Modelling the components of binaries in the Hyades: the dependence of the mixing-length parameter on stellar mass

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dc.authoridYakut, Kadri/0000-0003-2380-9008
dc.contributor.authorYildiz, M.
dc.contributor.authorYakut, K.
dc.contributor.authorBakis, H.
dc.contributor.authorNoels, A.
dc.date.accessioned2025-01-27T20:27:05Z
dc.date.available2025-01-27T20:27:05Z
dc.date.issued2006
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractWe present our findings based on a detailed analysis of the binaries of the Hyades, in which the masses of the components are well known. We fit the models of the components of a binary system to observations so as to give the observed total V and B-V of that system and the observed slope of the main sequence in the corresponding parts. According to our findings, there is a very definite relationship between the mixing-length parameter and the stellar mass. The fitting formula for this relationship can be given as alpha = 9.19 (M/M-circle dot-0.74)(0.053)-6.65, which is valid for stellar masses greater than 0.77 M-circle dot. While no strict information is gathered for the chemical composition of the cluster, as a result of degeneracy in the colour-magnitude diagram, by adopting Z = 0.033 and using models for the components of 70 Tau and theta(2) Tau we find the hydrogen abundance to be X = 0.676 and the age to be 670 Myr. If we assume that Z = 0.024, then X = 0.718 and the age is 720 Myr. Our findings concerning the mixing-length parameter are valid for both sets of the solution. For both components of the active binary system V818 Tau, the differences between radii of the models with Z = 0.024 and the observed radii are only about 4 per cent. More generally, the effective temperatures of the models of low-mass stars in the binary systems studied are in good agreement with those determined by spectroscopic methods.
dc.identifier.doi10.1111/j.1365-2966.2006.10275.x
dc.identifier.endpage1948
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.issue4
dc.identifier.scopus2-s2.0-33744550598
dc.identifier.scopusqualityQ1
dc.identifier.startpage1941
dc.identifier.urihttps://doi.org/10.1111/j.1365-2966.2006.10275.x
dc.identifier.urihttps://hdl.handle.net/20.500.12428/22576
dc.identifier.volume368
dc.identifier.wosWOS:000237812700040
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 : abundances
dc.subjectbinaries : eclipsing
dc.subjectstars : evolution
dc.subjectstars : interiors
dc.subjectopen clusters and associations : individual : Hyades
dc.titleModelling the components of binaries in the Hyades: the dependence of the mixing-length parameter on stellar mass
dc.typeArticle

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