paper

The Uranus System from Occultation Observations (1977-2006): Rings, Pole Direction, Gravity Field, and Masses of Cressida, Cordelia, and Ophelia

arXiv:2401.04634

Abstract

From 31 Earth-based and three Voyager 2 occultations spanning 1977--2006, we determine the orbital elements of the nine main Uranian rings with typical RMS residuals of 0.2 -- 0.4 km and 1- errors in and of order 0.1 km, registered on an absolute radius scale accurate to 0.2 km at the 2- level. The ring shows more substantial scatter. In addition to the free modes in the ring and in the ring, we find two additional outer Lindblad resonance (OLR) modes ( and ) and a possible inner Lindblad resonance (ILR) mode in the ring. No normal modes are detected for rings 6, 5, 4, , or . Five normal modes are forced by small moonlets: the 3:2 inner ILR of Cressida with the ring, the 6:5 ILR of Ophelia with the ring, the 23:22 ILR of Cordelia with the ring, the 14:13 ILR of Ophelia with the outer edge of the ring, and the counterpart 25:24 OLR of Cordelia with the ring's inner edge. We determine the width-radius relations for nearly all of the detected mode. We find no convincing evidence for librations of any of the rings. The Uranus pole direction at epoch TDB 1986 Jan 19 12:00 is and . We determine the zonal gravitational coefficients , and fixed at , with a correlation coefficient , for a reference radius 25559 km. From the amplitudes and resonance radii of normal modes forced by moonlets, we determine the masses of Cressida, Cordelia, and Ophelia. Their estimated densities decrease systematically with increasing orbital radius and generally follow the radial trend of the Roche critical density for a shape parameter .

94 pages, 53 figures