Stochastic Electron Acceleration in Shell-Type Supernova Remnants

TL;DR

This paper investigates how stochastic electron acceleration by fast mode waves in turbulent regions behind supernova remnant shocks explains observed high-energy emissions, linking shock properties to acceleration efficiency.

Contribution

It introduces a model for stochastic electron acceleration in supernova remnants that accounts for turbulence and shock parameters, explaining observed emissions.

Findings

Model explains X-ray and gamma-ray observations of specific supernova remnants.

Acceleration is most efficient in a dissipative layer behind shocks.

Predictions can be tested with upcoming X-ray and gamma-ray observations.

Abstract

We study the stochastic electron acceleration by fast mode waves in the turbulent downstream of weakly magnetized collisionless astrophysical shocks. The acceleration is most efficient in a dissipative layer, and the model characteristics are determined by the shock speed, density, magnetic field, and turbulence decay length. The model explains observations of shell-type supernova remnants RX J1713.7-3946 and J0852.0-4622 and can be tested by observations in hard X-rays with the HXMT and NuSTAR or gamma-rays with the GLAST.