Investigation of the viscous potential using an MHD simulation

The viscous contribution to the polar cap potential, the viscous potential, is typically swamped by the much larger reconnection potential or obscured by rapidly changing solar wind conditions. We used the Lyon-Fedder-Mobarry (LFM) magnetohydrodynamic simulation to study the response of the viscous potential to a variety of ideal conditions both in the solar wind and the ionosphere.

We found that the viscous potential in LFM increases with either increasing solar wind density or velocity, with a relation that is similar to some previous empirical results in form but different in detail. The density dependence scales as n⁰.⁴³⁹ (in cm⁻³) and velocity scales as Vx¹.³³ (in km s⁻¹). Combining these results with a reference value, the viscous potential in LFM can be predicted using the formula ΦV = (0.00431)n⁰.⁴³⁹Vx¹.³³ kV.