Document Type
Conference Paper
Rights
This item is available under a Creative Commons License for non-commercial use only
Disciplines
1.3 PHYSICAL SCIENCES
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
Recommended Citation
Reville, B,. Duffy, P., & O'Suillivan, S. (2006). The nonlinear amplification of magnetic fields by cosmic rays at supernova remnant shocks, 33rd EPS Conference on Plasma Phys. Rome, 19 - 23 June. doi:10.21427/dgzw-f436
Funder
COSMOGRID.
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