EFFECTS ON THE JOVIAN MAGNETOSHEATH ARISING FROM SOLAR-WIND FLOW AROUND NONAXISYMMETRIC BODIES

We investigate the MHD structure of the Jovian magnetosheath along the Sun-Jupiter line and, particularly, the region where the interplaneta ry magnetic field (IMF) exerts a large influence on the magnetosheath flow (the ''magnetic barrier''). We do this by integrating numerically the dissipationless MHD equations in their ''magnetic string'' formul ation. The lack of axisymmetry of the magnetospheric obstacle introduc es corresponding asymmetries in the Jovian magnetosheath. The dominant effect on the flow is produced by the IMF component orthogonal to Jul ,iter's rotational equator. The thicknesses of the magnetosheath and m agnetic barrier depend sensitively on the orientation of the IMF, decr easing monotonically as the inclination of the IMF to the rotational e quator decreases. The magnetic barrier practically disappears when the IMF vector lies in the equator. For an arbitrary orientation of the I MF the magnetosheath magnetic field along the stagnation streamline is not only compressed as the magnetopause is approached but also rotate s smoothly toward the direction of the Jovian rotation axis. This effe ct is absent in the case of flow around axisymmetric obstacles, such a s the terrestrial magnetosphere.