Revised O+ mixing ratio in the Io torus during the Voyager era.

Details Revised O+ mixing ratio in the Io torus during the Voyager era. Revised O+ mixing ratio in the Io torus during the Voyager era.

Jul 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997dps....29.1812t&link_type=abstract

American Astronomical Society, DPS meeting #29, #18.12; Bulletin of the American Astronomical Society, Vol. 29, p.1004

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Scientific paper

The canonical value of the O+ mixing ratio ([O+]/[e-]) in the Io plasma torus during the Voyager encounter is 0.4 based primarily on UVS measurements of the 833 Angstroms emission line (Shemansky, J. Geophys. Res., 92, 6141, 1987). This ratio is important in modeling the relative neutral source rates of oxygen and sulfur to the torus; and hence, the loss rates and abundances at Io. By assuming the in-situ measurement of electron temperature of 5 eV (Sittler and Strobel, J. Geophys. Res., 92, 5741, 1987), we find that the O+ mixing ratio must be reduced by 25% to match the UVS spectra. This brings the value in closer agreement with the nearly simultaneous ground-based observations by Morgan and Pilcher (Astrophys. J., 253, 406, 1982) of the [OII] lambda lambda 3726, 3729 emission. An even further reduction is warranted if the revised in-flight UVS calibration by Holberg et al. (Astrophys. J., 375, 716, 1991) is used. We use the Colorado Io Torus Emissions Package (CITEP; see Taylor et al., J. Geophys. Res., 100, 19541, 1995) to compare the UVS and ground-based observations. We also compare with later observations of O(+) emission from HST, Galileo, and other satellites, and discuss the new mixing ratio in relation to observed spatial and temporal variations. This work was supported in part by JPL/Galileo grant 958675.

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