Simulation Studies of the Effect of Solar Wind Velocity Fluctuations on the Viscous Potential
Abstract
Observations of the value of the transpolar potential as a function of the interplanetary magnetic field (IMF) show a nonzero intercept. This residual potential in the absence of merging with the IMF is attributed to a mechanical interaction with the solar wind. Global MHD simulations also develop a residual value of the transpolar potential and exhibit magnetospheric convection when the IMF is zero. This residual value is known as the viscous potential, and it is dependent on solar wind speed and density. In this study, we examine the effect of solar wind velocity fluctuations along the Y and Z axes on the viscous potential. Velocity fluctuations in the Z-direction appear to have significant effects on the viscous potential, whereas velocity in the Y-direction appear to have little or no effect. We will discuss the variation in any effect on the viscous potential as a function of the period and amplitude of the solar wind velocity fluctuations.
- Publication:
-
AGU Fall Meeting Abstracts
- Pub Date:
- December 2016
- Bibcode:
- 2016AGUFMSM13A2176B
- Keywords:
-
- 2724 Magnetopause and boundary layers;
- MAGNETOSPHERIC PHYSICSDE: 2728 Magnetosheath;
- MAGNETOSPHERIC PHYSICSDE: 2772 Plasma waves and instabilities;
- MAGNETOSPHERIC PHYSICSDE: 2784 Solar wind/magnetosphere interactions;
- MAGNETOSPHERIC PHYSICS