ИСТИНА

The purpose of the present numerical simulation is to analyze density fragmentation process in small molecular clouds shocked by a shock wave of supernova blast remnants. We consider dynamical formation of MC structures associated with KelvinHelmholtz and Richtmayer-Meshkov instabilities taking place in a zone of the cloud and interstellar medium interaction. Form driving effects for one and two cloud systems are studied. The MC gas flow evolution is derived by solving the time dependent equations of mass, momentum, and energy conservation. High resolution numerical grids (more than two billion nodes) were used in parallel calculations on multiprocessor hybrid computers. The first of modelling task was a single cloud SW/MC interaction. In the second case two initially spatially perceptible clouds with pre-established gravitational fields interact with the post-shock medium. The peculiarities of cloud-clump-shell fragmentation and formation of generated structures are discussed.