Helium shell bursts of accreting carbon-oxygen dwarfs

Details Helium shell bursts of accreting carbon-oxygen dwarfs Helium shell bursts of accreting carbon-oxygen dwarfs

Aug 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992azh....69..784t&link_type=abstract

Astronomicheskij Zhurnal (ISSN 0004-6299), vol. 69, no. 4, p. 784-792.

Astronomy and Astrophysics

Astronomy

4

Accretion Disks, B Stars, Carbon Stars, Stellar Envelopes, Thermal Instability, White Dwarf Stars, Critical Mass, Helium, Oxygen

Scientific paper

The accretion of helium by a degenerate carbon-oxygen (oxygen-neon) dwarf results in recurrent shell explosions in its envelope. This numerical study of the thermal explosion within the framework of 1D hydrodynamics shows that for a complete loss of the accumulated envelope, its mass must exceed a limit that depends on dwarf mass that is greater than about 1.8 x 10 exp -1.75 M(CO)/solar mass. The thermal instability of helium burning in these envelopes results, for M(CO) greater than 0.6 solar mass, in an explosion of supernova scale and in the expulsion of envelope matter with a velocity of about 10 exp 9 cm/s. The partial helium burning during a thermal shell explosion can account for the enhanced carbon abundance in envelopes of R CrB stars.

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