Effects of finite plasma pressure on centrifugally driven convection in Saturn's magnetosphere

Details Effects of finite plasma pressure on centrifugally driven convection in Saturn's magnetosphere Effects of finite plasma pressure on centrifugally driven convection in Saturn's magnetosphere

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsm11a1999l&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SM11A-1999

Physics

[2730] Magnetospheric Physics / Magnetosphere: Inner, [2740] Magnetospheric Physics / Magnetospheric Configuration And Dynamics, [2753] Magnetospheric Physics / Numerical Modeling, [2760] Magnetospheric Physics / Plasma Convection

Scientific paper

We have previously shown simulation results for centrifugally driven plasma convection in Saturn's inner magnetosphere, using the Rice Convection Model, including a continuously active distributed plasma source, and effects of the Coriolis force and the pickup current. These simulations result in a quasi-steady state, in which fast, narrow inflow channels alternate with slower, wider outflow channels, consistent with Cassini Plasma Spectrometer observations. Comparison of different plasma source models indicates that the inner plasma source distribution is a key element in determining the plasma convection pattern. Previous simulations, however, did not include the effects of finite plasma pressure and the associated gradient-curvature drift. We will investigate here the effects of finite plasma pressure and gradient-curvature drift by giving the cold plasma a finite temperature. We will also add a source of hot tenuous plasma at the outer simulation boundary in an attempt to simulate the injection/dispersion events observed by Cassini.

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