Photometric observations and orbital period variations of HS 0705 + 6700 and NY Vir

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dc.contributor.authorÇamurdan C.M.
dc.contributor.authorZengin Çamurdan D.
dc.contributor.authorIbanoglu C.
dc.date.accessioned2019-10-27T08:33:07Z
dc.date.available2019-10-27T08:33:07Z
dc.date.issued2012
dc.departmentEge Üniversitesien_US
dc.description.abstractWe present photometric observations of two post-common-envelope stars, NY Vir (=PG 1336-018) and HS 0705 + 6700. The V band CCD observation of NY Vir was performed by a 40 cm telescope at Ege University Observatory and the R band observations of HS 0705 + 6700 were performed by 100 cm telescope at TÜBTAK National Observatory. The new light curves were analyzed by the WD code and the physical parameters of stars were determined. We obtained new mid-eclipse timings for HS 0705 + 6700 and combined them with those previously published data. The analysis of the O-C residuals yields a period of about 8.06 ± 0.28 yr and an amplitude of 98.5 s for the system HS 0705 + 6700, which is attributed to the third star physically bounded to the evolved eclipsing pair. A mass function of 1.2 × 10-4 M? for the third star is obtained. The existence of a third star is also confirmed by the light curve analysis, indicating light contribution of about 0.043 at phase 0.25 in R-bandpass of the eclipsing pair. Using mass-luminosity relationship of the low mass stars we estimate a mass of 0.12 M? with an orbital inclination of about 20°. The O-C residuals obtained for the system NY Vir were represented by a downward parabola which indicates orbital period decrease in the system. Using the coefficient of quadratic term we calculate a rate of orbital period decrease of about dP/dt = -4.09 × 10-8days yr-1. The period decrease we have measured in NY Vir may be explained by angular momentum loss from the binary system. © 2011 Elsevier B.V. All rights reserved.en_US
dc.description.sponsorship2006/FEN/004en_US
dc.description.sponsorshipThe authors thank Ege University observatory for allowing us telescope times. We also thank TÜBİTAK for a partial support using T100 telescope with project number 10CT100-98. This study forms part of the Ph.D. thesis of CMÇ and was supported by the Ege University Research Project (2006/FEN/004). The authors are grateful to Prof. Dr. Ö.L. Deg^irmenci for helping the period variation analysis ( Deg^irmenci, 2011 ). --en_US
dc.identifier.doi10.1016/j.newast.2011.08.004
dc.identifier.endpage330en_US
dc.identifier.issn1384-1076
dc.identifier.issn1384-1076en_US
dc.identifier.issue3en_US
dc.identifier.scopusqualityQ3en_US
dc.identifier.startpage325en_US
dc.identifier.urihttps://doi.org/10.1016/j.newast.2011.08.004
dc.identifier.urihttps://hdl.handle.net/11454/26659
dc.identifier.volume17en_US
dc.indekslendigikaynakScopusen_US
dc.language.isoenen_US
dc.relation.ispartofNew Astronomyen_US
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanıen_US
dc.rightsinfo:eu-repo/semantics/closedAccessen_US
dc.subjectBinariesen_US
dc.subjectEclipsing-starsen_US
dc.subjectIndividual(HS 0705 + 6700, NY Vir)en_US
dc.subjectStarsen_US
dc.titlePhotometric observations and orbital period variations of HS 0705 + 6700 and NY Viren_US
dc.typeArticleen_US

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