  We compare the results for the dynamical evolution of star clusters derived
from anisotropic gaseous models with the data from N-body simulations of
isolated and one-component systems, each having modest number of stars. The
statistical quality of N-body data was improved by averaging results from many
N-body runs, each with the same initial parameters but with different sequences
of random numbers used to initialize positions and velocities of the particles.
We study the development of anisotropy, the spatial evolution and energy
generation by three-body binaries and its N-dependence. We estimate the
following free parameters of anisotropic gaseous models: the time scale for
collisional anisotropy decay and the coefficient in the formulae for energy
generation by three-body binaries. To achieve a fair agreement between N-body
and gaseous models for the core in pre- as well as in post-collapse only the
energy generation by binaries had to be varied by N. We find that anisotropy
has considerable influence on the spatial structure of the cluster particularly
for the intermediate and outer regions.
