Cosmic-ray particle transport in weakly turbulent plasmas. 2. Mean free path of cosmic-ray protons.

Details Cosmic-ray particle transport in weakly turbulent plasmas. 2. Mean free path of cosmic-ray protons. Cosmic-ray particle transport in weakly turbulent plasmas. 2. Mean free path of cosmic-ray protons.

Aug 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993jplph..50...85s&link_type=abstract

Journal of Plasma Physics, Vol. 50, No. 1, p. 85 - 107

Physics

Plasma Physics

10

Scientific paper

The authors use the general Fokker-Planck coefficients derived in the first paper of this series, which describe the interaction of energetic charged particles with weak plasma turbulence in a magnetized plasma, to calculate the mean free path λ of cosmic-ray particles along the uniform background magnetic field. This quantity is a key parameter for confining energetic charged particles in cosmic plasmas, and can be experimentally inferred from interplanetary in-situ observations of solar particle events. The calculation is performed for two recent models of the random electromagnetic field: the dynamical-wave turbulence model and the plasma-wave turbulence model. Of particular interest are the consequences of the occurring linear resonance broadening on λ resulting either from dynamical-turbulence decay with time and damping of the left-handed plasma waves in the warm background plasma near the proton gyrofrequency respectively. The authors compare the resulting mean free path with interplanetary observations, and they derive decisive predictions that will allow future tests of these models with solar particle event data.

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