Evolution of the white dwarf mass and spin in cataclysmic variables

Details Evolution of the white dwarf mass and spin in cataclysmic variables Evolution of the white dwarf mass and spin in cataclysmic variables

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.251p..30k&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 251, July 1, 1991, p. 30P-32P. SERC-supported research.

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Cataclysmic Variables, Spin Dynamics, Stellar Evolution, Stellar Mass Accretion, White Dwarf Stars, Computational Astrophysics, Novae, Secular Variations, X Ray Sources

Scientific paper

The spin-up of the white dwarf in nonmagnetic CVs during secular evolution is considered. If this is unresisted, CVs are quenched as boundary-layer emitters once the binary period has decreased by about 1 hr. Angular momentum loss in nova explosions may, however, prevent the star reaching breakup. If the explosions remove (1 + epsilon) x the mass accreted between outbursts, values in the range between 0.5 and 1 allow CVs to be modest boundary-layer emitters for most of their lifetimes. Spectral effects will limit their detection as soft X-ray sources.

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