  We present new Fokker-Planck models of the evolution of globular clusters,
including gravitational tidal shocks. We extend our calculations beyond the
core collapse by adopting three-body binary heating. Effects of the shocks are
included by adding the tidal shock diffusion coefficients to the ordinary
Fokker-Planck equation: the first order heating term, <dE>, and the second
order energy dispersion term, <dE^2>. As an example, we investigate the
evolution of models for the globular cluster NGC 6254. Using the Hipparcos
proper motions, we are now able to construct orbits of this cluster in the
Galaxy. Tidal shocks accelerate significantly both core collapse and the
evaporation of the cluster and shorten the destruction time from 24 Gyr to 18
Gyr. We examine various types of adiabatic corrections and find that they are
critical for accurate calculation of the evolution. Without adiabatic
corrections, the destruction time of the cluster is twice as short.
  We examine cluster evolution for a wide range of the concentration and tidal
shock parameters, and determine the region of the parameter space where tidal
shocks dominate the evolution. We present fitting formulae for the core
collapse time and the destruction time, covering all reasonable initial
conditions. In the limit of strong shocks, the typical value of the core
collapse time decreases from 10 t_{rh} to 3 t_{rh} or less, while the
destruction time is just twice that number. The effects of tidal shocks are
rapidly self-limiting: as clusters lose mass and become more compact, the
importance of the shocks diminishes. This implies that tidal shocks were more
important in the past.
