Bimodal accretion in a GX5-1 and a possible constraint on its rotation period

Details Bimodal accretion in a GX5-1 and a possible constraint on its rotation period Bimodal accretion in a GX5-1 and a possible constraint on its rotation period

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.232..487b&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 232, June 1, 1988, p. 487-495.

Statistics

Computation

2

Accretion Disks, Neutron Stars, Polar Caps, Stellar Magnetic Fields, Stellar Rotation, X Ray Binaries, Computational Astrophysics, Mass Transfer, Power Spectra, Stellar Oscillations

Scientific paper

In this paper it is argued that the low-mass X-ray binary GX5-1 exhibits two modes of accretion, which account for the two separate branches seen in an intensity versus hardness ratio diagram of the emission from the source. In one mode, accretion at high rates occurs more or less uniformly over the stellar surface, and this corresponds to the normal branch in the intensity versus hardness ratio diagram. In the other mode, at a somewhat lower accretion rate, the magnetic field of the star prevents the disk from reaching the star, and the field channels the accretion flow from some magnetospheric radius, which depends upon the accretion rate, on to small polar caps; this is identified with the QPO branch in the intensity versus hardness ratio diagram. If the quasi-periodic oscillations are due to the interaction of the disk with the magnetic field, as in the beat-frequency model, then the rotation period of the neutron star is shown to be, under certain assumptions regarding the spectrum, longer than 0.1 s.

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