  The previous two companion papers demonstrate that slowly varying
perturbations do not result in adiabatic cutoffs and provide a formalism for
computing the long-term effects of time-dependent perturbations on stellar
systems. Here, the theory is implemented in a Fokker-Planck code and a suite of
runs illustrating the effects of shock heating on globular cluster evolution
are described. Shock heating alone results in considerable mass loss for
clusters with $R_g\lta8\kpc$: a concentration $c=1.5$ cluster with $R_g=8\kpc$
loses up to $95\%$ of its initial mass in $15\Gyr$. Only those with
concentration $c\lta1.3$ survive disk shocks inside of this radius. Other
effects, such as mass loss by stellar evolution, will increase this survival
bound. Loss of the initial halo together with mass segregation leads to mass
spectral indices, $x$, which may be considerably larger than their initial
values.
