The models aim to explore the extent to which supernova remnants (SNRs) retain memory of the asymmetries that arise stochastically in the neutrino-heating layer due to hydrodynamic instabilities (e.g., convective overturn and the standing accretion shock instability) during the first seconds after core bounce.

These models incorporate all relevant physical processes to describe the complexities in supernova evolution and the subsequent interaction of stellar debris with the progenitor star's wind. The 3D graphics illustrate the distribution of ejecta at the age of the Cassiopeia A SNR and demonstrate that the chemical and physical properties of its ejecta can be explained in terms of asymmetries that originated from stochastic processes during the first seconds of the supernova blast.

Numerical code: PLUTO.

Simulations performed at CINECA (Italy).

References:

- S. Orlando, A. Wongwathanarat, H.-T. Janka, et al. 2021, A&A 645, A66

- S. Orlando, A. Wongwathanarat, H.-T. Janka, et al. 2022, A&A 666, A2