J/AJ/169/85 Photometry & parameters of eclipsing contact binairies (Xu+, 2025)
Photometric and spectroscopic investigations of three large amplitude contact
binaries.
Xu X., Li K., Liu F., Yan Q.-X., Wang Y.-F., Cui X.-Y., Wang J.-Y.,
Gao X., Sun G.-Y., Wu C.-Y., Li M.-Z.-M.
<Astron. J., 169, 85 (2025)>
=2025AJ....169...85X 2025AJ....169...85X
ADC_Keywords: Binaries, eclipsing; Photometry; Spectroscopy; Optical; Infrared;
Stars, double and multiple
Keywords: Eclipsing binary stars ; Close binary stars ; Mass ratio ;
Fundamental parameters of stars ; Stellar evolution
Abstract:
We performed photometric and spectroscopic studies of three large
amplitude contact binaries: NSVS 2418361, ATLAS J057.1170+31.2384, and
NSVS 7377875. The amplitudes of these three systems' light curves are
more than 0.7mag. We analyzed the light curves using the
Wilson-Devinney code to yield physical parameters. The photometric
solutions suggested that NSVS 7377875 belongs to an A-subtype contact
binary, while the others are classified as W-subtype ones.
Furthermore, the mass ratio of NSVS 7377875 is higher than 0.72, so it
belongs to H-subtype contact binaries. Since their light curves have
unequal height at two maxima, which is called the O'Connell effect, a
dark spot on the primary component for each target was required to get
a better fit of the light curves. The orbital period investigation
shows that the period of NSVS 2418361 is increasing, indicating a mass
transfer from the the less massive component to the more massive one,
while the other targets exhibit no long-term variation. Our spectral
subtraction analysis of LAMOST spectra revealed excess emissions in
the Hα line, indicating chromospheric activity in all the three
targets. The Gaia distance was applied to estimate the absolute
parameters of the three targets, and we obtained their evolutionary
state. The relationships between the energy transfer parameter of
76 H-subtype contact binaries and their bolometric luminosity ratios,
as well as their contact degree, were presented. We discovered that
H-subtype systems have less efficient energy transfer rate, which
corresponds to the conclusion proposed by Csizmadia & Klagyivik.
Description:
We conducted photometric observations on the three contact binaries
using Weihai Observatory 1.0m telescope of Shandong University, the
60cm Ningbo Bureau of Education and Xinjiang Observatory Telescope
(NEXT), and the 60cm telescope at the Xinglong Station of National
Astronomical Observatories (XL60), all located in China.
ASASSN-V J034828.11+311418.4, hereafter J034828, was observed on 2023
December 6 with Cousins I and R filters using WHOT.
ASASSN-V J073802.91+585021.6, hereafter J073802, was observed on 2021
December 10 and 11 with the g, r, and i filters using NEXT.
ASASSN-V J084000.43+363927.9, hereafter J084000, was observed on 2022
December 29 with the Cousins I and R filters using XL60.
Our three systems have also been observed by various photometric
surveys, including Super Wide Angle Search for Planets (SuperWASP or
SWASP; Butters+, 2010A&A...520L..10B 2010A&A...520L..10B), Catalina Real-time Transient
Survey (CRTS; Drake+2009, J/ApJ/696/870), and Zwicky Transient
Facility (ZTF). Additionally, the Transiting Exoplanet Survey
Satellite (TESS; Sharma+2018, J/MNRAS/473/200) observed two of our
targets: J034828 was observed by Sectors 42, 43, 44, and 71
(2021 August-2023 November), while J073802 was observed by Sectors 47,
60, and 74 (2021 December-2024 January).
Spectroscopic observations were also conducted using the Large Sky
Area Multi-Object Fiber Spectroscopic Telescope (LAMOST; also known as
the Guoshoujing Telescope). In its low-resolution mode, the spectral
resolution is approximately 1800, covering a wavelength range from
3700 to 9000Å. J034828, J073802, and J084000 have been observed by
LAMOST in low-resolution R∼1800 and we found six spectra from Data
Release 10 (DR7 available on CDS, V/156).
We also queried the atmospheric parameters from Gaia DR3 (I/355, I/357).
