  Coalescing binary black holes experience a ``kick'' due to anisotropic
emission of gravitational waves with an amplitude as great as 200$ km/s. We
examine the orbital evolution of black holes that have been kicked from the
centers of triaxial galaxies. Time scales for orbital decay are generally
longer in triaxial galaxies than in equivalent spherical galaxies, since a
kicked black hole does not return directly through the dense center where the
dynamical friction force is highest. We evaluate this effect by constructing
self-consistent triaxial models and integrating the trajectories of massive
particles after they are ejected from the center; the dynamical friction force
is computed directly from the velocity dispersion tensor of the self-consistent
model. We find return times that are several times longer than in a spherical
galaxy with the same radial density profile, particularly in galaxy models with
dense centers, implying a substantially grea
