Physics
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsm41b..02h&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SM41B-02
Physics
2753 Numerical Modeling, 2756 Planetary Magnetospheres (5443, 5737, 6033), 5737 Magnetospheres (2756), 6275 Saturn
Scientific paper
The steady-state version of Faraday's law tells us that the circulation of magnetic flux in a planetary magnetosphere must be conservative in the sense that [vrBz] = 0, where vr is the radial component of plasma (ExB) drift, Bz is the poloidal magnetic-field component, both evaluated at the equatorial plane, and [vrBz] represents an average of vrBz over both azimuth and time. The centrifugal interchange instability is thought to drive radial transport in the magnetospheres of Jupiter and Saturn. Most theoretical models of this radial transport process share the feature (often assumed at the outset) that inflow and outflow sectors are of comparable azimuthal width, and therefore, according to Faraday's law, of comparable radial velocity magnitude. Cassini observations in Saturn's inner magnetosphere [e.g., Chen and Hill, this session] have revealed that the inflow sectors are of much smaller azimuthal width, and hence much larger radial velocity magnitude, than the intervening outflow sectors. Recent numerical simulations with the Rice Convection Model [Wu et al., this session] suggest that the extreme mismatch between the widths of inflow versus outflow sectors may result from the presence of an active plasma source within the region of observation, coupled with the Coriolis acceleration of the outflowing plasma.
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