Titan (moon)
![]() Titan in natural color from the Cassini spacecraft (2005). Only the moon's dense atmosphere, colored orange by organonitrogen haze particles, is visible. | |
Discovery | |
---|---|
Discovered by | Christiaan Huygens |
Discovery date | March 25, 1655 |
Designations | |
Pronunciation | /ˈtaɪtən/ |
Saturn VI | |
Adjectives | Titanian |
Orbital characteristics[1] | |
Periapsis | 1186680 km |
Apoapsis | 1257060 km |
1221870 km | |
Eccentricity | 0.0288 |
15.945 d | |
Inclination | 0.34854° (to Saturn's equator) |
Satellite of | Saturn |
Physical characteristics | |
2576±2 km (0.404 Earths)[2] | |
8.3×107 km2 | |
Volume | 7.16×1010 km3 (0.066 Earths) |
Mass | (1.3452±0.0002)×1023 kg (0.0225 Earths)[2] |
Mean density | 1.8798±0.0044 g/cm3[2] |
1.352 m/s2 (0.14 g) | |
2.639 km/s | |
Synchronous | |
Zero | |
Albedo | 0.22[3] |
Temperature | 93.7 K (−179.5 °C)[4] |
8.2[5] to 9.0 | |
Atmosphere | |
Surface pressure | 146.7 kPa |
Composition by volume | Variable[6][7] Stratosphere: 98.4% nitrogen (N2), 1.4% methane (CH4); Lower troposphere: 95% N2, 4.9% CH4 |
Titan (or Saturn VI) is the largest moon of Saturn. It is the only natural satellite known to have a dense atmosphere,[8] and the only object other than Earth for which clear evidence of stable bodies of surface liquid has been found.[9]
Titan is the sixth ellipsoidal moon from Saturn. Frequently described as a planet-like moon, Titan has a diameter roughly 50% larger than Earth's moon and is 80% more massive. It is the second-largest moon in the Solar System, after Jupiter's moon Ganymede, and it is larger by volume than the smallest planet, Mercury, although only half as massive. Titan was the first known moon of Saturn, discovered in 1655 by the Dutch astronomer Christiaan Huygens, and was the fifth moon of a planet apart from the Earth to be discovered.[10]
Titan is primarily composed of water ice and rocky material. Much as with Venus prior to the Space Age, the dense, opaque atmosphere prevented understanding of Titan's surface until new information accumulated with the arrival of the Cassini–Huygens mission in 2004, including the discovery of liquid hydrocarbon lakes in the satellite's polar regions. The surface is geologically young; although mountains and several possible cryovolcanoes have been discovered, it is smooth and few impact craters have been found.
The atmosphere of Titan is largely composed of nitrogen; minor components lead to the formation of methane and ethane clouds and nitrogen-rich organic smog. The climate—including wind and rain—creates surface features similar to those of Earth, such as sand dunes, rivers, lakes and seas (probably of liquid methane and ethane), and deltas, and is dominated by seasonal weather patterns as on Earth. With its liquids (both surface and subsurface) and robust nitrogen atmosphere, Titan's methane cycle is viewed as an analog to Earth's water cycle, although at a much lower temperature.
The satellite is thought as a possible host for microbial extraterrestrial life or, at least, as a prebiotic environment rich in complex organic chemistry with a possible subsurface liquid ocean serving as a biotic environment.[11][12][13]
Discovery and naming
![](http://upload.wikimedia.org/wikipedia/commons/thumb/a/a4/Christiaan_Huygens-painting.jpeg/130px-Christiaan_Huygens-painting.jpeg)
Titan was discovered on March 25, 1655, by the Dutch astronomer Christiaan Huygens. Huygens was inspired by Galileo's discovery of Jupiter's four largest moons in 1610 and his improvements on telescope technology.[14] Christiaan, with the help of his brother Constantijn Huygens, Jr., began building telescopes around 1650. Christiaan Huygens discovered this first observed moon orbiting Saturn with the first telescope they built.[15]
He named it simply Saturni Luna (or Luna Saturni, Latin for "Saturn's moon"), publishing in the 1655 tract De Saturni Luna Observatio Nova. After Giovanni Domenico Cassini published his discoveries of four more moons of Saturn between 1673 and 1686, astronomers fell into the habit of referring to these and Titan as Saturn I through V (with Titan then in fourth position). Other early epithets for Titan include "Saturn's ordinary satellite".[16] Titan is officially numbered Saturn VI because after the 1789 discoveries the numbering scheme was frozen to avoid causing any more confusion (Titan having borne the numbers II and IV as well as VI). Numerous small moons have been discovered closer to Saturn since then.
The name Titan, and the names of all seven satellites of Saturn then known, came from John Herschel (son of William Herschel, discoverer of Mimas and Enceladus) in his 1847 publication Results of Astronomical Observations Made at the Cape of Good Hope.[17] He suggested the names of the mythological Titans (Ancient Greek: Τῑτάν), sisters and brothers of Kronos, the Greek Saturn. In Greek mythology, the Titans were a race of powerful deities, descendants of Gaia and Uranus, that ruled during the legendary Golden Age.
