Computer Science
Scientific paper
Jul 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986sci...233...97k&link_type=abstract
Science (ISSN 0036-8075), vol. 233, July 4, 1986, p. 97-102.
Computer Science
60
High Temperature Plasmas, Planetary Magnetic Fields, Planetary Magnetospheres, Space Plasmas, Uranus Atmosphere, Electron Energy, Miranda, Proton Energy, Spectrograms, Voyager 2 Spacecraft
Scientific paper
Inferences are drawn on the morphology and composition of the Uranus magnetosphere based on low-energy charged particle data collected by Voyager 2. Proton and electron energies in the magnetosphere attained energies of 4 and 1.2 MeV, respectively, although electron intensities surpassed the proton intensities at most energy levels. Protons dominated in the ion energy regime 0.6-1.0 MeV. The ion and electron spectra were Maxwellian below about 200 keV and had a power law distribution at energies over 590 keV. The power law was reduced by a factor of nearly three inside the orbit of Miranda. The proton population is dense enough to polymerize CO and CH4 ice surfaces within 10,000-100,000 yr. The data indicated that the particles are swept out at least to the orbit of Titania by the satellites. The morphology of the magnetosphere closely resembles that around Jupiter, except that plasma sheet distorsion from particle loading is negligible in regions within 15 Uranus radii.
Armstrong Thomas P.
Axford Wiliam Ian
Cheng Andrew F.
Gloeckler George
Krimigis Stamatios M.
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