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


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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.

作者简介

A. Babakov

Institute for Computer Aided Design

Email: chechetv@gmail.com
俄罗斯联邦, Moscow, 123056

M. Popov

École Normale Supérieure de Lyon; Keldysh Institute of Applied Mathematics

Email: chechetv@gmail.com
法国, Lyon; Moscow, 125047

V. Chechetkin

Keldysh Institute of Applied Mathematics; National Research Nuclear University MEPhI; Kurchatov Institute of Atomic Energy

编辑信件的主要联系方式.
Email: chechetv@gmail.com
俄罗斯联邦, Moscow, 125047; Moscow, 115409; Moscow, 123182

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