Objects:
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RA (2000) DE Designation(s) (Period)
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07 38 02.88 +58 50 21.7 J073802 = NSVS 2418361 (Per=0.3596081d)
03 48 28.08 +31 14 18.4 J034828 = UCAC4 607-009784 (Per=0.2527926d)
08 40 00.54 +36 39 28.6 J084000 = NSVS 4817512 (Per=0.2649852d)
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
targets.dat 57 3 List of targets (Table added by CDS with data from
Table 1)
table3.dat 73 392 Photometric observation of J034828, J073802, and
J084000
table9.dat 75 1160 Eclipsing times and O-C values of the three targets
table13.dat 106 52 Physical parameters of 52 H-subtype contact
binaries
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See also:
V/156 : LAMOST DR7 catalogs (Luo+, 2019)
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
I/357 : Gaia DR3 Part 3. Non-single stars (Gaia Collaboration, 2022)
V/119 : Catalogue of field contact binary stars (Pribulla+, 2003)
J/AJ/106/2096 : Limb-darkening coefficients in binaries (Van Hamme 1993)
J/A+AS/133/7 : V photometry of YY CMi (Niarchos+ 1998)
J/A+A/426/1001 : Catalog of contact binary stars (Csizmadia+, 2004)
J/ApJ/629/1055 : Evolution of close binary systems (Yakut+, 2005)
J/MNRAS/373/1483 : W UMa type and CAB stars dynamical evolution (Eker+, 2006)
J/ApJ/696/870 : Catalina Real-time Transient Survey (CRTS) (Drake+, 2009)
J/other/A+ARV/17.251 : Stars observed with Doppler imaging (Strassmeier, 2009)
J/MNRAS/412/1787 : Physical parameters of 62 eclipsing binaries (Deb+, 2011)
J/other/BASI/40.51 : Cl* NGC 2539 CKY V3 and V4 BV light curves (Kiron+, 2012)
J/AJ/143/99 : Photometry of W UMa eclipsing binaries (Terrell+, 2012)
J/AJ/146/157 : Differential BVRI photometry of FI Boo (Christopoulou+, 2013)
J/ApJS/208/9 : Intrinsic colors and temperatures of PMS stars (Pecaut+, 2013)
J/AJ/145/9 : BVRI LCs of the early-type binary V382 Cyg (Yasarsoy+, 2013)
J/MNRAS/430/2029 : Initial masses of W UMa type contact binar. (Yildiz+, 2013)
J/AJ/145/39 : Differential BV(RI)c light curves of PY Vir (Zhu+, 2013)
J/ApJ/788/48 : X-ray through NIR photometry of NGC 2617 (Shappee+, 2014)
J/MNRAS/448/2890 : Observation of six NSVS eclipsing binaries (Dimitrov+, 2015)
J/A+A/590/A45 : GU Mon BV light curves (Lorenzo+, 2016)
J/PASJ/69/62 : First analysis of the binary IK Boo (Kriwattanawong+, 2017)
J/MNRAS/473/2004 : TESS-HERMES Survey Data Release 1 catalog (Sharma+, 2018)
J/AJ/158/104 : LL Com BVR bands photometry & times of light minimum (Hu+, 2019)
J/AJ/157/111 : Study of three early-type contact twin binaries (Yang+, 2019)
J/AJ/159/189 : Eclipse timings for 9 contact binaries (Li+, 2020)
J/ApJS/247/50 : Late-type contact binaries in CSS DR1 (Sun+, 2020)
J/ApJ/922/122 : BVRcIc LCs of two contact binaries (Li+, 2021)
J/AJ/162/13 : Parameters estimation for 173 eclipsing binaries (Li+, 2021)
J/ApJS/256/14 : RVs from LAMOST MRS DR7 stellar spectra (Zhang+, 2021)
J/AJ/164/202 : Extrem. Low Mass Ratio Contact Binaries I. 10 syst. (Li+, 2022)
J/A+A/672/A176 : Mass-ratio distribution of contact binary stars (Pesta+, 2023)
J/ApJS/271/32 : ASAS-SN eclipsing contact binaries with Gaia DR3 (Li+, 2024)
Byte-by-byte Description of file: targets.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- ID Target identifier
9- 36 A28 --- Simbad Simbad identifier
38- 46 F9.7 d Per [0.25/0.36] Period
48- 52 F5.2 mag Vmag [13.4/15.5] V-band magnitude
54- 57 F4.2 mag Amp [0.75/0.83] Amplitude
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- ID Target identifier (1)
9- 9 A1 --- Filt1 Filter in light curve 1 (2)
11- 23 F13.5 d HJD1 ? Heliocentric Julian date, light curve 1
25- 29 F5.3 mag dMag1 [0.09/1.93]? Magnitude difference, light curve 1
31- 31 A1 --- Filt2 ? Filter in light curve 2 (2)
33- 45 F13.5 d HJD2 ? Heliocentric Julian date, light curve 2
47- 51 F5.3 mag dMag2 [0.02/1.65]? Magnitude difference, light curve 2
