Physics
Scientific paper
Aug 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990p%26ss...38..995l&link_type=abstract
Planetary and Space Science (ISSN 0032-0633), vol. 38, Aug. 1990, p. 995-1009. Research supported by NSERC.
Physics
2
Centrifugal Force, Io, Planetary Ionospheres, Planetary Rotation, Plasma Currents, Plasma Turbulence, Density Distribution, Ionospheric Propagation, Jupiter (Planet)
Scientific paper
A quantitative model of plasma diffusion from the Io torus, driven by the centrifugal force of Jupiter's rotation, is developed. It is argued that the unstable mode of perturbation, which would lead to a system of deterministic motion of plasma, should be dominated by a more turbulent mode of motion in order to effect a longer trapping time of the Iogenic plasma as implied by the observations. The energy of the turbulent motion is derived internally from the centrifugal potential of the planetary rotation. The length scale of the turbulence cells is determined by the interaction between the magnetospheric plasma and the dissipative ionosphere, and found to be of order 0.1 Rj for the Jovian magnetosphere. Since the cells are smaller than the dimension of the system, the transport of the plasma can be studied as a problem of eddy diffusion, governed by the Fokker-Planck equation. A specific model is established based on the above considerations.
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