ENA Emissions at Saturn

Details ENA Emissions at Saturn ENA Emissions at Saturn

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agusmsm13a..01c&link_type=abstract

American Geophysical Union, Spring Meeting 2009, abstract #SM13A-01

Physics

5719 Interactions With Particles And Fields, 5737 Magnetospheres (2756), 5780 Tori And Exospheres

Scientific paper

Composite images of hydrogen atoms (30-50 keV) and oxygen atoms (64-144 keV) have been combined for the first ~150 days of 2007 and 2008 when the Cassini spacecraft viewed the equatorial plane of Saturn from high latitudes (>35°N). Observation from these elevated latitudes allows projection of the emissions onto the equatorial plane of Saturn, from which the gross morphology of the emissions can be evaluated by combining many days' worth of ENA images. The projected images were corrected for slant viewing geometry and for Compton-Getting effects in the energetic protons and oxygen ions that generated the ENA emissions. In sun-fixed coordinates, the H emissions tend of concentrate on the nightside of Saturn just outside the orbit of Rhea (8.7 RS), while the oxygen emissions also concentrate on the nightside but between the orbits of Rhea and Dione (6.3 RS). In rotating coordinates (SLS longitude), single or double sources exist in both the H and O emissions. These sources may extend over 90° in longitude and appear at different longitudes at different times for different species. These sources persist for weeks or longer. There is no evidence for spiral patterns in the long-term ENA averages. The appearance and disappearance of individual ENA sources in SLS longitude suggests different sources rotate at different speeds, which may be related to the double sources observed in SKR periodicities.

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