Volume 439, Number 3, September I 2005
|Page(s)||1057 - 1060|
|Section||Stellar structure and evolution|
|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
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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