View source for Astronomy:Titania (moon)

{{Short description|Largest moon of Uranus}}
{{Infobox planet
| name                     = Titania
| image                    = Titania (moon) color, edited.jpg
| image_scale               =
| image_alt                = A round spherical body is almost fully illuminated. The surface has a mottled appearance with bright patches among relatively dark terrain. The terminator is located near the right edge. A large crater can be seen at the terminator in the upper half of the image. Another bright crater can be seen at the bottom. A large canyon runs from the darkness at the lower-right side to visible center of the body.
| caption                  = ''Voyager 2'' image of Titania's southern hemisphere{{refn | Along the terminator are visible the moon's largest known [[Astronomy:Impact crater|impact crater]], [[Astronomy:Gertrude (crater)|Gertrude]], at upper right and several enormous canyon-like [[Earth:Graben|graben]]s (the [[Astronomy:Messina Chasmata|Messina Chasmata]] above, Belmont Chasma near bottom) at lower right.| group = caption}}
| alt_names                = 
| mpc_name                 = Uranus III
| pronounced               = {{IPAc-en|t|ə|ˈ|t|ɑː|n|i|ə|,_|t|ə|ˈ|t|eɪ|n|i|ə}}<ref>{{Cite dictionary |url=http://www.lexico.com/definition/Titania |archive-url=https://web.archive.org/web/20200302074449/https://www.lexico.com/definition/titania |url-status=dead |archive-date=March 2, 2020 |title=Titania |dictionary=Lexico UK English Dictionary |publisher=[[Organization:Oxford University Press|Oxford University Press]]}} Lexico/OED. Only the first pronunciation is used in ''A Midsummer Night's Dream'', e.g. Shakespeare Recording Society (1995) ''The Tempest'' (audio CD). The second is used by interviewees in a podcast by the Folger Shakespeare Library, but not by the narrator: [https://www.folger.edu/shakespeare-unlimited/shakespearean-moons-uranus Brave New Worlds: The Shakespearean Moons of Uranus]</ref> 
| adjectives               = Titanian {{IPAc-en|t|ə|ˈ|t|ɑː|n|i|ə|n}}<ref>Lewis (2002) ''Anthony Burgess: A Biography'', p. 387</ref>{{efn|Spelled the same as the adjectival form of Saturn's moon [[Astronomy:Titan (moon)|Titan]], but may be pronounced differently.}}
| discoverer               = William Herschel
| discovered               = January 11, 1787<ref name="Herschel 1787" />
| semimajor                = {{val|435910|u=km}}<ref name="orbit" />
| eccentricity             = {{val|0.0011}}<ref name="orbit" />
| period                   = {{val|8.706234|u=d}}<ref name="orbit" />
| avg_speed                = 3.64&nbsp;km/s{{efn|name=calculated|Calculated on the basis of other parameters.}}
| inclination              = {{val|0.340|u=°}} (to Uranus's equator)<ref name="orbit" />
| satellite_of             = [[Astronomy:Uranus|Uranus]]
| mean_radius              = {{val|788.4|0.6|u=km}} ({{val|0.1235|u=Earths}})<ref name="Widemann Sicardy et al. 2009" />
| surface_area             = {{val|7820000|u=km<sup>2</sup>}}{{efn | Surface area derived from the radius ''r'' : 4π''r''². }}
| volume                   = {{val|2065000000|u=km<sup>3</sup>}}{{efn | Volume ''v'' derived from the radius ''r'' : 4π''r''<sup>3</sup>/3. }}
| mass                     = {{val|3.400|0.061|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|1.711|0.005|u=g/cm<sup>3</sup>}}<ref name="Widemann Sicardy et al. 2009" />
| surface_grav             = {{Gr|3.400|788.4|3}} [[Physics:Acceleration|m/s²]]{{efn | Surface gravity derived from the mass ''m'', the [[Physics:Gravitational constant|gravitational constant]] ''G'' and the radius ''r'' : ''Gm/r''². }}
| escape_velocity          = {{V2|3.400|788.4}} km/s{{efn | Escape velocity derived from the mass ''m'', the [[Physics:Gravitational constant|gravitational constant]] ''G'' and the radius ''r'' : {{math|{{radical|2Gm/r}}}}. }}
| rotation                 = presumed synchronous<ref name="Smith Soderblom et al. 1986" />
| albedo =
  {{plainlist |
* 0.35 (geometrical)
* 0.17 (Bond)<ref name="Karkoschka, Hubble 2001" />
  }}
| magnitude                = 13.9<ref name="Newton Teece 1995" />
| temp_name1               = solstice<ref name="Widemann Sicardy et al. 2009" />
| mean_temp_1              = {{nowrap|70 ± 7}}&nbsp;[[Kelvin|K]]
| max_temp_1               = 89&nbsp;K
| min_temp_1               = 60&nbsp;K
| atmosphere               = yes
| atmosphere_composition =
  {{plainlist |
* [[Chemistry:Carbon dioxide|carbon dioxide]] (?)
* [[Chemistry:Nitrogen|nitrogen]] (?)
* [[Chemistry:Methane|methane]] (?)
  }}
| surface_pressure         = <1–2&nbsp;[[Pascal (unit)|mPa]] (10–20&nbsp;[[Bar (unit)|nbar]])
| note                     = no
}}

