines, not the continuum, presenting problems for a physical mechanism (szkody et al. 2013). of the 9 known larps, 7 were found in sdss. these objects have prominent humps due to cyclotron harmonics at high fields and low optical depth (wickramasinghe & ferrario 2000). finding larps in sdss data is not easy as the dependence of the harmonics on field strength moves them into different regions of color space. schmidt et al. (2005) calculated the sdss color ranges for various fields but there has as yet been no systematic search to find all the candidates. they estimate these could be a major contribution to the magnetic white dwarf population. several groups are using the sdss database to further understand the properties of the known cvs and to find further ones. a large hst program led by boris gänsicke is obtaining uv spectra of 40 cvs (including 12 discovered by sdss) to characterize the temperature of the white dwarf and the mass accretion rates over a variety of orbital periods and compositions. when combined with gaia distances, the masses of these white dwarfs will also be determined, leading to improved understanding of the evolution of close binaries. carter et al. (2013) discovered 29 new cvs in doing spectroscopic followup of am cvn candidates selected by color in the photometric database. breedt and gänsicke (2011) are obtaining spectra of the faintest cvs in sdss that are being discovered by crts (see section below). 2.2 sdss ii: segue and sn besides the legacy extension, sdss ii (2005-2008) contained the sloan extension for galactic understanding and exploration (segue) and a supernova survey. these results are contained in dr8. the main goal of segue was to explore the milky way, including its structure, history, kinematics, evolution and dark matter by mapping the positions, velocities, composition and temperatures of 240,000 stars (see figure 1 for the coverage compared to legacy). while this survey mainly targetted white dwarfs and giants, several cvs were included as their colors matched those of white dwarfs. the sn survey involved repeated imaging of the same region of the sky (stripe 82) during 3 months of each year. the repeat imaging over 275 deg2 with about 20 measurements on each object identified hundreds of new transient sources (sako et al. 2008). while the main goal was identifying sn, other types of variable stars were also found. the analysis of all the light curves of variable objects is ongoing and may include some cvs. a catalog of 13,051 variable sources brighter than g=20.5 from 1998-2007 stripe 82 data is in sesar et al. (2007). bhatti et al. (2010) provide a catalog of light curves for 221,842 point sources for half of the entire stripe 82 data. 2.3 sdss iii: segue-2, boss, apogee and marvels sdss iii (2008-2014) continues the segue project and adds 3 new enterprises. segue-2 obtained spectra of 119,000 stars with a concentration on the stellar halo with distances of 10-60 kpc. these data appeared in dr8 while dr9 updated the stellar parameters and added catalogs. the baryon oscillation spectroscopic survey (boss) updated the sdss fibers to 1000 and is producing spectra of many galaxies and quasars. while the target selection is not as optimal as it was in the 56 cataclysmic variables from sdss: a review and a look forward to lsst legacy survey, there are a few cvs which emerge in the spectra. dr9 was the first public release of boss spectra, while dr10 contains the latest data. the apo galactic evlution experiment (apogee) uses ir spectra to observe red giants throughout the galaxy. the first data appear in dr10. finally, the multiobject apo radial velocity exoplanet large-area survey (marvels) is monitoring the radial velocities of 11,000 bright stars to look for planets. 2.4 sdss iv: the future plans are underway to extend sdss from 2014-2020 with a continuation that involves apogee-2, eboss and manga. apogee-2 will continue the milky way exploration using apo and extend to the south with a 2.5m telescope at las campanas. eboss will continue boss but add 2 segments of interest to cvs: a time-domain spectroscopic survey (tdss ) that will obtain spectra of 100,000 variable sources and the spectroscopic identification of erosita sources (spiders). mapping nearby galaxies at apo (manga) will obtain spatially resolved spectra of 10,000 nearby galaxies. 3 current surveys several surveys are now ongoing and searching for objects that vary. the catalina real-time transient survey (crts; drake et al. 2009) consists of 3 telescopes: a 1.5m on mt. lemmon, a 0.7m on catalina and a 0.5m at siding springs. at the time of this meeting, 1022 potential cvs with outburst magnitudes brighter than 17 were posted on the web page nesssi.cacr.caltech.edu/catalina/brightcv.html. this page has a column that denotes whether the object is in the sdss photometric database and provides a direct link to sdss. since most of the objects were found at outburst, the quiescent magnitudes tend to be very faint (20-22nd mag) and therefore difficult to followup spectroscopically. several groups are now following up on the crts sources (woudt et al. 2012; thorstensen & skinner 2012). as noted above, elme breedt is also leading a project using gemini and other large telescopes to categorize the faintest crts sources that have 5 color photometry in sdss. the panoramic survey telescope & rapid response system (panstarrs1) is using an 1.8m telescope on haleakala, hawaii to complete a 2010-2013 northern sky transient survey which observes the available sky several times a month (tonry et al. 2012). one of the 12 key projects involves variables and explosive transients. a data release is planned for 2014 and a second telescope is under development. the palomar transient factory (ptf) involves the palomar 48 in schmidt telescope to image the sky from 2009-2014 to a magnitude of 21 on timescales from minutes to years to find new transients and variables, including cvs (rau et al. 2009). recent improvements (called iptf) have led to pipeline products that provides candidates within 30 minutes for spectroscopic followup. the followup spectroscopy is accomplished with the palomar 1.5m and other telescopes and some of that is available in wiserep (yaron & gal-yam 2012). skymapper is a robotic 1.35m survey telescope in siding springs, australia that is imaging the entire southern sky 36 times over 5 years in a series of 6 filters to 22nd mag that will provide spectral types of stars as well as variability information (keller et al. 2007). the data will be made public through the virtual observatory. in addition to these single, wide-field telescope surveys, there are 2 all-sky surveys which are using 2-4 cameras to image the sky. one is the all sky automated survey (asas) which images the entire sky to 14th mag in v and i bands from las campanas, chile and haleakala, maui (pojmanski 1997). the other is the mobile astronomical system of telescope-robots (master) which images to 19th mag at sites from russia and argentina (lipunov et al. 2010). 4 the future: lsst the future for investigation of variability lies with the large synoptic survey telescope (lsst). this 8.4m telescope situated in chile will image 18,000 deg2 of sky about 1000 times over 10 years (2020-2030). it uses 6 filters and will reach r = 24.5 mag on single nights and 27.5 on co-added images. the survey will produce alerts within minutes of observation as well as long term catalogs that will be made public. details may be found in the online science book (http://www.lsst.org/lsst/scibook). this survey will go several magnitudes fainter than sdss and should be able to find the population of period bounce systems that are predicted by models, as well as find unusual long term variability such as found by honeycutt et al. (2003) during their long term monitoring with roboscope. however, the difficulty lies in planning spectroscopic followup for 24-25 mag objects, which will require a lot of observing time on the largest telescopes available. time series photometry for short period, low amplitude variables will still be possible, but the problems of smart classification to pick out interesting variables from the multitude each night and the ensuing spectral confirmation remain to be solved. 5 conclusions the sdss has provided a significant database of cvs including a consistent set of medium resolution spectra for 285 systems and a photometric database that 57 p. szkody likely contains many more at faint magnitudes down to 22. due to the fainter magnitude limit compared to previous surveys, followup observations resulted in a large change in the observed orbital period distribution of cvs that has resolved some discrepancies in close binary evolution. current and future surveys rely on discoveries based primarily on variability, and so uncover large numbers of dwarf novae. as these surveys push further into the galactic plane and to fainter magnitudes with larger telescopes, the true space density of cvs and the distribution among types will become better known. however, the detailed information that comes from spectroscopy will be difficult to obtain for the faintest systems. acknowledgement the work with sdss data took place by many individuals over many years, starting with the sdss collaboration and extending to the public. support for the cv part of the research was provided by nsf grants ast 97-30792, ast 0607840 and ast 1008734 and nasa grant hst-go-12870.07a. funding for sdssiii has been provided by the alfred p. sloan foundation, the participating institutions, the national science foundation, and the u.s. department of energy office of science. the sdss-iii web site is http://www.sdss3.org/. sdss-iii is managed by the astrophysical research consortium for the participating institutions of the sdss-iii collaboration including the university of arizona, the brazilian participation group, brookhaven national laboratory, carnegie mellon university, university of florida, the french participation group, the german participation group, harvard university, the instituto de astrofisica de canarias, the michigan state/notre dame/jina participation group, johns hopkins university, lawrence berkeley national laboratory, max planck institute for astrophysics, max planck institute for extraterrestrial physics, new mexico state university, new york university, ohio state university, pennsylvania state university, university of portsmouth, princeton university, the spanish participation group, university of tokyo, university of utah, vanderbilt university, university of virginia, university of washington, and yale university. references [1] arras, p., townsley, d. m. & bildsten, l.: 2006, apj 643, l119. doi:10.1086/505178 [2] bhatti, w. a. et al. : 2010, apjs 186, 233. doi:10.1088/0067-0049/186/2/233 [3] breedt, e. & gänsicke, b. t.: 2011, aspcs 447, 203. [4] carter, p. j. et al.: 2013, mnras 429, 2143. doi:10.1093/mnras/sts485 [5] drake, a. j. et al.: 2009, apj 696, 870. doi:10.1088/0004-637x/696/1/870 [6] gänsicke, b. t. et al.: 2009, mnras 397, 2170. doi:10.1111/j.1365-2966.2009.15126.x [7] green, r. f., schmidt, m. & liebert, j.: 1986, apjs 61, 305. [8] hagen, h. j. et al.: 1995, aaps 111, 195. [9] honeycutt, r. k. et al.: 2003, aspcs 292, 329. [10] howell, s. b., nelson, l. a. & rappaport, s.: 2001, apj 550, 897. doi:10.1086/319776 [11] keller, s., bessell, m., schmidt, b. & francis, p.: 2007, aspcs 364, 177. [12] knigge, c.: 2011, aspcs 447, 3. [13] lipunov, v. et al.: 2010, adast 30l. [14] mukadam, a. s. et al.: 2013, aj 146, 54. [15] pojmanski, g.: 1997, aa 47, 467. [16] rau, a. et al.: 2009, pasp 121, 1334. [17] sako, m. et al.: 2008, aj 135, 348. [18] schmidt, g. d. et al.: 2005, apj 630, 1037. [19] sesar, b. et al.: 2007, apj 134, 2236. [20] szkody, p. et al.: 2003, aj 126, 1499. [21] szkody, p. et al.: 2010, apj 710, 64. doi:10.1088/0004-637x/710/1/64 [22] szkody, p. et al.: 2011, aj 142, 181. [23] szkody, p. et al.: 2013, apj 775, 66. doi:10.1088/0004-637x/775/1/66 [24] thorstensen, j. r. & skinner, j. n.: 2012, aj 144, 81. [25] tonry, j. l. et al.: 2012, apj 750, 99. doi:10.1088/0004-637x/750/2/99 [26] voges, w. et al.: 1999, aap 349, 389. [27] wickramasingeh, d. t. & ferrario, l.: 2000, pasp 112, 873. [28] woudt, p. et al.: 2012, mnras 421, 2414. [29] yaron, o. & gal-yam, a.: 2012, pasp 124, 668. doi:10.1086/666656 [30] york, d. g. et al.: 2000, aj 120, 1579. 58 http://dx.doi.org/10.1086/505178 http://dx.doi.org/10.1088/0067-0049/186/2/233 http://dx.doi.org/10.1093/mnras/sts485 http://dx.doi.org/10.1088/0004-637x/696/1/870 http://dx.doi.org/10.1111/j.1365-2966.2009.15126.x http://dx.doi.org/10.1086/319776 http://dx.doi.org/10.1088/0004-637x/710/1/64 http://dx.doi.org/10.1088/0004-637x/775/1/66 http://dx.doi.org/10.1088/0004-637x/750/2/99 http://dx.doi.org/10.1086/666656 cataclysmic variables from sdss: a review and a look forward to lsst figure 1: the sky coverage of the legacy and segue surveys in galactic (left) and celestial (right) coordinates, from www.sdss.org/dr7. discussion linda schmidtobreick: wouldn’t you expect the pulsating white dwarfs in accreting systems to be hotter than single white dwarfs? due to accretion, you would get a thin hot layer that influences the measured temperature but not necessarily the pulsation. paula szkody: yes, most accreting white dwarfs are indeed observed to be hotter than single white dwarfs. however, there are several parameters that could affect the pulsations (instability strip) in these accreting white dwarfs besides the temperature. the accreting ones are spun up by the accretion and the composition of the atmosphere is different due to the mass transfer from the secondary. right now, we don’t have enough data to distinguish which of these parameters are determining whether an accreting white dwarf will pulsate or not. 59 introduction sdss sdss i,ii legacy survey sdss ii: segue and sn sdss iii: segue-2, boss, apogee and marvels sdss iv: the future current surveys the future: lsst conclusions 246 acta polytechnica ctu proceedings 2(1): 246–251, 2015 246 doi: 10.14311/app.2015.02.0246 recurrent novae — a review k. mukai1,2 1cresst and x-ray astrophysics laboratory, nasa/goddard space flight center, greenbelt, md 20771, usa 2department of physics, university of maryland, baltimore county, 1000 hilltop circle, baltimore, md 21250, usa corresponding author: koji.mukai@nasa.gov abstract in recent years, recurrent nova eruptions are often observed very intensely in wide range of wavelengths from radio to optical to x-rays. here i present selected highlights from recent multi-wavelength observations. the enigma of t pyx is at the heart of this paper. while our current understanding of cv and symbiotic star evolution can explain why certain subset of recurrent novae have high accretion rate, that of t pyx must be greatly elevated compared to the evolutionary mean. at the same time, we have extensive data to be able to estimate how the nova envelope was ejected in t pyx, and it turns to be a rather complex tale. one suspects that envelope ejection in recurrent and classical novae in general is more complicated than the textbook descriptions. at the end of the review, i will speculate that these two may be connected. keywords: cataclysmic variables symbiotic stars recurrent novae individual: t pyx. 1 introduction nova eruptions are understood to be powered by thermonuclear runaway (tnr) on the surface of accreting white dwarfs. hundreds of objects in the galaxy have been seen to experience one nova eruption: these are called classical novae (cne). recurrent novae (rne) are objects that have been seen to experience multiple nova eruptions. there are currently 10 confirmed rne in the galaxy. between 10−6 and 10−4 m� of hydrogen rich material needs to be accreted to reach the critical temperature and density required for tnr. the critical mass is lower for more massive white dwarfs with higher gravity. therefore, we expect rne to contain near chandrasekhar mass white dwarf accreting at a high rate. this makes rne candidate progenitors of type ia supernova. for this reason, and because the recurrent nature of these objects allows studies that one cannot undertake for cne, rne have become the subject of intensive study. it is impossible to present a comprehensive review of rne in the space allotted; for that, the readers are referred to schaefer (2010) and anupama (2013). in this review, i will present selected highlights from multiwavelength campaigns on recent rn outbursts, highlighting the work of the e-nova collaboration1. i will also include results on several cne: some of these system may be unrecognized or unconfirmed rne, and others provide a useful comparison. i will also present some quiescent observations. i will discuss implications on the white dwarf mass, the ejecta mass, the quiescent accretion rate,and the evolutionary scenarios for rne and cne. 1.1 x-ray bursts: a cautionary tale although rne provide a unique opportunity to compare multiple nova episodes and possibly to compare accreted vs. ejected mass, only a handful of eruptions are observed for each system. this is in stark contrast to the studies of x-ray bursts, which are tnrs on accreting neutron stars. for example, linares et al. (2012) studied 398 x-ray bursts detected from the transient x-ray binary in the globular cluster, terzan 5, as the accretion changed by a factor of ∼5. this allowed these authors to study the relationship between the persistent luminosity, the burst recurrence time and the burst fluence, and thereby test the theory of tnr on neutron stars. unfortunately, analogous tests have not been possible yet in the case of rne. yet, even in the case of x-ray bursts, puzzles remain (galloway et al. 2008). one is the burst oscillations observed during the decay. the drifting period of burst oscillations reflect the spin period of the neutron star atmosphere, which changes as the atmosphere expands and then contracts during the course of a burst. the presence of the oscillations during the decay, however, requires inhomogeneous burning over the neutron star 1https://sites.google.com/site/enovacollab/ 246 http://dx.doi.org/10.14311/app.2015.02.0246 recurrent novae — a review surface, even though one might expect uniform burning at this stage. the other is that pairs of bursts can occur with very short (<10 min) recurrence times, much too short to have accreted sufficient fuel for a new burst, judging by the persistent x-ray luminosity. this requires a reservoir of unburnt fuel on or very near the neutron star surface. thus, our theoretical understanding of x-ray bursts appears incomplete. it may well be that the current theories of nova outbursts are equally incomplete regarding, e.g., the recurrence times of rne. 2 selected recent results 2.1 ejecta geometry montez et al. (in preparation) have detected extended x-ray emission in the chandra observations of rs oph obtained in 2009 and 2011. these structures are wellseparated from the central x-ray source in the e-w direction, and were seen to expand from 2009 to 2011. this x-ray emitting bipolar outflow appears to follow the same angular expansion curve inferred for radio and hubble space telescope (hst) bipolar structures observed earlier. the implied current expansion velocity is very high (of order 4,000 km s−1. one possible origin of the bipolar flow is that rs oph produced a true, well-collimated, jet near the time of nova eruption. another is that an initially spherical ejecta encountered an equatorial torus and slowed down except in the polar directions. since rs oph is an rn in a symbiotic binary, the wind of the giant mass donor is a potential source of such a torus (mohamed et al. 2013). however, similar shaping of the ejecta might also occur in cataclysmic variables (cvs), with a roche-lobe filling mass donor on or near the main sequence. in a series of simulations of the 2010 eruption of u sco by drake & orlando (2010), the accretion disk is destroyed by the blast wave. this interaction causes the ejecta to expand away from the orbital plane. one particular simplifying assumption used by these authors, that of a uniform density disk, is a cause for concern, and independent simulations are needed to confirm their results in general. nevertheless, the possibility that disk-blast wave interactions create bipolar outflow should be kept in mind for all novae, whether the underlying binary is a symbiotic system or a cv. the above-mentioned results on rs oph and u sco are both about the outflow during the most recent outbursts of rne, and may apply to cne as well. in contrast, one type of study unique to rne is the analysis of light echoes produced by ejecta from previous outbursts, as sokoloski et al. (2013) did for t pyx. the arrangement of the echo location on the sky and the progression of echos from east to west suggest a ringlike structure from a previous outburst. the delay times for echoes along the north-south axis suggest a distance of 4.8±0.5 kpc for t pyx. moreover, the time lags between different echoes suggest that the ring is inclined ∼30–40◦ relative to the plane of the sky. this is most likely to reflect the binary inclination, somewhat higher than values previously inferred for t pyx. regardless of the precise inclination angle, the very fact that an equatorial ring was formed by the ejecta is worth noting. 2.2 novae in symbiotic systems four of the known galactic recurrent novae are in symbiotic binaries: rs oph, t crb, v745 sco, and v3890 sgr. they are all s type systems: they have a normal red giant mass donor, an orbital separation of order 1 au, and an orbital period of order 1–2 years. in the other subtype, the d (dusty) type, the mass donor is an agb star; the d type systems have a much wider orbit than the s type systems. before 2010, all known tnr events in symbiotic systems were either a very slow “symbiotic novae,” or very fast rne (mikolajewska 2008). it is important to note that tnr can lead to a quasi-static configuration without explosive mass loss in symbiotic novae. also noteworthy is the fact that the accretion rate is high enough in the 4 s type symbiotic systems to produce rne. if we take 10−7 m� yr−1 as the typical wind mass loss rate of a normal red giant, then this implies either roche-lobe overflow or a very efficient mechanism to capture the wind, such as wind roch-lobe overflow (mohamed & podiadlowski 2010), although m giants in symbiotic binaries may have higher mass-loss rates (seaquist & taylor 1990). in march 2010, a d-type symbiotic system, v407 cyg, became a nova. it was noteworthy for being the first nova to be detected as gev γ-ray source with fermi lat (abdo et al. 2010); it was the subject of an intensive multiwavelength from radio to x-rays (nelson et al. 2012; chomiuk et al. 2012). the x-rays were predominantly from the shock between the nova blast wave and the wind of the mira type mass donor; interestingly, v407 cyg became x-ray bright after the gev signal faded. the thermal emission from the flashionized agb wind was the dominant source of radio signal. while we learned a lot about the nova event, we are left with one important question: how often does v407 cyg experience nova eruptions? is it an unrecognized rn, or are the eruptions much less frequent? 2.3 long period cvs darnley et al. (2012) proposed to classify novae into red giant, sub-giant, and main sequence systems. the orbital periods of the “sub-giant” systems are in the range 10 hrs to 6 days. according to the ritter & kolb catalog version 7.20 (ritter & kolb 2003), there are 46 247 k. mukai systems (excluding one uncertain entry in the catalog) in this orbital period range. of the confirmed rne, v894 cra, u sco and ci aql belong to this group, and a fourth, v2487 oph, probably has an orbital period in this range. the evolution of such long-period cvs has not been studied extensively to date, compared to those with periods under 10 hrs, for which the basic framework and much more have been established (knigge et al. 2011). cvs with similarly long orbital periods include several novae not known to be recurrent (gk per, v1017 sgr), supersoft sources (e.g., mr vel, cal 83), and v sge and other systems that may be related to supersoft sources. one possibility is that these systems are currently undergoing thermal timescale mass transfer (ttmt; schenker et al. 2002) or did so in the past. the evolution of cvs with p>10 hrs should be studied further, and a search for additional nova outbursts of systems like gk per may be worthwhile. 2.4 quiescent x-ray observations figure 1: possible white dwarf mass of v2487 oph for the magnetic (dashed line) and the non-magnetic (solid line) cases of the known recurrent novae, t crb and v2487 oph are bright hard x-ray sources detected with integral and with swift bat (see, e.g., baumgartner et al. 2013). when such hard x-ray emission is detected, it can constrain both the white dwarf mass and the accretion rate in quiescence. in both magnetic and nonmagnetic cases, hard x-rays are generated when the supersonic accretion flow encounters the white dwarf surface and is shock-heated. the hot plasma must radiatively cool before settling onto the white dwarf surface. in the case of magnetic cvs, the accretion flow is radial and its velocity is approximately at the freefall value (aizu 1973). the observed x-ray spectrum is multi-temperature in nature, with shock temperatures typically in the 10–50 kev range. the spectral curvature in the hard x-ray range is a reliable measure of the shock temperature, and can be used to infer the white dwarf mass (see, e.g., yuasa et al. 2010). the situation may well be more complex for the boundary layer of non-magnetic cvs, but the maximum temperature is unlikely to exceed that expected for strong shocks from keplerian velocity, and quiescent dwarf novae appear to follow the “keplerian strong shock” relationship (byckling et al. 2010). some authors have speculated that v2487 oph may contain a magnetic white dwarf, based solely on its bright, hard x-ray emission. however, i measure a shock temperature of ∼50 kev using the bat survey 8-channel spectrum, which corresponds to either a ∼0.9 m� magnetic white dwarf or a >1.24 m� non-magnetic white dwarf. given the rn nature of this object, and given that repeated xmm-newton observations have not revealed a spin modulation, the latter interpretation seems more likely. 2.5 high mass transfer rate: evolutionary or temporary? patterson et al. (2013) made the following simple prediction, based on average secular mass accretion rate: cvs above the period gap should experience nova eruptions once every 10,000 years or so, while those below the gap should recur once every 1 million year. for these normal cvs to be a rn, the accretion rate needs to be elevated by many orders of magnitudes above the secular mean. this is in contrast to the long-period systems with a sub-giant mass donor, where ttmt may drive a very high accretion rate. similarly, in symbiotic systems, the mass loss rate from the donor is high enough, although the fraction that can be captured by the white dwarf is highly uncertain. let us now consider the census of known classical and recurrent novae of various types with the above expectations in mind. among symbiotic stars, most novae are extremely slow and often referred to as symbiotic novae, the slowness suggestive of low-mass white dwarfs. the four wellknown symbiotic recurrent novae are all in s-type systems: the short recurrence time and the high velocity of the ejecta both suggest these to have massive white dwarfs. the bifurcation of novae in symbiotic stars into two such extreme groups is very different from the situation in cvs, and should be investigated further. although only a single outburst is known, the outburst properties of v407 cyg makes it a candidate rn in this context. since it is in a d type symbiotic system, with a much greater binary separation, an estimate of its quiescent accretion rate, when one is obtained, may tell us about how white dwarfs accrete in symbiotic stars, not to mention providing a clue as to its likely recurrence time. u sco, ci aql, and v894 cra are long-period systems; v2487 oph may belong in this group, although its orbital period has not been determined yet. the ttmt 248 recurrent novae — a review scenario points to the general framework for why these systems can be rne. more research is needed to understand why some long-period systems are sss, others rne, and yet others cne (as far as we know). this leaves im nor (in the period gap) and t pyx (below the gap) in the orbital period range with very low secular accretion rate and with only a small number of known classical novae (v1794 cyg, v per, ...). it is interesting to note that, while many classical novae are known above the gap (orbital period in the 3–10 hr range), no rne are known in this regime. this could purely a matter of small number statistics. at the same time, it could be that the mechanism elevating the accretion rate of t pyx and im nor far above the secular mean is much less effective for systems above the gap. 2.6 multi-wavelength observations of t pyx multi-frequency radio monitoring of novae is a powerful technique that allows us to estimate the total ejected mass in a relatively simple manner, although complications often arise (see, e.g., roy et al. 2012 and references therein.) the nova ejecta is initially optically thick in the radio, thus the brightening traces the angular expansion of the ejecta. as the ejecta becomes optically thin, first from the highest frequencies then progressively to lower frequencies, this allows the amount of mass to be estimated, as long as we have a handle on the temperature and clumping of the ejecta. at the same time, we know that early x-ray emission from novae is likely due to shocks in the ejecta (e.g., o’brien et al. 1994). with this mind, the e-nova collaboration has begun multi-wavelength observations of recent novae using the much improved karl g. jansky vla in the radio, and swift and other observatories in the x-rays. t pyx is one of the major targets of the e-nova collaboration. the radio and x-ray results are presented by nelson et al. (2014) and chomiuk et al. (2014), respectively. t pyx was largely undetected in the radio for the first ∼60 days since the discovery of the 2011 outburst, then started to rise around day ∼100. it was also x-ray faint during the first several months, and then started to rise slightly after the onset of the radio rise. the x-ray photons detected with swift xrt are a mixture of optically thin emission from the shocked shell and the supersoft emission from the still nuclear burning surface. it is difficult to disentangle the two using short snapshot observations, hence it is difficult to determine, e.g., the turn-on time of the supersoft emission. in the optical, t pyx remained near peak optical magnitude for 2 or 3 months, depending on where one defines the peak to have ended and decline to have begun. this implies a large photospheric radius, perhaps of order 5×107 km (∼ a third of an au; assuming a blackbody with a temperature of 10,000k, a distance of 4.8 kpc, and av ∼ 1.0, this radius corresponds to a visual magnitude of v∼7.9). this is well outside the central binary, yet it only takes of order 1 day for matter traveling at 600 km s−1 to reach this distance. for a shell at a distance of 1×108 km to have an optical depth of 1, which implies a column density of order 3 g cm−2 (assuming electron scattering dominates the opacity), the total mass of the shell must be greater than ∼ 5.0 × 10−7 m�. so the duration of optical peak implies either a continuous ejection of ∼ 5× 10−7 m� per day for several months, or that t pyx went into a quasi-static, red giant-like configuration during the peak, and ejected the extended atmosphere with a significant delay. in the latter case, the total mass of the extended atmosphere must be much greater than 5×10−7 m�, because it is a filled sphere and not a thin shell. schaefer et al. (2013) presented the detailed visual light curve of t pyx during the initial rise. until it reached v∼7.7, it can be modeled well assuming a uniform expansion of the ejecta, then the observed brightness drops below this model. if we equate this instance with the time when the optical depth of the ejecta dropped below 1.0, we infer that an initial shell of ∼ 6× 10−7 m� was ejected. such a small ejection is easy to hide in the radio data, although there is one detection on day 17 that could be interpreted as due to this. on the other hand, continuous mass ejection of ∼ 5 × 10−7 m� per day is difficult to reconcile with the deep radio non-detections followed by rapid brightening around day 60. rather, the radio data are consistent with a prolonged period of quasi-stationary configuration, and a delayed ejection of a more massive (of order 10−5 m�) shell. in addition, if the latter system was ejected with a larger velocity, then we expect shocked x-ray emission when it catches up with the initial ejecta. the existing x-ray data are broadly consistent with such a picture. 2.7 the cause of elevated mass transfer rate for t pyx, we have a clear-cut case that the mass transfer rate is elevated by several order of magnitudes above the evolutionary mean (gilmozzi & selvelli 2007). the same presumably applies to im nor as well. irradiation of the donor is often invoked as the explanation. however, theorists have long concluded that this requires hard photons, and therefore theoretical studies largely focus on x-ray binaries (see, e.g., hameury et al. 1986; king 1989). to quote from ritter (2000), “energy emitted in certain spectral ranges, 249 k. mukai as e.g., euv radiation and soft x-rays, is unlikely to reach the photosphere of the donor.” to reach the photosphere of k or m type dwarfs, irradiating flux needs to be able to penetrate above 1024 cm−2 of column, thus requiring strong flux above 10 kev. therefore, supersoft sources or photospheric emission of otherwise very hot white dwarf only irradiates the chromosphere and above, and not the photosphere. the irradiation mechanism studied in above-mentioned papers cannot work when the irradiating flux is in the form of soft x-ray and euv photons. while v1500 cyg is sometimes taken as an example of a system that is experiencing enhanced accretion rate due to irradiation, this is not necessarily the case. this is because one well-established effect of irradiation is to increase the luminosity of the existing structures, be it the secondary or the accretion disk. in fact, according to somers & naylor (1999), the elevated brightness of v1500 cyg, which is currently an asynchronous polar due to its 1975 nova eruption, is due to an orbitally modulated component, not due to the spin modulated component. since accretion luminosity should be modulated on the spin period, we know that the extra light is due to the irradiated face of the secondary. in this picture, the reflection of the gradually decreasing postnova white dwarf flux explains the secular changes in the brightness of v1500 cyg, without invoking variable accretion rate. thomas et al. (2008) obtained phase-resolved kband photometry of old novae of various ages since outburst. they were also able to interpret their results without invoking changing accretion rate. rather, in their interpretation, variable irradiation, and hence variable reflection, changes the brightness of the existing structures, the accretion disk and the secondary. at a minimum, this points out that an enhanced brightness is insufficient to prove an enhanced accretion rate. these studies also suggest that irradiation by a postnova does not lead to enhanced mass transfer, although they do not yet constitute a solid proof. if not irradiation, what other mechanisms can potentially enhance the mass transfer? here i speculate that the post-nova common envelope phase might be ultimately responsible, as follows. the ring geometry of the ejecta of t pyx (§2.1) suggests that the secondary plays a role in shaping the geometry of the ejecta. in symbiotic systems, slow novae can stay in the “plateau” phase for decades, whereas no such example is known among cvs, again implying that the secondary plays a role in ejecting the nova envelope. the potential role played by the common envelope system was first pointed out by macdonald (1980) and later studied quantitatively by, e.g., livio et al. (1990). the general consensus is that the common envelope phase can contribute to the ejection of the nova envelope, but only if the ejecta is moving more slowly than the orbital motion of the mass donor. the multi-wavelength data on t pyx indeed suggests that the envelope may have been in a quasi-stationary configuration for 2–3 months, as it is for decades in slow symbiotic nova. the possibility that many novae in cvs may not be able to eject the bulk of the envelope, if it were not for the common-envelope phase, should therefore be investigated. if common envelope phase is an important factor in the envelope ejection process, then this implies that the binary must have lost angular momentum. while the orbital period of t pyx was seen to increase after the 2010 eruption (patterson et al., this volume), the period increase only constrains the combination of ejected mass and angular momentum loss. if more than the minimum allowed mass was ejected, so was angular momentum. so the proposed scenario is that of a common-envelope interaction during the nova eruption, resulting in an impulsive angular momentum loss, which drives a higher accretion rate for the ensuing decades. i suggest that such a scenario deserves serious, quantitative analysis. 