Kinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution

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dc.authoridBilir, Selcuk/0000-0003-3510-1509
dc.contributor.authorKaratas, Y
dc.contributor.authorBilir, S
dc.contributor.authorEker, Z
dc.contributor.authorDemircan, O
dc.date.accessioned2025-01-27T20:50:35Z
dc.date.available2025-01-27T20:50:35Z
dc.date.issued2004
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractThe kinematics of 237 chromospherically active binaries (CABs) were studied. The sample is heterogeneous with different orbits and physically different components from F to M spectral-type main-sequence stars to G and K giants and supergiants. The computed U, V, W space velocities indicate that the sample is also heterogeneous in velocity space. That is, both kinematically younger and older systems exist among the non-evolved main sequence and the evolved binaries containing giants and subgiants. The kinematically young (0.95 Gyr) subsample (N = 95), which is formed according to the kinematical criteria of moving groups, was compared with the rest (N = 142) of the sample (3.86 Gyr) to investigate any observational clues of binary evolution. Comparing the orbital period histograms between the younger and older subsamples, evidence was found supporting the finding of Demircan that the CABs lose mass (and angular momentum) and evolve towards shorter orbital periods. The evidence of mass loss is noticeable on the histograms of the total mass (M-h + M-c), which is compared between the younger (only N = 53 systems available) and older subsamples (only N = 66 systems available). The orbital period decrease during binary evolution is found to be clearly indicated by the kinematical ages of 6.69, 5.19 and 3.02 Gyr which were found in the subsamples according to the period ranges of log P less than or equal to 0.8, 0.8 < log P <= 1.7 and 1.7 < log P less than or equal to 3, respectively, among the binaries in the older subsample.
dc.identifier.doi10.1111/j.1365-2966.2004.07588.x
dc.identifier.endpage1092
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.issue3
dc.identifier.scopus2-s2.0-1942538981
dc.identifier.scopusqualityQ1
dc.identifier.startpage1069
dc.identifier.urihttps://doi.org/10.1111/j.1365-2966.2004.07588.x
dc.identifier.urihttps://hdl.handle.net/20.500.12428/25527
dc.identifier.volume349
dc.identifier.wosWOS:000220847700029
dc.identifier.wosqualityQ1
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherOxford Univ Press
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.subjectstars : activity
dc.subjectbinaries : spectroscopic
dc.subjectstars : chromospheres
dc.subjectstars : evolution
dc.subjectstars : kinematics
dc.titleKinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution
dc.typeReview Article

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