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Binary Evolution Models with Rotation

Published online by Cambridge University Press:  26 May 2016

N. Langer,
S.-C. Yoon,
J. Petrovic and
A. Heger
N. Langer
Affiliation:
Astronomical Institute, P.O. Box 80000, NL-3508 TA Utrecht, The Netherlands
S.-C. Yoon
Affiliation:
Astronomical Institute, P.O. Box 80000, NL-3508 TA Utrecht, The Netherlands
J. Petrovic
Affiliation:
Astronomical Institute, P.O. Box 80000, NL-3508 TA Utrecht, The Netherlands
A. Heger
Affiliation:
Department of Astronomy and Astrophysics, Enrico Fermi Institute, The University of Chicago, 5640 S. Ellis Avenue, Chicago IL 60637, USA

Abstract

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We discuss the first available binary evolution models which include up-to-date rotational physics for both components, as well as angular momentum accretion and spin-orbit coupling. These models allow a self-consistent computation of the mass transfer efficiency during Roche-lobe overflow phases, and a determination of the transition from quasi-conservative to non-conservative evolution. Applications to massive binary systems lead to predictions for the spin rates of compact objects in binaries, and for the occurrence of gamma-ray bursts from collapsars in binaries. Rotational effects in accreting white dwarfs are found to stabilise the shell burning and decrease the carbon abundance in progenitor models for Chandrasekhar-mass Type Ia supernovae, and to potentially avoid a detonation of the white dwarf within the sub-Chandrasekhar mass scenario.

Information

Type
Session 4 Rotation and Stellar Evolution
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004, pp. 535 - 544
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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