'''Titania''' ({{IPAc-en|t|ə|ˈ|t|ɑː|n|i|ə|,_|t|ə|ˈ|t|eɪ|n|i|ə}}), also designated '''Uranus III''', is the largest of the [[Astronomy:Moons of Uranus|moons of Uranus]] and the eighth largest moon in the [[Astronomy:Solar System|Solar System]] at a diameter of {{convert|1578|km}}, with a surface area comparable to that of {{wipe|Australia}}. Discovered by William Herschel in 1787, it is named after the queen of the fairies in Shakespeare's ''A Midsummer Night's Dream''. Its orbit lies inside [[Astronomy:Uranus|Uranus]]' [[Astronomy:Magnetosphere|magnetosphere]].

Titania consists of approximately equal amounts of ice and [[Earth:Rock (geology)|rock]], and is probably differentiated into a rocky core and an icy [[Earth:Mantle (geology)|mantle]]. A layer of liquid water may be present at the [[Earth:Core–mantle boundary|core–mantle boundary]]. Its surface, which is relatively dark and slightly red in color, appears to have been shaped by both impacts and endogenic processes. It is covered with numerous [[Astronomy:Impact crater|impact crater]]s reaching up to {{convert|326|km}} in diameter, but is less heavily cratered than [[Astronomy:Oberon (moon)|Oberon]], outermost of the five large moons of Uranus. It may have undergone an early endogenic resurfacing event which obliterated its older, heavily cratered surface. Its surface is cut by a system of enormous [[Earth:Canyon|canyon]]s and [[Earth:Fault scarp|scarps]], the result of the expansion of its interior during the later stages of its evolution. Like all major moons of Uranus, Titania probably formed from an [[Astronomy:Accretion disk|accretion disk]] which surrounded the planet just after its formation.

[[Physics:Infrared|Infrared]] spectroscopy conducted from 2001 to 2005 revealed the presence of water [[Earth:Ice|ice]] as well as frozen [[Chemistry:Carbon dioxide|carbon dioxide]] on Titania's surface, suggesting it may have a tenuous carbon dioxide [[Astronomy:Atmosphere|atmosphere]] with a surface pressure of about 10 nanopascals (10<sup>−13</sup>&nbsp;bar). Measurements during Titania's occultation of a [[Astronomy:Star|star]] put an upper limit on the surface pressure of any possible atmosphere at 1–2&nbsp;mPa (10–20&nbsp;nbar).

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 Titania, which allowed mapping of about 40% of its surface.

== Discovery and naming ==

Titania was discovered by William Herschel on January 11, 1787, the same day he discovered Uranus's second largest moon, [[Astronomy:Oberon (moon)|Oberon]].<ref name="Herschel 1787" /><ref name="Herschel 1788" /> He later reported the discoveries of four more satellites,<ref name="Herschel 1798" /> although they were subsequently revealed as spurious.<ref name="Struve1848" /> For nearly the next 50 years, Titania and Oberon would not be observed by any instrument other than William Herschel's,<ref name="Herschel 1834" /> although the moon can be seen from [[Astronomy:Earth|Earth]] with a present-day high-end amateur telescope.<ref name="Newton Teece 1995" />

[[File:Titania Earth Moon Comparison.png|thumb|left|250px|Size comparison of Earth, the Moon, and Titania]]

All of Uranus's moons are named after characters created by William Shakespeare or Alexander Pope. The name Titania was taken from the Queen of the Fairies in ''A Midsummer Night's Dream''.<ref name="Kuiper 1949" /> The names of all four satellites of Uranus then known were suggested by Herschel's son [[Biography:John Herschel|John]] in 1852, at the request of William Lassell,<ref name="Lassell 1852" /> who had discovered the other two moons, [[Astronomy:Ariel (moon)|Ariel]] and [[Astronomy:Umbriel (moon)|Umbriel]], the year before.<ref name="Lassell 1851" />

