Issue |
A&A
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 |
Models for the soft X-ray emission of post-outburst classical novae
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 (~),
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
© ESO, 2005
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