Simulation of the collision dynamics of molecular clouds using heterogeneous systems

The paper presents the results of computer simulation of the collision of rotating mo-lecular clouds in the interstellar medium. As the matter is compressed in the cloud collision region, the gas density increases here, the Jeans wavelength decreases, which leads to a change in the shape and fragmentation of clouds and their remnants. The density of gas in these clumps increases by many orders of magnitude, gravitationally bound regions arise with the possible formation of star clusters in these zones. The process of star origination is accompanied by complex spatial and temporal transformations of interstellar gas, determined by the nonlinear interaction of the turbulence of the medium, gravity, changes in the distribution of the magnetic field and radiation at the prestellar stage of evolution. The rotation of molecular clouds has a great influence on the ongoing processes. The effects of rotation in the modeling of collision processes began to be taken into account in simulation relatively recently. The evolution of pre-stellar regions, from the time they originate in high energy streams to the time they reach protostellar density, spans a huge range of scales, leading to a major computational problem in numerical simulation. Modeling of such astrophysical processes on ultra-high-resolution computa-tional grids requires a significant increase in computer power with the organization of parallel computing on heterogeneous systems.