HR: 09:44h
AN: SM41B-08    [Abstracts]
TI: Energy Budget in Global Magnetosphere-Ionosphere simulations.
AU: * Rastaetter, L
EM: lr@waipio.gsfc.nasa.gov
AF: Community-Coordinated Modeling Center, Code 696, NASA GSFC, Greenbelt, MD 20771 United States
AU: Kuznetsova, M
EM: Maria.M.Kuznetsova@nasa.gov
AF: Community-Coordinated Modeling Center, Code 696, NASA GSFC, Greenbelt, MD 20771 United States
AU: Hesse, M
EM: Michael.Hesse@nasa.gov
AF: Community-Coordinated Modeling Center, Code 696, NASA GSFC, Greenbelt, MD 20771 United States
AU: Gombosi, T I
EM: tamas@umich.edu
AF: CSEM, College of Engineering, University of Michigan, Ann Arbor, MI 48109 United States
AU: Raeder, J
EM: j.raeder@unh.edu
AF: Space Sciene Center, University of New hampshire, Durham, NH 03824 United States
AB: After determining the boundary of the magnetosphere and magnetosheath through plasma flow line tracing that separates the magnetosheath from the magnetosphere and magnetotail, we can determine surface integrals of various energy fluxes and calculate energy content in the volume inside the surface. To assess the flow of energy from the solar wind into the magnetosphere, however, the time-dependent shape has to be taken into account in addition to integrals over the magnetosphere surface at a given time. In this work we estimates changes of total magnetospheric energy content from energy flow on the surface and from volume changes and compare these to volume integrals of the internal energy. Simulations of storm events used in this study were performed at CCMC using the BATSRUS (T. Gombosi) and UCLA-GGCM (J. Raeder) models. In order to obtain definitions of magnetosphere regions independently for the flow surface we use thresholds of physical variables such as the magnetic field strength, plasma density and temperature to distinguish magnetotail lobes, plasma sheet, and inner magnetosphere and to calculate contributions to the total energy conent in these regions. Our simulations complement results obtained with the LFM model (Guild et al., 2004, EOS Trans. AGU {\bf 85}(17), Joint. Assem. Suppl., Abstract SM33A-19) and GUMICS-4 model (Palmroth et al., 2003, JGR {\bf 108}, 1048). These simulations are part of the MHD code validation and verification efforts that are performed at the CCMC.
DE: 2740 Magnetospheric configuration and dynamics
DE: 2744 Magnetotail
DE: 2753 Numerical modeling
DE: 2764 Plasma sheet
DE: 2784 Solar wind/magnetosphere interactions
SC: SPA-Magnetospheric Physics [SM]
MN: 2004 AGU Fall Meeting