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

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.