FUV Spectroscopy of Io's SO2 Atmosphere and Surface -- Cycle 3 High

Details FUV Spectroscopy of Io's SO2 Atmosphere and Surface -- Cycle 3 High FUV Spectroscopy of Io's SO2 Atmosphere and Surface -- Cycle 3 High

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993hst..prop.4600c&link_type=abstract

HST Proposal ID #4600

Physics

Hst Proposal Id #4600

Scientific paper

Cycle 1 HST observations of Io have provided new insights into the nature of Io's surface albedo, the distribution of the SO2 atmosphere, and the extent and excitation of the FUV airglow emissions. FOC images show an anti-correlation between the brightness at 4000 A and 2800 A, due to either surface SO2 frost or SO2 gas absorption above the frost at the shorter wavelength. FOS spectra of the albedo spectrum at high signal to noise clearly show SO2 gas absorption bands near 1900-2000 A and evidence up to 1000 times spatial variation in the SO2 gas column from the 2300 A spectrum. The FOS and GHRS airglow spectra have for the first time resolved the extent of the FUV emission lines (1.7 Io radii in diameter), and found that these lines decrease by a factor of 4-5 within 15 minutes of Io's passing into eclipse. This suggests that in shadow either the SO2 atmosphere condenses onto the surface or the ionosphere recombines rapidly: the difference between these two possibilities is very significant. In cycle 3 we propose to scan across Io with a small FOS aperture to obtain spatially resolved spectra of the known bright and dark regions to discriminate between gas absorption and surface albedo changes. We will also obtain FUV spectra of Io emerging from eclipse to determine the time scale on which the FUV airglow emission lines recover their intensity on return into sunlight.

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