The First Photometric Study of NSVS 1461538: A New W-subtype Contact Binary with a Low Mass Ratio and Moderate Fill-out Factor

Kim, Hyoun-Woo; Kim, Chun-Hwey; Song, Mi-Hwa; Jeong, Min-Ji; Kim, Hye-Young

doi:10.5140/jass.2016.33.3.185

Cited by 4 publications

(3 citation statements)

References 37 publications

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“…In the figure, the top, middle, and bottom panels show plots of the q number distribution and the q-M diagrams of the more-and less-massive components, respectively. Kim et al (2016) investigated the q frequency distribution for 98 LMCBs among the 100 systems listed by Yıldiz & Doğan (2013), excluding two systems (V376 And and V535 Ara) with temperatures exceeding 8000 K. They showed A:W distribution ratios of 4:25, 29:7, and 16:17 for q q 0.4 log 0.4 > =-(…”

Section: Notementioning

confidence: 99%

Simultaneous Photometric and Spectroscopic Analysis of V505 Lacertae, a Photospherically and Chromospherically Active Contact Binary Star

Jeong,

Kim,

Hong

et al. 2024

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New BVR photometric and high-resolution spectroscopic observations of V505 Lac are presented with Transiting Exoplanet Survey Satellite (TESS) photometric data. The orbital period has experienced a secular decrease during the past 16 yr. A clear anticorrelation in the primary and secondary eclipse timing variation (PSETV) obtained from the TESS data is also identified. A double-lined radial velocity (RV) curve is secured, and the effective temperatures of the less- and more-massive stars (Stars 1 and 2, respectively) are measured. Using a spectral subtraction technique, excess emissions are detected in the time-series Ca ii H and K and Hα lines for Star 2. Simultaneous analysis of the light and RV curves using the Wilson–Devinney (WD) code reveals that V505 Lac is a photospherically and chromospherically active W-subtype contact binary system. The component-star masses and radii are determined to an accuracy of approximately 1%. The WD spot model is individually applied to 221 light curves segmented from the TESS data so as to derive the spot parameters of a cool spot on Star 2. The combined variations in both longitude and colatitude among the spot parameters appear to be strongly associated with those of both the anticorrelation in the PSETV and the O’Connell effect in the TESS light curves. Robust negative linear relationships between the PSETV anticorrelation size and the O’Connell effect magnitude are found for the first time. Mass–radius, mass–luminosity, and mass ratio–mass diagrams of contact binaries, along with the mass ratio frequency distribution, are presented in an attempt to elucidate the evolutionary characteristics of these systems.

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Section: Notementioning

confidence: 99%

Simultaneous Photometric and Spectroscopic Analysis of V505 Lacertae, a Photospherically and Chromospherically Active Contact Binary Star

Jeong,

Kim,

Hong

et al. 2024

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“…If the more massive component is cooler, the binary star is a W-type binary star (Binnendijk 1970(Binnendijk , 1977. Research has shown that when q ≥ 0.4, there are more W-type binaries than A-type; 0.25 ≤ q ≤ 0.4, there are a even distribution of W-type binaries and Atype ones; q<0.25, the number of A-type binaries are more than W-type binaries (Kim et al 2016). Zhang et al (2020) has presented the secondary stars of A-type binaries are evolved from initial more massive stars, while the ones of W-type are formed via mass transfer.…”

Section: Introductionmentioning

confidence: 99%

The first photometric investigation of the contact binary OQ Cam

Guo,

Li,

Xia

et al. 2020

Preprint

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The first charge-coupled device photometric light curves in B, V, R c , and I c bands of the short-period contact binary star OQ Cam are presented. Through analyzing the light curves with the Wilson-Devinney code, it is found that OQ Cam is a W-type shallow contact binary star with a contact degree of f =20.2%. Based on the O-C analyzing, the orbit period displays a long term increasing with a rate of dP/dt = 4.40×10 −7 day •year −1 . The increasing in orbit period can be interpreted by mass transfer from the less massive component to the more massive one. As the orbit period increasing, OQ Cam would evolve from the present shallow contact configuration to a none contact stage. So it may be a potential candidate to confirm the thermal relaxation oscillation theory.

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“…If the more massive component is cooler, the binary star is a W-type binary star (Binnendijk 1970(Binnendijk , 1977. Research has shown that when q ≥ 0.4, there are more W-type binaries than A-type; 0.25 ≤ q ≤ 0.4, there are an even distribution of W-type binaries and A-type ones; q<0.25, the number of A-type binaries are more than W-type binaries (Kim et al 2016). Zhang et al (2020) has presented the secondary stars of A-type binaries are evolved from initial more massive stars, while the ones of W-type are formed via mass transfer.…”

Section: Introductionmentioning

confidence: 99%

The first photometric investigation of the contact binary OQ Cam

Guo

Xia

et al. 2020

Res. Astron. Astrophys.

View full text Add to dashboard Cite

The first charge-coupled device photometric light curves in B, V, Rc , and Ic bands of the short-period contact binary star OQ Cam are presented. Through analyzing the light curves with the Wilson-Devinney code, it is found that OQ Cam is a W-type shallow contact binary star with a contact degree of f = 20.2%. Based on the O – C analyzing, the orbit period displays a long term increasing with a rate of dP/dt = 4.40 × 10−7 d yr−1. The increasing in orbit period can be interpreted by mass transfer from the less massive component to the more massive one. As the orbit period increases, OQ Cam would evolve from the present shallow contact configuration to a non-contact stage. So it may be a potential candidate to confirm the thermal relaxation oscillation theory.

show abstract

The First Photometric Study of NSVS 1461538: A New W-subtype Contact Binary with a Low Mass Ratio and Moderate Fill-out Factor

Cited by 4 publications

References 37 publications

Simultaneous Photometric and Spectroscopic Analysis of V505 Lacertae, a Photospherically and Chromospherically Active Contact Binary Star

Simultaneous Photometric and Spectroscopic Analysis of V505 Lacertae, a Photospherically and Chromospherically Active Contact Binary Star

The first photometric investigation of the contact binary OQ Cam

The first photometric investigation of the contact binary OQ Cam

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