Linking core-collapse supernova explosions to supernova remnants through 3D MHD modeling

TL;DR

This paper uses 3D MHD simulations to connect the physical and morphological features of supernova remnants with their parent supernova explosions, enhancing understanding of explosion processes through comparison with observations of Cas A.

Contribution

It presents a comprehensive 3D MHD model tracing the evolution from core-collapse supernovae to remnants, linking explosion anisotropies to remnant morphology, a novel approach in supernova research.

Findings

Simulated SNR evolution matches observed features of Cas A.

Linked physical and chemical properties of SNRs to explosion mechanisms.

Provided insights into the complex phases of supernova explosions.

Abstract

The structure and morphology of supernova remnants (SNRs) reflect the properties of the parent supernovae (SNe) and the characteristics of the inhomogeneous environments through which the remnants expand. Linking the morphology of SNRs to anisotropies developed in their parent SNe can be essential to obtain key information on many aspects of the explosion processes associated with SNe. Nowadays, our capability to study the SN-SNR connection has been largely improved thanks to multi-dimensional models describing the long-term evolution from the SN to the SNR as well as to observational data of growing quality and quantity across the electromagnetic spectrum which allow to constrain the models. Here we used the numerical resources obtained in the framework of the "Accordo Quadro INAF-CINECA (2017)" together with a CINECA ISCRA Award N.HP10BARP6Y to describe the full evolution of a SNR from the core-collapse to the full-fledged SNR at the age of 2000 years. Our simulations were compared with observations of SNR Cassiopeia A (Cas A) at the age of $\sim 350$~years. Thanks to these simulations we were able to link the physical, chemical and morphological properties of a SNR to the physical processes governing the complex phases of the SN explosion.