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MHD Simulation of the Supernova Remnant Dynamics Taking into Account the Neutral Plasma Component

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Abstract

The technique and results of three-dimensional modeling of a radiative shock wave that occurs when a supernova remnant expands into the surrounding interstellar medium are presented. The aim of the calculations is to analyze the hydrodynamic instability in a dense layer of matter formed during the deceleration of the remnant in the interstellar gas. The layer structure, which largely determines the efficiency of cosmic ray generation, depends on a number of factors and, in particular, on the rate of radiative cooling of the interstellar plasma, the magnitude of the magnetic field, and the presence of a neutral component in the ionized medium. The creation of a methodology and software for assessing these factors is the defining motivation for this work. For modeling, the MARPLE3D software package (Keldysh Institute of Applied Mathematics, Russian Academy of Sciences) is used, which was developed to solve problems of magnetic radiative gas dynamics on high-performance computing systems of the cluster type.

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ACKNOWLEDGMENTS

The author thanks her colleagues S.I. Blinnikov, V.A. Gasilov, and S.I. Glazyrin for their useful discussions about the formulation of problems and the results of computational experiments.

Funding

This study was supported by the Russian Science Foundation (grant no. 21-11-00362).

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Authors and Affiliations

  1. Keldysh Institute of Applied Mathematics, Russian Academy of Sciences, Moscow, Russia

    Yu. S. Sharova

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  1. Yu. S. Sharova
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Correspondence to Yu. S. Sharova.

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Sharova, Y.S. MHD Simulation of the Supernova Remnant Dynamics Taking into Account the Neutral Plasma Component. Math Models Comput Simul 14, 654–661 (2022). https://doi.org/10.1134/S2070048222040111

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