Simulating the viscous interaction under a variety of solar wind conditions, with some comparisons to satellite data

Details Simulating the viscous interaction under a variety of solar wind conditions, with some comparisons to satellite data Simulating the viscous interaction under a variety of solar wind conditions, with some comparisons to satellite data

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm13a1591b&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SM13A-1591

Physics

[2724] Magnetospheric Physics / Magnetopause And Boundary Layers, [2736] Magnetospheric Physics / Magnetosphere/Ionosphere Interactions, [2753] Magnetospheric Physics / Numerical Modeling, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions

Scientific paper

The viscous interaction is a mode of energy transport between the solar wind and Earth's magnetosphere. Its effects are often difficult to isolate from other effects in in-situ measurements. Therefore, it can be useful to simulate the viscous interaction under a variety of solar wind conditions, which are often impossible to find in satellite data. We have used the Lyon-Fedder-Mobarry simulation to look at the viscous potential in Earth's ionosphere for a variety of solar wind velocities, densities, and magnetic field strengths and clock angles. Where possible, we have compared those results to low and high altitude satellite measurements. We will also present the results of our search for direct indications of viscous cells in the low latitude boundary layer in the magnetotail, and their signature in ionospheric plasma circulation.

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