  Angular momentum loss via the emission of gravitational waves must eventually
drive compact binaries containing black holes and/or neutron stars to coalesce.
The resulting events are primary candidate sources for detectors such as VIRGO
and LIGO. We present calculations of gravitational radiation waveforms and
luminosities for the coalescence of a black hole-neutron star binary, performed
in the quadrupole approximation using a Newtonian smooth particle hydrodynamics
code. We discuss the dependence of the waveforms and the total emitted
luminosity as well as the final configuration of the system on the initial mass
ratio and the degree of tidal locking.
