Interplanetary magnetic fields and the propagation of cosmic rays
Abstract
Results and limitations of the diffusionconvection model for cosmicray propagation in the interplanetary space are presented. The first part discusses magnetic field fluctuations on various scales, in particular the power spectral representation and its relation to cosmic ray diffusion in pitch angle and real space, and the nonresonant scattering at magnetic field discontinuities. The second part analyzes how far the diffusion model can be used to obtain a unified view for the propagation of both galactic and solar cosmic rays. It is shown that mean free paths derived from timeintensity profiles of solar events increase when solar injection processes are taken into account. A picture is obtained in which the local mean free path is on the average relatively large (of the order 0.1 AU for rigidities below a few hundered MV). The propagation conditions are highly variable, ranging from locally almost convective transport to scatterfree propagation. Some of the limitations of the diffusion model are mentioned, and the concept of collimated convection is discussed.
 Publication:

Zeitschrift fur Geophysik
 Pub Date:
 1974
 Bibcode:
 1974ZGeo...40..667W
 Keywords:

 Cosmic Plasma;
 Galactic Radiation;
 Interplanetary Magnetic Fields;
 Particle Motion;
 Solar Cosmic Rays;
 Convection;
 Diffusion Theory;
 Mean Free Path;
 Power Spectra;
 Resonance Scattering;
 Scatter Propagation;
 Solar Wind