  We present the first calculations of the gravitational radiation produced by
nonaxisymmetric dynamical instability in a rapidly rotating compact star. The
star deforms into a bar shape, shedding $\sim 4\%$ of its mass and $\sim 17\%$
of its angular momentum. The gravitational radiation is calculated in the
quadrupole approximation. For a mass $M \sim 1.4$ M$_{\odot}$ and radius $R
\sim 10$ km, the gravitational waves have frequency $\sim 4$ kHz and amplitude
$h \sim 2 \times 10^{-22}$ at the distance of the Virgo Cluster. They carry off
energy $\Delta E/M \sim 0.1\%$ and radiate angular momentum $\Delta J/J \sim
0.7\%$.
