A theory of hydrogen shell flashes on accreting white dwarfs. I - Their progress and the expansion of the envelope. II - The stable shell burning and the recurrence period of shell flashes

Details A theory of hydrogen shell flashes on accreting white dwarfs. I - Their progress and the expansion of the envelope. II - The stable shell burning and the recurrence period of shell flashes A theory of hydrogen shell flashes on accreting white dwarfs. I - Their progress and the expansion of the envelope. II - The stable shell burning and the recurrence period of shell flashes

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...257..752f&link_type=abstract

Astrophysical Journal, Part 1, vol. 257, June 15, 1982, p. 752-779.

Computer Science

Numerical Analysis

133

Binary Stars, Hydrogen, Nuclear Fusion, Stellar Envelopes, Stellar Mass Accretion, White Dwarf Stars, Hydrostatics, Novae, Numerical Analysis, Steady State, Stellar Evolution, Stellar Models, Stellar Structure, Thermal Stability, Thermodynamic Properties

Scientific paper

The behavior of hydrogen shell burning in the accreted envelope of white dwarfs is studied, and the progress of hydrogen shell flashes and the resultant expansion of the envelope is examined. It is shown that the most important parameter of flash strength is the proper pressure P of the burning shell, which is defined in terms of the weight of the overlying layers. It is proved that expansion is more rapid and greater for greater P and that when P is low the shell flash is weak and the envelope settles in thermal equilibrium even before it expands to solar radius. When P is high enough, a nova explosion results; the necessary envelope mass for a nova is as large as 0.00001 solar masses. The thermal properties of shell burning and recurrent properties of shell flashes are discussed in order to predict how hydrogen shell burning proceeds on an accreting white dwarf.

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