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Classical Nova Evolution: Clues from Soft X-Ray Emission

Published online by Cambridge University Press:  12 April 2016

James MacDonald
James MacDonald*
Affiliation:
University of Delaware, Department of Physics and Astronomy, Newark, DE 19716, USA

Abstract

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Multi-wavelength observations have shown that, after optical decline, the stellar remnants of classical nova outbursts evolve at constant, near-Eddington, bolometric luminosity to high effective temperature (> 2 105 K), before turning off. Here we briefly review the observations of classical novae in this phase of evolution, and discuss what the soft X-ray observations tell us about the mass of the underlying white dwarf and the rate of mass change due to stellar winds and accretion from the stellar companion.

Type
Novae & Symbiotic Stars
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 281 - 287
Copyright
Copyright © Kluwer 1996

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