An improved method for constructing models of self-gravitating tori around black holes

Abstract

General-relativistic models of self-gravitating tori around black holes are constructed with a self-consistent-field method in compactified coordinates. The numerical code is highly accurate and robust, allowing for the construction of models that exactly fill their Roche lobe, when a cusp exists. As a first application, we focus on self-consistent models with cusp, having different values of constant specific angular momentum. Scaling all results with the mass of the black hole, we find evidence that models with constant specific angular momentum that can fill their Roche lobe are still limited by $l<4M_{\mathrm{BH}}$ (as is the case for models constructed in a fixed background metric) even for heavy tori.

13 pages, 6 figures, accepted for publication in Int. J. Mod. Phys. D

References in corpus (6)

• The Supernova -- Gamma-Ray Burst Connection
• Merger of binary neutron stars to a black hole: Disk mass, short gamma-ray bursts, and quasinormal mode ringing
• Accurate evolutions of unequal-mass neutron-star binaries: properties of the torus and short GRB engines
• Numerical relativity confronts compact neutron star binaries: a review and status report
• Stability of general-relativistic accretion disks
• Influence of self-gravity on the runaway instability of black hole-torus systems

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