Email this article Mathematical Simulation of a Massive Star Evolution Based on a Gasdynamical Model
- Authors: Babakov A.V.1, Popov M.V.2,3, Chechetkin V.M.3,4,5
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Affiliations:
- Institute for Computer Aided Design
- École Normale Supérieure de Lyon
- Keldysh Institute of Applied Mathematics
- National Research Nuclear University MEPhI
- Kurchatov Institute of Atomic Energy
- Issue: Vol 10, No 3 (2018)
- Pages: 357-362
- Section: Article
- URL: https://journals.rcsi.science/2070-0482/article/view/202381
- DOI: https://doi.org/10.1134/S2070048218030031
- ID: 202381
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Abstract
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.
About the authors
A. V. Babakov
Institute for Computer Aided Design
Email: chechetv@gmail.com
Russian Federation, Moscow, 123056
M. V. Popov
École Normale Supérieure de Lyon; Keldysh Institute of Applied Mathematics
Email: chechetv@gmail.com
France, Lyon; Moscow, 125047
V. M. Chechetkin
Keldysh Institute of Applied Mathematics; National Research Nuclear University MEPhI; Kurchatov Institute of Atomic Energy
Author for correspondence.
Email: chechetv@gmail.com
Russian Federation, Moscow, 125047; Moscow, 115409; Moscow, 123182
