View source for Astronomy:Umbriel (moon)

{{short description|Moon of Uranus}}
{{Infobox planet
| name               = Umbriel
| alt_names          = 
| mpc_name           = Uranus II
| pronounced         = {{IPAc-en|ˈ|ʌ|m|b|r|i|ə|l}}<ref name="dict-def" />
| adjectives         = Umbrielian
| image              = PIA00040 Umbrielx2.47.jpg
| image_scale         =
| image_alt          = A round spherical body with its left half illuminated. The surface is dark and has a low contrast. There are only a few bright patches. The terminator is slightly to the right from the center and runs from the top to bottom. A large crater with a bright ring on its floor can be seen at the top of the image near the terminator. A pair of large craters with bright central peaks can be seen along the terminator in the upper part of the body. The illuminated surface is covered by a large number of craters.
| caption            = Umbriel as seen by ''Voyager 2'' in 1986. At the top is the large crater [[Astronomy:Wunda (crater)|Wunda]], whose walls enclose a ring of bright material.
| discoverer         = William Lassell
| discovered         = October 24, 1851
| orbit_ref          =<ref name="orbit" />
| semimajor          = {{val|266000|u=km}}
| eccentricity       = {{val|0.0039}}
| period             = {{val|4.144|u=[[Day|d]]}}
| avg_speed          = 4.67 km/s (calculated)
| inclination        = {{val|0.128|u=°}} (to Uranus's equator)
| satellite_of       = [[Astronomy:Uranus|Uranus]]
| mean_radius        = {{val|584.7|2.8|u=km}} (0.092 Earths)<ref name="Thomas 1988" />
| surface_area       = {{val|4296000|u=km2}} (0.008 Earths){{efn|name=surface area|Surface area derived from the radius ''r'' : <math>4\pi r^2</math>.}}
| volume             = {{val|837300000|u=km3}} (0.0008 Earths){{efn|name=volume|Volume ''v'' derived from the radius ''r'' : <math>4\pi r^3/3</math>.}}
| mass               = {{val|1.275|0.028|e=21|u=kg}}<ref name="Jacobson 2014">R. A. Jacobson (2014) 'The Orbits of the Uranian Satellites and Rings, the Gravity Field of the Uranian System, and the Orientation of the Pole of Uranus'. ''The Astronomical Journal'' 148:5</ref>
| density            = {{val|1.39|0.16|u=g/cm3}}<ref name="Jacobson Campbell et al. 1992" />
| surface_grav       = {{Gr|1.275|584.7|2}} [[Physics:Acceleration|m/s<sup>2</sup>]] (~&nbsp;0.023 [[Physics:G-force|g]]){{efn|name=surface gravity|Surface gravity derived from the mass ''m'', the [[Physics:Gravitational constant|gravitational constant]] ''G'' and the radius ''r'' : <math>Gm/r^2</math>.}}
| escape_velocity    = {{V2|1.275|584.7|2}} km/s{{efn|name=escape velocity|Escape velocity derived from the mass ''m'', the [[Physics:Gravitational constant|gravitational constant]] ''G'' and the radius ''r'' : <math>\sqrt{\frac{2Gm}{r} }</math>.}}
| rotation           = presumed synchronous<ref name="Smith Soderblom et al. 1986" />
| axial_tilt         = 0<ref name="Smith Soderblom et al. 1986" />
| albedo =
{{plainlist |
* 0.26 (geometrical)
* 0.10 (Bond)<ref name="Karkoschka 2001, Hubble" />
}}
| magnitude          = 15.1<ref>{{cite web|url=https://britastro.org/2021/observers-challenge-the-moons-of-uranus|title=Observer's Challenge – The Moons of Uranus|author=Andy Wilson|publisher=British Astronomical Association|access-date=2023-03-01|date=December 1, 2021}}</ref>
| temp_name1         = solstice<ref name="Grundy Young et al. 2006" />
| mean_temp_1        = ≈&thinsp;75&nbsp;[[Kelvin|K]]
| max_temp_1         = 85&nbsp;K
| min_temp_1         = ?
| atmosphere         = no
| surface_pressure   = zero (presumed to be extremely low)
| note               = no
}}

'''Umbriel''' {{IPAc-en|ˈ|ʌ|m|b|r|i|ə|l}} is a [[Astronomy:Moons of Uranus|moon of Uranus]] discovered on October 24, 1851, by William Lassell. It was discovered at the same time as [[Astronomy:Ariel (moon)|Ariel]] and named after a character in Alexander Pope's 1712 poem ''The Rape of the Lock''. Umbriel consists mainly of [[Earth:Ice|ice]] with a substantial fraction of [[Earth:Rock (geology)|rock]], and may be differentiated into a rocky core and an icy [[Earth:Mantle (geology)|mantle]]. The surface is the darkest among Uranian moons, and appears to have been shaped primarily by impacts. However, the presence of canyons suggests early endogenic processes, and the moon may have undergone an early endogenically driven resurfacing event that obliterated its older surface.

Covered by numerous [[Astronomy:Impact crater|impact crater]]s reaching {{convert|210|km|mi|abbr=on}} in diameter, Umbriel is the second most heavily cratered satellite of Uranus after [[Astronomy:Oberon (moon)|Oberon]]. The most prominent surface feature is a ring of bright material on the floor of [[Astronomy:Wunda (crater)|Wunda]] crater. This moon, like all moons of Uranus, probably formed from an [[Astronomy:Accretion disk|accretion disk]] that surrounded the planet just after its formation. The Uranian system has been studied up close only once, by the spacecraft ''[[Astronomy:Voyager 2|Voyager 2]]'' in January 1986. It took several images of Umbriel, which allowed mapping of about 40% of the moon's surface.

