Non-thermal images of SN 1006: from radio to gamma-rays

TL;DR

This paper presents a new method for synthesizing non-thermal emission maps of supernova remnant SN 1006 across radio, X-ray, and gamma-ray bands, accounting for particle injection, magnetic fields, and electron losses, and compares these models with observations.

Contribution

The paper introduces a novel modeling approach for SNR emission maps that incorporates shock obliquity, magnetic field behavior, and electron energy losses, improving the understanding of non-thermal radiation.

Findings

Models match radio and X-ray observations well.

Gamma-ray models require parameter adjustments for better fit.

Highlights the importance of magnetic field and injection parameters in SNR emission modeling.

Abstract

Supernova remnants (SNRs) are believed to be the main sources of galactic cosmic rays. Discovery of the non-thermal component in X-ray spectrum of SN 1006 in 1995 and detection of a number of SNRs by H.E.S.S. strengthen the investigation of SNRs. SN 1006 remains to be one of the most interesting objects for high-energy astrophysics. Electrons accelerated by the shock are the source of the non-thermal radiation in radio, X-rays (via synchrotron emission) and \gamma-rays (via inverse-Compton process). Experimental images of SN 1006 are known in all these bands, including the very-high energy \gamma-ray range. An important task is therefore to model the distribution of the surface brightness in SNRs. We develop a method for synthesis of SNR maps due to the non-thermal radiation of electrons in radio, X-rays and \gamma-rays. In particular, the method takes into account the injection of particles and the behaviour of magnetic field at shocks with different obliquities as well as the radiation losses of electrons downstream of the shock. The method is used to model images of SN 1006. The images well correlate with the observations in radio and X-ray but not in \gamma-ray range. For coincide in \gamma-ray range it is needed to increases parameters \eta and E_{f}.