Stability of Neptune's ring arcs in question

@article{Dumas1999StabilityON,
  title={Stability of Neptune's ring arcs in question},
  author={Christophe Dumas and Richard Terrile and Bradford A. Smith and Glenn Schneider and Eric Edward Becklin},
  journal={Nature},
  year={1999},
  volume={400},
  pages={733-735}
}
Although all four of the gas-giant planets in the Solar System have ring systems, only Neptune exhibits ‘ring arcs’—stable clumps of dust that are discontinuous from each other. Two basic mechanisms for confining the dust to these arcs have been proposed. The firstrelies on orbital resonances with two shepherding satellites, while the second invokes a single satellite (later suggested to be Galatea) to produce the observed ring arc structures. Here we report observations of the ring arcs and… 
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References

SHOWING 1-10 OF 26 REFERENCES
An Explanation for Neptune's Ring Arcs
TLDR
Analysis of Voyager data shows that a radial distortion with an amplitude of approximately 30 kilometers is traveling through the ring arcs, a perturbation attributable to the nearby satellite Galatea, and the arcs appear to be azimuthally confined by a resonant interaction with the same satellite.
Shepherding model for Neptune's arc ring
An incomplete arc ring has recently been discovered around Neptune1. Here, a model to explain the confinement of this ring is developed. The ring may be azimuthally confined near a triangular
Images of Neptune's ring arcs obtained by a ground-based telescope
Neptune has a collection of incomplete narrow rings, known as ring arcs, which should in isolation be destroyed by differential motion in a matter of months. Yet since first discovered by stellar
The Dynamics of the Neptunian Adams Ring's Arcs
We examine the resonant forcing of a narrow ringlet by a nearby satellite on an inclined, but circular, orbit. The general techniques that we develop are used to study the dynamics of Neptune's ring
Where Exactly Are the Arcs of Neptune
Abstract We show that periodic close encounters between Neptune's arc particles and the nearby satellite Galatea lead to a usually neglected secular perturbation on the osculating longitude at epoch
Collisional Simulations of Neptune's Ring Arcs
Abstract The currently accepted model for Neptune arc confinement relies on the radial and azimuthal confining perturbations due to the nearby satellite, Galatea. This model calls for arc particle
Occultation detection of a neptunian ring-like arc
The apparent closest approach of the star SAO186001 to Neptune was observed photoelectrically on 22 July 1984 at Cerro Tololo Inter-American Observatory. A 32% signal drop lasting about 1.2 s was
Neptune and Triton
The first reconnaissance of all the major planets of the Solar System culminated in the Voyager 2 encounter with Neptune in August 1989. Neptune itself was revealed as a planet with gigantic active
Orbits of the six new satellites of Neptune
Orbital elements are presented for the six small satellites of Neptune, 1989N1 through 1989N6, discovered by Voyager 2. Details of the image and orbit analyses are examined. The solution for the
Stellar Occultation Observations of Neptune's Rings: 1984-1988
Abstract Data from eight stellar occultations by Neptune between 1984 and 1988 are analyzed to set limits on the optical depths of the continuous Adams and Le Verrier Rings, and to search for
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