HR: 15:05h
AN: SH53B-06    [Abstracts]
TI: Understanding tansport of electrons in electron/He3 rich events using a direct Monte-Carlo approach
AU: Roth, I
EM: ilan@ssl.berkeley.edu
AF: Space Science Lab, University of California, Berkeley, CA 94720, United States
AU: * Li, G
EM: ganli@ssl.berkeley.edu
AF: Space Science Lab, University of California, Berkeley, CA 94720, United States
AU: * Li, G
EM: ganli@ssl.berkeley.edu
AF: IGPP, University of California, Riverside, CA 92521, United States
AU: Wang, L
EM: windsound@ssl.berkeley.edu
AF: Space Science Lab, University of California, Berkeley, CA 94720, United States
AU: Wang, L
EM: windsound@ssl.berkeley.edu
AF: Department of Physics, University of California, Berkeley, CA 94720, United States
AU: Lin, R
EM: rlin@ssl.berkeley.edu
AF: Space Science Lab, University of California, Berkeley, CA 94720, United States
AU: Lin, R
EM: rlin@ssl.berkeley.edu
AF: Department of Physics, University of California, Berkeley, CA 94720, United States
AB: Impulsive solar energetic particle (SEP) events are characterized by a high e/p ratio and over-abundance of He3. To decipher the underlying acceleration process of these events, it is crucial to deduce precisely the injection time of electrons and ions from the observed time intensity profiles at 1 AU. In a collisionless plasma like the solar wind, the propagation of electrons and ions follows the Parker spiral magnetic field lines, subject to pitch angle scattering due to the presence of solar wind magnetic turbulence. The effect of the pitch angle scattering is to alter particle pitch angles in a random manner during their propagation, leading to a prolonged propagation time and a less-focused pitch angle distribution. In this work, we study the transport of electrons in impulsive SEP events. The pitch angle scattering is investigated using a direct Monte-Carlo technique where the underlying Fokker-Planck transport equation is solved by casting it to a set of equations describing single particle's motion. By following the trajectories of individual particles, the time intensity profiles and pitch angle distributions at 1 AU are obtained. We discuss the comparison of our simulation results to observations by WIND/3DP and its implications on the interplanetary turbulence spectrum.
DE: 7519 Flares
DE: 7859 Transport processes
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting