Far-ultraviolet spectroscopy of Io from Cassini

Details Far-ultraviolet spectroscopy of Io from Cassini Far-ultraviolet spectroscopy of Io from Cassini

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003dps....35.0207h&link_type=abstract

American Astronomical Society, DPS meeting #35, #02.07; Bulletin of the American Astronomical Society, Vol. 35, p.912

Astronomy and Astrophysics

Astronomy

Scientific paper

During the Cassini flyby of the Jupiter system (December 2000 - January 2001), the Ultraviolet Imaging Spectrograph (UVIS) obtained spectral images of Io, resulting in the measurement of neutral oxygen and sulfur emissions at Io. We present the results from four observations performed at distances of 131-169 RJ. During these observations, Cassini was in the unique position of observing Io's sub-jovian and anti-jovian hemispheres. The observations were performed using the Cassini UVIS FUV channel, which covers the 111.5-191.2 nm wavelength range over 1024 spectral pixels. The UVIS has 64 pixels in the spatial dimension. These observations were all performed using the low-resolution, 0.48 nm (1.5 mrad) entrance slit. Io is the most dynamic body in the solar system, being the most volcanically active and the most temporally variable in many aspects. Observations at practically all wavelengths have continued to yield information on Io's changingvolcanoes, surface, and atmosphere. We use these far-UV images and spectra to determine the approximate spatial extent of the neutral species making up Io's atmosphere, and to understand the processes acting on the atmosphere of Io.

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