Determination of Age and Original Chemical Composition of Binary Stars

A numerical method is presented, which is able to determine quantitatively the age t and the initial abundances of helium and metals (Y 0 , Z 0 ) of a given binary system. Input data are simply the values of mass m , temperature T eff and surface gravity g , of both stars. The procedure works for de...

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Bibliographic Details
Published in:International Astronomical Union Colloquium 1993, Vol.137, p.472-473
Main Authors: Ferluga, S., Antillon, M.
Format: Article
Language:English
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Summary:A numerical method is presented, which is able to determine quantitatively the age t and the initial abundances of helium and metals (Y 0 , Z 0 ) of a given binary system. Input data are simply the values of mass m , temperature T eff and surface gravity g , of both stars. The procedure works for detached main-sequence binaries, and it does not require any preliminary hypothesis about surface abundances or age. It is assumed that the two stars evolve parallely with no interaction.
ISSN:0252-9211
DOI:10.1017/S0252921100018285