EDP Sciences
Free Access
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

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

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.