IMF control and convection in the Jovian magnetosphere.

Abstract

The dependence of the Jovian non-Io-related decametric emission on solar wind parameters demonstrates that the energy of the solar wind is imparted to the Jovian magnetosphere. This paper considers if, and then how, the steady-state reconnection model can be used for the understanding of this energy transfer process. Referring to the observationally obtained values of key parameters as much as possible, we investigate if the steady state model as commonly applied for the earth's magnetosphere can be adopted as a reasonable approximation for the Jovian magnetosphere as well. We find that rapid rotation of the planet does not present a serious obstacle to a steady progress of reconnection since the motion of the field lines is governed by the magnetosheath plasma and the slipping occurs at the ionospheric ends. Next we discuss the convection generated by reconnection for northward and southward polarities of the interplanetary magnetic field, and address the field line motion in the tail and the current system generated in the ionosphere. Influence of the centrifugal force on the motion of field lines in the inner region of the magnetosphere is also discussed.