Voyager 2 image of Titania's southern hemisphere
|Discovered by||William Herschel|
|Discovery date||January 11, 1787|
|Pronunciation||// or //[a]|
|Alternative names||Uranus III|
|Semi-major axis||435910 km|
|Orbital period||8.706234 d|
|Inclination||0.340° (to Uranus's equator)|
|Mean radius||788.4±0.6 km (0.1235 Earths)|
|Surface area||7820000 km2[b]|
|Mass||(3.527±0.09)×1021 kg (5.908×10−4 Earths)|
|Mean density||1.711±0.005 g/cm³|
|Equatorial surface gravity||0.38 m/s²[d]|
|Escape velocity||0.773 km/s[e]|
|Rotation period||presumed synchronous|
|Surface pressure||<10–20 nbar|
Titania is the largest of the moons of Uranus and the eighth largest moon in the Solar System at a diameter of 1,578 kilometres (981 mi). Discovered by William Herschel in 1787, Titania is named after the queen of the fairies in Shakespeare's A Midsummer Night's Dream. Its orbit lies inside Uranus's magnetosphere.
Titania consists of approximately equal amounts of ice and rock, and is probably differentiated into a rocky core and an icy mantle. A layer of liquid water may be present at the core–mantle boundary. The surface of Titania, 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 impact craters reaching up to 326 kilometres (203 mi) in diameter, but is less heavily cratered than the surface of Uranus's outermost moon, Oberon. Titania probably underwent an early endogenic resurfacing event which obliterated its older, heavily cratered surface. Titania's surface is cut by a system of enormous canyons and 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 accretion disk which surrounded the planet just after its formation.
Infrared spectroscopy conducted from 2001 to 2005 revealed the presence of water ice as well as frozen carbon dioxide on the surface of Titania, which in turn suggested that the moon may possess a tenuous carbon dioxide atmosphere with a surface pressure of about one 10 trillionth of a bar. Measurements during Titania's occultation of a star put an upper limit on the surface pressure of any possible atmosphere at 10–20 nbar.
As of 2013, the Uranian system has been studied up close only once, by the spacecraft Voyager 2 in January 1986. It took several images of Titania, which allowed mapping of about 40% of the moon’s surface.
Discovery and naming
Titania was discovered by William Herschel on January 11, 1787, the same day he discovered Uranus's second largest moon, Oberon. He later reported the discoveries of four more satellites, although they were subsequently revealed as spurious. For nearly fifty years following their discovery, Titania and Oberon would not be observed by any instrument other than William Herschel's, although the moon can be seen from Earth with a present-day high-end amateur telescope.
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. The names of all four satellites of Uranus then known were suggested by Herschel's son John in 1852, at the request of William Lassell, who had discovered the other two moons, Ariel and Umbriel, the year before.
Titania was initially referred to as "the first satellite of Uranus", and in 1848 was given the designation Uranus I by William Lassell, although he sometimes used William Herschel's numbering (where Titania and Oberon are II and IV). 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 Uranus III.
Shakespeare's character's name is pronounced //, but the moon is often pronounced //, by analogy with the familiar chemical element titanium. The adjectival form, Titanian, is homonymous with that of Saturn's moon Titan. The name Titania is ancient Greek in origin, meaning "Daughter of the Titans."
Titania orbits Uranus at the distance of about 436,000 kilometres (271,000 mi), being the second farthest from the planet among its five major moons.[f] Titania's orbit has a small eccentricity and is inclined very little relative to the equator of Uranus. Its orbital period is around 8.7 days, coincident with its rotational period. In other words, Titania is a synchronous or tidally locked satellite, with one face always pointing toward the planet.
Titania's orbit lies completely inside the Uranian magnetosphere. This is important, because the trailing hemispheres of satellites orbiting inside a magnetosphere are struck by magnetospheric plasma, which co-rotates with the planet. This bombardment may lead to the darkening of the trailing hemispheres, which is actually observed for all Uranian moons except Oberon (see below).
