Treatment of realistic tidal field in Monte Carlo simulations of star
  clusters
  We present a new implementation of the Monte Carlo method to simulate the
evolution of star clusters. The major improvement with respect to the
previously developed codes is the treatment of the external tidal field taking
into account for both the loss of stars from the cluster boundary and the
disk/bulge shocks. We provide recipes to handle with eccentric orbits in
complex galactic potentials. The first calculations for stellar systems
containing 21000 and 42000 equal-mass particles show good agreement with direct
N-body simulations in terms of the evolution of both the enclosed mass and the
Lagrangian radii provided that the mass-loss rate does not exceed a critical
value.
