A model for dwarf novae as progenitors of Type I supernovae

Details A model for dwarf novae as progenitors of Type I supernovae A model for dwarf novae as progenitors of Type I supernovae

Jan 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...243l..27s&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 243, Jan. 1, 1981, p. L27-L31.

Astronomy and Astrophysics

Astrophysics

16

Dwarf Novae, Stellar Evolution, Stellar Mass Accretion, Stellar Models, Supernovae, White Dwarf Stars, Abundance, Binary Stars, Carbon, Helium, Nitrogen, Oxygen, Stellar Envelopes, Thermonuclear Reactions

Scientific paper

It is suggested that a Type I supernova event can be produced as a result of accretion at low rates (less than 10 to the -10th solar mass/year) onto the white dwarf component of a dwarf-nova close binary. At these low rates, diffusion of the CNO nuclei out of the accreted hydrogen envelope can occur on the accretion time scale, and nuclear burning will occur mainly by the proton-proton chain. Studies of this process show that, when the CNO abundance in the envelope is less than 0.0025 of solar, no thermonuclear flash occurs and no mass is lost. The result of the evolution is a gradually increasing layer of helium beneath the hydrogen-burning shell.

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