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P. D. Feldman, T. B. Ake, A. F. Berman, H. W. Moos, D. J. Sahnow, D. F. Strobel, H. A. Weaver (JHU), P. R. Young (CfA), FUSE Solar System Team
The spectrum of the Io plasma torus in the range 995--1087 Å\ was recorded at ~0.3 Å\ resolution by the Far Ultraviolet Spectroscopic Explorer (FUSE) on January 20, 2000. Five orbits of data were obtained in point-and-shoot mode (no tracking of the moving target) with the East ansa of the torus initially centered in the 30'' \times 30'' aperture of the FUSE LiF spectrographs yielding a total observation time of 3405 seconds. The spectral resolution exceeds by a factor of ten that of the data obtained by the Hopkins Ultraviolet Telescope (HUT) during the Astro-1 mission (Moos et al., ApJ 382, L105, 1991). This region of the spectrum is dominated by resonance multiplets of \ion{S}{3} at 1018 Å\ and \ion{S}{4} at 1070 Å, whose multiplet structure is nearly completely resolved, as well as numerous \ion{S}{2} multiplets originating on the 2\!Do state of the ground configuration. Weak emission from the resonance multiplets of \ion{Cl}{3} at 1011 Å\ and \ion{Cl}{2} at 1071 Å\ are seen, the former being stronger with two components roughly one-tenth the brightness of the main components of \ion{S}{3} \lambda1018. Although collision strengths for Cl ions are not readily available, the isoelectronic relationship between S and Cl ions suggests an abundance of Cl+2 of a few percent relative to S+, similar to the result found by Küppers and Schneider (GRL 27, 513, 1999) for Cl+ from optical spectra. The ratio of \ion{S}{4} to \ion{S}{3} brightness is about twice that observed by HUT, which when the different slit geometries are accounted for supports the analysis by Hall et al. (ApJ 420, L45, 1994) that \ion{S}{4} emissions originate from a region more extended out of the centrifugal plane than the \ion{S}{3} emissions. We also note the detection of weak \ion{He}{2} emission at 1025.3 Å, on the blue wing of geocoronal Lyman-\beta. The origin of the helium ions is not clear at this time.
This work is based on data obtained for the Guaranteed Time Team by the NASA-CNES-CSA FUSE mission operated by the Johns Hopkins University. Financial support to U. S. participants has been provided by NASA contract NAS5-32985.
The author(s) of this abstract have provided an email address for comments about the abstract: pdf@pha.jhu.edu