Interplanetary transport of solar cosmic rays

Details Interplanetary transport of solar cosmic rays Interplanetary transport of solar cosmic rays

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993nuphs..33..200a&link_type=abstract

Nuclear Physics B Proceedings Supplements, Volume 33, Issue 1-2, p. 200-207.

Physics

Nuclear Physics

Scientific paper

Quasilinear theories successfully describing interplanetary cosmic ray diffusion have up to now neglected the fact that the high-frequency, dissipative part of the scattering solar wind turbulence cannot be Alfvénic or magnetostatic. We have therefore attempted to give a more realistic model of an observed interplanetary turbulence spectrum. The most simple picture we find requires the dissipation range to be constituted of parallel dispersive whistler, electron and ion cyclotron waves in a warm plasma (β ~ 1). From this model the interplanetary mean free path of solar energetic electrons and protons has been calculated. The result is compared with the empirical findings for this parameter. Since the theoretical values are systematically larger additional scattering processes could now be helpful to decrease the mean free path to the observed values. Possible candidates could be nonlinear resonance broadening or nonresonant scattering processes.

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