Implications of Multipoint Solar Wind Observations for MHD Predictions of Magnetospheric Dynamics

Details Implications of Multipoint Solar Wind Observations for MHD Predictions of Magnetospheric Dynamics Implications of Multipoint Solar Wind Observations for MHD Predictions of Magnetospheric Dynamics

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsm22a0218a&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SM22A-0218

Physics

2111 Ejecta, Driver Gases, And Magnetic Clouds, 2134 Interplanetary Magnetic Fields, 2427 Ionosphere/Atmosphere Interactions (0335), 2736 Magnetosphere/Ionosphere Interactions, 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

Traditionally event oriented MHD modeling is based on observations from a single upstream monitor (e.g., Wind, ACE) extrapolated as a boundary condition over the entire upstream edge of the simulation domain. Occasionally more than one spacecraft is observing the solar wind in the upstream region during a disturbed interval. In those cases data from the different satellites can be used to evaluate spatial structures in the solar wind and the sensitivity of the MHD simulations to uncertainties in the solar wind parameters can be determined. An event that meets this criteria occurred during a magnetic storm on May 24, 2000 when solar wind observations from four spacecraft (Wind, ACE, IMP-8 and Geotail) were available. After taking into account the different spatial locations of the satellites and shifting the observations by the solar wind velocity, it was found that the time series of the observed magnetic field and plasma bulk parameters did not coincide. An analysis was carried out by calculating cross correlation coefficients between parameters taken at each pair of spacecraft. Then the solar wind parameters from each of these spacecraft were used to drive global MHD simulations of the magnetosphere. The power deposited in the ionosphere for each simulation was calculated and compared with that observed by the VIS instrument on Polar. Cross correlation coefficients of the ionospheric power and the cross polar cap potential difference from the simulation output from each pair of solar wind inputs were calculated. Finally the simulation output cross correlations with the input cross correlations were compared. Implications for the use of such an analysis to determine the reliability of forecasts of magnetospheric activity based on observations at a few points in the solar wind will be discussed.

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