3 summary and conclusions recent rn eruptions have be subjected to intense multi-wavelength observing campaigns using advanced facilities, including the karl g. jansky vla, many ground-based optical/ir telescopes, hst, swift and other x-ray observatories. although not a new discovery as such, recent images of nova ejecta demonstrates once again that they are not spherically symmetric. in the case of t pyx, the multi-wavelength data strongly suggest that there was a initial, small ejection and a much larger, delayed ejection. these facts together suggest that the binary companion, via common-envelope interaction, may be involved in the ejection process. it is expected that rne harbor massive white dwarfs accreting at a very high rate. while the accretion rate may be high in some subset of rne for evolutionary reasons (symbiotic rne, and long-period systems), this is definitely not the case for t pyx and im nor. unfortunately, there is a serious difficulty with the commonly invoked mechanism of irradiation, when the irradiation is by soft x-ray and euv photons. i presented a possible scenario involving impulsive angular momentum loss during the common envelope phase. acknowledgement i thank my colleagues in the e-nova collaboration, particularly drs. nelson, sokoloski, and chomiuk, for stimulating discussion. 250 recurrent novae — a review references [1] abdo, a.a. et al.: 2010, sci. 329, 817. doi:10.1126/science.1192537 [2] aizu, k.: 1973, prog theor. phys. 49, 1184. doi:10.1143/ptp.49.1184 [3] anupama, g.g.: 2013, iausymp 281, 154. 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[35] yuasa, t. et al.: 2010, a&a 520, a25 discussion christian knigge: regarding the possibility that irradiation might enhance the mass accretion rate: i think that an enhancement is possible, at least via irradiation-driven winds from the donor. in fact, this model was first proposed for sss, where the irradiation is all in the soft x-ray/euv regime. koji mukai: it is true that the viability of irradiation-driven wind to enhance the accretion rate is a separate issue. i feel that sometimes the direct effect of irradiation is often too casually invoked as the explanation, and my intent was to advise caution. 251 http://dx.doi.org/10.1126/science.1192537 http://dx.doi.org/10.1143/ptp.49.1184 http://dx.doi.org/10.1088/0004-637x/761/2/173 http://dx.doi.org/10.1088/0004-637x/788/2/130 http://dx.doi.org/10.1088/0004-637x/746/1/61 http://dx.doi.org/10.1088/2041-8205/720/2/l195 http://dx.doi.org/10.1086/592044 http://dx.doi.org/10.1093/mnras/241.3.365 http://dx.doi.org/10.1088/0067-0049/194/2/28 http://dx.doi.org/10.1088/0004-637x/748/2/82 http://dx.doi.org/10.1086/168836 http://dx.doi.org/10.1088/0067-0049/187/2/275 http://dx.doi.org/10.1088/0004-637x/773/1/55 http://dx.doi.org/10.1046/j.1365-8711.2002.05999.x http://dx.doi.org/10.1088/2041-8205/770/2/l33 introduction x-ray bursts: a cautionary tale selected recent results ejecta geometry novae in symbiotic systems long period cvs quiescent x-ray observations high mass transfer rate: evolutionary or temporary? multi-wavelength observations of t pyx the cause of elevated mass transfer rate summary and conclusions 293 acta polytechnica ctu proceedings 2(1): 293–296, 2015 293 doi: 10.14311/app.2015.02.0293 non relational models for the management of large amount of astronomical data b. l. martino1, m. federici 2 1associated inaf iaps 2istituto di astrofisica e planetologia spaziali, inaf iaps via fosso del cavaliere 100, 00133 roma, italy corresponding author: brunolmartino@iasi.cnr.it abstract the objective of this paper is the comparison between two different database typologies: the relational and the nonrelational architecture, in the context of the applications related to the use and distribution of astronomical data. the specific context is focused to problems quite different from those related to administrative and managerial environments within which were developed the leading technologies on which are based the modern systems of massive storage of data. the data provided by astronomical instrumentation are usually filtered out by the front-end system (trigger, anticoincidence, dsp etc.), so they do not require special controls of congruence. moreover, the related storage systems must be able to ensure an easy growth, minimizing human systemistic interventions and automating the related actions. the use of a non-relational architecture (nosql), offers great advantages during the insertion of informations within a data base, while the response speed of the queries is mainly tied to their type and complexity. keywords: dbms mongodb nosql mysql gsc catalog. 1 using dbms a careful planning of the use of a file system allows to store informations in a rational way but, whatever the criterion used to organize an archive based only on files, it is not possible to build a search system that can guarantee sufficient flexibility. the user of a database, conceived in this manner, is required to know in detail its structure and it’s organization. almost any application focused on the analysis of astronomical data may read data in fits format (wells et al., 1981) fits format allows to add to a collection of data a set of additional information used to allow their better characterization. a dbms (data base management system) is a software infrastructure designed to operate on large data sets with the goal of optimizing the data: • storage • access • sharing • protection a dbms allows, through the use of its command language, the imposition of constraints of consistency, the creation of indexes to improve performance and retrieval of data independently from their physical representation. well-known examples of the use of advanced databases in high-energy physics are represented by spires (bourne et al., 2003), opera (agafonova et al., 2009) and !chaos (bisegni, 2012) and is consolidated practice their adoption as a storage medium in the ground segment. 1.1 relational models the relational databases today are the most popular; the model they are based it was proposed by codd (1970). the relational model allows access to data at the logical level by providing a complete independence from their physical organization. the logical representation of the data in the relational model is based on the concept of relationship, in algebraic terms; it is common to use the term ”table” in place of ”algebraic relationship” and the term ”relationship” to indicate an association between the data. the language sql (date et al., 1997) is the standard language ”de facto” for defining, manipulating and interrogation of relational databases; this is a declarative language and not procedural. in the relational model a logical unit of work is defined transaction and is constituted by a sequence of operations of reading and writing, which must meet some properties, known as acid property (from atomicity, consistency, isolation, durability). atomicity: a transaction is an atomic unit of operations, validated or canceled depending on whether or not they reach a successful conclusion (rollback / commit); consistency: at 293 http://dx.doi.org/10.14311/app.2015.02.0293 b. l. martino, m. federici the end of the transaction if the initial state is correct, even the final state must be; isolation: the action of a transaction should not interfere with each other; duration: the effects of a transaction must be persistent; the most popular relational databases are oracle (kunh, 2010) and mysql (schwartz, 2012)). 1.2 non relational models recently, have been developed a series of new dbms systems, to provide an high horizontal scalability, in order to achieve high performance in the read / write operations of database distributed across multiple servers geographically delocalized (cloud). many of these new systems are called nosql data stores. the definition of nosql, which stands for ”not only sql” or ”not relational”, was used for the first time in 1998 for an open source relational database. the non-relational systems, do not attempt to provide the classic acid guarantees, typical of relational databases, but embrace the model b.a.s.e. (basic available, soft-state, eventual consistency) where some constraints are relaxed: basic available: the database can operate even if a part is no longer available; soft-state: the system status may change over time even in absence of input data; eventual consistency: the data may not be updated immediately, but will be consistent throughout the system within a finite time as stated by the cap theorem (lynch et al., 2002) can not be achieved consistency, availability and partition tolerance at the same time but only two of these features at a time. the systems based on nonrelational architecture follow the base model and are those that allow to overcome the major limitation of the rdbms (relational data base management system): the scalability. in many areas, consistency and/or availability offered by relational databases are not essential, e.g. in astronomy and astrophysics applications. in a highly available and tolerant partitioning system, alteration of data base will reach all nodes not instantly but within a finite time, if a reading is done on a node is not synchronized with the last write, it returns the last valid data (stale data). 2 dbms nosql a property of nosql database is to be free of pattern (schemaless), with consequent advantages and disadvantages like ease of deployment, but sometimes, more difficulties to construct complex queries. the nonrelational logical models not have the same expressive power of the relational model and can be classified into four main families: key-value, column-family, document store and graph. the most common are the mongodb nosql architecture (chodorow, 2011), hbase (george, 2011) and cassandra (lakshman et al., 2010); their characteristics are summarized in figure 1. mongodb is a document-oriented database, which is based on aggregates, which may have a structure with multiple hierarchical levels and groups that can be variously indexed. mongodb uses the javascript language, which is inherently single-threaded while cassandra uses the language cql (cassandra query language, simplified variant of sql), which allows the management of distributed databases. both rely on the file system of the machine on which they were installed without introducing data abstractions. hbase is a distributed database (based on the project hadoop (sammer, 2012) written in java, that uses storage devices located on different hosts also geographically distributed, interconnected via networks. hbase uses hdfs, a portable and scalable distributed file system initially developed for the framework hadoop. figure 1: key features of nosql architectures. to carry out complex operations is used the mapreduce paradigm (dean et al., 2004), which allows to divide the computation in many elaborations of lower complexity to achieve the processing of large datasets in parallel on multiple cores/cpu/computer. 3 mysql vs mongodb in order to evaluate the possible use with advantage of non-relational architectures in astronomy and astrophysics area we realized the mdbirs system (showed in figure 2), composed by 10 pc, equipped with intel i7, 16gbytes of ram, 2 hd 1tbytes connected via ethernet lan at 1gbit of speed figure 2: the mdbirs system. 294 non relational models for the management of large amount of astronomical data in order to assess objectively the behavior of the system tests were carried out so as not to make use of the advanced characteristics of the query languages used. for this reason it was chosen as the working set of data the gsc catalog (stars general catalog). gsc is composed of a single table and is used primarily to provide support for the planning and guiding stars of the hst observations (dalcanton, 2009), the jwst (gardner at al., 2006), gaia (busso et al., 2012) and some groundbased telescopes of new generation. furthermore, the services provided by the machines on which they are installed databases are not affected by processes (user or system) not strictly essential to their functioning and the software installed on the machines which host the test has been aligned to the same versions. the databases under test are the two most widely used open source architectures in the world, mysql for its versatility, speed and diffusion and mongodb for its attitude to the horizontal growth (scalability) and its robustness. starting from the data available, have been generated some of the series of samples of increasing amplitude, so as to highlight the behavior of the two systems both with regard to populate the database, than to retrieve the information of interest. the test was performed using queries significant from the point of view of the community of users, which allow to highlight the behavior of databases in real operating conditions. in particular: • query1: selection on healpix (mapping system applied to the celestial sphere) • query 2: selection of objects in a spatial region which satisfy some conditions in magnitude and color • query 3: selection of non-stellar objects which meet a condition in color • query 4: computing of the average magnitudo, resolution of one degree square 4 test results the database engine installed by default in mysql since version 5.0 (innodb) is transactional, acid compliant and uses the row-level locking strategy (constraint of exclusive use for the time necessary to perform the required actions). the data entry test was made from data provided in csv (text data whose fields are marked by the separator character comma.) as shown by the graph in figure 3, the behavior of mongodb is faster than mysql, thanks to the absence of checks carried out on the integrity of the data; information are stored in files as key-value pairs. figure 3: insert performances vs data set size. regarding the execution time of the test queries, the results are shown in the graph of figure 4 and are substantially comparable. in the case of the gsc catalog , the occupation of the relevant mysql table is about 116 gbytes of data collection while the corresponding mongodb occupies about 657 gbytes (the size is 5 times bigger). the tables were not associated with indexes, so searches are performed on the whole set of data with a time dependent to amplitude of the set itself. figure 4: queries performances vs data set size. 5 future activities mongodb is a good choice to obtain good safety and performances using local data sharding. our goal is to achieve a full geographic data delocalization (cloud) in order to obtain: continuity of access to data (total disaster recovery) to the user community optimized average access time we evaluated two possible scenarios: hbase: hadoop based nosql data base cassandra: the apache cassandra database hbase is a masterslave system including two types of machines: hmaster: access control hregionserver: local data replication by using the stargate plugin can be achieved local caches able to speed up response times by minimizing the network traffic to the master. every region server keeps a copy of the data so the system ensures very 295 b. l. martino, m. federici high reliability. it is a nosql solution initially developed by facebook which has in the p2p architecture its focal point. 6 conclusions mongodb has proven much more efficient and fast in data entry and is particularly suited to the management of flows of data to be stored without downtime. in the configuration we used the rate of loading is about 15000 rows/sec (the average rows length is 256 bytes). by using more powerful hardware such as high speed network interfaces (10 gbit/sec or higher) it’s possible to greatly increase the speed of data acquisition. regarding the search of data in the database the results show a behavior strongly dependent on the number of records and the presence or absence of critical elements such as complex calculations. the command language of mongodb does not contain any advanced mathematical primitives as in the case of mysql, which can rely on a large library of mathematical functions. the use of mongodb on structures designed to be handled by a rdbms is inappropriate because it does not exploits the potential of its schemaless organization (nosql). acknowledgement we thanks paola marrese by asdc-asi for providing us the test data, , the director of iaps-inaf prof pietro ubertini, and a special thanks to franco giovannelli and his staff for allowing us to participate to this workshop references [1] wells, d. c., greisen, e. w., and harten, r. h.: 1981, a flexible image transport system. astronomy & astrophysics supplement series, 44, 363-370. [2] bourne, c. p., hahn, t. b.: 2003, a history of online information services, 1963-1976, mit press. [3] agafonova, n., et al.: 2009, the detection of neutrino interactions in the emulsion/lead target of the opera experiment, journal of instrumentation. doi:10.1088/1748-0221/4/06/p06020 [4] bisegni, c.: 2012, thesis in computer science, university tor vergata, rome. [5] codd, e.f.: 1970, a relational model of data for large shared data banks, communications of the acm 13 (377-387). doi:10.1145/362384.362685 [6] c. j. date, c. j., darwen, h.: 1997, a guide to the sql standard: a users guide to the standard database language sql, addison wesley. [7] kuhn, d.: 2010, pro oracle database 11g administration, apress. doi:10.1007/978-1-4302-2971-1 [8] schwartz, b.: 2012, high performance mysql: optimization, backups, and replication, o’reilly. [9] lynch, n., gilbert, s.: 2002, brewer’s conjecture and the feasibility of consistent, available, partition-tolerant web services, acm sigact news, volume 33 issue 2, pg. 51-59. [10] chodorow, k.: 2011, scaling mongodb, o’reilly. [11] george, l: 2011, hbase: the definitive guide, o’reilly. [12] lakshman, a., malik, p.: 2010, cassandra: a decentralized structured storage system, acm sigops operating systems review, vol. 44, no.2. doi:10.1145/1773912.1773922 [13] sammer, e.: 2012, hadoop operations, o’reilly. [14] dean, j., ghemawat, s.: 2004, mapreduce: simplified data processing on large clusters, in osdi’04: sixth symposium on operating system design and implementation, san francisco, ca, december. [15] dalcanton, j.j.: 2009, 18 years of science with the hubble space telescope, nature jan 1;457(7225):41-50. [16] gardner, j. p., at al.: 2006, the james webb space telescope, space science reviews. doi:10.1007/s11214-006-8315-7 [17] busso, g., de angeli, f., montegriffo, p.: 2012, the gaia photometric data processing, in proc. spie 8442, space telescopes and instrumentation 296 http://dx.doi.org/10.1088/1748-0221/4/06/p06020 http://dx.doi.org/10.1145/362384.362685 http://dx.doi.org/10.1007/978-1-4302-2971-1 http://dx.doi.org/10.1145/1773912.1773922 http://dx.doi.org/10.1007/s11214-006-8315-7 using dbms relational models non relational models dbms nosql mysql vs mongodb test results future activities conclusions 156 acta polytechnica ctu proceedings 2(1): 156–160, 2015 156 doi: 10.14311/app.2015.02.0156 outburst properties of v1504 cyg and v344 lyr j. k. cannizzo1,2 1cresst, dept. of phys., umbc, baltimore, md 21250, usa 2nasa/gsfc/astroparticle physics lab., greenbelt, md 20771, usa corresponding author: john.k.cannizzo@nasa.gov abstract i begin by reviewing dwarf novae and the disk instability theory, and then present an overview of three ideas for producing superoutbursts in the su uma stars − the thermal tidal instability, irradiation-induced secondary mass overflow, and the plain vanilla disk limit cycle instability. i discuss the properties of the outbursts in two su uma systems observed by kepler in the context of the three theories. i conclude with a look beyond the su uma systems. keywords: cataclysmic variables dwarf novae optical photometry individual: v1504 cyg, v344 lyr, u gem, ss cyg. 1 introduction 1.1 disk instability model the outbursts in dwarf novae (dne), a subclass of cataclysmic variables (cvs warner 1995), are thought to be due to a limit cycle instability operating within the accretion disk (smak 1984) that episodically stores up matter (during quiescence) and dumps a fraction of it onto the accreting wd (during outburst). the basic disk instability model is now generally accepted as the correct explanation for dwarf nova outbursts (smak 1984, cannizzo 1993a, lasota 2001). the strongest point of the model is its prediction of a dividing line between novalike and dwarf nova systems (smak 1984), a line which has no free parameters1. for the systems above this line, the rate of accretion feeding into the outer disk is such that the entire disk is always in a hot, ionized state. other strengths of the theory include its natural ability to account for slow and fast decays of dn outbursts as being due either to viscous or thermal decay, the natural tendency of the model to produce alternating long and short outbursts (cannizzo 1993b), and the fact that the outer disk radius router continues to contract in quiescence following a dn outburst, whereas in the secondary mass-overflow model there is a one-to-one relation between disk luminosity and router (ichikawa & osaki 1992). smak (1984) was the first to use the relation between the fast rate of decay in dwarf nova outbursts and orbital period (i.e., the bailey relation) to constrain the value of the shakura-sunyaev (1973) alpha parameter in the ionized disk, αhot ' 0.1. the high fidelity kepler data now enable us to trace deviations from strictly exponential decay for the fast decays (cannizzo et al. 2012=c12), and also to utilize the slow rate of decay, wherein the entire disk resides in a hot, ionized state. the fact that the viscous and thermal time scales differ by a factor h/r means that this ratio can be directly calculated to be ∼0.01 − 0.02 (cannizzo 1998; menou, hameury, & stehle 1999). although successful as a model for outbursts, it has been known for some time that there must be various add-ons to the theory in order to have a complete theory for the accretion disk, including something like a coronal siphon flow (meyer & meyer-hofmeister 1994) or some other type of evaporative instability (e.g., shaviv & wehrse 1986) to transfer matter from the disk onto the wd during quiescence to get accretion. 1.2 su uma systems the su uma stars represent short orbital period dwarf novae (dne), porb < 2 hr, displaying normal outbursts (nos) and superoutbursts (sos) long outbursts with superhumps (shs). although the contrast between nos and sos seems quite dramatic, van paradijs (1983) has shown that the properties of sos, seen in systems below the period gap, can be understood as a natural continuation of the long outbursts in dne above the period gap porb > 3 hr. in addition, sos are defined by the existence of shs, modulations in the outburst 1 for ∼10 yr it appeared that the best studied dwarf nova, ss cyg, was on the wrong side of the line (harrison et al. 1999, schreiber, hameury, & lasota 2003). however, this prognosis was based on an incorrect distance (159 ± 12 pc). the corrected distance (114± 2 pc) reconciles data and theory (miller-jones et al. 2013). 156 http://dx.doi.org/10.14311/app.2015.02.0156 outburst properties of v1504 cyg and v344 lyr light curve at periods a few percent longer than the orbital period. the prevailing theory is that when the outer disk edge surpasses the point of 3:1 resonance with the binary orbit, an eccentric disk develops that precesses progradely in the binary frame (whitehurst 1988). more recent work indicates that the disk is not statically eccentric but has a fundamental “breathing” mode − oscillating between circular and eccentric (montgomery 2012ab). these shs are referred to as positive superhumps (pshs) since their periods exceed porb; there also exist negative superhumps (nshs) with periods a little less than porb thought to be indicative of a tilted, retrogradely precessing disk (patterson et al. 1993). the two disk states can and sometimes do coexist (montgomery 2012ab). in recent years three scenarios have emerged to account for sos: (i) the thermal-tidal instability (tti osaki 1989) which combines the normal disk instability model and the precessing disk model, (ii) irradiationinduced enhanced mass overflow from the mass-losing star, and (iii) the plain disk instability (pdi) model (cannizzo et al. 2010=c10). in a recent series of papers osaki & kato (2013abc) have discussed the relative merits of these three models within the context of recent kepler observations of v1504 cyg and v344 lyr. 2 kepler observations of v1504 cyg and v344 lyr c12 find that the durations of the nos within a supercycle increase monotonically, whereas the durations of the quiescence intervals between nos can either increase monotonically, or else increase to a local maximum about half way to the next so, and then decrease. these supercycles for which the recurrence times for nos reach a maximum roughly half way between sos present a challenge for the tti model, in which one expects a monotonic increase in disk mass, angular momentum, and triggering radius as the next so approaches. osaki & kato (2013c) acknowledge this difficulty, and also point out that this criticism, given by c12, applies equally well to the pdi calculations presented by c10. this is a good point − in fact the calculations presented in c10 did not show any variation in recurrence time for nos. figure 1 shows the latest pdi calculations of sos in a su uma. ok13a discuss the amplitude of the precursor dip and note that, at shorter wavelengths, the dip tends to stand out more strongly. one of the best examples is examples is in oy car (porb = 1.51 hr; mauche & raymond 2000) where simultaneous visual and euv (∼100 å) observations are presented of a so. embedded precursors which are simultaneously small in the optical and large in the euv provide a challenge to both tti and pdi models. in the tti model, the amplitude of the precursor can be precisely controlled by tweaking the strength of the increase in tidal torque accompanying the crossing of the 3:1 resonance radius by router, and the delay time ttti, delay accompanying its onset. for the sos there can be no precursors, as in the early tti models (e.g., ichikawa, hirose, & osaki 1993), or there can be precursors which are well-defined both in v and euv wavelengths, e.g., in models with ttti, delay = 1.75 d (schreiber, et al. 2004, see their fig. 3). v344 lyr figure 1: a comparison of kepler data on v344 cyg with two sos in a long light curve using the pdi model. a new idea introduced in ok13a is that the presence of time-varying nshs, when they are present, gives us a handle on variations in the outer disk radius. larwood (1998) gives a general expression for the (nodal) precessional frequency associated with a tilted disk ωnpr = ωorb − ωnsh which is based on the surface density distribution σ(r) and accretion disk tilt angle θ, ωnpr = 2πνnpr = −3 4 gm2 a3 ∫ σr3dr∫ σωr3dr cos θ, (1) where m2 is the secondary mass and a the binary separation. for a nominal power law distribution in surface density, νnpr νorb = −η 3 7 q√ 1 + q (router a )3/2 cos θ, (2) where η is a constant of order unity. the observed νnsh(t) variations in v1504 cyg reveal a disk contraction between nos, superposed on a longer term expansion between sos. this approach was criticized by smak (2013) who argued that, if one takes the time derivative of larwood’s pnsh equation, one obtains an expression with five terms (see his eqn. [7]), only one of which is related to the outer disk radius. 157 j. k. cannizzo the disk instability model provides a definitive prediction of σ(r) at all times, and therefore one may carry out a calculation of the long-term accretion disk evolution relevant for an su uma system, and do a direction comparison of νnsh calculated using the exact and approximate expressions. the results are shown in figure 2. the panels show the light curve, disk mass, disk radius, and the exact and approximate calculations for νnsh. the approximate expression gives a very good representation of the exact formula, which vindicates the underlying idea of ok13a and supports their use of νnsh(t) to track router(t). figure 2: a calculation of the pdi model for a su uma system. shown are (i) the kepler light curve, (ii) the disk mass, in units of 1023 g, (iii) the outer disk radius, in units of 1010 cm, (iv) the nsh frequency calculated using the larwood formula, and (v) the nsh frequency calculated using the approximate formula given ok13abc, taking η = 1.5. there is actually only one small difference between osaki’s tti and the pdi model for superoutbursts, namely, in the tti model there is a strong and brief contraction of the outer disk radius due to the (hypothesized) strong increase in tidal torque from the secondary star. an obvious way to distinguish between the two models is to closely monitor the outer disk radius in an eclipsing su uma star during the early onset of a so to see if there is a sudden, brief decrease in router. smak (2013) argues that this observation has already been carried out and shows no such contraction; ok13c counter that the time period in question was well into the so and therefore missed the start of the so. 3 looking beyond the su uma systems ok13abc argue that the precursor in sos is due to the onset of the tti, whereas i have argued it is a natural consequence of the pdi. an obvious next step would be to look in detail at long dn outbursts in systems where we do not expect the tti to operate − systems above the period gap where the outer disk radius never reaches the 3:1 radius. even if one accepts the fundamental tenet of the tti, namely a causal relation between whitehurst’s precessing eccentric disk and the di, it could not possibly be a factor because the disks in long period systems are never subject to the 3:1 instability. if one sees precursors in long dn outbursts in these systems, then they must be due to a more general aspect of the di. the two best studied dne are both longward of the period gap and should not experience the 3:1 instability − u gem and ss cyg. they have > 100 yr light curves, but unfortunately the bulk of the data is not precise enough to enable any statement to be made about the detailed shape of the outburst onset. cannizzo (2012) examined the aavso data for these systems, and found brief stretches of the light curves for which the number of observations entering into daily means exceeds ∼103, concomitant with the use of digital photometry. although still not on a par with kepler data, these data do afford a more detailed look at the outburst light curve shapes than the usual data. there are two long outbursts in u gem and one in ss cyg for which a statement can be made concerning the shape of the outburst light curve during outburst onset; one of the u gem outbursts shows no obvious precursor, one does, and the one ss cyg long outburst also does. in fact, the flattened shape of the precursor is similar to that seen in fig. 13 (panel 2) of cannizzo (1993b) in modeling ss cyg. these outbursts provide a hint that embedded precursors during long outbursts may not be confined to the su uma systems. 4 summary kepler light curves of short period dne have resparked interest in the nature of sos and led to the question: is the thermal-tidal instability needed, or can the plain vanilla version of the accretion disk limit cycle do the job all by itself? a detailed time-resolved study of an eclipsing su uma system during so onset should settle the question − if there is a dramatic contraction of the disk at so onset, the tti would be preferred; if not, the plain di model would be sufficient. also, recent work 158 outburst properties of v1504 cyg and v344 lyr by osaki & kato has shown that the time varying nsh frequencies νnsh(t) can be taken as a surrogate for the outer disk radius variations router(t). finally, it may be necessary to look beyond the short period dwarf novae to gain perspective on the nature of embedded precursors in long outbursts. references [1] cannizzo, j.k.: 1993a, in accretion disks in compact stellar systems ed., j.c. wheeler (singapore: world scientific), 6. [2] cannizzo, j.k.: 1993b, apj, 419, 318. doi:10.1086/173486 [3] cannizzo, j.k.: 1998, apj, 494, 366. doi:10.1086/305210 [4] cannizzo, j.k.: 2012, apj, 757, 174. doi:10.1088/0004-637x/757/2/174 [5] cannizzo, j.k., smale, a.p., wood, m.a., et al.: 2012, apj, 747, 117. doi:10.1088/0004-637x/747/2/117 [6] cannizzo, j.k., still, m.d., howell, et al.: 2010, apj, 725, 1393. doi:10.1088/0004-637x/725/2/1393 [7] harrison, t.e., mcnamara, b.j., szkody, p., et al.: 1999, apj, 515, l93. doi:10.1086/311982 [8] ichikawa, s., hirose, h., osaki, y.: 1993, pasj, 45, 243. [9] ichikawa, s., osaki, y.: 1992, pasj, 44, 15. [10] larwood, j.: 1998, mnras, 299, l32. doi:10.1046/j.1365-8711.1998.01978.x [11] lasota, j.-p.: 2001, new astron. rev., 45, 449. doi:10.1016/s1387-6473(01)00112-9 [12] mauche, c.w., raymond, j.c.: 2000, apj, 541, 924. doi:10.1086/309489 [13] menou, k., hameury, j.-m., stehle, r.: 1999, mnras, 305, 79. [14] meyer, f., meyer-hofmeister, e.: 1994, a&a, 288, 175. [15] miller-jones, j.c.a., sivakoff, g.r., knigge, c., et al.: 2013, science, 340, 950. doi:10.1126/science.1237145 [16] montgomery, m.m.: 2012a, apj, 745, l25. doi:10.1088/2041-8205/745/2/l25 [17] montgomery, m.m.: 2012b, apj, 753, l27. doi:10.1088/2041-8205/753/2/l27 [18] osaki, y.: 1989, pasj, 41, 1005. [19] osaki, y., kato, t.: 2013a, pasj, 65, 50. [20] osaki, y., kato, t.: 2013b, astro-ph/1305.5877. [21] osaki, y., kato, t.: 2013c, astro-ph/1309.3722. [22] patterson, j., thomas, g., skillman, d.r., diaz, m.: 1993, apjs, 86, 235. [23] schreiber, m.r., hameury, j.-m., lasota, j.-p.: 2003, a&a, 410, 239. [24] schreiber, m.r., hameury, j.-m., lasota, j.-p.: 2004, a&a, 427, 621. [25] shakura, n.i., sunyaev, r.a.: 1973, a&a, 24, 337. [26] shaviv, g., wehrse, r.: 1986, a&a, 159, l5. [27] smak, j.: 1984, acta astron., 34, 161. [28] smak, j.: 2013, acta astron., 63, 109. [29] van paradijs, j.: 1983, a&a, 125, l16. [30] warner, b.: 1995, cataclysmic variables (cambridge: cambridge univ. press). [31] whitehurst, r.: 1988, mnras, 232, 35. discussion margaretha pretorius: if there is no tidal instability how do you make superhumps? john cannizzo: the tidal instability is not being disputed. in both osaki’s thermal-tidal instability model and the plain disk instability model superhumps are due to a precessing eccentric disk which becomes manifest when the outer disk radius surpasses the the 3:1 radius. the question is then whether this has anything to do with the superoutbursts: osaki would say yes, i would say no. raymundo baptista: yesterday i showed inferred αcold values for three quiescent su uma stars, which show αcold ∼ 10−1 ∼ αhot. my interpretation is that this eliminates the possibility of the disc instability model to explain their outbursts. could you please comment on this? john cannizzo: what’s the temperature of that gas? raymundo baptista: about 6000 k. 159 http://dx.doi.org/10.1086/173486 http://dx.doi.org/10.1086/305210 http://dx.doi.org/10.1088/0004-637x/757/2/174 http://dx.doi.org/10.1088/0004-637x/747/2/117 http://dx.doi.org/10.1088/0004-637x/725/2/1393 http://dx.doi.org/10.1086/311982 http://dx.doi.org/10.1046/j.1365-8711.1998.01978.x http://dx.doi.org/10.1016/s1387-6473(01)00112-9 http://dx.doi.org/10.1086/309489 http://dx.doi.org/10.1126/science.1237145 http://dx.doi.org/10.1088/2041-8205/745/2/l25 http://dx.doi.org/10.1088/2041-8205/753/2/l27 j. k. cannizzo john cannizzo: one of the limitations of the standard disk instability theory has always been that it’s not a complete theory certainly it doesn’t work at all to describe the quiescent state. if you take the model seriously, the plots in the movie i showed indicate temperatures in quiescence of ∼2000-3000 k. also, we see significant evidence for accretion during quiescence mainly through soft x-ray emission, which is not predicted by the di theory since in quiescence the accretion rate would be zero. so the bottom line is that the quiescence gas you observe must be due to something extrinsic to the di model. 