  Numerical simulation of evolution of a cluster of a finite number of
gravitating bodies interacting only by their intrinsic gravity has been carried
out. The goal of the study was to reveal the main characteristic phases of the
spatial distribution of material bodies constituting the cluster. In solving
the problem, the possibility of interbody collisions was taken into account,
the collisions being assumed to be absolutely inelastic. Forces external to the
body cluster under consideration were ignored. Among all the internal force
factors acting within the cluster, only the gravitational interaction was taken
into account. The total mass of all the gravitating bodies of the cluster was
assumed to remain constant during the entire evolution. The Cauchy problem with
natural initial conditions was considered. To check the process of solution,
the so-called rotation curve was used which represents the current radial
distribution of orbital velocities of the cluster bodies. The numerical
analysis showed time variations of the model cluster rotation curve and,
particularly, the fact that the rotation curve horizontal section is only a
short moment in evolution of the gravitating bodies cluster. The results
obtained within the scope of classical mechanics show that it is possible to
represent all the rotation curve variations for the observed galaxies without
appealing to the hypothesis of non-observable gravitating "dark matter".
