Hopkins Ultraviolet Telescope determination of the Io torus electron temperature

Details Hopkins Ultraviolet Telescope determination of the Io torus electron temperature Hopkins Ultraviolet Telescope determination of the Io torus electron temperature

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...420l..45h&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 420, no. 1, p. L45-L48

Astronomy and Astrophysics

Astronomy

12

Electron Energy, Io, Plasma Temperature, Sulfur, Toruses, Ultraviolet Astronomy, Ultraviolet Spectra, Ultraviolet Spectrometers, Ultraviolet Telescopes, Voyager 1 Spacecraft, Voyager 2 Spacecraft

Scientific paper

Sulfur ion emissions from the Io plasma torus observed by the Hopkins Ultraviolet Telescope (HUT) in 1990 December have been analyzed to determine the effective temperature of the exciting electrons. Spectra were obtained with a long slit that extended from 3.1 to 8.7 Jupiter radii RJ on both dawn and dusk torus ansae. The average temperature of electrons exciting S(2+) emissions from the dawn ansa is (4800 +/- 2400) K lower than on the dusk ansa, a dawn-dusk asymmetry comparable in both sign and magnitude to that measured by the Voyager Ultraviolet Spectrograph (UVS) experiment. Emissions from S(2+) ions are generated in a source region with electron temperatures in the range 32,000-56,000 K; S(3+) ion emissions are excited by electrons that average 20,000-40,000 K hotter. This distinct difference suggests that the S(3+) emission source region is spatially separate from the S(2+) source region. Estimated relative aperture filling factors suggest that the S(3+) emissions originate from a region more extended out of the centrifugal plane than the S(2+) emissions.

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