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The Formation and Evolution of Symbiotic Stars

Published online by Cambridge University Press:  12 April 2016

R.F. Webbink
R.F. Webbink*
Affiliation:
Department of Astronomy, University of Illinois1011 W. Springfield Ave., Urbana, IL 61801, U.S.A

Abstract

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The evolutionary origins of symbiotic stars containing (i) disk-accreting main sequence stars, (ii) wind-fed, shell-burning white dwarfs, and (iii) disk-accreting neutron stars are described. Of particular interest are those white dwarf systems which have orbital periods too short to have escaped tidal mass transfer prior to becoming symbiotics. We show here that, under suitable circumstances, low-mass, long period binaries may undergo quasi-conservative mass transfer, rather than evolving through common envelope evolution to the cataclysmic variable state, thus accounting for the existence of these systems. Approximate expressions are given for the lifetimes, and relative efficiencies (mass accreted/mass of donor) for different modes of interaction among symbiotic binary systems.

Type
Session 5. Symbiotic Phenomena and Stellar Evolution. Conclusions.
Information
International Astronomical Union Colloquium , Volume 103: The Symbiotic Phenomenon , 1988 , pp. 311 - 321
Copyright
Copyright © Kluwer 1988

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