Physics
Scientific paper
Sep 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987jgr....92.9963w&link_type=abstract
Journal of Geophysical Research (ISSN 0148-0227), vol. 92, Sept. 1, 1987, p. 9963-9970.
Physics
21
Io, Jupiter Atmosphere, Magnetohydrodynamic Waves, Planetary Magnetic Fields, Planetary Magnetospheres, Wave Interaction, Nonuniform Plasmas, Toruses, Wave Propagation, Jupiter, Satellites, Io, Interactions, Alfven Waves, Magnetosphere, Numerical Methods, Magnetic Fields, Torus, Reflection, Power, Ionosphere, Resonance, Hypotheses, Structure, Features, Plasma, Propogation, Scale, Calculations, Diagrams, Density
Scientific paper
A numerical solution for the propagation of the Alfven waves produced by Io is presented. The waves are shown to interact strongly with the torus and magnetic-field inhomogeneities. Substantial reflection occurs from the magnetospheric medium, and only about a quarter of the wave power will reach the ionosphere on its first pass. It is concluded that both WKB and ray-tracing arguments are inappropriate, contrary to previous studies. A more realistic picture may be that of a whole field line or L shell resonating in an eigenmode. The Alfven structure behind Io and some possible features that it may exhibit are discussed. In particular, it may be possible to produce decametric arcs that are more closely spaced than ray tracing permits by exciting higher-harmonic eigenmodes of Io's L shell.
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