160 introduction disk instability model su uma systems kepler observations of v1504 cyg and v344 lyr looking beyond the su uma systems summary acta polytechnica ctu proceedings doi:10.14311/app.2016.6.0034 acta polytechnica ctu proceedings 6:34–39, 2016 © czech technical university in prague, 2016 available online at http://ojs.cvut.cz/ojs/index.php/app the dubins traveling salesman problem with constrained collecting maneuvers petr váňa∗, jan faigl dept. of computer science, czech technical university in prague, technická 2, 166 27 prague, czech republic ∗ corresponding author: vanapet1@fel.cvut.cz abstract. in this paper, we introduce a variant of the dubins traveling salesman problem (dtsp) that is called the dubins traveling salesman problem with constrained collecting maneuvers (dtsp-cm). in contrast to the ordinary formulation of the dtsp, in the proposed dtsp-cm, the vehicle is requested to visit each target by specified collecting maneuver to accomplish the mission. the proposed problem formulation is motivated by scenarios with unmanned aerial vehicles where particular maneuvers are necessary for accomplishing the mission, such as object dropping or data collection with sensor sensitive to changes in vehicle heading. we consider existing methods for the dtsp and propose its modifications to use these methods to address a variant of the introduced dtsp-cm, where the collecting maneuvers are constrained to straight line segments. keywords: dubins vehicle, dtsp, non-holonomic vehicle, path planning, collecting maneuver. 1. introduction the dubins traveling salesman problem (dtsp) [1] has been subject of studies for many years. the problem is to find a shortest tour visiting a given set of target locations by the dubins vehicle [2] that models a fix-wing aircraft (or car-like vehicle) with a limited minimal turning radius and a constant forward velocity. the herein studied path planning problem is motivated by surveillance and rescue missions to visit a set of target locations by a fix-wing aerial vehicle. such a problem can be formulated as the variant of the combinatorial optimization the traveling salesman problem (tsp) where the target locations have to be connected by dubins maneuvers. the problem is to determine a sequence of visits to the targets together with the most suitable heading of the vehicle at each target location such that the total tour length is minimized. dubins proved that the optimal path between two configurations of the dubins vehicle can be found analytically by enumerating six possible maneuvers [2]. however, it is necessary to determine the optimal headings to find the optimal maneuver analytically, which in fact depend on the optimal sequence of visits to the targets. therefore, this challenging problem is called the dubins traveling salesman problem (dtsp) rather than just the tsp to distinguish computational challenges arising from the constrained turning radius. the dtsp is np-hard [3] as for zero minimal turning radius, the problem becomes the tsp. even though an ordinary formulation of the dtsp provides a solution of the problem to visit a set of target locations by an aircraft, the problem considered in this paper requires to perform specific collecting maneuvers to reliably accomplish the mission. such a requirement is arising from the need to get a visual contact with the drop-off location. then, the vehicle figure 1. an example of the dtsp-cm instance with straight collecting maneuvers in a cargo airdrop mission. target locations are depicted as small green disks, maneuvers are the red straight line segments, and particular trajectories for a reliable cargo drop-off are in green. the blue curves stand for the dubins maneuvers which connect the determined collecting maneuvers into the closed tour. is required to move straight ahead during the dropping phase itself. an example solution of such an object dropping mission is depicted in fig. 1. in this paper, we propose a novel extension of the ordinary dtsp to address the requirement of specific maneuvers for target accomplishment. the introduced problem is called the dubins traveling salesman problem with collecting maneuvers (dtsp-cm). further, we study a special case of the dtsp-cm where collecting maneuvers are straight line segments (denoted as the dtsp-scm) and we propose modifications of the existing approaches to the dtsp to solve this constrained variant of the dtsp-cm. the paper is organized as follows. an overview of the related work with various dtsp approaches 34 http://dx.doi.org/10.14311/app.2016.6.0034 http://ojs.cvut.cz/ojs/index.php/app vol. 6/2016 dubins traveling salesman problem is provided in section 2. the proposed problem is formally introduced in section 3 and modifications of the existing dtsp approaches are proposed in section 4. evaluation of the proposed modifications of the existing approaches is presented in section 5. finally, conclusion remarks are in section 6. 2. related work various approaches have been proposed to address the dtsp that can be broadly divided into three main classes: 1) decoupled approaches, 2) sampling-based approaches, 3) and evolutionary-based approaches. in this section, a brief overview of representative approaches of each particular class is provided to clarify the context for the introduced dtsp-cm and proposed modifications of the particular approaches to solve the constrained variant of the dtsp-cm with straight line collecting maneuvers. probably the first approach to the dtsp is the alternating algorithm (aa) introduced in [1] which can be categorized as a decoupled approach, since it addresses the dtsp in two consecutive steps. first, a sequence of visits to the targets is determined, e.g., by a solution of the underlying euclidean tsp without considering the vehicle motion constraint. in the second step, headings at the target locations are established by applying straight line segments for even segments followed by closing the tour with dubins maneuvers for odd segments. a similar decoupled strategy has been utilized also in the receding horizon based approach [4] with the horizont of two or three target locations ahead which significantly outperforms the original aa in terms of the solution quality. sampling-based approaches [5, 6] represent the second class of existing solutions for the dtsp. these approaches are based on sampling of possible headings into a finite discrete set and the dtsp is transformed into the generalized asymmetric tsp (gatsp) and further into the atsp by noon-bean transformation [7]. the resulting atsp can be then solved by existing solvers such as concorde [8] or lkh [9]. the third class of the dtsp approaches are evolutionary based algorithms [10]. they encoded solutions into individuals in the population and used similar crossover and mutation operators like for the standard tsp. although evolutionary based approaches can be computationally demanding, their main advantage is the ability to search for a global optima. in [11], authors proposed a novel memetic algorithm to improve performance of the evolutionary based approach by utilizing a local optimization method. recently, the evolutionary multi-objective algorithm nsga-ii [12] has been deployed in [13] to address path planning for data collection in a wireless sensor network that is formulated as the dtsp. the authors consider a bi-objective optimization criterion where the first objective is to minimize the tour length and the second objective is to maximize the time when the vehicle is in the vicinity of the sensor. the problem formulation [13] is similar to the herein proposed dtsp-cm in the considering an influence of the executed maneuver type at the target locations; however, the authors of [13] do not explicitly constraint the type of the maneuver and rather optimize a bi-objective function. on the other hand, the proposed dtsp-cm problem formulation explicitly restricts the collecting maneuver to be one of the specified type with the aim to improve robustness of the solution execution and the mission accomplishment. 3. problem statement the proposed formulation of the dubins traveling salesman problem with collecting maneuvers (dtspcm) is motivated by surveillance missions with fixwing aerial vehicles where the goal is not only to visit the target locations but also to execute a prescribed maneuver for each target. similarly to the dtsp, also in the dtsp-cm, the dubins vehicle [2] is constrained to move only forward at the constant speed v and has the minimum turning radius restricted to ρ. the motion of the vehicle can be described as: ẋ ẏ θ̇  = v  cos θ sin θ u ρ  , |u| ≤ 1, (1) where u is the control input. the state of the dubins vehicle q is represented as a triplet q = (x, y, θ) and q ∈ se(2), where (x, y) ∈ r2 is the vehicle position in a plane and θ ∈ s1 is the vehicle heading at (x, y). the dtsp-cm stands to determine a closed shortest curvature-constrained tour for which all targets are accomplished by executing a maneuver from a specified set of acceptable collecting maneuvers. each target i is defined by its position pi in the plane and a set of collecting maneuvers ti. the dtsp-cm is formally defined for n target locations p = (p1, . . . , pn) where pi ∈ r2, corresponding collecting maneuvers t = {t1, . . . , tn}, and the minimal turning radius of the vehicle ρ. in the dtsp-cm, the dubins vehicle is requested to accomplish all given targets by the particular collecting maneuvers joined in a single closed tour satisfying the vehicle motion constraints (1). therefore, it is necessary to determine both the collecting maneuvers m = {τi, . . . , τn}, τi ∈ ti, and the sequence of the visits to the targets σ = {σ1, . . . , σn}. notice, a set of possible collecting maneuvers ti can be infinite, e.g., as an arbitrary selection of the heading angle θ from the set θ ∈ (0, 2π〉 in the ordinary dtsp. the final closed tour consists of the particular collecting maneuvers that are connected to a closed tour by the shortest possible paths respecting the vehicle motion (1), i.e., dubins maneuvers. therefore the total tour 35 petr váňa, jan faigl acta polytechnica ctu proceedings (a) . crossing maneuver (b) . dropping maneuver figure 2. examples of straight collecting maneuvers of the dtsp-scm length l givenm and σ can be computed as: l(m,σ) = n−1∑ i=1 d(g(τσi ), f(τσi+1)) +d(g(τσn ), f(τσ1)) + n∑ i=1 l(τi), (2) where the function f(τi) represents the starting point of the maneuver τi, and g(τi) is the end point of the maneuver, d(g(τi), f(τj)) stands for the length of the dubins maneuver connecting collecting maneuvers τi and τj , and the symbol l(τi) stands for the length of the τi maneuver. the aim is to minimize the tour length in the dtsp-cm, and therefore, the problem is formulated as the optimization problem formalized in problem 3.1. based on the set of collecting maneuvers, the optimization problem can be both discrete or piecewise continuous. the problem is not always fully continuous, since the length of the dubins maneuver is also only piecewise continuous [14]. problem 3.1 (dtsp-cm). minimizem,σ l(m,σ) subject to ∀i : τi ∈ ti 3.1. dtsp-cm with straight collecting maneuvers (dtsp-scm) based on the proposed formulation of the dtsp-cm we further investigate its special variant with collecting maneuvers limited to straight line segments with a prescribed length and its relative position to the particular target location. such limited maneuvers are motivated by real scenarios where the vehicle needs to stay at its course while data from sensors are measured or a cargo is dropped to the particular target location. we call this problem the dtsp with straight collecting maneuvers and denote it as the dtsp-scm in the rest of this paper. having the possible fulfilling maneuver as a straight line segment for which the supporting line is passing the target location, the problem is to find the segment orientation for each target, i.e., we need to determine the vehicle heading at each target location as in the ordinary dtsp. the considered straight collecting maneuver can be specified by two parameters that determine its relative position to the target location: 1) the parameter α represents a distance of the maneuver starting point to the target location; 2) and the parameter β that specifies the end of the collecting maneuver from the target location. for both parameters we can consider positive or negative values according to their relative location to target location defined by the vehicle motion. thus, positive values denote the positions of the maneuver endpoints that are on the approaching side to the target locations (the vehicle is approaching the target), while the negative values denote the position of the endpoints for which the vehicle recedes the target location. the length of the maneuver l(τ) is always positive, and therefore, we define it as l(τ) = |α− β|, l(τ) > 0. (3) we consider two types of straight collecting maneuvers. the first type represents a situation where the target location lies directly on the collecting maneuver. such a maneuver is called the crossing maneuver (α > 0 and β < 0) and it is motivated by robotic scenarios to precisely measure some location and where the vehicle cannot change its heading during the sensing phase. an example of the crossing maneuver is depicted in fig. 2a. the second type of straight collecting maneuvers is a so-called dropping maneuver. in this case, the target location is at the maneuver direction, but not necessary on the maneuver itself, α > 0 and β > 0. this type of maneuver can be used for planning object dropping, since the vehicle is required to focus the target while moving on the straight line segment to ensure a precise airdrop location [15]. after the object dropping, the vehicle can continue in an arbitrary direction and does not need to achieve the target location itself. an example of the dropping maneuver is depicted in fig. 2b. formally, the dtsp-scm is a variant of the optimization problem 3.1. in contrast to the general dtsp-cm, the straight collecting maneuvers have a constant length, since the parameters α and β are fixed for the particular problem instance. therefore, the total length l(m) of all collecting maneuvers can be determined l(m) = n∑ i=1 l(τi) = n∑ i=1 |α− β| (4) and its value is constant that can be computed before solving the particular instance of the dtsp-scm. this property enables to consider only dubins maneuvers length while minimizing the tour length, which significantly simplifies possible methods addressing the dtsp-scm. furthermore, it is possible to modify approaches for the dtsp to address the proposed dtsp-smc due to the constant length of the collecting maneuver. proposed modifications for existing dtsp approaches are presented in the next section. 36 vol. 6/2016 dubins traveling salesman problem 4. solution of the dtsp-scm the main advantage of the proposed dtsp-scm over more general the dtsp-cm is that it is possible to solve the dtsp-scm in a relatively straightforward way by approaches developed for the dtsp with only slight modifications. this is possible because the length of the individual collecting maneuver is constant, and thus the sum of all collecting maneuvers (4) is a constant value and it is not needed to consider individual lengths during the optimization process. hence, we can build solvers for the dtsp-scm on the existing methods for the dtsp. the proposed modifications of the selected representative approaches for each of three classes of the dtsp approaches introduced in section 2 are presented in this section. for decoupled approaches, we can still utilize a solution of the euclidean tsp to determine the sequence of visits to the targets. however, we can expect that such a sequence can be farther from the optimum when the collecting maneuvers are getting longer. a modification of the original aa [1] to utilize collecting maneuvers is straightforward. in solving the ordinary dtsp, vehicle headings are determined for each target location. instead of that, we can determine directions of collecting maneuvers using the direction in odd segments. then, we can connect even segments by the dubins maneuvers to create a closed tour, and thus solve the dtsp-scm. the sampling-based approach [5] is another option how to address the proposed dtsp-scm. instead of sampling the vehicle heading at each target location, we need to sample a set of collecting maneuvers corresponding to each particular target location in the dtsp-scm. in [5], the authors propose to create a distance graph which is an instance of the gatsp. for the proposed dtsp variant with collecting maneuvers, the resulting instance of the gatsp has twice the number of vertices. however, the size of the gatsp instance can be reduced back to the original size by a simple transformation as follows. the length of the utilized collecting maneuver is added to the length of the dubins maneuver which together form a continuous path. similarly the evolutionary-based algorithms [10, 11] are also suitable for a straightforward extension to address the proposed dtsp-scm. here, the chromosome representing the individual needs to be modified to contain the collecting maneuver instead of the vehicle heading only. in addition, the evaluation function needs to be modified to respect the total tour length according to (2). 5. evaluation results several problem instances of the dtsp-scm have been solved to demonstrate usability of the newly proposed variant of the dtsp with straight collecting maneuvers. a small quadrotor helicopter has been simulated in the realistic gazebo simulator [16] with a physical model based on the pixhawk flight controller. figure 3. simulated quadrotor helicopter dropping red ball object. an example of graphical output from the simulator is depicted in fig. 3. the helicopter has been requested to fly at the altitude 20 m with the speed 5 m.s-1 and the minimal turning radius has been set to ρ = 7 m to imitate realistic conditions of a real aircraft. the dropping distance has been set to approximately 9.5 m and the used straight collecting maneuvers have the parameters: α = 12 m and β = 8 m. we have conducted two types of evaluation scenarios. the first scenario is designed to validate a precision of the airdrop maneuvers without and with the explicit consideration of the straight collecting maneuvers in the proposed dtsp-scm. the second scenario is designed to evaluate performance of the proposed modifications of the existing solutions for the dtsp in solving instances of the introduced dtspscm. 5.1. precision of the airdrop first, we found solutions of the ordinary dtsp and the proposed dtsp-scm using the sampling based approach with the lkh solver [17]. the evaluation instance is generated for 10 target locations (n = 10) with the relative density d = 0.3 defined as: d = ρ √ n s , (5) where s is the size of the bounding box where all target locations are positioned. we consider solution of 10 random instances with n = 10 solved by each particular approach (dtsp and dtsp-scm) to obtain statistically significant results. hence, 100 simulated intersection of the dropped object with ground have been recorded. in the used simulated environment, a limited precision of the gps and all the motors were considered except of air resistance. the obtained locations of the dropped object are visualized in fig. 4 where a direction of all dropping maneuvers is rotated to the same orientation to draw all locations within the same figure. it can be easily seen that objects dropped without explicit consideration of the straight collecting maneuvers (i.e., a solution of the ordinary dtsp) are often dropped with a longer distance error from the desired target 37 petr váňa, jan faigl acta polytechnica ctu proceedings ● ● ●● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ●● ● ● ● ● ●● ● ● ●● ● ● ● ● ●● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ●● ● −10 −5 0 5 −5 0 5 10 xerror [m] y e rr or [m ] method ● dtsp dtsp−scm airdrop target figure 4. locations of the dropped object to the target location as a result of the performing dtsp solution and a solution of the newly introduced dtspscm. all measurements are normalized by the position of the airdrop and the target location. 0.0 2.5 5.0 7.5 10.0 12.5 0255075100 percent of dataset [%] e rr or d is ta nc e [m ] solver dtsp dtsp−scm figure 5. precision of the airdrop maneuver obtained by solution of the dtsp and the newly proposed formulation of the dtsp-scm location than for the case when the trajectory is found as a solution of the dtsp-scm. the distance of the real position of the dropped object to its expect position at the target location is depicted in fig. 5. the error for the solutions of the dtsp-scm is almost half of the error for the dtsp. 5.2. performance of dtsp approaches in the dtsp-scm the proposed modifications of the existing approaches for the dtsp to address the introduced dtsp-scm have been evaluated in a series of dtsp-scm instances according to the number of target locations n and their density d determined by (5). six algorithms for the dtsp-scm has been compared. in particular, the proposed modifications of approaches: alternating algorithm (aa) [1], local iterative optimization [18], genetic algorithm [10], memetic algorithm [11], and sampling-based approach [6] with the lkh solver [17] (denoted as the sampling+lkh) and with the optimal concorde solver [8], denoted as the sampling+concorde. due to high computational requirements of the genetic, memetic, and sampling● ● ● ● ● ● ● ● ● ● ●● ● ● ● ● ● ● ● ● ● ● ● ● 0 1 2 3 10 20 50 100 number of target positions r at io o f s ol ut io n le ng th to th e re fe re nc e le ng th method ● ● ● ● ● ● aa lio genetic memetic sampling+lkh sampling+con. figure 6. average ratios of the solution length to the reference length of the best found solution depending on the number of target locations with the relative density d = 0.3 ● ● ● ● ●● ● ● ● ● ●● ● ● ● ● ● ● 0 1 2 0.2 0.3 0.4 density of target positions r at io o f s ol ut io n le ng th to th e re fe re nc e le ng th method ● ● ● ● ● ● aa lio genetic memetic sampling+lkh sampling+con. figure 7. average ratios of the solution length to the reference length of the best found solution depending on the density of n = 20 target locations based algorithms, their computational time has been limited to 1 hour. for sampling based approach, a series of solutions is found with iteratively increasing number of samples until the time limit is reached [19]. therefore, all the algorithms provide a solution, albeit more demanding approach (i.e., based on the concorde solver) for less samples than faster heuristic lkh solver, which solves more iterations within the same time limit. the considered number of target locations n has been selected from the set n ∈ {10, 20, 50, 100} and the density d has been selected from the set d ∈ {0.2, 0.3, 0.4}. for each particular scenario defined by the n and d, 20 random instances were generated. for each problem instance, the best found solution (among all solutions found by all approaches) has been selected as a reference solution that allows to aggregate the results into a single solution quality indicator as the ratio of the length of the found tour to the length of the reference solution. average ratios and standard deviations (shown as error bars) are presented in fig. 6 and fig. 7 depending on the number of target locations n and for the particular density of the target locations d, respectively. the results indicate that superior solutions 38 vol. 6/2016 dubins traveling salesman problem are found by the sampling-based approaches. the lkh heuristic approach provides better results than the concorde solver because of limited computational time, and thus solutions with finer discretizations are not computed within the dedicated time limit by the optimal concorde solver. 6. conclusion in this paper, we propose a new variant of the dtsp formulation to address specific requirements of the collecting maneuvers to accomplish visitation of each target location. the proposed variant of the dtsp is called the dubins traveling salesman problem with collecting maneuvers (dtsp-cm). further, we considered collecting maneuvers restricted to straight line segments with fixed length and its specified relative position to the target that is denoted as the dtsp with straight collecting maneuvers (dtsp-scm). for the dtsp-scm, we propose modifications of the existing approaches to the dtsp to address the prescribed constrained collecting maneuvers. the proposed modifications of the algorithms have been evaluated in several scenarios including evaluation of the proposed problem formulation to the precision of the cargo delivery in airdrop maneuvers. the presented results indicate that the proposed formulation improves the reliability of the mission accomplishment. moreover, the presented evaluation results also provide an overview of the performance of particular approaches to the dtsp in the dtsp-scm formulation, where the sampling based methods provide the best found solution among the evaluated approaches. acknowledgements the presented work has been supported by the czech science foundation (gačr) under research project no. 16-24206s. the support of grant no. sgs16/235/ohk3/3t/13 to petr váňa is also gratefully acknowledged. references [1] k. savla, e. frazzoli, f. bullo. on the point-to-point and traveling salesperson problems for dubins’ vehicle. in proceedings of the american control conference, pp. 786–791. ieee, 2005. doi:10.1109/acc.2005.1470055. 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[15] c. w. hewgley, o. yakimenko. precision guided airdrop for vertical replenishment of naval vessels. in proceedings of the 20th aiaa aerodynamic decelerator systems technology conference, pp. 4–7. 2009. doi:10.2514/6.2009-2995. [16] gazebo robot simulator. [cited 31 oct 2016]. [17] k. helsgaun. lkh solver 2.0.7. www.akira.ruc.dk/~keld/research/lkh. [cited 31 oct 2016]. [18] p. váňa, j. faigl. on the dubins traveling salesman problem with neighborhoods. international conference on intelligent robots and systems (iros) pp. 4029–4034, 2015. doi:10.1109/iros.2015.7353945. [19] p. váňa, j. faigl. on sampling based methods for the dubins traveling salesman problem with neighborhoods. acta polytechnica ctu proceedings 2(2):57–61, 2015. doi:10.14311/app.2015.1.0057. 39 http://dx.doi.org/10.1109/acc.2005.1470055 http://dx.doi.org/10.2307/2372560 http://dx.doi.org/10.1109/cdc.2007.4434503 http://dx.doi.org/10.1109/cdc.2006.376928 http://dx.doi.org/10.1109/acc.2011.5991501 http://dx.doi.org/10.2514/1.48949 http://dx.doi.org/10.1287/opre.39.4.623 http://dx.doi.org/10.1016/s0377-2217(99)00284-2 http://dx.doi.org/10.1109/isie.2012.6237270 http://dx.doi.org/10.1016/j.cja.2014.04.024 http://dx.doi.org/10.1109/4235.996017 http://dx.doi.org/10.1016/j.cor.2016.07.004 http://dx.doi.org/10.1137/100816079 http://dx.doi.org/10.2514/6.2009-2995 www.akira.ruc.dk/~keld/research/lkh http://dx.doi.org/10.1109/iros.2015.7353945 http://dx.doi.org/10.14311/app.2015.1.0057 acta polytechnica ctu proceedings 6:34–39, 2016 1 introduction 2 related work 3 problem statement 3.1 dtsp-cm with straight collecting maneuvers (dtsp-scm) 4 solution of the dtsp-scm 5 evaluation results 5.1 precision of the airdrop 5.2 performance of dtsp approaches in the dtsp-scm 6 conclusion acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.12.0074 acta polytechnica ctu proceedings 12:74–78, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app correlation analysis of vehicle frontal impact parameters josef mík∗, jana kadlecová department of vehicle technology, čvut v praze, konviktská 20, 12000 prague ∗ corresponding author: mikjosef@fd.cvut.cz abstract. the article considers a possible improvement of road vehicle safety by using ecall – a system which initiates an emergency call in case of traffic accident. a possible way of better description of a frontal impact accident of a vehicle is examined and enriched by the information from the onboard e-call unit. in this article, we analyze results of frontal crash tests with different types of barriers and overlapping area and look for the correlation between the individual vehicle and collision parameters in order to provide a better description of the severity of the accident by the ecall system. the relation among the selected parameters is described using the correlation analysis. keywords: crash test, ecall, cotrrelation. 1. introduction in a long-term timeframe, there is a noticeable decrease in the amount of road accidents, casualties and fatal victims of road accidents in europe. it is mostly achieved thanks to newly accepted legislation measures increasing road safety and minimizing consequences of road accidents. one of these measures is a mandatory installation of the ecall system – an emergency call system in case of a road accident. the system is to be launched and installed on all newly produced vehicles in april 2018 [1]. based on the information obtained from passive safety systems installed in the vehicle and additional ecall system sensors, the ecall system automatically detects a road accident and consequently sends a minimum set of data (msd) message to the emergency service and at the same time establishes a voice communication with 112 service. the operator of the emergency service decides on the measures and safety services dispatched to the accident site based on the information obtained in the msd message and from oral communication with passengers of the crashed vehicle. the basic structure of the msd message contains the following information about the vehicle and the accident: • version of msd format; • identification of msd; • ecall activation type; • vin code for vehicle (iso 3779)[2]; • fuel type; • vehicle direction; • recent vehicle location n1, n2; • number of passengers (locked safety belts). a set of additional information, which can be used for more accurate description of consequences of accident, is described in this article. this was concluded based on results of series of crash tests. 2. experiment description a background for the analysis is data obtained from a series of front impact collision of vehicles category m1. results of these crash tests are shown in table 1. calculated resulting injury criteria coefficient hic and 3 ms head criteria are represented in table 2. as it can be seen from table 1 and 2, the constellations of test vehicles contain vehicles equipped with different types of passive safety systems. activation of the frontal airbag was a monitored parameter. as for the collision partner, a solid barrier with a 100 the following parameters were selected for correlation analysis: • overlapping of the frontal area – indicates overlapping of the frontal area of the test vehicle with the collision partner in percent; • collision velocity (v0) – calculated based on the video of the collision from high-speed cameras; • the weight of the vehicle – calculated based on measurements performed on separate wheels with plate weights; • kinetic energy of the vehicle(ek) – is calculated based on the vehicle weight, and collision velocity (equation 1) ek = 1 2 ∗m ∗ v 2, (1) where: ek – kinetic energy of the vehicle right before the collision [j], m – weight of the vehicle [kg], v – collision velocity [m*s−2]; • maximal acceleration of the vehicle body – estimated from the acceleration of the vehicle body during the collision in x direction; 74 http://dx.doi.org/10.14311/app.2017.12.0074 http://ojs.cvut.cz/ojs/index.php/app vol. 12/2017 correlation analysis of vehicle frontal impact parameters test vehicle collision vehicle characteristics partner overlap [%] front airbag v0 [km*h−1] m [kg] ek [kj] amax [m*s−2] deformation [mm] škoda fabia rigid barrier 100 yes 50,77 1208 120,13 620 447 škoda favorit rigid barrier 100 no 47,3 875 75,53 459,8 508 škoda rapid rigid barrier 100 yes 45 1235 96,48 378,1 416 škoda rapid rigid barrier 100 no 14,92 1122 9,64 115,6 127 renault 5 gtd rigid barrier 40 no 52,2 938,6 98,67 345 700 škoda roomster deform. barrier 40 yes 56,18 1542 187,76 no no škoda fabia škoda octavia 33 yes 50 1157 111,59 176 815 table 1. results of crash tests – characteristic of test vehicles. test vehicle collision partner driver manikin other manikin amax [m*s−2] hic [-] location in the vehicle amax [m*s−2] hic [-] škoda fabia solid barrier 510 302,94 passenger 2277 4139 škoda favorit solid barrier 2490 2205,6 child p3 708,8 706 škoda rapid solid barrier 460 180,42 ne ne no škoda rapid solid barrier no ne ne ne no renault 5 gtd solid barrier no no child p3 856,6 612 škoda roomster deform. barrier no 359,25 passenger ne 358,64 škoda fabia škoda octavia no no no no no table 2. results of crash tests – hic criteria of test manikins. • resulting deformation of the vehicle (ξ) – estimated from visual documentation of the test vehicle after the accident (photos and video from the high-speed cameras), based on comparison with photo documentation of the test vehicle before the collision; • maximal acceleration of the manikin driver’s head (amax) – estimated from the acceleration acting on the driver manikin’s head during the impact. the resulting acceleration curve was calculated from the accelerations of the manikin head in x, y and z axis based on the equation 2. the overall progress of result acceleration was then filtered with standard frequency filter cfc1000. acelk = √ a2 x + a2 y + a2 z, (2) where: acelk – resulting acceleration [m*s−2], ax, ay, az – acceleration of the manikin head measured in x, y, z [m*s−2]; • hic criteria value for the driver manikin – head injury criteria was calculated from the result acceleration curve based on the equation 3. in case there was no contact of the manikin head with the vehicle interior the time interval of 36 ms was selected for time t1 to t2 (estimated from the speed camera recordings), in casethere was a collision, a 15 ms time interval t1 to t2 was selected. hic criteria value is then the maximum value in the selected interval for the result acceleration hic = [ 1 t1 − t2 ∗ ∫ t2 t1 adt ]2,5 ∗ (t1 − t2), (3) where: hic – value of head injury criteria [-], a – result acceleration [g], t1 – start of the time interval for hic calculation, t2 – end of the time interval for hic calculation. results of crash tests are summarized in tables 1 and 2. 3. correlation analysis of crash test results analysis of the crash tests results was made based on correlation analysis between selected parameters presented in table 1 and 2, considering if it is suitable to use them for estimation of the severity of the accident by ecall system. the relationship between parameters is expressed by a regression function using the least squares method (equation 4) 75 josef mík, jana kadlecová acta polytechnica ctu proceedings yi − ŷi yi − ayx + byx ∗ xi ... yi − ŷi · yi − ayx − byx ∗ xi ... f ( ayx, byx ) = 1 n ∑n i=1 (4) where: ŷi – aligned value (theoretical), yi – emperical values, ayx, byx – equation coefficients. the reliability of regression estimation was determined by the correlation coefficient ryx. correlation dependency is considered to be poor tight if the value of correlation coefficient is lower than 0.3. in case the value is higher than 0.8, then correlation dependency is considered to be very tight. if the value lies in the interval from 0.3 to 0.8 the correlation dependency is considered to be mild tight. 