Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...283..241m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 283, Aug. 1, 1984, p. 241-248.
Astronomy and Astrophysics
Astrophysics
32
Cataclysmic Variables, Dwarf Novae, Stellar Evolution, Supernovae, White Dwarf Stars, Carbon Stars, Magnetohydrodynamic Turbulence, Stellar Composition, Stellar Cores, Stellar Envelopes, Stellar Mass Accretion, Thermonuclear Reactions
Scientific paper
The long term evolution of carbon-oxygen white dwarfs accreting solar composition material at fixed rate is investigated in order to determine whether short-period cataclysmic binary systems are likely to be Type I supernova progenitors. In addition to mass loss from the white dwarf in response to hydrogen shell flashes in the accreted material, a number of previously neglected physical processes are considered, including mass loss due to helium flashes, dredge-up of core material by turbulence induced by shears due to accretion of angular momentum, and mass loss by stellar winds during the hot remnant phase. The most important of these processes is shear-induced turbulence which leads to severe constraints on the range of system parameters for which supernovae can occur. It is found that the white dwarf can explode as a Type I supernova only if it is initially massive (more than about 0.9 solar mass) and the accretion rate is high (more than about 3 x 10 to the -8th solar mass per year). The secondary (donor) star also has to be sufficiently massive to fuel the evolution to supernova including mass loss from the system during the course of the evolution. No systems are known which satisfy all these constraints. For the Galaxy, the frequency of supernovae from cataclysmic variables is estimated to be much less than 3 x 10 to the -3rd per year, at least an order of magnitude less than observed.
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