HR: 0800h
AN: SM21A-0315    [Abstracts]
TI: ICME and CIR Geomagnetic Storms as Seen by ENA Images and Ring Current Distributions
AU: * Grimes, E
EM: eric@auburn.edu
AF: Auburn University, Physics Department 206 Allison Lab, Auburn, AL 36849, United States
AU: Perez, J D
EM: perez@physics.auburn.edu
AF: Auburn University, Physics Department 206 Allison Lab, Auburn, AL 36849, United States
AU: Miller, M K
EM: millemk@auburn.edu
AF: Auburn University, Physics Department 206 Allison Lab, Auburn, AL 36849, United States
AU: Brandt, P C
EM: brandpc1@jhuapl.edu
AF: The Johns Hopkins University, Applied Physics Laboratory, Laurel, MD 20723, United States
AU: Jahn, J
EM: jjahn@swri.edu
AF: Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238, United States
AB: Geomagnetic storms in the Earth's magnetosphere have been classified as due to solar wind dominated by interplanetary coronal mass ejections (ICMEs) or by corotating interaction regions (CIRs). The different characteristics of these storms have been determined primarily from measurements at geosynchronous orbit and ground magnetometers. Borovsky and Denton [2006] have identified 21 differences between ICME and CIR driven storms. We present ENA images and deconvolved proton distributions from MENA and HENA onboard the IMAGE satellite for storms during 2004. The density, temperature, and pressure of the trapped ring current protons with energies from a few keV to more than 30 keV for the inner magnetosphere are presented during various phases of the two kinds of storms. Differences between ICME and CIR driven storms are affirmed and/or modified based upon these observations.
DE: 2730 Magnetosphere: inner
DE: 2778 Ring current
DE: 2784 Solar wind/magnetosphere interactions
DE: 7954 Magnetic storms (2788)
SC: SPA-Magnetospheric Physics [SM]
MN: 2007 Fall Meeting