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Soft X-Ray Emission from Classical Novae in Outburst

Published online by Cambridge University Press:  12 April 2016

Sumner Starrfield ,
James W. Truran ,
Warren M. Sparks ,
Joachim Krautter  and
James MacDonald
Sumner Starrfield
Affiliation:
IGPP and Theoretical Division, Los Alamos National Laboratory and Department of Physics and Astronomy, Arizona State University
James W. Truran
Affiliation:
Department of Astronomy, University of Illinois
Warren M. Sparks
Affiliation:
Applied Theoretical Division, Los Alamos National Laboratory
Joachim Krautter
Affiliation:
Landessternwarte, Königstuhl
James MacDonald
Affiliation:
Landessternwarte, Königstuhl

Abstract

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Theoretical modeling of novae in outburst predicts that they should be active emitters of radiation at soft X-ray wavelengths twice during their outburst. The first time occurs very early in the outburst when only a very sensitive all sky survey will be able to detect them. This period lasts only a few hours for the very fastest novae. They again become bright in X-rays late in the outburst when the remnant object becomes very hot and is still luminous. Both simulations and observations show that novae can remain very hot for months to years. It is important to observe them at these late times because a measurement both of the flux and temperature can provide information about the mass of the white dwarf, the turn-off time scale, and the energy budget of the outburst.

Type
2. Models of Observations
Information
International Astronomical Union Colloquium , Volume 122: Physics of Classical Novae , 1990 , pp. 306 - 310
Copyright
Copyright © Springer-Verlag 1990

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