Spherically symmetric near-critical accretion onto neutron stars

Details Spherically symmetric near-critical accretion onto neutron stars Spherically symmetric near-critical accretion onto neutron stars

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...356..572m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 356, June 20, 1990, p. 572-579. Research sponsored by DOE.

Statistics

Computation

27

Computational Astrophysics, Neutron Stars, Stellar Mass Accretion, Stellar Interiors, Stellar Luminosity

Scientific paper

Numerical and approximate analytic solutions for time-independent, spherically symmetric, radiation pressure-dominated accretion flows are presented. For flows with luminosities at infinity, L-infinity, sufficiently close to the Eddington limit L-crit, the flow velocity profile is qualitatively different from the modified free-fall profile v(r) = (1 - L-infinity/L-crit)exp 1/2 (2GM/r)exp 1/2. Advective contributions to the comoving radiation flux decelerate the flow within a criical radius, and, in this settling region, the velocity of the flow decreases linearly with decreasing radius.

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