Absolute Dimensions and Apsidal Motion of the Young Detached System LT Canis Majoris

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dc.authoridBilir, Selcuk/0000-0003-3510-1509
dc.authoridBAKIS, VOLKAN/0000-0002-3125-9010
dc.contributor.authorBakis, Volkan
dc.contributor.authorBulut, Ibrahim
dc.contributor.authorBilir, Selcuk
dc.contributor.authorBakis, Hicran
dc.contributor.authorDemircan, Osman
dc.contributor.authorHensberge, Herman
dc.date.accessioned2025-01-27T20:29:22Z
dc.date.available2025-01-27T20:29:22Z
dc.date.issued2010
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractNew high-resolution spectra of the short-period (P similar to 1.76 days) young detached binary LT CMa are reported for the first time. By combining the results from an analysis of new radial-velocity curves and published light curves, we determine values for the masses, radii, and temperatures as follows: M-1 = 5.59 (0.20)M-circle dot, R-1 = 3.56 (0.07) R-circle dot, and T-eff1 = 17000 (500) K for the primary and M-2 = 3.36 (0.14)M-circle dot, R-2 = 2.04 (0.05) R-circle dot, and T-eff2 = 13140 (800) K for the secondary. Static absorbtion features apart from those coming from the close binary components were detected in the several spectral regions. If these absorbtion features are from a third star, as the light-curve solutions support, its radial velocity is measured to be RV3 = 70 (8) km s(-1) The orbit of the binary system has been proved to be eccentric (e = 0.059) and thus apsidal motion exists. The estimated linear advance in longitude of periastron corresponds to an apsidal motion of U = 69 +/- 5 yr for the system. The average internal structure constant, log k(2,obs) = -2.53 of LT CMa, is found to be smaller than its theoretical value of log k(2,theo) = -2.22, suggesting that the stars would have a more central concentration in mass. The photometric distance of LT CMa (d = 535 +/- 45 pc) is found to be much smaller than the distance of the CMa OB1 association (1150 pc), which rules out membership. A comparison with current stellar evolution models for solar metallicity indicates that LT CMa (35 Myr) is much older than the CMa OB1 association (3 Myr), confirming that LT CMa is not a member of CMa OB1. Kinematical and dynamical analyses indicate that LT CMa is orbiting the Galaxy in a circular orbit, and belongs to the young thin-disk population.
dc.description.sponsorshipScientific and Technological Research Council of Turkey (TUBITAK) [TBAG 149T449]; TUBITAK National Observatory [09ARTT150-431-0]
dc.description.sponsorshipThis work has been supported by the Scientific and Technological Research Council of Turkey (TUBITAK) under the Project Number: TBAG 149T449. Observations in this study are granted by The TUBITAK National Observatory under the Project Number: 09ARTT150-431-0. We thank to anonymous referee who helped to improve the early version of the manuscript with his/her very useful comments.
dc.identifier.doi10.1093/pasj/62.5.1291
dc.identifier.endpage1299
dc.identifier.issn0004-6264
dc.identifier.issn2053-051X
dc.identifier.issue5
dc.identifier.scopus2-s2.0-79251516114
dc.identifier.scopusqualityQ2
dc.identifier.startpage1291
dc.identifier.urihttps://doi.org/10.1093/pasj/62.5.1291
dc.identifier.urihttps://hdl.handle.net/20.500.12428/22923
dc.identifier.volume62
dc.identifier.wosWOS:000283885700020
dc.identifier.wosqualityQ2
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherOxford Univ Press
dc.relation.ispartofPublications of The Astronomical Society of Japan
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WoS_20250125
dc.subjectstars: binaries: eclipsing
dc.subjectstars: early-type
dc.subjectstars: evolution
dc.subjectstars: fundamental parameters
dc.subjectstars: individual (LT Canis Majoris)
dc.titleAbsolute Dimensions and Apsidal Motion of the Young Detached System LT Canis Majoris
dc.typeArticle

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