  We present the results of Monte Carlo simulations for the dynamical evolution
of star clusters containing two stellar populations with individual masses m1
and m2 > m1, and total masses M1 and M2 < M1. We use both King and Plummer
model initial conditions and we perform simulations for a wide range of
individual and total mass ratios, m2/m1 and M2/M1. We ignore the effects of
binaries, stellar evolution, and the galactic tidal field. The simulations use
N = 10^5 stars and follow the evolution of the clusters until core collapse. We
find that the departure from energy equipartition in the core follows
approximately the theoretical predictions of Spitzer (1969) and Lightman & Fall
(1978), and we suggest a more exact condition that is based on our results. We
find good agreement with previous results obtained by other methods regarding
several important features of the evolution, including the pre-collapse
distribution of heavier stars, the time scale on which equipartition is
approached, and the extent to which core collapse is accelerated by a small
subpopulation of heavier stars. We briefly discuss the possible implications of
our results for the dynamical evolution of primordial black holes and neutron
stars in globular clusters.