Titania was initially referred to as "the first satellite of Uranus", and in 1848 was given the designation '''{{nowrap|Uranus I}}''' by William Lassell,<ref name="Lassell 1848" /> although he sometimes used William Herschel's numbering (where Titania and Oberon are II and IV).<ref name="Lassell 1850" /> In 1851 Lassell eventually numbered all four known satellites in order of their distance from the planet by [[Roman numerals]], and since then Titania has been designated '''{{nowrap|Uranus III}}'''.<ref name="Lassell, letter 1851" />

Shakespeare's character's name is pronounced {{IPAc-en|t|ᵻ|ˈ|t|eɪ|n|j|ə}}, but the moon is often pronounced {{IPAc-en|t|aɪ|ˈ|t|eɪ|n|i|ə}}, by analogy with the familiar chemical element [[Chemistry:Titanium|titanium]].<ref name="Webster" /> The adjectival form, ''Titanian'', is homonymous with that of Saturn's moon [[Astronomy:Titan (moon)|Titan]]. The name ''Titania'' is ancient Greek for "Daughter of the Titans".

== Orbit ==

Titania orbits Uranus at the distance of about {{convert|436000|km}}, being the second farthest from the planet among its five major moons after Oberon.{{efn | The five major moons are [[Astronomy:Miranda (moon)|Miranda]], [[Astronomy:Ariel (moon)|Ariel]], [[Astronomy:Umbriel (moon)|Umbriel]], Titania and Oberon. }} Titania'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 8.7&nbsp;days, coincident with its rotational period. In other words, Titania is a [[Astronomy:Synchronous orbit|synchronous]] or tidally locked satellite, with one face always pointing toward the planet.<ref name="Smith Soderblom et al. 1986" />

Titania's orbit lies completely inside the Uranian [[Astronomy:Magnetosphere|magnetosphere]].<ref name="Grundy Young et al. 2006" /> This is important, because the trailing hemispheres of satellites orbiting inside a magnetosphere are struck by magnetospheric 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 Oberon (see below).<ref name="Grundy Young et al. 2006" />

Because Uranus orbits the Sun almost on its side, and its moons orbit in the planet's equatorial plane, they (including Titania) are subject to an extreme seasonal cycle. Both northern and southern [[Astronomy:Poles of astronomical bodies#Geographic poles|poles]] spend 42 years in a 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 southern hemisphere was illuminated. 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.<ref name="Miller & Chanover 2009" /><ref name="Arlot Dumas et al. 2008" />

== Composition and internal structure ==

[[File:PIA00039 Titania.jpg|thumb|left|''Voyager 2'''s highest-resolution image of Titania shows moderately cratered plains, enormous rifts and long scarps. Near the bottom, a region of smoother plains including the crater Ursula is split by the graben Belmont Chasma.|alt=A round spherical body with its left half illuminated. The surface has a mottled appearance with bright patches among relatively dark terrain. The terminator is slightly to the right from the center and runs from the top to bottom. A large crater with a central pit can be seen at the terminator in the upper half of the image. Another bright crater can be seen at the bottom intersected by a canyon. The second large canyon runs from the darkness at the lower-right side to visible center of the body.]]

Titania is the largest and most massive Uranian moon, and the eighth most massive moon in the Solar System.{{efn | The seven moons more massive than Titania are [[Astronomy:Ganymede (moon)|Ganymede]], [[Astronomy:Titan (moon)|Titan]], [[Astronomy:Callisto (moon)|Callisto]], [[Astronomy:Io (moon)|Io]], Earth's [[Astronomy:Moon|Moon]], [[Astronomy:Europa (moon)|Europa]], and [[Astronomy:Triton (moon)|Triton]].<ref name="JPLSSD" /> }} Its density of 1.71&nbsp;g/cm<sup>3</sup>,<ref name="Jacobson Campbell et al. 1992" /> which is much higher than the typical density of Saturn's satellites, indicates that it consists of roughly equal proportions of water ice and dense non-ice components;<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.<ref name="Smith Soderblom et al. 1986" /> The presence of water ice is supported by [[Physics:Infrared|infrared]] spectroscopic observations made in 2001–2005, 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 slightly stronger on Titania's leading hemisphere than on the trailing hemisphere. This is the opposite of what is observed on Oberon, where the trailing hemisphere exhibits stronger water ice signatures.<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 Titania by 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 solar [[Physics:Ultraviolet|ultraviolet]] radiation or energetic charged particles coming from the magnetosphere of Uranus. The latter process would explain the asymmetry in its distribution, because 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 Titania's interior. The escape of CO<sub>2</sub> from the interior may be related to the past geological activity on this moon.<ref name="Grundy Young et al. 2006" />

