The photometric study of a neglected near contact binary: BS vulpeculae

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dc.contributor.author Zhu, L.-Y.
dc.contributor.author Zejda, Miloslav
dc.contributor.author Mikulášek, Zdeněk
dc.contributor.author Liška, Jiří
dc.contributor.author Qian, Sheng-Bang
dc.contributor.author de Villiers, Stefanus Nicholas
dc.date.accessioned 2012-08-28T09:13:48Z
dc.date.available 2012-08-28T09:13:48Z
dc.date.issued 2012
dc.identifier.citation The astronomical journal. 2012, vol. 144, no. 2, art. no. 37. cs
dc.identifier.issn 0004-6256
dc.identifier.issn 1538-3881
dc.identifier.uri http://hdl.handle.net/10084/94964
dc.description.abstract We present a detailed study of the close eclipsing binary BS Vulpeculae. Although it is relatively bright (V: 10.9-11.6 mag) and belongs to short-periodic variable stars (P = 0.48 days), it is rather neglected. To perform a thorough period analysis, we collected all available photometric observations that span the time interval of 1898-2010. Observations include archive photographic plate measurements and visually determined eclipse minima timings done in 1979-2003, which were later shown to be biased to accommodate the existing linear ephemeris. Applying our own direct period analysis we found a well-defined shortening of the orbital period of dP/dt = –6.70(17) × 10–11 = –2.11(6) ms yr–1, which implies a continual mass flow from the primary to the secondary component. Using the 2003 version of the Wilson-Van Hamme code, our new complete BV(IR)C light curves were analyzed and the physical parameters of the system were derived. We found that BS Vul is a near contact binary system with the primary component filling its critical Roche lobe. The luminosity enhancement on the left shoulder of the secondary minimum shown in the light curves can be explained as a result of a persistent hot spot on the secondary due to the mass transfer from the primary component to the secondary one and heating the facing hemisphere of the secondary component, which is consistent with our result of period analysis. With the period decrease, BS Vul will evolve toward the contact phase. It is another good observational example as predicted by the theory of thermal relaxation oscillations. cs
dc.language.iso en cs
dc.publisher Institute of Physics Publishing cs
dc.relation.ispartofseries The astronomical journal cs
dc.relation.uri http://dx.doi.org/10.1088/0004-6256/144/2/37 cs
dc.subject binaries cs
dc.subject eclipsing cs
dc.subject stars: individual (BS Vul) cs
dc.subject stars: evolution cs
dc.title The photometric study of a neglected near contact binary: BS vulpeculae cs
dc.type article cs
dc.identifier.location Není ve fondu ÚK cs
dc.identifier.doi 10.1088/0004-6256/144/2/37
dc.type.status Peer-reviewed cs
dc.description.source Web of Science cs
dc.description.volume 144 cs
dc.description.issue 2 cs
dc.description.firstpage art. no. 37 cs
dc.identifier.wos 000306299900046

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