Physics of Shocks with Strong Cosmic Ray Acceleration

Details Physics of Shocks with Strong Cosmic Ray Acceleration Physics of Shocks with Strong Cosmic Ray Acceleration

Feb 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sgrb.confe..20e&link_type=abstract

Presented at the KITP Conference: Supernova and Gamma-Ray Burst Remnants, Feb 9, 2006, Kavli Institute for Theoretical Physics,

Physics

Scientific paper

The theory of diffusive shock acceleration (DSA) operating instrong, nonrelativistic shocks, clearly allows for the mechanism to behighly efficient. However, it is still an open question if actualcollisionless shocks, such as those in young supernova remnants (SNRs), areas efficient as predicted. Fortunately, the nonlinear feedback effectsresulting from efficient DSA should produce observable consequencesincluding changes in the morphology of the remnant and a strongly amplifiedmagnetic field. I will outline the theory for nonlinear DSA and apply it torecent observations of young SNRs. Preliminary work on magnetic fieldamplification will also be presented. This work, which employs awell-tested Monte Carlo simulation, will self-consistently determine theplasma flow, magnetic field, and particle spectrum. Amplified magneticfields may result in large increases in the maximum particle energyproduced in a given shock.

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