HR: 17:00h
AN: SH44C-05    [Abstracts]
TI: Simulations of Diffusion in Solar Energetic Particle Events
AU: * Pei, C
EM: pei@lpl.arizona.edu
AF: Lunar and Planetary Laboratory, The University of Arizona 1629 E University BLVD, Tucson, AZ 85721, United States
AU: Jokipii, J
EM: jokipii@lpl.arizona.edu
AF: Lunar and Planetary Laboratory, The University of Arizona 1629 E University BLVD, Tucson, AZ 85721, United States
AU: Giacalone, J
EM: giacalon@lpl.arizona.edu
AF: Lunar and Planetary Laboratory, The University of Arizona 1629 E University BLVD, Tucson, AZ 85721, United States
AB: New observations by high-sensitivity instruments onboard the ACE spacecraft show that Fe and O may share similar injection profiles close the solar surface, and that diffusion dominates the transport of these particles (Mason et al 2006). Multi-spacecraft observations by Helios and IMP-8 also confirm the spatial diffusion is important (Wibberenz & Cane 2006). The "reservoir" phenomenon or "spatial invariance" states that during the decay phase of individual gradual solar energetic particle events, the intensities measured by different spacecraft are nearly equal, even if these spacecraft are separated by several AU in radius and by 70 degrees in latitude. Results from our multidimensional numerical model, based on Parker's transport equation, with reasonable values of κ_\perp and κ_\| are compared with observations from Ulysses, IMP-8, and ACE. We demonstrate that most of the features of the "reservoir" phenomenon can be reproduced by a transport model which includes drift, energy loss, and spatial diffusion.
DE: 7513 Coronal mass ejections (2101)
DE: 7514 Energetic particles (2114)
DE: 7519 Flares
DE: 7859 Transport processes
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting