Radial diffusion in Saturn's radiation belts - A modeling analysis assuming satellite and ring E absorption

Details Radial diffusion in Saturn's radiation belts - A modeling analysis assuming satellite and ring E absorption Radial diffusion in Saturn's radiation belts - A modeling analysis assuming satellite and ring E absorption

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983jgr....88..808h&link_type=abstract

Journal of Geophysical Research, vol. 88, Feb. 1, 1983, p. 808-818.

Astronomy and Astrophysics

Astronomy

33

Magnetospheric Proton Density, Natural Satellites, Particle Diffusion, Planetary Magnetospheres, Proton Belts, Saturn (Planet), Saturn Rings, Astronomical Models, Capture Effect, Diffusion Coefficient, Magnetically Trapped Particles, Planetary Magnetic Fields, Saturn, Radial Diffusion, Radiation Belts, Models, Analysis, Satellites, Rings, E Ring, Absorption, Density Profiles, Pioneer 11, Voyager 1, Amplitude, Magnetosphere, Calculations, Data, Parameters, Optical Properties, Depth, Radial Distance, Phases,

Scientific paper

A modeling analysis is carried out of six experimental phase space density profiles for nearly equatorially mirroring protons using methods based on the approach of Thomsen et al. (1977). The form of the time-averaged radial diffusion coefficient D(L) that gives an optimal fit to the experimental profiles is determined under the assumption that simple satellite plus Ring E absorption of inwardly diffusing particles and steady-state radial diffusion are the dominant physical processes affecting the proton data in the L range that is modeled. An extension of the single-satellite model employed by Thomsen et al. to a model that includes multisatellite and ring absorption is described, and the procedures adopted for estimating characteristic satellite and ring absorption times are defined. The results obtained in applying three representative solid-body absorption models to evaluate D(L) in the range where L is between 4 and 16 are reported, and a study is made of the sensitivity of the preferred amplitude and L dependence for D(L) to the assumed model parameters. The inferred form of D(L) is then compared with that which would be predicted if various proposed physical mechanisms for driving magnetospheric radial diffusion are operative at Saturn.

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