EDP Sciences
Free Access
Volume 439, Number 3, September I 2005
Page(s) 1061 - 1073
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361:20042622
Published online 12 August 2005

A&A 439, 1061-1073 (2005)
DOI: 10.1051/0004-6361:20042622

Models for the soft X-ray emission of post-outburst classical novae

G. Sala and M. Hernanz

Institut d'Estudis Espacials de Catalunya and Institut de Ciències de l'Espai (CSIC), Campus UAB, Facultat de Ciències, Torre C5-parell, 2a planta, 08193 Bellaterra (Barcelona), Spain
    e-mail: [sala;hernanz]@ieec.uab.es

(Received 29 December 2004 / Accepted 12 April 2005 )

We developed a hydrostatic and stationary white dwarf envelope model for the study of the post-outburst phases of classical novae and their soft X-ray emission. We considered several white dwarf masses and chemical compositions typical of classical novae. Our results show that the luminosity, maximum effective temperature, and envelope masses depend on the white dwarf mass and on the chemical composition. Envelope masses for which equilibrium solutions exist are pretty small (~ $ 10^{-7}{-}10^{-6}~ M_{\odot}$), thus leading to a short duration of the soft X-ray emitting phase of classical novae, in agreement with most observations. The models we present provide a useful tool for the determination of the white dwarf properties from observable parameters in the X-ray range.

Key words: stars: novae, cataclysmic variables -- stars: white dwarfs -- X-rays: binaries

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© ESO 2005

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