Dynamical evolution of globular clusters after core collapse.

This review describes work on the evolution of a stellar system during the phase which starts at the end of core collapse. It begins with an account of the model of Henon, Goodman (1984), and Inagaki and Lynden-Bell (1983), as well as evaporative models, and modifications to these models which are needed in the core. Next, these models are related to more detailed numerical calculations of gaseous models, Fokker-Planck models, N-body calculations, etc., and some problems for further work in these directions are outlined. The review concludes with a discussion of the relation between theoretical models and observations of the surface density profiles and statistics of actual globular clusters.