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On the evolution of massive close binaries

Published online by Cambridge University Press:  26 May 2016

Norbert Langer ,
Stephan Wellstein  and
Jelena Petrovic
Norbert Langer
Affiliation:
Sterrekundig Instituut, Universiteit Utrecht, Princetonplein 5, NL-3584 CC Utrecht, Nederland
Stephan Wellstein
Affiliation:
Lehrstuhl Astrophysik, Institut für Physik, Universität Potsdam, Am Neuen Palais 10, D-14414 Potsdam, BRD
Jelena Petrovic
Affiliation:
Sterrekundig Instituut, Universiteit Utrecht, Princetonplein 5, NL-3584 CC Utrecht, Nederland

Abstract

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We discuss which fraction of the matter flowing to the companion during a Roche lobe overflow phase can actually be accreted by the secondary star. Employing new evolutionary models for massive close binaries which include the effects of rotation for both components as well as angular momentum accretion and spin-orbit coupling, we propose a physical model to calculate the accretion efficiency in Case A and B systems. We provide examples showing that both cases, high and low accretion efficiency, do occur within these models, as it seems required by observed post-mass transfer systems. Furthermore, we discuss late evolutionary stages of such binaries, with emphasis on the formation of compact objects: what are their spin rates, which systems can produce black holes, which gamma-ray bursts?

Type
Part 2. Interiors of Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 275 - 280
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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