Radial variations in the Io plasma torus during the Cassini era

Details Radial variations in the Io plasma torus during the Cassini era Radial variations in the Io plasma torus during the Cassini era

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005jgra..11012223d&link_type=abstract

Journal of Geophysical Research, Volume 110, Issue A12, CiteID A12223

Physics

12

Planetary Sciences: Solar System Objects: Io, Planetary Sciences: Comets And Small Bodies: Atmospheres (1060), Planetary Sciences: Comets And Small Bodies: Composition (1060), Planetary Sciences: Comets And Small Bodies: Plasma And Mhd Instabilities (2149, 2752, 7836)

Scientific paper

A radial scan through the midnight sector of the Io plasma torus was made by the Cassini Ultraviolet Imaging Spectrograph on 14 January 2001, shortly after closest approach to Jupiter. From these data, Steffl et al. (2004a) derived electron temperature, plasma composition (ion mixing ratios), and electron column density as a function of radius from L = 6 to 9 as well as the total luminosity. We have advanced our homogeneous model of torus physical chemistry (Delamere and Bagenal, 2003) to include latitudinal and radial variations in a manner similar to the two-dimensional model by Schreier et al. (1998). The model variables include: (1) neutral source rate, (2) radial transport coefficient, (3) the hot electron fraction, (4) hot electron temperature, and (5) the neutral O/S ratio. The radial variation of parameters 1-4 are described by simple power laws, making a total of nine parameters. We have explored the sensitivity of the model results to variations in these parameters and compared the best fit with previous Voyager era models (Schreier et al., 1998), Galileo data (Crary et al., 1998), and Cassini observations (Steffl et al., 2004a). We find that radial variations during the Cassini era are consistent with a neutral source rate of 700-1200 kg/s, an integrated transport time from L = 6 to 9 of 100-200 days, and that the core electron temperature is largely determined by a spatially and temporally varying superthermal electron population.

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