Titania 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 {{convert|520|km}} is about 66% of the radius of the moon, and its mass is around 58% of the moon's mass—the proportions are dictated by moon's composition. The pressure in the center of Titania is about 0.58&nbsp;GPa (5.8&nbsp;kbar).<ref name="Hussmann Sohl et al. 2006" /> The current state of the icy mantle is unclear. If the ice contains enough ammonia or other [[Chemistry:Antifreeze|antifreeze]], Titania may have a subsurface ocean at the core–mantle boundary. The thickness of this ocean, if it exists, is up to {{convert|50|km}} and its temperature is around 190&nbsp;[[Kelvin|K]] (close to the water–ammonia eutectic temperature of 176&nbsp;K).<ref name="Hussmann Sohl et al. 2006" /> However the present internal structure of Titania depends heavily on its thermal history, which is poorly known. Recent studies suggest, contrary to earlier theories, that Uranus largest moons like Titania in fact could have active subsurface oceans.<ref>{{cite web | url=https://www.nasa.gov/feature/jpl/new-study-of-uranus-large-moons-shows-4-may-hold-water | title=New Study of Uranus' Large Moons Shows 4 May Hold Water | date=4 May 2023 }}</ref>

== Surface features ==

[[File:Titania (moon) labeled.jpg|thumb|Titania with some surface features labeled. The south pole is situated close to the unlabeled bright crater below and left of the crater Jessica.]]

Among Uranus's moons, Titania is intermediate in brightness between the dark Oberon and Umbriel and the bright Ariel and [[Astronomy:Miranda (moon)|Miranda]].<ref name="Karkoschka, Hubble 2001" /> Its surface shows a strong [[Physics:Opposition surge|opposition surge]]: its reflectivity decreases from 35% at a phase angle of 0° ([[Earth:Albedo|geometrical albedo]]) to 25% at an angle of about 1°. Titania has a relatively low [[Physics:Bond albedo|Bond albedo]] of about 17%.<ref name="Karkoschka, Hubble 2001" /> Its surface is generally slightly red in color, but less red than that of [[Astronomy:Oberon (moon)|Oberon]].<ref name="Bell1991" /> However, fresh impact deposits are bluer, while the smooth plains situated on the leading hemisphere near [[Astronomy:Ursula (crater)|Ursula crater]] and along some grabens are somewhat redder.<ref name="Bell1991" /><ref name="Plescia 1987" /> There may be an asymmetry between the leading and trailing hemispheres;<ref name="Buratti1991" /> the former appears to be redder than the latter by 8%.{{efn | The color is determined by the ratio of albedos viewed through the green (0.52–0.59&nbsp;μm) and violet (0.38–0.45&nbsp;μm) Voyager filters.<ref name="Bell1991" /><ref name="Buratti1991" /> }} However, this difference is related to the smooth plains and may be accidental.<ref name="Bell1991" /> The reddening of the surfaces probably results from [[Astronomy:Space weathering|space weathering]] caused by bombardment by charged particles and micrometeorites over the age of the [[Astronomy:Solar System|Solar System]].<ref name="Bell1991" /> However, the color asymmetry of Titania is more likely related to accretion of a reddish material coming from outer parts of the Uranian system, possibly, from irregular satellites, which would be deposited predominately on the leading hemisphere.<ref name="Buratti1991" />

Scientists have recognized three classes of geological feature on Titania: [[Astronomy:Impact crater|craters]], chasmata ([[Earth:Canyon|canyon]]s) and [[Astronomy:Rupes|rupes]] ([[Earth:Escarpment|scarps]]).<ref name="USGS: Titania Nomenclature" /> The surface of Titania is less heavily cratered than the surfaces of either Oberon or Umbriel, which means that the surface is much younger.<ref name="Plescia 1987" /> The crater diameters reach 326&nbsp;kilometers for the largest known crater, [[Astronomy:Gertrude (crater)|Gertrude]]<ref name="USGS: Titania: Gertrude" /> (there can be also a degraded basin of approximately the same size).<ref name="Plescia 1987" /> Some craters (for instance, [[Astronomy:Ursula (crater)|Ursula]] and Jessica) are surrounded by bright impact ejecta (rays) consisting of relatively fresh ice.<ref name="Smith Soderblom et al. 1986" /> All large craters on Titania have flat floors and central peaks. The only exception is Ursula, which has a pit in the center.<ref name="Plescia 1987" /> To the west of Gertrude there is an area with irregular topography, the so-called "unnamed basin", which may be another highly degraded impact basin with the diameter of about {{convert|330|km}}.<ref name="Plescia 1987" />

