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• W2158759063 endingPage "3422" @default.
• W2158759063 startingPage "3397" @default.
• W2158759063 abstract "An electron distribution in Jupiter's magnetosphere as a function of energy, pitch angle and spatial coordinates is derived from a comparison of model calculations of the planet's synchrotron radiation with the radio data; the distribution is consistent with the information available from the Pioneer data. The model calculations are based upon the magnetic field configurations as derived by Acuna and Ness [1976a, b] (the O 4 model) and Davis, Jones and Smith [quoted in Smith and Gulkis, 1979] (the P 11 (3,2) A model) from the Pioneer data. The electrons are assumed to diffuse radially inwards with a rate D=3 × 10 −9 L³ s −1 (where L is McIlwain's value) and have a lifetime against local losses τ=4 × 10 6 L −0.6 s, in agreement with the values derived by Goertz et al. [1979] from the Pioneer data. The number density of electrons with E ≥20 MeV at L=3 is in agreement with the values measured by the spacecraft, but the energy distribution appears to be much flatter. Electrons are absorbed with survival probabilities of ∼0.5 diffusing inwardly past Amalthea's sweeping region (for 20‐MeV electrons) and ∼0.35 past the ring, respectively. An energy dependent pitch angle scattering is found to occur at Amalthea's orbit, and there is no pitch angle scattering present near the ring." @default.
• W2158759063 created "2016-06-24" @default.
• W2158759063 creator A5084819648 @default.
• W2158759063 date "1981-05-01" @default.
• W2158759063 modified "2023-09-26" @default.
• W2158759063 title "A comparison of the radio data and model calculations of Jupiter's synchrotron radiation, 1. The high energy electron distribution in Jupiter's inner magnetosphere" @default.
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• W2158759063 doi "https://doi.org/10.1029/ja086ia05p03397" @default.
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