Structure of the Jovian magnetosphere as Determined by 3-D Multi-Fluid Simulations

Details Structure of the Jovian magnetosphere as Determined by 3-D Multi-Fluid Simulations Structure of the Jovian magnetosphere as Determined by 3-D Multi-Fluid Simulations

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsm22b0241r&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SM22B-0241

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2459 Planetary Ionospheres (5435, 5729, 6026, 6027, 6028), 2756 Planetary Magnetospheres (5443, 5737, 6030), 6218 Jovian Satellites

Scientific paper

The Jovian magnetosphere is highly structured due to the presence of different sources of plasma within it. These sources include light ions from the Jovian ionosphere, sulfur and oxygen ions from Io and the Io plasma torus and hydrogen and oxygen sputtered from the other Galilean moons. These different sources are modeled by high-resolution 3-d multi-fluid simulations that are able to determine the individual contributions from the different ion species. The simulations have an inner radius 2 RJ and extended out to several hundred RJ down the tail. We show that the size of the Jovian magnetosphere is dependent on the magnitude of the Jovian ionospheric outflow rate, and this outflow produces mass loading of the magnetosphere out to large distances. The Io torus is shown to be very stable and that other means of perturbing it such as from Io itself is needed to enhance its possible outward. At radial distances near the outer Galilean moons, the story is very much different as the magnetosphere undergoes a transition from a corotational regime to a non-corotational region. In this case, convection of plasma allows it to move further out into the magnetosphere to cause additional dragging of field lines. This transition in the convection pattern of plasma is seen in association with the strong warping of the magnetic field at the outer Galilean moons.

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