Non-thermal X-rays and interstellar gas toward the \gamma-ray supernova remnant RX J1713.7-3946: Evidence for X-ray enhancement around CO and HI clumps

TL;DR

This study investigates the relationship between X-ray emission and interstellar gas in the supernova remnant RX J1713.7-3946, revealing enhanced X-ray emission around gas clumps likely due to magnetic field amplification from shock interactions.

Contribution

It provides observational evidence linking X-ray enhancement to gas clumps and supports magnetic field amplification as a key factor in cosmic-ray acceleration in supernova remnants.

Findings

X-ray enhancement around CO and HI clumps on a parsec scale.

Decreased X-ray emission inside the gas clumps on a 0.1 pc scale.

Magnetic field amplification due to shock interaction with gas clumps.

Abstract

RX J1713.7-3946 is the most remarkable very-high-energy \gamma-ray supernova remnant which emits synchrotron X-rays without thermal features. We made a comparative study of CO, HI and X-rays in order to better understand the relationship between the X-rays, and the molecular and atomic gas. The results indicate that the X-rays are enhanced around the CO and HI clumps on a pc scale but are decreased inside the clumps on a 0.1 pc scale. Magnetohydrodynamic numerical simulations of the shock interaction with molecular and atomic gas indicate that the interaction between the shock waves and the clumps excite turbulence which amplifies the magnetic field around the clumps (Inoue et al. 2012). We suggest that the amplified magnetic field around the CO and HI clumps enhances the synchrotron X-rays and possibly the acceleration of cosmic-ray electrons.