Orbit and rotation
![](http://upload.wikimedia.org/wikipedia/commons/thumb/3/3f/Titan%27s_orbit.svg/220px-Titan%27s_orbit.svg.png)
Titan orbits Saturn once every 15 days and 22 hours. Like many of the other satellites of the gas giants and Earth's Moon, its rotational period is identical to its orbital period; Titan is thus tidally locked in synchronous rotation with Saturn, and always shows one face to the planet. Because of this, there is a sub-Saturnian point on its surface, from which the planet would appear to hang directly overhead. Longitudes on Titan are measured westward from the meridian passing through this point.[18] Its orbital eccentricity is 0.0288, and the orbital plane is inclined 0.348 degrees relative to the Saturnian equator.[1] Viewed from Earth, the moon reaches an angular distance of about 20 Saturn radii (just over 1.2 million kilometers) from Saturn and subtends a disk 0.8 arcseconds in diameter.
The small, irregularly shaped satellite Hyperion is locked in a 3:4 orbital resonance with Titan. A "slow and smooth" evolution of the resonance—in which Hyperion would have migrated from a chaotic orbit—is considered unlikely, based on models. Hyperion probably formed in a stable orbital island, while the massive Titan absorbed or ejected bodies that made close approaches.[19]
Bulk characteristics
Titan is 5,150 km across, compared to 4,879 km for the planet Mercury, 3,474 km for Earth's Moon, and 12,742 km for the Earth. Before the arrival of Voyager 1 in 1980, Titan was thought to be slightly larger than Ganymede (diameter 5,262 km) and thus the largest moon in the Solar System; this was an overestimation caused by Titan's dense, opaque atmosphere, which extends many kilometres above its surface and increases its apparent diameter.[20] Titan's diameter and mass (and thus its density) are similar to those of the Jovian moons Ganymede and Callisto.[21] Based on its bulk density of 1.88 g/cm3, Titan's bulk composition is half water ice and half rocky material. Though similar in composition to Dione and Enceladus, it is denser due to gravitational compression.
Titan is likely differentiated into several layers with a 3,400 km rocky center surrounded by several layers composed of different crystal forms of ice.[22] Its interior may still be hot and there may be a liquid layer consisting of a "magma" composed of water and ammonia between the ice Ih crust and deeper ice layers made of high-pressure forms of ice. The presence of ammonia allows water to remain liquid even at temperatures as low as 176 K (−97 °C) (for eutectic mixture with water).[23] Evidence for such an ocean has recently been uncovered by the Cassini probe in the form of natural extremely-low-frequency (ELF) radio waves in Titan's atmosphere. Titan's surface is thought to be a poor reflector of ELF waves, so they may instead be reflecting off the liquid–ice boundary of a subsurface ocean.[24] Surface features were observed by the Cassini spacecraft to systematically shift by up to 30 km between October 2005 and May 2007, which suggests that the crust is decoupled from the interior, and provides additional evidence for an interior liquid layer.[25]
An early 2000 study by the DLR Institute of Planetary Research at Berlin-Adlershof placed Titan in a "large icy satellite" group along with the Galilean moons Callisto and Ganymede.[26]
Atmosphere
![](http://upload.wikimedia.org/wikipedia/commons/thumb/b/b7/Titan-Complex_%27Anti-greenhouse%27.jpg/220px-Titan-Complex_%27Anti-greenhouse%27.jpg)
Titan is the only known moon with more than a trace of atmosphere, and is the only dense, nitrogen-rich atmosphere in the Solar System aside from the Earth's. Observations of the atmosphere, made in 2004 by Cassini, suggest that Titan is a "super rotator", like Venus, with an atmosphere that rotates much faster than its surface.[27] Observations from the Voyager space probes have shown that the Titanian atmosphere is denser than Earth's, with a surface pressure about 1.45 times that of Earth's. Titan's atmosphere is about 1.19 times as massive as Earth's overall,[28] or about 7.3 times more massive on a per surface area basis. It supports opaque haze layers that block most visible light from the Sun and other sources and renders Titan's surface features obscure.[29] Titan's lower gravity means that its atmosphere is far more extended than Earth's.[30] The atmosphere of Titan is opaque at many wavelengths and a complete reflectance spectrum of the surface is impossible to acquire from orbit.[31] It was not until the arrival of the Cassini–Huygens mission in 2004 that the first direct images of Titan's surface were obtained.[32]
The atmospheric composition in the stratosphere is 98.4% nitrogen with the remaining 1.6% composed mostly of methane (1.4%) and hydrogen (0.1–0.2%).[7] There are trace amounts of other hydrocarbons, such as ethane, diacetylene, methylacetylene, acetylene and propane, and of other gases, such as cyanoacetylene, hydrogen cyanide, carbon dioxide, carbon monoxide, cyanogen, argon and helium.[6] The hydrocarbons are thought to form in Titan's upper atmosphere in reactions resulting from the breakup of methane by the Sun's ultraviolet light, producing a thick orange smog.[33]
Climate
![](http://upload.wikimedia.org/wikipedia/commons/thumb/d/da/Vortex_on_saturn%27s_moon_titan.png/220px-Vortex_on_saturn%27s_moon_titan.png)
Titan's surface temperature is about 94 K (−179 °C, or −290 °F). At this temperature water ice has an extremely low vapor pressure, so the atmosphere is nearly free of water vapor. The haze in Titan's atmosphere contributes to the moon's anti-greenhouse effect by reflecting sunlight back into space, making its surface significantly colder than its upper atmosphere.[34] The moon receives just about 1% of the amount of sunlight Earth gets.[35] Titan's clouds, probably composed of methane, ethane or other simple organics, are scattered and variable, punctuating the overall haze.[20] This atmospheric methane conversely creates a greenhouse effect on Titan's surface, without which Titan would be far colder.[36] The findings of the Huygens probe indicate that Titan's atmosphere periodically rains liquid methane and other organic compounds onto the moon's surface.[37]