4. dependency of the vehicle body deformation from collision velocity the dependency of the deformation of the vehicle from collision velocity is represented in figure 1. from all the crash tests, only collisions with a rigid barrier with 100% overlapped were used for correlation analysis. these values are shown in the figure as blue dots with a line regression function. it is possible to calculate correlation coefficient from the coefficient of determination r2 as it is shown in the equation 5. r = √ r2 = √ 0, 9433 = 0, 9712 (5) the resulting value of the regression coefficient is r = 0.9712 so we can consider correlation dependency as very tight. but a small amount of input data has to be considered. in figure 1 there are also shown other values which were not used for the regression analysis because of a different type of collision parameters. these are the data obtained from crash tests with the vehicle renault 5 gdi, which was collided with a rigid barrier with 40% overlap, and a skoda fabia sedan, which was collided with another vehicle skoda octavia with 33% overlap. it is visible from figure 1 that the value of the resulting deformation is increasing with decreasing overlap of the collision area. 5. the dependency of maximum acceleration on the kinetic energy of the vehicle the next parameter that we consider in this research is the dependency between the value of maximum acceleration, which impacts the vehicle body during a crash, and the value of the vehicle’s kinetic energy, which is transformed into the vehicle’s body deformation during the collision. the values for individual vehicles are incorporated in the graph in figure 2. as in the case of the dependency between vehicle body deformation and collision velocity, the regressive function describes only vehicles that suffered a frontal collision with a rigid barrier with 100% overlap. the values that are applicable to personal vehicles can also be found in the graph. to describe the dependency, an exponential regression function was chosen as it has a higher value for correlation coefficient than a linear function. the graph describing the equation of the regression function can be found in figure 2, as well as the determination coefficient r2. equation 6 establishes the value of the correlation coefficient through a determination coefficient. r = √ r2 = √ 0, 9103 = 0, 954 (6) according to the resulting value of the correlation coefficient r = 0,954 it is possible to see the correlation dependency as very high. however, it is necessary to take into consideration the small number of input values on the basis of which the function was solved. the graph in figure 2 also contains the values of acceleration for the renault 5 gtd (40% overlap) and the škoda fabia sedan (33% overlap) with the lesser percentage of overlap. the graph demonstrates that the maximum acceleration influencing these vehicles with an equal value of the consumed kinetic energy in the case of vehicles with a 100% overlap is smaller. in the case of the škoda fabia sedan, however, part of the kinetic energy was given to another vehicle, škoda octavia, that was moved by 9,28 meters from its original position before the crash, as well as accelerated. for this reason, the tested vehicle was slowed down, which does not happen in case of frontal collision with a rigid barrier. this parameter, therefore, should not be considered. 6. the dependencies of the hic criteria on the speed of the vehicle in this chapter, the correlation of the possibility of the driver’s head injury and the speed of the vehicle is considered in order to study the severity of injuries passengers of the car can suffer during a traffic accident. as it is clear from the results of the car collision that an airbag can have a serious impact on the resulting value of the hic criteria, the correlation assumes that the airbag was used. the graph in figure 3 presents values which also include the values established for the passenger mannequin. the linear regression function presented in the graph is applicable to a restraint system of a vehicle that has an airbag. the quantity of the correlation coefficient is calculated by equation 7. r = √ r2 = √ 0, 9024 = 0, 9499 (7) 76 vol. 12/2017 correlation analysis of vehicle frontal impact parameters figure 1. dependency of the deformation of the vehicle from collision velocity. figure 2. dependency of the deformation of the vehicle from collision velocity. 77 josef mík, jana kadlecová acta polytechnica ctu proceedings figure 3. dependency of the deformation of the vehicle from collision velocity. according to the resulting value of the correlation coefficient r = 0,9499 it is possible to see the correlation dependency as very high. however, it is necessary to take into consideration the small number of input values on the basis of which the function was solved. to establish the regression function we have used only 3 input hic values. in the case where we need to describe the seriousness of the injuries suffered by the passengers in a traffic accident, it is better to use the ais method instead of the resulting value of the criterion of the injuries. the ais method describes the seriousness of the injuries suffered by individual parts of the human body using a number in the 0 – 6 interval. this possibility is considered in the research described by [3] in the bibliography. 7. conclusion the problem of the estimation of the consequences arising from a vehicle collision was solved on the basis of establishing a dependency between the chosen vehicle parameters. in the chosen pairs of the parameters one quantity was possible to measure with ecall while another quantity was to be estimated. the dependency between the chosen parameters was described with a regression function and its accuracy was verified on the basis of the value of the correlation coefficient. in all three cases the accuracy of the quantity’s dependence of the correlation coefficient rxy was verified. in all three cases, this coefficient came out to be higher than 0,8 and therefore we can establish the dependency between the chosen quantities to be very high. however, in considering the outcome we also have to bear in mind the low number of quantities on the basis of which the correlation analysis was carried out. this fact considerably undermines the reliability of the results. to strengthen the reliability of the results it is necessary to carry out a correlation on the basis of a higher number of crash tests with different impact velocities. another way to acquire data for statistical analysis is to create a fem or multi-body model and to carry out a simulation of collision impact with simulation software. this would also allow for the repetition of the scenario with the same model and an easy change in input parameters. references [1] e. 2015/758. požadavky na schválení typu pro zavedení palubního systému ecall využívajícího linku tísňového volání 112. [2] i. 3779:2009. road vehicles – vehicle identification number (vin) – content and structure. [3] h. kovandová, h. krejčí, j. kovanda. crash tests of vehicles – selected experiments and analysis. in: transactions on transport sciences, vol. 6, no. 4/2013, issn: 1802-9876, pg. 193-202. 78 acta polytechnica ctu proceedings 12:74–78, 2017 1 introduction 2 experiment description 3 correlation analysis of crash test results 4 dependency of the vehicle body deformation from collision velocity 5 the dependency of maximum acceleration on the kinetic energy of the vehicle 6 the dependencies of the hic criteria on the speed of the vehicle 7 conclusion references 192 acta polytechnica ctu proceedings 2(1): 192–196, 2015 192 doi: 10.14311/app.2015.02.0192 the role of magnetic field for quiescence-outburst models in cvs s. de bianchi1,2, v. f. braga3, s. gaudenzi1 1dept. of physics, università degli studi di roma ”la sapienza”, piazzale a. moro 5, 00185 rome, italy 2école normale supérieure, cnrs-umr 8547, rue d’ulm 45, 75005 paris, france 3dept. of physics, università tor vergata, via della ricerca scientifica 1, 00133 rome, italy corresponding author: silvia.debianchi@uniroma1.it abstract in this paper we present the elementary assumptions of our research on the role of the magnetic field in modelling the quiescence-outbursts cycle in cataclysmic variables (cvs). the behaviour of the magnetic field is crucial not only to integrate the disk instability model (osaki 1974), but also to determine the cause and effect nexus among parameters affecting the behavior of complex systems. on the ground of our interpretation of the results emerging from the literature, we suggest that in models describing dne outbursts, such as the disk instability model, the secondary instability model (bath 1973) and the thermonuclear runaway model (mitrofanov 1978), the role of the magnetic field is at least twofold. on the one hand, it activates a specific dynamic pathway for the accreting matter by channelling it. on the other hand, it could be indirectly responsible for switching a particular outburst modality. in order to represent these two roles of the magnetic field, we need to integrate the disk instability model by looking at the global behaviour of the system under analysis. stochastic resonance in dynamo models, we believe, is a suitable candidate for accomplishing this task. we shall present the mhd model including this mechanism elsewhere. keywords: cataclysmic variables dwarf novae intermediate polars magnetic field disk instability model secondary instability model thermonuclear runaway model. 1 introduction in the last decades, methods and models used to describe dne outburst cycles achieved several results (bath & van paradijs 1983, cannizzo & mattei 1998, cannizzo 2012). however, there is no unique model that predicts these cycles (smith 2007), as well as their underlying mechanism. the limit-cycle model for dwarf nova outbursts is generally accepted, but there are still uncertainties about how to explain all the details, especially for the su uma stars (smith 2007). even if we know that the secondary stars in dne are magnetically active, yet it is unknown how they maintain a dynamo in the presence of tidal forces or whether there is differential rotation (smith 2007). crawford et al. (2008), for instance, when presenting their results of the detection of the first observed outburst of dw cnc, asked the question of what caused the outburst observed. dw cnc experienced a magnitude change of ∼4 mag showing a behavior similar to those systems whose outbursts are due to disk instability. however, with respect to pspin and porb, dw cnc shares characteristics of those systems whose outbursts are due to a mass transfer event. therefore, a decision for which mechanism was responsible for the first detected outburst could not be made. precisely in order to overcome this kind of problems of undecidability a deeper analysis of our models’ ability to explain dne outbursts is needed. 2 disk instability model and secondary instability model: some open questions each of our best available models, such as the disk instability model (dim), the secondary instability model (sim) and thermonuclear runaway (tnr) model, taken separately, shows weaknesses in predicting the outburst-quiescence cycles of many systems, such as v513 cas for outbursts during standstills (hameury & lasota 2014). dim is generally accepted as reproducing an explanation of dne outbursts and invokes an intrinsic modulation of the accretion rate in the disk. however, as seen in the case of dw cnc, the model does not satisfactorily account for all systems and suffers of some structural problems. the first one has been inherited by the disk model of shakura & sunyaev (1973) which was based on a constant value of α, a parameter that stores all unknown information of the complex friction processes. a constant α does not account for a reliable outburst amplitude (smak, 1984) and the pa192 http://dx.doi.org/10.14311/app.2015.02.0192 the role of magnetic field for quiescence-outburst models in cvs rameter appeared to be an ad hoc solution for strictly regular outbursts (bath 2004). studies concerning its variation or a turbulent α parameter aimed to the appropriate simulation of the disk instability by applying suitable corrections (latter & papaloizou 2012; penna et al. 2013; potter & balbus 2014). a second problem consists in the fact that dim does not appropriately model the observed fluctuations, due to the assumption of a constant value for mass transfer rate ṁ. third, dim shows weaknesses in predicting global changes in the disk structure, such as whether thin disk accretion can make a transition to advection-dominated flow (narayan & yi 1994, 1995a, 1995b) or how an accretion disk creates and powers jets at its center (king 2012). as an alternative to dim, sim assumes a mechanism triggering the outbursts based on mass transfer modulation from the secondary star (bath et al. 1974). by combining dynamical instabilities of the secondary, time evolution of the accretion disk together with thermonuclear burning due to accreted material, sim produces reliable results: outbursts during standstills in z cam systems can be explained only by appealing to instabilities in the flow from the secondary (hameury & lasota 2014). it seems then that the sim is decisive in predicting cvs like z cam variables and, possibly, su uma variables. nevertheless, its application has not been always straightforward. osaki (1985), for instance, explained the superoutbursts of su uma variables by using sim, but later denied this possibility in favor of a thermal-tidal-instability (tti) model (osaki 1989). finally, smak (1996) suggested a hybrid ttisim model, which is still debated today (osaki & kato 2013). 3 magnetic field and outburst modality in order to enrich the theoretical scenarios in dealing with dne outburst-quiescence cycle, the (tnr) model shows interesting implications, even if the improvement of the tnr model launched by shara (1982) never brought to a decisive point. tnr introduces a time parameter describing the recurrence of outbursts accounting for both classical novae (cne) and dne outbursts and their differences (shara 1982) and also accounts for dnos and x-ray flux variations concerning some representative systems like u gem, ss cyg, ex hya, z cam, cy cnc, ah her, cn ori, kt per. more importantly, tnr can be associated to one of the processes that causes nitrogen to carbon enhancement observed on the surface of the wd in vw hyi and u gem (sion 2014). in tnr models, outbursts are the product of thermonuclear burning onto the wd surface (mitrofanov 1978; 1980). in the presence of a magnetic field of the order of 3 · 106 − 3 · 107 g on the surface of the degenerate component, a local accumulation of hydrogen could generate, through thermal instability, a thermonuclear burning responsible of the outburst. for this process to occur, an intense magnetic field 106−108 g is required; primaries with such fields do exist in intermediate polars (ips) and polars that owe their properties to the very primary magnetic field (patterson 1994). therefore, the magnetic field strength on the wd surface allows us to distinguish novae, dwarf novae and novalike stars. in exploring models that go beyond the use of tnr alone, livio (1983) emphasized the importance of the magnetic fields in cvs (livio & verbunt 1988; meyer-hofmeister et al. 1996). as livio (1983) shows, nova explosions can be inhibited if the magnetic field strength is over a certain limit, explaining in this way why active novae are absent among polars while novae can be found among the ips. figure 1: upper limits on the magnetic field strength for which nova outbursts can occur (provided that matter is confined to polar caps) as a function of the accretion rate, for various white dwarf masses. reproduced from livio, m., 1983, astronomy and astrophysics, 121, l7, with permission from astronomy and astrophysics, c©eso. livio’s approach allows one to determine upper limits on the magnetic field strength for which nova outbursts can occur when polar caps are present. these upper limits can be represented as a function of the accretion rate and for different wd masses (see figure 1). even if a magnetic field more intense than a certain critical value could inhibit nova explosions (livio 1983), a magnetic field is strictly correlated, on an intensity-dependent scale, to different modes of accretion and thermonuclear runaways. these modes in193 s. de bianchi, v. f. braga, s. gaudenzi clude the channeling of the accreted matter into magnetic polar caps, the alteration of radiative and conductive opacities, interference with the development of convection that likely is also present in non magnetic cvs. furthermore, the magnetic field of the wd itself may affect the nova outbursts, e.g. by enhancing mass loss in the equatorial plane (livio et al. 1988; prialnik & livio 1995). this reveals how the magnetic field activates different and specific dynamic pathways. in other words, to focus on the role of a variable magnetic field and its effects can be helpful for identifying common features of both magnetic and non-magnetic cvs, as well as for obtaining crucial information on the magnetic field responsible for switching a particular outburst modality. indeed, according to livio (1983), the pressure at the base of the accreted matter is the physical parameter that determines the outcomes of a tnr: pb = gmwd r2 wd ∆macc acap (1) when pb exceeds a critical value of some 1019dyne/cm2, ignition occurs. it should be noted that, for higher cno abundances, the critical pressure for the occurrence of an outburst is lower. this fact leads us to the investigation of cno abundances and of the presence of material accumulating during quiescence, in order to speculate on the triggering of an outburst. it means that a function of “prediction” and not of mere “description” can be added to the model. figure 2: e(b-v) varies with both the orbital phase and the percentile quiescence time (t%). 2175 å absorption bump is believed to be caused by c60. e(b-v) takes the highest value at the “heart” of the quiescence. c60 molecules could be reasonably supposed to be affecting the modulation of time elapsing between the outbursts. reproduced from gaudenzi et al. (2011), astronomy and astrophysics 525, a147 with permission from astronomy and astrophysics, c©eso. more importantly, the analysis of uv spectra revealed the presence of fullerenes as an intrinsic source of reddening in ss cyg (gaudenzi et al. 2011, see figure 2). density gradients in the disk may influence the accumulation of molecules in specific sites of the disk itself where they are accreted and/or ejected during the quiescence-outburst cycle. along with accretion/ejection mechanisms, a major role in determining the structure and the stability of the disk might be played by the solid-gaseous phase transitions of fullerenes (gaudenzi et al. 2012) at 5855 k (hussien et al. 2008). on the ground of the hypothesis that the quiescence-outburst phase transition is the effect of a stochastic resonance mechanism, the presence of material accumulated in the disk could trigger wave amplification within the disk even during quiescence. this would introduce in our modelling of the disk instability an amplification of stochastic resonance induced by turbulent fluctuations (benzi & pinton 2011). 4 magnetic field and accretion behaviour seminal numerical studies of the influences of a magnetic field on the flow structure were performed in the early 1990s either in the frame of simplified models (king 1993; wynn & king 1995; wynn et al. 1997; king & wynn 1999; norton et al. 2004; ikhsanov et al. 2004; norton et al. 2008) or in a limited region of the stellar magnetosphere (koldoba et al. 2002; romanova et al. 2003, 2004). in the last few years, there have been attempts to develop a comprehensive 3d numerical model to calculate the flow structure in close binaries (zhilkin & bisikalo 2009, 2010; bisikalo & zhilkin 2012). according to our interpretation of the results of 3d mhd simulation of bisikalo & zhilkin (2012), it emerges that the value of the magnetic induction on the surface of the accreting star activates the dynamic pathway and, in doing so, distinguishes two different modalities of accretion. in the numerical model, bisikalo & zhilkin (2012) take into account radiative heating and cooling,as wells as diffusion of the magnetic field due to dissipation of currents in turbulent vortexes, magnetic buoyancy, and wave mhd turbulence. the interesting result consists in that if the magnetic field induction grows, the cross-section of the stream decreases and the accretion rate decreases as well, thereby influencing density and pressure, and thus affecting the possibility of triggering an outburst. we interpret the nonmonotonic variation of the magnetic field behaviour and its consequences reported in (bisikalo & zhilkin 2012) as stochastic oscillations of b. in particular, magnetic field values around 106g could originate phase transitions between polar and ip. based on our previous work (gaudenzi et al. 2012), we suggest that the dynamic pathway of accretion can account for instabilities of many cvs and discloses the possibility of acquiring an ability to predict their behaviour as transition ob194 the role of magnetic field for quiescence-outburst models in cvs jects. the physics behind this process concerns the amplification of stochastic resonance induced by turbulent fluctuations, i.e. the amplitude of the external periodic perturbation needed for stochastic resonance to occur is much smaller than the one estimated by the equilibrium probability distribution of the unperturbed system (benzi & pinton 2011). 5 discussion and conclusion in order to enrich the theoretical scenario we stressed the relevance of the accretion process that may change the surface magnetic field of an accreting wd significantly (cumming 2002), and, in agreement with (livio 1983), that the magnetic field of the wd itself may affect the nova outburst. we also remarked that the accumulation of some type of molecules, such as c60 molecules within the disk is important to understand the behavior of dne in quiescence and that the cno abundances also depend on the presence of a magnetic field (even of a weak one). if we want to predict the behavior of a complex system, such as dne outbursts cycles, neither dim nor any other model taken alone is sufficient. in fact, dim explains why thermal instability leads to outbursts, but it does not provide exact information at the level of the global system in the quiescent phase, e.g. whether there are transition from a state to another, and how to determine time-dependent α variations. in order to obtain more information about the dne outburst-quiescence cycle, we shall work on a model that is able to predict future states of these systems, as well as to describe the present state, without appealing to ad hoc assumptions. as previously stated, local, small-scale turbulences, may likely represent the physical outcome of stochastic oscillations of the magnetic field. among the other mechanisms, such as a strong differential rotation and vertical density gradients (pudritz 1981b), turbulences can be responsible for the generation of a large-scale magnetic field (pudritz 1981a). therefore, the development of mean field dynamo theory is crucial in order to overcome some difficulties related to current models in accounting for the role of the magnetic field generated in a turbulent medium. this theory, if appropriately modified, could allow us to calculate the overall structure of the global field without any detailed knowledge of the small-scale turbulence. even if this echoes earlier works by shakura & sunyaev (1973) there is a characteristic of the mean field dynamo theory that makes it different from earlier theories. it builds up a large-scale magnetic field trying to achieve a global redistribution of the angular momentum, whereas other models assume a smallscale field and a local viscosity. therefore, in order to gain knowledge on the underlying mechanism producing outbursts, such as the one presented in dw cnc, we will 1) simulate the interaction among thermonuclear runaway and magnetic field leading to a specific modification of the α viscosity parameter to be integrated in the model (switching the outburst modality); 2) model dynamic pathways of accretion due to the magnetic field behaviour by means of a mhd model that takes into account stochastic resonance in a mean field dynamo model. we shall present and discuss this simulation elsewhere, but we presented here the theoretical assumptions that inspired our study. references [1] bath, g.t.: 1973, nphs, 246, 84. 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[54] zhilkin, a.g., bisikalo, d.v.: 2010, adspr, 45, 2420. 196 http://dx.doi.org/10.1093/mnras/sts185 http://dx.doi.org/10.1093/mnras/stu519 http://dx.doi.org/10.1086/377514 http://dx.doi.org/10.1086/421867 http://dx.doi.org/10.1086/160376 http://dx.doi.org/10.1086/131295 http://dx.doi.org/10.1080/00107510601181175 http://dx.doi.org/10.1093/mnras/286.2.436 introduction disk instability model and secondary instability model: some open questions magnetic field and outburst modality magnetic field and accretion behaviour discussion and conclusion 303 acta polytechnica ctu proceedings 2(1): 303–307, 2015 303 doi: 10.14311/app.2015.02.0303 gloria and study of cataclysmic variables r. hudec1,2, v. šimon1,2 1astronomical institute, academy of sciences of the czech republic, cz-25165 ondřejov, czech republic 2czech technical university in prague, faculty of electrical engineering, prague, czech republic corresponding author: rene.hudec@asu.cas.cz abstract we report here on the ongoing eu fp7 project gloria (global robotic-telescopes intelligent array) with emphasis on possibility of investigation of cataclysmic variables by users. gloria will enable the first free and open-access network of robotic telescopes in the world. we show several examples of the not often used topics (but suitable for gloria) for the studies of activity of cataclysmic variables, e.g. search for outbursts in intermediate polars and the fluctuations of brightness in their quiescence, and investigation of the optical counterparts of supersoft x-ray sources. keywords: catalysmic variables: optical photometry spectroscopy: low-dispersion spectra data mining robotic telescopes project eu fp7 gloria. 1 introduction the research in astronomy poses two main challenges, namely 1) the immensity of the sky and 2) the huge amount of astronomical data being gathered. in fact, astronomers are nowadays facing great difficulty in finding the resources to analyze the increasing flood that modern astronomy instruments generate,insufficient computing power, insufficiently powerful software tools, and not enough hours in the day. the sky comprises 40 000 square degrees (144 million square minutes). the future professional projects (like lsst) intend to observe a very significant fraction of it on a regular basis. in order to meet the abovementioned challenges, an increasing number of astronomical projects have begun to try to foster citizen participation to help analyze data by using collaborative internet application (the so-called web 2.0). gloria stands for “global robotic-telescopes intelligent array”. gloria will be the first free and open-access network of robotic telescopes in the world. it represents a web 2.0 environment where users can do research in astronomy by observing with robotic telescopes, and/or by analyzing data that other users have acquired with gloria, or from other free access databases like the european virtual observatory (http://www.euro-vo.org). the gloria project (http://gloria-project.eu) represents the first attempt to create a network of about 20 robotic telescopes for public access, education, science and much much more. the gloria network has 17 network telescopes now. few others are expected to join us soon. many internet communities have already formed to speed-up scientific research, to collaborate in documenting something, or for social projects. research in astronomy can benefit from attracting many eyes to the sky – to detect something in the sky requires looking at the right place at the right time. our robotic telescopes can search the sky, but the vast quantities of data they produce are far greater than astronomers have time to analyze. gloria will provide a way of putting thousands eyes and minds on an astronomy problem. gloria is intended to be a web 2.0 structure, with the possibility of doing real experiments. the community will not only generate content, as in most web 2.0, but it will control telescopes around the world, both directly and via scheduled observations. the community will take decisions for the network and it will give “intelligence” to gloria, while the drudge work (such as drawing up telescope schedules that satisfy various constraints) will be done by algorithms that will be developed for the purpose. gloria project will define free standards, protocols and methodology for the following purposes: controlling robotic telescopes and all related instrumentation (i.e. cameras, filter-wheels, domes...); giving web access to the network: access to an arbitrary number of robotic telescopes via a web portal; conducting online experiments (it will be possible to design specific web environments for controlling telescopes for research on a specific scientific issue; conducting off-line experiments (it will be possible to design specific web environments for analyzing astronomical meta-data produced by gloria or other databases). 303 http://dx.doi.org/10.14311/app.2015.02.0303 r. hudec, v. šimon the main part of gloria is represented by providing access to robotic telescopes, online experiments (observations), offline experiments (research on acquired images), live broadcasting, social network + community, and support. 2 objectives and benefits of gloria project the world-wide network of robotic telescopes (gloria) does not intend to compete with lsst, but our underlying idea is that “the more eyes we put on the sky, the more and greater the scientific discoveries will be achieved”. thus, in order to try to improve the way we are doing astronomy research, this project aims to build the first open access world wide network of robotic telescopes to serve citizens from around the world for free, but competing for observing time. hence gloria is indeed an “intelligent array” and it bases its intelligence in its community of users (sanchez moreno et al. 2013). like most web 2.0 projects, gloria implements a reputation-based scoring system to reward user contributions, driven by parameters such as the quality of the gathered and processed images, number of hours invested in the observations etc., as well as the votes granted by the rest of the community that finally evaluate the quality of the work done. at the end of month 24 (october 2013) the consortium produced a standard for adding new telescopes and experiments to this network. unlike other private, profitable ongoing initiatives, the gloria network will provide a free, twofold service to the community: 1. giving citizens (including professional and amateur astronomers) free access to a network of 17 robotic telescopes spread into 4 continents and both hemispheres. in the case of professional astronomers, preferences will be given to those of developing countries who will lack astronomical facilities in their own nations. 2. giving citizens an easy web access to all the data collected by the robotic telescopes. beside giving service to research, in order to manage gloria main objective of fostering astronomical research, by allowing near continuous observations of a given target thanks to its world-wide network facilities, the following additional tangible outcomes will be pursued: 1. gloria will enable more telescopes to join, producing methodology, standards, software, and documentation oriented to teach professional and amateurs astronomers to robotize their telescopes and to integrate them into the gloria network. 2. gloria will enable more research goals to be pursued, producing methodology, standards, software, and documentation oriented to teach amateurs and professional astronomers to design new web experiments and to integrate them into the gloria network. 3. gloria will encourage participation in order to increase in number its community of citizen scientists. newcomers are very welcomed. 4. gloria will give free access to knowledge to everybody. all knowledge (software, manual, standards, documents, astronomical images, data, etc) produced by the gloria consortium and by the community will have copyleft licenses. 5. gloria intends to continue in the future. since the maintenance of the distributed telescopes is paid by their owners, the cost of the core part is very cheap. the consortium believes that an economic model based in public and private subventions and donations is very possible for a project like this to go on beyond 2014. 2.1 impact the gloria partners really believe in the enormous power of astronomy as a center of interest in scientific and human training of our young people. the children of today will be the astronomers of tomorrow. in order to enroll newcomers and awaken interest in astronomy among children, during 2012-14 we will organize the live internet broadcast of 5 astronomical events: 4 eclipses and a transit of venus, which will be made from the gloria network, with associated activities in all schools of the partners countries, with the aim of getting students and teachers participating in researchbased science education and improving their motivation to push the barriers of science education further. 2.2 the gloria consortium gloria brings together a critical mass of scientific and technological leaders with extensible expertise in tic and astronomical research, dissemination and developed of technological projects. the gloria consortium includes these institutions: upm–technical university of madrid computer science faculty–spain (project coordination); auav–astronomical institute, academy of sciences of the czech republic; csic–spanish research council–spain (scientific coordination); cvtu– czech technical university–czech republic, ip-ascr– institute of physics of the academy of sciences of the czech republic; iac–astrophysic institute of canarias–el teide observatory–spain; inaf–istituto nazionale di astrofisica–italy; sao–special astrophysical observatory–russia; ucdnuid–university college dublin–ireland; uc–university of chile– chile; uma–university of málaga–spain; uoxf– oxford university–u.k.; uniwarsaw–university of warsaw–poland. 304 gloria and study of cataclysmic variables 3 gloria and cataclysmic variables cataclysmic variables (cvs) represent important targets for gloria observations mainly because of the unique properties of their activity. the category of these systems as a whole displays a very broad range of the optical activity observable by the common ccd photometers (e.g. flickering on the timescale of minutes and the amplitude of several tenths of magnitude, the orbital modulation sometimes with the amplitude of more than a magnitude, outbursts or transitions between the high and low states on the timescales of days or weeks and the amplitudes of several magnitudes). the basic properties of the optical emission of cvs need to be taken into account for the optimal strategy of monitoring of these targets in citizen science mode. we will show some examples of activity of various types of cvs which can be the targets for the gloria observers. 3.1 distribution of cataclysmic variables the sky generally, celestial objects are not distributed uniformly in the sky mainly because of the structure of our galaxy. as shown by warner (1995), most known cvs are observed over the whole sky. the reason is that cvs represent rather low-luminosity population, hence only the nearby such objects are bright enough to be observed. this relatively isotropic distribution implies that all the observatories at any latitude, included in gloria, will have the opportunity to choose a sufficiently large amount of suitable cvs. only known classical novae concentrate toward the galactic plane and the galactic bulge. the reason for this is the high optical luminosity in their explosion, hence even the objects at the large distances from the earth are observable. the direction toward the center of the galaxy is therefore also suitable for searching for explosions of classical novae with a monitor. this favors the gloria observatories located in the southern hemisphere. 