A photometric study of eclipsing binary V351 Pegasi

Albayrak, B.; Djurašević, G.; Selam, S. O.; Atanacković-Vukmanović, O.; Yılmaz, M.

doi:10.1016/j.newast.2004.09.002

Cited by 8 publications

(2 citation statements)

References 6 publications

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“… References in . (1) Yang, Qian & Zhu (2005a); (2) Zhang, Zhang & Deng (2005); (3) Barone et al (1988); (4) Djurasevic et al (2004); (5) Ozdemir et al (2002); (6) Lu & Rucinski (1999); (7) Albayrak et al (2005); (8) Gurol (2005); (9) Hrivnak, Guinan & Lu (1995). …”

Section: Dynamical Stability Limitmentioning

confidence: 99%

The dynamical stability of W Ursae Majoris-type systems

Li¹,

Zhang²

2006

Monthly Notices of the Royal Astronomical Society

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Theoretical study indicates that a contact binary system would merge into a rapidly rotating single star due to tidal instability when the spin angular momentum of the system is more than a third of its orbital angular momentum. Assuming that W UMa contact binary systems rigorously comply with the Roche geometry and the dynamical stability limit is at a contact degree of about 70%, we obtain that W UMa systems might suffer Darwin's instability when their mass ratios are in a region of about 0.076--0.078 and merge into the fast-rotating stars. This suggests that the W UMa systems with mass ratio $q\leq0.076$ can not be observed. Meanwhile, we find that the observed W UMa systems with a mass ratio of about 0.077, corresponding to a contact degree of about 86% would suffer tidal instability and merge into the single fast-rotating stars. This suggests that the dynamical stability limit for the observed W UMa systems is higher than the theoretical value, implying that the observed systems have probably suffered the loss of angular momentum due to gravitational wave radiation (GR) or magnetic stellar wind (MSW).Comment: 4 pages, 3 figures, published in MNRAS (2006MNRAS.369.2001

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Section: Dynamical Stability Limitmentioning

confidence: 99%

The dynamical stability of W Ursae Majoris-type systems

Li¹,

Zhang²

2006

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Rucinski et al (2007) detected no additional component orbiting the binary, neither was one found spectroscopically by D' Angelo et al (2006). Albayrak et al (2005) obtained photometric data in the BV R bands and published a model which included spots. A low orbital inclination was found (i = 63 • ), the fill-out factor of f = 20.64 per cent and very similar effective temperatures of the components.…”

Section: V351 Pegmentioning

confidence: 99%