Hydrogen and helium burning in the degenerate envelope of a carbon-oxygen dwarf

Details Hydrogen and helium burning in the degenerate envelope of a carbon-oxygen dwarf Hydrogen and helium burning in the degenerate envelope of a carbon-oxygen dwarf

Oct 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979pazh....5..531t&link_type=abstract

(Pis'ma v Astronomicheskii Zhurnal, vol. 5, Oct. 1979, p. 531-536.) Soviet Astronomy Letters, vol. 5, Sept.-Oct. 1979, p. 284-28

Astronomy and Astrophysics

Astronomy

Carbon Stars, Dwarf Stars, Novae, Stellar Envelopes, Thermonuclear Reactions, Helium, Hydrogen, Stellar Evolution, Stellar Mass Accretion

Scientific paper

A simple analytic method assuming a thermal steady state is used to analyze the thermal evolution of thin degenerate envelopes. Certain thermonuclear-flash parameters are estimated as a function of the accretion rate, including the interflash period, the mass of the accumulated shell, the energy of the flash, the total number of outbursts, and the overall duration of the nova phase. The shortest interflash period admitted by this model is about 10 yr, in agreement with the interflare periods observed in recurrent novae.

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