Absolute dimensions and apsidal motion of the eccentric binary V731 Cephei

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dc.authoridBilir, Selcuk/0000-0003-3510-1509
dc.authoridSlechta, Miroslav/0000-0002-6819-2331
dc.authoridLee, Jae W/0000-0002-8756-0195
dc.authoridBAKIS, VOLKAN/0000-0002-3125-9010
dc.contributor.authorBakis, V.
dc.contributor.authorZejda, M.
dc.contributor.authorBulut, I.
dc.contributor.authorWolf, M.
dc.contributor.authorBilir, S.
dc.contributor.authorBakis, H.
dc.contributor.authorDemircan, O.
dc.date.accessioned2025-01-27T20:27:04Z
dc.date.available2025-01-27T20:27:04Z
dc.date.issued2008
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractA detailed analysis of new and existing photometric, spectroscopic and spatial distribution data of the eccentric binary V731 Cep was performed. Spectroscopic orbital elements of the system were obtained by means of cross-correlation technique. According to the solution of radial velocities with UBVRc and I-c light curves, V731 Cep consists of two main-sequence stars with masses M-1 = 2.577 (0.098) M-circle dot, M-2 = 2.017 (0.084) M-circle dot, radii R-1 = 1.823 (0.030) R-circle dot, R-2 = 1.717 (0.025) R-circle dot and temperatures T-eff1 = 10700 (200) K, T-eff2 = 9265 (220) K separated from each other by a = 23.27 (0.29) R-circle dot in an orbit with inclination of 88 degrees.70 (0.03). Analysis of the O-C residuals yielded a rather long apsidal motion period of U = 10000 (2500) yr compared to the observational history of the system. The relativistic contribution to the observed rates of apsidal motion for V731 Cep is significant (76 per cent). The combination of the absolute dimensions and the apsidal motion properties of the system yielded consistent observed internal structure parameter (log (k) over bar (2,obs) = -2.36) compared to the theory ( log (k) over bar (2,theo) = -2.32). Evolutionary investigation of the binary by two methods (Bayesian and evolutionary tracks) shows that the system is t = 133(26) Myr old and has a metallicity of [M/H] = -0.04(0.02) dex. The similarities in the spatial distribution and evolutionary properties of V731 Cep with the nearby (rho similar to 3 degrees.9) open cluster NGC 7762 suggest that V731 Cep could have been evaporated from NGC 7762.
dc.description.sponsorshipCOMU Scientific Research Foundation [BAP2008/37]; Ministry of Education of Czech Republic [MSM0021620860]; Czech Science Foundation [GA CR 205/06/0217]
dc.description.sponsorshipThe authors would like to thank Dr Antonio Cabrera-Lavers for his help in extracting extinction data from RC stars and to the referee, Professor E. F. Guinan, for his useful comments that improved the readability of this paper. This study is part of a project funded by COMU Scientific Research Foundation under project code BAP2008/37. The research of MW was supported by the Research Programme MSM0021620860 of the Ministry of Education of Czech Republic. Participation of MZ in this study was endorsed by the grant GA CR 205/06/0217 of the Czech Science Foundation.
dc.identifier.doi10.1111/j.1365-2966.2008.13757.x
dc.identifier.endpage407
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.issue1
dc.identifier.scopus2-s2.0-52949087515
dc.identifier.scopusqualityQ1
dc.identifier.startpage399
dc.identifier.urihttps://doi.org/10.1111/j.1365-2966.2008.13757.x
dc.identifier.urihttps://hdl.handle.net/20.500.12428/22569
dc.identifier.volume390
dc.identifier.wosWOS:000260528800056
dc.identifier.wosqualityQ1
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherOxford Univ Press
dc.relation.ispartofMonthly Notices of The Royal Astronomical Society
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WoS_20250125
dc.subjectbinaries: eclipsing
dc.subjectstars: early-type
dc.subjectstars: evolution
dc.subjectstars: fundamental parameters
dc.subjectstars: individual: V731 Cephei
dc.titleAbsolute dimensions and apsidal motion of the eccentric binary V731 Cephei
dc.typeArticle

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