Numerical simulations of diffusive shock acceleration in SNRs

TL;DR

This paper introduces a new numerical model for nonlinear diffusive shock acceleration in supernova remnants, coupling hydrodynamics with particle transport to study cosmic ray spectra and the role of shocks.

Contribution

It presents a novel coupled hydrodynamic and particle transport model for simulating cosmic ray acceleration in SNRs, including forward and reverse shocks.

Findings

Cosmic ray spectra are computed for SNRs.

Reverse shock significantly influences CR ion and positron production.

Model advances understanding of particle acceleration mechanisms.

Abstract

A new numerical model of the nonlinear diffusive shock acceleration is presented. It is used for modeling of particle acceleration in supernova remnants. The model contains coupled spherically symmetric hydrodynamic equations and the transport equations for energetic protons, ions and electrons. The forward and reverse shocks are included in the consideration. The spectra of cosmic rays released into interstellar medium from a supernova remnant are determined. The role of the reverse shock in the production of CR ions and positrons is discussed.