Chaotic Loss Cones, Black Hole Fueling and the M-Sigma Relation

Details Chaotic Loss Cones, Black Hole Fueling and the M-Sigma Relation Chaotic Loss Cones, Black Hole Fueling and the M-Sigma Relation

2003-02-14

arxiv.org/abs/astro-ph/0302296v2

Astrophys.J. 606 (2004) 788-798

Astronomy and Astrophysics

Astrophysics

29 pages, 6 figures

Scientific paper

10.1086/382497

In classical loss cone theory, stars are supplied to a central black hole via gravitational scattering onto low angular momentum orbits. Higher feeding rates are possible if the gravitational potential near the black hole is non-axisymmetric and the orbits are chaotic. Motivated by recently published, self-consistent models, we evaluate rates of stellar capture and disruption in triaxial nuclei. Rates are found to substantially exceed those in collisionally-resupplied loss cones, as long as an appreciable fraction of the orbits are centrophilic. The mass captured by a black hole after a given time in a steep nucleus scales as the fifth power of the velocity dispersion, and the accumulated mass in 10^10 yr is of the correct order to reproduce the M-sigma relation. Triaxiality can solve the "final parsec problem" of decaying black hole binaries by increasing the flux of stars into the binary's loss cone.

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