3D MHD Simulations from the Onset of the SN to the Full-fledged SNR: Role of Ejecta Clumps on Matter Mixing
Abstract
The physical properties and the morphology of supernova remnants (SNRs) partially reflect the structure of the stellar progenitor and possible asymmetries developed soon after their parent supernova (SN) explosions. The aim of this work is to bridge the gap between SNe and their remnants by investigating how the various chemically homogeneous layers at the time of the explosion map into the resulting abundance pattern observed when the remnant is fully developed. To this end, we have performed three-dimensional magneto-hydrodynamical simulations starting soon after the SN and following the interaction of the SN ejecta with the CSM (consisting in the wind of the stellar progenitor), obtaining the physical scenario of a SNR. As stellar progenitor, we have considered the case of a 19 M⊙ red supergiant. We investigated how the evolution of a post-explosion large-scale anisotropy in the ejecta and the role of its initial parameters (position, dimension, density and velocity contrast) can affect the ejecta distribution and the matter mixing of heavy elements in the remnant, covering 5000 years of evolution.
- Publication:
-
Supernova Remnants: An Odyssey in Space after Stellar Death II
- Pub Date:
- June 2019
- Bibcode:
- 2019sros.confE..91T