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

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

2005-02-04

arxiv.org/abs/astro-ph/0502092v1

Astronomy and Astrophysics

Astrophysics

5 pages, 1 figure, accepted for publication in Astronomy & Astrophysics

Scientific paper

10.1051/0004-6361:20042587

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 Msun white dwarf with 50% degree of mixing between solar-like accreted material and the ONe degenerate core, or on a 1.0 Msun ONe white dwarf with 25% mixing.

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