== Discovery and name ==
Umbriel, along with another Uranian satellite, [[Astronomy:Ariel (moon)|Ariel]], was discovered by William Lassell on October 24, 1851.<ref name="Lassell 1851" /><ref name="Lassell, letter 1851" /> Although William Herschel, the discoverer of [[Astronomy:Titania (moon)|Titania]] and [[Astronomy:Oberon (moon)|Oberon]], claimed at the end of the 18th century that he had observed four additional moons of Uranus,<ref name="Herschel 1798" /> his observations were not confirmed and those four objects are now thought to be spurious.<ref name="Struve 1848" />

All of Uranus's moons are named after characters created by William Shakespeare or Alexander Pope. The names of all four satellites of Uranus then known were suggested by [[Biography:John Herschel|John Herschel]] in 1852 at the request of Lassell.<ref name="Lassell 1852" /> Umbriel is the "dusky melancholy sprite" in Alexander Pope's ''The Rape of the Lock'',<ref name="Kuiper 1949" /> and the name suggests the [[Social:Latin|Latin]] ''umbra'', meaning ''shadow''. <!--The adjectival form of the name is ''Umbrielian''.--> The moon is also designated '''Uranus&nbsp;II'''.<ref name="Lassell, letter 1851" />

== Orbit ==
Umbriel orbits Uranus at the distance of about {{convert|266000|km|mi|abbr=on}}, being the third farthest from the planet among its [[Astronomy:Moons of Uranus|five major moons]].{{efn|The five major moons are [[Astronomy:Miranda (moon)|Miranda]], [[Astronomy:Ariel (moon)|Ariel]], Umbriel, Titania and Oberon.}} Umbriel's orbit has a small [[Astronomy:Orbital eccentricity|eccentricity]] and is [[Astronomy:Orbital inclination|inclined]] very little relative to the [[Astronomy:Equator|equator]] of Uranus.<ref name="orbit" /> Its [[Astronomy:Orbital period|orbital period]] is around 4.1&nbsp;Earth days, coincident with its rotational period. In other words, Umbriel is a [[Astronomy:Synchronous orbit|synchronous]] or tidally locked satellite, with one face always pointing toward its parent planet.<ref name="Smith Soderblom et al. 1986" /> Umbriel's orbit lies completely inside the [[Earth:Magnetosphere of Uranus|Uranian magnetosphere]].<ref name="Grundy Young et al. 2006" /> This is important, because the trailing [[Sphere#Hemisphere|hemispheres]] of airless satellites orbiting inside a magnetosphere (like Umbriel) are struck by magnetospheric [[Physics:Plasma|plasma]], which co-rotates with the planet.<ref name="Ness Acuña et al. 1986" /> This bombardment may lead to the darkening of the trailing hemispheres, which is actually observed for all Uranian moons except [[Astronomy:Oberon (moon)|Oberon]] (see below).<ref name="Grundy Young et al. 2006" /> Umbriel also serves as a sink of the magnetospheric charged particles, which creates a pronounced dip in energetic particle count near the moon's orbit as observed by ''Voyager 2'' in 1986.<ref name="Krimigis Armstrong et al. 1986" />

Because Uranus orbits the [[Astronomy:Sun|Sun]] almost on its side, and its moons orbit in the planet's equatorial plane, they (including Umbriel) are subject to an extreme seasonal cycle. Both northern and southern [[Astronomy:Poles of astronomical bodies#Geographic poles|poles]] spend 42 years in complete darkness, and another 42 years in continuous sunlight, with the Sun rising close to the [[Zenith|zenith]] over one of the poles at each [[Astronomy:Solstice|solstice]].<ref name="Grundy Young et al. 2006" /> The ''Voyager 2'' flyby coincided with the southern hemisphere's 1986 summer solstice, when nearly the entire northern hemisphere was unilluminated. Once every 42 years, when Uranus has an [[Astronomy:Equinox|equinox]] and its equatorial plane intersects the Earth, mutual [[Astronomy:Occultation|occultation]]s of Uranus's moons become possible. In 2007–2008 a number of such events were observed including two occultations of Titania by Umbriel on August 15 and December 8, 2007 as well as of Ariel by Umbriel on August 19, 2007.<ref name="Miller Chanover 2009" /><ref name="Arlot Dumas et al. 2008" />

Currently Umbriel is not involved in any orbital resonance with other Uranian satellites. Early in its history, however, it may have been in a 1:3 resonance with [[Astronomy:Miranda (moon)|Miranda]]. This would have increased Miranda's orbital eccentricity, contributing to the internal heating and geological activity of that moon, while Umbriel's orbit would have been less affected.<ref name="Tittemore Wisdom 1990" /> Due to Uranus's lower oblateness and smaller size relative to its satellites, its moons can escape more easily from a mean motion resonance than those of [[Astronomy:Jupiter|Jupiter]] or [[Astronomy:Saturn|Saturn]]. After Miranda escaped from this resonance (through a mechanism that probably resulted in its anomalously high orbital inclination), its eccentricity would have been damped, turning off the heat source.<ref name="Tittemore Wisdom 1989" /><ref name="Malhotra Dermott 1990" />

== Composition and internal structure ==
[[File:Umbriel Earth Moon Comparison.png|thumb|left|250px|Size comparison of [[Astronomy:Earth|Earth]], the Moon, and Umbriel.]]

Umbriel is the third-largest and fourth-most massive of the Uranian moons. Although Umbriel is the 13th-largest moon in the Solar System, it is only the 14th-most massive.{{efn|Due to the current [[Observational error|observational error]], it is not yet known for certain whether [[Astronomy:Ariel (moon)|Ariel]] is more massive than Umbriel.<ref name="JPLSSD"/>}} The moon's density is 1.39&nbsp;g/cm<sup>3</sup>,<ref name="Jacobson Campbell et al. 1992"/> which indicates that it mainly consists of [[Earth:Ice|water ice]], with a dense non-ice component constituting around 40% of its mass.<ref name="Hussmann Sohl et al. 2006"/> The latter could be made of [[Earth:Rock (geology)|rock]] and [[Chemistry:Carbon|carbon]]aceous material including heavy [[Chemistry:Organic compound|organic compound]]s known as [[Astronomy:Tholin|tholin]]s.<ref name="Smith Soderblom et al. 1986" /> The presence of water ice is supported by [[Physics:Infrared|infrared]] spectroscopic observations, which have revealed [[Chemistry:Crystalline|crystalline]] water ice on the surface of the moon.<ref name="Grundy Young et al. 2006" /> Water ice [[Physics:Absorption band|absorption band]]s are stronger on Umbriel's leading hemisphere than on the trailing hemisphere.<ref name="Grundy Young et al. 2006" /> The cause of this asymmetry is not known, but it may be related to the bombardment by charged particles from the [[Earth:Magnetosphere of Uranus|magnetosphere of Uranus]], which is stronger on the trailing hemisphere (due to the plasma's co-rotation).<ref name="Grundy Young et al. 2006" /> The energetic particles tend to [[Physics:Sputtering|sputter]] water ice, decompose [[Chemistry:Methane|methane]] trapped in ice as [[Physics:Clathrate hydrate|clathrate hydrate]] and darken other organics, leaving a dark, carbon-rich [[Chemistry:Residue|residue]] behind.<ref name="Grundy Young et al. 2006" />