Clouds typically cover 1% of Titan's disk, though outburst events have been observed in which the cloud cover rapidly expands to as much as 8%. One hypothesis asserts that the southern clouds are formed when heightened levels of sunlight during the Titanian summer generate uplift in the atmosphere, resulting in convection. This explanation is complicated by the fact that cloud formation has been observed not only post–summer solstice but also at mid-spring. Increased methane humidity at the south pole possibly contributes to the rapid increases in cloud size.[38] There had been summer in Titan's southern hemisphere until 2010, when Saturn's orbit, which governs the moon's motion, tilted the northern hemisphere towards the Sun.[39] When the seasons switch, it is expected that ethane will begin to condense over the south pole.[40]
Surface features
![](http://upload.wikimedia.org/wikipedia/commons/thumb/4/45/Map_of_Titan_-_April_2011.jpg/300px-Map_of_Titan_-_April_2011.jpg)
The surface of Titan has been described as "complex, fluid-processed, [and] geologically young".[41] It is believed that both: Titan has been around since the solar system's formation, and a recent event shaped Titan's surface.[42] Titan’s atmosphere is twice as thick as the Earth's, making it difficult for astronomical instruments to image its surface in the visible light spectrum.[43] The Cassini spacecraft is using infrared instruments, radar altimetry and synthetic aperture radar (SAR) imaging to map portions of Titan during its close fly-bys of the moon. The first images revealed a diverse geology, with both rough and smooth areas. There are features that seem volcanic in origin, which probably disgorge water mixed with ammonia. There are also streaky features, some of them hundreds of kilometers in length, that appear to be caused by windblown particles.[44][45] Examination has also shown the surface to be relatively smooth; the few objects that seem to be impact craters appeared to have been filled in, perhaps by raining hydrocarbons or volcanoes. Radar altimetry suggests height variation is low, typically no more than 150 meters. Occasional elevation changes of 500 meters have been discovered and Titan has mountains that sometimes reach several hundred meters to more than 1 kilometer in height.[46]
Titan's surface is marked by broad regions of bright and dark terrain. These include Xanadu, a large, reflective equatorial area about the size of Australia. It was first identified in infrared images from the Hubble Space Telescope in 1994, and later viewed by the Cassini spacecraft. The convoluted region is filled with hills and cut by valleys and chasms.[47] It is criss-crossed in places by dark lineaments—sinuous topographical features resembling ridges or crevices. These may represent tectonic activity, which would indicate that Xanadu is geologically young. Alternatively, the lineaments may be liquid-formed channels, suggesting old terrain that has been cut through by stream systems.[48] There are dark areas of similar size elsewhere on the moon, observed from the ground and by Cassini; it had been speculated that these are methane or ethane seas, but Cassini observations seem to indicate otherwise (see below).
Liquids
![](http://upload.wikimedia.org/wikipedia/commons/thumb/e/e8/PIA10008_Seas_and_Lakes_on_Titan.jpg/220px-PIA10008_Seas_and_Lakes_on_Titan.jpg)
The possibility of hydrocarbon seas on Titan was first suggested based on Voyager 1 and 2 data that showed Titan to have a thick atmosphere of approximately the correct temperature and composition to support them, but direct evidence was not obtained until 1995 when data from Hubble and other observations suggested the existence of liquid methane on Titan, either in disconnected pockets or on the scale of satellite-wide oceans, similar to water on Earth.[49]
The Cassini mission confirmed the former hypothesis, although not immediately. When the probe arrived in the Saturnian system in 2004, it was hoped that hydrocarbon lakes or oceans might be detectable by reflected sunlight from the surface of any liquid bodies, but no specular reflections were initially observed.[50] Near Titan's south pole, an enigmatic dark feature named Ontario Lacus was identified[51] (and later confirmed to be a lake).[52] A possible shoreline was also identified near the pole via radar imagery.[53] Following a flyby on July 22, 2006, in which the Cassini spacecraft's radar imaged the northern latitudes (which were then in winter), a number of large, smooth (and thus dark to radar) patches were seen dotting the surface near the pole.[54] Based on the observations, scientists announced "definitive evidence of lakes filled with methane on Saturn's moon Titan" in January 2007.[9][55] The Cassini–Huygens team concluded that the imaged features are almost certainly the long-sought hydrocarbon lakes, the first stable bodies of surface liquid found outside of Earth. Some appear to have channels associated with liquid and lie in topographical depressions.[9] Channels in some regions have created surprisingly little erosion, suggesting erosion on Titan is extremely slow, or some other recent phenomena may have wiped out older riverbeds and landforms.[56][42] The liquid erosion features appear to be a very recent occurrence. [42] Overall, the Cassini radar observations have shown that lakes cover only a few percent of the surface, making Titan much drier than Earth.[57] Although most of the lakes are concentrated near the poles (where the relative lack of sunlight prevents evaporation), a number of long-standing hydrocarbon lakes in the equatorial desert regions have also been discovered, including one near the Huygens landing site in the Shangri-La region which is about half the size of Utah's Great Salt Lake. The equatorial lakes are probably "oases", i.e. the likely supplier is underground aquifers.[58]
In June 2008, the Visual and Infrared Mapping Spectrometer on Cassini confirmed the presence of liquid ethane beyond doubt in Ontario Lacus.[59] On December 21, 2008, Cassini passed directly over Ontario Lacus and observed specular reflection in radar. The strength of the reflection saturated the probe's receiver, indicating that the lake level did not vary by more than 3 mm (implying either that surface winds were minimal, or the lake's hydrocarbon fluid is viscous).[60][61]
Specular reflections are indicative of a smooth, mirror-like surface, so the observation corroborated the inference of the presence of a large liquid body drawn from radar imaging. The observation was made soon after the north polar region emerged from 15 years of winter darkness.
