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

被引：0
|
作者：
Babakov A.V. [1 ]
Popov M.V. [2 ,3 ]
Chechetkin V.M. [3 ,4 ,5 ]
机构：
[1] Institute for Computer Aided Design, Russian Academy of Sciences, Moscow
[2] École Normale Supérieure de Lyon, CRAL (UMR CNRS 5574), Université de Lyon 1, Lyon
[3] Keldysh Institute of Applied Mathematics, Russian Academy of Sciences, Moscow
[4] National Research Nuclear University MEPhI, Moscow
[5] Kurchatov Institute of Atomic Energy, Moscow
来源：
Mathematical Models and Computer Simulations | 2018年 / 10卷 / 3期
基金：
俄罗斯科学基金会;
关键词：
aerohydrodynamics; astrophysics; conservative difference schemes; gravity; mathematical modeling; numerical methods; parallel algorithms; supernovae; vortex structures;
D O I：
10.1134/S2070048218030031
中图分类号：
学科分类号：
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.
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收藏
页码：357 / 362
页数：5
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