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 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 a considerable mass loss for clusters with Rg < S kpc: a concentration c = 1.5 cluster with Rg = 8kpc loses up to 95% of the initial mass in 15 Gyr. Only those with concentration c < 1.3 survive disk shock 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 induces, x, which may be considerably large than their initial values.