Other
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dda....41.1107s&link_type=abstract
American Astronomical Society, DDA meeting #41, #11.07; Bulletin of the American Astronomical Society, Vol. 41, p.940
Other
Scientific paper
Although it is common practice to model the damping of linear density waves Saturn's rings as a Newtonian viscous fluid, the complicated multimodal and time dependent behavior of the other edge of the B ring would appear to require a more complicated rheology. Local N-body simulations of a dense ring demonstrate that the rate of angular momentum transport is mediated by gravitational interactions between clumps of particles that are radially separated by the Toomre wavelength for axisymmetric gravitational instabilities. The measured angular momentum transport is also varies irregularly in time even when averaged over a simulation cell that is close to a square kilometer in area. Near the outer edge of the B ring, the scale of particle clumping becomes so large that the non-uniformity of the surface density is visible in the higher resolution Cassini images. As the scale of the clump size and orbital separation increases, the time required to achieve a steady-state effective viscosity also increases.
A theoretical expression for the viscous transport in a dense ring will be presented that allows for non-uniformity in time and space. This expression predicts a viscoelastic response when the ring is strongly forced on an orbital time scale.
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