Titania's surface is intersected by a system of enormous faults, or scarps. In some places, two parallel scarps mark depressions in the satellite's crust,<ref name="Smith Soderblom et al. 1986" /> forming [[Earth:Graben|graben]]s, which are sometimes called canyons.<ref name="Croft 1989" /> The most prominent among Titania's canyons is Messina Chasma, which runs for about {{convert|1500|km}} from the equator almost to the south pole.<ref name="USGS: Titania Nomenclature" /> The grabens on Titania are {{convert|20|–|50|km}} wide and have a relief of about 2–5&nbsp;km.<ref name="Smith Soderblom et al. 1986" /> The scarps that are not related to canyons are called rupes, such as [[Astronomy:Rousillon Rupes|Rousillon Rupes]] near Ursula crater.<ref name="USGS: Titania Nomenclature" /> The regions along some scarps and near Ursula appear smooth at ''Voyager''<nowiki>'s</nowiki> image resolution. These smooth plains were probably resurfaced later in Titania's geological history, after the majority of craters formed. The resurfacing may have been either endogenic in nature, involving the eruption of fluid material from the interior (cryovolcanism), or, alternatively it may be due to blanking by the impact ejecta from nearby large craters.<ref name="Plescia 1987" /> The grabens are probably the youngest geological features on Titania—they cut all craters and even smooth plains.<ref name="Croft 1989" />

The geology of Titania was influenced by two competing forces: [[Astronomy:Impact crater|impact crater]] formation and endogenic resurfacing.<ref name="Croft 1989" /> The former acted over the moon's entire history and influenced all surfaces. The latter processes were also global in nature, but active mainly for a period following the moon's formation.<ref name="Plescia 1987" /> They obliterated the original heavily cratered terrain, explaining the relatively low number of impact craters on the moon's present-day surface.<ref name="Smith Soderblom et al. 1986" /> Additional episodes of resurfacing may have occurred later and led to the formation of smooth plains.<ref name="Smith Soderblom et al. 1986" /> Alternatively smooth plains may be ejecta blankets of the nearby impact craters.<ref name="Croft 1989" /> The most recent endogenous processes were mainly tectonic in nature and caused the formation of the canyons, which are actually giant cracks in the ice crust.<ref name="Croft 1989" /> The cracking of the crust was caused by the global expansion of Titania by about 0.7%.<ref name="Croft 1989" />

[[File:Messina Chasma.jpg|thumb|upright|Messina Chasma—a large canyon on Titania|alt=The right half of a round spherical body that is illuminated. The terminator runs along the right edge. A large crater with a central pit can be seen at the terminator in the upper half of the image. A large canyon runs from the darkness at the lower-right side to visible center of the body.]]

