Profiling Saturn's rings by radio occultation

Details Profiling Saturn's rings by radio occultation Profiling Saturn's rings by radio occultation

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986icar...68..120m&link_type=abstract

Icarus (ISSN 0019-1035), vol. 68, Oct. 1986, p. 120-166. NASA-supported research.

Computer Science

56

Radio Occultation, Saturn Rings, Algorithms, Diffraction, Random Noise, Thermal Noise, Transmittance, Voyager 1 Spacecraft, Saturn, Rings, Radio Methods, Occultations, Diffraction, Wavelengths, Voyager 1 Mission, Stability, Opacity, Optical Properties, Structure, Ringlets, Gaps, Waves, Geometry, Diagrams, Parameters, Calculations, Comparisons, Encke Division, A Ring, C Ring, F Ring, Radius, Spacecraft Observations, Theoretical Studies

Scientific paper

Diffraction of radio waves is a prominent phenomenon in Voyager 1 radio occultation measurements of Saturn's rings. For Voyager at Saturn, phase instability limits radial resolution to values of about 200 m for optically thin rings. For more opaque rings, useful signal-to-noise ratios are the limiting factor: the resolution achieved at 3.6 cm λ is typically 200 - 400 m over Ring C and the Cassini Division, 1 - 4 km over Ring A, and is greater than about 4 km over Ring B. For Voyager 2 at Uranus, the achievable resolution at 3.6 cm λ should approach 30 m as long as the normal opacity does not exceed ≡2. Reconstructed profiles of limited regions of Saturn's rings illustrate the technique. These reveal a remarkable array of small-scale (≡1 km) ring structures. Profiles reconstructed over the full extent of the rings are available currently at 4.2 km and 900 m resolutions, and will be available presently at 400 m resolution.

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