Physics
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsm51d..02a&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #SM51D-02
Physics
2740 Magnetospheric Configuration And Dynamics, 2744 Magnetotail, 2764 Plasma Sheet, 2784 Solar Wind/Magnetosphere Interactions, 2788 Storms And Substorms
Scientific paper
In recent years, global magnetohydrodynamic (MHD) simulations have been driven by input from solar wind monitoring spacecraft and have produced results that are in good agreement with observations within the magnetosphere. Discrepancies between MHD results and satellite observations in the magnetosphere are a result of MHD limitations and the uncertainty in the three-dimensional structure of the solar wind. For example, the manner in which the solar wind propagates from the monitor spacecraft (often at the L1 point, ~ 200 RE upstream of Earth) to Earth and whether large- and small-scale features seen at the spacecraft actually impact the magnetosphere are significant. This study uses global MHD simulations to examine case studies of magnetic storms where there was more than one spacecraft monitoring the solar wind to delineate the effect of observed meso- and macro-scale structures on the dynamics of the magnetosphere. To do so, we run the MHD simulation for each set of available solar wind parameters and compare the results of these runs in the magnetosphere. The effect on the magnetosheath and on the location of dayside reconnection is examined in detail.
Ashour-Abdalla Maha
Coroniti Ferdinan V.
El-Alaoui Mostafa
Peroomian Vahé
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