Energy Partition between Energetic Electrons and Turbulent Magnetic Field in Supernova Remnant RX J1713.7-3946

Abstract

Current observations of supernova remnant (SNR) RX J1713.7-3946 favor the leptonic scenario for the TeV emission, where the radio to X-ray emission is produced via the synchrotron process and the $\gamma$-ray emission is produced via the inverse Comptonization of soft background photons, and the electron distribution can be inferred from the observed $\gamma$-ray spectrum with a spectral inversion method. It is shown that the observed correlation between the X-ray and $\gamma$-ray brightness of SNR RX J1713.7-3946 can be readily explained with the assumption that the energy density of energetic electrons is proportional to that of the magnetic field in such a scenario. A 2D magnetohydrodynamic simulation is then carried out to model the overall emission spectrum. It is found that the total energy of electrons above $\sim 1$ GeV is equal to that of the magnetic field. This is the first piece of observational evidence for energy equipartition between energetic electrons and magnetic field in the downstream of strong collision-less astrophysical shocks of SNRs.

3 figures. to appear on ApJ

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• The Hunt for Pevatrons: The Case of Supernova Remnants
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• Fermi Large Area Telescope observations of the supernova remnant HESS J1731-347
• Evolution of High-Energy Particle Distribution in Mature Shell-Type Supernova Remnants
• The structure of TeV-bright shell-type supernova remnants
• Gamma rays and neutrinos from RX J1713.7-3946 in a lepto-hadronic scenario
• Radial Profiles of Non-thermal Emission from Supernova Remnant RX J1713.7-3946
• Multiwavelength study of non-thermal emission in the Swift J1834.9-0846/W41 region