ИСТИНА

It is known that the nucleation of stars in the universe occurs, as a rule, in areas of the interstellar medium, where nebulae - gas and dust clouds consisting of molecular hydrogen, can collide with each other, changing their state during dynamic interaction with gravitational and magnetic fields. The gravitational-turbulent description of these processes is quite common in explaining the reasons for the creation of pre-stellar regions as a consequence of the collision of molecular clouds. We adhere to this approach with some simplification, assuming that the main factor in the dynamic transformations of gas formations is the influence on the collision process of mainly the kinetic energy of the clouds, separating these effects from the effects of gravitational collapse and from the influence of magnetic fields. To simulate gas-dynamic processes of different scales, a parallel numerical code was developed using grids with improved resolution, which was used in a numerical experiment on highperformance computers. The simulation showed that sharp changes in the distribution of matter in the shock core of new formations can be triggered by the Kelvin-Helmholtz instability and nonlinear thin-shell instability, which lead to sharp perturbations of the gas density in the resulting clumps, outer shells and gas filaments, with density fluctuations in the external interstellar medium. A predictive analysis of the appearance of possible pre-stellar zones during the evolution of new cloud formations is given.