Uranian ring orbits from earth-based and Voyager occultation observations
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Cited by (77)
Uranus ring occultation observations: 1977–2006
2023, IcarusNoncircular features in saturn's rings II: The C ring
2014, IcarusCitation Excerpt :The identification of numerous normal modes co-existing on the sharp edges of ringlets and gaps is probably the most important new result of the present study. Although such modes had been seen in the very narrow Uranian γ and δ rings (French, 1988a), where they extend across the entire width of each ring, only the outer edge of the B ring has been previously known to exhibit what we may call “edge modes” (Spitale and Porco, 2010; Nicholson et al., 2014). The distribution of modes is in excellent agreement with theoretical predictions, with ILR-type modes on outer ringlet (and inner gap) edges and OLR-type modes on inner ringlet (and outer gap) edges, as illustrated in Figs. 16 and 17.
Noncircular features in Saturn's rings I: The edge of the B ring
2014, IcarusCitation Excerpt :All of our orbit fits were carried out using a well-tested nonlinear least-squares routine, based on the Leavenberg–Marquardt algorithm. This routine is essentially that same as that used by French et al. (1988) for their fits to Uranian ring occultation data, by French et al. (1993) to fit the 28 Sgr data for Saturn’s rings, and most recently by French et al. (2010) to study features in the Cassini Division. The underlying geometric model is the heliocentric calculation documented in Appendix B of French et al. (1993).
Keck and VLT AO observations and models of the uranian rings during the 2007 ring plane crossings
2013, IcarusCitation Excerpt :These calculations were all performed for a viewing geometry similar to that of Uranus in July 2004, i.e., a ring opening angle of ∼11°. Of particular note for the present paper is the relative insensitivity of the I/F on the precise value of τ0 for the main rings, since τ0 > 0.15 (Stone and Miner, 1986; French et al., 1988) and, given the relatively small ring opening angles, the effective line-of-sight optical depth under these conditions is very large. We therefore keep τ0 fixed for the main rings, leaving as free parameters only their location and radial extent.
- 1
Now at Department of Astronomy, Wellesley College, Wellesley, MA 02181.
- 2
Guest Observer, Cerro Tololo Interamerican Observatory, La Serena, Chile.
- 3
Now at the Department of Physics and Astronomy.