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The stability of the oscillation motion of charged grains in the Saturnian ring systemA perturbation approach for the gravitoelectrodynamic forces encountered in the corotating plasma environment of Saturn is used to determine the stability of charged grains, given a random initial velocity. Attention is given to the implications of the Northrop and Hill (1982) and Mendis et al. (1982) results for the formation of the Saturnian ring system, and it is suggested that the marginal z stability radius at 1.5245 Saturn radii for Kepler-launched particles is due to an erosion process with ejecta of the order 0.05-0.5 microns, rather than that of the previously suggested plasma. The diffuseness of the Saturnian rings beyond the F ring is also explained in terms of instability, while a new critical radius for r instability is suggestd for the optical depth feature at 1.72 Saturn radii. The F ring is analyzed in detail.
Document ID
19850041194
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Xu, R.-L.
(California, University La Jolla, CA; Chinese Academy of Sciences, Institute of Space Physics, Beijing, People's Republic of, United States)
Houpis, H. L. F.
(California, University La Jolla, CA, United States)
Date Acquired
August 12, 2013
Publication Date
February 1, 1985
Publication Information
Publication: Journal of Geophysical Research
Volume: 90
ISSN: 0148-0227
Subject Category
Lunar And Planetary Exploration
Accession Number
85A23345
Funding Number(s)
CONTRACT_GRANT: NSG-7102
CONTRACT_GRANT: NSG-762
CONTRACT_GRANT: NAGW-399
CONTRACT_GRANT: NGR-05-009-110
CONTRACT_GRANT: NSF AST-81-08706
Distribution Limits
Public
Copyright
Other

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