Modeling the Enceladus plume–plasma interaction
Article first published online: 10 FEB 2010
Copyright 2010 by the American Geophysical Union.
Geophysical Research Letters
Volume 37, Issue 3, February 2010
How to Cite
2010), Modeling the Enceladus plume–plasma interaction, Geophys. Res. Lett., 37, L03202, doi:10.1029/2009GL041613., , and (
- Issue published online: 10 FEB 2010
- Article first published online: 10 FEB 2010
- Manuscript Accepted: 5 JAN 2010
- Manuscript Revised: 29 DEC 2009
- Manuscript Received: 4 NOV 2009
 We investigate the chemical interaction between Saturn's corotating plasma and Enceladus' volcanic plumes. We evolve a parcel of ambient plasma as it passes through a prescribed H2O plume using a physical chemistry model adapted for water-group reactions. The flow field is assumed to be that of a plasma around an electrically-conducting obstacle centered on Enceladus and aligned with Saturn's magnetic field, consistent with Cassini magnetometer data. We explore the effects on the physical chemistry due to: (1) a small population of hot electrons, (2) a plasma flow decelerated in response to the pickup of fresh ions, and (3) the source rate of neutral H2O. The model confirms that charge exchange dominates the local chemistry and that H3O+ dominates the water-group composition downstream of the Enceladus plumes. We also find that the amount of fresh pickup ions depends heavily on both the neutral source strength and on the presence of a persistent population of hot electrons.