TALK ABSTRACT:
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Evidence has been mounting for the existence of black holes with
masses from 100 to 10000 M_sun associated with stellar clusters. Such
intermediate-mass black holes (IMBHs) will encounter other black
holes in the dense cores of these clusters. The binaries produced in
these encounters will encounter other objects as well thus changing
the orbital characteristics of the binaries. These binaries and their
subsequent mergers due to gravitational radiation are important sources of
gravitational waves. We will present the results of numerical simulations
of sequences of high mass ratio three-body encounters, which will help
(1) clarify the nature of the interactions of intermediate-mass black
holes in globular clusters, (2) constrain formation models of IMBHs, and
(3) help determine what types of detectable gravitational wave signatures
are likely.