Near-critical spherical accretion onto magnetized neutron stars - Modified magnetospheric radius

Details Near-critical spherical accretion onto magnetized neutron stars - Modified magnetospheric radius Near-critical spherical accretion onto magnetized neutron stars - Modified magnetospheric radius

Apr 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...257..807m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 257, no. 2, p. 807-810.

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Magnetic Stars, Neutron Stars, Pulsar Magnetospheres, X Ray Binaries, Computational Astrophysics, Radiation Pressure, Stellar Luminosity, Stellar Mass Accretion

Scientific paper

Theoretical considerations are presented which indicate that the magnetospheric radius, r(m), of an accreting neutron star starts expanding rather than contracting at high accretion rates, because of sufficiently strong feedback radiation pressure, due to the repulsive effect of the radiation pressure on the accretion flow around a magnetized neutron star. It is shown that, as the mass accretion rate exceeds some transition value, the magnetosphere starts expanding because of relatively stronger radiation pressure. The canonical relationship between r(m) and mass accretion rate, r(m) proportional to (mass accretion rate) exp -2/7, is modified by an introduction of a factor epsilon, which depends on the Eddington luminosity of the neutron star.

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