Spin-up and spin-down in intermediate polars and X-ray pulsars

Details Spin-up and spin-down in intermediate polars and X-ray pulsars Spin-up and spin-down in intermediate polars and X-ray pulsars

Feb 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990ap%26ss.164...79w&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 164, no. 1, Feb. 1990, p. 79-85.

Statistics

Computation

8

Cataclysmic Variables, Computational Astrophysics, Pulsars, X Ray Binaries, Pulsar Magnetospheres, Stellar Magnetic Fields, Stellar Rotation, White Dwarf Stars

Scientific paper

The accretion torque theory of Wang (1987) is applied to the spin periods of intermediate polars and X-ray pulsars. It is shown that, if the primaries are spinning near their equilibrium values, the range of positive and negative values of P/P observed in intermediate polars is readily understood in terms of relatively small variations of mass transfer rate M of the kind generated either by long term (about 1000-yr) cycling of M suggested by the nova hibernation model, or by the short term (about 10-yr) variations caused by magnetic cycling in the secondary stars. The variations in spin rates of the disk-fed X-ray pulsars Her X-1 and Cen X-3 can also be accounted for by the latter process.

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