  The Jovian magnetosphere is complicated by the multiple plasma sources and
ion species present within it, as well as fast rotation with its dipole axis
titled from its rotational axis. To date global models of Jovian have neglected
the presence of the different ion species as well as the tilted nature of the
dipole axis. This paper reports the results of the first multi-fluid global
modeling of these effects in a single self-consistent study for processes
occurring in the outer magnetosphere. In the inner magnetosphere the model
densities are shown to be comparable to observed densities with much of the
density variables due to the wobble. The wobble enables plasma to be
transported to higher latitudes and then centrifugal acceleration leads to
radial transport of the plasma. At the interface between the middle and outer
magnetosphere, the wobble produces a sinusoidal modulation of the plasma
properties, which yields at a fixed observing point two density peaks, each
with the planetary period. However, because of solar wind forcing and the fast
rotation of Jupiter, torques are exerted on the outer magnetospheric plasma
such that the azimuthal speed between the southern and northern hemispheres are
unequal. This leads to the asymmetric square wave modulation of the plasma
properties in the outer magnetosphere such that only one density peak is seen
each planetary period in the outer magnetosphere. This differential speed leads
to reconnection in the tail at the planetary period and enhanced ejection of
plasma down the tail at the planetary period. These processes could explain the
periodicity seen in the New Horizons' data without the need for invoking
arbitrary solar wind conditions. The energetic particles generated by these
processes are shown to map to the arc-like structures seen in the dusk side
auroral features.
