TX_1~ABS:AT/ADD:TX_2~ABS:AT


42 http://journals.cihanuniversity.edu.iq/index.php/cuesj CUESJ 2023, 7 (2): 42-48

ReseaRch aRticle

Investigation Light Curve Analysis for Short Period Eclipsing 
Binary CN Andromeda
Chiman I. Hussein

Department of General Science, College of Basic Education, Salahaddin University, Kurdistan Region, Iraq

ABSTRACT

In this article research, drawing and analyzing the light curve of short period binary (SPB) star CN Andromeda (CN And) with B, V, R, 
and I. Light curve fitting and results for the trajectory parameters of the CN And were obtained and compared with those obtained by 
previous works. The author will determine the size, luminosity and masse of the Individual star as well as the orbital size and orientation 
of the binary system. Also calculate the bolometric magnitude, reflection coefficient and absolute parameters for short period binary star. 
These coefficients are needed when analyzing light curves for eclipsing binary stars analyzed to facilitate getting numerical values for their 
relative and absolute characteristics. Some parameters are also fixed or calculated during light curve modeling. The graph of the dimmer 
binary luminosity in one complete orbital period is known as light curve. Furthermore, calculating the bolometric magnitude, reflection 
coefficients, armpit, and absolute parameters for CN, and these terms are very important for understanding the properties of CN And.

Keywords: Absolute parameter, bolometric magnitude, light curve, photometric analysis and binary star CN Andromeda

INTRODUCTION

The majority of star systems are multi or binary star 
(BS) ones. Some portions of binary system has two 
stars that is enough apart to allow for the resolution 

of the individual stars. The eclipsing binary (EB) is made up 
of two stars whose orbits cause them to alternately obscure 
one another from Earth’s perspective. Any periodic change 
over time relates to the redistribution for an object between 
the stars when the system loses or gains angular momentum. 
The period decreases, or if the vas versa appears, the period 
increases.[8,10,13] The evolution of eclipsing binaries light 
curves (LC), or magnitude versus time analysis, produces 
more accurate data thanks to ongoing improvements in 
observational techniques.[9,16] Since the early 20th century, 
significant efforts have been made to develop LC, to find 
and understand these systems. This has been inspired by the 
finding of transiting extrasolar planets. Evaluating for BS. 
Processing of transfer, mass lose, and angular momentum 
loss. They are sometimes called by W UMa type EB, 
because their LC is shaped and described. These systems’ 
orbital durations typically range from 0.1 to 2 days, and 
the component mass ratios are typically between 0.1 and 
0.5.[11,17,20] Form these points, the LC is very important for 
studying the CN And.

It is impressive how precisely the basic physical features can 
be identified. The masses and diameters of stars are frequently 
known with >1% accuracy. Although their masses may differ 
for various reasons, most contact binaries have eclipse depths in 

the LC that are typically equal because both components have 
almost the same surface temperature shows in Figure 1.[18,21]

Photometric plates were used as detectors in the initial 
surveys.[5,7] For several reasons, the study of close BS is 
interesting. For instance, one of the fundamental objectives of 
stellar astronomy is to comprehend the structure and evolution 
of stars. The BS is crucial to our galaxy’s ongoing effort to 
comprehend the cosmos and its elements.[24,27] BS is particularly 
significant, since they are the major and most comprehensive 
source of information on the basic characteristics of stars: (Mass, 
size, radii, luminosities, velocities, separation distance, period,… 
etc.), and extra homes may be determined by understanding 
these homes supply information approximately stars whose 
proximity outcomes research them. A light curve is a graph of 
intensity through the years. One of these graphs is made using 
counting the number of photons coming from a supply over 
some time.[19,29] The importance of the LC, studying LC of EB 

Corresponding Author: 
Chiman I. Hussein, General Science Department, College of 
Basic Education, Salahaddin University, Kurdistan Region, Iraq. 
E-mail: Chiman.hussen@su.edu.krd

Received: March 23, 2023 
Accepted: June 07, 2023 
Published: October 10, 2023

DOI: 10.24086/cuesj.v7n2y2023.pp42-48

Copyright © 2023 Chiman I. Hussein. This is an open-access article distributed 
under the Creative Commons Attribution License (CC BY-NC-ND 4.0).