3.2 peak magnitudes of cvs the catalog of downes et al. (2001) shows that the apparent peak magnitudes of various cv types differ from each other. the reason is that there is a significantly different typical optical luminosity of each type. the explosions of classical novae dominate in the brightest part of the distribution. their peak magnitude is often near 9–10 (but some of them may be even brighter), so they are easily detectable even by small-aperture, wide-field monitors. the brightest known dwarf novae in outburst can reach about 10–12 mag but about 13 mag is more typical. cvs with strongly magnetized white dwarf (polars) (e.g. warner 1995) are rather faint systems (13–20 mag), so their observing requires the largest available telescopes. 3.3 prospects of cv investigation by gloria below we give some examples of cv types suitable for investigation within gloria project. dwarf novae with their large-amplitude (3–5 mag) outbursts with the typical recurrence time from weeks to months (e.g. warner 1995; hameury et al. 1998) are definitely very promising targets even for the modest telescopes included in gloria. we also emphasize the need of observing the outbursts of some intermediate polars (i.e. cvs with a mildly magnetized white dwarf) (e.g. warner 1995). these systems may be promising gloria targets, as illustrated by the optical activity of do dra/2a 1150+720 (fig. 1). what typical features of activity of this object can be explored by gloria telescopes? (1) rare strong outbursts with the amplitude of 4–5 mag, lasting for several days and separated by ∼800 days. these short outbursts with the decay faster than exponential and faster than predicted for non-magnetic dwarf novae are in accordance with angelini & verbunt’s (1989) model for outbursts in a disk with a large missing inner region (caused by the magnetosphere of the white dwarf). (2) strong and unpredictable fluctuations on a timescale of several days or weeks (much longer than the orbital period). figure 1: the light curve of the intermediate polar do dra with rare outbursts. the points denote the one-day means, the v symbols represent the upper limits of brightness. adapted from šimon (2000). the short outbursts or rather flares of uncertain origin may occur in various intermediate polars but since they are short, extensive monitoring is needed to detect them (van amerongen & van paradijs 1989; warner 1995). supersoft x-ray sources (van den heuvel et al. 1992) represent another example of interesting objects to be investigated by gloria experiments. since the very soft x-ray emission is easily absorbed both inside 305 r. hudec, v. šimon the source and the interstellar medium, only a small fraction of supersoft x-ray sources is observable in the x-ray spectral region. the specific spectroscopic properties of their optical emission give a hope to discover more such objects even without detecting their x-ray emission (steiner & diaz 1998). the system v sge (herbig et al. 1965) can be considered to be a member of this category (steiner & diaz 1998; greiner & van teeseling 1998). since it is relative bright (10– 13 mag(v )), it is easily observable by various robotic telescopes. v sge shows a very complicated long-term optical activity. its outbursts were observed mainly in the first half of the twentieth century (šimon & mattei (1999). however, this activity changed considerably with time. a segment of the long-term activity starting in the 1960s is displayed in fig. 2). it consists of the one-day means of brightness. the high/low state transitions occurred in some time segments. they were separated by the so-called flat segments (e.g. in the surroundings of jd 2 445 000), in which only small fluctuations of brightness remained. we can thus conclude that observing at various times captures this object in different phases of its strong activity. figure 2: long-term activity of the supersoft xray source v sge in the optical band (aavso and afoev data). notice the large variations of activity on the timescale of several years (from the segments with only small fluctuations to the segments with the large-amplitude transitions between the high and low states). adapted from šimon & mattei (1999). dividing the series of the optical (ccd and photoelectric) observations of v sge, obtained at different nights (fig. 3), into the groups according to the states of the long-term activity enables to obtain the profile of the typical orbital modulation (the orbital ephemeris of smak 1995 was used). this figure shows the intensity transfered from magnitudes. although the profile of the orbital modulation can be resolved in the individual night series, the orbital period of 12.34 hours (smak 1995) does not enable to observe the whole period from a given observing site, so a multisite campaign is desirable, especially because the orbital modulation and the long-term variations of brightness are superimposed. this means that observations obtained by gloria may provide valuable information. when the intensity of a given nigh series belonging to a given such group is shifted to match a template, it is possible to obtain the mean profile of the orbital modulation characteristic for the group (fig. 3). figure 3: photoelectric and ccd observations of v sge in the intensity scale, folded with the orbital phase (the orbital ephemeris of smak 1995). the sorting into three groups is marked. adapted from šimon et al. (2002). the cv in pegasus (found in eruption in may 8, 2010) can serve as an excellent example of a bright object which can be easily detected by amateurs and small cameras and/or telescopes. this object represented a rare type of dwarf nova with very long recurrence time (67 years) but with very large amplitudes (hudec 2010). we note that the second flare of this cv in 1942 was found using astronomical photographic archives which are perfectly suitable for this kind of work, i.e. searches for past historical flare events (hudec 1999 and 2007, hudec et al. 2012). only very few such objects are known because they can easily escape detection. in this regard, we also note that the sky contains many yet unknown transients of various kinds. they are identified and attract attention only when they show themselves in their outbursts. the follow-up observations then can lead to the study of their type. one such object detected by a very small telescope is the lǐska flare star. it is an example of the astronomical discovery of a very rare event with a small amateur telescope (lǐska et al. 2014). we suggest that this object is a new flare dme star of uv ceti type based on its color, x-ray emission, and the properties of the optical light curve of the flare, identical with the x-ray sources rx j1118.3+1347 and 2e 1115.8+1403.in simbad, these 2 sources are given as different sources but this is probably wrong and it is only one source. the object may be similar to the exosat x-ray source exo 020528+1454.8 = g 035–027 with a dme flare star counterpart detected by hudec et al. (1988). 306 gloria and study of cataclysmic variables figure 4: photoelectric and ccd observations of v sge from fig. 3, now sorted into three groups according to their mean intensity (the orbital ephemeris of smak 1995). the individual curves of each group were shifted in intensity to match the template. the scale of the ordinate is identical for all three plots. adapted from šimon et al. (2002). the observations and research of cvs are expected to be supervised by gloria scientists. everybody can join us at http://gloria-project.eu, and this involves both citizen science and students, as well as professional astronomers. typically 20 percent of robotic telescopes (rts) observing time is expected to be used for gloria users, but some telescopes such as bart will provide up to 40 percent. acknowledgement gloria is project supported by the eu fp7 program (no. 283783). the scientific part of the study is linked to the the ga cr grant 13-39464j (optical analyses) while the long–term x–ray analyses are related to ga cr grant 113-33324s. we used the observations from the aavso international database (massachusetts, usa) and the afoev database operated in strasbourg, france. we thank the variable star observers worldwide whose observations contributed to this analysis as well. references [1] angelini, l., verbunt, f., 1989, mnras, 238, 697 doi:10.1093/mnras/238.3.697 [2] downes, r. a., et al., 2001, pasp, 113, 764 doi:10.1086/320802 [3] greiner, j., van teeseling, a., 1998, a&a, 339, l21 [4] hameury, j.-m., et al., 1998, mnras, 298, 1048 doi:10.1111/j.1365-8711.1998.01773.x [5] herbig, g. h., et al., 1965, apj, 141, 617 doi:10.1086/148149 [6] hudec, r., 2010, the astronomer’s telegram, no. 2619 [7] hudec, r., et al., 1988, astronomical institutes of czechoslovakia, bulletin (issn 0004-6248), vol. 39, no. 5, p. 296-302 [8] hudec, r., et al., 2012, acta polytechnica, ibws2011 proceedings, 1(52) [9] hudec, r., 2007, in exploring the cosmic frontier: astrophysical instruments for the 21st century. eso astrophysics symposia, isbn 978-3-540-39755-7. germany, p.79 doi:10.1007/978-3-540-39756-4 25 [10] hudec, r., 1999, an introduction to the world’s large plate archives, acta historica astronomiae, vol.6, 28 [11] lǐska, j., et al., 2014, acta polytechnica, accepted [12] sanchez moreno, f. m., et al., 2013, glorora documentation package [13] šimon, v., mattei, j. a., 1999, a&as, 139, 75 [14] šimon, v., 2000, a&a, 360, 627 [15] šimon, v., hric, l., petŕık, k., et al., 2002, a&a, 393, 921 [16] smak, j., 1995, acta astron., vol. 45, 361 [17] steiner, j. e., diaz, m. p., 1998, pasp, 110, 276 doi:10.1086/316139 [18] van amerongen, s., van paradijs, j., 1989, a&a, 219, 195 [19] van den heuvel, e. p. j., et al., 1992, a&a, 262, 97 [20] warner, b., 1995, cataclysmic variable stars, cambridge univ. press, cambridge doi:10.1017/cbo9780511586491 307 http://dx.doi.org/10.1093/mnras/238.3.697 http://dx.doi.org/10.1086/320802 http://dx.doi.org/10.1111/j.1365-8711.1998.01773.x http://dx.doi.org/10.1086/148149 http://dx.doi.org/10.1007/978-3-540-39756-4_25 http://dx.doi.org/10.1086/316139 http://dx.doi.org/10.1017/cbo9780511586491 introduction objectives and benefits of gloria project impact the gloria consortium gloria and cataclysmic variables distribution of cataclysmic variables the sky peak magnitudes of cvs prospects of cv investigation by gloria 132 acta polytechnica ctu proceedings 1(1): 132–138, 2014 132 doi: 10.14311/app.2014.01.0132 auger highlights antonella castellina 1 for the pierre auger collaboration 2 1istituto nazionale di astrofisica oato and infn torino 2observatorio pierre auger, av. san mart́ın norte 304, 5613 malargüe, argentina (full author list : http://www.auger.org/archive/authors 2012 12.html) corresponding author: castellina@to.infn.it abstract the pierre auger observatory has been designed to investigate the origin and nature of the ultra high energy cosmic rays using a hybrid detection technique. a review of selected results is presented, with the emphasis given to the measurement of energy spectrum, mass composition and arrival directions. keywords: ultra high energy cosmic rays sources energy spectrum primary composition. 1 introduction understanding the sources, nature and propagation properties of the cosmic rays at ultra high energies (e > 1018 ev) is one of the key questions in astroparticle physics. from the experimental point of view, their study can be performed indirectly, by exploiting the extensive air showers they produce by interacting with the nuclei in the earth atmosphere. among the different features characterizing the spectral shape, the region between' 1018−1019 ev is thought to host the transition from galactic to extragalactic cosmic rays. different models explain it as due to e+/e− pair production of protons with the photons of the cosmic microwave background (cmb) [1], or more traditionally to the intersection of a steep galactic component and the onset of a flatter extragalactic one [2]. at even higher energies, above ' 4 1019 ev, a cut-off in the cosmic ray flux is expected, due to photo-pion production of extragalactic protons in the cmb (the ”gzk cut-off” [3]) , although the same feature could arise when reaching the limits in the maximum energy of the sources. however, the all particle spectrum cannot provide a discrimination among the different hypotheses, and the determination of the primary composition is mandatory to reach any reliable conclusion. the analysis of the arrival directions and their anisotropy can give further insight into the sources and provide information about the magnetic fields which the ultra high energy (uhe) cosmic rays experience during their travel to earth. the pierre auger observatory has been specifically designed to investigate the origin and the nature of ultra high energy cosmic rays. it is located in malargüe, argentina, and consists of a surface array (sd) of 1660 water cherenkov stations on an area of ' 3000 km2, overlooked by 27 air fluorescence telescopes (fd) grouped in four sites [4]. thanks to the possibility of combining the information from the surface array, measuring the lateral distributions of secondary particles at the ground, and the fluorescence telescopes, observing the longitudinal profile, the reconstruction capabilities are enhanced with respect to the individual detector components. 2 the energy spectrum the energy spectrum above 2.5 1018 ev has been determined using the data from the sd [5], considering only events up to 60◦. the exposure is obtained by integrating the number of active stations over time; the overall acceptance uncertainty is ' 3% [6]. the energy calibration is derived directly from data, using a subset of high quality hybrid events, i.e. events reconstructed by both the fd and the sd [7]. despite the low duty cycle of the fd, the energy spectrum could be extended to 1018 ev using hybrid events, thanks to the good energy resolution and low threshold, thus investigating the transition region in detail [8]. the total systematic uncertainty in the energy scale is about 22%, the main contribution coming from the uncertainty in the fluorescence yield (14%) and in the reconstruction of the longitudinal profile (10%). the sd and hybrid spectra can be combined using a maximum likelihood method, since both have the same systematic uncertainties in the energy scale. the normalization uncertainties are on the contrary independent and have been used as additional constraints in the 132 http://dx.doi.org/10.14311/app.2014.01.0132 auger highlights procedure. the resulting spectrum is shown in fig.1; a fit with three power laws is shown by the dashed lines, while the solid line indicates the result of a fit with two power laws and a smooth function. the ankle feature is present at an energy of 1018.62 ev; the cutoff is clearly seen with a significance of 20 σ. different astrophysical models can be compared to our data; however, the energy spectrum can be described by both a heavy or proton composition at the highest energies and the information must be complemented by independent measurements of the primary composition. figure 1: the combined auger energy spectrum. only statistical uncertainties are shown. the systematic uncertainty on the energy scale is 22%. a comparison of the auger results with data from hires, telescope array and yakutsk has been recently performed [9]. the various fluxes can be rescaled assuming that any difference among them be due solely to energy scale and not to aperture calculations or energy resolution. the differences found are entirely consistent with the systematic energy uncertainties quoted by the experiments. 3 the nature of the primaries the most direct information about composition can be obtained by measuring the longitudinal development of showers in hybrid events, thus determining the mean depth of maximum development, xmax, and its fluctuation, rms(xmax). for each event, xmax depends on the depth of first interaction of the primary in the atmosphere and on the subsequent development of the shower; for this reason, the interpretation of the results in terms of composition is complicated by the uncertainties in the hadronic interaction models used in simulations. about six years of hybrid data have been analyzed applying fd quality cuts and ensuring that no bias with respect to the cosmic ray composition is introduced in the data sample [10]. having been corrected for the detector resolution, the xmax and its fluctuations are detector independent and can be directly compared to the predictions of different models, as shown in fig.2. both observables show a change for e > 5 1018 ev towards an increasingly heavy composition in comparison to the model predictions. the average resolution of xmax ' 20 g/cm2 in the considered energy range. figure 2: < xmax > and rms(xmax) as a function of energy, compared with the predictions of air shower simulations using different hadronic interaction models. in general, different values for rms(xmax) are allowed for different combinations of elements [11]. the fluctuations predicted by the considered hadronic interaction models and shown in fig.2 are evaluated only for pure compositions . a different conclusion, leading to a light composition up to the highest energies, has been drawn from the data of the hires and telescope array. however, a direct comparison of their results with the auger ones is not possible, as the detector biases are included in their simulation. furthermore, their dataset is smaller that that of auger. a lenghty discussion about this comparison can be found in [12] (and refs. therein). starting from an extension of the heitler model of ex133 antonella castellina tensive air showers [13], a method for interpreting the results of xmax and rms(xmax) in terms of mass composition has been developed. as discussed in [14], xmax is only function of the mean logarithmic mass < ln a >, and as such it carries information on the average composition. on the contrary, both the shower-to-shower fluctuations and the dispersion in the mass distribution contribute to rms(xmax). this information can be used to extract the < lna > and its variance from the observables and to build the plots shown in fig.3, where the size of the data points increases with increasing energy. the energy evolution of the composition is common to all models; reduced systematic uncertainties will allow in the future to test or even exclude some of them. different consequences from the astrophysical point of view can be derived from this comparison. extragalactic sources of protons seem to be disfavored by our composition result, within the uncertainties on the hadronic interaction models used to interpret the data. in a propagation scenario, nuclei from nearby sources could produce small mass dispersion at earth, as propagation would not be able to degrade mass and energy. if on the other hand the proton component is depleted by the reach of a rigidity dependent end of the injection spectrum, and if sources are uniformly distributed, hard injection spectra with low energy cutoff, together with local sources, could explain the data [15, 16]. figure 3: the pierre auger data in the (< lna > , σ2 lna) plane for different hadronic interaction models. grey contours limit the allowed region, the systematic uncertainties are shown by the black lines. 4 primary photons and neutrinos uhe primary photons and neutrinos can provide invaluable information about the astrophysics of cosmic rays. their detection would be a direct proof of the gzk cutoff; limits on exotic models [17] and tests for new physics [18] could be obtained from a positive or negative result on their detection. in both cases, their search is based on the characteristic features of the showers they produce in comparison to the hadronic ones. primary photons produce late developing showers, a characteristic further enhanced by the lpm effect [19]. the deeper xmax, observable by the fd, is associated to a more dispersed distribution of the arrival time of the particles at ground level. at a given distance from the shower axis, the arrival time of the first particles is delayed with respect to a planar shower front and the radius of curvature is thus expected to decrease for photon induced showers. these observables can be recorded by means of the sd. the upper limits derived from both the sd and the hybrid data collected by auger are shown in fig.4 and discussed in [20, 21]. astrophysical scenarios are favoured with respect to top-down models. figure 4: upper limits on the integral photon flux. different expectations are shown for comparison. primary neutrinos can produce showers characterized by a significant electromagnetic component; the huge hadronic background can be eliminated by looking at large zenith angles. ντ can interact by charged current in the earth crust, producing earth-skimming upward-going showers; neutrinos of any flavour can interact in the atmosphere by neutral or charged current giving rise to downward-going events. assuming a diffuse neutrino flux ' k e−2, 90% cl limits on their flux are obtained, as shown in fig.5. neutrinos from point sources were also searched for, over a broad declination range (north of ' −65◦ and 134 auger highlights south of ' 55◦), for eν > 1017 ev. for a differential neutrino flux ' kps e −2, 90% cl limits of ' 5 · 10−7 and 2.5 · 10−6 gev cm−2 s−1 have been obtained for up-going and down-going events respectively [22]. figure 5: differential and integrated upper limits on the single flavour e−2 ν flux (thin black lines: downward-going ν, thick red line: earth-skimming ν). different models are shown for comparison and discussed in [23] 5 anisotropies the spatial distribution of the arrival directions of uhe cosmic rays as a function of energy is a key observable to provide information about their sources and nature, complementary to those of energy spectrum and composition. particles of uhe are most probably extragalactic, and if the observed cutoff in the spectrum can be attributed to the gzk propagation effect we could expect their sources to be confined in our courtyard, within about 100 mpc. in 2007 [24] the auger collaboration reported the observation of a correlation between the arrival directions of the highest energy cosmic rays and the positions of nearby agn from the véron-cetty-véron catalogue [25]. the result came from an analysis of indipendent data with a priori parameters determined from an exploratory scan; this allowed to avoid the use of penalty factors which would be needed in a posteriori analyses. the most recent update of this search is shown in fig.6 [26]: the fraction of correlating cosmic rays is (33±5)% (28 events correlating out of a total of 84). the probability of this correlation to occur by chance if the true distribution of arrival directions is isotropic stays below 1%. the independent averages of 10 consecutive events are also shown (black dots). a recent comparison of our result with the telescope array and the yakutsk ones showed that the correlating fractions are compatible [27]. more data are necessary to show whether this correlation is statistically significant or not. figure 6: the correlating fraction as a function of the total number of time-ordered events. different confidence levels are shown, together with the isotropy value p=0.21 and the current estimate of all data, pdata = 0.33± 0.05. another possible scenario is that the anisotropy is dominated by cosmic rays originating from the vicinity of centaurus a, the nearest active galaxy with an estimated distance of about 3.8 mpc, since 19 events out of 7.6 expected have arrival directions within 24◦ of cena. a kolmogorov-smirnov test shows that the chance probability for this to happen is 4%. directionally aligned events, or ”multiplets”, can be expected from the same source after deflection in the magnetic fields, showing a correlation between the arrival direction and the inverse of energy. the largest multiplet found was one 12-plet, but also in this case the probability for it to come from an isotropic distribution is ' 6% [28]. potential sources of galactic cosmic rays have been looked for by performing a blind search for neutron primaries [29]. in fact, due to the relativistic time dilatation the uhe neutron mean decay length is (9.2× e/eev ) kpc; above 2 eev, neutron emitters can be searched for in the whole galaxy. auger can detect neutron showers by a simple search for an excess of proton-like showers from a specific direction in the sky. no candidates have been found, bringing to a median flux upper limit of 0.0114 n km−2 yr−1 above 1 eev. the absence of a neutron flux from the galaxy, which could be expected in the hypothesis of sources steadily emitting protons and neutrons with similar luminosity, could be a hint that the sources at eev energy could be e.g. extragalactic, transient or weak but densely distributed. the large scale distribution of the arrival directions of cosmic rays is another fundamental tool in the search for their origin. the results from a study performed using data from the sd array are shown in fig.7 [30]. no significant anisotropies are observed, resulting in the most stringent bounds on the first harmonic amplitude above 2.5 1017 ev. 135 antonella castellina figure 7: equatorial dipole component (top) and phase of the first harmonic (bottom) as a function of energy. the obtained limits already exclude some of the galactic models (labeled in fig.7 with a and s, indicating antisymmetric and symmetric galactic magnetic fields), according to which the cosmic rays at these energies are galactic and can escape by diffusion and drift motion. in the model labeled gal, cosmic rays are assumed to be galactic at all energies, and the anisotropy is due to purely diffusive motion caused by the turbulent component of the galacic magnetic field. in extragalactic models, the transition is put at the second knee and the cosmic rays large scale distribution is influenced by the relative motion of the observer with respect to the frame of the source. assuming that the frame in which the cosmic ray distribution at these energies is isotropic is coincident with the cosmic microwave background rest frame, a small anisotropy (the extragalactic compton-getting effect, labeled c-g xgal) is expected. interestingly, the phase of the first harmonic shows a smooth transition between a common phase of ' 270◦ below 1 eev and ' 100◦ above 5 eev. a consistency of the phase in ordered energy intervals can indeed be expected in presence of a real underlying anisotropy, standing out of the background more prominently than the amplitude. however, no confidence level can for the moment be assigned to this result, being an ”a posteriori” observation. the study of the large scale anisotropy has been performed for the first time with auger data as a function of both the right ascension and the declination and expressed in terms of dipole and quadrupole amplitudes [31]. no significant deviations from isotropy are detected. under the hypothesis that any anisotropy is dominated by these moments, the 99% cl upper limits can be derived, as shown in fig.8. figure 8: 99% cl upper limits on the dipole and quadrupole momenta as a function of energy. as an example of the power of the measurement to discriminate among different astrophysical models, the experimental limits are compared in the figure with the expectations from a toy model, in which the sources of protons and iron are stationary and uniformly distributed in the galactic disk. being the expected amplitudes for protons largely above the allowed upper limits, we can exclude this scenario for the light component of eev primary cosmic rays. 6 future developments the pierre auger observatory has reached a cumulative exposure of more than 26000 km2sr yr. new information about the characteristics of the primary cosmic rays have been derived, opening at the same time more questions and pointing to the need of an 136 auger highlights extension of the life time of auger. the measurement of composition of the primary particles from the eev region up to the highest energies has emerged as the key for hitting the hottest scientific questions: a) understand the origin of flux suppression discussed in sect.2, if due to the reach of the maximum energy at injection or to the gzk effect (a clear signature of which would be the observation of a flux of primary photons and neutrinos); b) perform composition driven anisotropy searches; c) determine the energy at which the transition from galactic to extragalactic sources of cosmic rays takes place. acknowledgement the author wishes to thank the organizers for the warm hospitality in mondello and the stimulating and interesting discussions during the workshop. references [1] v. berezinski, a. gazizov, s. grigorieva: 2006, phys.rev.d 74, 043005. doi:10.1103/physrevd.74.043005 [2] a.m. hillas: 2006, in cosmology, galaxy formation and astroparticle physics on the pathway to the ska klöckner, h.-r., jarvis, m., rawlings, s. (eds.) april 10th-12th 2006, oxford, united kingdom. [3] k. greisen: 1966, phys. rev. lett. 16, 748; g.t. zatsepin and v.a. kuzmin: 1966, sov. phys. jetp lett. 4, 78. [4] the pierre auger collaboration: 2010, nucl.instr.meth. a 620, 227. doi:10.1016/j.nima.2010.04.023 [5] the pierre auger collaboration: 2008, phys.rev.lett. 101, 061101. doi:10.1103/physrevlett.101.061101 [6] the pierre auger collaboration: 2010, nucl.instr.methods a613, 29. [7] r. pesce for the pierre auger collaboration: 2011, in 32nd int.cosmic ray conf., beijing, china; arxiv:1107.4809. [8] m. settimo for the pierre auger collaboration: 2012, eur.phys.j. plus 127, 87. [9] b. dawson et al. for the pierre auger, telescope array and yakutsk collaborations: 2012, in int.symposium on future directions in uhecr physics, cern. [10] p. facal for the pierre auger collaboration: 2011, in 32nd int.cosmic ray conf., beijing, china; arxiv:1107.4804. [11] k.-h. kampert, m. unger: 2012, astrop.phys. 35, 660. [12] e. barcikowski et al. for the pierre auger, telescope array and yakutsk collaborations: 2012, in int.symposium on future directions in uhecr physics, cern. [13] j. matthews: 2005, astrop.phys. 22, 387. [14] the pierre auger collaboration: 2013, jcap 02, 026. [15] a.m. taylor, m. ahlers, f.a. aharonian: 2011, phys.revd84, 105007. doi:10.1103/physrevd.84.105007 [16] d. allard: 2012, astrop.phys. 39-40, 33. doi:10.1016/j.astropartphys.2011.10.011 [17] p. battacharije and g. sigl: 2000, phys.rep.327, 109. [18] m. galaverni and g. sigl: 2008, phys.rev.lett.100, 021102. [19] l.d. landau, i.ya. pomeranchuk: 1953, dokl.acad.nauk.92, 553; a.b. migdal: 1956, phys.rev.103, 1811. [20] the pierre auger collaboration: 2009, astrop. phys.31, 399; 2008, astrop. phys.29, 243. [21] v. scherini for the pierre auger collaboration: 2012, in int.symposium on future directions in uhecr physics, cern. [22] the pierre auger collaboration: 2012, apj.lett. l4, 755. [23] the pierre auger collaboration: 2013, adv.in high energy phys.res., 2013, 708680. [24] the pierre auger collaboration: 2007, science 318, 938. [25] m.p. véron-cetty, p. véron: 2006, a&a 445, 773. [26] k.-h. kampert for the pierre auger collaboration: 2011, highlight talk in 32nd int. cosmic ray conf., beijing, china. [27] o. deligny et al. for the pierre auger, telescope array and yakutsk collaborations: 2012, in int.symposium on future directions in uhecr physics, cern. 137 http://dx.doi.org/10.1103/physrevd.74.043005 http://dx.doi.org/10.1016/j.nima.2010.04.023 http://dx.doi.org/10.1103/physrevlett.101.061101 http://dx.doi.org/10.1103/physrevd.84.105007 http://dx.doi.org/10.1016/j.astropartphys.2011.10.011 antonella castellina [28] the pierre auger collaboration: 2012, astrop.phys. 35, 354. doi:10.1016/j.astropartphys.2011.10.004 [29] the pierre auger collaboration: 2012, apj 760, 148. doi:10.1088/0004-637x/760/2/148 [30] the pierre auger collaboration: 2011, astrop.phys. 34, 627. doi:10.1016/j.astropartphys.2010.12.007 [31] the pierre auger collaboration: 2012, apj.suppl. 203, 34; 2013, apj.lett. 762, l13. 138 http://dx.doi.org/10.1016/j.astropartphys.2011.10.004 http://dx.doi.org/10.1088/0004-637x/760/2/148 http://dx.doi.org/10.1016/j.astropartphys.2010.12.007 introduction the energy spectrum the nature of the primaries primary photons and neutrinos anisotropies future developments 46 acta polytechnica ctu proceedings 2(1): 46–49, 2015 46 doi: 10.14311/app.2015.02.0046 transient processes in a binary system with a white dwarf. d. a. kononov1, d. v. bisikalo1, v. b. puzin1, a. g. zhilkin1 1institute of astronomy of the ras, moscow, russia corresponding author: dkononov@inasan.ru abstract using the results of 3d gas dynamic numerical simulations we propose a mechanism that can explain the quiescent multihumped shape of light curves of wz sge short-period cataclysmic variable stars. analysis of the obtained solutions shows that in the modeled system an accretion disk forms. in the outer regions of the disk four shock waves occur: two arms of the spiral tidal shock; “hot line”, a shock wave caused by the interaction of the circum-disk halo and the stream from the inner lagrangian point; and the bow-shock forming due to the supersonic motion of the accretor and disk in the gas of the circum-binary envelope. in addition, in our solutions we observe a spiral precessional density wave in the disk. this wave propagates from inside the disk down to its outer regions and almost rests in the laboratory frame in one orbital period. as a results every next orbital period each shock wave passes through the outer part of the density wave. supplying these shocks with extra-density the precessional density wave amplifies them, which leads to enhanced energy release at each shock and may be observed as a brightening (or hump) in the light curve. since the velocity of the retrograde precession is a little lower that the orbital velocity of the system, the same shock wave at every next orbital cycle interacts with the density wave later than at the previous cycle. this causes the observed shift of the humps over binary phases. the number of the shock waves, interacting with the density wave determines the largest number of humps that may be observed in one orbital period of a wz sge type star. keywords: cataclysmic variables dwarf novae optical spectroscopy photometry numerical simulations individual: ss cyg ≡ bd+42◦ 4189a. 1 introduction wz sge stars (subclass of su uma stars) are deeply evolved close binary systems with very short orbital periods (∼ 80) min and low mass ratios of the components (q < 0.1). as a rule these objects are very faint (fainter than 15m). the most remarkable observational feature of these stars in quiescence are their multi-humped orbital light curves. usually astronomers call them double-humped.there are a number of models proposed to explain a double-humped shape of the light curves of wz sge stars. one of them, advocated by aviles et al. (2010), explains the formation of the humps by visibility conditions of two arms of the tidal spiral shock caused by the action of the 2:1 tidal resonance. another model, mentioned, for instance, by wolf (1998) and silvestri et al., (2012) supposes that the stream from the inner lagrangian point may overflow the disk after it ricochets on the disk rim and forms an additional hot spot at the opposite side of the disk, i.e. two hot spots give two humps in the light curve. these two models would have worked perfectly had not there been a number of observational facts that cannot be explained by them. we, above, deliberately called the light curves of wz sge stars “multihumped” instead of commonly used “double-humped”, since there are a number of works where observers report from one to four humps in one orbital period (see, e.g., araujo-betancor et al. (2005), katysheva & shugarov (2009), kitsionas et al. (2005), and pavlenko (2009)). besides, as shown in the mentioned papers, even in the same system the number of the humps varies depending on the epoch of observations. thus, only two bright sources, implied by the models, described above, are not enough to explain more than two humps. one more feature of the humps that cannot be explained by, say, the visibility conditions of the arms of the tidal shock is that they tend to shift over binary phase when observed in time-distant nights. the point is that the positions of the tidal shock arms in an accretion disk are determined by the roche potential and fixed in the coordinate frame, rotating along with the binary. thus, their contributions must always be observed at the same binary phases in every night. it is commonly accepted that the most important observational manifestations of cvs and, in particular, wz sge stars, come from gas dynamical processes initiated by the mass transfer between the components. 