Diffusive Shock Acceleration with Magnetic Amplification by Non-resonant Streaming Instability in SNRs

Abstract

We investigate the diffusive shock acceleration in the presence of the non-resonant streaming instability introduced by Bell (2004). The numerical MHD simulations of the magnetic field amplification combined with the analytical treatment of cosmic ray acceleration permit us to calculate the maximum energy of particles accelerated by high-velocity supernova shocks. The estimates for Cas A, Kepler, SN1006, and Tycho historical supernova remnants are given. We also found that the amplified magnetic field is preferentially oriented perpendicular to the shock front downstream of the fast shock. This explains the origin of the radial magnetic fields observed in young supernova remnants.

18 pages, 9 figures, accepted to ApJ

References in corpus (2)

• Modeling Bell's Non-resonant Cosmic Ray Instability
• Variation of cosmic ray injection across supernova shocks

Cited by in corpus (5)

• A kinetic approach to cosmic ray induced streaming instability at supernova shocks
• Dynamical Feedback of Self-generated Magnetic Fields in Cosmic Ray Modified Shocks
• Non-Maxwellian Proton Velocity Distributions in Nonradiative Shocks
• 3-D Model of Broadband Emission from Supernova Remnants Undergoing Non-linear Diffusive Shock Acceleration
• Evolution of Magnetic Fields and Cosmic Ray Acceleration in Supernova Remnants