Cihan University-Erbil Scientific Journal (CUESJ)



Hussein: Light Curve Analysis for Short Period Eclipsing Binary CN Andromeda

43 http://journals.cihanuniversity.edu.iq/index.php/cuesj CUESJ 2023, 7 (2): 42-48

to decide their houses, is a fundamental effect which ought to 
be allowed while reading the light curve of EB. The evolution 
of a star depends almost entirely on its mass and chemical 
composition.[3,31] The light and radial velocity curves were 
analyzed simultaneously using Wilson-Devinney 1971 (W-D) 
code to derive the optical and physical measurements of the BS 
components.[12,25] The discovery of transits of extra solar planets 
earlier this century has spurred considerable efforts to generate 
very high-quality LC that can be used to explore and study planets. 
This system instruments, observation methods, and analyzing 
data techniques were improved to now detect lunar eclipses to a 
depth of 600 ppm on individual goals.[14,35] In 1949 astronomer 
Hoffmeister discovered CN Andromeda (CN And), first reporting 
for exhibits β Lyr-like light variations. In 1956, Tsesevich found 
it’s an Algol-like binary for periodic orbit 2,599 days. In 1976, 
Bozkurt reported asymmetric changes for light curve B and V. 
In 1996, Bozkurt found strongly emission X-ray of main system. 
Van Hamme proposed LC analyzing in 2001. In 2005, spectral 
types for components proposed by Zola are in the range F5-G5. 
In 2010, Rucinski announced recently radial velocities and LC 
analyzing for system, the variation of periodic orbit for CN And. 
Also, LC in the B, G, R, and I filters of CN And published. In 2015, 
Koju and Beaky illustrated system cycle variation and O’Connell 
effect. Maxted in 2016 describe flexible LC model. In 2017, 
Yilmaz studied LC and orbital period analysis of VX LAC. Menon 
in 2020 details evolutionary model for massive contact BSs. For 
extending these works, investigation LC analysis for CN And.

THE IMPORTANT INFORMATION ABOUT 
CN AND BS

Third suspected component of the system is a red dwarf with a mass 
of about 0.1100 M☉, at 38 ± 4 years’ the orbit around the binary. 
The variability of the star CN And (BD = +39059, GSC = 2787 
– 1815, PPM = 42831, TYC 2787 – 1815-1, RA = 00 h 20 m 
30.60 s, Dec = +40 13 m 33.8 s spectral type F5V near contact 
was observed by Hoffmeister in 1949.[29] Based on the image 
data[15,32] classified the system as an Algol-like binary Skelton and 
Smits classified, it as a W UMa-like system.[23,32] The information 
about BS CN And for the first and second stars is very important, 
the period of CN Andromeda is 0.46279 days and contains in 
Table 1. Its eclipse depths differ by some 0.3000 mages in V. it is 
also an active solar-type binary with components of spectral type 
in the F5 to G5 range. For the first star, we have the following 
information M1 = 1.4330, R1=1.4800, L1=3.400 and T1=6450. 
Furthermore, for the second star, the following information exist 
M2=0.5520, R2=0.9500, L2=0.4000, and T2=4726.

The CN Andromeda has been observed by many authors 
and the V band light curve of CN Andromeda shows in 
Figure 2.[33,34] In this work, we study the phenomenon known 
as the dark coefficient and its relationship to the BS system 
shows in Figure 3, an approach that lies within atmospheric 
studies. In addition, we selected a CN And star using filters 
(B, G, R, and I), and for each star, a certain temperature was 
used, as indicated by the program Van Hamme, as well as the 
darkness of the limbs as well as the reflection effect.