Except for water, the only other compound identified on the surface of Umbriel by the infrared spectroscopy is [[Chemistry:Carbon dioxide|carbon dioxide]], which is concentrated mainly on the trailing hemisphere.<ref name="Grundy Young et al. 2006" /> The origin of the carbon dioxide is not completely clear. It might be produced locally from [[Chemistry:Carbonate|carbonate]]s or organic materials under the influence of the energetic charged particles coming from the magnetosphere of Uranus or the solar [[Physics:Ultraviolet|ultraviolet]] radiation. This hypothesis would explain the asymmetry in its distribution, as the trailing hemisphere is subject to a more intense magnetospheric influence than the leading hemisphere. Another possible source is the [[Physics:Outgassing|outgassing]] of the primordial CO<sub>2</sub> trapped by water ice in Umbriel's interior. The escape of CO<sub>2</sub> from the interior may be a result of past geological activity on this moon.<ref name="Grundy Young et al. 2006" />

Umbriel may be differentiated into a rocky core surrounded by an icy [[Earth:Mantle (geology)|mantle]].<ref name="Hussmann Sohl et al. 2006" /> If this is the case, the radius of the core (317&nbsp;km) is about 54% of the radius of the moon, and its mass is around 40% of the moon's mass—the parameters are dictated by the moon's composition. The pressure in the center of Umbriel is about 0.24&nbsp;GPa (2.4&nbsp;kbar).<ref name="Hussmann Sohl et al. 2006" /> The current state of the icy mantle is unclear, although the existence of a subsurface ocean is considered unlikely.<ref name="Hussmann Sohl et al. 2006" />

== Surface features ==
Umbriel's surface is the darkest of the Uranian moons, and reflects less than half as much light as Ariel, a sister satellite of similar size.<ref name="JPLSSD" /> Umbriel has a very low [[Physics:Bond albedo|Bond albedo]] of only about 10% as compared to 23% for Ariel.<ref name="Karkoschka 2001, Hubble" /> The reflectivity of the moon's surface decreases from 26% at a phase angle of 0° ([[Physics:Geometric albedo|geometric albedo]]) to 19% at an angle of about 1°. This phenomenon is called [[Physics:Opposition surge|opposition surge]]. The surface of Umbriel is slightly blue in color,<ref name="Bell McCord 1991" /> while fresh bright impact deposits (in [[Astronomy:Wunda (crater)|Wunda]] crater, for instance)<ref name="Plescia 1987" /> are even bluer. There may be an asymmetry between the leading and trailing hemispheres; the former appears to be redder than the latter.<ref name="Buratti Mosher 1991" /> The reddening of the surfaces probably results from [[Astronomy:Space weathering|space weathering]] from bombardment by charged particles and [[Astronomy:Micrometeoroid|micrometeorites]] over the age of the [[Astronomy:Solar System|Solar System]].<ref name="Bell McCord 1991" /> However, the color asymmetry of Umbriel is likely caused by accretion of a reddish material coming from outer parts of the Uranian system, possibly, from irregular satellites, which would occur predominately on the leading hemisphere.<ref name="Buratti Mosher 1991" /> The surface of Umbriel is relatively homogeneous—it does not demonstrate strong variation in either albedo or color.<ref name="Bell McCord 1991" />

