A Diffusive Equilibrium Density Model for a Two-Species Plasma in Saturn's Magnetosphere

Details A Diffusive Equilibrium Density Model for a Two-Species Plasma in Saturn's Magnetosphere A Diffusive Equilibrium Density Model for a Two-Species Plasma in Saturn's Magnetosphere

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufm.p51d..01p&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #P51D-01

Physics

2756 Planetary Magnetospheres (5443, 5737, 6033), 5737 Magnetospheres (2756)

Scientific paper

Measurements of the upper hybrid resonance frequency by the Radio and Plasma Wave Science (RPWS) instrument have been used to derive electron densities for more than 50 Cassini passes through Saturn's inner magnetosphere between July 1, 2004 and September 1, 2007. As the latitudinal and radial distributions of these density measurements have expanded, increasingly more complex density models have been developed to describe the distribution of plasma inside L=9. The early radial outflow model [Persoon et al., Geophys. Res. Lett., 32, L23105, 2005] found that the electron density has a radial dependence of R- 3.63, but the model was restricted to density measurements in the equatorial plane. As density measurements at higher latitudes became available, a simple centrifugal potential model [Persoon et al., Geophys. Res. Lett., 33, L18106, 2006] was developed for the plasma distribution along the planetary magnetic field lines. This early centrifugal potential model, however, had a limited latitudinal distribution and was able to resolve only one ion species in the plasma distribution. Recent plasma density measurements acquired at higher latitudes have made it possible to resolve two distinct plasma components, assumed to be the water group ions (W+) and the hydrogen ions (H+). When compared to the centrifugal potential model, the density measurements for 5

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