  We have carried out N-body simulations for rotating star clusters with equal
mass and compared the results with Fokker-Planck models. These two different
approaches are found to produce fairly similar results, although there are some
differences with regard to the detailed aspects. We confirmed the acceleration
of the core collapse of a cluster due to an initial non-zero angular momentum
and found a similar evolutionary trend in the central density and velocity
dispersion in both simulations. The degree of acceleration depends on the
initial angular momentum. Angular momentum is being lost from the cluster due
to the evaporation of stars with a large angular momentum on a relaxation time
scale.
