HR: 1340h
AN: SH23A-1138    [Abstracts]
TI: Perpendicular Transport in the Inner Heliosphere: A Quick and Dirty Approach
AU: * Lampa, F
EM: flampa@uos.de
AF: University of Osnabrueck, Dept. of Physics, Barbarastr. 7, Osnabrueck, 49076, Germany
AU: Kallenrode, M
EM: mkallenr@uos.de
AF: University of Osnabrueck, Dept. of Physics, Barbarastr. 7, Osnabrueck, 49076, Germany
AB: In previous studies, particle transport in the inner heliosphere is regarded as one dimensional along the archimedian spiral; any perpendicular transport is neglected. We extend Roelof's equation of focused transport to accommodate perpendicular transport in the plane of ecliptic. Numerically, this additional term is solved with the implicit Laasonen scheme for azimuthal instead of perpendicular transport - which is identical in the inner heliosphere where the archimedian field is almost radial. For typical ratios λ_\|/λ_\perp perpendicular transport close to the Sun is unreasonably strong. For a ratio scaled with a spiral angle dependent function we find that (a) azimuthal spread over some ten degrees occurs within a few hours, (b) the variation of maximum intensities with longitude is comparable to the ones inferred from multi-spacecraft observations, and (c) on a given field line intensity- and anisotropy-time profiles are modified such that fits with the 2D transport model give different combinations of injection profiles and mean free paths.
DE: 7514 Energetic particles (2114)
DE: 7524 Magnetic fields
DE: 7859 Transport processes
DE: 7863 Turbulence (4490)
DE: 7867 Wave/particle interactions (2483, 6984)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting