Radial accretion of H-rich material onto a He white dwarf

Details Radial accretion of H-rich material onto a He white dwarf Radial accretion of H-rich material onto a He white dwarf

Aug 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...239..988k&link_type=abstract

Astrophysical Journal, Part 1, vol. 239, Aug. 1, 1980, p. 988-998.

Computer Science

Numerical Analysis

36

Helium, Hydrogen, Novae, Stellar Envelopes, Stellar Mass Accretion, White Dwarf Stars, Abundance, Hydrodynamics, Numerical Analysis, Stellar Evolution, Stellar Models

Scientific paper

The nova outburst is modeled by spherically accreting H-rich material onto a 1 solar mass He white dwarf at a rate of 10 to the -8th solar mass/yr. The star accretes for 5848 years, when the nuclear reactions run away near the base of the accreted envelope. The nuclear-energy generation rate rises to 4.6(8) solar luminosities, and the envelope expands in response to it. However, nova-like mass ejection does not occur because the envelope is of insufficient mass, the base of the envelope is only mildly electron degenerate, and there is no enrichment of the CNO abundance. To overcome these limiting conditions, it is suggested that the H-rich material be accreted either more slowly than 10 to the -10th solar mass/yr or with angular momentum. Outbursts resulting in the former case should be similar to the nova models computed by Starrfield, Truran, and Sparks. Outbursts in the latter case should be strengthened, and novae might result because the H-rich material will be mixed into the surface layers of the white dwarf, as first suggested by Kippenhahn and Thomas (1978).

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