Physics
Scientific paper
Aug 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992adspr..12...47m&link_type=abstract
(Planetary magnetospheric physics II; Proceedings of Symposium 5 and the Topical Meetings of the Interdisciplinary Scientific Co
Physics
3
Gas Giant Planets, Planetary Magnetic Fields, Planetary Magnetotails, Conservation Laws, Jupiter (Planet), Magnetic Field Configurations, Magnetic Flux, Neptune (Planet), Plasma Density, Saturn (Planet), Solar Planetary Interactions, Uranus (Planet), Voyager 2 Spacecraft
Scientific paper
The distant planetary magnetotails of Jupiter, Saturn, Uranus, and Neptune are assumed to be partially open, hot, long plasma cavities generally in pressure equilibrium with the solar wind. Most of the magnetosheath magnetic field lines drape around the magnetotails. Conservation of momentum density, magnetic field, plasma density, and energy density fluxes are invoked at the tail boundaries to determine the shape of the magnetotails and the variations of plasma and magnetic field characteristics with distance down the magnetotail. Voyager observations are used to initialize calculations in the near-planet portions of each magnetotail. Estimates of magnetotail cross sections, magnetic field strengths, and plasma densities are described as a function of downstream distance. The model accurately predicts properties of the Jovian magnetotail at least as far as Saturn's orbit.
Kurth Willaim S.
Lepping Ronald P.
Macek Wieslaw M.
Sibeck David G.
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