HR: 11:20h
AN: SM22B-05 INVITED     [Abstracts]
TI: Global evolution of the high energy magnetospheric electron population during substorms.
AU: * Donovan, E F
EM: eric@phys.ucalgary.ca
AF: Dept. of Physics and Astronomy University of Calgary, 2500 University Drive, Calgary, AB T2N 1N4 Canada
AU: Spanswick, E L
EM: emma@phys.ucalgary.ca
AF: Dept. of Physics and Astronomy University of Calgary, 2500 University Drive, Calgary, AB T2N 1N4 Canada
AU: Voronkov, I O
EM: igor@phys.ucalgary.ca
AF: Dept. of Physics and Astronomy University of Calgary, 2500 University Drive, Calgary, AB T2N 1N4 Canada
AU: Friedel, R H
EM: friedel@lanl.gov
AF: LANL Space & Remote Sensing Sci, ISR-2 MS-D436, Los Alamos, NM 87545 United States
AU: Aksnes, A
EM: arve.aksnes@ift.uib.no
AF: Dept. if Physics and Technology University of Bergen, Allegaten 55, Bergen, N-5007 Norway
AU: Henderson, M G
EM: mghenderson@lanl.gov
AF: LANL Space & Remote Sensing Sci, ISR-2 MS-D436, Los Alamos, NM 87545 United States
AB: The substorm phenomenology of the magnetospheric high energy electron population has been thoroughly studied with geosynchronous particle observations. We have a much less developed understanding of the radial extent and evolution of, for example, substorm injections. Riometer absorption has been shown to be a good proxy for the integrated high energy electron flux near the equatorial plane, provided specific conditions are met [Baker et al., JGR, 86, 2295, 1981]. In recent work, we are attempting to map out, in advance of NASA's upcoming Time History of Events and Mesoscale Interactions During Substorms (THEMIS) project, the capabilities and limitations of the three techniques we now have (ie., X-ray imaging, riometers, and in situ particle observations) to characterize the mesoscale response of the high energy electron population to this most dynamic phase of the substorm. In this paper, we use data from a latitudinally distributed array of riometers in conjunction with in situ particle data and global X-ray images to explore the L-value dependence of the evolution of the high energy electron population during the substorm expansive phase.
DE: 2704 Auroral phenomena (2407)
DE: 2716 Energetic particles, precipitating
DE: 2730 Magnetosphere--inner
DE: 2740 Magnetospheric configuration and dynamics
SC: SPA-Magnetospheric Physics [SM]
MN: 2004 AGU Fall Meeting