Dst index in the 2008 GEM Modeling Challenge - Model performance for Moderate and Strong Magnetic Storms

Details Dst index in the 2008 GEM Modeling Challenge - Model performance for Moderate and Strong Magnetic Storms Dst index in the 2008 GEM Modeling Challenge - Model performance for Moderate and Strong Magnetic Storms

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm51a1744r&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM51A-1744

Physics

Plasma Physics

[7833] Space Plasma Physics / Mathematical And Numerical Techniques, [7924] Space Weather / Forecasting, [7954] Space Weather / Magnetic Storms, [7959] Space Weather / Models

Scientific paper

The GEM 2008 modeling challenge efforts are expanding beyond comparing in-situ measurements in the magnetosphere and ionosphere to include the computation of indices to be compared. The Dst index measures the largest deviations of the horizontal magnetic field at 4 equatorial magnetometers from the quiet-time background field and is commonly used to track the strength of the magnetic disturbance of the magnetosphere during storms. Models can calculate a proxy Dst index in various ways, including using the Dessler-Parker Sckopke relation and the energy of the ring current and Biot-Savart integration of electric currents in the magnetosphere. The GEM modeling challenge investigates 4 space weather events and we compare models available at CCMC against each other and the observed values of Dst. Models used include SWMF/BATSRUS, OpenGGCM, LFM, GUMICS (3D magnetosphere MHD models), Fok-RC, CRCM, RAM-SCB (kinetic drift models of the ring current), WINDMI (magnetosphere-ionosphere electric circuit model), and predictions based on an impulse response function (IRF) model and analytic coupling functions with inputs of solar wind data. In addition to the analysis of model-observation comparisons we look at the way Dst is computed in global magnetosphere models. The default value of Dst computed by the SWMF model is for Bz the Earth's center. In addition to this, we present results obtained at different locations on the Earth's surface. We choose equatorial locations at local noon, dusk (18:00 hours), midnight and dawn (6:00 hours). The different virtual observatory locations reveal the variation around the earth-centered Dst value resulting from the distribution of electric currents in the magnetosphere during different phases of a storm.

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