Document Type

Conference Paper

Rights

This item is available under a Creative Commons License for non-commercial use only

Disciplines

1.3 PHYSICAL SCIENCES

Publication Details

33rd EPS Conference on Plasma Phys.

Rome, 19 - 23 June 2006

ECA Vol.30I, P-4.056 (2006)

http://epsppd.epfl.ch/Roma/pdf/P4_056.pdf

Abstract

A central problem in the theory of cosmic ray acceleration at supernova shock fronts is the generation of turbulent magnetic fields needed to scatter particles across a shock front. In this paper we build on previous studies [1], [2] into the effect of streaming cosmic rays produced by the outer shocks of supernova remnants on the stochastic component of the magnetic field. A three dimensional, MHD code has been constructed which demonstrates the nonlinear growth of the turbulent field.

DOI

https://doi.org/10.21427/dgzw-f436

Funder

COSMOGRID.

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