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The Formation of White Dwarfs in Close Binary Systems*†

Published online by Cambridge University Press:  12 April 2016

Ronald F. Webbink
Ronald F. Webbink*
Affiliation:
Department of Astronomy, University of Illinois, Urbana, Illinois 61801

Abstract

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Three major modes of interaction in binary systems are identified, corresponding to (I) physical contact, (II) tidal mass loss from a star with a radiative envelope, and (III) tidal mass loss from a star with a convectlve envelope. The qualitative evolution of binary systems in each of these cases is outlined, leading to the formation of single white dwarfs, long-period remnants of quasi-conservative mass transfer, or short-period cataclysmic binaries. The origin of short-period double white dwarfs in a second phase of mass transfer is outlined. Implications for the frequency of different systems of these types, and of planetary nebulae with close binary nuclei, are discussed.

Type
Colloquium Session VII
Information
International Astronomical Union Colloquium , Volume 53: White Dwarfs and Variable Degenerate Stars , August 1979 , pp. 426 - 447
Copyright
Copyright © The University of Rochester 1979

Footnotes

*

Paper presented at IAU Colloquium No. 53, “White Dwarfs and Variable Degenerate Stars,” held at the University of Rochester, Rochester, New York, July 30 to August 2, 1979.

†

Research supported by National Science Foundation grant AST 78-12309.

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