Spatial structure of X-ray filaments in SN 1006

TL;DR

This paper models the spatial distribution of accelerated particles in SN 1006, showing that X-ray observations align with NLDSA predictions of efficient shock acceleration and magnetic field amplification.

Contribution

It provides a detailed calculation of particle spectra and spatial distribution, confirming NLDSA predictions with observational data.

Findings

Chandra X-ray data are consistent with NLDSA predictions.

Magnetic field amplification upstream of the shock is about a factor of 10.

Efficient particle acceleration occurs at SN 1006's shock.

Abstract

The theory of Non-Linear Diffusive Shock Acceleration (NLDSA) predicts the formation of a precursor upstream of the shock, where accelerated particles diffuse and induce magnetic field amplification through streaming instability. The non detection of this precursor in X-rays in {\it Chandra} observations of the north-eastern region of SN 1006 (G329.6+14.6) led to impose an upper limit to the X-ray emission generated by accelerated electrons diffusing in this precursor, at an emissivity level of <1.5 per cent of the emission from the downstream region (Long et al. 2003). This has been used as an argument against Fermi acceleration at this shock. Here we calculate the spectrum and spatial distribution of accelerated particles in SN 1006 and show that Chandra results (including more recent data) are in perfect agreement with the predictions of NLDSA suggesting efficient particle acceleration and magnetic field amplification upstream of the shock by a factor ~10.