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

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

2008-01-29

arxiv.org/abs/0801.4488v1

Astronomy and Astrophysics

Astrophysics

18 pages, 9 figures, accepted to ApJ

Scientific paper

10.1086/529580

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.

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