Classical nova models with accretion heating at accretion rates of 10-9 and 10-10 M per year

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Abstract

Two evolutionary sequences of accretion onto a 1.25 M C-O white dwarf are computed for Ṁ = 10-10 M yr-1 and Ṁ = 10-9 M yr-1 and are carried through the thermonuclear runaway and the dynamical phases of mass loss, followed by contraction of the remnant and decline. Improved algorithms are used for diffusion during the accretion phase and for the computation of mass loss. Accretional heating is taken into account. We conclude that outbursts typical of classical novae may be achieved for the adopted rather high accretion rates that are compatible with observations. The heavy element mass fractions in the ejecta are found to be 0.31 and 0.19, the maximal velocities reached are 2300 and 1600 km s-1, and mass loss lasts for ∼12 and ∼25 days, respectively, for the two models. The effect of diffusion and its dependence on the accretion rate are discussed.

Original languageEnglish
Pages (from-to)665-669
Number of pages5
JournalAstrophysical Journal
Volume385
Issue number2
DOIs
StatePublished - 1 Feb 1992

Keywords

  • Accretion, accretion disks
  • Novae, cataclysmic variables
  • Stars: abundances
  • Stars: evolution
  • Stars: mass loss

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