A priority of space exploration: observation of Saturn's rings from a Saturn orbiter

1984 ◽  
Vol 75 ◽  
pp. 739-742
Author(s):  
André Brahic
Keyword(s):  
Complex System ◽  
Space Exploration ◽  
Ring System ◽  
Electromagnetic Properties ◽  
Small Particles ◽  
Saturn’S Rings ◽  
A Priority ◽  
Saturn's Rings ◽  
Phase Angles

AbstractObservations of Saturn’s ring by Voyager spacecrafts have revealed a much more complex system than expected. So many basical physical meehanisms are involved that more data are required. The logical next step after Voyager is the launch of an orbiter around Saturn. Significant improvements of our knowledge about the ring system could be obtained with the highest possible resolution, with observations with a large variety otf phase angles, with multiple occultation experiments, with observations of the evolution of selected area with time, and with observations of small particles phenomena and electromagnetic properties of the spokes.

Small particles and self-gravity wakes in Saturn's rings from UVIS and VIMS stellar occultations

Icarus ◽  
2016 ◽  
Vol 279 ◽  
pp. 36-50 ◽  
Author(s):  
Richard G. Jerousek ◽  
Joshua E. Colwell ◽  
Larry W. Esposito ◽  
Philip D. Nicholson ◽  
Matthew M. Hedman
Keyword(s):  
Small Particles ◽  
Stellar Occultations ◽  
Saturn’S Rings ◽  
Self Gravity ◽  
Saturn's Rings

A review of radar observations of Saturn’s rings

1984 ◽  
Vol 75 ◽  
pp. 49-55 ◽  
Author(s):  
Steven J . Ostro ◽  
Gordon H. Pettengill
Keyword(s):  
Ring System ◽  
Radar Observations ◽  
Jet Propulsion ◽  
Tracking Station ◽  
The Past ◽  
Microwave Radar ◽  
Radar Echoes ◽  
Saturn’S Rings ◽  
Saturn's Rings ◽  
Arecibo Observatory

Saturn’s rings are the most distant radar-detected planetary entity, and the only radar-detected ring system. Neither distinction is likely to be reinquished during this century.Ten years have passed since the initial detection of radar echoes from Saturn’s rings (Goldstein and Morris, 1973) shattered prevailing notions that typical ring particles were 0.1 to 1 mm in size. (The single fact that microwave radar echoes are detectable requires a substantial density of particles larger than about one centimeter.) During the past decade, additional radar studies of the rings have been conducted, using the λ13.5-cm and λ12.6-cm systems at the Jet Propulsion Laboratory’s Goldstone Tracking Station and the λ112.6-cm system at the National Astronomy and Ionosphere Center’s Arecibo Observatory.

Structure and dynamical processes in Saturn's rings

1984 ◽  
Vol 75 ◽  
pp. 393-395
Author(s):  
Richard J. Terrile
Keyword(s):  
High Resolution ◽  
Large Scale ◽  
Large Scale Structure ◽  
Ring Structure ◽  
Ring System ◽  
Scale Structure ◽  
Dynamical Processes ◽  
Saturn’S Rings ◽  
Saturn's Rings

The Voyager encounters have provided the first high resolution look at the Saturn ring system. Images of the rings reveal several classes of dynamical processes active in creating and maintaining large scale structure. These classes include variable ring features attributable to the influence of external satellite resonances, ring structure induced by the shepherding effects from external and possibly internal satellites, smooth eccentric ringlets contained within clear gaps in the ring and the dynamics of spokes which may represent a transient ring atmosphere.

Physical properties of Saturn's rings

1984 ◽  
Vol 75 ◽  
pp. 211-217 ◽  
Author(s):  
Jeffrey N. Cuzzi
Keyword(s):  
Particle Size ◽  
Radio Occultation ◽  
Particle Density ◽  
Bulk Material ◽  
Small Particles ◽  
Water Ice ◽  
Saturn’S Rings ◽  
Saturn's Rings ◽  
Classical Ring ◽  
Sharp Cutoff

A review is given of important features of the rings, touching only lightly on aspects covered by other speakers (Spokes, E ring). This extended abstract will only convey the high points of the talk.Most of the material in Saturn's rings is concentrated in the B ring, with a lesser amount in the A ring and only small amounts in the C ring and Cassini Division. There is a very different character to these classical ring regions; the C and Cassini particles are darker and more neutral in color; (Smith et al. 1981, 1982). The A and B regions contain nearly all of the “small” particles, from microns to millimeters. Overall, however, the particles are fairly well characterized by Voyager radio occultation results as roughly following an r-3powerlaw between about 1 cm and a few meters (Tyler et al. 1982, Marouf et al. 1982). A fairly sharp cutoff in the size distribution is seen at radii varying with location from about 1 to about 5 meters. The material of the ring particles is probably mostly water ice (see e.g., Pollack 1975) but the redness of the rings requires the presence of minor constitutents. Combinations of ground-based radar and radio emission observations (Pollack 1975, Cuzzi and Pollack 1978; Pettengill, this issue) strongly indicate that the non-icy component comprises a small fraction of the total bulk material. In fact, mass densities derived from density waves (e.g. Holberg et al. 1982) and CRAND measurements (Cooper et al. 1982) combined with Voyager particle size measurements indicate a particle density more like that of snow or frost than that of pure ice.

