Implications of the GSFC Q3 model for trapped particle motion

Details Implications of the GSFC Q3 model for trapped particle motion Implications of the GSFC Q3 model for trapped particle motion

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988jgr....93.5505a&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 93, June 1, 1988, p. 5505-5512.

Statistics

Computation

9

Astronomical Models, Magnetically Trapped Particles, Particle Motion, Planetary Magnetospheres, Uranus Atmosphere, Adiabatic Conditions, Atmospheric Models, Charged Particles, Uranus Satellites

Scientific paper

The Uranus magnetic field model of Connerney et al. (1987), designated GSFC Q3, is used to compute field geometric invariant parameters that determine the adiabatic motion of energetic charged particles trapped in the Uranian magnetosphere, performing computations only for points located along the Voyager 2 flyby trajectory. The L-shell values computed along the Voyager-2 trajectory were compared with L shell values corresponding to the orbital positions for the Uranian satellites Ariel, Umbriel, Miranda, and Titania for a time period centered on the time of the Voyager 2 closest approach to the planet. Bimodal distributions of L minima asociated with the orbital motion of the moons are obtained, thus complicating the model predictions and correlations with charged particle data. The location of charged particle absorption signatures associated with the sweeping effects of the Uranian satellites is reasonably predicted, but significant discrepancies remain which cannot be explained by Q3 model uncertainties.

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