  We review recent progress in computational methods for studying the dynamical
evolution of large star clusters. After describing some highlights of a new
comparison of different models, including N-body models, we mention in detail
recent developments in three codes which allow models with anisotropic
distributions of velocity to be studied: (i) a Fokker-Planck code using finite
differences, (ii) a Monte Carlo code and (iii) a gaseous model code.
