Neptune's rings

Neptune's rings

Four dark planetary rings around Neptune, discovered in 1976 during close observation of an occultation of a star by Neptune and confirmed during the Voyager 2 flyby in 1989 (see table). The Adams and Le Verrier rings are quite thin. The Adams ring has several brighter arcs of material, first observed from Earth. Two broad rings, Galle and Plateau, are diffuse sheets of fine particles. The Plateau has a brighter edge at a distance of about 57 500 km from the planet.
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He said Jupiter's rings are made up of particles about a thousandth of a millimeter in diameter each, while Neptune's rings are almost entirely made of dust.
Neptune's rings are also mostly dust, and even Uranus has broad sheets of dust between its narrow main rings.
By comparison, Jupiter's rings contain mostly small, micron-sized particles, Neptune's rings are also mostly dust, and even Uranus has broad sheets of dust between its narrow main rings.
Each has a family of small moons and a set of dark rings (Neptune's rings were suspected, then confirmed by Voyager 2).
Neptune's rings clump together into arcs while the ones around Uranus possibly reach down into its atmosphere.
Neptune's Rings "On May loth of last year, a handful of widely scattered observing teams witnessed an occultation by Neptune; as it turned out, two weeks later another occultation by the same planet was observed from Cerro Tololo in Chile.
From afar, Neptune's rings look like partial "ring arcs," seemingly interrupted in places as they circled the planet.
Mark Showalter, from the SETI Institute, discovered the Moon in a series of images of Neptune's rings, notes the NASA release.
Only Neptune's rings have been previously observed to have persistent arcs, and there also a resonance is probably responsible for preventing particles from spreading around the ring's circumference.
Beginning in 1980, Neptune's rings were detected by ground-based and airborne telescopic observations of stellar occultations.