Numerical Simulations of Plasma Transport in Saturn's Inner Magnetosphere

Details Numerical Simulations of Plasma Transport in Saturn's Inner Magnetosphere Numerical Simulations of Plasma Transport in Saturn's Inner Magnetosphere

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agusmsm14a..05h&link_type=abstract

American Geophysical Union, Spring Meeting 2009, abstract #SM14A-05

Physics

2712 Electric Fields (2411), 2732 Magnetosphere Interactions With Satellites And Rings, 2736 Magnetosphere/Ionosphere Interactions (2431), 2753 Numerical Modeling, 2756 Planetary Magnetospheres (5443, 5737, 6033)

Scientific paper

The Rice Convection Model (RCM), a numerical simulation code developed over several decades for the study of plasma motion in Earth's inner magnetosphere, has been adapted for the study of centrifugally-driven plasma transport in the inner magnetosphere of Saturn (2 < L < 12). We have incorporated into the RCM code a continuously active plasma source deriving from the observed Enceladus neutral water vapor plume. The neutral water vapor source peaks at L=4 (the orbit of Enceladus), but the resulting plasma source peaks farther out (5.5 < L < 7.5) because that is where the ambient electron population has sufficient temperature to ionize water vapor. The inclusion of this continuously active distributed plasma source has elucidated many aspects of the resulting interchange plasma transport, including in particular the observed and heretofore unexplained fact that the longitudinal sectors of outflow are broader, and therefore slower, than the interspersed sectors of inflow.

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