  Compact astrophysical objects that rotate rapidly may encounter the dynamical
``bar instability.'' The bar-like deformation induced by this rotational
instability causes the object to become a potentially strong source of
gravitational radiation. We have carried out a set of long-duration simulations
of the bar instability with two Eulerian hydrodynamics codes. Our results
indicate that the remnant of this instability is a persistent bar-like
structure that emits a long-lived gravitational radiation signal.