THE LIGHT CURVE MODEL

The profundities of the essential and auxiliary minimums 
within the orbital LC are distinctively demonstrating that the 

Figure 1: Shows LC for binary star system[8]

temperatures of the two stars, although similar, they are the 
difference. For this reason, the attempt to model the system 
as W UMa with thermally exposed components failed. The 
foundation for the bright fringe analysis was created using 
W-D’s composite light fringe and differential correction 
program in 1971 adjusted by Wilson (1979) to incorporate 
the spiral speed. The overhauled form of the program utilized 
(May 2003 form) incorporates the expansion of round pixels 

Figure 2: The V band light curve of CN And

Figure 3: Cataclysmic BS photograph for CN And



Hussein: Light Curve Analysis for Short Period Eclipsing Binary CN Andromeda

44 http://journals.cihanuniversity.edu.iq/index.php/cuesj CUESJ 2023, 7 (2): 42-48

and Kurucz’s demonstrate atmosphere, it adjusts the LC to 
bandwidth standard rather than the effective wavelength 
dimming. By studying this curve, a large number of 
fundamental astrophysical quantities can be determined in LC 
analysis. Illustrating the LC shown in Figure 5, the choice of 
LD rules is restricted to those implemented in the light curve 
codec we are using. It is important to generate results for 
several coefficients of difference to determine their effect on 
the solution.

THE PHOTOMETRIC ANALYSIS OF CN AND

In arrange to decide, the photometric and geometric parameters 
to analysis, an overhauled adaptation of the W-D program was 
utilized, consolidating the expansion of photosphere focuses 
and altering the LC at diverse transfer speeds. Introductory 
values were gotten from distributed LC arrangements. After 
numerous tests, we have determined a set of parameters that 
are representative of the observed LC shows in Figure 6. The 
parameters adopted in the solution are as takes after: the 
temperature of first star is 6150K, the value of LD coefficients 
(x1=x2=0.4860) for V, 0.589 for B, 0.401 for R, and 0.475 
for I bands), the value of the gravity-darkening coefficients 
(g1=g2=0.320), the esteem of the Albedo (A1=A2=0.50).[1,6,33] 
The tuning parameters utilized are orbital slant (i), normal 
temperature of the moment star (T1) the possibilities of the 
components Ω1 and Ω2, as well as the monochromatic. The 
tuning parameters used are orbital inclination (i), mass 
ratio (q), average temperature of the second star (T2) the 
potentials of the components (Ω1 and Ω2), as well as the 
monochromatic luminosity for first star (L1). Fitting for 
calculating LC is stamped with strong lines in Figure 4 in V, 
B, R, and I bands. The photometric parameters are recorded 
in Tables 2 and 3. The LC within the show do not coordinate 
the watched information wells close the 0.2500 phase. For 
solving these, LC is as follows. Since there is asymmetry in 
the height of the CN And insulation curve and in each band 
as seen in Figure 5, the second maximum is the brightest 
point, for coming up with the aim that main half of the curve. 
Insulation is disturbed by a cool place. Let the 0.500–1.000 
phase is unaffected by the point, at the same time, only 0.5 of 
the isolation curve is adjusted to produce binary parameters.

Where Ω1 and Ω2 are surfaces potential components, C1 
and C2 are potential components, f1 and f2 are fill out of the 
major and minor stars components, and L1 and L1 are absolute 
parameters for component in the unit of solar Luminosity’s.

THE ABSOLUTE PARAMETERS OF CN AND

Flux for the star is the total amount of energy intercepted 
by the detector divided by the area of the detector, and the 
unit of flux is (Joule/meter2). For determining the absolute 
parameters of CN And using equations (2) to (5), contains in 
references.[4,5] Utilizing Matlab program for calculating the 
parameters and recording in Table 4.

 A p m m3 2
1 274 5= +. ( ).  (1)

 R Ar1 1= , R Ar2 2=  (2)

Figure 4: Gometrically of CN And created by PHOEBE at stages 0.00, 
0.25, 0.50, and 0.75 individually

Figure 5: Descripts plot LC of eclipsing contact binary for CN And, 
one much brighter than the other



Hussein: Light Curve Analysis for Short Period Eclipsing Binary CN Andromeda

45 http://journals.cihanuniversity.edu.iq/index.php/cuesj CUESJ 2023, 7 (2): 42-48

