Non-axisymmetric Instabilities in Thick Self-Gravitating Tori Around Black Holes in Dynamical General Relativistic Framework

Details Non-axisymmetric Instabilities in Thick Self-Gravitating Tori Around Black Holes in Dynamical General Relativistic Framework Non-axisymmetric Instabilities in Thick Self-Gravitating Tori Around Black Holes in Dynamical General Relativistic Framework

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aps..ses.hc008k&link_type=abstract

American Physical Society, 77th Annual Meeting of the Southeastern Section of the APS, October 20-23, 2010, abstract #HC.008

Astronomy and Astrophysics

Astrophysics

Scientific paper

Thick self-gravitating accretion disks around black holes play a major role in several astrophysical scenarios of gamma-ray bursts. These objects can form as a result of massive star core collapse, merger of two neutron stars or a neutron star and a black hole, they have very high densities and relativistic rotation speeds. In this study, we address stability of thick constant angular momentum accretion tori using a fully dynamical general relativistic framework. We have performed evolutions of several accretion tori models and identified two distinct types of non-axisymmetric instabilities. The first type corresponds to the Papaloizou-Pringle instability, enhanced by a motion of the central black hole. The second type corresponds to the I-mode, previously found in Newtonian studies. We discuss the types, growth rates and pattern speeds of the unstable modes, as well as the detectability of the gravitational waves from such objects.

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