Apsidal motion and photometric elements of the eccentric eclipsing binary KL CMa

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dc.contributor.authorBulut, I.
dc.date.accessioned2025-01-27T20:41:43Z
dc.date.available2025-01-27T20:41:43Z
dc.date.issued2008
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractThe Hipparcos and ASAS light curves of the recently discovered eccentric orbit binary KL CMa were analyzed by using the Wilson-Devinney program. The analysis of the light curves and all available minimum times have revealed that the system is detached, with the orbital eccentricity e = 0.131 +/- 0.007, the rate of change of the longitude of periastron (omega) over dot = 0.037 +/- 0.014 degrees cycle(-1), corresponding to an apsidal motion period of U = 46.9 +/- 17.7 yr. The apsidal motion of the system has been confirmed by the significant difference on the longitude of the periastron (omega) obtained from two light curves (Hipparcos and ASAS) in two different epochs. Preliminary absolute parameters of the components have been computed taking into account the result of light curves analysis. (C) 2007 Elsevier B.V. All rights reserved.
dc.identifier.doi10.1016/j.newast.2007.06.008
dc.identifier.endpage27
dc.identifier.issn1384-1076
dc.identifier.issue1
dc.identifier.scopus2-s2.0-34548433332
dc.identifier.scopusqualityQ2
dc.identifier.startpage24
dc.identifier.urihttps://doi.org/10.1016/j.newast.2007.06.008
dc.identifier.urihttps://hdl.handle.net/20.500.12428/24219
dc.identifier.volume13
dc.identifier.wosWOS:000250432600004
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 : close
dc.subjectstars : binaries : eclipsing
dc.subjectstars : individual : KL CMa
dc.titleApsidal motion and photometric elements of the eccentric eclipsing binary KL CMa
dc.typeArticle

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