On July 8, 2009, Cassini's VIMS observed a specular reflection indicative of a smooth, mirror-like surface, off what today is called Jingpo Lacus, a lake in the north polar region shortly after the area emerged from 15 years of winter darkness.[62][63]
Radar measurements made in July 2009 and January 2010 indicate that Ontario Lacus is extremely shallow, with an average depth of 0.4–3.2 m, and a maximum depth of 2.9–7.4 m.[64] In contrast, the northern hemisphere's Ligeia Mare has depths exceeding 8 m, the maximum measurable by the radar instrument.[64]
During six flybys of Titan from 2006 to 2011, Cassini gathered radio-metric tracking and optical navigation data from which investigators could roughly infer the changing shape of the moon. The density of Titan is consistent with a body that is about 60% rock and 40% water. The team’s analyses suggest that the surface of the moon can rise and fall by up to 10 metres during each orbit. That degree of warpage suggests that Titan’s interior is relatively deformable, and that the most likely model of Titan is one in which an icy shell dozens of kilometres thick floats atop a global ocean.[65] The team's findings, together with the results of previous studies, hint that Titan’s ocean may lie no more than 100 km below the moon’s surface.[65][66].
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Photo of infrared specular reflection off Jingpo Lacus, a lake in the north polar region | Perspective radar view of Bolsena Lacus (lower right) and other northern hemisphere hydrocarbon lakes | Contrasting images of the number of lakes in Titan's northern hemisphere (left) and southern hemisphere (right) | Two images of Titan's southern hemisphere acquired one year apart, showing changes in south polar lakes |
Impact craters
![](http://upload.wikimedia.org/wikipedia/commons/thumb/8/8e/Titancrater.jpg/220px-Titancrater.jpg)
Radar, SAR and imaging data from Cassini have revealed few impact craters on Titan's surface.[42] These impacts appear to be relatively young, opposed to the moon's age.[42] The few impact craters discovered include a 440 km wide two-ring impact basin named Menrva seen by Cassini's ISS as a bright-dark concentric pattern.[68] A smaller, 60 km wide, flat-floored crater named Sinlap[69] and a 30 km crater with a central peak and dark floor named Ksa have also been observed.[70] Radar and Cassini imaging have also revealed a number of "crateriforms", circular features on the surface of Titan that may be impact related, but lack certain features that would make identification certain. For example, a 90 km wide ring of bright, rough material known as Guabonito has been observed by Cassini.[71] This feature is thought to be an impact crater filled in by dark, windblown sediment. Several other similar features have been observed in the dark Shangri-la and Aaru regions. Radar observed several circular features that may be craters in the bright region Xanadu during Cassini's April 30, 2006 flyby of Titan.[72]
Many of Titan's craters or probable craters display evidence of extensive erosion, and all show some indication of modification.[67] Most large craters have breached or incomplete rims, despite the fact that some craters on Titan have relatively more massive rims than those anywhere else in the Solar System. However, there is little evidence of formation of palimpsests through viscoelastic crustal relaxation, unlike on other large icy moons.[67] Most craters lack central peaks and have smooth floors, possibly due to impact-generation or later eruption of cryovolcanic lava. While infill from various geological processes is one reason for Titan's relative deficiency of craters, atmospheric shielding also plays a role; it is estimated that Titan's atmosphere reduces the number of craters on its surface by a factor of two.[73]
The limited high resolution radar coverage of Titan obtained through 2007 (22%) suggested the existence of a number of nonuniformities in its crater distribution. Xanadu has 2–9 times more craters than elsewhere. The leading hemisphere has a 30% higher density than the trailing hemisphere. There are lower crater densities in areas of equatorial dunes and in the north polar region (where hydrocarbon lakes and seas are most common).[67]
Pre-Cassini models of impact trajectories and angles suggest that where the impactor strikes the water ice crust, a small amount of ejecta remains as liquid water within the crater. It may persist as liquid for centuries or longer, sufficient for "the synthesis of simple precursor molecules to the origin of life".[74]
Cryovolcanism and mountains
![](http://upload.wikimedia.org/wikipedia/commons/thumb/f/fa/Tortola_Facula_in_infrared.jpg/220px-Tortola_Facula_in_infrared.jpg)
![](http://upload.wikimedia.org/wikipedia/commons/thumb/3/30/Sotra_Facula.jpg/220px-Sotra_Facula.jpg)
Scientists have long speculated that conditions on Titan resemble those of early Earth, though at a much lower temperature. The detection of Argon 40 in the atmosphere in 2004 indicated that volcanoes had spawned plumes of "lava" composed of water and ammonia.[75] Global maps of the lake distribution on Titan's surface revealed that there is not enough surface methane to account for its continued presence in its atmosphere, and thus that a significant portion must be added through volcanic processes.[76]
Still there is a paucity of surface features which can be unambiguously interpreted as cryovolcanoes.[77] One of the first of such features revealed by Cassini radar observations in 2004, called Ganesa Macula, resembles the geographic features called "pancake domes" found on Venus, and was thus initially thought to be cryovolcanic in origin, although the American Geophysical Union refuted this hypothesis in December 2008. The feature was found to be not a dome at all, but appeared to result from accidental combination of light and dark patches.[78][79] In 2004 Cassini also detected an unusually bright feature (called Tortola Facula), which was interpreted as a cryovolcanic dome.[80] No similar features have been identified as of 2010.[81] In December 2008, astronomers announced the discovery of two transient but unusually long-lived "bright spots" in Titan's atmosphere, which appear too persistent to be explained by mere weather patterns, suggesting they were the result of extended cryovolcanic episodes.[23]
