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- W2506139685 abstract "A dust disc within a planetary magnetosphere constitutes a novel type of dust-ring current. Such an azimuthal current carrying dust disc is subject to the dusty plasma analog of the well known finite-resistivity 'tearing' mode instability in regular plasma current sheets, at long wavelengths. It is proposed that the presently observed fine ringlet structure of the Saturnian ring system is a relic of this process operating at cosmogonic times and breaking up the initial proto-ring (which may be regarded as an admixture of fine dust and plasma) into an ensemble of thin ringlets. It is shown that this instability developes at a rate that is many orders of magnitude faster than any other known insta- bility, when the disc thickness reaches a value that is comparable to its present observed value. Among the most exciting and significant discoveries made by the recent Voyagers 1 and 2 encounters with Saturn was the overall fine structure of the ring system. The classical pic- ture of a few more or less broad discs separated by gaps and discontinuities, based on Earth bound observations, has been replaced by the post encounter one wherein the ring system is seen to be composed of tens of thousands or more of extremely narrow ringlets, the narrowest of which have widths ~ 1 km (e.g., see Lane et aL, 1981). A few of these 'ringlets' are shown to be associated with spiral density waves that are similar to the waves believed to be responsible for the spiral structure of galaxies (Cuzzi et aL, 1981). A few others are shown to be associated with spiral bending waves (Shu et aL, 1983), of the type that are believed to be responsible for the warping of the discs of spiral galaxies (Hunter and Toomre, 1969). Both these types of waves are apparently excited by resonances with the various satellites of Saturn. Several other ringlets including a few isolated ones in the C-ring may also be associated with satellite resonances (J. B. Holberg, 1983, private communication; see also, Holberg et aL, 1982; or Esposito et al., 1983). However, all these account for less than one percent of all the observed ringlets. Clearly some other mechanism is required to explain the bulk of them. The hypothesis that 'shepherd' satellites were responsible for the confinement of the narrow rings of Uranus (Goldreich and Tremaine, 1979) gained credibility with the Voyager 1 discovery of two nearby small satellites on either side of the narrow F-ring of Saturn. Consequently, several authors (Lissauer et al., 1981; H6non, 1981) have postulated the existence of embedded moonlets in order to both confine the Saturnian ringlets and to clear the gaps between them. Incidentally, Dermott and Gold (1977) had proposed, in the Uranian context, that the rings could be held in place by a moonlet within the ring itself. In this" @default.
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- W2506139685 date "1983-01-01" @default.
- W2506139685 modified "2023-09-24" @default.
- W2506139685 title "THE FINE S TRUCTURE OF THE SATURNIAN R ING S YSTEM" @default.
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