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Scientific paper
Dec 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7439b&link_type=abstract
HST Proposal ID #7439
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Hst Proposal Id #7439 Solar System
Scientific paper
An excess of H-LyAlpha emission from Uranus' sunlit hemisphere has been detected by the IUE satellite since 1982, and some excess was confirmed with the Voyager 2 UVS during the 1986 encounter with Uranus. This emission is additional to the scattered solar and IPM H-LyAlpha, and must be produced by internal processes in the upper atmosphere, such as aurora or other unidentified mechanisms. IUE has observed very large short- and long-term intensity variations that support an auroral source. However, although Voyager detected UV auroral emissions by H2 in the sunlit hemisphere, it did not detect a large H-LyAlpha auroral emission there, making it impossible to provide conclusive evidence that the H-LyAlpha enhancements are due to aurora. Auroral emissions are spatially confined, and resolution of the emission spatial distribution could yield the needed evidence, or could alternatively provide observational clues to other possible causes of these variations. Uranus' intrinsically weak H-LyAlpha emission { 1600 R on average} has not allowed for such an experiment in the past. This program will image Uranus H-LyAlpha emission with STIS, which will have the high sensitivity in the far-UV {STIS/FUV MAMA} required to perform this experiment. The 6 allotted orbits have been re-organized, due to MAMA SAA restrictions, into a set of two orbits that will provide basic spatial information, and a more complete 4-orbit set that will fully map the emissions over two Uranus rotations.
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