Rings of Jupiter
The planet Jupiter has a system of rings known as the rings of Jupiter or the Jovian ring system. The main and halo rings consist of dust ejected from the moons Metis, Adrastea, and other unobserved parent bodies as the result of high-velocity impacts. In visible and near-infrared light, the rings have a reddish color, except the halo ring, which is neutral or blue in color.
About Rings of Jupiter in brief
The planet Jupiter has a system of rings known as the rings of Jupiter or the Jovian ring system. It was the third ring system to be discovered in the Solar System, after those of Saturn and Uranus. The main and halo rings consist of dust ejected from the moons Metis, Adrastea, and other unobserved parent bodies as the result of high-velocity impacts. In visible and near-infrared light, the rings have a reddish color, except the halo ring, which is neutral or blue in color. The age of the ring system is not known, but it may have existed since the formation of Jupiter. A ring could possibly exist in Himalia’s orbit. One possible explanation is that a small moon had crashed into Himalia and the force of the impact caused material to blast off Himalia. The appearance of the main ring depends on the viewing geometry. In forward-scattered light all Jovan rings are especially bright. The brightness continues to increase in the direction of Jupiter and has a maximum near the ring’s center at 126,000 km, although there is a pronounced gap near the Metidian orbit at 128,000 km. There is a thin ringlet just outside the orbit of Metis. The third ringlet is found inward, outside the central gap of the central Metis orbit, and is found to consist of two different parts: a narrow part extending from 128,.000 to 129,000km, which includes three narrow, narrow ringlets.
The outer boundary of themain ring, located at 129,100 km,. or slightly beyond the orbit of Adrasto, is very thin. The size of the dust in the rings varies, but the cross-sectional area is greatest for nonspherical particles of radius about 15 μm in all rings except halo. The haloRing is probably dominated by submicrometre dust. It is probably in the range of 1011 to 1016 kg. The principal attributes of the known Jovain Rings are listed in the table. The ring system was first observed in 1979 by the Voyager 1 space probe and thoroughly investigated in the 1990s by the Galileo orbiter. It has also been observed by the Hubble Space Telescope and from Earth for several years. The total mass of thering system is poorly known, but is likely to be between 1011 and 1016 kg. It includes two wide, thick and faint outer \”gossamer rings\”, named for the moons of whose material they are composed: Amalthea and Thebe. It also includes a narrow ringlet extending from 127,000 to 127,500 km and three outer ringlets, which include three narrow parts which include a narrow and narrow part of the outer ringlet which includes two narrow parts of the inner ring. The inner ring is not marked by any satellite and is located at about 122,500 km. Thus the width of theMain ring is around 6, 500 km.
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This page is based on the article Rings of Jupiter published in Wikipedia (as of Nov. 07, 2020) and was automatically summarized using artificial intelligence.
