Abstract
Multiwavelength 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 show that, in principle, EUV and soft X-ray observations can be used to determine the mass of the underlying white dwarf and place limits on the rate of mass loss by stellar winds and the rate of mass gain due to accretion from the stellar companion. We also describe our model atmosphere calculations of EUV/Soft X-ray emission from hot, high gravity stars and their application to the EUVE all-sky survey detection of Nova Cygni 1992 (V1974 Cyg).
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