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EP: Fachverband Extraterrestrische Physik
EP 11: Heliosphäre
EP 11.5: Talk
Thursday, March 29, 2007, 10:45–11:00, H46
The Influence of the Interplanetary Magnetic Field on Particle Propagation in the Heliosphere — •Oliver Sternal1, Bernd Heber1, Adri Burger2, Horst Fichtner3, and Phillip Dunzlaff1 — 1Institut für Experimentelle und Angewandte Physik, Christian-Albrechts-Universität zu Kiel, Leibnizstr. 11/405, D-24118 Kiel, Germany — 2School of Physics, North-West University (Potchefstroom Campus), 2520 Potchefstroom, South Africa — 3Institut für Theoretische Physik,Lehrstuhl IV: Weltraum- und Astrophysik, Ruhr-Universität Bochum, D-44780 Bochum, Germany
The propagation of energetic particles in the vicinity of the Sun is described by the Parker transport equation. It includes the physical processes of diffusion, drift, convection and adiabatic energy changes. The modulation of the particle spectra can be modelled numerically and the solutions can be tested against the in-situ observations of spacecraft, e.g. IMP, SOHO or Ulysses.
One important part of the numerical simulations is the configuration of the heliospheric magnetic field. Since its exact geometry is still an open question, we study the effect of different magnetic field models on the particle propagation and compare our model results to Ulysses measurements.