A comprehensive photometric study of the Algol-type eclipsing binary: BG Pegasi

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dc.authoridPuskullu, Caglar/0000-0001-9213-0969
dc.authoridSoydugan, Faruk/0000-0002-5141-7645
dc.contributor.authorSoydugan, Esin
dc.contributor.authorSoydugan, Faruk
dc.contributor.authorSenyuz, T.
dc.contributor.authorPuskullu, C.
dc.contributor.authorDemircan, O.
dc.date.accessioned2025-01-27T20:24:36Z
dc.date.available2025-01-27T20:24:36Z
dc.date.issued2011
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractThis study presents new photometric observations of classical Algol type binary BC Peg with a delta Scuti component The light curve modeling was provided with the physical parameters of the component stars in the BC Peg system for the first time After modeling light curves in B and V filters, the eclipse and proximity effects were removed from the light curve to analyze intrinsic variations caused by the hotter component of the system Frequency analysis of the residuals light represents the multi-mode pulsation of the more massive component of the BC Peg system at periods of 0.039 and 0 047 clays Two frequencies could be associated with non-radial (l = 2) modes The total amplitude of the pulsational variability in the V light curve was found to be about 0 045 mag The long-term orbital period variation of the system was also investigated for the first time The O-C analysis indicates periodic variation superimposed on a downward parabola The secular period variation means that the orbital period of the system is decreasing at a rate of -5 5 seconds per century, probably due to the magnetic activity of the cooler component. The tilted sinusoidal O-C variation may be caused by the gravitational effect of an unseen component around the system (C) 2010 Elsevier B V All rights reserved
dc.description.sponsorshipTurkish Scientific and Technical Research Council [107T634]; Canakkale Onsekiz Mart University Research Foundation [2008/72]
dc.description.sponsorshipWe wish to thank the Turkish Scientific and Technical Research Council (Grant No 107T634) and Canakkale Onsekiz Mart University Research Foundation (Project No. 2008/72) for supporting this study.
dc.identifier.doi10.1016/j.newast.2010.08.003
dc.identifier.endpage78
dc.identifier.issn1384-1076
dc.identifier.issue2
dc.identifier.scopus2-s2.0-77956405829
dc.identifier.scopusqualityQ2
dc.identifier.startpage72
dc.identifier.urihttps://doi.org/10.1016/j.newast.2010.08.003
dc.identifier.urihttps://hdl.handle.net/20.500.12428/22288
dc.identifier.volume16
dc.identifier.wosWOS:000283407500004
dc.identifier.wosqualityQ3
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.subjectEclipsing - technique
dc.subjectPhotometry - stars
dc.subjectIndividual (BG Peg)
dc.titleA comprehensive photometric study of the Algol-type eclipsing binary: BG Pegasi
dc.typeArticle

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