Envelope models for the supersoft X-ray emission of V1974 Cyg
arXiv:astro-ph/0502092 · doi:10.1051/0004-6361:20042587
Abstract
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.
5 pages, 1 figure, accepted for publication in Astronomy & Astrophysics