The near-contact binary star RZ Dra revisited

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dc.contributor.authorErdem, A.
dc.contributor.authorZola, S.
dc.contributor.authorWiniarski, M.
dc.date.accessioned2025-01-27T20:41:49Z
dc.date.available2025-01-27T20:41:49Z
dc.date.issued2011
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractThis paper presents the absolute parameters of RZ Dra. New CCD observations were made at the Mt. Suhora Observatory in 2007. Two photometric data sets (1990 BV and 2007 BVRI) were analysed using modern light-curve synthesis methods. Large asymmetries in the light curves may be explained in terms of a dark starspot on the primary component, an A6 type star. Due to this magnetic activity, the primary component would appear to belong to the class of Ap-stars and would show small amplitude with delta Scuti-type pulsations. With this in mind, a time-series analysis of the residual light curves was made. However, we found no evidence of pulsation behaviour in RZ Dra. Combining the solutions of our light curves and Rucinski et al. (2000)'s radial velocity curves, the following absolute parameters of the components were determined: M(1) = 1.63 +/- 0.03 M(circle dot), M(2) = 0.70 +/- 0.02 M, R(1) = 1.65 +/- 0.02R(circle dot), R(2) = 1.15 +/- 0.02 R(circle dot), L(1) = 9.72 +/- 0.30 L(circle dot) and L(2) = 0.74 +/- 0.10 L(circle dot). The distance to RZ Dra was calculated as 400 +/- 25 pc, taking into account interstellar extinction. The orbital period of the system was studied using updated O-C information. It was found that the orbital period varied in its long-period sinusoidal form, superimposed on a downward parabola. The parabolic term shows a secular period decrease at a slow rate of 0.06 +/- 0.02 s per century and is explained by the mass loss via magnetized wind of the Ap-star primary. The tilted sinusoidal form of the period variation may be considered as an apparent change and may be interpreted in terms of the light-time effect due to the presence of a third body. (c) 2010 Elsevier B.V. All rights reserved.
dc.description.sponsorshipCanakkale Onsekiz Mart University Research Foundation
dc.description.sponsorshipThis study was supported by Canakkale Onsekiz Mart University Research Foundation. We thank Dr. Esin Soydugan for her useful comments and suggestions. We also thank caglar Puskullu and Naci Erkan for their assistance during observations at Canakkale Onsekiz Mart University Observatory.
dc.identifier.doi10.1016/j.newast.2010.06.006
dc.identifier.endpage11
dc.identifier.issn1384-1076
dc.identifier.issue1
dc.identifier.scopus2-s2.0-77954977599
dc.identifier.scopusqualityQ2
dc.identifier.startpage6
dc.identifier.urihttps://doi.org/10.1016/j.newast.2010.06.006
dc.identifier.urihttps://hdl.handle.net/20.500.12428/24246
dc.identifier.volume16
dc.identifier.wosWOS:000282116700002
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: binaries: eclipsing
dc.subjectStars: fundamental parameters
dc.subjectTechnique: photometry
dc.subjectStars: individual (RZ Dra)
dc.titleThe near-contact binary star RZ Dra revisited
dc.typeArticle

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