HR: 1400h
AN: SM53A-04    [Abstracts]
TI: Energy Transport, Storage, and Dissipation in the Magnetosphere During Substorms.
AU: * Halford, A J
EM: alexa.halford@gmail.com
AF: CU Boulder/LASP, 1234 innovation Drive, Boulder, CO 80303, United States
AU: Baker, D
EM: Daniel.Baker@lasp.colorado.edu
AF: CU Boulder/LASP, 1234 innovation Drive, Boulder, CO 80303, United States
AU: Weygand, J
EM: jweygand@igpp.ucla.edu
AF: IGPP Department of Earth and Space Sciences University of California, Los Angeles, PO Box 951567 3845 Slichter Hall, Los Angeles, CA 90095-1567, United States
AB: Magnetospheric substorms represent a global interaction between the solar wind, magnetosphere, and ionosphere. Energy transported from the solar wind into the magnetosphere is largely stored in the tail until it is released (primarily into the ionosphere and the ring current). The Akasofu epsilon parameter (ε=4π L / μ v B² sin ⁴ θ / 2), and multiple empirically determined formulas for energy dissipation into the ionosphere (joule heating and particle precipitation) and the ring current have been considered for such global interactions. An energy budget and estimation of total energy in the tail has been created for 12 isolated substorms that occurred during 2001. Considerable complexity and individuality of substorms is observed with substantial differences in the input and dissipation pattern for individual events. Our analysis is compared with previous published results.
DE: 2784 Solar wind/magnetosphere interactions
DE: 2788 Magnetic storms and substorms (7954)
DE: 2790 Substorms
SC: SPA-Magnetospheric Physics [SM]
MN: 2007 Joint Assembly