Energy Budget in Global Magnetosphere-Ionosphere simulations.

Details Energy Budget in Global Magnetosphere-Ionosphere simulations. Energy Budget in Global Magnetosphere-Ionosphere simulations.

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsm41b..08r&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SM41B-08

Physics

2740 Magnetospheric Configuration And Dynamics, 2744 Magnetotail, 2753 Numerical Modeling, 2764 Plasma Sheet, 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

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 85(17), Joint. Assem. Suppl., Abstract SM33A-19) and GUMICS-4 model (Palmroth et al., 2003, JGR 108, 1048). These simulations are part of the MHD code validation and verification efforts that are performed at the CCMC.

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