Computer simulations of cosmic-ray diffusion near supernova remnant shock waves

Details Computer simulations of cosmic-ray diffusion near supernova remnant shock waves Computer simulations of cosmic-ray diffusion near supernova remnant shock waves

Jan 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989plap.work...45m&link_type=abstract

In ESA, Proceedings of an International School and Workshop on Plasma Astrophysics, Volume 1 p 45-52(SEE N89-24910 18-75)

Astronomy and Astrophysics

Astrophysics

Cosmic Rays, Plasma Acceleration, Plasma Diffusion, Plasma-Particle Interactions, Shock Wave Propagation, Supernova Remnants, Computerized Simulation, Interstellar Matter, Magnetohydrodynamic Waves, Planetary Magnetic Fields, Trapped Particles

Scientific paper

A plasma simulation model was used to study the resonant interactions between streaming cosmic-ray ions and a self-consistent spectrum of Alfven waves, such as might exist in the interstellar medium upstream of a supernova remnant shock wave. The computational model is a hybrid one, in which the background interstellar medium is an MHD fluid and the cosmic-rays are discrete kinetic particles. The particle sources for the electromagnetic fields are obtained by averaging over the fast cyclotron motions. When the perturbed magnetic field is larger than 10 percent of the background field, the macro- and microphysics are no longer correctly predicted by quasi-linear theory. The particles are trapped by the waves and show sharp jumps in their pitch-angles relative to the background magnetic field, and the effective ninety-degree scattering time for diffusion parallel to the background magnetic field is reduced to between 5 and 30 cyclotron periods. Simulation results suggest that Type 1 supernova remnants may be the principal sites of cosmic ray acceleration.

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