Mathematical Simulation of a Massive Star Evolution Based on a Gasdynamical Model

Аннотация

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