Understanding the low and high energy electron &proton radiation belts of Saturn

Details Understanding the low and high energy electron &proton radiation belts of Saturn Understanding the low and high energy electron &proton radiation belts of Saturn

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja....13423s&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #13423

Physics

Scientific paper

As the inner Jovian magnetosphere, the innermost part of the magnetosphere of Saturn is populated with extended solid surfaces, dust and gas clouds, plasma and energetic particles (electrons, protons, ions and neutral atoms). From a very limited set of measurements obtained along the Pioneer 11 and Voyager 1 &2 trajectories during their flyby close to the planet many years ago, the radiation belts of Saturn appeared less energetic than the Jovian ones, but very less as we have expected it and deduced it from the main magnetospheric characteristics of Saturn. The interactions between the all components of the kronian system, continually acting, explain these observations. To be convinced of this fact, we propose to use the results coming from a three-dimensional physical model of the electron and proton radiation belts. Before discussing on the effects of some kronian system s components on the radiation belts, the physical model is described (theoretic approach, physical processes modelled, assumptions) and comparisons with data sets are shown. The effects of the physical processes on the distribution of trapped energetic particles (electrons &protons) deduced from the resolution of the transport equation in a (energy, latitude, radial distance) phase space can be then displayed and discussed. The differences between the electron and proton radiation belts are also bring out.

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