Hydrodynamic instability in supernova remnants3D ModelNoAI
The animation shows the evolution of a supernova blast wave from the outburst to the expanded remnant at the age of 350 years. Only a small portion of the remnant is reproduced. All scales are normalized to allow for easy inspection of the remnant structure at all evolutionary phases. The initial blast wave radius is ~ 1e8 km (100 millions km), the final radius is ~ 8e13 km (2.5 parsec). The bar at the bottom shows the age (in years) and radius (in parsec = 3.09e13 km) of the blast wave in logarithmic scale. The small-scale features visible in the remnant interior are the results of hydrodynamic instability developing at the contact discontinuity between the shock-heated stellar debris (the ejecta) and the shock-heated ambient medium.
MHD simulation performed with the FLASH code.
Reference: Orlando et al. 2016, 822, id. 22.
Credits: INAF-Osservatorio Astronomico di Palermo.
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