Plasma transport in a rapidly rotating axisymmetric magnetosphere with asymmetric plasma distribution and non-uniform ionospheric conductivities: General equations and preliminary implications

Details Plasma transport in a rapidly rotating axisymmetric magnetosphere with asymmetric plasma distribution and non-uniform ionospheric conductivities: General equations and preliminary implications Plasma transport in a rapidly rotating axisymmetric magnetosphere with asymmetric plasma distribution and non-uniform ionospheric conductivities: General equations and preliminary implications

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm23a1910a&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM23A-1910

Physics

[2756] Magnetospheric Physics / Planetary Magnetospheres

Scientific paper

Numerous explanations have been proposed since the discovery of significant rotational modulation effects in the axisymmetric magnetosphere of Saturn, but they still remain conceptual in essence. Cassini plasma, magnetic field and radio observations indeed revealed some intriguing and unique properties of Saturn’s magnetosphere that are not yet fully taken into account in existing theoretical models. Our long-term objective is to combine all of them into a complete formalism. In order to study consistently the large-scale convection and describe the transport of mass and angular momentum in the magnetosphere of Saturn, we first derive and discuss here the general equations governing the time-evolution of a multicomponent plasma embedded in a differentially rotating magnetosphere which includes various longitudinal and/or latitudinal asymmetries (plasma distribution, ionospheric conductivities) and, consequently, various field-aligned and/or transverse current systems, as constrained by Cassini multi-instrumental observations.

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