A granular flow model for dense planetary rings

Details A granular flow model for dense planetary rings A granular flow model for dense planetary rings

Sep 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icar...63..406b&link_type=abstract

Icarus (ISSN 0019-1035), vol. 63, Sept. 1985, p. 406-420.

Physics

84

Flow Characteristics, Particle Collisions, Planetary Rings, Rotating Disks, Angular Momentum, Atmospheric Models, Density Wave Model, Kinematics, Luminosity, Perturbation Theory, Solids Flow, Viscous Flow, Planets, Rings, Models, Flow, Density, Viscosity, Particles, Rotation, Disk, Pressure, Hydrodynamics, Kinetics, Collisions, Density Waves, Perturbations, Origin, Ellipicity, Ringlets, Features, B Ring, Saturn, Uranus, Kinematics, Calculations, Liquids, Energy, Angular Momentum, Luminosity, Damping, Width,

Scientific paper

The authors study the viscosity of a differentially rotating particle disk in the limiting case where the particles are densely packed and their collective behavior resembles that of a liquid. The pressure tensor is derived from the equations of hydrodynamics and from a simple kinetic model of collisions described by Haff (1983). They find that density waves and narrow circular rings are unstable if the liquid approximation applies. The resulting development of nonlinear perturbations may give rise to "splashing" of the ring material in the vertical direction. These results may help in understanding the origin of the ellipticities of ringlets, the nonaxisymmetric features near the outer edge of the Saturnian B ring, and the unexplained residuals in kinematic models of the Saturnian and Uranian rings.

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