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1.3 PHYSICAL SCIENCES
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 ,  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.
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 2006.