The stability of the oscillation motion of charged grains in the Saturnian ring system

Details The stability of the oscillation motion of charged grains in the Saturnian ring system The stability of the oscillation motion of charged grains in the Saturnian ring system

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985jgr....90.1375x&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 90, Feb. 1, 1985, p. 1375-1384.

Physics

12

Celestial Mechanics, Charged Particles, Planetary Rotation, Saturn Rings, Space Plasmas, Angular Velocity, Corotation, Motion Stability, Perturbation Theory, Planetary Gravitation, Saturn Atmosphere, Saturn, Rings, Motion, Charged Particles, Oscillations, Stability, Grains, Velocity, Perturbations, Gravity Properties, Electrodynamics, Corotation, Plasma, Environment, Magnetic Fields, Dipoles, Formation, Radius, Erosion, Ejecta, Diffusivity, Optical Properties, Depth

Scientific paper

A 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.

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