Numerical simulation of plasma transport driven by the Io torus

Details Numerical simulation of plasma transport driven by the Io torus Numerical simulation of plasma transport driven by the Io torus

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992georl..19..957y&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 19, no. 10, May 22, 1992, p. 957-960.

Physics

Plasma Physics

23

Computerized Simulation, Io, Jupiter (Planet), Planetary Magnetospheres, Plasma Dynamics, Toruses, Magnetohydrodynamic Flow, Magnetohydrodynamic Stability, Mathematical Models, Plasma Physics

Scientific paper

The Rice convection model (RCM) has been modified to a form suitable for Jupiter (RCM-J) to study plasma interchange motion in and near the Io plasma torus. The net result of the interchange is that flux tubes, heavily loaded with torus plasma, are transported outward, to be replaced by tubes containing little low-energy (less than 1 keV) plasma. The process is numerically simulated in terms of time evolution from an initial torus that is longitudinally asymmetric and with gradually decreasing density outward from Io's orbit. In the simulations, the nonlinear stage of the instability characteristically exhibits out-reaching fingers of heavily-loaded flux tubes that lengthen at an accelerating rate. The principal finding is that the primary geometrical form of outward transport of torus plasma in Jupiter's magnetosphere is through long, outward-moving fingers of plasma. In the simulations, the fingers mainly form in the active sector of the Io torus (the heavier side of the asymmetric torus), and they are spaced longitudinally roughly 20 deg apart.

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