Numerical simulation of compression of rotating clouds

The problem of numerical simulation of star production processes is discussed. The problem is considered in the general form in two aspects: star evolution and formation of near the star disk and evolution of protostar shell. The difference in the behaviour of shells of massive and small-mass protostars is determined by the difference in dynamic factors affecting them. In massive protostar H2 compact region is the main factor, in small-mass one - stellar wind