The relation between orbital and spin periods in massive X-ray binaries

Details The relation between orbital and spin periods in massive X-ray binaries The relation between orbital and spin periods in massive X-ray binaries

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...223..196w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 223, no. 1-2, Oct. 1989, p. 196-206.

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Computation

83

Pulsars, Stellar Orbits, Supergiant Stars, X Ray Binaries, B Stars, Computational Astrophysics, Spin-Orbit Interactions, Stellar Luminosity, Stellar Mass, Stellar Winds

Scientific paper

The relation between the orbital period and the spin period of pulsars in massive X-ray binaries is studied. The spin periods of the neutron stars are explained in terms of the equilibrium spin period when the corotation velocity at the magnetospheric radius equals the Keplerian velocity. The theory of equilibrium spin periods is applied to the wind-fed pulsars in massive X-ray binaries. The spin periods found for systems with a classical Be star are in agreement with the equilibrium spin periods calculated for the slow equatorial wind of the Be star, using the wind structure as derived from the free-free IR excess of the stellar wind.

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