46 http://dx.doi.org/10.14311/app.2015.02.0046 transient processes in a binary system with a white dwarf. therefore, in order to understand what happens in wz sge stars and what structures and processes contribute to their observational manifestations one needs to study gas dynamics of these objects. in this paper we, by means of 3d gas dynamic simulations, aim to investigate the flow structure in a representative of wz sge stars and propose a physical model, capable to explain the multi-humped nature of their light curves. in section 2 we describe the simulations and show their results. in section 3, based on the results of gas dynamic simulations we consider a physical model of the formation of the humps in orbital light curves of wz sge stars. in section “conclusions” we summarize our results and discuss further studies. 2 numerical simulations to investigate flow structure in wz sge stars we have performed gas dynamic simulations of a close binary system having the parameters of v455 and. this system is one of the brightest representatives of the class and has well defined parameters (araujo-betancor et al. (2005)) that are as follows. the secondary mass is msec = 0.07m�, and the primary mass (white dwarf) is mwd = 0.6m�. the binary separation of the system is a = 0.56r�. the mass transfer rate in the system is estimated as ṁ = 10−11m�/year. the orbital period of the system is porb = 81.08 min. to model the flow structure in the v455 and system we use a numerical hd/mhd code “nurgush” (zhilkin & bisikalo (2009)). when modeling, we set the magnetic field of the accretor equal to zero, so this is a pure gas dynamic case. the simulations are conducted until the system enters a quasi-stationary regime, i.e. the total mass of the disk varies by less than 2% in one orbital period. approaching this regime takes approximately 30 orbital periods. the results of the calculations are shown in fig. 1. in its panels we show density distributions in the equatorial plane of the system for two time moments τ = 33.53porb and τ = 34.13porb. analysis of the obtained results shows that an elliptic accretion disk forms in the system. one also can see that in the disk a spiral density wave occurs. its approximate location is denoted by the white dashed lines. this precessional density wave, first described by bisikalo et al. (2004), occurs due to the retrograde precession (apsidal motion) of elliptic flow lines, caused by the tidal action of the secondary. the angular velocity of the retrograde precession of this wave (its absolute value) is only a few precent lower than the orbital angular velocity of the system. this means that in the observer’s frame in one orbital period this wave almost rests and, in the frame, rotating with the binary, it makes almost a round during the same period. this effect is wellseen in fig. 1 where at two time moments, separated by approximately 0.6porb, the outer part of the wave occupies almost opposite locations. figure 1: density distributions in the equatorial plane of the system for two time moments τ = 33.53porb (top panel) and τ = 34.13porb (bottom panel). the white dashed line denotes the position of the precessional density wave. 3 model of the multi-humped light curve in fig. 1 one can clearly see that the precessional spiral density wave in our solution propagates down to the outer regions of the accretion disk. from our previous studies (see, e.g., bisikalo & kononov (2010), kononov et al. (2012)) we know that in the outer regions of the disk four most powerfull shock waves should form. these are: two arms of the spiral tidal shock; “hot line”, a shock wave caused by the interaction of the circumdisk halo and the stream from the inner lagrangian point; and the bow-shock forming due to the supersonic motion of the accretor and disk in the gas of the 47 d. a. kononov et al. circum-binary envelope. since, as we noted above, the precessional density wave rests in the observer’s frame and propagates down to the outer regions of the disk, the latter four shocks must pass through its outer part in every next orbital period. when a shock wave passes through the outer part of the density wave it is supplied with extra-density. this must cause amplification of the shock wave. indeed in fig. 2, where we plot pressure distributions for the time moments, corresponding to those of fig. 1, we can see that in the location of the outer part of the density wave pressure increases. the cases shown in fig.2 correspond to time moments when the density wave interacts with the arms of the tidal shock. in the upper panel of fig. 2 the density wave interacts with the closer-to-donor arm of the tidal shock. note that at this moment the pressure in the location of the opposite arm is remarkably lower. in the lower panel the farther-from-donor arm of the tidal shock is more pronounced, while the opposite arm is “inactive”. summarizing the above behavior, we can propose the following model that can explain the formation of the humps in quiescent orbital light curves of wz sge stars. in a system an elliptic accretion disk forms. under the tidal action of the secondary, in this disk, a precessional density wave develops. this wave propagates down to the outer regions of the disk. since the angular velocity of the retrograde precession of the wave is only a few percent lower than the orbital angular velocity of the system, the density wave almost rests in the observers frame. thus the four main shock waves also located in the outer regions of the disk consecutively pass through the outer part of the density wave every next orbital period. when the shock wave interacts with the density wave it is supplied with extra-density and, hence, amplified. the amplification of the shock wave must increase the energy release at the shock that should be seen as a hump in the light curve of the system. we should note that our model can explain not only the origin of the humps but, as well, their behavior. in particular, in the frame of our model, we can easily explain why the humps shift over binary phases from night to night. the point is that the angular velocity of the retrograde precession is not exactly the same as the orbital velocity of the system, it is a little lower. thus, at the next round a shock wave approaches the outer part of the density wave a little later than at the previous one and the interaction between the two waves starts later. the corresponding humps, hence, must shift forward over the binary phase. one more feature of the wz sge light curves that should be explained is the varying number of the humps. we show above that in principle one can observe not two but up to four humps in the light curve, since the density wave may interact with four most powerful shock waves located in the outer regions of the disk. however, the number of seen humps may depend on the visibility conditions of the amplified shock. for example, if a shock is amplified when it is situated at the moment of observations at the opposite from the observer side of the disk, radiation from the shock must pass through the disk and, in principle, may be reduced. besides, the shocks may be of different power. in order to have a clear answer to this question we need to have more observations. figure 2: pressure distributions in the equatorial plane of the system for two time moments τ = 33.53porb (top panel) and τ = 34.13porb (bottom panel). the black dashed line denotes the position of the precessional density wave. 4 conclusions we have performed 3d gas dynamic simulations of the flow structure in a short-period cataclysmic variable star of wz sge type. analysis of the results has shown 48 transient processes in a binary system with a white dwarf. that in the system an elliptic accretion disk forms. in the disk a precessional density wave develops. the wave propagates down to the outer regions of the disk. bisikalo et al. (2004) showed that the angular velocity of the retrograde precession of this wave is only a few percent lower than the orbital velocity of the system. thus, the precessional density wave almost rests in the observer’s frame. from our previous studies we know that in the outer regions of the disk four shock waves form. every next orbital cycle these shocks consecutively pass through the outer part of the density wave. as a result every shock is supplied with extra-density and amplified. the amplification of a shock causes enhanced energy release and may be seen in the light curve as a hump. since the density wave retrogradely precess with the velocity that is a little lower than the orbital velocity, at every next round the same shock passes through the outer part of the density wave a little later. thus the corresponding hump in the light curve at every next round occurs at a later binary phase. this, in the frame of our model, allows us to explain the observational fact that the humps shift over binary phases when observed at different nights. the variable number of the humps may be explained by the visibility conditions of the amplified shock wave. our studies of wz sge stars continue and with further accumulation of observational results we expect to have a more detailed model of the formation of light curves in these cataclysmic variable stars. acknowledgement this work is supported by the russian foundation for basic research (projects 11-02-00076, 12-02-00047, 1302-00077, 13-02-00939, 12-02-31031), the federal targeted program ”science and science education for innovation in russia 2009–2013”, grant of the president of russia for young scientists (mk-2432.2013.2) references [1] aviles, a.; zharikov, s.; tovmassian, g. at al.: 2010, the astrophysical journal, 711(1), 389-398. doi:10.1088/0004-637x/711/1/389 [2] wolf s., et al.: 1998, a&a, 332, 984. [3] n. m. silvestri, p. szkody, a. s. mukadam et al.: 2012, the astronomical journal, doi:10.1088/0004-6256/144/3/84 [4] araujo-betancor, s.; gänsicke, b. t.; hagen, h.-j. at al.: 2005, a&a, 430, 629-642. [5] katysheva, n., shugarov, s.: 2009, journal of physics: conference series, 172(1), 12-44. [6] s. kitsionas, o. giannakis, e. harlaftis, h., et al.: 2005, the astrophysics of cataclysmic variables and related objects, asp conference series, 330, [7] pavlenko e.,: 2009, journal of physics: conference series, 172(1), id. 012071. [8] a.g. zhilkin, d.v. bisikalo: 2009, asp conference series, 406, 118 123. [9] d. v. bisikalo, a. a. boyarchuk, p. v. kaigorodov, o . a. kuznetsov, and t. matsuda: 2004, astronomy reports, 48(6), 449456. doi:10.1134/1.1767212 [10] bisikalo, d. v., kononov, d. a.: 2010 memorie della societ? astronomica italiana, 81, 187 [11] kononov, d. a., giovannelli, f., bruni, i. and bisikalo, d. v.: 2012, astronomy & astrophysics, 538, id.a94, 7 49 http://dx.doi.org/10.1088/0004-637x/711/1/389 http://dx.doi.org/10.1088/0004-6256/144/3/84 http://dx.doi.org/10.1134/1.1767212 introduction numerical simulations model of the multi-humped light curve conclusions 264 acta polytechnica ctu proceedings 2(1): 264–268, 2015 264 doi: 10.14311/app.2015.02.0264 on the 2011 outburst of the recurrent nova t pyxidis l. izzo1, m. della valle2, a. ederoclite3, m. henze4 1dip. di fisica, sapienza university of rome, p.le a. moro 2, rome; icranet, p.le della repubblica 10, pescara, italy 2inaf osservatorio di capodimonte, salita moiariello 16, 80131 napoli, italy 3centro de estudios de fisica del cosmos de aragón, plaza san juan 1, planta 2, teruel, e44001, spain 4european space astronomy centre, p.o. box 78, 28692 villanueva de la cañada, madrid, spain corresponding author: luca.izzo@gmail.com abstract we discuss the nebular phase emission during the 2011 outburst of the recurrent nova t pyxidis and present preliminary results on the analysis of the line profiles. we also present some discussions about the binary system configurations and the x-ray emission, showing that the white dwarf mass should be larger than 0.8 m�. keywords: spectroscopy x-rays individual: t pyx. 1 introduction the 2011 outburst of the recurrent nova t pyx shed more light on some interesting characteristics of this peculiar nova. the optical evolution was not very different from the last (1966) outburst, showing the 8 days ’shoulder’ before the final rise to the maximum luminosity, which was reached ∼ 30 days from the initial outburst. the distance of t pyx was determined from light echoes to be 4.8 ± 0.5 kpc [1], which is marginally consistent within the errors with the value of 3.5 ± 0.4, estimated from the application of the maximum magnitude versus rate of decline (mmrd) relation [2] to the light curve of the 1966 outburst [3]. the presence of a clumpy ring with an inclination of 30-40 degrees, embedded within a spherical shell, was also recently reported using hubble space telescope observations during the nebular phase [1]. a variation of the orbital period after the 2011 outburst was detected, indicating an ejected mass in the outburst of 3 × 10−5 m� [4]. also, the orbital period was found to have increased during the long quiescence period between the last two outbursts of t pyx. moreover, with respect to the 1966 epoch, when no advanced x-ray and radio detectors were available, we have now a good knowledge of the emission of t pyx at these frequencies during its outburst [5]. in the previous work [6], we have presented the early spectral evolution, up to two months after the initial outburst. we have shown the hybrid spectral transition he/n fe ii he/n and initial ejecta velocities. in this work, we present the optical observations of the nebular phase, which was marked by the onset of the supersoft x-ray source (sss) emission which happened during the seasonal gap [7]. the optical observations presented here were obtained with the high-resolution spectrograph sarg, mounted on the 3.5m telescope nazionale galileo (tng) located at la palma. spectra with power resolution of r = 29000 were obtained but the complete sample, which includes also observations obtained at the very large telescope, will be presented in ederoclite et al. in preparation. then we briefly discuss the x-ray emission and finally we provide an updated scheme of the binary system configuration in t pyx, taking into account the recent results. 2 the nebular phase of t pyx the nebular phase in novae is easily recognized by the absence of absorption lines and the presence of forbidden emission lines, e.g. [oiii] and [nii], in the optical spectra, similarly to planetary nebula cases. indeed, these emission lines are due to photo-ionization of the ejecta by the central hot white dwarf (wd). at the same time, forbidden transitions originate mainly in rarified environments, so that any structure observed in corresponding line profiles is mainly due to the distribution of the material and not to self-absorption mechanisms. the analysis of the [oiii] 4959-5007 and [nii] 5755 λλ profiles can consequently provide hints on the geometry of the ejecta. these line profiles are well described by a large flat top base (vexp,1 ≈ 1700 km/s) overlapped by a saddleshaped and brighter emission, with vexp,2 ≈ 600 km/s, see fig. 1 for the case of the [oiii] 5007 λ. the high resolution allows us to detect a castellated structure on 264 http://dx.doi.org/10.14311/app.2015.02.0264 on the 2011 outburst of the recurrent nova t pyxidis the top of the profiles which is due to the presence of a clumpy ejecta structure. the saddle-shaped configuration suggests a non-spherical geometry of the ejecta, as generally discussed in [8] and further developed in several publications. in order to estimate the asphericity from forbidden lines we have used a method first presented in [9]. an analytic expression for the line profiles i(l) from an anisotropic distribution of the nova ejecta was provided: i(l) = k ( c v0 )α+1 ×[ lα−2 2 − lα−2 1 α− 2 l2(1 − 3cos2i) + lα2 − lα1 α (1 − sin2i) ] , l ≤ l1;[ lα−2 2 − lα−2 α− 2 l2(1 − 3cos2i) + lα2 − lα α (1 − sin2i) ] , l ≥ l1; (1) where c is the speed of light, v0 is the velocity at the inner radius of the expanding shell (we have assumed the maximum velocity observed for the bright profile, v0 ≈ 600 km/s), α describes the variation of the shell’s velocity with the distance form the wd, and l = (λ− λ0)/λ0 = v/c is our variable. the quantity -0.006-0.004-0.002 0.000 0.002 0.004 0.006 0 5.´ 10-13 1.´ 10-12 1.5´ 10-12 displacement l from @oiiid λλ 5007 fl ux he rg �c m 2 � s� a ng l figure 1: the saddle-shaped profile in the [oiii] 5007 line and the best fit (red line) obtained with the method described in the text. l2 = v2/c corresponds to the zero intensity along the wing of the line profile. a grid-search algorithm was developed to find the best fit for the inclination angle i that the binary orbital plane forms with the line of sight. for all the three lines, we find a large angle i ≈ 60 ± 10 degree, see also tab. 1, which contrasts some estimation of the i given before the 2011 outburst [14], and suggests a larger value for the binary inclination angle, see also [1]. we note that this approach does not take into account the presence of a clumpy structure. a more detailed approach is needed, and will be presented elsewhere. 3 the configuration of the binary system it is clear from the nebular spectra that the emission in t pyx is well described by quasi-spherical ejecta, which give rise to the larger flat top profile, and an equatorial ring of material, which is slower and gives rise to the saddle-shaped profiles. the origin of this equatorial ring is unknown: it is possible that it formed during the interaction of the main ejecta with pre-existing gas, which is equatorially distributed around the binary system (an hypothesis presented in [13]); another possibility can be that the early interaction of the ejecta with the secondary star could influence the subsequent expansion [10], but other mechanisms can also work. in all cases, it is necessary to shed light on the observed asphericity in t pyx, and the first ingredient we need is the mass of the wd. table 1: fit results of the line profiles of [oiii] 4959, 5007 and [nii] 5755, using the approach developed in [9]. ident. wavelength ( å) i (degree) v1 (km/s) α k (erg/cm2/s/ang) 4959 59 ± 10 465 ± 6 -2.2 ± 0.3 (3.7 ± 0.1) × 10−15 5007 59 ± 10 477 ± 6 -2.3 ± 0.3 (1.09 ± 0.03) × 10−14 5755 60 ± 10 444 ± 6 -2.8 ± 0.3 (6.8 ± 0.5) × 10−16 265 l. izzo et al. � � � � � � � � figure 2: the location of the t pyx parameters (green stars) with respect to the m 31 nova correlations presented in [20]: (1) the ton-toff correlation, for t pyx measured from the time of maximum brightness; (2) the kt-toff relation, with kt given by the average value kt=55.7 ev; (3) the relation between ton and t2 and (4) the correlation between ton and the expansion velocity as measured from the hα emission line. x-ray observations of the sss phase can in principle provide this physical quantity. the sss emission is caused by stable hydrogen burning in the matter that was not ejected during the nova outburst. this burning matter forms an envelope around the wd and can be observed once the ejected material becomes optically thin to soft x-rays. the duration of the sss phase is inversely related to the wd mass [11], since more massive wds need to accrete less matter to trigger an outburst. given its recurrent nature, t pyx is expected to contain a massive wd. the sss phase of t pyx was first detected about 90 days after the outburst [7], when an increase in soft x-rays was observed by the swift-xrt [12]. t pyx remained in this state for ≈ 200 days, although around day 190 the luminosity started to decline. we do not enter here into a discussion on the details of this emission, which will be described in a forthcoming work. what is interesting in the context of this work is the relatively short duration of the sss phase, which suggest a large wd mass. observations obtained before 2011 reported a wd mass of 0.7 m� and a mass ratio of q = 0.2 [14], which implies a secondary star of 0.14 m�. the orbital period was observed with high accuracy to be porb = 1.8295 hrs. with some assumption on the type of the companion star, we can infer the mass of the secondary which overfills its roche lobe: ∆m2 = ρ2 4 3π(∆r2)3, where ρ2 is the density and ∆r2 the dimensions of the overfilling envelope of the secondary. from the q value and the absence of signatures of the secondary in optical spectra during the quiescent phase [3], we can assume that it is a low-mass m-type star. its density can be well approximated using the eggleton formula ρ2 = 107porb(hrs) −2 g cm−3 [15], while its radius can be derived from the patterson et al. formula r2 = 0.62m0.61 2 r� [16]. the roche lobe size of the secondary is related to the q parameter through l2 = 1.631q1/3m 1/3 1 porb(hrs) 2/3 1010 cm [17]. the result is that the envelope overfilling the secondary roche lobe is related to the wd mass. from the recent estimate of the mass ejecta after the 2011 266 on the 2011 outburst of the recurrent nova t pyxidis outburst (3 × 10−5m�, [4]), and assuming that every observed t pyx outbursts ejected similar masses, we obtain a total mass ejected from t pyx of about 2× 10−4 m�. if this mass was accreted onto the wd from the secondary we can obtain a lower limit on the wd mass from the above formula. this results in mwd ≥ 0.8 m�. 4 final considerations our last result requires some important remarks. first, it was proposed that the mass ejected in t pyx is larger than the one accreted [3]. we do not consider this possibility in this work, i.e., that all the accreted mass results to be the ejected one. we know that this is not exactly true, since the sss phase is due to the burning of accreted hydrogen which is not ejected in the nova outburst. the mass of this burning envelope can be estimated assuming that the energy source for the sss phase is the gravitational contraction [18], but this contribution can be neglected. second, there is the possibility that a fraction of the matter overfilling the secondary’s roche lobe would flow out from the external lagrangian point l2, leading to the formation of an asymmetric structure around the binary system. such a mechanism would operate only if the primary roche lobe has been filled by accreted gas, leading to the detection of transient heavy elements in absorption (thea) during the early phases of the outburst [19], whose presence, in this case, is not certain. moreover, in tight systems where the secondary is less massive than the wd (q < 1) also centrifugal forces can contribute to such an outflow. there is again observational evidence that t pyx shares many properties common to other novae. as an example of this, we compare t pyx to the unbiased sample of m31 novae [20], in particular with respect to the correlations between some optical and x-ray observables: the blackbody temperature of the sss emitter, the turn-on and turn-off time of the sss emission, the expansion velocity of the ejecta and the t2 determined from the r-band light curve [21], see fig. 2. we see that t pyx lies in the same region occupied by classical novae observed in m31. all these results need to be figured in a unique picture for t pyx and can shed more light on cv systems with a mass ratio of less than unity. further results and conclusions will given in izzo et al. (2015) in preparation. acknowledgement we are very grateful to r. williams, s. n. shore, e. mason, d. de martino and r. gilmozzi for precious discussions. m.h. acknowledges support from an esa fellowship. references [1] sokoloski, j. l., crotts, a. p. s., uthas, h., et al.: 2013, apj 770, 33. [2] della valle, m. & livio, m.: 1998, apj 506, 818. [3] selvelli, p., cassatella, a., gilmozzi, r., et al.: 2008, a&a 492, 787. [4] patterson, j., oksanen, a., monard, b., et al.: 2013, arxiv/1303.0736. [5] nelson, t., chomiuk, l., roy, n., et al.: 2012, apj, 785, 78. [6] izzo, l., et al.: 2012, mem. s.a.it. s. 83, 830. [7] schwarz, g. j., osborne, j. p., page, k., et al.: 2011, atel 3754. [8] payne-gaposchkin, c. h.: 1957, the galactic novae. [9] vainu bappu, m. k. & menzel, d. h.: 1954, apj 119, 508. doi:10.1086/145857 [10] hutchings, j. b.: 1972, mnras 155, 357. doi:10.1093/mnras/155.3.357 [11] starrfield, s., truran, j. w., sparks, w. m., et al.: 1991, in extreme ultraviolet astronomy, ed. r. malina & s. bowyer, newyork, pergamon, p. 168. [12] gehrels, n., et al.: 2004, apj, 611, 1005. doi:10.1086/422091 [13] williams, r.: 2012, aj, 144, 98. [14] uthas, h., knigge, c. & steeghs, d.: 2010, mnras, 409,237. doi:10.1111/j.1365-2966.2010.17046.x [15] eggleton, p. p.: 1983, apj, 268, 368. doi:10.1086/160960 [16] patterson, j., kemp, j., harvey, d. a., et al.: 2005, pasp, 117, 1204. doi:10.1086/447771 [17] paczynski, b.: 1971, ara&a, 9, 183. doi:10.1146/annurev.aa.09.090171.001151 [18] krautter, j., oegelman, h., starrfield, s., et al.: 1996, apj, 456, 788. [19] williams, r., mason, e., della valle, m., et al.: 2008, apj, 685, 451. doi:10.1086/590056 [20] henze, m., pietsch, w., haberl, f., et al.: 2014, a&a, 563, a2. [21] della valle, m. & livio, m.: 1995, apj, 452, 704. 267 http://dx.doi.org/10.1086/145857 http://dx.doi.org/10.1093/mnras/155.3.357 http://dx.doi.org/10.1086/422091 http://dx.doi.org/10.1111/j.1365-2966.2010.17046.x http://dx.doi.org/10.1086/160960 http://dx.doi.org/10.1086/447771 http://dx.doi.org/10.1146/annurev.aa.09.090171.001151 http://dx.doi.org/10.1086/590056 l. izzo et al. discussion christian knigge: the system parameter we estimated in uthas et al. 2011 should be used with caution. they are based on a radial velocity study, and parameters resulting from such studies are known to be biased quite often. christian knigge: you consider r2 and l2 differing by ≈ 20%. are you really saying this could be the physical configuration, i.e. that the donor is overflowing the roche lobe by this amount ? luca izzo: the results that i’ve presented comes out naturally from formulae and physical considerations based on fixed binary parameters, as mwd = 0.7 m�, q = 0.2, porb = 1.8295 hrs, and considering the donor as a low mass m-type star. following a work by patterson et al., we obtain the r2 value, while from paczynski the value of l2. their interpretation depends obviously on a binary parameter as q presented in the uthas et al. work. anyway, other works consider that value of q as the actual one working in t pyx case. 268 introduction the nebular phase of t pyx the configuration of the binary system final considerations acta polytechnica ctu proceedings doi:10.14311/app.2017.12.0050 acta polytechnica ctu proceedings 12:50–55, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app the relation between driver behavior and intelligent transport system alica kalašováa,∗, simona kubíkováb, ján kapustab a univerzitná 1,âă010 26, žilina, slovak republic, supervisor of department of road and urban transport b univerzitná 1,âă010 26, žilina, slovak republic, phd. student ∗ corresponding author: alica.kalasova@fpedas.uniza.sk abstract. the main objective of slovakia’s transport policy is to reduce the number of traffic accidents and increase safety on our roads. implementation of intelligent transport systems presents one of the possibilities how to meet this goal. acceptance of these systems by motor vehicle drivers and other road traffic participants is necessary in order for them to fulfill their purpose. only if the drivers will accept intelligent transport systems, it is possible to flexibly and effectively manage road traffic flexibly and effectively. from the perspective of a driver it concerns, in particular, the possibility of using alternative routes when traffic accidents or other obstacles occurs on the route that would significantly affect the continuity and safety of road traffic. thanks to these technologies, it is possible to choose the appropriate route while driving, of course based on the criterion, which the driver considers the most important during the transport from origin to destination (driving time, distance from origin to destination, fuel consumption, quality of infrastructure). information isare provided to the driver through variable message signs or directly in the vehicle (rds-tmc). another advantage of intelligent transport systems is a positive impact on psychological well-being of the driver while driving. additional information about the possible obstacles, weather conditions and dangerous situations that occur on the roads as well as alternative routes are provided to the driver well in advance. this paper is mainly focused on how the drivers perceive the influence of intelligent transport systems in žilina region. keywords: safety, accidents, its. 1. introduction the slovak republic has implemented into its legislation aâălegally binding act of the european union, directive 2010/40/eu of the european parliament and of the council of 7 july 2010 on the framework for the deployment of intelligent transport systems in the field of road transport and for interfaces with other modes of transport. thereby, the slovak republic committed to meet the conditions of implementation and use of intelligent transport systems. however, effort exists to improve this situation through the adoption of act no. 317/2012 coll. on intelligent transport systems in road transport and amending and supplementing certain acts, as well as by adopting national road safety plan of the slovak republic in the years 2011-2020 and program to support the development of intelligent transport systems and national system of traffic information. the basis of these documents is a promising creation of a so-called vision of zero accident rate in the field of transport safety. in this context that regarding the european area of road traffic safety, the european commission enforces reduction of the number of road traffic fatalities by half in comparison with 2010 as a priority for years 2011 to 2020[1]. in recent years, the slovak republic managed to lower the number of traffic accidents. the ambitious objective of slovakia’s commitment under the european road safety charter to reduce the number of fatalities in road accidents to half by 2010, in comparison with 2002, when 610 people were killed on our roads, was not fulfilled. we managed to lower the number to 345 fatalities, which represents a 43% decrease. even though we failed to meet the commitment mentioned above, subsequent statistical indicators of accident rates in the slovak republic, which show a downward trend, are positively perceived in slovakia as well as in the european union[2]. figure 1 shows the decrease of accident rates on our roads from 2000 to 2015. this decrease is caused by the development and evolution of automotive technology (especially the development of active and passive safety of vehicles) as well as by better and more suitable roads, better traffic signs, proper traffic management and organizational measures and also by the use of intelligent transport systems. the rapid decline of accident rate between 2008 and 2009 was caused by the adoption of new laws and decree in our legislative related to traffic safety[3]. this paper is focused mainly on the analysis of traffic situation in žilina region, specifically on the section between the city of bytča and ivachnová village. the intensity of vehicles on this section is one of the highest in the region. the application of intelligent transport systems is one of the most effective 50 http://dx.doi.org/10.14311/app.2017.12.0050 http://ojs.cvut.cz/ojs/index.php/app vol. 12/2017 the relation between driver behavior and intelligent transport system figure 1. evolution of accident rates in the slovak republic from 2000 to 2015. city road name intensity traffic accidents ružomberok d1 19636 3 hlboké nad váhom-strečno i/18 26087 86 šútovo-kraľovany i/18 21225 5 kraľovany-dolný kubín i/70 13766 8 vrútky-kraľovany i/18 21758 33 kraľovany-sliače i/18 21861 31 žilina-terchová ii/583 5366 39 terchová-párnica ii/583 3843 5 table 1. traffic accident rates on the selected sections of road network in 2014. ways how to improve traffic situation on this road section. 2. characteristic of the selected section of road network selected section of road network consists of the first and second class roads and d1 motorway. the statistics of traffic accidents based on the section and type of road are listed in the following table 1. presented data are from 2014. the table shows that the most traffic accidents in 2014 on a selected road network were documented on the section from hlboké nad váhom to strečno (road i/18), where the highest intensity of vehicles per 24 hours was also recorded. 2.1. measurement of road network safety indicators of accident rates usually determine the safety on roads. safety is the result of risk and level of risk influence. the risk is expressed by the number of traffic accidents and the level of risk influence is specified through intensity. the indicators always refer to the same period of time, which is in this case one year. this enables us to determine the frequency of traffic accidents. frequency = n/t (1) where: n – number of traffic accidents, t – time period [year]. relative accident rate represents the probability of occurrence of traffic accident on individual sections. it is calculated as the ratio between the number of traffic accidents and traffic performance. when calculating this indicator, it is necessary to distinguish whether it is a calculation of relative accident rate at intersections or on sections between intersections[4]. r = n 365 ∗ rpdi ∗ t ∗ 106 (2) for intersections r = n 365 ∗ rpdi ∗ l ∗ t ∗ 106 (3) for sections where: n – number of traffic accidents, rpdi – annual average of daily intensities, t – time period, l – length of examined section. another indicator that is used to assess safety is the density of traffic accidents. it refers to the number of road accidents and to the section length, thus intensity is not taken into account. it is calculated according to the formula: h = n l ∗ t (4) where: h – density of traffic accidents, n – number of traffic accidents, t – time period, l – length of examined section. frequency of accidents, relative accident rate and density of accidents were the indicators used in this paper. these indicators were calculated based on the statistical data from 2014 and they are listed in table 2[5, 6]. as shown in table 2, relative accident rate which depends on the transport performance is not critical in any case. however, it should be noted that property damage only (pdo) accidents were not taken into account since these statistics were not available. otherwise, the values of relative accident rate would be much higher. the highest value of density of traffic accidents (3,1 accidents per one kilometer) was recorded on the stretch from hlboké nad váhom to strečno, which is the section of road i/18. also in this case, property damage only accidents were not included in the calculation. this analysis shows that it is necessary to solve the traffic situation on the given section mainly through long-term organizational measures as well as by the application of intelligent transport systems. voluntary acceptance of intelligent transport systems by drivers and other road traffic participants is necessary in order for it to be effective. a questionnaire survey, whose main goal was to identify the requirements and needs of road users as well as the level of perception of intelligent transport systems was conducted within the žilina region. 51 a. kalašová, s. kubíková, j. kapusta acta polytechnica ctu proceedings section rpdi [veh/24] l [km] n [number of accidents] r [%] h [number of accidents/km/year] ružomberok 19636 3,06 3 13,67899 0,980392157 hlboké nad váhomstrečno 26087 27,7 86 32,60631 3,104693141 šútovo-kraľovany 21225 5,2 5 12,41155 0,961538462 kraľovany-dolný kubín 13766 18,1 8 8,79652 0,44198895 vrútky-kraľovany 21758 15,7 33 26,46686 2,101910828 kraľovany-sliače 21861 27,2 31 14,28334 1,139705882 žilina-terchová 5366 24,5 39 81,27463 1,591836735 terchová-párnica 3843 20,4 5 17,47337 0,245098039 table 2. accident indicators. 