Diffusion and mixing in classical nova precursors

Details Diffusion and mixing in classical nova precursors Diffusion and mixing in classical nova precursors

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...375l..27i&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 375, July 1, 1991, p. L27-L29.

Astronomy and Astrophysics

Astrophysics

18

Novae, Stellar Composition, Stellar Mass Accretion, White Dwarf Stars, Carbon, Diffusion, Nitrogen, Oxygen

Scientific paper

Numerical experiments have been conducted to determine the degree of enhancement of CNO elements in the envelope of an initially cold 1-solar-mass carbon-oxygen white dwarf accreting hydrogen-rich material at rates expected in cataclysmic variables. Only ordinary particle diffusion and convective mixing have been considered, and the enhancements found are a consequence of the diffusive intermixing of hydrogen with carbon and oxygen; this mixing causes a hydrogen-burning thermonuclear runaway to begin below the surface of the original white dwarf.

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