| Issue |
A&A
Volume 439, Number 3, September I 2005
|
|
|---|---|---|
| Page(s) | 1057 - 1060 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361:20042587 | |
| Published online | 12 August 2005 | |
Envelope models for the supersoft X-ray emission of V1974 Cyg
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:
7
February
2005
The evolution of the soft X-ray emission of V1974 Cyg
has been simulated by a white dwarf envelope model with steady hydrogen
burning. The comparison of the results obtained from ROSAT observations with
the results of our envelope models indicates that the post-outburst
evolution of the nova can be explained by steady H-burning
on either a 0.9 
white dwarf with 50% degree
of mixing between solar-like accreted material and the
ONe degenerate core, or on a 1.0 
ONe white dwarf with 25% mixing.
Key words: stars: individual: V1974 Cygni / stars: novae, cataclysmic variables / stars: white dwarfs / X-rays: binaries
© ESO, 2005
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