3. analysis of perception of intelligent transport systems from the perspective of drivers the survey was conducted electronically through a website, as well as by personal conversations with residents who possess a valid driving license. data was collected during one month, from april 13, 2015 to may 19, 2015. subsequently, the data were was analyzed and evaluated graphically and in tables. the tool called ,"sample size calculator" was used to determine the minimum sample size that is required for sufficient explanatory power of the survey, in which we set up the population of registered drivers in žilina region to 414âă678, we chose 95% confidence interval and permissible margin of error was 5% (fig. 2). the minimum sample was set to 384 respondents. a total of 519 respondents participated in the survey and therefore we can conclude, that the survey has sufficient explanatory power. figure 2. sample size calculator. the first part of the questionnaire was focused on the categorization of respondents according to age, sex and also according to the fact whether the respondent is an active or passive driver (fig. 3). the purpose and regularity of trips made during the week were also examined (fig. 4). when choosing the route, every driver prefers the figure 3. percentage of active and passive drivers. route that best suits his needs and criteria. essential criteria for choosing the most appropriate route are fuel consumption, time accessibility of the destination point, distance between origin and destination, the danger of traffic accidents and so on. the evaluation scale was as follows: 0 – irrelevant, 1 – the least significant, 5 – the most important. weighted arithmetic means of importance of the individual criteria are calculated from these values and they are graphically processed in table 3, which shows that the most important criterion for men in both age categories is the quality of transport infrastructure. time accessibility of destination point is the most important for women. traffic congestions and delays on roads can be eliminated through the opportunity to use an alternative route, to which the vehicle will be diverted via information systems installed directly in the vehicle (rds-tmc) or through information systems situated on roads that contain information for the entire traffic flow (variable message signs). in the questionnaire survey, respondents were also asked whether they would be willing to take an alternative route offered by the information system in case of traffic accident or the occurrence of other obstacles on their original route. the results are shown in fig. 5. the most frequent answer of the respondents was that they are willing to accept an alternative route even if the distance to the destination would rise by 52 vol. 12/2017 the relation between driver behavior and intelligent transport system figure 4. purpose of transport and routing of traffic flows. criteria men 18-26 men 27-65 women 18-26 women 27-65 fuel consumption 3,59 3,52 3,10 3,75 travel time 3,79 3,95 3,96 4,13 distance between origin and destination 3,27 3,39 3,40 3,75 quality of road infrastructure 3,80 3,97 3,90 4,13 possibility of congestion 3,48 3,66 3,42 3,50 possibility of road accident 3,23 2,71 3,52 3,69 table 3. criteria for route selection – weighted arithmetic mean. figure 5. acceptability of alternative route due to the length of detour (left) and with respect to the prolongation of travel time (right). 53 a. kalašová, s. kubíková, j. kapusta acta polytechnica ctu proceedings more than 2 km and time accessibility would increase in the interval from 6 to 10 minutes. sufficient awareness of drivers concerning road traffic situation is another way how to avoid roads with high intensities, congestions or road sections where a traffic accident occurred. therefore, when planning the transport, it is appropriate to have the actual current traffic information, which can be detected by the driver before or during the trip through information technologies. according to the survey, the most frequently used means of obtaining traffic information is the radio, as can be seen in figure 6. figure 6. information systems used and their share in obtaining traffic information. in the next question, we asked whether the drivers would appreciate intelligent transport systems, which would alert them about the possible dangers and which of the dangerous situations are the most important to them. the survey shows that women consider the information about black ice and fog to be the most important and the least important are for them warnings concerning dead-end streets. men consider the information about traffic accident and black ice to be the most important and the least important are for them warnings about dead-end streets and one-way roads. the evaluation scale was as follows: 0 – irrelevant, 1 – the least significant, 5 – the most important. weighted arithmetic means, which is processed graphically in figure 7, were calculated based on the values obtained. figure 7. evaluation of the importance of warning for driver about dangerous traffic situation. the last part of the questionnaire was devoted to active safety components. it was examined, whether the drivers consider the presence of selected components of active safety to be necessary. active safety components are defined as systems and devices that help to prevent the occurrence of traffic accidents and thus increase the safety of road transport. table 4 shows which systems the respondents consider to be the most important. the evaluation scale was as follows: 0 – irrelevant, 1 – the least significant, 5 – the most important. the weights of importance were evaluated based on the weighted arithmetic mean. an overall analysis of the questionnaire shows that the drivers are open to new possibilities of using intelligent transport systems, especially with regards to the increase of their own safety while travelling by a motor vehicle. 4. conclusion building telematics technologies is expensive. it is therefore not possible to apply them to all roads. however, they should form an essential part of motorways, expressways and first class roads, mainly because of high traffic intensity on these roads. several cities, where it will be necessary to solve growing traffic problems by building intelligent transport systems, were chosen, based on the analysis of traffic – transport processes, which was performed within the implementation of the national system of traffic information in individual regional capitals and in some larger cities. sections of road network that pass through the cities of žilina, martin and ružomberok were examined in this paper. these sections have the highest vehicle intensities and it is therefore necessary to solve the traffic issues through the use of intelligent transport systems. telematics technologies have a positive impact on traffic and its characteristics (intensity, density, speed, etc.) reduction in the number of traffic accidents can be achieved by reducing the intensity on congested road sections. the use of variable message signs to inform drivers about the current traffic situation and possible obstacles that affect the road capacity appears to be a suitable tool for reducing the risk of traffic accidents. intelligent transport systems have a positive effect on psychological well-being of the driver while driving. awareness plays an important role not only in warning about current traffic situation but also in planning the transport before it actually starts. drivers can check road traffic situation thanks to the topical and real-time information. road safety may be improved by reducing the number of traffic accidents and minimize their consequences and thus society can save hundreds of thousands of euros. the main benefit of reducing the number of traffic accidents remains minimization or complete elimination of the negative impacts of traffic accidents on mental and physical aspects of people involved in traffic accidents as well as their relatives. 54 vol. 12/2017 the relation between driver behavior and intelligent transport system ecall 3,54 3,55 4,13 3,94 parking assistant 1,89 2,26 2,63 3,00 cruise control 2,66 2,76 2,85 3,06 stop & go 1,66 1,61 2,67 2,94 automatic system for the detection of congestions 2,86 3,11 3,35 3,88 lane departure 2,56 3,16 3,63 3,81 maintaining safety distance 3,86 2,97 3,23 3,56 traffic signs 2,42 2,37 2,60 3,19 table 4. evaluation of the importance of active safety systems’ application in vehicles. references [1] a. kalašová, j. paľo. dopravné inžinierstvo – organizácia a riadenie. žilina: edis vydavateľstvo žu v žiline, 2003. 162 s., isbn 80-8070-076-1. [2] národný plán sr pre becep 2011-2020, july 2014. [online] available from: http://www.becep.sk/file_download/6/narodny_ plan_sr_pre_becep_2011_2020.pdf. [3] j. ondruš, s. kubíková. interakcia bezpečnosti a inteligentných dopravných systémov. vedecký – recenzovaný online časopis – svet dopravy, july 2014. issn 1338-9629, available from: http: //www.svetdopravy.sk/interakcia-bezpecnosti-a\ -inteligentnych-dopravnych-systemov. [4] centrum dopravního výzkumu. jak lze měřit bezpečnost? [online], available from: http://www.czrso.cz/clanky/ jak-lze-merit-bezpecnost-1-cast. [5] road accident investigation guidelines for road engineers, 2007. available from: http: //www.who.int/roadsafety/news/piarc_manual.pdf. [6] m. sørensen, r. elvik. black spot management and safety analysis of road networks – best practice guidelines and implementation steps. tøi report 919/2007, oslo, july 2014. isbn 978-82-480-0809-5, available from: http: //www.toi.no/getfile.php/publikasjoner/t%d8i% 20rapporter/2007/919-2007/919-2007-nett.pdf. 55 http://www.becep.sk/file_download/6/narodny_plan_sr_pre_becep_2011_2020.pdf http://www.becep.sk/file_download/6/narodny_plan_sr_pre_becep_2011_2020.pdf http://www.svetdopravy.sk/interakcia-bezpecnosti-a\-inteligentnych-dopravnych-systemov http://www.svetdopravy.sk/interakcia-bezpecnosti-a\-inteligentnych-dopravnych-systemov http://www.svetdopravy.sk/interakcia-bezpecnosti-a\-inteligentnych-dopravnych-systemov http://www.czrso.cz/clanky/jak-lze-merit-bezpecnost-1-cast http://www.czrso.cz/clanky/jak-lze-merit-bezpecnost-1-cast http://www.who.int/roadsafety/news/piarc_manual.pdf http://www.who.int/roadsafety/news/piarc_manual.pdf http://www.toi.no/getfile.php/publikasjoner/t%d8i%20rapporter/2007/919-2007/919-2007-nett.pdf http://www.toi.no/getfile.php/publikasjoner/t%d8i%20rapporter/2007/919-2007/919-2007-nett.pdf http://www.toi.no/getfile.php/publikasjoner/t%d8i%20rapporter/2007/919-2007/919-2007-nett.pdf acta polytechnica ctu proceedings 12:50–55, 2017 1 introduction 2 characteristic of the selected section of road network 2.1 measurement of road network safety 3 analysis of perception of intelligent transport systems from the perspective of drivers 4 conclusion references 205 acta polytechnica ctu proceedings 1(1): 205–209, 2014 205 doi: 10.14311/app.2014.01.0205 expected hard x-ray and soft gamma-ray from supernovae keiichi maeda1,2, yukikatsu terada3, aya bamba4 1department of astronomy, kyoto university, japan 2kavli institute for the physics and mathematics of the universe (wpi), university of tokyo, japan 3department of physics, saitama university, japan 4department of physics and mathematics, college of science and engineering, aoyama gakuin university, japan corresponding author: keiichi.maeda@kusastro.kyoto-u.ac.jp abstract high energy emissions from supernovae (sne), originated from newly formed radioactive species, provide direct evidence of nucleosynthesis at sn explosions. however, observational difficulties in the mev range have so far allowed the signal detected only from the extremely nearby core-collapse sn 1987a. no solid detection has been reported for thermonuclear sne ia, despite the importance of the direct confirmation of the formation of 56ni, which is believed to be a key ingredient in their nature as distance indicators. in this paper, we show that the new generation hard x-ray and soft γ-ray instruments, on board astro-h and nustar, are capable of detecting the signal, at least at a pace of once in a few years, opening up this new window for studying sn explosion and nucleosynthesis. keywords: nuclear reaction nucleosynthesis abundances supernovae: general. 1 introduction supernova (sn) explosions trigger (or are triggered by) explosive nucleosynthesis, and they are believed to be main production sites of heavy elements in the universe. the resulting yields are sensitive to explosion mechanism(s), and thus studying nucleosynthesis products is important to uncover the still-debated explosion mechanism. especially important is the production of 56ni – this is the origin of fe (as a result of the radioactive decay chain 56ni → 56co → 56fe), and the decay is believed to provide a source of emissions from (many classes of) sne through thermalization of emitted γ-rays and positrons. in type ia supernovae (sne ia), about half of an exploding white dwarf in mass is processed into 56ni, supporting their huge luminosities as distance indicators. however, the most direct evidence in this scenario is still missing – there has been no solid detection of the decay γ-rays from sne except for sn 1987a (e.g., dotani et al., 1987; sunyaev et al., 1987). especially, no solid detection has been reported for sne ia (see milne et al., 2004 for a review). from a theoretical point of view, studying this high energy emission has been restricted to one-dimensional models (see milne et al., 2004, for a review) despite the importance of multi-dimensional structures of the explosion both in theory and observation (e.g., kasen et al., 2009; maeda et al., 2010a). most previous studies also focused on the emission in the mev range. in this paper, we present our radiation transfer simulations of the high energy emission based on the state-of-the-art sn ia explosion models. we extend our analysis to hard x-ray and soft γ-ray regimes, for which dramatic improvement is expected in the observational sensitivities thanks to new generation observatories like nustar (koglin et al., 2005) or astro-h (takahashi et al., 2010). we predict that these telescopes are capable of detecting the radioactive decay signals from sne ia, at a rate of once in a year or at least once in a few years. we also briefly comment on perspectives for core-collapse sne. 2 expected characteristics we performed radiation transfer simulations (maeda et al. 2012) based on a series of two-dimensional delayed detonation models by kasen et al. (2009). the delayed detonation model is among the most popular scenarios for sne ia, resulting from a near-center ignition of thermonuclear sparks within a chandrasekhar-mass white dwarf (khokhlov, 1991). conditions for the initial triggers have not been clarified from the first principle (e.g., seitenzahl et al., 2013), thus kasen et al. (2009) adopted various conditions (i.e., distribution of the sparks) and produced a range of the ejecta models. in this scenario, different initial conditions can be associated with observed diversities. figure 1 shows examples of the ejecta structure. the model dd2d asym 04 is for bright sne ia (resulting in ∼ 1m� of 56ni), while 205 http://dx.doi.org/10.14311/app.2014.01.0205 keiichi maeda, yukikatsu terada, aya bamba figure 1: examples of the delayed-detonation models (kasen et al., 2009; see also maeda et al., 2010b). the mass fractions of si (left) and 56ni (right) are shown, on a logarithmic scale. the axes are in 10, 000 km s−1. dd2d iso 04 is for fainter ones (∼ 0.4m� of 56ni). generally, this model sequence predicts more asymmetric structure for fainter sne ia (note that the initial condition of model dd2d asym 04 is indeed more asymmetric than dd2d iso 04, but the post-explosion ejecta are less asymmetric). examples of the synthetic spectra are shown in figure 2. the spectra are characterized by the decay lines, compton scattering continuum, and the low energy cut off by the photoelectric absorption. at 20 days, the decay lines from 56ni → 56co (e-folding time of ∼ 8.8 days) are more important than those from 56co→ 56fe (∼ 113 days) as characterized by strong lines in the soft γ-ray range (e.g., the 158 kev line followed in strength by the 270 and 480 kev lines). later on, the strong lines are mostly in the mev range (i.e., the 847 kev line as the strongest) except for the annihilation line. the cut off energy becomes higher as time goes by due to the increasing contribution to the emission from the deeper part where the mean atomic number and photoelectric cross sections are larger. thus, overall the spectra evolve from soft to hard as time goes by. this indicates that follow-up of sne at relatively early phases is important in hard x-ray and soft γ-ray range. the classical 1d model w7 has lower energy cut off than the delayed detonation model sequence, since the w7 model has less extended explosive nucleosynthesis in the surface layer than the delayed detonation model. due to increasing transparency, the emission is sensitive to model variants (including the viewing direction) in the earlier phase, while the mass of 56ni plays a dominant role in the later phase. thus, observation at relatively early phases in (relatively) soft bands can provide unique diagnostics in clarifying the explosion mechanism(s). in the multi-d delayed detonation model sequence, a unique prediction is that faint sne ia should show larger variations in the high energy emission arising from various viewing directions than brighter ones. such prediction can be tested once there are at least a few samples of high energy emission detected for sne ia. another diagnostics using the ‘soft’ bands includes the surface composition analysis from the photoelectric absorption, e.g., the different behavior shown for the w7 model and delayed detonation models. 3 observational perspectives table 1 summarizes expected detectability of extragalactic sne ia at various band passes by a few current and future instruments. while detecting the mev lines from the 56co decay has been challenged in the past, even with spi on board integral and 106 s exposure (roques et al., 2003; see also isern et al., 2013), this is limited to extremely nearby sne ia up to 5 6 mpc (or 8 mpc for extremely bright sne ia). such nearby events are expected only once in a decade. this frustrating situation in the mev range will be improved only when the sensitivity is improved by an order of magnitude, hopefully by proposed new generation observatories like grips (greiner et al., 2012; see also summa et al., 2013). we propose that new generation hard-x and/or soft γ-ray instruments can change the situation. in hard xrays, nustar has been already launched. astro-h is scheduled for launch in 2015, which will be attached with hxi (hard x-ray) and sgd (soft γ-ray). these instruments are expected to have 106 s exposure sensitivities sufficient to reach sne ia at 15 (conservative estimate) or 25 mpc (optimistic estimate) (tab. 1). the ‘line detection’ is more challenging, and we estimate the distance for the 5σ detection of the 158 kev line is ∼ 10 − 15 mpc for model dd2d asym 04 and ∼ 3 − 5 mpc for the other two models shown in table 1. figure 3 shows simulations for expected signals from sne ia at 15 mpc, by convolving the synthetic spectra 206 expected hard x-ray and soft gamma-ray from supernovae 10 10020 50 20010 − 8 10 − 7 10 − 6 10 − 5 10 − 4 no rm al iz ed c ou nt s s k ev energy (kev) dd2d_asym_04_dc2 15mpc 10 10020 50 20010 − 8 10 − 7 10 − 6 10 − 5 10 − 4 no rm al iz ed c ou nt s s k ev energy (kev) w7 15mpc 10 10020 50 20010 − 8 10 − 7 10 − 6 10 − 5 10 − 4 no rm al iz ed c ou nt s s k ev energy (kev) dd2d_iso_04_dc3 15mpc figure 2: detector response simulations for an exposure of 106 seconds for selected models (tab. 1), for hxi (black) and sgd (red) on board astro-h. the model spectra at 20 days after the explosion are used as input, placed at distances of 15 mpc. the sensitivity curves are adopted from kokubun et al. (2010), tajima et al. (2010), and takahashi et al. (2010). note that the photon count is very low in the hxi band for all the models at this distance, thus an apparent detection by hxi (left panel) just comes from the statistical fluctuation. table 1: expected detectability (for an exposure of 106 s centered at the peak date in each band pass). shown here are limiting distance and the expected number of sne ia within the distance (shown in parenthesis). ‘cons’ and ‘opt’ are conservative and optimistic estimates, respectively. see maeda et al. (2012) for details. dd2d asym 04 w7 dd2d iso 04 m(56ni)/m� 1.02 0.64 0.42 band (kev) instrument mpc (sne year−1) 60–80 hxi 13.9 (0.43) 17.7 (0.96) 10.5 (0.09) nustar (cons.) 13.0 (0.43) 16.5 (0.70) 9.7 (0.09) nustar (opt.) 18.4 (1.13) 23.3 (2.52) 13.8 (0.43) 158 spi 4.6 (<0.09) 2.9 (<0.09) 2.3 (<0.09) sgd (cons.) 22.2 (2.09) 14.2 (0.43) 11.4 (0.09) sgd (opt.) 38.5 (6.70) 24.6 (2.96) 19.7 (1.57) 200–460 spi 3.7 (<0.09) 2.7 (<0.09) 2.3 (<0.09) sgd (cons.) 11.6 (0.09) 8.6 (0.09) 7.1 (0.09) sgd (opt.) 20.2 (1.74) 14.8 (0.43) 12.3 (0.26) 812 spi 4.3 (<0.09) 2.6 (<0.09) 2.0 (<0.09) grips 16.8 (0.87) 10.0 (0.09) 7.6 (0.09) 847 spi 7.7 (0.09) 5.4 (<0.09) 4.6 (<0.09) grips 29.8 (4.52) 21.0 (2.00) 18.0 (1.04) and designed sensitivity curves of hxi and sgd (here the adopted sensitivity curve corresponds to our ‘optimistic’ case). in 2011-2012, 6 sne ia were discovered within ∼ 20 mpc, 3 of which were within ∼ 15 mpc (from the asiago sn catalog; barbon et al., 1999). most of these were discovered soon after the explosion, and especially the nearest ones were all discovered within a week after the explosion – thus, too follow-up at the hard x and soft γ-ray peak (2 3 weeks after the explosion) is feasible. with 106 s exposure, we predict that a few (optimistic) or one (conservative) sne ia per year are reachable by astro-h. 207 keiichi maeda, yukikatsu terada, aya bamba 100 1000 1e-8 1e-7 1e-6 sgd hxi (b) 60 day fl ux [c m 2 s 1 k ev 1 ] energy (kev) 100 1000 1e-8 1e-7 1e-6 sgd hxi (a) 20 day fl ux [c m 2 s 1 k ev 1 figure 3: examples of synthetic spectra at (a) 20 days and (b) 60 days after the explosion. shown here are angleaveraged spectra for models dd2d asym 04 (red line), w7 (gray; nomoto et al., 1984), and dd2d iso 04 (dark blue) (at 10 mpc). the angle-dependent spectra seen from two opposite directions are shown for dd2d iso 04 (green and cyan) at 20 days. at 60 days the angle dependence is small. the angle dependence is small for dd2d asym 04 at both epochs. sensitivity curves for an exposure with 106 seconds of hxi and sgd on board astro-h (tajima et al., 2010; takahashi et al., 2010) are shown by black lines. 4 discussion and conclusions according to our simulations of radioactive decay signals from sne ia, the new generation hard x-ray and soft γ-ray observatories (either nustar or astro-h) are expected to be capable of detecting these signals from sne ia up to ∼ 20 mpc with 106 s exposure. this will hopefully lead to nearly annual detections, dramatically changing the field. we thus propose follow-up of nearby sne ia by these telescopes in a too mode. with a standard set up with a few 105 s exposure, the detection will be limited to extremely nearby objects (i.e., up to ∼8 12 mpc for sne ia with average brightness), but still there is a good chance of first solid detection of the signal from sne ia. once detected, it will provide various diagnostics on explosive nucleosynthesis and explosion mechanisms, and here a combination of hard x-ray and soft γ-ray will be essential. a similar argument applies for core-collapse sne. by combining results from similar simulations for corecollapse sne (maeda, 2006) and those obtained for sne ia (maeda et al., 2012), we find the following. sne iip (an explosion of a red supergiant) is not a promising target in the soft bands, since the thick h envelope is still opaque in the early phase where the 56ni decay can provide the strong emission in these band passes. among different types of core-collapse sne, sne iib/ib/ic (an explosion of a he or c+o star) are most promising. we estimate that the peak date in the high energy emission will be similar to (or a bit delayed than) that of sne ia (i.e., 2 3 weeks since the explosion). the smaller amount of 56ni here (typically ∼ 0.1m�), taking into account the delayed peak date, results in the expected horizon as 5 − 8 mpc (conservative and optimistic). such nearby objects are rare, but expected to be discovered at a rate of a few in a decade according to the past statistics. acknowledgement km thanks franco giovannelli and the organizers of frascati workshop 2013 for creating the friendly and stimulating atmosphere. the work by km has been supported by wpi initiative, mext, japan. the authors acknowledge financial support by grant-in-aid for scientific research from mext (22684012, 23340055, 23740141). references [1] barbon, r., et al.: 1999, a&as, 139, 531 [2] dotani, t., et al.: 1987, nature, 330, 230 doi:10.1038/330230a0 208 http://dx.doi.org/10.1038/330230a0 expected hard x-ray and soft gamma-ray from supernovae [3] greiner, j., et al.: 2012, exp. astron., 34, 551 doi:10.1007/s10686-011-9255-0 [4] isern, j., et al.: 2013, a&a, 552, 97 [5] kasen, d., röpke, f.k., woosley, s.e.: 2009, nature, 460, 869 doi:10.1038/nature08256 [6] koglin, j.e., et al.: 2005, proc. spie, 5900, 266 [7] kokubun, m., et al.: 2010, proc. spie, 7732, 33 doi:10.1117/12.857933 [8] khokhlov, a.: 1991, a&a, 245, 114 [9] maeda, k.: 2006, apj, 644, 385 [10] maeda, k., et al.: 2010a, nature, 466, 82 doi:10.1038/nature09122 [11] maeda, k., et al.: 2010b, apj, 712, 624 doi:10.1088/0004-637x/712/1/624 [12] maeda, k., et al.: 2012, apj, 760, 54 doi:10.1088/0004-637x/760/1/54 [13] milne, p.a., et al.: 2004, apj, 613, 1101 doi:10.1086/423235 [14] nomoto, k., thielemann, f.-k., yokoi, k.: 1984, apj, 286, 644 [15] roques, j.p., et al.: 2003, a&a, 411, l91 [16] seitenzahl, i.r., et al.: 2013, mnras, 429, 1156 [17] summa, a., et al.: 2013, a&a, 554, 67 [18] sunyaev, r.a., et al.: 1987, nature, 330, 227 doi:10.1038/330227a0 [19] tajima, t., et al.: 2010, proc. spie, 7732, 34 [20] takahashi, t., et al.: 2010, proc. spie., 7732, 27 209 http://dx.doi.org/10.1007/s10686-011-9255-0 http://dx.doi.org/10.1038/nature08256 http://dx.doi.org/10.1117/12.857933 http://dx.doi.org/10.1038/nature09122 http://dx.doi.org/10.1088/0004-637x/712/1/624 http://dx.doi.org/10.1088/0004-637x/760/1/54 http://dx.doi.org/10.1086/423235 http://dx.doi.org/10.1038/330227a0 introduction expected characteristics observational perspectives discussion and conclusions 325 acta polytechnica ctu proceedings 2(1): 325–327, 2015 325 doi: 10.14311/app.2015.02.0325 golden era of cataclysmic variables and related objects ii: concluding remarks r. hudec1,2 1astronomical institute, academy of sciences of the czech republic, cz-25165 ondřejov, czech republic 2czech technical university in prague, faculty of electrical engineering, prague, czech republic corresponding author: rene.hudec@asu.cas.cz abstract the cataclysmic variables continue to represent important part of modern astrophysics, as demonstrated, already second time, by the productive and successful conference golden era of cataclysmic variables and related objects ii held on mondello (palermo) in september 2013. keywords: stars variable stars cataclysmic variables. 1 introduction cataclysmic variables (cvs) belong to important targets of modern (and multispectral) astrophysics, as they represent in many aspects the true astrophysical laboratory, in which various physical processes and models can be observed, investigated, simulated, and tested. they even may play a significant role in the generation of galactic x-ray background, a consequence of surprisingly large fraction of cvs in hard x-ray sources detected by esa satellite integral. despite of large theoretical and experimental progress in the last years there are still numerous important questions to be answered. even for well known and studied objects such as ss cyg or ae aqr, there are still different opinions in the astronomical community about their nature and involved physical processes. the cv field is quite complex and interdisciplinary, and it is obvious that only such complex approach has a chance to deliver reliable answers to our questions. many important questions regarding investigation of cvs and related objects were addressed in mondello, not only during scientific sessions, but also during numerous discussions among participants (see figs. 2 to 11). there were plenty opportunities for such discussions during coffee breaks, breakfasts, lunches and dinners, and also during various social activities, all this enjoying the pleasant atmosphere of sicily (including delicious food, coffee, and wine). 2 few subjective comments the cataclysmic variables conference in mondello (palermo) represents, in my opinion, another successful workshop confirming prof. franco giovanelli/vulcano theorem (adopted from his famous vulcano frascati workshops), namely that one can make serious science even keeping smiling. as already confirmed before by long series of vulcano frascati (and analogous) workshops, the key for successful and highly productive workshop is as follows: nice environment, dining and staying together, enough (and good) wine (or beer in countries like czech republic). and great participants and speakers, of course, and last but not least experienced conference organizers. there was really wide international participation of both field leaders as well as young scientists in our conference many of them have got the possibility to meet the famous senior scientists they know from the literature for the first time. personally, i have much appreciated the high quality of most of invited and review talks. in my opinion, this is nowadays not very common as we face the problem of declining quality of such talks at numerous other conferences. there were nice carefully prepared reviews by various key speakers covering both theory as well as experiment. these lectures have illustrated and demonstrated the great progress both in theory as well as observation/experiment of cvs (although there was lively discussion this time whether we indeed have enough new observations or not) and related objects over last years. in addition to that, some new and mostly detailed observations on particular cvs were presented and discussed, mostly by young scientific fellows. as for the previous cv conference, the frequent conclusion of numerous speakers was as follows: we need more and better data, as well as better statistics. in addition to that, prospects of some of the new future 325 http://dx.doi.org/10.14311/app.2015.02.0325 r. hudec experiments/projects still need to be better formulated. in general, there is a need for better monitoring, multilambda observations, and in this direction robotic telescopes (rts, e.g. gloria) and novel space experiments may help, as also proposed and discussed during the workshop. 3 selected pictures in my opinion, the following selected pictures taken during the workshop may much better illustrate the scope, atmosphere, and success of the conference better than any further words. the authors of these pictures are rene hudec (21 pictures) and nataly katysheva (6 pictures). figure 1: the japanese delegation wearing traditional kimono during the welcome reception (left). the delicious italian coffee served during the coffee breaks at the hotel terrace (right). figure 2: meeting colleagues and having discussions represented, apart from scientific sessions, a key point of the workshop. figure 3: scientific talks: the discipline of conference participants in attending was great. figure 4: sometimes, the discussion among participants was quite lively figure 5: the main conference organizers and key persons at action (left) and russian delegation enjoying the delicious wine of sicily at the dinner (right). figure 6: the workshop artistic performance (left) and the beautiful sunset observed from the conference hotel terace (right). figure 7: are these conference participants both showing their estimate of the accretion disk radius? 326 golden era of cataclysmic variables and related objects ii: concluding remarks figure 8: the delicious desserts served after the meals surely contributed to the workshop success as well. figure 9: some (not all) conference participants enjoyed mare and swimming pool bar. figure 10: sometimes the discussions continued either at hotel bar, or at dining. figure 11: these two pictures surely belongs to the workshop highlights. figure 12: the etruscan wine tasting and departure for the conference trip. figure 13: the conference trip to segesta. 4 conclusions the international workshop golden era of cataclysmic variables and related objects ii, apart of presenting and discussing numerous contributions, promoted in an effective way further contacts among international cvs community. in my opinion, we definitely need this type of workshop, probably every two years. if compared to the situation two years ago when various future meeting sites were proposed and discussed, i have got feeling that this time, the opinion of majority of participants was quite unique: franco giovanelli and his team and palermo/sicily remains to be the best option. to conclude, lets hope to meet again in palermo in 2015 for at least so productive cv workshop as was the one in 2013. acknowledgement our thanks are due to the conference organizers, speakers and participants, restaurant and hotel staff, artists, and to all those not mentioned above but who contributed to the success of our conference as well. the authors of pictures in this contribution are rene hudec and nataly katysheva. my personal involvement in cv astrophysics (and consequently in the involvement in the cv mondello (palermo) conference) was supported by grants 13-39464j and 13-33324s by gacr. 327 introduction few subjective comments selected pictures conclusions acta polytechnica ctu proceedings doi:10.14311/app.2017.8.0017 acta polytechnica ctu proceedings 8:17–19, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app microscopic evaluation of the quality of dental replacement františka pešlováa,b,∗, daniela koštialikováa, richard veselýc, andrej dubeca, maxim puchninb a faculty of industrial technology in púchov, alexander dubček university of trenčín, i. krasku 491/30, púchov, slovakia b czech technical university in prague, faculty of mechanical engineering, karlovo nám. 13, 121 32 prague 2, czech republic c czech technical university in prague, faculty of mechanical engineering, department of enterprise management and economics, karlovo nám. 13, 121 32 prague 2, czech republic ∗ corresponding author: abstract. the permanent tooth replacements including metal-ceramic crowns are a convenient solution for the renewing of the original function of the whole set of teeth as well as of the natural appearance. development and preparation of suitable tooth replacement presents a real challenge for dental engineers as the replacement has to meet all the conditions and requirements of the dental medicine as well as patient's needs and wishes. the preparation of the metal-ceramic crown is a sophisticated process and the dental engineer has to prepare always a unique replacement on demand. in dental medicine there is a wide spectrum of inorganic and organic materials used for manufacturing of dental replacements. each of the material has specific properties leading to distinct applications. besides the material properties, the attention has to be paid to the aesthetic function and biocompatibility of the material to ensure the complete restoration of the whole set of teeth. keywords: metal-ceramic crown, dental replacement, microstructure. 