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Symbiotic Binary Stars

Published online by Cambridge University Press:  07 August 2017

Scott J. Kenyon
Scott J. Kenyon*
Affiliation:
Harvard-Smithsonian Center for Astrophysics 60 Garden Street, Cambridge, MA 02138

Abstract

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This paper briefly reviews the physical properties of symbiotic stars: long-period interacting binaries composed of a red giant primary star and a hot companion. Two types of binaries produce symbiotic optical spectra: semi-detached systems with a main sequence secondary and detached systems with a white dwarf secondary. Semi-detached symbiotics resemble cataclysmic variables and Algol binaries, but on a much larger scale, and undergo dwarf nova-like eruptions. Wind accretion powers detached systems; occasional thermonuclear runaways produce symbiotic novae - distant cousins of classical novae.

Keywords

stars: binaries: symbioticsaccretion discsstars: mass loss
Type
Invited Papers
Information
Symposium - International Astronomical Union , Volume 151: Evolutionary Processes in Interacting Binary Stars , 1992 , pp. 137 - 146
Copyright
Copyright © Kluwer 1992 

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