Other
Scientific paper
Dec 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7316n&link_type=abstract
HST Proposal ID #7316
Other
Hst Proposal Id #7316 Solar System
Scientific paper
Saturn's medium-sized icy satellites display a diverse range of surface alteration caused by one or more external processes. We will investigate the role of magnetospheric charged particle interactions with the surfaces of these satellites by searching for spectral signatures of ion- irradiated ice. To do this, we will complete the investigation begun in cycle 6 by obtaining the first high S/N, ultraviolet wavelength spectra of Enceladus and Tethys to wavelengths as short as 1800 Angstrom . We will search in particular for the strong Hartley band of ozone at 2600 Angstrom ; O_3 is formed by the impact of O^+ ions in ice. We have recently used this band to identify ozone on Ganymede, which resides in a plasma environment similar to that of Saturn's satellites. A spectrum of Rhea's trailing hemisphere also shows evidence of possible O_3 absorption. Enceladus and Tethys are key to this effort because they exhibit significantly higher UV albedos than Rhea, Dione, or Iapetus. Enceladus, in particular, shows evidence of recent resurfacing, and is, therefore, an important end-member for our study. Enceladus and Tethys reside in a portion of Saturn's magnetosphere where the ion density is high, but the average energy per impacting ion is low, providing a crucial test of these parameters in the formation of chemical contaminants in the surface ice. Other possible absorbers include H_2O_2, HO_2, SO_2, and simple hydrocarbons which show distinct UV structure. No other telescope or instrument is capable of these measurements.
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