Width of Injection/Dispersion Events in Saturn's Inner Magnetosphere

Details Width of Injection/Dispersion Events in Saturn's Inner Magnetosphere Width of Injection/Dispersion Events in Saturn's Inner Magnetosphere

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsm43b..03c&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SM43B-03

Physics

2463 Plasma Convection (2760), 6033 Magnetospheres (2756), 6275 Saturn

Scientific paper

Longitudinally localized injection and drift dispersion of hot plasma are frequently observed by the Cassini Plasma Spectrometer (CAPS) and the Cassini Magnetospheric Imaging Instrument (MIMI) in Saturn's magnetosphere. These signatures provide direct evidence for the major convective process in the inner magnetosphere of a rapidly rotating planet, in which the radial transport of plasma is expected to comprise hot, tenuous plasma moving inward and cooler, denser plasma moving outward. Previous analyses of Cassini plasma observations are consistent with this scenario, but suggest further that the hot inflow sectors are significantly narrower than the adjacent cooler outflow sectors, a property that was not anticipated theoretically. Here we quantify this property by calculating the fraction of the available time that is occupied by injection structures in a two-year data set containing 429 such structures. This fraction is found to be small, typically ~ 3 - 7%, with no obvious dependence on SKR longitude. We will expand our data set by including the very young injection events discussed by Burch et al. [2005 GRL], which were excluded by the selection criteria in our previous study.

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