Simulating the Structure of Currents in the Middle Jovian Magnetosphere

Details Simulating the Structure of Currents in the Middle Jovian Magnetosphere Simulating the Structure of Currents in the Middle Jovian Magnetosphere

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsm12a0828l&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SM12A-0828

Physics

2704 Auroral Phenomena (2407), 2708 Current Systems (2409), 2740 Magnetospheric Configuration And Dynamics, 2756 Planetary Magnetospheres (5443, 5737, 6030)

Scientific paper

We have developed a new global magnetohydrodynamic (MHD) simulation of the interaction between the solar wind and the magnetosphere of a rapidly rotating planet and applied it to Jupiter. The main source of plasma in the Jovian magnetosphere is thought to be the Io plasma torus. At Jupiter the Alfven velocity approaches the speed of light at 1RJ. Since the time step necessary to advance the MHD equations goes as the inverse of the Alfven velocity in explicit simulations, it is impractical to include the Io torus in the simulation domain. Therefore in previous simulations the Io torus source has been modeled by setting the inner boundary condition [c.f. Walker et al., Planet Space Sci., 49, 237, 2001]. In this calculation we have used a semi-implicit approach in which we add inertia to the highest frequency modes. With this approach the time step is proportional to the inverse of the convection velocity. Therefore we can include the torus source self-consistently. We are using the simulation to study the configuration of the middle (r<60RJ) Jovian magnetosphere with emphasis on the field aligned currents that couple the magnetosphere to the ionosphere. We will compare the configuration from the new model with that from the existing code.

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