53- 53 A1 --- Filt3 ? Filter in light curve 3 (2)
55- 67 F13.5 d HJD3 ? Heliocentric Julian date, light curve 3
69- 73 F5.3 mag dMag3 [4e-3/0.81]? Magnitude difference, light curve 3
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Note (1): Full names of objects as follows:
J034828 = ASASSN-V J034828.11+311418.4 (129 occurrences)
J073802 = ASASSN-V J073802.91+585021.6 (112 occurrences)
J084000 = ASASSN-V J084000.43+363927.9 (151 occurrences)
Note (2): Filters as follows:
R = Cousins R-band (640nm); 278 occurrences
I = Cousins I-band (798nm); 272 occurrences
r = r-band (622nm); 111 occurrences
i = i-band (762nm); 111 occurrences
g = g-band (477nm); 112 occurrences
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Byte-by-byte Description of file: table9.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- ID Target identifier (1)
9- 22 F14.6 d BJD [2454002/2460340] Barycentric Julian Date
24- 29 F6.4 d e_BJD [0/9e-3] Uncertainty in BJD
31- 38 F8.1 --- E [-24852/2169] Cycle number
40- 47 F8.5 d O-C [-0.03/0.02] Observed - Model
49- 56 F8.5 d Res [-0.011/0.012] Mean Residual
58- 75 A18 --- Tel Telescope (2)
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Note (1): Full names of objects as follows:
J034828 = ASASSN-V J034828.11+311418.4 (646 occurrences)
J073802 = ASASSN-V J073802.91+585021.6 (370 occurrences)
J084000 = ASASSN-V J084000.43+363927.9 (144 occurrences)
Note (2): Telescopes as follows:
ASAS-SN = the All-Sky Automated Survey for SuperNovae
(Shappee+2014, J/ApJ/788/48;
Christy+, 2023MNRAS.519.5271C 2023MNRAS.519.5271C) consisting of
24 telescopes distributed around the globe
(11 occurrences)
CRTS = the Catalina Real-time Transient Survey
(Drake+2009, J/ApJ/696/870) consisting of three
Steward Observatory telescopes in Arizona, US
(11 occurrences)
Kjurkchieva et al. = Kjurkchieva+ (2017RMxAA..53..133K 2017RMxAA..53..133K) using the
30cm Rozhen Observatory telescope in Bulgaria
(4 occurrences)
NEXT = the 60cm Ningbo Bureau of Education and Xinjiang
Observatory Telescope in China (2 occurrences)
SWASP = the Super Wide Angle Search for Planets
(Butters+, 2010A&A...520L..10B 2010A&A...520L..10B) consisting of
two telescopes, one in La Palma and one in
South Africa (166 occurrences)
TESS = the Transiting Exoplanet Survey Satellite
(Sharma+2018, J/MNRAS/473/200)
WHOT = the Weihai Observatory 1.0m telescope of
Shandong University in China (2 occurrences)
XL60 = the 60cm telescope at the Xinglong Station of National
Astronomical Observatories in China (2 occurrences)
ZTF = the Zwicky Transient Facility using the Palomar
Observatory telescopes in California, US
(24 occurrences)
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Byte-by-byte Description of file: table13.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 26 A26 --- Name Target Name
28- 28 A1 --- Type Type (1)
30- 34 F5.3 d Per [0.21/1.89] Period
36- 40 F5.3 --- q [0.7/1] Mass ratio
42- 46 F5.3 --- f [1e-3/0.92] Fill-out factor (2)
48- 52 I5 K Temp1 [3942/36000] Temperature, Primary
54- 58 I5 K Temp2 [3692/34415] Temperature, Secondary
60- 64 F5.2 Msun Mass1 [0.5/27.9]? Mass, Primary
66- 70 F5.2 Msun Mass2 [0.4/20.8]? Mass, Secondary
72- 77 F6.2 Rsun Rad1 [0.6/782]? Radius, Primary
79- 82 F4.2 Rsun Rad2 [0.5/8.5]? Radius, Secondary
84- 92 F9.2 Lsun L1 [0.1/141906]? Luminosity, Primary
94-101 F8.2 Lsun L2 [0.07/89950]? Luminosity, Secondary
103-106 A4 --- Ref Reference(s) (3)
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Note (1): Type as follows:
A = a contact binary system in which the more massive component has a
higher temperature (34 occurrences)
W = a contact binary system in which the more massive component has a
lower temperature (18 occurrences)
Note (2): The fill-out factor describes the contact degree of a contact binary,
it can be calculated using
f=(Ωin-Ω)/(Ωout-Ω), where ωin and
Ωout are the potentials of the inner and outer Lagrangian
equipotential surface, and Ω is the actual potential.
