  We present the first post core collapse models of initially rotating star
clusters, using the numerical solution of an orbit-averaged 2D Fokker-Planck
equation. Based on the code developed by Einsel & Spurzem (1999), we have
improved the speed and the stability and included the steady three-body binary
heating source. We have confirmed that rotating clusters, whether they are in a
tidal field or not, evolve significantly faster than non-rotating ones.
Consequences for observed shapes, density distribution, and kinematic
properties of young and old star clusters are discussed. The results are
compared with gaseous and 1D Fokker-Planck models in the non-rotating case.
