Neutron tori around Kerr black holes

Details Neutron tori around Kerr black holes Neutron tori around Kerr black holes

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...422..219w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 422, no. 1, p. 219-226

Computer Science

Numerical Analysis

16

Astronomical Models, Black Holes (Astronomy), Computerized Simulation, Merging Routines, Neutron Stars, Stellar Mass, Stellar Structure, Toroids, Angular Momentum, Equations Of State, Gamma Ray Bursts, Numerical Analysis, Supernovae

Scientific paper

Models of stationary, axisymmetric, non-self-gravitating tori around stellar mass Kerr black holes are calculated. Such objects may form as a result of a merger between two neutron stars, a neutron star and a stellar mass black hole, or a 'failed supernova' collapse of a single rapidly rotating star. We explore a large range of parameters: the black hole mass and angular momentum, the torus mass, angular momentum and entropy. Physical conditions within the tori are similar to those in young and hot neutron stars, but their topology is different, and the range of masses and energies is much larger.

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