  It has recently been shown that the rate of angular momentum relaxation in
nearly-Keplerian star clusters is greatly increased by a process termed
resonant relaxation (Rauch & Tremaine 1996), who also argued that tidal
disruption of stars in galactic nuclei containing massive black holes could be
noticeably enhanced by this process. We describe here the results of numerical
simulations of resonant tidal disruption which quantitatively test the
predictions made by Rauch & Tremaine. The simulation method is based on an
N-body routine incorporating cloning of stars near the loss cone and a
semi-relativistic symplectic integration scheme. We also briefly describe the
discovery of chaos in the Wisdom-Holman symplectic integrator applied to highly
eccentric orbits and propose a modified integration scheme that remains robust
under these conditions.
  We find that resonant disruption rates exceed their non-resonant counterparts
by an amount consistent with the predictions; in particular, we estimate the
net tidal disruption rate for a fully resonant cluster to be about twice that
of its non-resonant counterpart. No significant enhancement in rates is
observed outside the critical radius. Relativistic quenching of the effect is
found to occur for hole masses M>8*10^7 solar masses. The numerical results
combined with the observed properties of galactic nuclei indicate that for most
galaxies the resonant enhancement to tidal disruption rates will be very small.
