Physical electron belt model from Jupiter surface out to Europa

Details Physical electron belt model from Jupiter surface out to Europa Physical electron belt model from Jupiter surface out to Europa

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja....11155s&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #11155

Computer Science

Scientific paper

The three dimensional model, Salammbo-3D, has been developed to study spatial distribution of electron in the inner radiation belts of Jupiter. In a first time, this model was valid between L = 1 and L = 6, just inside Io orbit. Now, it has been extended up to L = 9.5, just inside Europa orbit. To allow this extension, a more realistic magnetic field than the tilted dipole magnetic field, used before, has been introduced. Two magnetic field models are available: the model of Connerney (1981) and the one of Khurana (1997). Both of them are composed of two parts: an internal magnetic field (derivable of a scalar potential) and a external magnetic field (due to the current sheet). Results deduced from Salammbo-3D, using these two different models, will be shown and compared. Two important results come out from this study. Firstly, the extension of our model outside Io orbit aims to show that Io do not play any role on relativistic electron dynamics i.e. it do not create losses of particles like Amalthea, Thebe and first two moons. The second important result is that external field, due to current sheet, only change radiation belts topology for L > 5. Then, to validate our 3D code from the Jovian surface up to Europa orbit, the results will be compared with two kinds of observations. A first comparison will be done with spacecraft data (Pioneer 10 and 11) and a second with radio observation (VLA). Indeed, with the help of Salammbo-3D and a synchrotron emission model, in situ 2D images of Jupiter synchrotron emission can be deduced. It is then possible to investigate on the global radiation belts shape by comparing simulations and VLA observations.

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