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The surface composition of Enceladus: clues from the Ultraviolet

Published online by Cambridge University Press:  06 April 2010

Amanda R. Hendrix  and
Candice J. Hansen
Amanda R. Hendrix
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, USA
Candice J. Hansen
Affiliation:
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, USA
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Abstract

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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.

Keywords

planets and satellites: generalplanets and satellites: Enceladus
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S263: Icy Bodies of the Solar System , August 2009 , pp. 126 - 130
Copyright
Copyright © International Astronomical Union 2010

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