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Title:
The E-ring in the vicinity of Enceladus. II. Probing the moon's interior—The composition of E-ring particles
Authors:
Postberg, F.; Kempf, S.; Hillier, J. K.; Srama, R.; Green, S. F.; McBride, N.; Grün, E.
Affiliation:
AA(Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, D-69117 Heidelberg, Germany), AB(Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, D-69117 Heidelberg, Germany; Institut für Geophysik und Extraterrestrische Physik, Universität Braunschweig, Mendelssohnstr. 3, 38106 Braunschweig, Germany), AC(Planetary and Space Sciences Research Institute, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK), AD(Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, D-69117 Heidelberg, Germany), AE(Planetary and Space Sciences Research Institute, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK), AF(Planetary and Space Sciences Research Institute, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK), AG(Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, D-69117 Heidelberg, Germany; Hawaii Institute of Geophysics and Planetology, University of Hawaii, 1680 East West Road, Honolulu, HI 96822, USA)
Publication:
Icarus, Volume 193, Issue 2, p. 438-454. (Icarus Homepage)
Publication Date:
02/2008
Origin:
ELSEVIER
DOI:
10.1016/j.icarus.2007.09.001
Bibliographic Code:
2008Icar..193..438P

Abstract

The population of Saturn's outermost tenuous E-ring is dominated by tiny water ice particles. Active volcanism on the moon Enceladus, embedded in the E-ring, has since late 2005 been known to be a major source of particles replenishing the ring. Therefore particles in the vicinity of Enceladus may provide crucial information about the dynamical and chemical processes occurring below the moon's icy surface. Here we present a statistical evaluation of more than 2000 impact ionisation mass spectra of Saturn's E-ring particles, with sizes predominantly below 1 μm, detected by the Cosmic Dust Analyser onboard the Cassini spacecraft. We focus on the identification of non-water features in spectra otherwise dominated by water ice signatures. Here we specify the categorisation of two different spectrum types, which probably represent two particle populations. Type I spectra imply pure water ice particles, whereas in Type II spectra organic compounds and/or silicate minerals are identified as impurities within the icy particles. This finding supports the hypothesis of a dynamic interaction of Enceladus' rocky core with liquid water.
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