In March, 2009, structures resembling lava flows were announced in a region of Titan called Hotei Orcus, which appears to fluctuate in brightness over several months. Though many phenomena were suggested to explain this fluctuation, the lava flows were found to rise 200 meters above Titan's surface, consistent with it having been erupted from beneath the surface.[82]
A mountain range measuring 150 km long, 30 km wide and 1.5 km high was also discovered by Cassini in 2006. This range lies in the southern hemisphere and is thought to be composed of icy material and covered in methane snow. The movement of tectonic plates, perhaps influenced by a nearby impact basin, could have opened a gap through which the mountain's material upwelled.[83] Prior to Cassini, scientists assumed that most of the topography on Titan would be impact structures, yet these findings reveal that similar to Earth, the mountains were formed through geological processes.[84] In December 2010, the Cassini mission team announced the most compelling possible cryovolcano yet found. Named Sotra Facula, it is one in a chain of at least three mountains, each between 1000 and 1500 m in height, several of which are topped by large craters. The ground around their bases appears to be overlaid by frozen lava flows.[85]
If volcanism on Titan really exists, the hypothesis is that it is driven by energy released from the decay of radioactive elements within the mantle, as it is on the Earth.[23] Magma on Earth is made of liquid rock, which is less dense than the solid rocky crust through which it erupts. Because ice is less dense than water, Titan's watery magma would be denser than its solid icy crust. This means that cryovolcanism on Titan would require a large amount of additional energy to operate, possibly via tidal flexing from nearby Saturn.[23] Alternatively, the pressure necessary to drive the cryovolcanoes may be caused by ice Ih "underplating" Titan's outer shell. The low-pressure ice, overlaying a liquid layer of ammonium sulfate, ascends buoyantly, and the unstable system can produce dramatic plume events. Titan is resurfaced through the process by grain-sized ice and ammonium sulfate ash, which helps produce a wind-shaped landscape and sand dune features.[86]
In 2008 Jeffrey Moore (planetary geologist of Ames Research Center) proposed an alternate view of Titan's geology. Noting that no volcanic features had been unambiguously identified on Titan so far, he asserted that Titan is a geologically dead world, whose surface is shaped only by impact cratering, fluvial and eolian erosion, mass wasting and other exogenic processes. According to this hypothesis, methane is not emitted by volcanoes but slowly diffuses out of Titan's cold and stiff interior. Ganesa Macula may be an eroded impact crater with a dark dune in the center. The mountainous ridges observed in some regions can be explained as heavily degraded scarps of large multi-ring impact structures or as a result of the global contraction due to the slow cooling of the interior. Even in this case Titan may still have an internal ocean made of the eutectic water–ammonia mixture with the temperature of 176 K (−97 °C), which is low enough to be explained by the decay of radioactive elements in the core. The bright Xanadu terrain may be a degraded heavily cratered terrain similar to that observed on the surface of Callisto. Indeed, were it not for its lack of an atmosphere, Callisto could serve as a model for Titan's geology in this scenario. Jeffrey Moore even called Titan Callisto with weather.[77][87]
Dark terrain
![](http://upload.wikimedia.org/wikipedia/commons/thumb/d/da/Titan_dunes_crop.png/220px-Titan_dunes_crop.png)
In the first images of Titan's surface taken by Earth-based telescopes in the early 2000s, large regions of dark terrain were revealed straddling Titan's equator.[88] Prior to the arrival of Cassini, these regions were thought to be seas of organic matter like tar or liquid hydrocarbons.[89] Radar images captured by the Cassini spacecraft have instead revealed some of these regions to be extensive plains covered in longitudinal sand dunes, up to 330 meters high[90] about a kilometer wide, and tens to hundreds of kilometers long.[91] The longitudinal (or linear) dunes are presumed to be formed by moderately variable winds that either follow one mean direction or alternate between two different directions. Dunes of this type are always aligned with average wind direction. In the case of Titan, steady zonal (eastward) winds combine with variable tidal winds (approximately 0.5 meters per second).[92] The tidal winds are the result of tidal forces from Saturn on Titan's atmosphere, which are 400 times stronger than the tidal forces of the Moon on Earth and tend to drive wind toward the equator. This wind pattern causes sand dunes to build up in long parallel lines aligned west-to-east. The dunes break up around mountains, where the wind direction shifts.
The sand on Titan might have formed when liquid methane rained and eroded the ice bedrock, possibly in the form of flash floods. Alternatively, the sand could also have come from organic solids produced by photochemical reactions in Titan's atmosphere.[90][92][93] Studies of dunes' composition in May 2008 revealed that they possessed less water than the rest of Titan, and are most likely to derive from organic material clumping together after raining onto the surface.[94]
Observation and exploration
![](http://upload.wikimedia.org/wikipedia/commons/thumb/c/c7/Titan%27s_thick_haze_layer-picture_from_voyager1.jpg/200px-Titan%27s_thick_haze_layer-picture_from_voyager1.jpg)
Titan is never visible to the naked eye, but can be observed through small telescopes or strong binoculars. Amateur observation is difficult because of the proximity of the satellite to Saturn's brilliant globe and ring system; an occulting bar, covering part of the eyepiece and used to block the bright planet, greatly improves viewing.[95] Titan has a maximum apparent magnitude of +8.2,[5] and mean opposition magnitude 8.4.[96] This compares to +4.6[96] for the similarly sized Ganymede, in the Jovian system.
