HR: 11:26h
AN: SM32A-04    [Abstracts]
TI: High Resolution Substorm Energetic Electrons seen in the Magnetotail by all 4 CLUSTER satellites
AU: * wu, p
EM: pwu@bu.edu
AF: Boston University, 725 Commonwealth Ave, Center for Space Physics, boston, ma 02215
AU: Fritz, T A
EM: fritz@bu.edu
AF: Boston University, 725 Commonwealth Ave, Center for Space Physics, boston, ma 02215
AU: Reed, R S
EM: beckee@bu.edu
AF: Boston University, 725 Commonwealth Ave, Center for Space Physics, boston, ma 02215
AU: Friedel, R
EM: friedel@lanl.gov
AF: LANL, IST-1, Mail Stop D-466, LANL, Los Alamos, NM 87545
AU: Reeves, G
EM: reeves@lanl.gov
AF: LANL, IST-1, Mail Stop D-466, LANL, Los Alamos, NM 87545
AU: Baker, D
EM: daniel.baker@lasp.colorado.edu
AF: LASP, University of Colorado, University of Colorado, Boulder, CO 80303
AU: Daly, P
EM: daly@mps.mpg.de
AF: MPS, Max-Planck-Str 2, Katlenburg-Lindau, 37191 Germany
AB: We report our examination of the 3-D pitch angle distributions (PAD) of energetic electrons as the Cluster satellites cross the earth's plasma sheet near their apogee in the nightside magnetosphere during the tail season (July, August, September, October) of year 2005. We identified several energetic electron injections in the tail plasma sheet associated with substorm events. Those events are all associated with continual switching of PADs from field aligned to the peak at 90 degree, which indicated to us that those energetic electrons are accelerated in different manners and they form different populations. The study of the evolution of the PAD gave us an impression that the Fermi and betatron accelerations play different roles along the tail. They compete with each other, depend on the radial distance. However, this idea needs to be further verified with the study of more events. The large separations of the 4 Cluster satellites in this tail season of 2005 provide a good opportunity for us to identify more energetic electron bursts events with better spatial and temporal clarity. Comparing the observation from these 4 different satellites will allow us to visualize the picture in many more dimensions and avoid vagueness as much as we can. Together with our collaboration with LANL and LASP, including more satellite data (e.g. Geosynchronous satellites, POLAR, IMAGE), we will report on a more integrated picture of the magnetotail energetic electron dynamics.
DE: 2740 Magnetospheric configuration and dynamics
DE: 2744 Magnetotail
DE: 2764 Plasma sheet
DE: 2772 Plasma waves and instabilities (2471)
DE: 2790 Substorms
SC: SPA-Magnetospheric Physics [SM]
MN: Fall Meeting 2005