  Gravitational radiation from a binary neutron star or black hole system leads
to orbital decay and the eventual coalescence of the binary's components.
During the last several minutes before the binary components coalesce, the
radiation will enter the bandwidth of the United States Laser Inteferometer
Gravitational-wave Observatory (LIGO) and the French/Italian VIRGO
gravitational radiation detector. The combination of detector sensitivity,
signal strength, and source density and distribution all point to binary
inspiral as the most likely candidate for observation among all the anticipated
sources of gravitational radiation for LIGO/VIRGO. Here I review briefly some
of the questions that are posed to theorists by the impending observation of
binary inspiral.