{| class="wikitable plainrowheaders sortable" style="float: right;"
|+ Named craters on Umbriel<ref name="usgs" />{{efn|name=spirits|Surface features on Umbriel are named for evil or dark spirits taken from various mythologies.<ref name="Strobell & Masursky 1987" />}}
! scope="col" | Crater
! scope="col" class="unsortable" | Coordinates
! scope="col" | Diameter (km)
! scope="col" | Approved
! scope="col" | Named after
! scope="col" | Ref
|-
! scope="row" | Alberich
| {{coord|33.6|S|42.2|E|dim:52.0km_globe:umbriel_type:landmark}}
| 52.0
| 1988
| [[Unsolved:Alberich|Alberich]] (Norse)
| {{WGPSN|163}}
|-
! scope="row" | Fin
| {{coord|37.4|S|44.3|E|dim:43.0km_globe:umbriel_type:landmark}}
| 43.0
| 1988
| Fin (Danish)
| {{WGPSN|1955}}
|-
! scope="row" | Gob
| {{coord|12.7|S|27.8|E|dim:88.0km_globe:umbriel_type:landmark}}
| 88.0
| 1988
| Gob ([[Religion:Paganism|Pagan]])
| {{WGPSN|2196}}
|-
! scope="row" | Kanaloa
| {{coord|10.8|S|345.7|E|dim:86.0km_globe:umbriel_type:landmark}}
| 86.0
| 1988
| [[Religion:Kanaloa|Kanaloa]] (Polynesian)
| {{WGPSN|2912}}
|-
! scope="row" | Malingee
| {{coord|22.9|S|13.9|E|dim:164.0km_globe:umbriel_type:landmark}}
| 164.0
| 1988
| Malingee (Australian Aboriginal mythology)
| {{WGPSN|3608}}
|-
! scope="row" | Minepa
| {{coord|42.7|S|8.2|E|dim:58.0km_globe:umbriel_type:landmark}}
| 58.0
| 1988
| Minepa (Makua people of Mozambique)
| {{WGPSN|3909}}
|-
! scope="row" | Peri
| {{coord|9.2|S|4.3|E|dim:61.0km_globe:umbriel_type:landmark}}
| 61.0
| 1988
| Peri (Persian)
| {{WGPSN|4657}}
|-
! scope="row" | Setibos
| {{coord|30.8|S|346.3|E|dim:50.0km_globe:umbriel_type:landmark}}
| 50.0
| 1988
| Setebos ([[Place:Patagonia|Patagonia]]n)
| {{WGPSN|5443}}
|-
! scope="row" | [[Astronomy:Skynd (crater)|Skynd]]
| {{coord|1.8|S|331.7|E|dim:72.0km_globe:umbriel_type:landmark}}
| 72.0
| 1988
| Skynd (Danish)
| {{WGPSN|5595}}
|-
! scope="row" | [[Astronomy:Vuver (crater)|Vuver]]
| {{coord|4.7|S|311.6|E|dim:98.0km_globe:umbriel_type:landmark}}
| 98.0
| 1988
| Vuver (Finnish)
| {{WGPSN|6460}}
|-
! scope="row" | Wokolo
| {{coord|30|S|1.8|E|dim:208.0km_globe:umbriel_type:landmark}}
| 208.0
| 1988
| Wokolo (Bambara people of West Africa)
| {{WGPSN|6568}}
|-
! scope="row" | [[Astronomy:Wunda (crater)|Wunda]]
| {{coord|7.9|S|273.6|E|dim:131.0km_globe:umbriel_type:landmark}}
| 131.0
| 1988
| Wunda (Australian Aboriginal mythology)
| {{WGPSN|6587}}
|-
! scope="row" | Zlyden
| {{coord|23.3|S|326.2|E|dim:44.0km_globe:umbriel_type:landmark}}
| 44.0
| 1988
| Zlyden (Slavic)
| {{WGPSN|6747}}
|}

Scientists have so far recognized only one class of geological feature on Umbriel—[[Astronomy:Impact crater|craters]].<ref name="usgs" /> The surface of Umbriel has far more and larger craters than do Ariel and [[Astronomy:Titania (moon)|Titania]]. It shows the least geological activity.<ref name="Plescia 1987" /> In fact, among the Uranian moons only Oberon has more impact craters than Umbriel. The observed crater diameters range from a few kilometers at the low end to 210&nbsp;kilometers for the largest known crater, Wokolo.<ref name="Plescia 1987" /><ref name="usgs" /> All recognized craters on Umbriel have central peaks,<ref name="Plescia 1987" /> but no crater has [[Astronomy:Ray system|rays]].<ref name="Smith Soderblom et al. 1986" />

Near Umbriel's equator lies the most prominent surface feature: Wunda crater, which has a diameter of about 131&nbsp;km.<ref name="usgsWunda" /><ref name="hunt" /> Wunda has a large ring of bright material on its floor, which may be an impact deposit<ref name="Plescia 1987" /> or a deposit of pure carbon dioxide ice, which formed when the radiolytically formed carbon dioxide migrated from all over the surface of Umbriel and then got trapped in relatively cold Wunda.<ref name=Sori2017/> Nearby, seen along the [[Astronomy:Terminator (solar)|terminator]], are the craters [[Astronomy:Vuver (crater)|Vuver]] and [[Astronomy:Skynd (crater)|Skynd]], which lack bright rims but possess bright central peaks.<ref name="Smith Soderblom et al. 1986" /><ref name="hunt" /> Study of limb profiles of Umbriel revealed a possible very large impact feature having the diameter of about 400&nbsp;km and depth of approximately 5&nbsp;km.<ref name="Moore Schenk et al. 2004" />

Much like other moons of Uranus, the surface of Umbriel is cut by a system of canyons trending northeast–southwest.<ref name="Croft1989" /> They are not, however, officially recognized due to the poor imaging resolution and generally bland appearance of this moon, which hinders geological mapping.<ref name="Plescia 1987" />

Umbriel's heavily cratered surface has probably been stable since the [[Astronomy:Late Heavy Bombardment|Late Heavy Bombardment]].<ref name="Plescia 1987" /> The only signs of the ancient internal activity are canyons and dark polygons—dark patches with complex shapes measuring from tens to hundreds of kilometers across.<ref name="Helfenstein Thomas et al. 1989" /> The polygons were identified from precise photometry of ''Voyager 2'''s images and are distributed more or less uniformly on the surface of Umbriel, trending northeast–southwest. Some polygons correspond to depressions of a few kilometers deep and may have been created during an early episode of tectonic activity.<ref name="Helfenstein Thomas et al. 1989" /> Currently there is no explanation for why Umbriel is so dark and uniform in appearance. Its surface may be covered by a relatively thin layer of dark material (so called ''umbral material'') excavated by an impact or expelled in an explosive volcanic eruption.{{efn|While a co-orbiting population of dust particles is another possible source of the dark material, this is considered less likely because other satellites were not affected.<ref name="Smith Soderblom et al. 1986" />}}<ref name="Buratti Mosher 1991" /> Alternatively, Umbriel's crust may be entirely composed of the dark material, which prevented formation of bright features like crater rays. However, the presence of the bright feature within Wunda seems to contradict this hypothesis.<ref name="Smith Soderblom et al. 1986" />

== Origin and evolution ==
[[File:Umbriel usgsx2.jpg|thumb|[[False color|False color]] image of Umbriel showing polygons|alt=A spherical blueish body with its surface covered by craters and polygons. The lower right part is smooth.]]

