Charged particle drifts in Saturn's inner and middle equatorial magnetosphere using different magnetospheric field models

Details Charged particle drifts in Saturn's inner and middle equatorial magnetosphere using different magnetospheric field models Charged particle drifts in Saturn's inner and middle equatorial magnetosphere using different magnetospheric field models

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm23a1908r&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM23A-1908

Physics

[2730] Magnetospheric Physics / Magnetosphere: Inner, [2740] Magnetospheric Physics / Magnetospheric Configuration And Dynamics, [2756] Magnetospheric Physics / Planetary Magnetospheres, [2760] Magnetospheric Physics / Plasma Convection

Scientific paper

Drifts of charged particles in Saturn's inner and middle magnetosphere are commonly treated as purely azimuthal. While for certain applications this assumption is adequate, there are a series of observations that may only be explained if more complex drift patterns are introduced. For instance, the organization of electron density as a function of SKR longitude within the Enceladus torus has been interpreted as evidence for a two-cell convection structure. The position of energetic electron depletions from Saturn's rings and moons is commonly found at locations that map away from the known orbits of such absorbers, even at distances deep in the dipolar magnetosphere of Saturn. In this presentation we report the results of tracing charged particle guding centers in different magnetospheric field models, in an attempt to explain some of these observations. The tracing is performed for different particle species and energies. We find that non-dipolar perturbations to Saturn's internal field (ring current and magnetopause current) have minor effects to the particle drifts shells inside 10-15 Saturn radii (Rs), except at periods of strong magnetospheric compression. We also model the effects of a dusk-dawn and dawn-dusk electric field. For the two-cell convection model we use a simple rotating electric field perturbation. Patricle drifts can become very complex for electrons and for energies that the gradient and curvature drifts become comparable to the corotational drift.

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