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 poles spend 42 years in a complete darkness, and another 42 years in continuous sunlight, with the sun rising close to the zenith over one of the poles at each solstice. 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 equinox and its equatorial plane intersects the Earth, mutual occultations 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.
Composition and internal structure
Titania is the largest and most massive Uranian moon, and the eighth most massive moon in the Solar System.[g] Its density of 1.71 g/cm³, 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; the latter could be made of rock and carbonaceous material including heavy organic compounds. The presence of water ice is supported by infrared spectroscopic observations made in 2001–2005, which have revealed crystalline water ice on the surface of the moon. Water ice absorption bands 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. The cause of this asymmetry is not known, but it may be related to the bombardment by charged particles from the magnetosphere of Uranus, which is stronger on the trailing hemisphere (due to the plasma's co-rotation). The energetic particles tend to sputter water ice, decompose methane trapped in ice as clathrate hydrate and darken other organics, leaving a dark, carbon-rich residue behind.
Except for water, the only other compound identified on the surface of Titania by infrared spectroscopy is carbon dioxide, which is concentrated mainly on the trailing hemisphere. The origin of the carbon dioxide is not completely clear. It might be produced locally from carbonates or organic materials under the influence of the solar 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 outgassing of the primordial CO2 trapped by water ice in Titania's interior. The escape of CO2 from the interior may be related to the past geological activity on this moon.
Titania may be differentiated into a rocky core surrounded by an icy mantle. If this is the case, the radius of the core 520 kilometres (320 mi) 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 GPa (5.8 kbar). The current state of the icy mantle is unclear. If the ice contains enough ammonia or other antifreeze, Titania may possess a liquid ocean layer at the core-mantle boundary. The thickness of this ocean, if it exists, is up to 50 kilometres (31 mi) and its temperature is around 190 K. However the present internal structure of Titania depends heavily on its thermal history, which is poorly known.
Among Uranus's moons, Titania is intermediate in brightness between the dark Oberon and Umbriel and the bright Ariel and Miranda. Its surface shows a strong opposition surge: its reflectivity decreases from 35% at a phase angle of 0° (geometrical albedo) to 25% at an angle of about 1°. Titania has a relatively low Bond albedo of about 17%. Its surface is generally slightly red in color, but less red than that of Oberon. However, fresh impact deposits are bluer, while the smooth plains situated on the leading hemisphere near Ursula crater and along some grabens are somewhat redder. There may be an asymmetry between the leading and trailing hemispheres; the former appears to be redder than the latter by 8%.[h] However, this difference is related to the smooth plains and may be accidental. The reddening of the surfaces probably results from space weathering caused by bombardment by charged particles and micrometeorites over the age of the Solar System. 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.
Scientists have recognized three classes of geological feature on Titania: craters, chasmata (canyons) and rupes (scarps). The surface of Titania is less heavily cratered than the surfaces of either Oberon or Umbriel, which means that it is much younger. The crater diameters range from a few kilometers at the low end to 326 kilometers for the largest known crater, Gertrude. Some craters (for instance, Ursula and Jessica) are surrounded by bright impact ejecta (rays) consisting of relatively fresh ice. All large craters on Titania have flat floors and central peaks. The only exception is Ursula, which has a pit in the center. 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 330 kilometres (210 mi).
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, forming grabens, which are sometimes called canyons. The most prominent among Titania's canyons is Messina Chasma, which runs for about 1,500 kilometres (930 mi) from the equator almost to the south pole. The grabens on Titania are 20–50 kilometres (12–31 mi) wide and have a relief of about 2–5 km. The scarps that are not related to canyons are called rupes, such as Rousillon Rupes near Ursula crater. The regions along some scarps and near Ursula appear smooth at Voyager's 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. The grabens are probably the youngest geological features on Titania—they cut all craters and even smooth plains.
