MATHEMATICAL SIMULATION OF A MASSIVE STAR EVOLUTION ON THE BASIS OF A GASDYNAMICAL MODEL
The FLOW method, coupled with an algorithm for self-gravity computations, is applied for three-dimensional modeling of astrophysical flows. This method is based on difference approximations of conservation laws, written for finite volumes. It is implemented within the simulation tool box FLUX, designed for computer systems of cluster architecture. The problem of hydrodynamic simulation in a model of a massive star of third generation (Pop III), which is a progenitor of pair instability supernova (PISN), is considered. Large-scale convective structures are produced under the neutral equilibrium conditions that significantly affect the process of a supernova explosion.