A Photometric Study of the Neglected Eclipsing Binary Bs Cassiopeiae

Yang, Yuangen; Wei, J. Y.; He, Jiajia

doi:10.1088/0004-6256/136/2/594

Cited by 14 publications

(4 citation statements)

References 28 publications

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“…continuous period change was derived. This pattern of orbital period changes also appears in many other shallow contact binaries (e.g., Qian et al 2013a,b;Yang et al 2008Yang et al , 2010Li et al 2015a;Li et al 2015b). For late-type binary IO Cnc, the cyclic variation may be interpreted as due to the magnetic activity of one or both components (Applegate 1992).…”

Section: Discussionsupporting

confidence: 63%

The first photometric investigations of the G-type shallow contact binary IO Cnc

Liao

Xiao

et al. 2021

Res. Astron. Astrophys.

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IO Cnc was classified to be a new G-type (G0) W UMa-type eclipsing binary system. Our first multicolor photometric solutions show that IO Cnc is a new W-subtype shallow contact binary with a fill-out factor of f = 16.1% and a low mass ratio of q = 3.12 (or 1/q = 0.32). During orbital period investigations, a cyclic variation and a downward parabolic variation with a rate of (−1.28 ± 0.43) × 10−7 d yr−1 was discovered in the observed–calculated (O − C) curve. The cyclic variation was analyzed by the light travel time effect (LTTE) via a potential red dwarf companion star, an orbital semi-major axis shorter than 4.88 ± 0.82 AU was obtained. Finally, we collect physical parameters of a sample of 50 G-type shallow contact binaries (f ≤ 20%), it is suggested that most of the G-type shallow contact binaries are undergoing a long-term and periodic orbital period changes, especially more systems show long-term decreases. The long-term orbital period decrease indicates that IO Cnc is in a mass transferring from the more massive component to the less massive one. With the long-term decrease of the orbital period, this shallow contact binary will evolve into a deeper contact one.

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Section: Discussionsupporting

confidence: 63%

The first photometric investigations of the G-type shallow contact binary IO Cnc

Liao

Xiao

et al. 2021

Res. Astron. Astrophys.

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“…The stars seem not to be coeval to each other. However, it is well known that there are several binaries such as YY CrB (Essam et al 2010), BS Cas (Yang, Wei, & He 2008), VZ Tri (Yang 2010). All these samples exhibit the same behaviour.…”

Section: Dal and Sipahimentioning

confidence: 99%

The Nature of V1464 Aql: A New Ellipsoidal Variable with a δ Scuti Component

Dal

Sipahi

2013

Publ. Astron. Soc. Aust.

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Taking into account the results obtained from the models and analyses of the BVRI light curves, we discuss the nature of V1464 Aql. The analyses indicated that the mass ratio of the system is q = 0.71 ± 0.02, while the inclination of the system (i) is 38°.45 ± 0°.22. Taking the primary component's temperature as 7 420 ± 192 K, we found that the temperature of the secondary is 6 232 ± 161 K. The mass of the primary component was found to be 1.74 ± 0.05 M ࣻ , while it is 1.23 ± 0.01 M ࣻ for the secondary. The primary component's radius was found to be 2.10 ± 0.05 R ࣻ , while it was found as 1.80 ± 0.01 R ࣻ for the secondary. Revealing that the system should not exhibit any eclipses, we demonstrated that the main variation with large amplitude should be caused due to the ellipsoidal effect. Indeed, the Fourier analysis also supported the result. For the first time in the literature, we revealed that the primary component is a δ Scuti star. The period of pulsation was found to be 58.482 ± 0.002, 58.482 ± 0.001, 60.966 ± 0.002, and 60.964 ± 0.003 min in BVRI bands, respectively. We plotted V1464 Aql in the log(P orb )-log (P pulse ) plane. Using more than 160 binaries, whose one or both components are pulsating, we derived a new linear fit in the log (P orb )-log (P pulse ) plane for each type of binary. Using the linear fit of each group, we obtained new calibrations between log (P orb ) and log (P pulse ) for different types of pulsating stars. In addition, a calibration has been obtained for the first time for the pulsating stars with spectral types O and B. V1464 Aql seems to be located near the other ellipsoidal and close binaries. Thus, we listed V1464 Aql as a new candidate for the ellipsoidal variables with a δ Scuti component.

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“…We adjusted the orbital period as 0 d .318666. It is well known that several binaries of W UMa type such as YY CrB (Essam et al, 2010), BS Cas (Yang et al, 2008), VZ Tri (Yang, 2010), exhibit large the period variation due to the large mass transfer.…”

Section: Discussionmentioning

confidence: 99%