Properties of the Io plasma torus inferred from Voyager EUV data

Details Properties of the Io plasma torus inferred from Voyager EUV data Properties of the Io plasma torus inferred from Voyager EUV data

May 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...238l..49s&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 238, May 15, 1980, p. L49-L52. NASA-Navy-supported research.

Astronomy and Astrophysics

Astrophysics

22

Far Ultraviolet Radiation, Io, Jupiter Atmosphere, Plasma Radiation, Toroidal Plasmas, Voyager Project, Electron Impact, Electron Transitions, Jupiter (Planet), Planetary Radiation, Resonance Scattering, Ultraviolet Absorption, Ultraviolet Spectroscopy, Jupiter, Satellites, Io, Properties, Plasmas, Toruses, Voyager Mission, Ultraviolet, Models, Spectrum, Emissions, Spectrometry, Electrons, Gases, Distribution, Temperatures, Density, Radius, Resonance, Ions, Absorption, Scattering, Brightness, Sulfur, Oxygen

Scientific paper

A physical model for the Io plasma torus is constructed to explain the EUV radiative emission observed by the Voyager UV spectrometer. Electron impact excitation rate coefficients for electronic transitions of S III, S IV, O II and O III are calculated by the method of distorted waves (Davis, Kepple, and Blaha, 1976); these coefficients account for the asymmetric shape of the 686 A feature. It is concluded that the electron gas must have a distribution function with a non-Maxwellian tail. An approximate representation of the distribution function as two temperature components requires a cold component of 3.5-4 eV and density of 2000 per cu cm and a hot component of about 100 eV and density of 50-100 per cu cm to satisfy observational constraints.

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