Numerical simulation reveals flow features and shock-induced dissipation in supernova remnants within varying interstellar medium.
In the present investigation, a supernova remnant (SNR) propagation inside the interstellar medium (ISM) is numerically simulated by solving the compressible magneto-hydrodynamic equations, employing a high-order finite volume methodology as implemented in the PLUTO solver. Flow features associated with the SNR propagated inside non-uniform ISM, is discussed thoroughly. The vortical coherent modes, identified through dynamic mode decomposition during the propagation of a SNR through a non-uniform ISM exhibit spatio-temporal decay behavior due to strong dissipation induced by the reverse shock and forward shock, respectively.
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Pal et al. (2025) studied this question.
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