Abstract
The solar wind-magnetosphere-ionosphere interaction at Jupiter is reproduced numerically adopting the nine-component magnetohydrodynamic simulation. Calculations take into account the magnetosphere-ionosphere coupling, Jovian rotation, and Io plasma source. High-speed rotating plasma inside restricted magnetospheric space causes expansion and contraction of magnetic field, forming super-rotation at radial distance 20∼30 Rj and co-rotation breakdown further outside. Field-perpendicular current that restores co-rotational delay beyond 30 Rj is connected via field-aligned current to the main oval in the ionosphere. Inside 20 Rj, there is almost co-rotation region (deviation from co-rotation less than 20 km/s). Particularly within 10 Rj, the deviation from co-rotation is less than 2 km/s. In the nearly co-rotating region, the Io plasma forms a disk structure through field-aligned redistribution. The interchange instability occurs near the outer wall of the Io plasma disk, and instability flow develops to vortex. Through this instability, a part of the centrifugal drift current supporting the Io plasma disk is connected to low-latitude field-aligned current that generates beads-like spots on the lower latitude side of the main oval. Resulting interchange instability comes to satisfy the structure of convection and enables further development of vortex. The Coriolis force acting on eastward flow inside the developing vortex makes this flow protrude further outward, forming eastward bending fingers. Inside 10 Rj, Io plasma transport by the interchange instability becomes slower, despite the center of the disk. Io plasma escapes from the inner magnetosphere with a time constant of 20 days if this slow transport is taken into account.
