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

作     者：Babakov, A.V. Popov, M.V. Chechetkin, V.M. 

作者机构：Institute for Computer Aided Design Russian Academy of Sciences Moscow 123056 Russian Federation École Normale Supérieure de Lyon CRAL (UMR CNRS 5574) Université de Lyon 1 Lyon France Keldysh Institute of Applied Mathematics Russian Academy of Sciences Moscow 125047 Russian Federation National Research Nuclear University MEPhI Moscow 115409 Russian Federation Kurchatov Institute of Atomic Energy Moscow 123182 Russian Federation 

出 版 物：《Mathematical Models and Computer Simulations》 (Math. Models Comput. Simul.)

年 卷 期：2018年第10卷第3期

页      面：357-362页

学科分类：07[理学] 0714[理学-统计学（可授理学、经济学学位）] 0701[理学-数学] 0812[工学-计算机科学与技术（可授工学、理学学位）] 070101[理学-基础数学] 

基　　金：Russian Science Foundation  RSF  (16-11-10339) 

主　　题：aerohydrodynamics astrophysics conservative difference schemes gravity mathematical modeling numerical methods parallel algorithms supernovae vortex structures 

摘      要：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. © 2018, Pleiades Publishing, Ltd.