Magnetic Field Amplification and Rapid Time Variations in SNR RX J1713.7-3946
arXiv:0711.4389 · doi:10.1086/527359
Abstract
Evidence is accumulating suggesting that collisionless shocks in supernova remnants (SNRs) can amplify the interstellar magnetic field to hundreds of microgauss or even milli-gauss levels, as recently claimed for SNR RX J1713.7-3946. If these fields exist, they are almost certainly created by magnetic field amplification (MFA) associated with the efficient production of cosmic rays by diffusive shock acceleration (DSA) and their existence strengthens the case for SNRs being the primary source of galactic cosmic ray ions to the `knee' and beyond. However, the high magnetic field values in SNRs are obtained exclusively from the interpretation of observations of radiation from relativistic electrons and if MFA via nonlinear DSA produces these fields the magnetic field that determines the maximum ion energy will be substantially less than the field that determines the maximum electron energy. We use results of a steady-state Monte Carlo simulation to show how nonlinear effects from efficient cosmic ray production and MFA reduce the maximum energy of protons relative to what would be expected from test-particle acceleration.
arXiv commentSubmitted to ApJ Letters October 2007, 5 pages with 2 figures
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Cited by in corpus (21)
- Observations of the young supernova remnant RX J1713.7-3946 with the Fermi Large Area Telescope
- Discovery of TeV Gamma Ray Emission from Tycho's Supernova Remnant
- A Detailed Study of the Molecular and Atomic Gas Toward the γ-ray SNR RX J1713.7-3946: Spatial TeV γ-ray and ISM Gas Correspondence
- Production of Magnetic Turbulence by Cosmic Rays Drifting Upstream of Supernova Remnant Shocks
- Gamma ray emission from SNR RX J1713.7-3946 and the origin of galactic cosmic rays
- Origin of Cosmic Rays
- Observations of the shell-type SNR Cassiopeia A at TeV energies with VERITAS
- Core-collapse model of broadband emission from SNR RX J1713.7-3946 with thermal X-rays and Gamma-rays from escaping cosmic rays
- Turbulence Dissipation and Particle Injection in Non-Linear Diffusive Shock Acceleration with Magnetic Field Amplification
- A Generalized Model of Nonlinear Diffusive Shock Acceleration Coupled to an Evolving Supernova Remnant
- Radio emission and nonlinear diffusive shock acceleration of cosmic rays in the supernova SN 1993J
- Postshock turbulence and diffusive shock acceleration in young supernova remnants
- A CR-hydro-NEI Model of Multi-wavelength Emission from the Vela Jr. Supernova Remnant (SNR RX J0852.0-4622)
- PIC simulations of the Thermal Anisotropy-Driven Weibel Instability: Field growth and phase space evolution upon saturation
- Non-Thermal X-ray Emission from the Northwestern Rim of the Galactic Supernova Remnant G266.2-1.2 (RX J0852.0-4622)
- 3-D Model of Broadband Emission from Supernova Remnants Undergoing Non-linear Diffusive Shock Acceleration
- Cosmic Ray Origin: Lessons from Ultra-High-Energy Cosmic Rays and the Galactic/Extragalactic Transition
- Dark Matter Search in Space: Combined Analysis of Cosmic Ray Antiproton-to-Proton Flux Ratio and Positron Flux Measured by AMS-02
- 3D simulations of the non-thermal broad-band emission from young supernova remnants including efficient particle acceleration
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- Molecular and atomic gas in the young TeV γ-ray SNRs RX J1713.7-3946 and RX J0852.0-4622; evidence for the hadronic production of γ-rays