EDP Sciences
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Volume 439, Number 3, September I 2005
Page(s) 1057 - 1060
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20042587

A&A 439, 1057-1060 (2005)
DOI: 10.1051/0004-6361:20042587

Envelope models for the supersoft X-ray emission of V1974 Cyg

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 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  $M_{\odot }$ white dwarf with 50% degree of mixing between solar-like accreted material and the ONe degenerate core, or on a 1.0 $M_{\odot }$ ONe white dwarf with 25% mixing.

Key words: stars: individual: V1974 Cygni -- stars: novae, cataclysmic variables -- stars: white dwarfs -- X-rays: binaries

SIMBAD Objects

© ESO 2005

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