The Effects of Solar Wind Structure on Magnetosphere Parameters

Details The Effects of Solar Wind Structure on Magnetosphere Parameters The Effects of Solar Wind Structure on Magnetosphere Parameters

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsm11b0437z&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SM11B-0437

Mathematics

Logic

2740 Magnetospheric Configuration And Dynamics, 2744 Magnetotail, 2764 Plasma Sheet, 2784 Solar Wind/Magnetosphere Interactions, 2788 Storms And Substorms

Scientific paper

During the ISTP program we demonstrated that in order to understand the magnetospheric response to solar wind and interplanetary magnetic field changes we had to simulate the magnetosphere using actual spacecraft observations as input to our global MHD models [Frank et al., 1995]. In these studies, we assumed that plasmas and fields observed by the spacecraft monitoring the solar wind were homogeneous and that all of the variations seen at the monitor reached the Earth. Although this approach allowed us to obtain qualitative agreement between the simulations and observations made within the magnetosphere, it has often limited our ability to quantitatively assess the validity of the model. In this study we have tested the assumptions made on the solar wind properties and propagation by modeling a magnetic storm on May 24, 2000 using data from five solar wind monitors (ACE, Wind, Imp-8, Geotail and Interball-1). We compare quantitatively the results of the five simulations assuming that each spacecraft was the only solar wind monitor and discuss the topological changes in the magnetospheric configuration caused by the different solar wind inputs. We use these results to assess quantitatively the errors encountered using a single spacecraft and homogeneous solar wind.

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