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Evolution of binary stars with mass loss

Published online by Cambridge University Press:  14 August 2015

Janusz Ziółkowski
Janusz Ziółkowski*
Affiliation:
N. Copernicus Astronomical Center Polish Academy of Sciences ul. Bartycka 18, 00-716 Warsaw, Poland

Abstract

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Three situations involving mass loss from binary systems are discussed. (1) Non-conservative mass exchange in semi-detached binaries. No quantitative estimate of this mechanism is possible at present. (2) Common envelope binaries. There are both theoretical and observational indications that this phase of evolution happens to many systems, even to some that are not very close initially (orbital periods ~ years). (3) Stellar winds in binaries. Observational evidence suggests that stellar winds from components of close binaries (especially semi-detached) are significantly stronger than from single stars at the same location in the H-R diagram. Theoretical arguments indicate that in some cases stellar wind may stabilize the component of a binary against the Roche lobe overflow. In some cases there is weak evidence of an anisotropy in the stellar wind.

Type
Session 7: Evolution with Mass Loss: Double Stars
Information
Symposium - International Astronomical Union , Volume 83: Mass Loss and Evolution of O-Type Stars , 1979 , pp. 383 - 399
Copyright
Copyright © Reidel 1979 

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