Inverse Compton emission from a cosmic-ray precursor in RX J1713.7-3946

TL;DR

This paper explains recent gamma-ray observations of supernova remnant RX J1713.7-3946 through inverse Compton emission from accelerated electrons, proposing a model where electron energy decreases over time and a cosmic-ray precursor causes extended gamma-ray emission.

Contribution

It introduces a novel explanation for the observed gamma-ray spectrum and spatial profile based on inverse Compton emission and cosmic-ray precursor effects.

Findings

Broken power-law gamma-ray spectrum explained by electron accumulation.

Extended gamma-ray emission interpreted as a cosmic-ray precursor.

Model suggests decreasing maximum electron energy over time.

Abstract

Recently, the High Energy Stereoscopic System (H.E.S.S.) reported two new interesting results for a gamma-ray emitting supernova remnant, RX J1713.7-3946 (G347.3-0.5). The first result is the establishment of a broken power-law spectrum of GeV-TeV gamma-rays. The other is a more extended gamma-ray spatial profile than the one in the X-ray band. In this paper, we show both of these results can be explained by inverse Compton emission from accelerated electrons. If the maximum energy of electrons being accelerated decreases with time, the broken power-law spectrum can be generated by accumulation. Furthermore, the extended component of gamma-ray profile can be interpreted as a CR precursor of currently accelerated electrons.