Other
Scientific paper
May 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000dda....31.0806m&link_type=abstract
American Astronomical Society, DDA Meeting #31, #08.06; Bulletin of the American Astronomical Society, Vol. 32, p.865
Other
Scientific paper
The leading model to account for the apse-alignment of the eccentric Uranian rings relies on the ring self-gravity alone to counter differential precession (in the case of m = 1 modes), and differential rotation (for all other m modes). In this model, the role of the ring viscosity is simply to produce a small apsidal shift between the inner and the outer ring streamlines. While ring observations have qualitatively confirmed several of its predictions, such as increasing eccentricity with streamline semi-major axis and small, negative apsidal shifts, the self-gravity model yields ring mass estimates based on the observed ring state severely at odds with observational mass estimates based on radio occultation constraints of particle sizes. Here we introduce a fluid pressure correction applicable to a highly collisional, compresible fluid with low particle velocity dispersion and finite particle sizes. In particular, we model a ring state where the particles are locked in their relative positions and jammed against their neighbors, and the velocity dispersion is so low that collisions are nearly elastic. We then find an equilibrium solution such that the ring self-gravity maintains apse-alignment not only against differential precession but the fluid pressure as well. We apply this model to the Uranian alpha ring, and show that, compared to the previous self-gravity model, it can increase the mass estimate for this ring by an order of magnitude.
Estrada Paul R.
Mosqueira Ignacio
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