Simulation of the interaction of oppositely directed particle flows

A mathematical model of the early stage of the formation of interstellar clouds resulting from the interaction of oppositely directed cosmic particle flows and evolution of the clouds into planetary systems is proposed. An important role in the evolution is played by mechanical energy dissipation caused mainly by particle collisions. The simulation is based on the classical $n$-body problem and the Newtonian theory of instantaneous collisions of rigid bodies with a relative velocity recovery factor smaller than unity. The performed computations suggest that this model is applicable in cosmogonic theories of planetary system formation.