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Abstract:
First order Fermi acceleration at the outer shocks of supernova remnants can be a very efficient process. The pressure of the cosmic rays may have a significant effect on the fluid properties of the upstream plasma, creating an extended shock precursor. It has been suggested by Bell (2004) that cosmic rays in the precursor will also have a strong influence on the macroscopic properties of the magnetic field. Observational evidence of bright X-ray synchrotron rims in several young supernova remnants support this theory. Amplification of the magnetic field beyond the linear regime, via the non-resonant current driven instability is investigated. We report on numerical calculations of magnetic field growth and the resulting transport properties of relativistic particles in the amplified field.