Umbriel is thought to have formed from an accretion disc or subnebula; a disc of gas and dust that either existed around Uranus for some time after its formation or was created by the giant impact that most likely gave Uranus its large [[Astronomy:Axial tilt|obliquity]].<ref name="Mousis 2004" /> The precise composition of the subnebula is not known; however, the higher density of Uranian moons compared to the [[Astronomy:Moons of Saturn|moons of Saturn]] indicates that it may have been relatively water-poor.{{efn|For instance, Tethys, a Saturnian moon, has a density of 0.97&nbsp;g/cm<sup>3</sup>, which suggests that over 90% of its composition is water.<ref name="Grundy Young et al. 2006" />}}<ref name="Smith Soderblom et al. 1986" /> Significant amounts of [[Chemistry:Nitrogen|nitrogen]] and [[Chemistry:Carbon|carbon]] may have been present in the form of [[Chemistry:Carbon monoxide|carbon monoxide]] (CO) and [[Chemistry:Nitrogen|molecular nitrogen]] (N<sub>2</sub>) instead of [[Chemistry:Ammonia|ammonia]] and methane.<ref name="Mousis 2004" /> The moons that formed in such a subnebula would contain less water ice (with CO and N<sub>2</sub> trapped as clathrate) and more rock, explaining the higher density.<ref name="Smith Soderblom et al. 1986" />

Umbriel's accretion probably lasted for several thousand years.<ref name="Mousis 2004" /> The impacts that accompanied accretion caused heating of the moon's outer layer.<ref name="Squyres Reynolds et al. 1988" /> The maximum temperature of around 180&nbsp;K was reached at the depth of about 3&nbsp;km.<ref name="Squyres Reynolds et al. 1988" /> After the end of formation, the subsurface layer cooled, while the interior of Umbriel heated due to decay of radioactive elements present in its rocks.<ref name="Smith Soderblom et al. 1986" /> The cooling near-surface layer contracted, while the interior expanded. This caused strong [[Physics:Stress (mechanics)|extensional stresses]] in the moon's crust, which may have led to cracking.<ref name="Hillier & Squyres 1991" /> This process probably lasted for about 200&nbsp;million years, implying that any endogenous activity ceased billions of years ago.<ref name="Smith Soderblom et al. 1986" />

The initial [[Physics:Accretion (astrophysics)|accretional heating]] together with continued decay of radioactive elements may have led to melting of the ice<ref name="Squyres Reynolds et al. 1988" /> if an [[Chemistry:Antifreeze|antifreeze]] like ammonia (in the form of [[Chemistry:Hydrate|ammonia hydrate]]) or some salt was present.<ref name="Hussmann Sohl et al. 2006" /> The melting may have led to the separation of ice from rocks and formation of a rocky core surrounded by an icy mantle.<ref name="Plescia 1987" /> A layer of liquid water (ocean) rich in dissolved ammonia may have formed at the core–mantle boundary. The eutectic temperature of this mixture is 176&nbsp;K. The ocean, however, is likely to have frozen long ago.<ref name="Hussmann Sohl et al. 2006" /> Among Uranian moons Umbriel was least subjected to endogenic resurfacing processes,<ref name="Plescia 1987" /> although it may like other Uranian moons have experienced a very early resurfacing event.<ref name="Helfenstein Thomas et al. 1989" />

== Exploration ==
[[File:Voyager_spacecraft.jpg|thumbnail|200px|The ''Voyager 2'' spacecraft]]
{{Further|Astronomy:Exploration of Uranus}}

So far the only close-up images of Umbriel have been from the ''[[Astronomy:Voyager 2|Voyager 2]]'' probe, which photographed the moon during its flyby of Uranus in January 1986. Since the closest distance between ''Voyager 2'' and Umbriel was {{convert|325000|km|mi|abbr=on}},<ref name="Stone 1987" /> the best images of this moon have a spatial resolution of about 5.2&nbsp;km.<ref name="Plescia 1987" /> The images cover about 40% of the surface, but only 20% was photographed with the quality required for geological mapping.<ref name="Plescia 1987" /> At the time of the flyby the southern hemisphere of Umbriel (like those of the other moons) was pointed towards the Sun, so the northern (dark) hemisphere could not be studied.<ref name="Smith Soderblom et al. 1986" /> No other spacecraft has ever visited Uranus or its moons.

==See also==
* [[Astronomy:List of natural satellites|List of natural satellites]]

== Notes ==

{{notes
| colwidth = 30em
| notes =

}}

== References ==

{{Reflist
| colwidth = 30em
| refs =

<ref name="dict-def">
{{MW|Umbriel}}
</ref>

<ref name="Smith Soderblom et al. 1986">
{{cite journal| doi = 10.1126/science.233.4759.43| last1 = Smith| first1 = B. A.| last2 = Soderblom| first2 = L. A.| last3 = Beebe| first3 = A.| last4 = Bliss| first4 = D.| last5 = Boyce| first5 = J. M.| last6 = Brahic| first6 = A.| last7 = Briggs| first7 = G. A.| last8 = Brown| first8 = R. H.| last9 = Collins| first9 = S. A.| date = July 4, 1986| title = Voyager 2 in the Uranian System: Imaging Science Results| journal = Science| volume = 233| issue = 4759| pages = 43–64| pmid = 17812889| bibcode = 1986Sci...233...43S| s2cid = 5895824| ref = {{sfnRef|Smith Soderblom et al.|1986}}| url = https://zenodo.org/record/1230972}}
</ref>

<ref name="Karkoschka 2001, Hubble">
{{cite journal| doi = 10.1006/icar.2001.6596| last = Karkoschka| first = Erich|  year = 2001| title = Comprehensive Photometry of the Rings and 16 Satellites of Uranus with the Hubble Space Telescope| journal = Icarus| volume = 151| issue = 1| pages = 51–68| bibcode = 2001Icar..151...51K| ref = {{sfnRef|Karkoschka, Hubble|2001}}}}
</ref>

<ref name="Hussmann Sohl et al. 2006">
{{cite journal| doi = 10.1016/j.icarus.2006.06.005| last1 = Hussmann| first1 = Hauke| last2 = Sohl| first2 = Frank| last3 = Spohn| first3 = Tilman| date = November 2006| title = Subsurface oceans and deep interiors of medium-sized outer planet satellites and large trans-neptunian objects| journal = Icarus| volume = 185| issue = 1| pages = 258–273| url = https://www.researchgate.net/publication/225019299| bibcode = 2006Icar..185..258H| ref = {{sfnRef|Hussmann Sohl et al.|2006}}}}
</ref>

