Thermal stability of hydrogen-burning shells in white dwarfs

Details Thermal stability of hydrogen-burning shells in white dwarfs Thermal stability of hydrogen-burning shells in white dwarfs

Oct 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...217..171v&link_type=abstract

Astrophysical Journal, Part 1, vol. 217, Oct. 1, 1977, p. 171-174.

Astronomy and Astrophysics

Astrophysics

5

Nuclear Fusion, Stellar Envelopes, Thermal Stability, White Dwarf Stars, Hydrogen, Stellar Evolution, Stellar Luminosity, Stellar Models

Scientific paper

Models have been constructed for degenerate stars of 1 solar mass with luminosities of 0.0001 to 10,000 suns and of 0.6 solar mass with luminosities of 0.001 to 100 suns with carbon-oxygen cores and hydrogen envelopes. These stars derive all their luminosity from hydrogen shell burning near their surfaces. The thermal stability of these models is investigated, and the models are found to be stable in all cases. This stability is greatest for the models with the least luminosity.

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