HR: 10:50h
AN: SA42A-03    [Abstracts]
TI: Global Energy Partition During Superstorms
AU: * Lu, G
EM: ganglu@ucar.edu
AF: High Altitude Observatory,National Center for Atmospheric Research, 3450 Mitchell Lane, Boulder, CO 80307-3000 United States
AU: Richmond, A D
EM: richmond@ucar.edu
AF: High Altitude Observatory,National Center for Atmospheric Research, 3450 Mitchell Lane, Boulder, CO 80307-3000 United States
AU: Evans, D S
EM: David.S.Evans@noaa.gov
AF: SEC/NOAA, 325 Broadway, Boulder, CO 80305 United States
AU: Kozyra, J U
EM: jukozyra@engin.umich.edu
AF: University of Michigan, 2455 Hayward, Ann Arbor, MI 48109-3000 United States
AU: Woods, T N
EM: tom.woods@lasp.colorado.edu
AF: LASP, University of Colorado, 1234 Innovation Dr., Boulder, CO 80303 United States
AU: Solomon, S C
EM: stans@ucar.edu
AF: High Altitude Observatory,National Center for Atmospheric Research, 3450 Mitchell Lane, Boulder, CO 80307-3000 United States
AU: Skoug, R
EM: rskoug@lanl.gov
AF: Space and Atmospheric Sciences, Los Alamos National Laboratory, Mail Stop D466, Los Alamos, NM 87545 United States
AB: The geomagnetic storms of October and November 2003 as well as July 2000 were among the most significant of the past decade. The solar disturbances associated with these superstorms included strong solar flares, solar energetic particles, and coronal mass ejections. All three storms reached minimum Dst values less than -400 nT and maximum AE values greater than 3000 nT. The purpose of this presentation is to provide a quantitative examination of global energy deposition during these three superstorms in terms of ionospheric Joule heating, auroral particle precipitation, and magnetospheric ring current injection. We will compare the magnetospheric and ionospheric energy deposition with the available solar wind energy inputs to shed new light on the relative geoeffectiveness of magnetic clouds versus fast solar wind streams during superstorms. Finally, we compare the various solar energetic outputs arriving at the Earth's geospace environment in the forms of solar radiation, solar energetic particles, and solar wind kinetic and magnetic energies, and we discuss their respective impacts on the upper atmosphere.
DE: 2118 Energetic particles, solar
DE: 2431 Ionosphere/magnetosphere interactions (2736)
DE: 2736 Magnetosphere/ionosphere interactions
DE: 2784 Solar wind/magnetosphere interactions
DE: 2788 Storms and substorms
SC: SPA-Aeronomy [SA]
MN: 2004 AGU Fall Meeting