<ref name="Jacobson Campbell et al. 1992">
{{cite journal| doi = 10.1086/116211| last1 = Jacobson| first1 = R. A.| last2 = Campbell| first2 = J. K.| last3 = Taylor| first3 = A. H.| last4 = Synnott| first4 = S. P.| date=June 1992 | title = The masses of Uranus and its major satellites from Voyager tracking data and earth-based Uranian satellite data| journal = The Astronomical Journal| volume = 103| issue = 6| pages = 2068–2078| bibcode = 1992AJ....103.2068J| ref = {{sfnRef|Jacobson Campbell et al.|1992}}}}
</ref>

<ref name="Grundy Young et al. 2006">
{{cite journal| doi = 10.1016/j.icarus.2006.04.016| last1 = Grundy| first1 = W. M.| last2 = Young| first2 = L. A.| last3 = Spencer| first3 = J. R.| last4 = Johnson| first4 = R. E.| last5 = Young| first5 = E. F.| last6 = Buie| first6 = M. W.| date=October 2006 | title = Distributions of H<sub>2</sub>O and CO<sub>2</sub> ices on Ariel, Umbriel, Titania, and Oberon from IRTF/SpeX observations| journal = Icarus| volume = 184| issue = 2| pages = 543–555| arxiv = 0704.1525| bibcode = 2006Icar..184..543G| s2cid = 12105236| ref = {{sfnRef|Grundy Young et al.|2006}}}}
</ref>

<ref name="Squyres Reynolds et al. 1988">
{{cite journal| doi = 10.1029/JB093iB08p08779| last1 = Squyres| first1 = S. W.| last2 = Reynolds| first2 = Ray T.| last3 = Summers| first3 = Audrey L.| last4 = Shung| first4 = Felix| year = 1988| title = Accretional Heating of the Satellites of Saturn and Uranus| journal = Journal of Geophysical Research| volume = 93| issue = B8| pages = 8779–8794| bibcode = 1988JGR....93.8779S| ref = {{sfnRef|Squyres Reynolds et al.|1988}}| hdl = 2060/19870013922| hdl-access = free}}
</ref>

<ref name="Moore Schenk et al. 2004">
{{cite journal| doi = 10.1016/j.icarus.2004.05.009| last1 = Moore| first1 = Jeffrey M.| last2 = Schenk| first2 = Paul M.| last3 = Bruesch| first3 = Lindsey S.| last4 = Asphaug| first4 = Erik| last5 = McKinnon| first5 = William B.| date=October 2004 | title = Large impact features on middle-sized icy satellites| journal = Icarus| volume = 171| issue = 2| pages = 421–443| url = http://planets.oma.be/ISY/pdf/article_Icy.pdf| bibcode = 2004Icar..171..421M| ref = {{sfnRef|Moore Schenk et al.|2004}}
}}
</ref>

<ref name="Mousis 2004">
{{cite journal|year=2004|doi=10.1051/0004-6361:20031515|bibcode=2004A&A...413..373M|pages=373&ndash;380 |volume=413 | first=O.|title=Modeling the thermodynamical conditions in the Uranian subnebula – Implications for regular satellite composition|journal=Astronomy & Astrophysics|last=Mousis|doi-access=free}}
</ref>

<ref name="Croft1989">
{{cite conference
| last = Croft
| first = S. K.
| title = New geological maps of Uranian satellites Titania, Oberon, Umbriel and Miranda
| date = 1989
| publisher = Lunar and Planetary Sciences Institute, Houston
| work = Proceedings of Lunar and Planetary Sciences
| volume = 20
| page = 205C
| bibcode = 1989LPI....20..205C
}}
</ref>

<ref name="Herschel 1798">
{{cite journal| doi = 10.1098/rstl.1798.0005| last = Herschel| first = William Sr.|  date = January 1, 1798| title = On the Discovery of Four Additional Satellites of the Georgium Sidus. The Retrograde Motion of Its Old Satellites Announced; And the Cause of Their Disappearance at Certain Distances from the Planet Explained| journal = Philosophical Transactions of the Royal Society of London| volume = 88| pages = 47–79| bibcode = 1798RSPT...88...47H| doi-access = free}}
</ref>

<ref name="Lassell 1851">
{{cite journal
| last = Lassell
| first = W.
| title = On the interior satellites of Uranus
| journal = [[Organization:Monthly Notices of the Royal Astronomical Society|Monthly Notices of the Royal Astronomical Society]]
| volume = 12
| date = 1851
| pages = 15–17
| bibcode = 1851MNRAS..12...15L
| doi=10.1093/mnras/12.1.15
| doi-access = free
}}
</ref>

<ref name="Plescia 1987">
{{cite journal| doi = 10.1029/JA092iA13p14918| last = Plescia| first = J. B.| date = December 30, 1987| title = Cratering history of the Uranian satellites: Umbriel, Titania and Oberon| journal = Journal of Geophysical Research| issn = 0148-0227| volume = 92| issue = A13| pages = 14,918–14,932| bibcode = 1987JGR....9214918P}}
</ref>

<ref name="Kuiper 1949">
{{cite journal|page=129|issue=360|doi=10.1086/126146|bibcode=1949PASP...61..129K|volume=61|journal=Publications of the Astronomical Society of the Pacific|year=1949|title=The Fifth Satellite of Uranus|last=Kuiper | first=G. P.|s2cid=119916925 |doi-access=free}}
</ref>

<ref name="Ness Acuña et al. 1986">
{{cite journal| doi = 10.1126/science.233.4759.85| last1 = Ness| first1 = Norman F.| last2 = Acuña| first2 = Mario H.| last3 = Behannon| first3 = Kenneth W.| last4 = Burlaga| first4 = Leonard F.| last5 = Connerney| first5 = John E. P.| last6 = Lepping| first6 = Ronald P.| last7 = Neubauer| first7 = Fritz M.| date=July 1986 | title = Magnetic Fields at Uranus| journal = Science| volume = 233| issue = 4759| pages = 85–89| pmid = 17812894| bibcode = 1986Sci...233...85N| s2cid = 43471184| ref = {{sfnRef|Ness Acuña et al.|1986}}}}
</ref>