The geology of Titania was influenced by two competing forces: impact crater formation and endogenic resurfacing. 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. They obliterated the original heavily cratered terrain, explaining the relatively low number of impact craters on the moon's present-day surface. Additional episodes of resurfacing may have occurred later and led to the formation of smooth plains. Alternatively smooth plains may be ejecta blankets of the nearby impact craters. 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. The cracking of the crust was caused by the global expansion of Titania by about 0.7%.
|Feature||Named after||Type||Length (diameter), km||Coordinates|
|Belmont Chasma||Belmont, Italy (The Merchant of Venice)||Chasma||238|
|Messina Chasmata||Messina, Italy (Much Ado About Nothing)||1,492|
|Rousillon Rupes||Roussillon, France (All's Well That Ends Well)||Rupes||402|
|Adriana||Adriana (The Comedy of Errors)||Crater||50|
|Bona||Bona (Henry VI, Part 3)||51|
|Calphurnia||Calpurnia Pisonis (Julius Caesar)||100|
|Elinor||Eleanor of Aquitaine (The Life and Death of King John)||74|
|Iras||Iras (Antony and Cleopatra)||33|
|Jessica||Jessica (The Merchant of Venice)||64|
|Katherine||Katherine (Henry VIII)||75|
|Lucetta||Lucetta (The Two Gentlemen of Verona)||58|
|Marina||Marina (Pericles, Prince of Tyre)||40|
|Mopsa||Mopsa (The Winter's Tale)||101|
|Phrynia||Phrynia (Timon of Athens)||35|
|Ursula||Ursula (Much Ado About Nothing)||135|
|Surface features on Titania are named for characters from Shakespeare's works.|
The presence of carbon dioxide on the surface suggests that Titania may have a tenuous seasonal atmosphere of CO2, much like that of the Jovian moon Callisto.[i] Other gases, like nitrogen or methane, are unlikely to be present, because the moon's weak gravity could not prevent them from escaping into space. At the maximum temperature attainable during Titania's summer solstice (89 K), the vapor pressure of carbon dioxide is about 3 nbar.
On September 8, 2001, Titania occulted a bright star (HIP106829) with a visible magnitude of 7.2; this was an opportunity to both refine the moon's diameter and ephemeris, and to detect any extant atmosphere. The data revealed no atmosphere to a surface pressure of 10–20 nanobars; if it exists, it would have to be far thinner than that of Triton or Pluto. 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.
The peculiar geometry of the Uranian system causes the moons' poles to receive more solar energy than their equatorial regions. Since the vapor pressure of CO2 is a steep function of temperature, 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 K, carbon dioxide sublimates and migrates to the opposite pole and to the equatorial regions, giving rise to a type of 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 billion years ago.
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 obliquity. The precise composition of the subnebula is not known; however, the relatively high density of Titania and other Uranian moons compared to the moons of Saturn indicates that it may have been relatively water-poor.[j] Significant amounts of nitrogen and carbon may have been present in the form of carbon monoxide and N2 instead of ammonia and methane. The moons that formed in such a subnebula would contain less water ice (with CO and N2 trapped as a clathrate) and more rock, explaining the higher density.
Titania's accretion probably lasted for several thousand years. The impacts that accompanied accretion caused heating of the moon's outer layer. The maximum temperature of around 250 K (−23 °C) was reached at a depth of about 60 kilometres (37 mi). 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. 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 million years, implying that any endogenous activity ceased billions of years ago.
The initial 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 ammonia hydrate) or salt was present. 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. The eutectic temperature of this mixture is 176 K (−97 °C). 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. However, the present knowledge of Titania's geological evolution is quite limited.
So far the only close-up images of Titania have been from the Voyager 2 probe, which photographed the moon during its flyby of Uranus in January 1986. Since the closest distance between Voyager 2 and Titania was only 365,200 kilometres (226,900 mi), the best images of this moon have a spatial resolution of about 3.4 km (only Miranda and Ariel were imaged with a better resolution). 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 Sun, so the northern (dark) hemisphere could not be studied.
