The mass spectrum of the white dwarfs in cataclysmic binaries

Details The mass spectrum of the white dwarfs in cataclysmic binaries The mass spectrum of the white dwarfs in cataclysmic binaries

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...158..161r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 158, no. 1-2, April 1986, p. 161-173.

Astronomy and Astrophysics

Astrophysics

61

Binary Stars, Cataclysmic Variables, Mass Spectra, Stellar Evolution, Stellar Mass Accretion, White Dwarf Stars, Angular Momentum, Bolometers, Dwarf Novae, Mass Transfer, Space Density

Scientific paper

Using a simple model for the secular evolution of cataclysmic binaries the authors investigate observational selection in favour of massive white dwarfs. For this they consider a V-magnitude-limited sample of cataclysmic binaries with bright accretion disks, i.e. nova-like systems and dwarf novae in outburst. They find that the selection effect is strong enough to account fully for the high mean white dwarf mass observed and that therefore the intrinsic mass spectrum of the white dwarfs in cataclysmic binaries need not be significantly different from that of single white dwarfs. Furthermore they find the following trends: the selection in favour of massive white dwarfs becomes stronger with increasing orbital period. The main reason for the strong selection is found to be the steep increase of the white dwarfs' gravitational potential with mass. In addition, the authors find that only a small fraction of cataclysmic binaries is actually observed. If the mass spectrum of the white dwarfs is not too different from that of single white dwarfs, the intrinsic space density must be of order 1 - 2×10-4pc-3.

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