Magnetic activity and orbital period variation of the eclipsing binary KV Gem

Zhang, Liyun; Pi, Qingfeng; Yang, Yuangen; Li, Zhongmu

doi:10.1016/j.newast.2013.09.002

Cited by 7 publications

(1 citation statement)

References 36 publications

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“…Moreover, the former may possibly result in the short-period oscillation of the O − C curve, which will be investigated further in our future observation. This kind of variation occurs in other contact binaries, such as CK Boo (Yang et al 2012), DF CVn (Dai et al 2011), KV Gem (Zhang et al 2014), DZ Psc (Yang et al 2013) and GSC 3576-0170 (Zhang et al 2010), whose magnetic activity may possibly result in the short-period oscillation.…”

Section: Intrinsic Light Variabilitymentioning

confidence: 90%

OO Aquilae: a solar-type contact binary with intrinsic light curve changes

Wei

Yang

et al. 2016

Res. Astron. Astrophys.

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New multi-color photometry of the solar-type contact binary OO Aql was obtained in 2012 and 2013, using the 60 cm telescope at Xinglong Station of the National Astronomical Observatories, Chinese Academy of Sciences. From two sets of light curves LC1 and LC2, photometric models were performed by using the 2003 version of the Wilson-Devinney code. The overcontact factor of the binary system was determined to be f = 37.0(±0.5)%. The intrinsic variability of this binary occurs in light maxima and minima, which could result from a possible third component and magnetic activity of the late type components. Based on all available light minimum times, the orbital period may change in a complicated mode, i.e., sudden period jumps or continuous period variations. The period of OO Aql may possibly undergo a secular period decrease with a rate of dP/dt = −3.63(±0.30) × 10−8 d yr−1, superimposed by two possible cyclic variations in the O – C curve. The long-term period decrease may be interpreted as conserved mass transfer from the more massive component to the less massive one. The 21.5-yr oscillation may be attributed to cyclic magnetic activity, and the 69.3-yr one may result from the light-time effect of an unseen tertiary body.

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Section: Intrinsic Light Variabilitymentioning

confidence: 90%

OO Aquilae: a solar-type contact binary with intrinsic light curve changes

Wei

Yang

et al. 2016

Res. Astron. Astrophys.

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The multi-band CCD photometric investigation of short-period eclipsing binary V1044 Her

Zhang

Han

et al. 2016

New Astronomy

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Photometric Study of Two Totally Eclipsing Contact Binaries: V789 Her and V1007 Cas

Li¹,

Xia²,

Hu³

et al. 2018

PASP

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Two sets of V and R c light curves of V789 Her and one complete set of BVR c I c light curves of V1007 Cas were observed and presented. By analyzing all these light curves together with the Sloan g′i′ light curves observed by Kjurkchieva et al., we determined that both systems are W-subtype contact binaries and that V789 Her is a medium contact system, while V1007 Cas is a shallow contact system. Because the two binaries show totally eclipsing primary minima, the photometric results are reliable. In addition, the light curves of the two systems are asymmetric, requiring a dark spot on the primary or the secondary component in the modeling. By compiling all available times of minimum light including literatures, SuperWASP archive and ours, we analyzed the orbital period variations. We derived that the O−C diagram of V789 Her displays a periodic oscillation whose period and amplitude are 29.2 years and 0.0179 days and the period of V1007 Cas exhibits a continuous decrease at dP/dt=−1.78(±0.09)×10 −7 days yr −1 . The cyclic period modulation of V789 Her is probably attributed to the light travel time effect via a tertiary companion with very small mass. The continuous period decrease of V1007 Cas may result from the mass transfer between the two components. However, we cannot rule out the possibility of angular momentum loss because V1007 Cas shows strong magnetic activity. By analyzing the evolutionary status of the components of the two systems, we determined that they exhibit typical characteristics of other W-subtype contact binaries.

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Magnetic activity and orbital period variation of the eclipsing binary KV Gem

Cited by 7 publications

References 36 publications

OO Aquilae: a solar-type contact binary with intrinsic light curve changes

OO Aquilae: a solar-type contact binary with intrinsic light curve changes

The multi-band CCD photometric investigation of short-period eclipsing binary V1044 Her

Photometric Study of Two Totally Eclipsing Contact Binaries: V789 Her and V1007 Cas

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