2005/02/04 by G. Sala, Gloria Sala, M. Hernanz +1 · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Astrophysics and Star Formation Studies #astro-ph
paper · pdf · doi:10.1051/0004-6361:20042587
5 pages, 1 figure, accepted for publication in Astronomy & Astrophysics
arxiv created 2005/02/04 · openalex publication_date 2005/08/12 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/01
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.