Observations of Titan prior to the space age were limited. In 1907 Spanish astronomer Josep Comas Solá suggested that he had observed darkening near the edges of Titan's disk and two round, white patches in its center. The deduction of an atmosphere by Kuiper in the 1940s was the next major observational event.[97]
The first probe to visit the Saturnian system was Pioneer 11 in 1979, which determined that Titan was probably too cold to support life.[98] The craft took the first images of the moon (including some of it and Saturn together), but these were of low quality; the first-ever close-up of Titan was taken on September 2, 1979.[99]
Titan was examined by both Voyager 1 and 2 in 1980 and 1981, respectively. Voyager 1's course was diverted specifically to make a closer pass of Titan. Unfortunately, the craft did not possess any instruments that could penetrate Titan's haze, an unforeseen factor. Many years later, intensive digital processing of images taken through Voyager 1's orange filter did reveal hints of the light and dark features now known as Xanadu and Shangri-la,[100] but by then they had already been observed in the infrared by the Hubble Space Telescope. Voyager 2 took only a cursory look at Titan. The Voyager 2 team had the option of steering the spacecraft to take a detailed look at Titan or to use another trajectory which would allow it to visit Uranus and Neptune. Given the lack of surface features seen by Voyager 1, the latter plan was implemented.
Cassini–Huygens
Even with the data provided by the Voyagers, Titan remained a body of mystery—a planet-like satellite shrouded in an atmosphere that makes detailed observation difficult. The intrigue that had surrounded Titan since the 17th-century observations of Christiaan Huygens and Giovanni Cassini was gratified by a spacecraft named in their honor.
The Cassini–Huygens spacecraft reached Saturn on July 1, 2004, and has begun the process of mapping Titan's surface by radar. A joint project of the European Space Agency (ESA) and NASA, Cassini–Huygens has proved a very successful mission. The Cassini probe flew by Titan on October 26, 2004, and took the highest-resolution images ever of the moon's surface, at only 1,200 km, discerning patches of light and dark that would be invisible to the human eye from the Earth. Huygens landed[101] on Titan on January 14, 2005, discovering that many of the moon's surface features seem to have been formed by flowing fluids at some point in the past.[102] On July 22, 2006, Cassini made its first targeted, close fly-by at 950 km from Titan; the closest flyby was at 880 km on June 21, 2010.[103] Present liquid on the surface has been found in abundance in the north polar region, in the form of many lakes and seas discovered by Cassini.[54] Titan is the most distant body from Earth[104] and the second moon in the Solar System to have a space probe land on its surface.
Huygens landing site
On January 14, 2005, the Huygens probe landed on the surface of Titan, just off the easternmost tip of a bright region now called Adiri. The probe photographed pale hills with dark "rivers" running down to a dark plain. Current understanding is that the hills (also referred to as highlands) are composed mainly of water ice. Dark organic compounds, created in the upper atmosphere by the ultraviolet radiation of the Sun, may rain from Titan's atmosphere. They are washed down the hills with the methane rain and are deposited on the plains over geological time scales.[105]
After landing, Huygens photographed a dark plain covered in small rocks and pebbles, which are composed of water ice.[105] The two rocks just below the middle of the image on the right are smaller than they may appear: the left-hand one is 15 centimeters across, and the one in the center is 4 centimeters across, at a distance of about 85 centimeters from Huygens. There is evidence of erosion at the base of the rocks, indicating possible fluvial activity. The surface is darker than originally expected, consisting of a mixture of water and hydrocarbon ice. The assumption is that the "soil" visible in the images is precipitation from the hydrocarbon haze above.
In March 2007, NASA, ESA, and COSPAR decided to name the Huygens landing site the Hubert Curien Memorial Station in memory of the former president of the ESA.[106]
Future missions
![](http://upload.wikimedia.org/wikipedia/commons/thumb/5/57/TSSM-TandEM-Montgolfiere.jpg/180px-TSSM-TandEM-Montgolfiere.jpg)
The Titan Saturn System Mission (TSSM) is a joint NASA/ESA proposal for exploration of Saturn's moons.[107] It envisions a hot-air balloon to float in the moon's atmosphere for six months. It was competing against the Europa Jupiter System Mission (EJSM) proposal for funding. In February 2009 it was announced that ESA/NASA had given the EJSM mission priority ahead of the TSSM,[108] although TSSM will continue to be studied for a later launch date. There has also been a proposal for a Titan Mare Explorer (TiME), which would be a low-cost lander that would splash down in a lake near Titan's north pole and float on the surface of the lake for 3 to 6 months. It could launch as early as 2016 and arrive in 2023.[109][110][111]
Prebiotic conditions and possible life
While the Cassini–Huygens mission was not equipped to provide evidence for biosignatures or complex organic compounds, it showed an environment on Titan that is similar, in some ways, to ones theorized for the primordial Earth.[112] Scientists surmise that the atmosphere of early Earth was similar in composition to the current atmosphere on Titan, with the important exception of a lack of water vapor on Titan.[113] The satellite is thought by some scientists as a possible host for microbial extraterrestrial life or, at least, as a prebiotic environment rich in complex organic compounds.