The stability of Saturn's rings

1951 ◽  
Vol 244 (874) ◽  
pp. 1-17 ◽  
Keyword(s):  
Small Particles ◽  
Saturnian System ◽  
Single Ring ◽  
Saturn’S Rings ◽  
The Stability ◽  
Conditions Of Stability ◽  
Saturn's Rings ◽  
Large Primary

Maxwell determined the conditions of stability of a single ring of small particles moving round a large primary. He also made some incomplete remarks on the effects of introducing a second ring. The present investigation considers in greater detail the stability of two rings of particles moving about a primary and subject to the gravitational attractions of the primary and of each other. It is shown that such a system, under conditions satisfied by the Saturnian system, is stable, the particles oscillating finitely about their mean positions. It is inferred that the Saturnian system, considered as a number of such rings, is therefore also stable.

scholarly journals Origin and Evolution of Saturn’s Rings

1983 ◽  
Vol 6 ◽  
pp. 435-442
Author(s):  
G.E. Morfill
Keyword(s):  
Ring System ◽  
Planetary Rings ◽  
Subsequent Evolution ◽  
Origin And Evolution ◽  
Saturn’S Rings ◽  
Saturn's Rings

AbstractThe formation of planetary rings is discussed in the context of formation theories of the gaseous planets. The subsequent evolution of Saturn’s ring system, both dynamically and mechanically, is described, and the consequences are compared with observations.

scholarly journals The cause of Encke's division in Saturn's ring

1922 ◽  
Vol 101 (710) ◽  
pp. 280-289 ◽  
Keyword(s):  
Satellite Orbit ◽  
Ring System ◽  
Satellite Orbits ◽  
Inner Radius ◽  
Saturn’S Rings ◽  
Saturn's Rings

In a former paper, the effect of satellites in producing divisions in Saturn’s Rings was discussed. The case taken was that where the satellite orbit and the rings were co-planar. The results afforded an explanation of the outer dimension of the Ring, Cassini’s Division, the inner radius of the bright ring, and the existence of the Crêpe Ring. But no reason was given for the existence of Encke’s Division, nor the numerous divisions reported by Lowell. In carrying the examination further, the fact that the satellite orbits are not precisely co-planar with the ring system must be considered. As given by the ‘Annuaire du Bureau des Longitudes,’ the inclination of the plane of the rings to the ecliptic is 28° 5·6', while the corresponding inclinations of the satellite orbits are— Mimas . . . . . . 27° 29·6', Dione . . . . . . 28° 4·4', Encelad us . . . 28° 4·3', Rhea . . . . . . 28° 22·8', Tethys . . . . . . 28° 40·5', Titan . . . . . . . 27° 39·7'. In the cases of Mimas, Tethys, and Titan, the differences are distinctly marked, the first being 36', or 0·01 of a radian. The effect of this inclination is examined in the sequel.

Comments on collision mechanics in ring systems

1984 ◽  
Vol 75 ◽  
pp. 407-422
Author(s):  
William K. Hartmann
Keyword(s):  
Asteroid Belt ◽  
Surface Erosion ◽  
Surface Layers ◽  
Ring Systems ◽  
Eclipse Observations ◽  
Saturn’S Rings ◽  
Saturn's Rings

ABSTRACTThe nature of collisions within ring systems is reviewed with emphasis on Saturn's rings. The particles may have coherent icy cores and less coherent granular or frosty surface layers, consistent with thermal eclipse observations. Present-day collisions of such ring particles do not cause catastrophic fragmentation of the particles, although some minor surface erosion and reaccretion is possible. Evolution by collisional fragmentation is thus not as important as in the asteroid belt.

Voyager UVS observations of stellar occultations by the rings of Saturn

1984 ◽  
Vol 75 ◽  
pp. 265-277
Author(s):  
J.B. Holbelg ◽  
W.T. Forrester
Keyword(s):  
Optical Depth ◽  
Distance Scale ◽  
Density Waves ◽  
Ring Density ◽  
Stellar Occultations ◽  
Saturn’S Rings ◽  
Saturn's Rings

ABSTRACTDuring the Voyager 1 and 2 Saturn encounters the ultraviolet spectrometers observed three separate stellar occultations by Saturn's rings. Together these three observations, which sampled the optical depth of the rings at resolutions from 3 to 6 km. can be used to establish a highly accurate distance scale allowing the identification of numerous ring features associated with resonances due to exterior satellites. Three separate observations of an eccentric ringlet near the location of the Titan apsidal resonance are discussed along with other ringlet-resonance associations occurring in the C ring. Density waves occurring in the A and B rings are reviewed and a detailed discussion of the analysis of one of these features is presented.

Profiling Saturn's rings by radio occultation

Icarus ◽  
1986 ◽  
Vol 68 (1) ◽  
pp. 120-166 ◽  
Author(s):  
Essam A. Marouf ◽  
G. Leonard Tyler ◽  
Paul A. Rosen
Keyword(s):  
Radio Occultation ◽  
Saturn’S Rings ◽  
Saturn's Rings
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