{| class="wikitable plainrowheaders"
|+ Named surface features on Titania<ref name="USGS: Titania Nomenclature" />
|-
! scope="col" | Feature
! scope="col" | Named after
! scope="col" | Type
! scope="col" | Length (diameter), km
! scope="col" | Coordinates
|-
! scope="row" | Belmont Chasma
| Belmont, Italy (''The Merchant of Venice'')
| rowspan="2" | [[Astronomy:Chasma|Chasma]]
| style="text-align: center;" | 238
| {{coord|-8.5|32.6|dim:238km_globe:titania}}
|-
! scope="row" | Messina Chasmata
| Messina, Italy (''Much Ado About Nothing'')
| style="text-align: center;" | 1,492
| {{coord|-33.3|335|dim:1492km_globe:titania}}
|-
! scope="row" | [[Astronomy:Rousillon Rupes|Rousillon Rupes]]
| Roussillon, {{wipe|France}} (''All's Well That Ends Well'')
| [[Astronomy:Rupes|Rupes]]
| style="text-align: center;" | 402
| {{coord|-14.7|23.5|dim:402km_globe:titania}}
|-
! scope="row" | Adriana
| Adriana (''The Comedy of Errors'')
| rowspan ="15" | [[Astronomy:Impact crater|Crater]]
| style="text-align: center;" | 50
| {{coord|-20.1|3.9|dim:50km_globe:titania}}
|-
! scope="row" | Bona
| Bona (''Henry VI, Part 3'')
| style="text-align: center;" | 51
| {{coord|-55.8|351.2|dim:51km_globe:titania}}
|-
! scope="row" | Calphurnia
| Calpurnia Pisonis (''Julius Caesar'')
| style="text-align: center;" | 100
| {{coord|-42.4|291.4 |dim:100km_globe:titania|name=Calphurnia crater}}
|-
! scope="row" | Elinor
| Eleanor of Aquitaine (''The Life and Death of King John'')
| style="text-align: center;" | 74
| {{coord|-44.8|333.6|dim:74km_globe:titania}}
|-
! scope="row" | [[Astronomy:Gertrude (crater)|Gertrude]]
| Gertrude (''Hamlet'')
| style="text-align: center;" | 326
| {{coord|-15.8|287.1|dim:326km_globe:titania}}
|-
! scope="row" | Imogen
| Imogen (Cymbeline)
| style="text-align: center;" | 28
| {{coord|-23.8|321.2|dim:28km_globe:titania}}
|-
! scope="row" | Iras
| Iras (''Antony and Cleopatra'')
| style="text-align: center;" | 33
| {{coord|-19.2|338.8|dim:33km_globe:titania}}
|-
! scope="row" | Jessica
| Jessica (''The Merchant of Venice'')
| style="text-align: center;" | 64
| {{coord|-55.3|285.9|dim:64km_globe:titania}}
|-
! scope="row" | Katherine
| Katherine (''Henry VIII'')
| style="text-align: center;" | 75
| {{coord|-51.2|331.9|dim:75km_globe:titania}}
|-
! scope="row" | Lucetta
| Lucetta (''The Two Gentlemen of Verona'')
| style="text-align: center;" | 58
| {{coord|-14.7|277.1|dim:58km_globe:titania}}
|-
! scope="row" | Marina
| Marina (''Pericles, Prince of Tyre'')
| style="text-align: center;" | 40
| {{coord|-15.5|316|dim:40km_globe:titania}}
|-
! scope="row" | Mopsa
| Mopsa (''The Winter's Tale'')
| style="text-align: center;" | 101
| {{coord|-11.9|302.2|dim:101km_globe:titania}}
|-
! scope="row" | Phrynia
| Phrynia (''Timon of Athens'')
| style="text-align: center;" | 35
| {{coord|-24.3|309.2|dim:35km_globe:titania}}
|-
! scope="row" | [[Astronomy:Ursula (crater)|Ursula]]
| Ursula (''Much Ado About Nothing'')
| style="text-align: center;" | 135
| {{coord|-12.4|45.2|dim:135km_globe:titania}}
|-
! scope="row" | Valeria
| Valeria (''Coriolanus'')
| style="text-align: center;" | 59
| {{coord|-34.5|4.2|dim:59km_globe:titania}}
|-
! scope="row" colspan="5" | Surface features on Titania are named for female characters or locations from Shakespeare's works.<ref name="Strobell & Masursky 1987" />
|}

== Atmosphere ==

The presence of carbon dioxide on the surface suggests that Titania may have a tenuous seasonal atmosphere of CO<sub>2</sub>, much like that of the Jovian moon Callisto.{{efn | The partial pressure of CO<sub>2</sub> on the surface of Callisto is about 10&nbsp;nPa (10&nbsp;pbar). }}<ref name="Widemann Sicardy et al. 2009" /> Other gases, like [[Chemistry:Nitrogen|nitrogen]] or [[Chemistry:Methane|methane]], are unlikely to be present, because Titania's weak gravity could not prevent them from escaping into space. At the maximum temperature attainable during Titania's [[Astronomy:Summer solstice|summer solstice]] (89&nbsp;K), the [[Physics:Vapor pressure|vapor pressure]] of carbon dioxide is about 300&nbsp;μPa (3&nbsp;nbar).<ref name="Widemann Sicardy et al. 2009" />

On September 8, 2001, Titania [[Astronomy:Occultation|occulted]] a bright star (HIP 106829) with a [[Astronomy:Apparent magnitude|visible magnitude]] of 7.2; this was an opportunity to both refine Titania's diameter and [[Astronomy:Ephemeris|ephemeris]], and to detect any extant atmosphere. The data revealed no atmosphere to a surface pressure of 1–2&nbsp;mPa (10–20&nbsp;nbar); if it exists, it would have to be far thinner than that of [[Astronomy:Triton (moon)|Triton]] or [[Astronomy:Pluto|Pluto]].<ref name="Widemann Sicardy et al. 2009" /> This upper limit is still several times higher than the maximum possible surface pressure of the carbon dioxide, meaning that the measurements place essentially no constraints on parameters of the atmosphere.<ref name="Widemann Sicardy et al. 2009" />

