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The surface compositon of Enceladus: clues from the ultraviolet

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dc.contributor.author Hendrix, Amanda R.
dc.contributor.author Hansen, Candice J.
dc.date.accessioned 2014-09-05T20:18:29Z
dc.date.available 2014-09-05T20:18:29Z
dc.date.issued 2009-08-03
dc.identifier.citation IAU Symposium 263 Icy bodies in the solar system, Rio de Janeiro, Brazil, August 3-7, 2009 en_US
dc.identifier.clearanceno 09-4870
dc.identifier.uri http://hdl.handle.net/2014/44692
dc.description.abstract The reflectance of Saturn’s moon Enceladus has been measured at far ultraviolet (FUV) wavelengths (115–190 nm) by Cassini’s UltraViolet Imaging Spectrograph (UVIS). At visible and near infrared (VNIR) wavelengths Enceladus’ reflectance spectrum is very bright, consistent with a surface composed primarily of H2O ice. At FUV wavelengths, however, Enceladus is surprisingly dark - darker than would be expected for pure water ice. We find that the low FUV reflectance of Enceladus can be explained by the presence of a small amount of NH3 and a small amount of a tholin in addition to H₂O ice on the surface. en_US
dc.description.sponsorship NASA/JPL en_US
dc.language.iso en_US en_US
dc.publisher Pasadena, CA : Jet Propulsion Laboratory, National Aeronautics and Space Administration, 2009 en_US
dc.subject planets en_US
dc.subject satellites en_US
dc.subject Enceladus en_US
dc.title The surface compositon of Enceladus: clues from the ultraviolet en_US
dc.type Presentation en_US


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