No other spacecraft has ever visited the Uranian system or Titania, and no mission is planned in the foreseeable future. One possibility, now discarded, was to send Cassini on from Saturn to Uranus in an extended mission; another is the Uranus orbiter and probe concept, evaluated around 2010. Uranus was also examined as part of one trajectory for a precursor interstellar probe concept, Innovative Interstellar Explorer.
- ti-TAH-nyə or ty-TAY-nee-ə. The former pronunciation is distinct from the adjectival form of Saturn's moon Titan.
- Surface area derived from the radius r : 4πr².
- Volume v derived from the radius r : 4πr³/3.
- Surface gravity derived from the mass m, the gravitational constant G and the radius r : Gm/r².
- Escape velocity derived from the mass m, the gravitational constant G and the radius r : √.
- The five major moons are Miranda, Ariel, Umbriel, Titania and Oberon.
- The seven moons more massive than Titania are Ganymede, Titan, Callisto, Io, Earth's Moon, Europa, and Triton.
- The color is determined by the ratio of albedos viewed through the green (0.52–0.59 μm) and violet (0.38–0.45 μm) Voyager filters.
- The partial pressure of CO2 on the surface of Callisto is about 10 pbar.
- For instance, Tethys, a Saturnian moon, has the density of 0.97 g/cm³, which implies it contains more than 90% of water.
- Herschel, W. S. (1787). "An Account of the Discovery of Two Satellites Revolving Round the Georgian Planet". Philosophical Transactions of the Royal Society of London 77: 125–129. doi:10.1098/rstl.1787.0016. JSTOR 106717.
- "Merriam-Webster online dictionary: titania". Merriam-Webster. 2009. Retrieved 2009-09-26.
- "Planetary Satellite Mean Orbital Parameters". Jet Propulsion Laboratory, California Institute of Technology. Retrieved 2009-10-06.
- Widemann, T.; Sicardy, B.; Dusser, R.; Martinez, C.; Beisker, W.; Bredner, E.; Dunham, D.; Maley, P.; Lellouch, E.; Arlot, J. -E.; Berthier, J.; Colas, F.; Hubbard, W. B.; Hill, R.; Lecacheux, J.; Lecampion, J. -F.; Pau, S.; Rapaport, M.; Roques, F.; Thuillot, W.; Hills, C. R.; Elliott, A. J.; Miles, R.; Platt, T.; Cremaschini, C.; Dubreuil, P.; Cavadore, C.; Demeautis, C.; Henriquet, P.; Labrevoir, O. (February 2009). "Titania's radius and an upper limit on its atmosphere from the September 8, 2001 stellar occultation" (PDF). Icarus 199 (2): 458–476. Bibcode:2009Icar..199..458W. doi:10.1016/j.icarus.2008.09.011.
- Jacobson, R. A.; Campbell, J. K.; Taylor, A. H.; Synnott, S. P. (June 1992). "The masses of Uranus and its major satellites from Voyager tracking data and earth-based Uranian satellite data". The Astronomical Journal 103 (6): 2068–2078. Bibcode:1992AJ....103.2068J. doi:10.1086/116211.
- Smith, B. A.; Soderblom, L. A.; Beebe, A.; Bliss, D.; Boyce, J. M.; Brahic, A.; Briggs, G. A.; Brown, R. H.; Collins, S. A. (4 July 1986). "Voyager 2 in the Uranian System: Imaging Science Results". Science 233 (4759): 43–64. Bibcode:1986Sci...233...43S. doi:10.1126/science.233.4759.43. PMID 17812889.
- Karkoschka, Erich (2001). "Comprehensive Photometry of the Rings and 16 Satellites of Uranus with the Hubble Space Telescope". Icarus 151 (1): 51–68. Bibcode:2001Icar..151...51K. doi:10.1006/icar.2001.6596.