The peculiar geometry of the Uranian system causes the moons' poles to receive more [[Physics:Solar energy|solar energy]] than their equatorial regions.<ref name="Grundy Young et al. 2006" /> Because the vapor pressure of CO<sub>2</sub> is a steep function of temperature,<ref name="Widemann Sicardy et al. 2009" /> this may lead to the accumulation of carbon dioxide in the low-latitude regions of Titania, where it can stably exist on high albedo patches and shaded regions of the surface in the form of ice. During the summer, when the polar temperatures reach as high as 85–90&nbsp;K,<ref name="Widemann Sicardy et al. 2009" /><ref name="Grundy Young et al. 2006" /> carbon dioxide [[Sublimation (phase transition)|sublimates]] and migrates to the opposite pole and to the equatorial regions, giving rise to a type of [[Earth:Carbon cycle|carbon cycle]]. The accumulated carbon dioxide ice can be removed from cold traps by magnetospheric particles, which sputter it from the surface. Titania is thought to have lost a significant amount of carbon dioxide since its formation 4.6&nbsp;billion years ago.<ref name="Grundy Young et al. 2006" />

== Origin and evolution ==

Titania 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:Obliquity|obliquity]].<ref name="Mousis 2004" /> The precise composition of the subnebula is not known; however, the relatively high density of Titania and other 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 the density of 0.97&nbsp;g/cm<sup>3</sup>, which implies it contains more than 90% of 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]] and 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 a clathrate) and more rock, explaining their higher density.<ref name="Smith Soderblom et al. 1986" />

Titania'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 {{convert|250|K|C}} was reached at a depth of about {{convert|60|km}}.<ref name="Squyres Reynolds et al. 1988" /> After the end of formation, the subsurface layer cooled, while the interior of Titania 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 extensional stresses in the moon's crust leading to cracking. Some of the present-day canyons may be a result of this. The process lasted for about 200&nbsp;million years,<ref name="Hillier & Squyres 1991" /> 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 were probably strong enough to melt the ice if some antifreeze like ammonia (in the form of [[Chemistry:Hydrate|ammonia hydrate]]) or [[Chemistry:Salt|salt]] was present.<ref name="Squyres Reynolds et al. 1988" /> Further melting may have led to the separation of ice from rocks and formation of a rocky core surrounded by an icy mantle. A layer of liquid water (ocean) rich in dissolved ammonia may have formed at the core–mantle boundary.<ref name="Hussmann Sohl et al. 2006" /> The eutectic temperature of this mixture is {{convert|176|K|C}}.<ref name="Hussmann Sohl et al. 2006" /> If the temperature dropped below this value, the ocean would have subsequently frozen. The freezing of the water would have caused the interior to expand, which may have been responsible for the formation of the majority of the canyons.<ref name="Plescia 1987" /> However, the present knowledge of Titania's geological evolution is quite limited. Whereas more up to date analysis suggest that larger moons of Uranus are not only capable of having active subsurface oceans; but in fact; presumed to have subterranean oceans beneath them.<ref>{{cite web | url=https://www.ndtv.com/science/nasa-says-4-of-uranus-large-moons-may-hold-water-4011923 | title=NASA Says 4 of Uranus' Large Moons May Hold Water }}</ref><ref>{{cite web | url=https://lifestyle.livemint.com/smart-living/environment/uranus-large-moons-may-hold-water-111683622469809.html | title=Uranus' large moons may hold water, new study find | date=9 May 2023 }}</ref>

== Exploration ==

{{main|Astronomy:Exploration of Uranus}}

So far the only close-up images of Titania 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&nbsp;2'' and Titania was only {{convert|365200|km|abbr=on}},<ref name="Stone 1987" /> the best images of this moon have a spatial resolution of about 3.4&nbsp;km (only Miranda and Ariel were imaged with a better resolution).<ref name="Plescia 1987" /> The images cover about 40% of the surface, but only 24% was photographed with the precision required for geological mapping. At the time of the flyby, the southern hemisphere of Titania (like those of the other moons) was pointed towards the [[Astronomy:Sun|Sun]], so the northern (dark) hemisphere could not be studied.<ref name="Smith Soderblom et al. 1986" />

No other spacecraft has ever visited the Uranian system or Titania. [[Astronomy:Cassini retirement|One possibility]], now discarded, was to send ''[[Astronomy:Cassini–Huygens|Cassini]]'' on from Saturn to Uranus in an extended mission. Another mission concept proposed was the Uranus orbiter and probe concept, evaluated around 2010. Uranus was also examined as part of one trajectory for a precursor interstellar probe concept, [[Engineering:Innovative Interstellar Explorer|Innovative Interstellar Explorer]].

