On the masses of the white dwarfs in cataclysmic variables

Details On the masses of the white dwarfs in cataclysmic variables On the masses of the white dwarfs in cataclysmic variables

Jun 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.208..783l&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 208, June 15, 1984, p. 783-797.

Mathematics

Probability

26

Binary Stars, Novae, Stellar Envelopes, Stellar Evolution, Stellar Mass, White Dwarf Stars, Companion Stars, Dwarf Novae, Mass To Light Ratios, Star Distribution, Stellar Mass Accretion, Stellar Structure

Scientific paper

The question of the masses of the white dwarfs in cataclysmic binaries is examined. The observational situation indicates (in spite of many uncertainties) that massive white dwarfs are more frequent in cataclysmic variable than among single white dwarfs. It is shown that selection effects can explain an overabundance of massive white dwarfs in novae but not in dwarf novae. It is proposed that the spiralling-in process in the common envelope favours the formation of more massive white dwarfs. A number of simplified spiralling-in calculations are performed which demonstrate that the probability of coalescence of the secondary with the primary core, or secondary dissipation, is higher in the case of a giant envelope than in the case of a super giant envelope. Consequently, binaries with primary core masses greater than about 0.7 solar mass (and thus massive white dwarf remnants), have a better chance of surviving common envelope evolution and are therefore better candidates for the formation of cataclysmic variables.

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