New absolute magnitude calibrations for W Ursa Majoris type binaries

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dc.authoridBilir, Selcuk/0000-0003-3510-1509
dc.authoridYaz Gokce, Esma/0000-0003-0958-2935
dc.contributor.authorEker, Z.
dc.contributor.authorBilir, S.
dc.contributor.authorYaz, E.
dc.contributor.authorDemircan, O.
dc.contributor.authorHelvaci, M.
dc.date.accessioned2025-01-27T20:43:45Z
dc.date.available2025-01-27T20:43:45Z
dc.date.issued2009
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractParallaxes of W UMa stars in the Hipparcos catalogue have been analyzed. 31 W UMa stars. which have the most accurate parallaxes (sigma(pi)/pi < 0.15) which are neither associated with a photometric tertiary nor with evidence of a Visual companion, were selected for re-calibrating the Period-Luminosity-Color (PLC) relation of W UMa stars. Using the Lutz-Kelker (LK) bias corrected (most probable) parallaxes. periods (0.26 < P < 0.87, P in days), and colors (0.04 < (B - V)(0) < 1.28) of the 31 selected W UMa, the PLC relation have been revised and re-calibrated. The difference between the old (revised but no( bias corrected) and the new (LK bias corrected) relations are almost negligible in predicting the distances of W UMa stars Up to about 100 pc. But, it increases and may become intolerable as distances of stars increase. Additionally, using (J - H)(0) and (H -K(s))(0) colors from 2MASS (Two Micron All Sky Survey) data, a PLC relation working with infrared data was derived. It can be used with infrared colors in the range -0.01 < (J-H)(0) < 0.58, and -0.10 < (H - K(s))(0) < 0.18. Despite of the fact that the 2MASS data refer to single epoch observations which are not guaranteed to be taken at maximum brightness of the W UMa stars. the established relation has been found surprisingly consistent and reliable in predicting LK corrected distances of W UMa stars. (C) 2009 WILEY-VCH Verlag GmbH & Co, KGaA, Weinheim
dc.description.sponsorshipTUBITAK [104T508, 106T688]; National Aeronautics and Space Administration
dc.description.sponsorshipThis work has been partially supported by TUBITAK 104T508 and 106T688. We Would also like to thank Prof. Dr. Utku Coskunoglu and Basar Coskunoglu correcting the English grammar and linguistics of the manuscript. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the NASA/IPAC Extra, galactic Database (NED) which is operated by the Jet Propulsion Laboratory. California Institute of Technology, under contract with the National Aeronautics and Space Administration.
dc.identifier.doi10.1002/asna.200811041
dc.identifier.endpage76
dc.identifier.issn0004-6337
dc.identifier.issue1
dc.identifier.scopus2-s2.0-58149308546
dc.identifier.scopusqualityQ3
dc.identifier.startpage68
dc.identifier.urihttps://doi.org/10.1002/asna.200811041
dc.identifier.urihttps://hdl.handle.net/20.500.12428/24357
dc.identifier.volume330
dc.identifier.wosWOS:000262682700009
dc.identifier.wosqualityQ3
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherWiley-V C H Verlag Gmbh
dc.relation.ispartofAstronomische Nachrichten
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WoS_20250125
dc.subjectbinaries: eclipsing
dc.subjectstars: distances
dc.subjectstars: fundamental parameters
dc.titleNew absolute magnitude calibrations for W Ursa Majoris type binaries
dc.typeArticle

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