A modeling of the effect of the rings of Jupiter on trapped >3-MeV electrons and protons is proposed. The effect is then added to the physical model Salammbô and discussed against in situ measurements obtained by the Pioneer 11 and Galileo Probe missions. It is first shown that there is no evidence of an effect of the rings on the Jovian radiation belts, thanks to the new internal magnetic field model proposed by the Juno mission. Two grain populations are then studied: small grains, with a radius lower than 100 μm, are shown to not affect observable >3-MeV trapped particles. The normal optical depth of grains with a radius larger than 2 cm, which may exist in the main ring, is constrained to be lower than 10 À7 by the Salammbô model.Plain Language Summary Four very faint dust rings exist very close to the giant planet Jupiter. In the ring's region, very energetic electrons and protons are trapped by the planetary magnetic field in what are called radiation belts. The first question addressed by this article is to determine if the rings affect the radiation belts of Jupiter. To do so, a numerical model of the radiation belts, named Salammbô, is used in conjunction with particle measurements gathered in situ by Pioneer 11 in 1974 and Galileo Probe in 1995. This article shows that the micrometer grains that populate the rings do not affect available measurements. The second topic covered by this article is about how the Salammbô model constrains the distribution of centimeter grains in the brightest ring of Jupiter, named the main ring.

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With the increase of sensitivity of devices to singleevent upsets (SEUs), the possibility to trigger an upset with incident electrons has been recently raised. All the mechanisms susceptible to trigger the SEUs are investigated in detail. New measurements performed on the field programmable gate array static random access memory based from Xilinx Spartan 6 at 1 MeV seem to confirm two SEU regions with the transition located around 10 MeV.