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12 - Dusty Rings

from III - Ring Systems by Type and Topic

Published online by Cambridge University Press:  26 February 2018

By
M. M. Hedman ,
F. Postberg ,
D. P. Hamilton ,
S. Renner  and
H.-W. Hsu
Edited by
Matthew S. Tiscareno  and
Carl D. Murray
M. M. Hedman
Affiliation:
University of Idaho Moscow, Idaho, USA
F. Postberg
Affiliation:
University of Heidelberg Heidelberg, GERMANY
D. P. Hamilton
Affiliation:
University of Maryland College Park, Maryland, USA
S. Renner
Affiliation:
University of Lille Lille, FRANCE
H.-W. Hsu
Affiliation:
University of Colorado Boulder, Colorado, USA
Matthew S. Tiscareno
Affiliation:
SETI Institute, California
Carl D. Murray
Affiliation:
Queen Mary University of London
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Summary

All of the giant planets in the outer Solar System possess rings composed primarily of particles less than 100 microns across. Such small particles are conventionally referred to as “dust grains” regardless of their composition, and so these rings are considered “dusty rings” (as opposed to the more famous main rings of Saturn and Uranus, whose particles are more than a millimeter across). Dusty rings are often very tenuous and so can be much more difficult to observe than Saturn's broad, bright, and dense main rings. Nevertheless, dusty rings are extremely interesting because they have very rich dynamics and are extremely sensitive probes of their environment.

The high surface-area-to-volume ratio of dust-sized grains makes them much more responsive to non-gravitational forces like solar radiation pressure, plasma drag, and torques from the planet's electromagnetic field. Furthermore, sub-millimeter particles can be lost from the ring system on relatively short timescales due to erosion via charged-particle and micrometeoroid bombardment or through ejection by the non-gravitational forces listed above. This means that small particles need to be constantly supplied to these rings from larger bodies, and indeed all of the known dusty rings are associated with larger objects that are the likely sources of dusty debris. The most dramatic example of this is Saturn's E ring, which is clearly supplied by material erupting from beneath the surface of the geologically active moon Enceladus. However, this is a special case, and most dusty rings are instead associated with denser rings (which are composed primarily of millimeter-to-metersized particles) or small moons. These objects can serve as dust sources because they are constantly being bombarded by micrometeoroids, and these impacts release fine debris that can escape the weak gravitational fields of these small bodies and go into orbit around the planet. Note that the amount of dust released by this process depends on the size, mass, and regolith properties of the source object, and calculations of the dust production rate based on simple estimates of impact ejecta velocity distributions suggest that source moons that are several kilometers across are the most efficient at producing dusty rings (Burns et al., 1999).

Type
Chapter
Information
Planetary Ring Systems
Properties, Structure, and Evolution
 , pp. 308 - 337
Publisher: Cambridge University Press
Print publication year: 2018

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