Diffusive Shock Acceleration with Magnetic Amplification by Non-resonant Streaming Instability in SNRs
Astrophysics
2009-11-13 v1
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.
Keywords
Cite
@article{arxiv.0801.4488,
title = {Diffusive Shock Acceleration with Magnetic Amplification by Non-resonant Streaming Instability in SNRs},
author = {V. N. Zirakashvili and V. S. Ptuskin},
journal= {arXiv preprint arXiv:0801.4488},
year = {2009}
}
Comments
18 pages, 9 figures, accepted to ApJ