Light curve analysis of a new W UMa system GSC 3581-1856

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dc.contributor.authorBulut, I.
dc.contributor.authorBulut, A.
dc.contributor.authorGunes, M.
dc.contributor.authorDemircan, O.
dc.date.accessioned2025-01-27T20:29:21Z
dc.date.available2025-01-27T20:29:21Z
dc.date.issued2018
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractNew BVRI photometric observations covering seven minima times for the eclipsing binary GSC 3581-1856 were presented. The light curves in BVRI colours were analysed by using PHOEBE code for the system parameters. New minima times were used in revising the light elements. The system is found a W-type contact binary with mass ratio of q = 1.3362 +/- 0.0042 and a fill out parameter of f = 16.89 +/- 3.17%. The smaller and less massive component was found hotter component (T-1 similar or equal to 5590 K). Lower temperature (T-2 = 5295 K) of the mass accreting more massive component is probably due to a disk or envelope around this star. The original temperature of the more massive secondary component would be at least T-2 similar or equal to 5590K. The preliminary absolute dimensions (M-1 = 0.78 +/- 0.01 M-circle dot, M-2 = 1.05 +/- 0.01 M-circle dot, R-1 = 0.92 +/- 0.10 R-circle dot, R-2 = 1.05 +/- 0.20 R-circle dot, L-1 = 0.86 +/- 0.20 L-circle dot and L-2 = 1.00 +/- 0.20 L-circle dot) indicate a relatively young marginal contact binary for GSC 3581-1856 system. The present luminosity of the less massive but hotter component would be not much different from its main sequence luminosity, and thus its original mass was estimated to be slightly more than one solar mass. This means it could be transferred and/or lost about 30% of its original mass which place the system in relatively young system in contact phase. (C) 2017 Elsevier B.V. All rights reserved.
dc.description.sponsorshipTurkish TUBITAK [114F166]
dc.description.sponsorshipThe authors thank to anonymous referee who helped to improve the early version of the manuscript with his/her very useful comments. This work has been supported by the Turkish TUBITAK under the Grant No. 114F166.
dc.identifier.doi10.1016/j.newast.2017.08.001
dc.identifier.endpage95
dc.identifier.issn1384-1076
dc.identifier.issn1384-1092
dc.identifier.scopus2-s2.0-85026750340
dc.identifier.scopusqualityQ2
dc.identifier.startpage90
dc.identifier.urihttps://doi.org/10.1016/j.newast.2017.08.001
dc.identifier.urihttps://hdl.handle.net/20.500.12428/22917
dc.identifier.volume58
dc.identifier.wosWOS:000412787300011
dc.identifier.wosqualityQ4
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherElsevier Science Bv
dc.relation.ispartofNew Astronomy
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/closedAccess
dc.snmzKA_WoS_20250125
dc.subjectStars
dc.subjectBinaries
dc.subjectClose - binaries
dc.subjectEclipsing - stars
dc.subjectIndividual
dc.subjectGSC 3581-1856
dc.titleLight curve analysis of a new W UMa system GSC 3581-1856
dc.typeArticle

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