Chaotic loss cones and black hole fueling

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 nonaxisymmetric 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 (rhosimilar tor(-2)) nucleus scales as sigma(5) with sigma the stellar velocity dispersion, and the accumulated mass in 10(10) yr is of the correct order to reproduce the M-circle-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.