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Astron. Astrophys. 326, 793-800 (1997)

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Simulations of cosmic ray cross field diffusion
in highly perturbed magnetic fields

G. Michaek 1 and M. Ostrowski 1, 2

1 Obserwatorium Astronomiczne, Uniwersytet Jagielloski, ul.Orla 171, Pl-30-244 Kraków, Poland
2 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany

Received 10 January 1997 / Accepted 20 May 1997


The process of particle cross-field diffusion in high amplitude Alfvénic turbulence is considered using the method of the Monte Carlo particle simulations. We derive the cross-field diffusion coefficient [FORMULA] and the parallel diffusion coefficient [FORMULA] in the presence of different 1-D, 2-D and 3-D turbulent wave field models and discuss the [FORMULA], [FORMULA] and [FORMULA] variations with the wave amplitude. [FORMULA] is compared also to the respective derived values of the magnetic field diffusion coefficient. We note substantial differences in the cross-field diffusion efficiency at the same perturbation amplitude, depending on the detailed form of the turbulent field considered. Vanishing of [FORMULA] at 1-D and 2-D turbulent fields is confirmed. For some types of the turbulent magnetic field an initial regime of sub-diffusive transport appears in the simulations. The derived values of [FORMULA] are weakly dependent on the wave form and scale as the inverse of the squared perturbation amplitude up to our highest non-linear amplitudes.

Key words: cosmic rays – MHD-turbulence – acceleration of particles – diffusion

Send offprint requests to: G. Michalek (michalek@oa.uj.edu.pl)


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© European Southern Observatory (ESO) 1997

Online publication: November 3, 1997