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Evolutionary Aspects of Circumstellar Matter in Binary Systems

Published online by Cambridge University Press:  14 August 2015

Miroslav Plavec
Miroslav Plavec*
Affiliation:
Dept. of Astronomy, Univ. of California, Los Angeles

Abstract

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Several groups of close binary stars are considered in an attempt to explain their present state as a consequence of a large-scale mass transfer or mass loss in the past: Algol-like semidetached binaries, some shell stars (AX Mon), some binary X-ray sources (Cen X-3, Her X-1), the recurrent nova T CrB, helium-rich binaries v Sgr and KS Per, and the symbiotic variables.

Algol-like binaries like U Sge cannot be products of a conservative case A of mass transfer; rather, mass loss from system and/or a temporary contact stage must be invoked. Nova T CrB as well as the symbiotic variables probably contain a mass-losing giant and a helium star, which again may be a product of a previous mass transfer of type B. Similarly, some of the X-ray sources may actually be binaries undergoing a second process of mass transfer. The systems v Sgr and KS Per may contain helium stars expanding to the right of the helium main sequence, while the other component may be a rather inactive main-sequence star. Some shell stars may be products of mass transfer. Mass loss from convective envelopes is also discussed.

Loss of mass and of angular momentum from many binary systems must be anticipated. Behavior of the mass-accreting stars may often be decisive for the appearance and evolution of the system.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 51: Extended Atmospheres and Circumstellar Matter in Spectroscopic Binary Systems , 1973 , pp. 216 - 259
Copyright
Copyright © Reidel 1973 

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