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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. doi:10.21427/dgzw-f436