Some properties of white-dwarf collapse in low-mass binaries

Details Some properties of white-dwarf collapse in low-mass binaries Some properties of white-dwarf collapse in low-mass binaries

Nov 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..97..121l&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 97, no. 1, Nov. 1983, p. 121-126.

Astronomy and Astrophysics

Astrophysics

13

Binary Stars, Gravitational Collapse, Stellar Rotation, White Dwarf Stars, Angular Momentum, Pulsars, Stellar Magnetic Fields, Stellar Mass Accretion, Tides

Scientific paper

Conditions for collapse of an accreting white dwarf in a low-mass close binary are analysed. It is shown that if the magnetic strength on the surface of a white dwarf is less than 105 - 106 G, a rotation barrier appears which prevents the direct formation of a neutron star. As a result, a time-scale for the collapse is defined by a specific time of momentum dissipation rather than by free-fall time-scale. It is noted that a tidal deformation of a white dwarf, intensified in a process of collapse, renders collapse in a low-mass close binary sharply anisotropic. Consequently fast moving radiopulsars can arise with velocities of some thousands km s-1.

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