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Black hole-neutron star (BHNS) binaries are important sources ofgravitational waves for second-generation interferometers, and BHNS mergers arealso a proposed engine for short, hard gamma-ray bursts. The behavior of boththe spacetime (and thus the emitted gravitational waves) and the neutron starmatter in a BHNS merger depend strongly and nonlinearly on the black hole'sspin. While there is a significant possibility that astrophysical black holescould have spins that are nearly extremal (i.e. near the theoretical maximum),to date fully relativistic simulations of BHNS binaries have includedblack-hole spins only up to $S/M^2$=0.9, which corresponds to the black holehaving approximately half as much rotational energy as possible, given theblack hole's mass. In this paper, we present a new simulation of a BHNS binarywith a mass ratio $q=3$ and black-hole spin $S/M^2$=0.97, the highest simulatedto date. We find that the black hole's large spin leads to the most massiveaccretion disk and the largest tidal tail outflow of any fully relativisticBHNS simulations to date, even exceeding the results implied by extrapolatingresults from simulations with lower black-hole spin. The disk appears to beremarkably stable. We also find that the high black-hole spin persists untilshortly before the time of merger; afterwards, both merger and accretion spindown the black hole.

Massive disk formation in the tidal disruption of a neutron star by a nearly extremal black hole