Ion Composition near Enceladus during Cassini Flybys: Measurements and Chemical Model

Details Ion Composition near Enceladus during Cassini Flybys: Measurements and Chemical Model Ion Composition near Enceladus during Cassini Flybys: Measurements and Chemical Model

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p51a1125g&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #P51A-1125

Physics

Plasma Physics

[5422] Planetary Sciences: Solid Surface Planets / Ices, [6280] Planetary Sciences: Solar System Objects / Saturnian Satellites, [7823] Space Plasma Physics / Ionization Processes

Scientific paper

The Cassini spacecraft has flown by Saturn’s moon Enceladus several times, with the most recent two during a few weeks prior to this meeting. The surprising discovery of the jets of water/ice from the southern hemisphere of this moon has stimulated considerable discussion regarding the possible nature and especially temperature of the internal reservoir for these jets. A possible explanation that has been suggested for the apparently liquid water internal to such a cold, icy body involves the possible presence of small amounts of species such as ammonia that would affect the melting point. Measurements during previous flybys have hinted at the existence of such species. We have been analyzing the ion composition data from the Cassini Plasma Spectrometer (CAPS) Ion Mass Spectrometer obtained during the recent Enceladus flybys and comparing the results with those of a chemical network model (Boice, this session). In addition to the ubiquitous water group ions we find nitrogen and some of its hydrides.

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