Abstract
Relativistic particle acceleration in collisionless shocks of supernova remnants is accompanied with magnetic field amplification by cosmic ray (CR) driven plasma instabilities. Bell’s fast CR-current instability is predicted to produce turbulence with a non-zero mean electric field in the shock precursor. We present a Monte Carlo model of Fermi shock acceleration explicitly taking into account an effective mean upstream electric field. Our model is nonlinear and includes the backreaction effects of efficient Fermi acceleration on the shock structure.
Highlights
The converging plasmas on either side of a collisionless shock allow particle acceleration as particles scatter nearly elastically between the upstream and downstream regions
The scattering centers are magnetic field fluctuations moving with the background plasma and multiple crossing of the collisionless shock front can result in significant energy gains for individual particles
There is strong evidence to show that anisotropic cosmic ray (CR) distributions in the shock precursor leads to the development of plasma instabilities and magnetic field amplification (MFA) (e.g. [2])
Summary
The converging plasmas on either side of a collisionless shock allow particle acceleration as particles scatter nearly elastically between the upstream and downstream regions. Several nonlinear models of efficient DSA in SNRs were constructed to account for the backreaction of accelerated particles on the dynamics of the background plasma which carries the scattering centers (see, for example, [5, 6, 7]).
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