<ref name="orbit">
{{cite web
| title = Planetary Satellite Mean Orbital Parameters
| publisher = Jet Propulsion Laboratory, California Institute of Technology
| url = http://ssd.jpl.nasa.gov/?sat_elem
}}
</ref>

<ref name="Lassell, letter 1851">
{{cite journal| doi = 10.1086/100198| last = Lassell| first = William|  date=December 1851 | title = Letter from William Lassell, Esq., to the Editor| journal = Astronomical Journal| volume = 2| issue = 33| page = 70| bibcode = 1851AJ......2...70L| ref = {{sfnRef|Lassell, .27.27letter.27.27|1851}}}}
</ref>

<ref name="Stone 1987">
{{cite journal| doi = 10.1029/JA092iA13p14873| last = Stone| first = E. C.| date = December 30, 1987| title = The Voyager 2 Encounter with Uranus| journal = Journal of Geophysical Research| issn = 0148-0227| volume = 92| issue = A13| pages = 14,873–14,876| bibcode = 1987JGR....9214873S| url = https://authors.library.caltech.edu/45315/1/1986-01.pdf}}
</ref>

<ref name="Bell McCord 1991">
{{cite conference
| last1 = Bell
| first1 = J. F. III
| last2 = McCord
| first2 = T. B.
| date = 1991
| title = A search for spectral units on the Uranian satellites using color ratio images
| conference = Lunar and Planetary Science Conference, 21st, Mar. 12–16, 1990
| publisher = Lunar and Planetary Sciences Institute
| location = Houston, TX, United States
| type = Conference Proceedings
| pages = 473–489
| bibcode = 1991LPSC...21..473B
}}
</ref>

<ref name="Lassell 1852">
{{cite journal
| last = Lassell
| first = W.
| date = 1852
| language = de
| title = Beobachtungen der Uranus-Satelliten
| journal = Astronomische Nachrichten
| volume = 34
| page = 325
| bibcode = 1852AN.....34..325.
}}
</ref>

<ref name="Hillier & Squyres 1991">
{{cite journal| doi = 10.1029/91JE01401| last1 = Hillier| first1 = John| last2 = Squyres| first2 = Steven W.| date=August 1991 | title = Thermal stress tectonics on the satellites of Saturn and Uranus| journal = Journal of Geophysical Research| volume = 96| issue = E1| pages = 15,665–15,674| bibcode = 1991JGR....9615665H}}
</ref>

<ref name="Miller Chanover 2009">
{{cite journal| doi = 10.1016/j.icarus.2008.12.010| last1 = Miller| first1 = C.| last2 = Chanover| first2 = N. J.| date=March 2009 | title = Resolving dynamic parameters of the August 2007 Titania and Ariel occultations by Umbriel| journal = Icarus| volume = 200| issue = 1| pages = 343–346| bibcode = 2009Icar..200..343M}}
</ref>

<ref name="Arlot Dumas et al. 2008">
{{cite journal| doi = 10.1051/0004-6361:200810134| last1 = Arlot| first1 = J. -E.| last2 = Dumas| first2 = C.| last3 = Sicardy| first3 = B.| date=December 2008 | title = Observation of an eclipse of U-3 Titania by U-2 Umbriel on December 8, 2007 with ESO-VLT| journal = Astronomy and Astrophysics| volume = 492| issue = 2| pages = 599–602| bibcode=2008A&A...492..599A| ref = {{sfnRef|Arlot Dumas et al.|2008}}| doi-access = free}}
</ref>

<ref name="JPLSSD">
{{cite web
| title = Planetary Satellite Physical Parameters
| publisher = Jet Propulsion Laboratory (Solar System Dynamics)
| url = http://ssd.jpl.nasa.gov/?sat_phys_par
| access-date = May 28, 2009
}}
</ref>

<ref name="Thomas 1988">
{{cite journal|year=1988|doi=10.1016/0019-1035(88)90054-1|bibcode=1988Icar...73..427T|pages=427&ndash;441 |volume=73 | first=P. C.|last=Thomas|title=Radii, shapes, and topography of the satellites of Uranus from limb coordinates|journal=Icarus|issue=3}}
</ref>

<ref name="Tittemore Wisdom 1990">
{{cite journal| doi = 10.1016/0019-1035(90)90125-S| last1 = Tittemore| first1 = William C.| last2 = Wisdom| first2 = Jack| date=June 1990 | title = Tidal evolution of the Uranian satellites: III. Evolution through the Miranda-Umbriel 3:1, Miranda-Ariel 5:3, and Ariel-Umbriel 2:1 mean-motion commensurabilities| journal = Icarus| volume = 85| issue = 2| pages = 394–443| bibcode = 1990Icar...85..394T| hdl = 1721.1/57632| hdl-access = free}}
</ref>

<ref name="Tittemore Wisdom 1989">
{{cite journal| doi = 10.1016/0019-1035(89)90070-5| last1 = Tittemore| first1 = William C.| last2 = Wisdom| first2 = Jack| date=March 1989 | title = Tidal evolution of the Uranian satellites: II. An explanation of the anomalously high orbital inclination of Miranda| journal = Icarus| volume = 78| issue = 1| pages = 63–89| bibcode = 1989Icar...78...63T| hdl = 1721.1/57632| hdl-access = free}}
</ref>

<ref name="Malhotra Dermott 1990">
{{cite journal| doi = 10.1016/0019-1035(90)90126-T| last1 = Malhotra| first1 = Renu| last2 = Dermott| first2 = Stanley F.| date=June 1990 | title = The role of secondary resonances in the orbital history of Miranda| journal = Icarus| volume = 85| issue = 2| pages = 444–480| issn = 0019-1035| bibcode = 1990Icar...85..444M| doi-access = free}}
</ref>

<ref name="Struve 1848">
{{cite journal
| last = Struve
| first = O.
| date = 1848
| title = Note on the Satellites of Uranus
| journal = Monthly Notices of the Royal Astronomical Society
| volume = 8
| issue = 3
| pages = 44–47
| bibcode = 1848MNRAS...8...43L
| doi=10.1093/mnras/8.3.43
| doi-access = free
}}
</ref>

