3-DIMENSIONAL TRANSPORT OF COSMIC-RAYS IN THE HELIOSPHERE

The three-dimensional transport of cosmic rays in the heliosphere is reviewed. We report on results from our numerical simulations including convection, anisotropic diffusion, drifts, and both adiabatic energy loss and shock acceleration. Our model-heliosphere incorporates a wavy current sheet and Corotating Interaction Regions due to the increase of solar wind speed away from the current sheet. We are able to model the latitudinal as well as longitudinal variations, which latter appear as 26- and 13-day intensity waves. Our simulations for solar-wind speed, magnetic field, and cosmic-ray variations seem in general form quite similar to observational findings. Quantitative predictions depend on a number of physical parameters as the parallel and perpendicular diffusion coefficients, as well as on assumptions made on the structure of the heliospheric magnetic fields.