Runaway Instability of Black Hole--Neutron Torus Systems

Details Runaway Instability of Black Hole--Neutron Torus Systems Runaway Instability of Black Hole--Neutron Torus Systems

Apr 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...461..320n&link_type=abstract

Astrophysical Journal v.461, p.320

Physics

17

Accretion, Accretion Disks, Stars: Binaries: Close, Black Hole Physics, Gamma Rays: Bursts, Methods: Numerical, Stars: Neutron

Scientific paper

We have obtained fully general relativistic equilibrium configurations of black hole-neutron torus systems and have analyzed their stability. Although several authors have discussed whether such systems can be sources of gamma-ray bursts, their arguments have been based on the qualitative nature of black hole-neutron torus systems because such configurations have not yet been solved. Moreover, since black hole-neutron torus systems are supposed to form after coalescence of binary neutron stars or after collapse of a massive star, a newly formed torus may be in a rather hot state. Therefore we have developed a numerical code that can handle configurations of cold and hot (0.1, 1, and 10 MeV) neutron tori.
Recently, polytropic tori around black holes have been shown to suffer a global runaway instability. As for neutron tori, the self-gravitating tori closely orbiting around the black holes with the mass range of 1-3 Msun are destroyed in a timescale ΔtTτ ≪ 1 s as a result of this instability. This is a much shorter timescale than the evolutionary timescale that is relevant for the current model of gamma-ray bursts based on the merger of binary neutron stars. This result probably excludes the possibility of neutron tori models for gamma-ray bursts as sources at cosmological distances.

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