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Criterion for Dynamical Instability of Mass Transfer in Binary Evolution

Published online by Cambridge University Press:  12 April 2016

Zhanwen Han ,
Philipp Podsiadlowski  and
Christopher A. Tout
Zhanwen Han
Affiliation:
Yunnan Observatory, NAOC, CAS, Kunming 650011, P. R.China
Philipp Podsiadlowski
Affiliation:
Astrophysics, NAPL, Oxford University, Keble Road, Oxford OX1 3RH, UK
Christopher A. Tout
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK

Abstract

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Using Eggleton’s code, we performed a series of binary evolution calculations in order to investigate the criterion for dynamical instability of mass transfer in binaries. In these calculations, we took the donor’s mass on the zero-age main sequence (ZAMS) from 0.8 to 1.9 M⊙. For each mass, we systematically varied the mass of the core at the beginning of mass transfer and the mass of the companion star. We assumed that mass transfer was completely non-conservative and that all the mass that was lost from the system carried with it the orbital angular momentum of the accreting component. We found that the critical mass ratio, above which mass transfer is dynamically unstable, is from 1.1 to 1.3 in these red-giant binary systems.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 187: Exotic Stars as Challenges to Evolution , 2002 , pp. 297 - 302
Copyright
Copyright © Astronomical Society of the Pacific 2002

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