Nonresonant Beam-Type Cyclotron Instability at the Supernova Shock: Analytical Linear Theory and Numerical Simulation of the Nonlinear Evolution

Details Nonresonant Beam-Type Cyclotron Instability at the Supernova Shock: Analytical Linear Theory and Numerical Simulation of the Nonlinear Evolution Nonresonant Beam-Type Cyclotron Instability at the Supernova Shock: Analytical Linear Theory and Numerical Simulation of the Nonlinear Evolution

Nov 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aps..dpp..7q16s&link_type=abstract

American Physical Society, Division of Plasma Physics Meeting, November 10-15, 1996, abstract #7Q.16

Physics

Plasma Physics

Scientific paper

Upstream from the supernova quasiparallel shock wave the hot component representing cosmic rays is locked at the shock front due to the scattering in the magnetic field fluctuations and is accelerated by the diffusive shock acceleration mechanism. Cosmic ray population being isotropic in the shock frame and drifting with the shock velocity relative to the interstellar plasma is shown to be unstable in respect to the non-resonant beam type electromagnetic instability similar to the fire-hose. Analysis of the dispersion relation of the instability shows that for powerlike distribution of cosmic ray particles f(ɛ)∝ ɛ-4 resulting from the diffusive shock acceleration, the maximum growth rate of magnetic fluctuations occurs at the wavelengths comparable with the gyroradius at the upper edge of the energy spectrum. Diffusion of cosmic ray particles caused by such extremely long fluctuations of the magnetic field is calculated and is shown to be especially important for the most energetic part of cosmic rays.

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