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Determination of Age and Original Chemical Composition of Binary Stars
Published online by Cambridge University Press: 12 April 2016
Abstract
A numerical method is presented, which is able to determine quantitatively the age t and the initial abundances of helium and metals (Y0, Z0) of a given binary system. Input data are simply the values of mass m, temperature Teff 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.
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- V. The changing interior
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- Copyright © Astronomical Society of the Pacific 1993