Regulation of the Centrifugal Interchange Cycle in Saturn's Inner Magnetosphere

Details Regulation of the Centrifugal Interchange Cycle in Saturn's Inner Magnetosphere Regulation of the Centrifugal Interchange Cycle in Saturn's Inner Magnetosphere

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsm43b..07k&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SM43B-07

Physics

2740 Magnetospheric Configuration And Dynamics, 2753 Numerical Modeling, 2756 Planetary Magnetospheres (5443, 5737, 6033), 6275 Saturn

Scientific paper

Multi-fluid modeling of Saturn's magnetosphere allows us to quantify the interchange of hot, tenuous plasma from the plasma sheet, with cold, denser plasma from the inner magnetosphere, consistent with bulk parameters of Cassini data. Single injection events are regularly seen by Cassini, but the global distribution of such events cannot be determined by one-dimensional observation. Multi-fluid simulations enable us to characterize the growth of multiple injection events, showing that their development is a global process, dependent on the plasma distribution of ions from Enceladus and forcing from the solar wind conditions. Interchange evolves similarly to Rayleigh-Taylor instabilities, with the exception that the heavy ions are driven outward by centrifugal forces instead of gravity. Previous simulations have studied the role of the interplanetary magnetic field (IMF) when it is parallel and anti- parallel to the planetary magnetic field. Centrifugal forcing is reduced when the IMF is parallel, but increased when the IMF is anti-parallel. This IMF configuration alters the shape of the plasma sheet. The interchange instability also develops under the normally quiet parallel IMF when the mass loading in the Enceladus torus is increased. We will investigate the role of +/- By on the growth, width and length of the interchange fingers. The derived energy characteristics of the interchanging plasmas are consistent with Cassini observations.

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