CCD Photometric Study and Period Investigation of V508 Oph

Xiang, Fu-Yuan; Yu, Yun-Xia; Xiao, Ting-Yu

doi:10.1088/0004-6256/149/2/62

Cited by 16 publications

(1 citation statement)

References 20 publications

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“…Compared with possible sinusoidal change (Lee et al 2007), the cyclic oscillations in O−C diagram of much more CCD times were usually explained by the light-travel time effect via the presence of a third body (Liao & Qian 2010;Qian et al 2011Qian et al , 2012Zhu et al 2013aZhu et al , 2013bQian et al 2015). The properties are similar to some A-type total-eclipse binaries, such as AU Tau (Xiang et al 2015a;Tvardovskyi et al 2018), V508 Oph (Xiang et al 2015b), EQ Tau (Li et al 2014).…”

Section: Discussionmentioning

confidence: 97%

New Photometric Investigations of G-type Contact Binary TU Boo

Wang

Meng

Jiang

et al. 2023

Res. Astron. Astrophys.

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Two sets of CCD photometric observations for contact binary TU Boo were obtained in 2020 and 2021, respectively. Different from its asymmetric light curves published from the literature, our BV RcIc-band curves show that the heights of maximum are almost equal. These distortions of light curves possibly indicate that the components have been active in past 25 yr, but they are stable in the last two years. For total-eclipse binary TU Boo, due to some star-spots on the surface of the components, the physical structure obtained by many investigators are different. Therefore, the symmetric multi-color light curves in 2020, 2021are important for understanding configuration and evolution for this system. By using the Wilson–Devinney (2013) program, it is confirmed that TU Boo is an A-type shallow-contact binary with the temperature difference of ∆T = 152K and fill-out of f = 14:67%. In the O–C diagram of orbital period analysis, a cyclic oscillation superimposed on a continuous decrease was determined. The long-term decreasing is often explained by the mass transfer from the more massive star to less massive one, this system will evolve into a deeper contact binary with time. The cyclic oscillations computed from much more CCD times of light minimum maybe result from the light-travel time effect via the presence of a third body. These characters of structure, evolution and ternary belong to typical A-type W UMa binaries with spectral G.

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Section: Discussionmentioning

confidence: 97%

New Photometric Investigations of G-type Contact Binary TU Boo

Wang

Meng

Jiang

et al. 2023

Res. Astron. Astrophys.

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The contact binary V344 Lacertae: is it a triple system?

Liu

Qian

et al. 2020

Astrophys Space Sci

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The first multi-color photometric study of the short-period contact eclipsing binary DE Lyn

et al. 2016

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We observed the contact eclipsing binary of DE Lyn using SARA 0.9 m telescope at Kitt Peak National Observatory on February 9, 11, and 27, 2015. In this study, we obtained the first full phase coverage BVRI CCD light curves, analyzed the orbital period variation, and extracted the orbital parameters. We calculated the linear and quadratic ephemeris, and thereby found that DE Lyn has a decreasing orbital period rate of −5.1(±0.4)×−5.1(±0.4)× 10−7 days/year. We assume this decreasing trend is the result of the more massive component (secondary) transferring mass to the less massive component (primary), and we obtained a mass transfer rate of dm/dt=7.06×10−7M⊙/yeardm/dt=7.06×10−7M⊙/year. By using the updated Wilson \u26 Devinney program, we found the orbital parameters of DE Lyn, which, in turn, enabled us to calculate the low degree of contact factor as f = 9.02( ± 0.01)%. In the future, its degree of contact will continue to increase and will evolve into an over-contact system

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CCD Photometric Study and Period Investigation of V508 Oph

Cited by 16 publications

References 20 publications

New Photometric Investigations of G-type Contact Binary TU Boo

New Photometric Investigations of G-type Contact Binary TU Boo

The contact binary V344 Lacertae: is it a triple system?

The first multi-color photometric study of the short-period contact eclipsing binary DE Lyn

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