<ref name="Buratti Mosher 1991">
{{cite journal| doi = 10.1016/0019-1035(91)90064-Z| last1 = Buratti| first1 = Bonnie J.| last2 = Mosher| first2 = Joel A.| date=March 1991 | title = Comparative global albedo and color maps of the Uranian satellites| journal = Icarus| volume = 90| issue = 1| pages = 1–13| issn = 0019-1035| bibcode = 1991Icar...90....1B}}
</ref>

<ref name="hunt">
{{cite book
| last = Hunt
| first = Garry E.
|author2=Patrick Moore
 | date = 1989
| title = Atlas of Uranus
| publisher = Cambridge University Press.
| isbn = 978-0-521-34323-7
| url = https://archive.org/details/atlasofuranus00hunt_1
| url-access = registration
| page = [https://archive.org/details/atlasofuranus00hunt_1/page/82 82]
| quote = Umbriel crater Skynd.
}}
</ref>

<ref name="Helfenstein Thomas et al. 1989">
{{cite journal| doi = 10.1038/338324a0| last1 = Helfenstein | first1 = P.| last2 = Thomas | first2 = P. C.| last3 = Veverka | first3 = J.| date =March 1989| title = Evidence from Voyager II photometry for early resurfacing of Umbriel| journal = Nature| volume = 338| issue = 6213| pages = 324–326| issn = 0028-0836| bibcode = 1989Natur.338..324H| s2cid = 4260333 | ref = {{sfnRef|Helfenstein Thomas et al.|1989}}}}
</ref>

<ref name="usgsWunda">
{{cite web
| title = Umbriel:Wunda
| publisher = United States Geological Survey, Astrogeology
| work = Gazetteer of Planetary Nomenclature
| url = http://planetarynames.wr.usgs.gov/jsp/FeatureNameDetail.jsp?feature=66756
| access-date = August 8, 2009
}}
</ref>

<ref name="usgs">
{{cite web
| title = Umbriel Nomenclature Table Of Contents
| publisher = United States Geological Survey, Astrogeology
| work = Gazetteer of Planetary Nomenclature
| url = http://planetarynames.wr.usgs.gov/jsp/FeatureTypes2.jsp?system=Uranus&body=Umbriel&systemID=7&bodyID=36&sort=AName&show=Fname&show=Lat&show=Long&show=Diam&show=Stat&show=Orig
| access-date = September 26, 2009
}}
</ref>

<ref name="Krimigis Armstrong et al. 1986">
{{cite journal| doi = 10.1126/science.233.4759.97| last1 = Krimigis| first1 = S. M.| last2 = Armstrong| first2 = T. P.| last3 = Axford| first3 = W. I.| last4 = Cheng| first4 = A. F.| last5 = Gloeckler| first5 = G.| last6 = Hamilton| first6 = D. C.| last7 = Keath| first7 = E. P.| last8 = Lanzerotti| first8 = L. J.| last9 = Mauk| first9 = B. H.| date = July 4, 1986| title = The Magnetosphere of Uranus: Hot Plasma and Radiation Environment| journal = Science| volume = 233| issue = 4759| pages = 97–102| pmid = 17812897| bibcode = 1986Sci...233...97K| s2cid = 46166768| ref = {{sfnRef|Krimigis Armstrong et al.|1986}}}}
</ref>

<ref name="Strobell & Masursky 1987">
{{cite journal
| last1 = Strobell
| first1 = M. E.
| last2 = Masursky
| first2 = H.
|date=March 1987
| title = New Features Named on the Moon and Uranian Satellites
| journal = Abstracts of the Lunar and Planetary Science Conference
| volume = 18
| pages = 964–965
| bibcode = 1987LPI....18..964S
}}
</ref>

<ref name=Sori2017>{{Cite journal|last1=Sori|first1=Michael M.|last2=Bapst|first2=Jonathan|last3=Bramson|first3=Ali M.|last4=Byrne|first4=Shane|last5=Landis|first5=Margaret E.|year=2017|title=A Wunda-full world? Carbon dioxide ice deposits on Umbriel and other Uranian moons|journal=Icarus|volume=290|pages=1–13|doi=10.1016/j.icarus.2017.02.029|bibcode = 2017Icar..290....1S }}</ref>
}}

== External links ==

* {{cite web | url = http://solarsystem.nasa.gov/planets/profile.cfm?Object=Ura_Umbriel | title = Umbriel Profile | publisher = NASA's Solar System Exploration | access-date = 2009-10-10  | archive-url = https://web.archive.org/web/20090826163708/http://solarsystem.nasa.gov/planets/profile.cfm?Object=Ura_Umbriel | archive-date = August 26, 2009 }}
* {{cite journal | bibcode = 1851AN.....33..259L | title = Entdeckung von 2 neuen Uranus Trabanten | volume = 33 | issue = 17 | date = 1852 | pages = 259–262 | first = Herrn W. | last = Lassell | journal = Astronomische Nachrichten | language = de | doi = 10.1002/asna.18520331707 | url = https://zenodo.org/record/1424629 }}
* {{cite web | url = http://www.eso.org/public/news/eso0737/ | title = Edge-on! | publisher = [[Astronomy:Very Large Telescope|Very Large Telescope]] | date = August 23, 2007 | access-date = 2010-01-14 }}
* [http://www.solarviews.com/eng/umbriel.htm Umbriel page] (including a [http://www.solarviews.com/raw/uranus/umbmap1.jpg labelled map of Umbriel]) at ''Views of the Solar System''
* [http://planetarynames.wr.usgs.gov/Page/UMBRIEL/target Umbriel Nomenclature] from the [http://planetarynames.wr.usgs.gov/ USGS Planetary Nomenclature web site]

{{Uranus}}
{{Moons of Uranus}}
{{Solar System moons (compact)}}

[[Category:Umbriel (moon)| ]]

{{Sourceattribution|Umbriel (moon)}}