Table 2: The output parameters for CN And

Numbers The output parameters

1 Lagrangian L1=3.3982 Lagrangian L2=0.3973

2 C inner=3.901906 C outer=3.559725

3 C1=3.901119 C2=3.901120

4 surface area one=2.733721 surface area 
two=1.145659

5 Ω1=2.65400 Ω1=2.65400

6 Ωinner=2.654547 Ωouter=2.416986

7 r1 (back)= 0.491417 r2 (back) = 0.325067

8 r1 (side) = 0.464739 r2 (side) = 0.292310

9 r1 (pole)= 0.435205 r2 (pole) = 0.280430

10 mean radius one=0.463787 mean radius 
two=0.299264

11 f1=0.002310 f1=0.002310

Table 3: LC fitting components of CN And

Parameters star one star two

Surface Potential Ω 2.654001 2.654001

Limb Darkening 0.8061 0.8329

Reflection 1.4328 0.9497

Temperature 6451.00 5376.00

Gravity Darkening 0.3210 0.3210

Distance of Separation 9.6201

Orbital Inclination 68.5099

Mass Ratio 
M
M

2

1







0.38520

Period of orbit 0.4627

 L R T1 1
2

1
4= , L R T2 2

2
2
4=  (3)

 M
M
q1 1

=
+

,  (4)

 M
M
q2
1

1
=

+
,  (5)

 F inner

inner outer

=
−
−

( )

( )
,Ω Ω

Ω Ω
1 2  (6)

THE BOLOMETRIC MAGNITUDES – MBOL1 
AND MBOL2

The astronomer Allen in (1976) constructed this relationship 
for computing the parameters.[2]

 M T
R
Rbol1 1
1

0

42 3600 5= − −. log( ) log( )  (7)

 M T
R
Rbol2 2
2

0

42 3600 5= − −. log( ) log( )  (8)

The formulas of equations (7) and (8) used for compute 
the Bolometric Magnitudes (BM), Utilizing Matlab program 
for calculating the parameters and recorded in Table 5 the 
radius of the sun is R0 = 69570000m. The present work shows 
the suitable armpit parameters for SP binary systems.

 g
c

T e
c
T

1
2

14 1
2

1

=
−λ λ[ ]

( )
 (9)

 g
c

T e
c
T

2
2

24 1
2

2

=
−λ λ[ ]

( )
 (10)

Computing the reflection coefficients using these 
equations.

 E t T
e

T
c
T

eff

c
T

1 1 2
4

1

1
2

1

2

2

1

=

−

−

( )
( )

( )
λ

λ

 (11)

 E t T
e

T
c
T

eff

c
T

2 2 1
4

1

2
2

2

2

1

1

=

−

−

( )
( )

( )
λ

λ

 (12)

THE LC FROM PRESENT OBSERVATIONS

The LC of CN And in V, B, I, and R bands was showed in 
Figure 4. A round for phasing = 0.00 and nearly flat for 
phasing = 0.50 primary eclipse was observed, which is total 
eclipsing configuration for system. Primarily, eclipse is clearly 
deeper than for secondary eclipse. The contrast between 
essential and auxiliary minima ranges in greatness from 0.260 
to 0.300 in groups V, B, I, and R. Then, the most least is more 
profound and happens when the hotter star passing behind 
cooler star. The shallower auxiliary least happens when the 
cooler star takes after the hotter star.

The distinction between the essential greatest stage = 
0.250 and the essential greatest. The minimum magnitude 
is about 0.460, 0.480, 0.480, and 0.500, magnitudes in I, V, 
R, and B bands. The different between secondary maximum 
phase = 0.750 and secondary minimum ranges from 0.230 
to 0.240 magnitude for I, V, R, and B bands. In the W UMa 
type system, because the two stars are so closer together, there 

Table 1: The coordinates of the equator and the equinox 2000, HD, and BD NO. For the short-lived binary (SP) star of (SQR) as used in the 
present work

BS Period day BH Eclipse depth Binary orbit RM Dec. Spectral type

H M S Deg M S

CN And 0.462796 +3959 0.3000 1.50×10−7 00 20 30.55 +40 13 33.8 F



Hussein: Light Curve Analysis for Short Period Eclipsing Binary CN Andromeda

46 http://journals.cihanuniversity.edu.iq/index.php/cuesj CUESJ 2023, 7 (2): 42-48

