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Determination of Age and Original Chemical Composition of Binary Stars

Published online by Cambridge University Press:  12 April 2016

S. Ferluga  and
M. Antillon
S. Ferluga
Affiliation:
Dipartimento di Astronomia, Università di Trieste Via G.B. Tiepolo, 11 - I 34131 Trieste, Italy
M. Antillon
Affiliation:
Dipartimento di Astronomia, Università di Trieste Via G.B. Tiepolo, 11 - I 34131 Trieste, Italy

Abstract

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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.

Type
V. The changing interior
Information
International Astronomical Union Colloquium , Volume 137: Inside the Stars , 1993 , pp. 472 - 473
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

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