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

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.

arXiv comment5 pages, 1 figure, accepted for publication in Astronomy & Astrophysics

References in corpus (6)

• Nucleosynthesis in Classical Novae: ONe vs. CO White Dwarfs
• X-ray emission from classical and recurrent-novae observed with ROSAT
• The frequency of occurrence of novae hosting an ONe white dwarf
• The Optical Spectroscopic Evolution of V1974 Cygni (Nova Cygni 1992)
• A study of the expanding envelope of Nova V1974 Cyg 1992 based on IUE high resolution spectroscopy
• A XMM-Newton observation of Nova LMC 1995, a bright supersoft X-ray source

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• Toward a unified light curve model for multi-wavelength observations of V1974 Cygni (Nova Cygni 1992)
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• V5116 Sgr, an Eclipsing Supersoft Post-Outburst Nova?
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• Nova M31N 2007-12b: Supersoft X-rays reveal an intermediate polar?
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• X-ray observations of classical novae. Theoretical implications
• Astrophysical Fluids of Novae: High Resolution Pre-decay X-ray spectrum of V4743 Sagittarii