Table 5: Subparameters adjusted for active short period of CN And

CN And Pass bands Mbol1 Mbol1 g1 g2 Eeff1 Eeff2

B

V

R

I

0.58897

0.48602

0.40099

0.47524

0.58897

0.486011

0.40099

0.47524

0.87849

0.81779

0.76771

0.78553

0.99329

0.93449

0.88572

0.90321

6.32448

6.79388

7.23628

7.12423

5.59357

5.94547

6.27219

6.13827

exist constant light variation in addition to lunar eclipses. In 
addition, the stars will suffer from gravitational distortion and 
heating effects. These effects show the asymmetric LC of the 
W UMa type system. The watched LC of CN And were found to 
be deviated around the essential and auxiliary crests, with the 
auxiliary top being brighter than the essential. The distinction 
in adequacy between stage at 0.750, brighter, and stage at 
0.250 shifts from 0.0390 to 0.04100 mag in groups V, B, I, and 
R. This can be more often than not clarified by the nearness of 
stains on binary system components. This indicates that the LC 
of CN And show the O’Connell effect.

CONCLUSIONS

From this study, the evolution of LC photometric observations 
for binary CN And is discussed, photometric arrangements have 

been gotten by solving V, B, R, and I. The absolute parameters 
and BM coefficients are computed for it. When modeling BS 
LC, ATLAS stellar atmosphere models calculations should be 
used rather than Al-Naimiys calculations,[4,7] which were based 
on Carbon and Gingerich models in 1969,[4,7] concluding the 
following points:-
1. It is need to conduct additional observations of the system 

using 1000 m telescopes. With optimum mass ratio of 
q = 0.306000. Binary may well be an A-type over contact 
BS, agreeing to the current photometric arrangement in 
Tables 3 and 4. The mass ratio is relatively close to the 
indicator-derived spectroscopic is 0.325000.

2. There is small variation between parameters when 
comparing it with the others related published work in 
the same area. Mentioned in Tables 4 and 5.

Table 4: Current work in relation to other research works

The name of star Mbol1 Mbol1 Mbol1 Mbol1 Mbol1 Mbol1 Mbol1

CN And binary star 1.4301 (2) 0.9200 (1) 1.3002 (5) 0.5101 (2) - - Van Hamme in 2001

1.47998 (2) 0.9402 (1) 1.41989 (1) 0.5602 (3) 3.5199 (8) 0.9980 (35) Prˇsa, A. in 2005

1.4801 (4) 0.9499 1.43298 (31) 0.5520 (2) 3.4003 0.4003 Siwak in 2010

1.4774 (2) 0.95003 1.4125 (2) 0.54775 (3) 3.5294 0.8753 Awadalla in 2016.

1.4502 (2) 0.9401 (1) 1.4003 (3) 0.54997 (2) 3.4102 (8) 0.9304 (5) Muhammed In 2019

1.3451 (2) 0.8733 (4) 1.2457 (3) 0.4951 (2) 3.1885 0.6441 (3) Helen in 2020.

1.4782 (3) 0.9456 1.4456 (2) 0.5497 3.3982 (4) 0.3973 Present work (2022)

Figure 6: LC fitting for V, B, R, and I filter for CN And, respectively



Hussein: Light Curve Analysis for Short Period Eclipsing Binary CN Andromeda

47 http://journals.cihanuniversity.edu.iq/index.php/cuesj CUESJ 2023, 7 (2): 42-48

3. That spin up at a rate around 100 times faster than the 
sun, indicating a significant level of magnetic activity. The 
current LC will be imply that the spots have vanished, 
symmetry, and volatility light curves are markers of spot 
activity.

4. Form the results appear that the primary star is the more 
enormous and hotter component, whereas the second star 
is the less enormous and cooler one.

5. The estimated orbital inclination of i = 82,000 suggesting 
that the CN And system is a general partial lunar eclipse. 
The higher mass component has a temperature T1 up to T 
= 6231 k higher than to the smaller component. It brings 
in less light. Geometric exposure F defined in equation (8) 
is 1.010%, which means that CN And is an overexposed 
BS, according to symmetry of the LC.

6. The increasing stellar wind that has caused long-term 
drop for orbital period can be described for CN And is 
an over contact BS with a shared convective envelope 
between both components (f = 24.900%).

