Magnetic field damping in the Vela Jr. SNR

Abstract

Vela Jr. (RX J0852.0−4622) is one of just a few known supernova remnants (SNRs) with the resolved shell across the whole electromagnetic spectrum from radio to very-high-energy (>100 GeV; VHE) gamma-rays. Its proximity and large size allow for detailed spatially resolved observations of the source making Vela Jr. one of the primary sources used for the study of particle acceleration and emission mechanisms in SNRs. High-resolution X-ray observations reveal steepening of the spectrum towards the interior of the remnant. In this study we aim for the self-consistent radiation model of Vela Jr. which at the same time would explain the broadband emission from the source and its spatially-dependent features. We solve the full particle transport equation combined with the high-resolution 1D hydrodynamic simulations (using Pluto code) and subsequently calculate the radiation from the remnant. We show that accounting for the damping of strong magnetic turbulence downstream of the forward shock might explain the observed radial dependence of the X-ray spectrum.