Abstract
Abstract Dynamical evolution of globular clusters is strongly influenced and often driven by tidal interactions with the Galaxy. Passing through the Galactic disk or near the bulge, globular clusters experience fast gravitational perturbations, the compressive tidal shocks. A succession of tidal shocks leads to kinematic heating of the clusters and their ultimate destruction. I present the latest Fokker-Planck models including the first and second order tidal diffusion coefficients. In the limit of strong shocks, the typical value of the core collapse time t cc decreases from 10 to 3 half-mass relaxation times, while the destruction time is just 2, t cc. 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.
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