7. According to the results, indicated that the chosen system 
could conjointly be a contact system and also absolutely 
the parameters of the components are determined with 
acceptable accuracy that the physical parameters are 
obtained in associate in suitable manner extremely 
uniform technique.

REFERENCES
1. S. H. Alebcar and L. P. Vaz. Limb darkening coefficients of 

illuminated Atmospheres Results for illuminated line - Blanketed 
modules. Journal of Astronomy Astrophysics Supplement, vol. 135, 
no. 2, pp. 555-566, 1999.

2. C. W. Allen. Astrophysical Quantities. 3rd ed. The Athlon Press, 
London, 1976.

3. H. Al-Naimiy. Linearized of limb darkening coefficients for use 
in Analysis of ES light curves. Journal of Astrophysics and space 
Sciences, vol. 53, no. 2, pp. 181-192, 1978.

4. H. M. K. Al-Naimiy. Star- spots studies for three short period RS 
CVn-type binaries. Journal of Astrophysics, vol. 44, no. 2, pp. 233-
247, 2001.

5. N. S. Awadalla, M. A. Hanna, M. N. Ismail, I. A. Hassan and M. 
A. Elkhamisy. Period variation study and light curve analysis of 
the ESGSC 02013-00288. Journal of Applied Mathematics and 
Nonlinear Sciences, vol. 1, no. 2, pp. 321-334, 2016.

6. D. Barrado, M. J. Fernandez and B. Montesinos. The age-mass 
relation for chromo spherically active binaries. L The evolutionary 
status. Journal of Astronomy and Astrophysics, vol. 290, pp.143-
157, 1994.

7. D. H. Bradstreet. Catalog and Atlas of Eclipsing Binaries. 
Department of Physics Science-Eastern University, New York, 
2004.

8. A. Claret. A new nonlinear limb darkening low for LTE stellar 
Atmosphere models. Journal of Astronomy and Astrophysics, 
vol. 401, no. 4, pp. 567-578, 2003.

9. A. Claret and A. Jimenez. Limb darkening for cooler 
stars - standard and irradiated Models. Journal of Astronomy and 
Astrophysics, vol. 230, 5, pp. 412-428, 1990a.

10. A. Claret. Comprehensive tables for the interpretation and 
modeling of the LC of eclipsing binaries. Journal of Astronomy 
and Astrophysics Supplement, vol. 131, no. 2, pp. 395-408, 1989.

11. K. Chun-Hwey, M. H. Song, J. N. Yoon, W. Han and M. J. Jeong. 
BD Andromeda: A new short- period RS CVn eclipsing binary star 
with a distant tertiary in a highly eccentric orbit. Journal of the 
Astrophysical, vol. 788, no. 134, pp. 22-29, 2014.

12. A. Cséki. The analysis of Super WASP photometric data for the 
over contact binary QW Gem. Journal of Serbian Astronomy, 
vol. 186, no. 3, pp. 47-51, 2013.

13. S. Daemgen, F. Hormuth, W. Brandner, C. Bergfors, M. Janson, S. 
Hippler and T. Henning. Bimarity of transit host stars. Journal of 
Astronomy and Astrophysics, vol. 498, no. 6, pp. 567-574, 2009.

14. J. Diaz-Cordoves, A. Claret and A. Gimenez. A linear and nonlinear 
limb darkening coefficients for LTE model Atmospheres. Journal 
of Astronomy and Astrophysics, vol. 110, no. 7, pp. 329-340, 1995.

15. J. Diaz-Cordoves and A. Gimenez. A new nonlinear approximation 
to the Darkening of hot stars. Journal of Astronomy, vol. 75, 
no. 8, pp. 175-189, 1992.

16. R. S. Donald, A. O. Jerome, W. Gur and F. W. William. Accurate 
Computation of LC and the Resister McLaughlin Effect in Multi 
body Eclipsing Systems. The Astronomical Journal, vol. 156, 
no. 297, pp. 48-63, 2018.

17. E. Gillen. New Low-mass ES systems in Praesepe discovered by 
K2. Journal of the Astrophysical, vol. 849, no. 1, pp. 25-38, 2017.

18. A. Essam, A. Nakhlawy and M. A. Rassem. The first photometric 
analyses and classification of the W- UMa ESsystems GSC 
1283-53 and GSC 702-1892. NRIAG Journal of Astronomy and 
Geophysics, vol. 2, no. 4, pp. 1-7, 2013.

