A model of dust production in the Neptune ring system
Abstract
Voyager 2 images of the Neptunian ring system show it to be relatively dusty with the fraction of micron-sized dust particles in the rings between about 0.2 and 0.7 (Smith et al 1989). We apply a numerical model developed for the dust bands (Colwell and Esposito, Icarus (in press)) to the Neptune system. Our results show that 1) the suggested distribution of dust fractions in the rings is not related to ring optical depth and may be due to different ring particle size distributions. 2) Collision velocities between the macroscopic ring particles must be ∼ 1 m/sec if they are to produce im fractions above 1/2. 3) The small moons of Neptune have regoliths for meteoroid excavation to produce the dust population at Voyager ring plane crossing. 4) Dust optical depths interior to 1989N3R are negligible unless there are macroscopic source bodies in that region.
- Publication:
-
Geophysical Research Letters
- Pub Date:
- September 1990
- DOI:
- 10.1029/GL017i010p01741
- Bibcode:
- 1990GeoRL..17.1741C
- Keywords:
-
- Astronomical Models;
- Neptune (Planet);
- Planetary Rings;
- Uranus (Planet);
- Voyager 2 Spacecraft;
- Cosmic Dust;
- Neptune Satellites;
- Regolith;
- Planetology: Fluid Planets: Rings and dust;
- Planetology: Solid Surface Planets and Satellites: Cratering;
- Planetology: Solid Surface Planets and Satellites: Surfaces;
- Planetology: Fluid Planets: Origin and evolution