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Ultraviolet observations of Phoebe from the Cassini UVIS

Show simple item record Hendrix, Amanda R. Hansen, Candice J. 2008-08-14T22:58:25Z 2008-08-14T22:58:25Z 2007-09-21
dc.identifier.citation Icarus 193 (2008) 323–333, doi:10.1016/j.icarus.2007.06.030 en_US
dc.identifier.clearanceno 07-2246
dc.description.abstract Observations of Saturn’s distant moon Phoebe were made at far-ultraviolet (FUV) (1100–1900 Å) and extreme-ultraviolet (EUV) (600–1100 Å) wavelengths by the Cassini Ultraviolet Imaging Spectrograph (UVIS) during the Cassini spacecraft flyby on June 11, 2004. These are the first UV spectra of Phoebe and the first detection of water ice on a Solar System surface using FUV wavelengths. The characteristics of water ice in the FUV are presented, and Hapke models are used to interpret the spectra in terms of composition and grain size; the use of both areal and intimate mixing models is explored. Non-ice species used in these models include carbon, ice tholin, Triton tholin, poly-HCN and kerogen. Satisfactory disk-integrated fits are obtained for intimate mixtures of ~10% H2O plus a non-ice species. Spatially resolved regions of higher (~20%) and lower (~5%) H2O ice concentrations are also detected. Phoebe does not display any evidence of volatile activity. Upper limits on atomic oxygen and carbon are 5 × 10¹¹ and 2 × 10¹² atoms/cm2, respectively, for solar photon scattering. The UVIS detection of water ice on Phoebe, and the ice amounts detected, are consistent with IR measurements and contribute to the evidence for a Phoebe origin in the outer Solar System rather than in the main asteroid belt. en_US
dc.description.sponsorship NASA/JPL en_US
dc.language.iso en_US en_US
dc.publisher Elsevier Inc. en_US
dc.subject Ultraviolet observations en_US
dc.subject Spectroscopy en_US
dc.subject Saturn en_US
dc.subject satellites en_US
dc.subject Ices en_US
dc.subject UV spectroscopy en_US
dc.title Ultraviolet observations of Phoebe from the Cassini UVIS en_US
dc.type Article en_US

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