Hydrogen shell flashes in massive accreting white dwarfs

Details Hydrogen shell flashes in massive accreting white dwarfs Hydrogen shell flashes in massive accreting white dwarfs

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...230..832s&link_type=abstract

Astrophysical Journal, Part 1, vol. 230, June 15, 1979, p. 832-838.

Astronomy and Astrophysics

Astrophysics

51

Binary Stars, Hydrogen, Stellar Evolution, Stellar Mass Accretion, White Dwarf Stars, Long Term Effects, Stellar Envelopes, Stellar Luminosity, Stellar Models, Stellar Structure, Thermonuclear Reactions, Variability

Scientific paper

In the present paper, the long-term evolution of massive accreting white dwarfs in close binary systems is discussed in context of several astrophysical problems. It is shown that high surface luminosity models with spherically symmetric accretion (rather than disk accretion) yield very short interflash periods for massive white dwarfs accreting at high rates. The shell flashes exhibited by the models are not strong enough to eject mass, as in classical novae. However, the repetitive hydrogen shell flashes with an interflash period of 17 years may be relevant to understanding the underlying variability of the blue component of symbiotic variables if the blue component is a white dwarf.

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