  We model the formation of black hole-neutron star (BH-NS) binaries via
dynamical interactions in globular clusters. We find that in dense, massive
clusters, 16-61% of the BH-NS binaries formed by interactions with existing BH
binaries will undergo mergers driven by the emission of gravitational
radiation. If the BHs are retained by the cluster after merging with a NS, the
BHs acquire subsequent NS companions and undergo several mergers. Thus, the
merger rate depends critically upon whether or not the BH is retained by the
cluster after the merger. Results from numerical relativity suggest that kick
imparted to a ~7 M_sun BH after it merges with a NS will greatly exceed the
cluster's escape velocity. In this case, the models suggest that the majority
of BH-NS mergers in globular clusters occur within 4 Gyrs of the cluster's
formation and would be unobservable by Advanced LIGO. For more massive BHs, on
the other hand, the post merger kick is suppressed and the BH is retained.
Models with 35 M_sun BHs predict Advanced LIGO detection rates in the range
0.04 - 0.7 per year. On the pessimistic end of this range, BH-NS mergers
resulting from binary-single star interactions in globular clusters could
account for an interesting fraction of all BH-NS mergers. On the optimistic
end, this channel may dominate the rate of detectable BH-NS mergers.