Formation of complex molecules
The Miller-Urey experiment and several following experiments have shown that with an atmosphere similar to that of Titan and the addition of UV radiation, complex molecules and polymer substances like tholins can be generated. The reaction starts with dissociation of nitrogen and methane, forming hydrogen cyanide and acetylene. Further reactions have been studied extensively.[114]
In October 2010, Sarah Horst of the University of Arizona reported finding the five nucleotide bases—building blocks of DNA and RNA—among the many compounds produced when energy was applied to a combination of gases like those in Titan's atmosphere. Horst also found amino acids, the building blocks of protein. She said it was the first time nucleotide bases and amino acids had been found in such an experiment without liquid water being present.[115]
Possible subsurface habitats
Laboratory simulations have led to the suggestion that enough organic material exists on Titan to start a chemical evolution analogous to what is thought to have started life on Earth. While the analogy assumes the presence of liquid water for longer periods than is currently observable, several theories suggest that liquid water from an impact could be preserved under a frozen isolation layer.[116] It has also been observed that liquid ammonia oceans could exist deep below the surface;[11][117] one model suggests an ammonia–water solution as much as 200 km deep beneath a water ice crust, conditions that, "while extreme by terrestrial standards, are such that life could indeed survive".[12] Heat transfer between the interior and upper layers would be critical in sustaining any sub-surface oceanic life.[11] Detection of microbial life on Titan would depend on its biogenic effects. That the atmospheric methane and nitrogen might be of biological origin has been examined, for example.[12]
Methane and life at the surface
It has been suggested that life could exist in the lakes of liquid methane on Titan, just as organisms on Earth live in water.[118] Such creatures would inhale H2 in place of O2, metabolize it with acetylene instead of glucose, and exhale methane instead of carbon dioxide.[118][119]
Although all living things on Earth (including methanogens) use liquid water as a solvent, it is speculated that life on Titan might instead use a liquid hydrocarbon, such as methane or ethane.[120] Water is a stronger solvent than methane.[121] However, water is also more chemically reactive, and can break down large organic molecules through hydrolysis.[120] A life-form whose solvent was a hydrocarbon would not face the risk of its biomolecules being destroyed in this way.[120]
In 2005, astrobiologist Chris McKay argued that if methanogenic life did exist on the surface of Titan, it would likely have a measurable effect on the mixing ratio in the Titan troposphere: levels of hydrogen and acetylene would be measurably lower than otherwise expected.[118]
In 2010, Darrell Strobel, from Johns Hopkins University, identified a greater abundance of molecular hydrogen in the upper atmospheric layers of Titan compared to the lower layers, arguing for a downward flow at a rate of roughly 1025 molecules per second and disappearance of hydrogen near Titan's surface; as Strobel noted, his findings were in line with the effects Chris McKay had predicted if methanogenic life-forms were present.[118][121][122] The same year, another study showed low levels of acetylene on Titan's surface, which were interpreted by Chris McKay as consistent with the hypothesis of organisms consuming hydrocarbons.[121] While restating the biological hypothesis, McKay cautioned that other explanations for the hydrogen and acetylene findings are more likely: the possibilities of yet unidentified physical or chemical processes (e.g., a surface catalyst accepting hydrocarbon or hydrogen), or flaws in the current models of material flow.[13] Composition data and transport models need to be substantiated, and, per Occam's razor, a physical or chemical explanation is preferred a priori over one of biology (given the simplicity of chemical catalysts versus the complexity of biological forms). Even so, McKay notes that discovery of either, including simply of a catalyst effective at 95°K (-180°C, -290°F), would be an important discovery.[13]
As NASA notes in its news article on the June 2010 findings: "To date, methane-based life forms are only hypothetical. Scientists have not yet detected this form of life anywhere".[121] As the NASA statement also says: "some scientists believe these chemical signatures bolster the argument for a primitive, exotic form of life or precursor to life on Titan's surface."[121]
Obstacles
Despite these biological possibilities, there are formidable obstacles to life on Titan, and any analogy to Earth is inexact. At a vast distance from the Sun, Titan is frigid (a fact exacerbated by the anti-greenhouse effect of its cloud cover), and its atmosphere lacks CO2. Because of these difficulties, scientists such as Jonathan Lunine have viewed Titan less as a likely habitat for life, than as an experiment for examining theories on the conditions that prevailed prior to the appearance of life on Earth.[123] While life itself may not exist, the prebiotic conditions of the Titanian environment and the associated organic chemistry remain of great interest in understanding the early history of the terrestrial biosphere.[112] Using Titan as a prebiotic experiment involves not only observation through spacecraft, but laboratory experiment, and chemical and photochemical modeling on Earth.[114]
Panspermia hypothesis
An alternate explanation for life's hypothetical existence on Titan has been proposed: if life were to be found on Titan, it would be statistically more likely to have originated from Earth than to have appeared independently, a process known as panspermia. It is theorized that large asteroid and cometary impacts on Earth's surface have caused hundreds of millions of fragments of microbe-laden rock to escape Earth's gravity. Calculations indicate that a number of these would encounter many of the bodies in the Solar System, including Titan.[124][125] On the other hand, Jonathan Lunine has argued that any living things in Titan's cryogenic hydrocarbon lakes would need to be so different chemically from Earth life that it would not be possible for one to be the ancestor of the other.[126]
Future conditions
Conditions on Titan could become far more habitable in the future. Six billion years from now, as the Sun becomes a red giant, surface temperatures could rise to ~200 K (−70 °C), high enough for stable oceans of water/ammonia mixture to exist on the surface. As the Sun's ultraviolet output decreases, the haze in Titan's upper atmosphere will be depleted, lessening the anti-greenhouse effect on the surface and enabling the greenhouse created by atmospheric methane to play a far greater role. These conditions together could create an environment agreeable to forms of life, and will persist for several hundred million years. This was sufficient time for simple life to evolve on Earth, although the presence of ammonia on Titan would cause the same chemical reactions to proceed more slowly.[127]
See also
References
- ^ a b Unless otherwise specified: "JPL HORIZONS solar system data and ephemeris computation service". Solar System Dynamics. NASA, Jet Propulsion Laboratory. Retrieved August 19, 2007.