19. P. B. Etazl and E. F. Milone. Light curve modeling of Eclipsing 
BS system. Journal of Springer-Verlag, vol.12, no. 3, pp. 113-121, 
2003.

20. A. Gemenez. General Relativistic periastron Advances in 
ESsystem. Astrophysical Journal, vol. 297, no. 6, pp. 405-412, 
1985.

21. R. L. Helen. Study of Eclipsing Binaries: LC& O-C Diagrams. 
Journal of Interpretation of Galaxies, vol. 8, no. 2, pp. 78-93, 
2020.

22. C. Hoffmeister. Mass transfer and possible third-body effect on 
the period variations of the near-contact binary CN Andromeda, 
Research in Astronomy and astrophysics, vol. 19, no. (8), pp.22-
31, 1949.

23. G. J. William. The Facts on File Dictionary of Astronomy. Harked 
those Books Ltd., New York, p. 512, 2006.

24. O. Malkov, E. Oblak,  E. A. Snegireva, and J. Torra. A catalogue 
of eclipsing variables. Journal of Astronomy and Astrophysics, 
vol. 446, no. 5, pp. 785-790, 2006.

25. P. F. L. Maxted. A fast, flexible light curve model for detached 
ES stars and transiting explants. Journal of Astronomy and 
Astrophysics Manuscript, vol. 12, no. 5, pp. 123-145, 2016.

26. A. Menon, N. Langer, S. E. de Mink, S. Justham, K. Sen, D. 
Szécsi, A. de Koter, M. Abdul-Masih, H. Sana, L. Mahy and P. 
Marchant. Detailed evolutionary models of massive contact 
binaries I. Journal of Model Grids and Synthetic Populations for 
the Magellanic Clouds, vol. 4, no. 6, pp. 1-21, 2020.

27. M. Pakravanfar, A. Poro and I. Safaei. New LC and Ephemeris of 
W UMa‐type binary star BX Pegasi. Journal of Occultation and 
Eclipse, vol. 6, no. 4, pp. 33-39, 2019.

28. A. Prsa and T. Zwitter. A computational guide to physics of 
eclipsing binaries. I demonstrations and perspectives. Journal of 
Astronomy Physics, vol. 628, no. 7, pp. 426-441, 2005.

29. S. M. Rucinski, J. M. Kreiner, M. Siwak and M. Drozdz. Physical 
parameters of components in close binary systems: II. Journal of 
Acta Astronomical, vol. 54, no. 5, pp. 195-206, 2010.

30. S. O. Selam. Key parameters of W UMa-Type contact binaries 
discovered by HIPPARCOS. Journal of Astronomy and Astrophysics, 
vol. 416, no. 2, pp. 1097-1109, 2004.

31. P. L. Skelton and D. P. Smits. Modelling of W UMa-type variable 
stars. South African Journal of Science, vol. 105, no. 3, pp. 120-
127, 2009.

32. D. Sukanta and P. Harinder. Physical parameters of 62 eclipsing 
BS using the all sky automated survey-3 data - I. Journal of 
Astronomy Society, vol. 412, no. 3, pp. 1787-1803, 2011.

33. W. Van Hamme. CN Andromeda: A broken contact binary. Journal 



Hussein: Light Curve Analysis for Short Period Eclipsing Binary CN Andromeda

48 http://journals.cihanuniversity.edu.iq/index.php/cuesj CUESJ 2023, 7 (2): 42-48

of the American Astronomical Society, vol. 122, 2, pp. 3436-3446, 
2001.

34. P. Vinod, J. C. Pandey, J. K. Mano and D. C. Srivastava. BVRI 
photometric and polar metric studies of W UMa type ESFO 

Hydra. Journal of New Astronomy, vol. 20, no. 5, pp. 52-61, 2013.
35. M. R. H. Nelson, H. V. Enavc, I. Ozavcı and D. Gumu. Light curve 

and orbital period analysis of VX LAC. Journal of Revista Mexicana 
de Astronomy Astrophysical, vol. 53, no. 2, pp. 29-36, 2017.