Postberg, F.; Kempf, S.; Hillier, J. K.; Srama, R.; Green, S. F.; McBride, N. and Grün, E.
|DOI (Digital Object Identifier) Link:||http://doi.org/10.1016/j.icarus.2007.09.001|
|Google Scholar:||Look up in Google Scholar|
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.
|Item Type:||Journal Article|
|Keywords:||Saturn; Enceladus; Interplanetary dust; Planetary rings|
|Academic Unit/Department:||Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Jonathan Hillier|
|Date Deposited:||13 Feb 2008|
|Last Modified:||04 Oct 2016 10:08|
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