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Supernova remnants (SNR’s) are the outcome of supernovae (SNe), the highly-energetic explosions that signal the death of massive stars. On explosion, the stellar material is ejected from the star, and travels freely until it reaches the circumstellar medium (CSM). The CSM contains the mass-loss from the progenitor star in the years leading up to the explosion.
When the expanding SN ejecta interacts with the CSM, some of the material will continue to propagate outward in what is known as the forward shock. Conversely, some of the material will travel backwards into the freely expanding ejecta after colliding with the CSM. This is known as the reverse shock.
Asymmetries were introduced into the model in the form of dense, high-velocity clumps within the initial remnant. This model shows the density profile of the asymmetric SNR in a uniform ambient environment at a time of 2,000 years after explosion.
This simulation was produced within the framework of the PRACE Summer of HPC 2020 program.