Dynamic Evolution of the Eclipsing Overcontact Binary Star System BI CVn

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dc.contributor.authorBulut, I.
dc.contributor.authorGunes, M.
dc.contributor.authorNehir, C.
dc.date.accessioned2026-02-03T12:02:21Z
dc.date.available2026-02-03T12:02:21Z
dc.date.issued2025
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractWe present a comprehensive analysis of BI CVn, an eclipsing overcontact binary system. New BVR photometric observations, combined with available spectroscopic data, were analyzed simultaneously using the Wilson-Devinney method to derive the orbital and physical parameters of the system. The resulting stellar parameters are M-1 = 0.58 +/- 0.01M(circle dot), M-2 = 1.42 +/- 0.02M(circle dot), R-1 = 0.88 +/- 0.01R(circle dot), R-2 = 1.31 +/- 0.01R(circle dot), with an orbital separation of a = 2.80 +/- 0.01R(circle dot). Based on all available CCD times of minimum light, including both ground-based and TESS observations, the (O - C) diagram of BI CVn was analyzed. The orbital period exhibits a long-term decrease at a rate of -2.3239 (+/- 0.0001) x 10(-8) day yr(-1), likely due to mass transfer from the more massive to the less massive component. Superimposed on this trend is a cyclic variation with a period of 56.84 +/- 0.08 yr, indicative of a light-travel time effect caused by a third body, whose estimated mass is 0.63 +/- 0.02M(circle dot). Using these derived parameters, we modeled the binary's evolution through non-conservative processes with the Binary Star Evolution code. The evolutionary tracks of the components were examined in multiple parameter planes, leading to an estimated merger timescale of approximately 2.70 Gyr.
dc.description.sponsorshipScientific and Technological Research Council of Turkiye (TUBITAK) [114F166]
dc.description.sponsorshipThe authors thank the anonymous referee who helped to improve the early version of the manuscript with his/her very useful comments. We gratefully acknowledge the observing time granted at the Ulupinar Observatory of Canakkale Onsekiz Mart University. This study utilized observational data obtained through a project supported by the Scientific and Technological Research Council of Turkiye (TUBITAK) under grant No. 114F166. This paper includes data collected by the Transiting Exoplanet Survey Satellite (TESS) mission. Funding for TESS is provided by the NASA Science Mission Directorate. TESS data presented in this work were obtained from the Mikulski Archive for Space Telescopes (MAST). This work also presents results from the Gaia mission, a project of the European Space Agency (ESA). Gaia data are processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for DPAC is provided by national institutions, in particular those participating in the Gaia MultiLateral Agreement (MLA). The Gaia mission website is: https://www.cosmos.esa.int/gaia, and the Gaia archive is accessible at: https://archives.esac.esa.int/gaia. Additionally, this research made use of the SIMBAD database, operated at CDS, Strasbourg, France, and NASA's Astrophysics Data System Bibliographic Services.
dc.identifier.doi10.1088/1674-4527/addded
dc.identifier.issn1674-4527
dc.identifier.issn2397-6209
dc.identifier.issue8
dc.identifier.scopus2-s2.0-105008876818
dc.identifier.scopusqualityQ2
dc.identifier.urihttps://doi.org/10.1088/1674-4527/addded
dc.identifier.urihttps://hdl.handle.net/20.500.12428/34712
dc.identifier.volume25
dc.identifier.wosWOS:001512071100001
dc.identifier.wosqualityQ2
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherIop Publishing Ltd
dc.relation.ispartofResearch in Astronomy and Astrophysics
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanı
dc.rightsinfo:eu-repo/semantics/closedAccess
dc.snmzKA_WOS_20260130
dc.subject(stars:) binaries: eclipsing
dc.subjectstars: fundamental parameters
dc.subjectstars: individual BI CVn
dc.titleDynamic Evolution of the Eclipsing Overcontact Binary Star System BI CVn
dc.typeArticle

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