On the secular evolution of accreting white dwarfs and Type I supernovae

Details On the secular evolution of accreting white dwarfs and Type I supernovae On the secular evolution of accreting white dwarfs and Type I supernovae

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...260..249f&link_type=abstract

Astrophysical Journal, Part 1, vol. 260, Sept. 1, 1982, p. 249-253.

Astronomy and Astrophysics

Astrophysics

32

Carbon Stars, Stellar Evolution, Stellar Mass Accretion, Supernovae, White Dwarf Stars, Helium, Hydrogen, Mass Transfer, Oxygen, Secular Variations, Stellar Envelopes, Stellar Models

Scientific paper

The growth of a carbon-oxygen white dwarf is investigated within the framework of the general shell-flash theory of accreting white dwarfs. Account is taken of the envelope restructuring in response to the shell flash and to possible mass loss from the white dwarf. Estimates are given for the amount of helium accumulated between successive hydrogen shell flashes. Significant helium accumulation is possible for mass-accretion rates greater than 10 to the -9 solar masses per year. The results are discussed in the context of exploding white-dwarf models of Type I supernovae.

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