- Newton, Bill; Teece, Philip (1995). The guide to amateur astronomy. Cambridge University Press. p. 109. ISBN 978-0-521-44492-7.
- Herschel, W. S. (1 January 1788). "On the Georgian Planet and Its Satellites". Philosophical Transactions of the Royal Society of London 78: 364–378. Bibcode:1788RSPT...78..364H. doi:10.1098/rstl.1788.0024.
- Herschel, William, Sr. (1 January 1798). "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". Philosophical Transactions of the Royal Society of London 88: 47–79. Bibcode:1798RSPT...88...47H. doi:10.1098/rstl.1798.0005.
- Struve, O. (1848). "Note on the Satellites of Uranus". Monthly Notices of the Royal Astronomical Society 8 (3): 44–47. Bibcode:1848MNRAS...8...43.
- Herschel, John (March 1834). "On the Satellites of Uranus". Monthly Notices of the Royal Astronomical Society 3 (5): 35–36. Bibcode:1834MNRAS...3Q..35H.
- Kuiper, G. P. (1949). "The Fifth Satellite of Uranus". Publications of the Astronomical Society of the Pacific 61 (360): 129. Bibcode:1949PASP...61..129K. doi:10.1086/126146.
- Lassell, W. (1852). "Beobachtungen der Uranus-Satelliten". Astronomische Nachrichten (in German) 34: 325. Bibcode:1852AN.....34..325.
- Lassell, W. (1851). "On the interior satellites of Uranus". Monthly Notices of the Royal Astronomical Society 12: 15–17. Bibcode:1851MNRAS..12...15L.
- Lassell, W. (1848). "Observations of Satellites of Uranus". Monthly Notices of the Royal Astronomical Society 8 (3): 43–44. Bibcode:1848MNRAS...8...43.
- Lassell, W. (1850). "Bright Satellites of Uranus". Monthly Notices of the Royal Astronomical Society 10 (6): 135. Bibcode:1850MNRAS..10..135L.
- Lassell, William (December 1851). "Letter from William Lassell, Esq., to the Editor". Astronomical Journal 2 (33): 70. Bibcode:1851AJ......2...70L. doi:10.1086/100198.
- Grundy, W. M.; Young, L. A.; Spencer, J. R.; Johnson, R. E.; Young, E. F.; Buie, M. W. (October 2006). "Distributions of H2O and CO2 ices on Ariel, Umbriel, Titania, and Oberon from IRTF/SpeX observations". Icarus 184 (2): 543–555. arXiv:0704.1525. Bibcode:2006Icar..184..543G. doi:10.1016/j.icarus.2006.04.016.
- Ness, Norman F.; Acuña, Mario H.; Behannon, Kenneth W.; Burlaga, Leonard F.; Connerney, John E. P.; Lepping, Ronald P.; Neubauer, Fritz M. (July 1986). "Magnetic Fields at Uranus". Science 233 (4759): 85–89. Bibcode:1986Sci...233...85N. doi:10.1126/science.233.4759.85. PMID 17812894.
- Miller, C.; Chanover, N. J. (March 2009). "Resolving dynamic parameters of the August 2007 Titania and Ariel occultations by Umbriel". Icarus 200 (1): 343–346. Bibcode:2009Icar..200..343M. doi:10.1016/j.icarus.2008.12.010.
- Arlot, J. -E.; Dumas, C.; Sicardy, B. (December 2008). "Observation of an eclipse of U-3 Titania by U-2 Umbriel on December 8, 2007 with ESO-VLT". Astronomy and Astrophysics 492 (2): 599–602. Bibcode:2008A&A...492..599A. doi:10.1051/0004-6361:200810134.
- "Planetary Satellite Physical Parameters". Jet Propulsion Laboratory (Solar System Dynamics). Retrieved 2009-05-28.
