Photographed by Voyager 2 in 1986
|Discovered by||William Herschel|
|Discovery date||March 13, 1781|
Average orbital speed
|6.80 km/s (15,200 mph; 24,500 km/h)|
|Inclination||0.773° to ecliptic|
6.48° to Sun's equator
1.02° to invariable plane
The planet is made of ice, gases and liquid metal. Its atmosphere contains hydrogen (1H), helium (2He) and methane. The temperature on Uranus is −197 °C (−322.6 °F; 76.1 K) near the top of its atmosphere, but its small solid core (about 55% the mass of Earth) is probably about 4,730 °C (8,540 °F; 5,000 K).
The distance between Uranus and the Sun is about 2.8 billion km. Uranus completes its orbit around the Sun in 84 earth years. It completes a spin around itself in 17 hours and 14 minutes. This means there are about 43,000 Uranian days in one Uranian year.
Moons[change | change source]
Uranus has 27 known moons. They are named for characters from the works of Shakespeare and Alexander Pope. The five biggest moons are Miranda, Ariel, Umbriel, Titania and Oberon. Many moons have yet to be discovered.
Exploring[change | change source]
Clouds[change | change source]
Uranus is covered in blue clouds. The top clouds, made of methane, are difficult to see. Lower clouds are thought to be frozen water. There are also violent storms. Wind speeds can reach 250 metres per second (900 km/h; 560 mph). Scientists are studying the clouds to try to understand the storms on the planet.
Rings[change | change source]
The planet Uranus has a system made of 13 rings which is far fewer than the rings of Saturn but more than those around Jupiter and Neptune. The rings of Uranus were discovered in 1977. More than 200 years ago, William Herschel also reported observing rings, but modern astronomers do not believe that he saw them, because they are very dark and faint. Two additional rings were discovered in 1986 in images taken by Voyager 2, and two outer rings were found in 2003–2005 by the Hubble Space Telescope. The rings are probably mainly composed of frozen water.
The rings of Uranus are thought to be relatively young, not more than 600 million years old. The Uranian ring system probably began from the collisional fragmentation of moons that once existed around the planet. After colliding, the moons probably broke up into many particles, which survived as narrow, optically dense rings only in zones of maximum stability.
General properties[change | change source]
The ring system of Uranus has thirteen distinct rings. In order of increasing distance from the planet they are: 1986U2R/ζ, 6, 5, 4, α, β, η, γ, δ, λ, ε, ν, μ rings. They can be divided into three groups: nine narrow main rings (6, 5, 4, α, β, η, γ, δ, ε), two dusty rings (1986U2R/ζ, λ) and two outer rings (μ, ν). The rings of Uranus consist mainly of macroscopic particles and little dust, although dust is known to be present in 1986U2R/ζ, η, δ, λ, ν and μ rings.
In addition to these well-known rings, there may be numerous optically thin dust bands and faint rings between them. These faint rings and dust bands may exist only temporarily. Some of them became visible during a series of ring plane-crossing events in 2007. A number of dust bands between the rings were observed in forward-scattering [a] geometry by Voyager 2. All rings of Uranus show azimuthal brightness variations.
The rings are made of an extremely dark material. The rings are slightly red in the ultraviolet and visible parts of the spectrum and grey in near-infrared. They show no identifiable spectral features. The chemical composition of the ring particles is not known. However, they cannot be made of pure water ice like the rings of Saturn because they are too dark, darker than the inner moons of Uranus. This shows that they are probably a mixture of the ice and a dark material. The nature of this material is not clear, but it may be organic compounds considerably darkened by the charged particle irradiation from the Uranian magnetosphere. The rings' particles may consist of a heavily processed material which was initially similar to that of the inner moons.
As a whole, the ring system of Uranus is unlike either the faint dusty rings of Jupiter or the broad and complex rings of Saturn, some of which are composed of very bright material—water ice. However, there are similarities with some parts of the latter ring system; the Saturnian F ring and the ε ring are both narrow, relatively dark and are shepherded by a pair of moons. The newly discovered outer rings of Uranus are similar to the outer G and E rings of Saturn. Narrow ringlets existing in the broad Saturnian rings also resemble the narrow rings of Uranus. In addition, dust bands observed between the main rings of Uranus may be similar to the rings of Jupiter. In contrast, the Neptunian ring system is quite similar to that of Uranus, although it is less complex, darker and contains more dust. The Neptunian rings are also positioned further from the planet.
Orbit and rotation[change | change source]
Uranus revolves around the Sun once every 84 Earth years. Its average distance from the Sun is roughly 3 billion km (about 20 AU). The intensity of sunlight on Uranus is about 1/400 that on Earth. Its orbital elements were first calculated in 1783 by Pierre-Simon Laplace. With time, discrepancies began to appear between the predicted and observed orbits, and in 1841, John Couch Adams first proposed that the differences might be due to the gravitational tug of an unseen planet. In 1845, Urbain Le Verrier began his own independent research into Uranus's orbit. On September 23, 1846, Johann Gottfried Galle found a new planet, later called Neptune, at nearly the position predicted by Le Verrier.
The rotational period of the interior of Uranus is 17 hours, 14 minutes, clockwise (retrograde). As on all giant planets, its upper atmosphere experiences very strong winds in the direction of rotation. At some latitudes, such as about two-thirds of the way from the equator to the south pole, visible features of the atmosphere move much faster, making a full rotation in as little as 14 hours.
Related pages[change | change source]
References[change | change source]
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- Burkert 2005, p. 295. sfn error: no target: CITEREFBurkert2005 (help)
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- "NASA's Hubble discovers new rings and moons around Uranus". Hubblesite. 2005. Retrieved June 9, 2007. CS1 maint: discouraged parameter (link)
- de Pater, Imke; Hammel H.B.; et al. (2007). "The dark side of the rings of Uranus". Science. 317 (5846): 1888–1890. doi:10.1126/science.1148103. PMID 17717152.
- Baines, Kevin H.; et al. (1998). "Near-Infrared absolute photometric imaging of the Uranian system". Icarus. 132: 266–284. doi:10.1006/icar.1998.5894.
- "Next Stop Uranus". 1986. Retrieved June 9, 2007. CS1 maint: discouraged parameter (link)
- Forbes, George 1909. History of Astronomy.
- O'Connor J.J. and Robertson E.F. (1996). "Mathematical discovery of planets". Retrieved June 13, 2007. CS1 maint: discouraged parameter (link)
- Peter J. Gierasch and Philip D. Nicholson (2004). "Uranus". NASA World Book. Archived from the original on August 11, 2011. Retrieved June 9, 2007. CS1 maint: discouraged parameter (link)
- These are the mean elements from VSOP87, together with derived quantities.
- Calculated using data from Seidelmann, 2007.
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- NASA's Uranus fact sheet
- Uranus Profile by NASA's Solar System Exploration
- Keck pictures of Uranus show best view from the ground Archived 2007-11-16 at the Wayback Machine — Press release with some photographs showing rings, satellites and clouds
- News reports of December 22, 2005 rings and moons discovery
- Planets—Uranus A kid's guide to Uranus.
- Uranus (planet) -Citizendium