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A Model for the Galactic Population of Supersoft X-Ray Sources

Published online by Cambridge University Press:  12 April 2016

L. Yungelson ,
A. Tutukov ,
A. Fedorova ,
M. Livio  and
J. W. Truran
L. Yungelson
Affiliation:
Institute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya Str., 109017 Moscow, Russia
A. Tutukov
Affiliation:
Institute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya Str., 109017 Moscow, Russia
A. Fedorova
Affiliation:
Institute of Astronomy of the Russian Academy of Sciences, 48 Pyatnitskaya Str., 109017 Moscow, Russia
M. Livio
Affiliation:
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
J. W. Truran
Affiliation:
Department of Astronomy and Astrophysics, Enrico Fermi Institute of Physics, University of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, USA

Abstract

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Three major sub-populations of Galactic supersoft X-ray sources may exist: semi-detached binaries with main sequence or subgiant donors, and symbiotic binaries (~550, ~460, and ~600 objects, respectively). Each group contains both permanent and transient sources. The intrinsic and interstellar absorptions reduce the number of observable sources to ~25. We derive the distributions of the sources over orbital periods, masses of the components, and ‘on’-times. The rate at which white dwarfs in Galactic binaries reach MCh is ~ 3 10−5 yr−1. The rate of He-shell detonations which may lead to supernovae may be up to 3 10−4 yr−1.

Type
Supernovae & Supersoft X-Ray Sources
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 417 - 420
Copyright
Copyright © Kluwer 1996

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