1. introduction the presented paper focuses on investigation of the randomly selected tooth replacements which were no longer suitable to be used in mouth cavity in a satisfying and predetermined way. from the aspect of materials engineering, the mentioned dental condition or phenomenon is based on the critical state of the dental replacement and it can be the cause of the occurrence of many other critical states. the given critical states lead to degradation of tooth replacements and it can even end in tooth replacement's fracture causing the functional and aesthetic defect as well. [1–4]. the main scope of the performed microscopic observations was to identify the initiation stimulus for rupture of a tooth replacement – the child patient's crown, which was used as tooth replacement after the injury. in relation to the given metal-ceramic crown (of the type seen in the 1), there was the rupture of the ceramic layer and its subsequent delaminating. the crown was supplied without any specific information (producer, chemical composition, life duration, etc.) 2. materials the metal-ceramic crown is a complex composite material with chemical composition given in the table 1 and 2. the identification of the phase composition was evaluated using scanning electron microscope (sem) jsm-7600f (jeol, jp) with energy dispersive spectroscopy (eds) x-max 50 mm2 (oxford instruments, gb) was used.the metallographic preparation of samples was performed in a standard and normalized way in order to carry out the microscopic investigation of the microstructure of used materials in their crosssections (fig. 2 ). metallographic preparation was made in standard way – selection of the material from the defect and from the intact location followed by grinding, polishing and etching. according to the fact mentioned herein before, the precise investigation of ceramics and metal microstructure were carried out. the detailed images (fig. 3) revealed the sites with the altered roughness. the occurrence of cavities was identified in sites where the metal was in contact with the ceramic layer and it led to the rupture of the ceramic layer. based on the microscopic observations, the penetration of ceramic material into the irregular areas of metal originating from the manufacturing process has been identified. that led to the deteriorative effect in relation to the metal – ceramics contact (fig. 4). the microscopic observation of the metal alloy quality revealed that the low-quality heterogeneous metal alloy was used for manufacturing of selected metalceramic crown which caused defects in contact layer between metal and ceramic material during manufacturing. besides the distribution of individual phases, 17 http://dx.doi.org/10.14311/app.2017.8.0017 http://ojs.cvut.cz/ojs/index.php/app f. pešlová, d. koštialiková, r. veselý et al. acta polytechnica ctu proceedings weight % o si sn k co al cr zr ti na sample nr.1 – ceramic 34,2 14,8 8,5 6,4 6,3 5,2 2,9 2,7 2,6 2,2 table 1. chemical composition of the ceramic part of the crown obtained by edx analysis weight % co cr w o si v s al k sample nr.1 – metal 57,2 22,7 6,9 2,1 1,4 0,6 0,5 0,5 0,3 table 2. chemical composition of the metal part of the crown obtained by edx analysis figure 1. metal-ceramic crown, detail. figure 2. metal-ceramic crown detailed image. figure 3. rupture in the site of the metal-ceramic material contact. figure 4. penetration of ceramic material. the low quality of materials was confirmed by chemical composition. the character of the microstructure (fig. 5) exhibits the imperfect primary crystallisation of co-cr alloy with the occurrence of undesired phases. [5–8]. 3. conclusion based on the microscopic evaluation, it can be concluded that individual microstructure of the metal alloy and contact layer between metal alloy and ceramic material indicates that evaluated metal alloy was not suitable for manufacturing of tooth replacement. the most significant evidence was obtained from the contact layer between metal and ceramic material where cavities were observed. the cavities are a source of oxidation which can lead to further degradation of the metal alloy. with the reference to the obtained results, we can come to the conclusion that the low quality materials used for manufacturing process of the metal-ceramic crown had caused defects that led to the degradation of the replacement. moreover, there was a danger of damaging other teeth as well as danger of ingestion or inhaling parts of metal or ceramic material. the work is showing an example that may occur in practice thus a regular inspections of patients tooth replacements are recommended. 4. results regulatory requirements for control samples preparation during the manufacturing of the replacements should be initiated despite the fact that preparation of samples for potential defect detection control may not be economical manufacturing process even though it is in the best interest of the patients. 18 vol. 8/2017 microscopic evaluation of the quality of dental replacement figure 5. microstructure of co-cr alloy . acknowledgements this work was supported by the slovak grant agency kega 006tnuad-4/2014, ministry of education youth and sport of the czech republic program npu1, project no lo127 references [1] y. wang. bioadaptability: an innovative concept for biomaterials. journal of materials science & technology 32(9):801 – 809, 2016. bioadaptation of biomaterials, doi:http://dx.doi.org/10.1016/j.jmst.2016.08.002. [2] h. hubálková, j. krňoulová. materiály a technologie v protetickém zubním lékařství. galén, praha, 2009. [3] r. g. craig, j. m. powers. restorative dental materials. mosby, st. louis, missouri, 11th edn., 2002. [4] h. hubálková, j. charvát, t. dostálová. faktory ovplyvňujúce životnosť fixnej zubnej náhrady. progresdent, 5th edn., 2004. [5] j. giacchi, c. morando, o. fornaro, h. palacio. microstructural characterization of as-cast biocompatible co-cr-mo alloys. materials characterization 62(1):53 – 61, 2011. doi:http://dx.doi.org/10.1016/j.matchar.2010.10.011. [6] j. giacchi, o. fornaro, h. palacio. microstructural evolution during solution treatment of co-cr-mo-c biocompatible alloys. materials characterization 68:49 – 57, 2012. doi:http://dx.doi.org/10.1016/j.matchar.2012.03.006. [7] j. e. lemons, f. misch-dietsch, m. s. mccracken. biomaterial for dental implants. in dental implant prosthetics, chap. 4, pp. 66–94. mosby, st. louis, missouri, 2015. [8] j. b. suzuki, d. lynn, l. d. terracciano-mortilla, c. e. misch. maintenance of dental implants. in dental implant prosthetics, chap. 34, pp. 964–981. mosby, st. louis, missouri, 2015. 19 http://dx.doi.org/http://dx.doi.org/10.1016/j.jmst.2016.08.002 http://dx.doi.org/http://dx.doi.org/10.1016/j.matchar.2010.10.011 http://dx.doi.org/http://dx.doi.org/10.1016/j.matchar.2012.03.006 acta polytechnica ctu proceedings 8:17–19, 2017 1 introduction 2 materials 3 conclusion 4 results acknowledgements references acta polytechnica ctu proceedings doi:10.14311/app.2017.12.0104 acta polytechnica ctu proceedings 12:104–107, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app the future of passenger air transport – very large aircraft and out key human factors affecting the operation and safety of passenger air transport petra skolilová ctu in prague, faculty of transportation sciences, czech republic correspondence: skolilova@fd.cvut.cz abstract. the article outlines some human factors affecting the operation and safety of passenger air transport given the massive increase in the use of the vla. decrease of the impact of the co2 world emissions is one of the key goals for the new aircraft design. the main wave is going to reduce the burned fuel. therefore, the eco-efficiency engines combined with reasonable economic operation of the aircraft are very important from an aviation perspective. the prediction for the year 2030 says that about 90% of people, which will use long-haul flights to fly between big cities. so, the a380 was designed exactly for this time period, with a focus on the right capacity, right operating cost and right fuel burn per seat. there is no aircraft today with better fuel burn combined with eco-efficiency per seat, than the a380. the very large aircrafts (vlas) are the future of the commercial passenger aviation. operating cost versus safety or co2 emissions versus increasing automation inside the new generation aircraft. almost 80% of the world aircraft accidents are caused by human error based on wrong action, reaction or final decision of pilots, the catastrophic failures of aircraft systems, or air traffic control errors are not so frequent. so, we are at the beginning of a new age in passenger aviation and the role of the human factor is more important than ever. keywords: vla, human factors, air transport, air traffic, security. 1. introduction the study of human factors deals with people’s interaction with their environments. in the case of general aviation, this is the study of pilot performance with influence on the emotions, stress, fatigue or design of cockpits or interaction with crewmembers, air traffic control personnel and others. fatigue is an expected aspect of life and there is a very thin border between normal daily fatigue (for example fatigue from lack of sleep) and the tough fatigue from continuous stress. typically, there are no significant marks or consequences. but the aftermath in general aviation environment can be disastrous[1]. 1.1. introduction of the air traffic markets situation aviation mega-cities (amcs) are the new phenomenon for the long-haul market. for long-haul flights we are rating the traffic over 2,000 nautical miles. more than 40% of all long-haul passengers are beginning or ending, at amcs and another 20% are between these 40 amcs. more than another 40 cities have a potential to grow to amcs. by the gmf of airbus, the a380 is the choice number one for these markets. the current markets situation is represented figure 1. the wide-body aircraft is a very important aspect of the aircraft market as well. these aircraft types are more focused on the routes for amcs than to the secondary cities. this is the right market opportunity for the highly efficient new a350xwb as well as the a330neo by the airbus. 1.2. very large aircraft according to airbus statistics before the vlas age, one million passengers per month were served by 200 aircrafts per day. but today, it is only 100 vla aircrafts connecting the world’s major hub. the passengers prefer to fly on a vla due to the high travel comfort which only the vla aircraft can provide. one of the most comfortable seating configurations is the 407 pax (passengers) on board configuration. but also, the maximum capacity of 853 seats are a highly desired option for airlines, which means they have the flexibility to mix comfort with revenue and cost per seat. but today, a typical configuration of an a380 is between 500-520 seats in three or four traveling class configurations. the capacity flexibility is one of the best airline tools how to optimize the right capacity at the right time between mature and expanding markets and their reaction you can read from figure 2[2]. we can find three key reasons why the vlas aircraft are the future of aviation: a) solution to sky congestion: reducing the number of aircrafts needed for transport of the ever-growing air passenger volume; b) solution to the changing demand at different times of the day; c) solution to overcrowded slots at the megacities airports. the standard solution, which is often implemented 104 http://dx.doi.org/10.14311/app.2017.12.0104 http://ojs.cvut.cz/ojs/index.php/app vol. 12/2017 the future of passenger air transport – very large aircraft figure 1. concentration of flights in long-haul markets [source: oag, airbus]. figure 2. new deliveries of vla by region [source: oag, airbus]. 105 petra skolilová acta polytechnica ctu proceedings on routes via the a380, is operating the a380 during peak hours and other aircraft types at non-peak hours during the day on the same routes. in fact, 50% of airports-pairs served by the a380 have another aircraft type in operation also. for the airlines it means to target the right capacity at the right time during the day, for example a combination of the a380 and a350xwb aircraft. the main markets for the vla are the long-haul markets between amcs. in these days they are mainly on the asia/pacific area, where more than 25% flights are served by the a380[2–4]. "from today until 2033, we forecast the demand for nearly 1,230 vla globally. the two largest markets are asia-pacific and the middle east. asia-pacific will represent 47% of the demand for vla over the next 20 years which can be clearly seen by the large number of vla today flying to from and within asiapacific followed by the middle east which today has the largest fleet and largest backlog"[2]. by the gmf prediction we can await an annual growth of the passenger air traffic around 4.7% and it will assist approximately 30,555 passengers’ aircraft during next 20 years. "this demand represents $4.4 trillion at book value over the next 20 years. of this demand for passenger aircraft, 40% will be for the replacement of ageing, less fuel efficient aircraft and 60% of the demand will be for growth"[3]. 2. human factors training in aviation safety means different things to different people. to the traveling public, the term ’safety’ means, at its most fundamental level, that we want to reach our destinations without getting hurt. since people do get hurt on occasion, it is logical to conclude that we are willing to accept some risk in traveling. whether consciously or subconsciously, we know that there is some chance, albeit a minute one, that we could be hurt or killed while traveling. today we average about 50 accidents in commercial airlines each year, but it means that the odds of any one flight being your last one are remote ( 1 to 4,9 million ) and given that more people are killed or injured in automobile accidents (approximately 44,000 deaths per year), ’safe’ is a reasonable word to apply to commercial aviation[5]. one of the first airlines to accept the human factors training was continental airlines. they accepted the existing format and settled the special training called cockpit resource management, evolved into their original training initially titled "crew coordination concepts", and later changed to "maintenance resource management"[6]. it covers communications with pilots, pilots with cabin crewmembers, labor with management, and companies with the government. the icao (international civil aviation organization) is a specialized agency of the united nations, which codifies the principles and techniques that aviation has developed and implemented a special human factors training called sms program: safety management system. the definition of sms: "a dynamic risk management system based on quality management system (qms) principles in a structure scaled appropriately to the operational risk, applied in a safety culture environment." 2.1. human reliability analysis (hra) it is well-established that the largest contribution to the probability of system failure in complex systems is human error. a risk assessment method of any value in aviation must consider human interactions and errors on system reliability. hra models human behavior to better understand human interactions with the rest of the system. a popular method used for human performance reliability prediction is the technique for human error rate prediction (therp). therp are model with five steps: (1.) define the system or process. (2.) identify and enumerate all human operations performed and their relationships to the system. (3.) predict error rates for each human operation. (4.) determine the effect of human error on the system. (5.) make changes that will reduce the system failure rate. pra has been used in chemical, transport, energy, aerospace and military. the first step in an hra is a study to identify the hazards and their impact on the scale. the scale is uses fault trees (ft). the hazards are assigned probabilities, which are propagated up the tree to establish the probability of the undesired top hazards. in practice, it means that the phase of mapping the hazards and human failures is followed by a practical modeling scenario with deductive logic and probabilistic tools called fault trees (ft). the ft are composed of three levels: the top level called type of accident which defines the accident scenario, the middle level are the intermediate failures causing the top level and the basic level are the failures that cause the top level to occur. developing the scenario is a highly sophisticated method with extreme dependency on source data of the model and good subject knowledge. it could be supported by probabilistic software tools. 3. conclusion in these days, more than 300 airbus a-380 are in service operating under the flags of 13 carriers: singapore airlines, emirates, qantas, air france, lufthansa, korean air, china southern airlines, malaysia airlines, thai airways international, british airways, asiana airlines, qatar airways and etihad airways using airports all over the world. one part of responsibility for passengers’ security is on airport management, how to manage the airports runways, taxiways, gate areas 106 vol. 12/2017 the future of passenger air transport – very large aircraft and terminals to accommodate this large and heavy aircraft and more than 700 pax per flight. what has resulted has been a relatively seamless, trouble-free adaptation on the part of airports, which reflects the results of thoughtful planning and analysis. the other part is the human factor. commercial air carriers continue to restructure. the world’s economic downturn beginning in 2008 forced many air carriers out of business and other to consolidate. as a result, air traffic management has had to, and will continue to, become more flexible in its contractual obligations with air carriers, their aeronautical revenue structures, and increasingly the use of their facilities. in the past, aviation safety improvements were characterized by a fly-crash-fix-fly approach. sometimes the causes would be weather-related or a mechanical failure, but more often the causes would be determined to be human factor error – usually the pilot. today we realize that it is much more productive to engineer a system in which causes of failure have been prevented. as one might imagine, there are many elements to this engineering effort. the understanding of hazard identification, risk management, system theory, human factors engineering, organizational culture, quality engineering and management, quantitative methods and decision theory must have a pillar in aviation development. the requirement for vlas will grow with the world’s network and as more people have the ability to fly. by 2032, this demand will result in a need for more than 1,300 vlas. given the projected growth in asia-pacific, both economic and air passenger traffic growth, the region’s demographics and urbanization trends, it is unsurprising that the region’s airlines will take 47% of these aircraft over the next 20 years. the middle east will be the second largest region in terms of demand for vlas, at 26%. this can be seen today in the size of the backlog of a380s within middle eastern carriers[3]. references [1] s. young. airport: planning & management 6th edition. mcgraw-hill companies, inc., 2011. [2] a. 2015. airbus. [online], přístup získán may 2015. [3] iata. the international air transport association. [online]. available: http://www.iata.org/about/pages/index.aspx. accessed mar 2015. [4] wttc. world travel & tourism council. [online]. available: www.wttc.org. přístup získán mar 2015. [5] the economist group. [online]. available: http://www.eiu.com/home.aspx. přístup získán apr 2015. [6] r. stanley, r. trollip. human factors for general aviation. jeppesen sanderson, 2011. 107 http://www.iata.org/about/pages/index.aspx www.wttc.org http://www.eiu.com/home.aspx acta polytechnica ctu proceedings 12:104–107, 2017 1 introduction 1.1 introduction of the air traffic markets situation 1.2 very large aircraft 2 human factors training in aviation 2.1 human reliability analysis (hra) 3 conclusion references acta polytechnica ctu proceedings doi:10.14311/app.2017.10.0048 acta polytechnica ctu proceedings 10:48–51, 2017 © czech technical university in prague, 2017 available online at http://ojs.cvut.cz/ojs/index.php/app shear strength of soils from the dobkovičky landslide in the central bohemian uplands determinated by laboratory tests jakub roháča,b,∗, petr kyclb, jan boháča, david mašína a charles university, faculty of science, albertov 6, prague b czech geological survey, klárov 3, prague ∗ corresponding author: jakub.rohac@geology.cz abstract. the aim of this paper is to evaluate soil shear strength from the dobkovičky landslide. the landslide was activated on june 6, 2013 after heavy rains and the d8 motorway, which was under construction at the time, was damaged. the laboratory tests were carried out on two types of soils, clay and tuff, both from the surface of the rupture. critical and residual friction angles were evaluated on both types of soils. keywords: laboratory tests, the dobkovičky landslide, shear strength. 1. introduction the plans for a highway connecting prague with dresden have been debated since the 1930s. construction of the first 4.2 km of the 92 km long d8 motorway began with section 0806 řehlovice ústí nad labem nearly 50 years later in 1984. the construction of the last remaining 16.2 km in section 0805 lovosice řehlovice was launched in 2007. this section crossed the central bohemian uplands, which represent the most geologically complex and problematic part of the motorway, in particular due to the presence of a large area of dormant and abandoned landslides known as “prackovice landslides” intersected by the motorway. on friday, june 7, 2013 the works were interrupted and the motorway under construction was damaged when heavy rains triggered a landslide near the village of dobkovičky (km 56.3-56.5). the damage was not restricted only to the motorway but also affected the single-track railway connecting lovosice with teplice between the stations dobkovičky and radejčín. the railway track was completely destroyed in the length of 200 m, including a 6 m high embankment. 2. dobkovičky landslide dobkovičky landslide (fig. 1) was activated in the well-mapped landslide area of prackovice, which is characterized by landslides in its geological history. the whole area from the river labe up to the railway embankment is covered by morphologically visible landslides. on june 3, 2013, the first cracks were observed in the area of dobkovičky quarry after 4 days of heavy rains. the dobkovičky landslide was activated in the evening of june 6, 2013. 2.1. landslide description the planar surface of the rupture was detected at a depth of 4-6.5 m below ground level by an engineeringgeological survey provided by the company az consult figure 1. picture of the landslide after collapse (summer 2013). [1]. the length was 470 meters and width was 200 meters. the maximum length of the movement in the center of the landslide was 49 m and the maximum speed of the movement was 1 meter per hour on june 8 [2]. 2.2. geology and hydrogeology the surface of the rupture of dobkovičky landslide consists of siltstone, altered basalt, tuff and anthropogenic material. the anthropogenic material is located in the center of the landslide in the form of a railway embankment and on the top of the landslide in the form of a dump of material from dobkovičky quarry. weathered chalky siltstone (clayey character, r6) represented the slip surface from the toe to the railway line as documented in the minor scarp and in the place of the railway embankment. basalt (r4) was 48 http://dx.doi.org/10.14311/app.2017.10.0048 http://ojs.cvut.cz/ojs/index.php/app vol. 10/2017 shear strenght of soils from the dobkovičky landslide figure 2. map of the landslide with sampling points. type sample depth [m] wl wp ip kts hv-p220 8.3m 59.3 24.8 34.5 kts1 hv-p212 2.3m 62.5 25.5 37 tf ig 208 6.5m 87.1 52.2 34.9 table 1. index properties documented above the railway embankment up to the main scarp. neogene tuff had a sandy clay character with pieces of coal. it had an irregular representation in the surface of the rupture. the main source of groundwater is quaternary debris. the stratum of fresh and weathered siltstone is considered as a hydrogeological insulator [3]. the general groundwater flow direction is from north-west to south-east. hydrogeology of dobkovičky quarry is characterized by fissured permeability, it can be assumed that most of the rainwater is drained through the fissures to the top of the impermeable siltstones and drained to the slope under the quarry. 3. sample description the laboratory tests were carried out on two types of soils, clay and tuff, both from the slip surface. samples were taken during the engineering-geological research in 2014 and 2015. there are 3 main ig types of material: kts1-cretaceous silt stone, olive-colored (borehole hv-p 212), kts-cretaceous siltstone, bluegray colored (borehole hv-p 220), and tf -tertiary tuff, yellow colored (borehole ig 208) [1]. sampling points are labeled on fig. 2. the grading curves of the three main ig types are shown in fig. 3. index properties are described in tab. 1, where wl is the liquid limit, wp is the plastic limit and ip is the plasticity index. 4. sample preparation and test procedures all of the laboratory tests were carried out in the laboratory of soil mechanic at the faculty of science. critical parameters were evaluated in a conventional triaxial apparatus and in a shearbox. residual parameters were evaluated in a ring shear apparatus. all of the laboratory tests were carried out on reconstituted soils the material was thoroughly mixed with distilled water until a homogeneous slurry was obtained. the final water content of the slurry was approximately 1.5 times higher than the liquid limit of the material. the material was then sieved through a 2 mm mesh sieve. 4.1. triaxial test ciup triaxial test (consolidated isotropic undrained with pore pressure measurement). the slurry was poured carefully into a consolidometer and consolidated to a vertical stress of approximately 80 kpa. the load was applied with increments of 10 kpa every day to prevent squeezing up the sides of the piston. after two weeks, the sample was extruded and its ends were trimmed to the correct length of 78 mm, the diameter was 38 mm. the sample was measured and the mass of the sample was determined. then the sample was placed into the triaxial cell on a base pedestal. radial drains were used for all of the samples to reduce the duration of the tests. top drainage was not used. the samples were isotropically consolidated and sheared in an undrained condition with pore pressure measurements. 4.2. shear box test tests were carried out on reconstituted slurry, which was consolidated to a vertical stress of 60 kpa, 100 kpa and 150 kpa. the speed of shear was lower than 0.0013 mm/min to ensure drained conditions. 4.3. ring shear test a bromhead ring shear apparatus was used for evaluation of the residual shear strength. the test was carried out, similarly to the previous apparatus, on reconstituted soils. slurry was consolidated to a vertical stress of 30 kpa, 50 kpa and 70 kpa. the speed of shear was lower than 0.023 mm/min. 5. results table 2 shows the results, the types of tests and the used stresses. eighteen laboratory test were carried out for evaluation of the shear strength of the soils from the dobkovičky landslide. nine of them were ciup (consolidated isotropic undrained with pore pressure measurement) triaxial tests, three were shear box tests and six were ring shear tests. the results of the three selected tests are shown in fig. 4. the shear parameters of the tuff are slightly higher than the clays. the residual parameters are approximately 49 j. roháč, p. kycl, j. boháč, d. mašín acta polytechnica ctu proceedings figure 3. grading curves of the three main ig types of soils, after [4] table 2. results of shear strength tests 1 2 of the critical parameters of the same sample, which confirms the known theory of soil mechanics [5]. 6. conclusions the presented laboratory tests confirm that shear strength depends on the movement of the slip surface. residual shear strength reached a value of between 13 and 15◦, which is approximately one half of the critical values [5]). it is planned to extend the number of laboratory tests within the study to create a detailed numerical model of the dobkovičky landslide. references [1] j. suchý. d8 odstranění sesuvu v km 56,300 56,500 + stabilizace oblasti kolem stavby d8 0805. tech. rep., az consult, 2014. [2] p. kycl. situační zpráva o sesuvu dobkovičky d8 km 56,300 ke dni 11. června 2013. tech. rep., česká geologická služba, 2013. [3] j. záruba. inženýrskogeologický doprůzkum, stabilitní výpočty v km 56,160 56,660. tech. rep., arcadis geotechnika, 2011. [4] z. j. s. j. plšková, m. předběžná zpráva d8-0805 lovosice-řehlovice, ii. etapa inženýrsko-geologického dopruzkumu v oblasti sesuvu dobkovičky a v jeho předpolí v km 56.300-56.500. tech. rep., 2016. [5] j. atkinson. the mechanics of soils and foundations. crc press, 2007. 50 vol. 10/2017 shear strenght of soils from the dobkovičky landslide figure 4. the results of performed tests 51 acta polytechnica ctu proceedings 10:48–51, 2017 1 introduction 2 dobkovicky landslide 2.1 landslide description 2.2 geology and hydrogeology 3 sample description 4 sample preparation and test procedures 4.1 triaxial test 4.2 shear box test 4.3 ring shear test 5 results 6 conclusions references acta polytechnica ctu proceedings doi:10.14311/app.2015.1.0029 acta polytechnica ctu proceedings 2:29–33, 2015 © czech technical university in prague, 2015 available online at http://ojs.cvut.cz/ojs/index.php/app x-copter studio michal koutný∗, ondřej pilát, patrik černý, maroš kasinec charles university in prague, faculty of mathematics and physics, ke karlovu 3, prague, czech republic ∗ corresponding author: xm.koutny+pair@gmail.com abstract. we present a project that aggregates various existing robotic software and serves as a platform to conveniently control a quadrocopter, mainly for research or educational purposes. user interface runs in a browser and other components are also made with portability in mind. we provide a common interface that unifies different quadrocopter models and we implemented it for the parrot ar.drone 2.0. the platform is data oriented, i.e., it is based on dataflow between user objects. we implemented several such objects for: data recording and replaying, inertial and visual localization and following a given path. keywords: robotics, quadcopter, ide. 1. motivation despite the fact that cheap hardware (such as parrot ar.drone 2.0 [1] or ready kits [2]) is available, there are not many possibilities for application programmers to develop software for these robots without need to distinguish between individual models. our aim is to provide a platform for development of software for quadrocopters. the target users are ai programmers or students and expected tasks are general algorithms (basic example in figure 1) for quadrocopters. the result should work with any robot compatible with our software (section 4.3). the testing should be further simplified by running the application without physical access to a quadrocopter either by using a simulator or data previously captured during live flights. at(xcheckpoint.reachedcheckpoint) { xcheckpoint.checkpoint = nextcheckpoint(); },; // x = 3 m, y = 1 m, z = 1.5 m var cp0 = checkpoint.new(3, 1, 1.5); xcheckpoint.checkpoint = cp0; figure 1. sample script that flies through computed checkpoints. it assumes there is created a dataflow graph with the node xcheckpoint in it. 2. related work 2.1. middleware for robotics probably most popular middleware for robotics is the robot operating system (ros) [3]. it supports communication between objects using publish–subscribe mechanism. it is open source, mainly targeted on linux platforms. similar project is urbi sdk, developed by former private company gostai [4]. the current maintainer is aldebaran robotics [5], unfortunately the community around urbi sdk is much smaller and much less active in comparison with ros. reasons why we chose urbi sdk despite this fact are in the section 3.2. 2.2. parrot ar.drone 2 api part of our project is an api for parrot ar.drone 2. various other projects are dealing with this. there is the official sdk [6] with c++ api, controltower [7] that provide java interface, a ros package ardrone_autonomy [8], uobject for urbi sdk [9] or implementation of czech technical university [10]. because none of the aforementioned fit to our requirements for os portability, stability, functionality or documentation, we implemented our own (see the section 4.3). 2.3. ground control system there is official application for parrot ar.drone [11] intended for mobile phone users allowing manual control and displaying only limited data from sensors. the pc application controltower [7] allows controlling quadrocopter with specialized computer peripheries and has airplane-like gui. more complex application is qgroundcontrol [12] that cooperates with pixhawk project [13] that encompasses own hardware and uses visual localization. 3. used technology 3.1. architecture our system is divided into three components. first interacts directly with a user, second controls the robot and the last one connects the former two. the components are separate processes that communicate with each other over network, with intention to run components on different machines. 29 http://dx.doi.org/10.14311/app.2015.1.0029 http://ojs.cvut.cz/ojs/index.php/app m. koutný, o. pilát, p. černý, m. kasinec acta polytechnica ctu proceedings 3.1.1. client client software is used to create and launch user scripts, edit them, manually control the robot and visualize data (e.g., directly from quadrocopter’s sensors). despite the technology challenges the client is thin – running in a web browser.1 3.1.2. server the server component conveys communication between the client and the actual control machine (further onboard). its task is to control the access to the onboard and monitor quality of the connection between the client and the onboard. in the case the overall connection latency (client–server and server– onboard) exceeds preset limits, a warning message is shown to the user. if the connection is lost, onboard execution is correctly terminated and user is notified too. 3.1.3. onboard the onboard is the main executive component. the robot control and data processing run here because it is closest to the robot. the onboard is executing commands obtained from the client and sends back various data selected by user. the onboard component is supposed to run under normal operating system.2 our implementation exploits a pc that communicates with quadrocopter via wi-fi. we did not test the onboard component directly on a robot.3 3.2. urbi sdk urbi sdk is a c++ middleware for robotics, which we based the onboard component on. basically it provides support for communication between user objects (uobjects) and schedules user jobs. communication is possible via so called uvars, which are slots of uobjects. sender just writes to these slots and a receiver’s callback handles the change of uvar’s value. this allows both apparently asynchronous communication and really asynchronous when a thread pool is used to run the callbacks. further, uobjects can run in different processes and urbi sdk ensures transparent messaging via tcp or udp sockets. orchestration user scripts (written in urbiscript) can be executed by the urbi runtime. urbiscript is a prototype-based object-oriented language conceptually similar to javascript. it is possible to implement uobject functionality exclusively in the urbiscript. we chose urbi sdk because of its portability (linux and windows systems are supported) and the own 1google chrome is strongly recommended, though mozilla firefox will also get by (without visualization of video data). 2we support windows 7/8 and ubuntu 14.04 systems. 3the hardware of parrot ar drone 2.0 theoretically should be able to run our onboard with limited performance. scripting language and runtime. considered alternative was robot operating system. 3.3. nodejs nodejs is a server-side javascript engine. recently, it became quite popular among developers of interactive web applications and various modules [14] exist that extend core functionality. it suited our needs for the server component. 3.4. html5 thanks to the standardization efforts many features that were earlier common only for desktop applications or via third party plug-ins (flash, java applets, native plug-ins) are now implemented directly in the browser, generally referred to as html5. to make client as multi-platform as possible, we decided to implement the client for the browser using aforementioned html5 technologies. most importantly, we use the web socket api [15] for sending data back to the client and