The Propagation of Energetic Particles in Different Heliospheric Magnetic Field Configurations

O. Sternal¹, B. Heber¹, A. Burger², H. Fichtner³

¹Institut fur experimentelle und angewandte Physik, Christian-Albrechts-Universitaet zu Kiel, Leibnizstr. 11, 24148 Kiel, Germany
²School of Physics, North-West University, 2520 Potchefstroom, South Africa
³Institut fur Theoretische Physik, Lehrstuhl IV: Weltraum und Astrophysik, Ruhr-Universitaet Bochum, 44780 Bochum, Germany

The propagation of energetic particles in the heliosphere is described by the Parker transport equation. It includes the physical processes of diffusion, drift, convection and adiabatic energy changes. For the modulation of the particles’ energy spectra the geometry of the heliospheric magnetic field is important, but still an unsolved problem. In this contribution we present calculations of the 7 MeV electron flux in the heliosphere and compare our results to spacecraft measurements.