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Published February 1982 | Published
Journal Article Open

Radial widths, optical depths, and eccentricities of the Uranian rings

Abstract

Observations of the stellar occultation by the Uranian rings of 15/16 August 1980 are used to estimate radial widths and normal optical depths for segments of rings 6, 5, 4, ɑ, β, η, y, and δ. Synthetic occultation profiles are generated to match the observed light curves. A review of published data confirms the existence of width-radius relations for rings ɑ and β, and indicates that the optical depths of these two rings vary inversely with their radial widths. Masses are obtained for rings ɑ and β, on the assumption that differential precession is prevented by their self-gravity. A quantitative comparison of seven є-ring occultation profiles obtained over a period of 3.4 yr reveals a consistent structure, which may reflect the presence of unresolved gaps and subrings. Elliptical models for rings 6, 5, 4, ɑ, β, and є are presented for comparison with the results of previous studies, particularly that of Elliot et al. (1981a).

Additional Information

© 1982 American Astronomical Society. Received 15 June 1981; revised 5 October 1981. 0bservations were made at Las Campanas Observatory as part of a joint agreement between the California Institute of Technology and the Carnegie Institution of Washington. The authors gratefully acknowledge the assistance of the staff of the Las Campanas Observatory in making the observations. The discussion in Sec. VI has benefited considerably from a detailed critique by J. L. Elliot, who also provided certain results in advance of publication. This research was supported in part by a NASA grant.

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Published - 1982AJ_____87__433N.pdf

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August 22, 2023
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