- Hussmann, H.; Sohl, Frank; Spohn, Tilman (November 2006). "Subsurface oceans and deep interiors of medium-sized outer planet satellites and large trans-neptunian objects". Icarus 185 (1): 258–273. Bibcode:2006Icar..185..258H. doi:10.1016/j.icarus.2006.06.005.
- Bell III, J.F.; McCord, T.B. (1991). "A search for spectral units on the Uranian satellites using color ratio images" (Conference Proceedings). Lunar and Planetary Science Conference, 21st, Mar. 12–16, 1990. Houston, TX, United States: Lunar and Planetary Sciences Institute. pp. 473–489.
- Plescia, J. B. (December 30, 1987). "Cratering history of the Uranian satellites: Umbriel, Titania and Oberon". Journal of Geophysical Research 92 (A13): 14,918–14,932. Bibcode:1987JGR....9214918P. doi:10.1029/JA092iA13p14918. ISSN 0148-0227.
- Buratti, Bonnie J.; Mosher, Joel A. (March 1991). "Comparative global albedo and color maps of the Uranian satellites". Icarus 90 (1): 1–13. Bibcode:1991Icar...90....1B. doi:10.1016/0019-1035(91)90064-Z. ISSN 0019-1035.
- USGS/IAU. "Titania Nomenclature Table Of Contents". Gazetteer of Planetary Nomenclature. USGS Astrogeology. Retrieved 2012-02-23.
- USGS/IAU (October 1, 2006). "Gertrude on Titania". Gazetteer of Planetary Nomenclature. USGS Astrogeology. Retrieved 2012-02-23.
- Croft, S. K. (1989). "New geological maps of Uranian satellites Titania, Oberon, Umbriel and Miranda". Proceeding of Lunar and Planetary Sciences 20 (Lunar and Planetary Sciences Institute, Houston): 205C.
- Strobell, M.E.; Masursky, H. (1987). "New Features Named on the Moon and Uranian Satellites". Abstracts of the Lunar and Planetary Science Conference 18: 964–65. Bibcode:1987LPI....18..964S.
- Mousis, O. (2004). "Modeling the thermodynamical conditions in the Uranian subnebula – Implications for regular satellite composition". Astronomy & Astrophysics 413: 373–380. Bibcode:2004A&A...413..373M. doi:10.1051/0004-6361:20031515.
- Squyres, S. W.; Reynolds, Ray T.; Summers, Audrey L.; Shung, Felix (1988). "Accretional Heating of the Satellites of Saturn and Uranus". Journal of Geophysical Research 93 (B8): 8779–8794. Bibcode:1988JGR....93.8779S. doi:10.1029/JB093iB08p08779.
- Hillier, John; Squyres, Steven W. (August 1991). "Thermal stress tectonics on the satellites of Saturn and Uranus". Journal of Geophysical Research 96 (E1): 15,665–15,674. Bibcode:1991JGR....9615665H. doi:10.1029/91JE01401.
- Stone, E. C. (December 30, 1987). "The Voyager 2 Encounter with Uranus". Journal of Geophysical Research 92 (A13): 14,873–14,876. Bibcode:1987JGR....9214873S. doi:10.1029/JA092iA13p14873. ISSN 0148-0227.
|Wikimedia Commons has media related to Titania (moon).|
- "Titania profile". NASA. 1999. Retrieved June 22, 2009.
- NASA archive of publicly released Titania images
- Sicardy, Bruno; Widemann, Thomas (2001). "Is there an atmosphere around Titania, satellite of Uranus?". Paris Observatory. Retrieved June 22, 2009.
- Widemann, Thomas (2009). "From Titania to large trans-Neptunian objects: ground-based stellar occultations in the quest for the billionth of atmospheric pressure". Paris Observatory. Retrieved June 22, 2009.
- Titania page (including labelled maps of Titania) at Views of the Solar System
- Titania nomenclature from the USGS Planetary Nomenclature web site