Steady spherical hypercritical accretion onto neutron stars

Details Steady spherical hypercritical accretion onto neutron stars Steady spherical hypercritical accretion onto neutron stars

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...376..234h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 376, July 20, 1991, p. 234-244.

Astronomy and Astrophysics

Astrophysics

57

Mass Transfer, Neutron Stars, Stellar Envelopes, Stellar Mass Accretion, Supernovae, Ionization, Mass Flow, Pair Production, Relativistic Effects, Steady State

Scientific paper

The present study of hypercritical accretion flows onto neutron stars considers steady-state, spherically symmetric flows whose accretion rate range is characterized by the carrying away of gravitational-accretion energy by neutrinos. The models used encompass pair production, radiation diffusion, and general relativistic effects. While pair pressure dominates throughout the accretion envelope when accretion rates above about 100 solar masses/yr, radiation diffusion becomes important when the accretion rate falls below about 0.001 solar masses/yr. At the lower accretion rates, free fall toward the neutron-star surface stops and an extended, quasi-static, radiation pressure-supported envelope emerges which is probably dynamically unstable.

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