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A salt-water reservoir as the source of a compositionally stratified plume on Enceladus
Whereas previous Cassini observations were compatible with a variety of plume formation mechanisms, these data eliminate or severely constrain non-liquid models and strongly imply that a salt-water reservoir with a large evaporating surface provides nearly all of the matter in the plume. Expand
Sodium salts in E-ring ice grains from an ocean below the surface of Enceladus
The identification of a population of E-ring grains that are rich in sodium salts, which can arise only if the plumes originate from liquid water, and the abundance of various salt components in these particles exhibit a compelling similarity to the predicted composition of a subsurface Enceladus ocean in contact with its rock core. Expand
Slow dust in Enceladus' plume from condensation and wall collisions in tiger stripe fractures
It is shown that repeated wall collisions of grains, with re-acceleration by the gas, induce an effective friction, offering a natural explanation for the reduced grain velocity, and suggests liquid water below Enceladus’ south pole. Expand
The E ring in the vicinity of Enceladus - I. Spatial distribution and properties of the ring particles
Abstract Saturn's diffuse E ring is the largest ring of the Solar System and extends from about 3.1 R S (Saturn radius R S = 60 , 330 km ) to at least 8 R S encompassing the icy moons Mimas,Expand
Plasma, plumes and rings: Saturn system dynamics as recorded in global color patterns on its midsize icy satellites
New global maps of the five inner midsize icy saturnian satellites, Mimas, Enceladus, Tethys, Dione, and Rhea, have been constructed in three colors (UV, Green and near-IR) at resolutions of 1Expand
Cassini Dust Measurements at Enceladus and Implications for the Origin of the E Ring
During Cassini's close flyby of Enceladus on 14 July 2005, the High Rate Detector of the Cosmic Dust Analyzer registered micron-sized dust particles enveloping this satellite; this asymmetric signature is consistent with a locally enhanced dust production in the south polar region of Encesladus. Expand
How the Enceladus dust plume feeds Saturn’s E ring
Abstract Pre-Cassini models of Saturn’s E ring [Horanyi, M., Burns, J., Hamilton, D., 1992. Icarus 97, 248–259; Juhasz, A., Horanyi, M., 2002. J. Geophys. Res. 107, 1–10] failed to reproduce itsExpand
Viscous Overstability in Saturn's B-Ring: II. Hydrodynamic Theory and Comparison to Simulations
We investigate the viscous oscillatory instability (overstability) of an unperturbed dense planetary ring, an instability that might play a role in the formation of radial structure in Saturn’sExpand
A belt of moonlets in Saturn’s A ring
Embedded moonlets found in Saturn’s A ring are probably the remnants of a shattered ring-moon of Pan size or larger, locally contributing new material to the older ring, which supports the theory of catastrophic ring creation in a collisional cascade. Expand
Viscous Overstability in Saturn's B Ring I. Direct Simulations and Measurement of Transport Coefficients
Local simulations with up to 60,000 self-gravitating dissipatively colliding particles indicate that dense unperturbed ring systems with optical depth ?> 1 can exhibit spontaneous viscous oscillatoryExpand