HR: 12:05h
AN: SH32A-08    [Abstracts]
TI: Galactic cosmic ray transport in the 3D heliosphere
AU: Zank, G P
EM: zank@ucr.edu
AF: University of California, Riverside, IGPP, University of California, Riverside, CA 92521, United States
AU: * Florinski, V
EM: vflorins@ucr.edu
AF: University of California, Riverside, IGPP, University of California, Riverside, CA 92521, United States
AU: Pogorelov, N V
EM: nikolaip@ucr.edu
AF: University of California, Riverside, IGPP, University of California, Riverside, CA 92521, United States
AB: Theoretical studies of cosmic-ray propagation have been to date restricted to simplified problem geometries due to certain symmetry assumptions related to the solar rotation or the relative motion between the Sun and the surrounding interstellar cloud. However, the heliosphere is an essentially three-dimensional structure lacking any symmetry owing to misalignment between the various plasma and neutral atom flows and the complex interaction between the interstellar and interplanetary magnetic fields at the heliopause. Here we present first results from the project currently underway at IGPP/UCR to develop a fully three-dimensional model of cosmic-ray propagation through the global heliosphere. Our model uses plasma and magnetic field background calculated on the basis of a complete 3D MHD-neutral global heliospheric models and includes drift and diffusive spatial transport as well as adiabatic acceleration or cooling in compressive or expanding plasma flows. Test result sets are compiled for the plasma topology corresponding to solar minimum conditions. Emphasis is placed on the role of the inner heliosheath as the region responsible for the bulk of the total heliospheric modulation.
DE: 2104 Cosmic rays
DE: 2124 Heliopause and solar wind termination
DE: 2126 Heliosphere/interstellar medium interactions
DE: 7807 Charged particle motion and acceleration
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Joint Assembly