Ultraviolet Spectra of Saturn's Satellites, Ion Modification of Surface Ice

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Hst Proposal Id #6715 Solar System

Scientific paper

Saturn's medium-sized icy satellites display a diverse rangeof surface alteration caused by one or more externalprocesses. We will investigate the role of magnetosphericcharged particle interactions with the surfaces of thesesatellites by searching for spectral signatures of ion-irradiated ice. To do this, we will obtain the first highS/N, ultraviolet wavelength spectra of Enceladus, Tethys,Dione, and the leading hemisphere of Rhea to wavelengths asshort as 2200 Angstrom . We will search in particular for thestrong Hartley band of ozone at 2600 Angstrom ; O_3 is formedby the impact of O^+ ions in ice. We have recently identifiedthis band in Ganymede, which resides in a plasma environmentsimilar to that of Saturn's satellites. A spectrum of Rhea'strailing hemisphere obtained by us also shows evidence ofpossible O_3 absorption that can be confirmed by observing thespectrum of the opposite hemisphere. The range of hemisphericalbedo differences from Enceladus to Rhea and the differencesin ion density and energy will allow us to determine therelative importance of plasma bombardment in the long-termalteration of these satellite surfaces. In addition to O_3,other possible UV absorbers incude peroxide, H_2O_2, theexpected photolysis product of O_3, SO_2, observed in Europaand apparently the preferred reaction product when S ispresent, and simple hydrocarbons which show distinct UVstructure. No other telescope or instrument is capable ofthese measurements.

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