A global model of the Jovian magnetosphere is presented based on magnetohydrodynamic (MHD) simulation that takes into account the interaction between a rapidly rotating magnetosphere and external plasma flow. In this study, a steady solar wind with, as well as without, the interplanetary magnetic field (IMF) is applied to the inflow boundary. The results clearly indicate that the global structure of the magnetic field lines of force is strongly affected by the rotation of Jupiter as well as by the solar wind. It is also found that magnetic reconnection at the tail region generates the plasma outflow and greatly modifies the corotational structure of the plasmas in the magnetosphere. Especially, when a relatively high-speed solar wind or a solar wind with a northward IMF collides with the magnetosphere, strong magnetic reconnection at the tail induces the tail-dusk flow, which is against the corotation. On the other hand, the evident tail-dusk flow does not appear in the case of a low-speed solar wind or in the case with a southward IMF. Thus the internal structure of the rotating magnetosphere could be altered qualitatively in response to changes in the solar wind parameters. ¿ 2001 American Geophysical Union