A Uranus orbiter and probe mission architecture was identified as the highest priority for a NASA [[Astronomy:Large strategic science missions|Flagship mission]] by the 2023–2032 [[Astronomy:Planetary Science Decadal Survey|Planetary Science Decadal Survey]]. The science questions motivating this prioritization include questions about the Uranian satellites' bulk properties, internal structure, and geologic history.<ref>{{Cite book |last1=Committee on the Planetary Science and Astrobiology Decadal Survey |url=https://www.nap.edu/catalog/26522 |title=Origins, Worlds, and Life: A Decadal Strategy for Planetary Science and Astrobiology 2023-2032 |last2=Space Studies Board |last3=Division on Engineering and Physical Sciences |last4=National Academies of Sciences, Engineering, and Medicine |date=2022 |publisher=National Academies Press |isbn=978-0-309-47578-5 |location=Washington, D.C. |doi=10.17226/26522|s2cid=248283239 }}</ref> A Uranus orbiter<ref>Mark Hofstadter, [http://www.spacepolicyonline.com/images/stories/PSDS%20GP1%20Hofstadter_Uranus%20Orbiter.pdf "Ice Giant Science: The Case for a Uranus Orbiter"], Jet Propulsion Laboratory/California Institute of Technology, ''Report to the Decadal Survey Giant Planets Panel,'' 24 August 2009</ref> was listed as the third priority for a NASA Flagship mission by the 2013-2022 [[Astronomy:Planetary Science Decadal Survey|Planetary Science Decadal Survey]], and conceptual designs for such a mission are currently being analyzed.<ref>Stephen Clark [http://spaceflightnow.com/2015/08/25/uranus-neptune-in-nasas-sights-for-new-robotic-mission/ "Uranus, Neptune in NASA’s sights for new robotic mission"], ''Spaceflight Now,'' August 25, 2015</ref> 

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

== Notes ==

{{Reflist| group = caption}}

{{notes
| colwidth = 30em
}}

== References ==

{{Reflist
| colwidth = 30em
| refs =

<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 = 4 July 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}}
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}}

== External links ==


* {{cite web
 |title       = Titania profile
 |date        = 1999
 |publisher   = NASA
 |url         = http://solarsystem.nasa.gov/planets/profile.cfm?Object=Ura_Titania
 |access-date  = June 22, 2009
 |url-status     = dead
 |archive-url  = https://web.archive.org/web/20090613033504/http://solarsystem.nasa.gov/planets/profile.cfm?Object=Ura_Titania
 |archive-date = June 13, 2009
}}
* [http://photojournal.jpl.nasa.gov/target/Titania NASA archive of publicly released Titania images]
* {{cite web
 |last1       = Sicardy
 |first1      = Bruno
 |last2       = Widemann
 |first2      = Thomas
 |date        = 2001
 |title       = Is there an atmosphere around Titania, satellite of Uranus?
 |publisher   = Paris Observatory
 |url         = http://www.obspm.fr/actual/nouvelle/mar02/titania.en.shtml
 |access-date  = June 22, 2009
 |url-status     = dead
 |archive-url  = https://web.archive.org/web/20130307044100/http://www.obspm.fr/actual/nouvelle/mar02/titania.en.shtml
 |archive-date = March 7, 2013
}}
* {{cite web
 |last        = Widemann
 |first       = Thomas
 |date        = 2009
 |title       = From Titania to large trans-Neptunian objects: ground-based stellar occultations in the quest for the billionth of atmospheric pressure
 |publisher   = Paris Observatory
 |url         = http://www.obspm.fr/actual/nouvelle/feb09/titania.en.shtml
 |access-date  = June 22, 2009
 |url-status     = dead
 |archive-url  = https://web.archive.org/web/20110604000111/http://www.obspm.fr/actual/nouvelle/feb09/titania.en.shtml
 |archive-date = June 4, 2011
}}
* [http://www.solarviews.com/eng/titania.htm Titania page] (including [http://www.solarviews.com/raw/uranus/titamap2.jpg labelled] [http://www.solarviews.com/raw/uranus/titamap1.jpg maps] of Titania) at ''Views of the Solar System''
* [http://planetarynames.wr.usgs.gov/Page/TITANIA/target Titania nomenclature] from the [http://planetarynames.wr.usgs.gov/ USGS Planetary Nomenclature web site]

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

[[Category:Titania (moon)| ]]

{{Sourceattribution|Titania (moon)}}