3D simulations of supernova remnants evolution including non-linear particle acceleration

TL;DR

This study uses 3D hydrodynamic simulations coupled with shock acceleration models to explore how energetic particles influence supernova remnant evolution, aligning with recent X-ray observations of Tycho's remnant.

Contribution

It introduces a novel coupling of kinetic shock acceleration models with 3D hydrodynamics to analyze supernova remnant morphology and particle acceleration effects.

Findings

Density profiles vary with particle injection level

Rayleigh-Taylor instability extent is unaffected by injection rate

Simulations support efficient proton acceleration in Tycho's remnant

Abstract

If a sizeable fraction of the energy of supernova remnant shocks is channeled into energetic particles (commonly identified with Galactic cosmic rays), then the morphological evolution of the remnants must be distinctly modified. Evidence of such modifications has been recently obtained with the Chandra and XMM-Newton X-ray satellites. To investigate these effects, we coupled a semi-analytical kinetic model of shock acceleration with a 3D hydrodynamic code (by means of an effective adiabatic index). This enables us to study the time-dependent compression of the region between the forward and reverse shocks due to the back reaction of accelerated particles, concomitantly with the development of the Rayleigh-Taylor hydrodynamic instability at the contact discontinuity. Density profiles depend critically on the injection level eta of particles: for eta up to about 10^-4 modifications are weak and progressive, for eta of the order of 10^-3 modifications are strong and immediate. Nevertheless, the extension of the Rayleigh-Taylor unstable region does not depend on the injection rate. A first comparison of our simulations with observations of Tycho's remnant strengthens the case for efficient acceleration of protons at the forward shock.