Note (3): References as follows:
1 = Kiron+2012, J/other/BASI/40.51
2 = Yuan, 2011RAA....11.1158Y 2011RAA....11.1158Y
3 = Lorenzo+2016, J/A+A/590/A45
4 = Michel+, 2019RAA....19...99M 2019RAA....19...99M
5 = Kjurkchieva+, 2017RAA....17...42K 2017RAA....17...42K
6 = Tavakkoli+, 2015NewA...37...64T 2015NewA...37...64T
7 = Poro+, 2021RAA....21..203P 2021RAA....21..203P
8 = Poro+, 2021AstL...47..402P 2021AstL...47..402P
9 = Poro+, 2024PASP..136b4201P 2024PASP..136b4201P
10 = Han+, 2019arXiv190602466H 2019arXiv190602466H
11 = Martignoni+, 2009RAA.....9.1270M 2009RAA.....9.1270M
12 = Niarchos+1998, J/A+AS/133/7
13 = Poro+, 2021ARep...65..543P 2021ARep...65..543P
14 = Tanriver, 2014NewA...28...79T 2014NewA...28...79T
15 = Elkhateeb+, 2014NewA...32...10E 2014NewA...32...10E
16 = Kriwattanawong+2017, J/PASJ/69/62
17 = Alton & Nelson, 2018MNRAS.479.3197A 2018MNRAS.479.3197A
18 = Kjurkchieva & Ibryamov, 2020SerAJ.200...19K 2020SerAJ.200...19K
19 = Elkhateeb+, 2014NewA...28...85E 2014NewA...28...85E
20 = Zola+, 2005AcA....55..389Z 2005AcA....55..389Z
21 = Kjurkchieva+, 2018PASA...35....8K 2018PASA...35....8K
22 = Devarapalli & Jagirdar, 2017AcAau.134..303D 2017AcAau.134..303D
23 = Dimitrov & Kjurkchieva, 2015, J/MNRAS/448/2890
24 = Kreiner+, 2003A&A...412..465K 2003A&A...412..465K
25 = Kjurkchieva+, 2019RAA....19...14K 2019RAA....19...14K
26 = Kiron+, 2011RAA....11.1469K 2011RAA....11.1469K
27 = Shanti Priya+, 2014RAA....14.1166S 2014RAA....14.1166S
28 = Kjurkchieva+, 2016RAA....16..135K 2016RAA....16..135K
29 = Zhu+2013, J/AJ/145/39
30 = Gao+ 2017NewA...56...10G 2017NewA...56...10G
31 = Joshi+, 2016RAA....16...63J 2016RAA....16...63J
32 = Acerbi+, 2022NewA...9701873A 2022NewA...9701873A
33 = Rattanamala+ 2024NewA..10802162R 2024NewA..10802162R
34 = Elkhateeb & Nouh, 2015NewA...34...47E 2015NewA...34...47E
35 = Deb & Singh, 2011, J/MNRAS/412/1787
36 = Bulut+, 2018NewA...58...90B 2018NewA...58...90B
37 = Kjurkchieva+, 2021NewA...8401401K 2021NewA...8401401K
38 = Yasarsoy & Yakut, 2013, J/AJ/145/9
39 = Yang+2019, J/AJ/157/111
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History:
From electronic version of the journal
(End) Prepared by [AAS], Robin Leichtnam CDS] 21-Nov-2025