Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...242..749t&link_type=abstract
Astrophysical Journal, Part 1, vol. 242, Dec. 1, 1980, p. 749-755.
Astronomy and Astrophysics
Astrophysics
55
Carbon Stars, Helium, Nuclear Fusion, Stellar Evolution, Stellar Mass Accretion, White Dwarf Stars, Binary Stars, Hydrogen, Novae, Supernovae, Thermonuclear Explosions
Scientific paper
The long-term evolution of an accreting carbon white dwarf of 1.2 solar masses is investigated. It is found that for a mass accretion rate of 10 to the -9th solar masses/yr a degenerate-helium-shell flash develops, whereas for an accretion rate of 5 x 10 to the -10th solar masses/yr a central carbon flash develops. An upper bound to the mass accretion rate for which a strong helium-shell flash occurs is estimated to be 3 x 10 to the -8th solar masses/yr, a value which is nearly independent of the initial mass of the carbon white dwarf. A weak helium-shell flash is indicated for mass accretion rates in excess of about 3 x 10 to the -8th solar masses/yr, while carbon ignition at high density (approximately 10 to the 10th g/cu cm), perhaps, leading to a strong helium-shell flash is indicated for high-mass white dwarfs accreting at rates below about 5 x 10 to the -10th solar masses/yr. The results are discussed in the context of the nova and Type I supernova phenomena.
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