Absolute dimensions and apsidal motion of the eccentric binary PT Velorum

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dc.authoridBAKIS, VOLKAN/0000-0002-3125-9010
dc.contributor.authorBakis, V.
dc.contributor.authorBakis, H.
dc.contributor.authorDemircan, O.
dc.contributor.authorEker, Z.
dc.date.accessioned2025-01-27T20:59:47Z
dc.date.available2025-01-27T20:59:47Z
dc.date.issued2008
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractHigh-resolution (lambda/d lambda similar to 41 000) echelle spectra of the eccentric binary system PT Vel were analysed. Precise spectroscopic orbital elements of the system were obtained by means of cross-correlation technique. According to the solution of radial velocities with Hipparcos and All Sky Automated Survey-3 (ASAS-3) light curves, PT Vel consists of two main-sequence stars with masses M-1 = 2.198 +/- 0.016 M-circle dot, M-2 = 1.626 +/- 0.009 M-circle dot, radii R-1 = 2.094 +/- 0.020 R-circle dot, R-2 = 1.559 +/- 0.020 R-circle dot and temperatures T-eff1 = 9250 +/- 150 K, T-eff2 = 7650 +/- 200 K separated from each other by A = 9.74 +/- 0.02 R-circle dot in an orbit inclined 88.2 degrees +/- 0.5. The projected rotational velocities of component stars were found to be (v sin i)(1) = 63 +/- 2 and (v sin i)(2) = 40 +/- 3 km s(-1) from the comparison of observed spectra with synthetic spectra which were calculated using model atmospheres. Our measurements of the projected rotational velocities indicate that both stars rotate synchronously. Analysis of longitude of periastron values obtained from light-curve analysis from different photometric sets of this moderately eccentric system (e = 0.127 +/- 0.006) has revealed a significant motion of the line of apsides of (w) over dot = 0.0097 +/- 0 degrees.0004 cycle(-1) corresponding to an apsidal motion period of U = 182.2 +/- 8.4 yr. The contribution from general relativity effects is moderate (similar to 9 per cent). A comparison with predictions from interior structure models shows the real stars to be more concentrated in mass than expected. Comparison of absolute dimensions with theoretical isochrones yielded an age of the system of 400 +/- 40 Myr.
dc.identifier.doi10.1111/j.1365-2966.2007.12822.x
dc.identifier.endpage1667
dc.identifier.issn0035-8711
dc.identifier.issue4
dc.identifier.scopus2-s2.0-40249104726
dc.identifier.scopusqualityQ1
dc.identifier.startpage1657
dc.identifier.urihttps://doi.org/10.1111/j.1365-2966.2007.12822.x
dc.identifier.urihttps://hdl.handle.net/20.500.12428/26831
dc.identifier.volume384
dc.identifier.wosWOS:000253711700039
dc.identifier.wosqualityQ1
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherBlackwell Publishing
dc.relation.ispartofMonthly Notices of The Royal Astronomical Society
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WoS_20250125
dc.subjectbinaries : eclipsing
dc.subjectbinaries : spectroscopic
dc.subjectstars : evolution
dc.subjectstars : fundamental parameters
dc.subjectstars : individual : PT Velorum
dc.titleAbsolute dimensions and apsidal motion of the eccentric binary PT Velorum
dc.typeArticle

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