- ^ a b c
Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1086/508812 , please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with
|doi=10.1086/508812
instead. - ^
Williams, D. R. (August 21, 2008). "Saturnian Satellite Fact Sheet". NASA. Retrieved 2000-04-18.
{{cite web}}
: Check date values in:|accessdate=
(help) - ^ Mitri, G.; Showman, Adam P.; Lunine, Jonathan I.; Lorenz, Ralph D. (2007). "Hydrocarbon Lakes on Titan" (PDF). Icarus. 186 (2): 385–394. Bibcode:2007Icar..186..385M. doi:10.1016/j.icarus.2006.09.004.
- ^ a b "Classic Satellites of the Solar System". Observatorio ARVAL. Retrieved June 28, 2010.
- ^ a b Niemann; H. B.; Bauer, S. J.; Carignan, G. R.; Demick, J. E.; Frost, R. L.; Gautier, D.; Haberman, J. A.; Harpold, D. N. (2005). "The abundances of constituents of Titan's atmosphere from the GCMS instrument on the Huygens probe". Nature. 438 (7069): 779–784. Bibcode:2005Natur.438..779N. doi:10.1038/nature04122. PMID 16319830.
- ^ a b c Coustenis, pp. 154–155
- ^ "News Features: The Story of Saturn". Cassini–Huygens Mission to Saturn & Titan. NASA & JPL. Retrieved January 8, 2007.
- ^ a b c Stofan, E. R.; Elachi, C.; Lunine, J. I.; Lorenz, R. D.; Stiles, B.; Mitchell, K. L.; Ostro, S.; Soderblom, L.; Wood, C. (2007). "The lakes of Titan". Nature. 445 (1): 61–64. Bibcode:2007Natur.445...61S. doi:10.1038/nature05438. PMID 17203056.
- ^
Nemiroff, R. and Bonnell, J. (March 25, 2005). "Huygens Discovers Luna Saturni". Astronomy Picture of the Day. NASA. Retrieved August 18, 2007.
{{cite web}}
: CS1 maint: multiple names: authors list (link) - ^ a b c
Grasset, O.; Sotin, C.; Deschamps, F. (2000). "On the internal structure and dynamic of Titan". Planetary and Space Science. 48 (7–8): 617–636. Bibcode:2000P&SS...48..617G. doi:10.1016/S0032-0633(00)00039-8.
{{cite journal}}
: CS1 maint: multiple names: authors list (link) - ^ a b c Fortes, A. D. (2000). "Exobiological implications of a possible ammonia-water ocean inside Titan". Icarus. 146 (2): 444–452. Bibcode:2000Icar..146..444F. doi:10.1006/icar.2000.6400.
- ^ a b c Mckay, Chris (2010). "Have We Discovered Evidence For Life On Titan". SpaceDaily. Retrieved June 10, 2010. Space.com. March 23, 2010. Cite error: The named reference "life?" was defined multiple times with different content (see the help page).
- ^ "Discoverer of Titan: Christiaan Huygens". European Space Agency. September 4, 2008. Retrieved April 18, 2009.
- ^ Telescope by Huygens, Christiaan Huygens, The Hague, 1683 Inv V09196, Rijksmuseum voor de Geschiedenis van de Natuurwetenschappen en van de Geneeskunde
- ^ Cassini, G. D. (1673). "A Discovery of two New Planets about Saturn, made in the Royal Parisian Observatory by Signor Cassini, Fellow of both the Royal Societys, of England and France; English't out of French". Philosophical Transactions. 8 (1673): 5178–5185. doi:10.1098/rstl.1673.0003.
- ^ Lassell (November 12, 1847). "Observations of Mimas, the closest and most interior satellite of Saturn". Monthly Notices of the Royal Astronomical Society. 8 (1): 42. Retrieved March 29, 2005.
- ^ "EVS-Islands: Titan's Unnamed Methane Sea". Retrieved October 22, 2009.
- ^ Bevilacqua, R. (1980). "Resonances and close approaches. I. The Titan-Hyperion case". Earth, Moon, and Planets. 22 (2): 141–152. Bibcode:1980M&P....22..141B. doi:10.1007/BF00898423.
{{cite journal}}
: Unknown parameter|coauthors=
ignored (|author=
suggested) (help) - ^ a b Arnett, Bill (2005). "Titan". Nine planets. University of Arizona, Tucson. Archived from the original on November 21, 2005. Retrieved April 10, 2005.
{{cite web}}
: Unknown parameter|deadurl=
ignored (|url-status=
suggested) (help) - ^ Lunine, J. (March 21, 2005). "Comparing the Triad of Great Moons". Astrobiology Magazine. Retrieved July 20, 2006.
- ^ Tobie, G.; Grasset, Olivier; Lunine, Jonathan I.; Mocquet, Antoine; Sotin, Christophe (2005). "Titan's internal structure inferred from a coupled thermal-orbital model". Icarus. 175 (2): 496–502. Bibcode:2005Icar..175..496T. doi:10.1016/j.icarus.2004.12.007.
- ^ a b c d Longstaff, Alan (February 2009). "Is Titan (cryo)volcanically active?". Astronomy Now: 19.
{{cite journal}}
: More than one of|work=
and|journal=
specified (help) - ^ "Titan's Mysterious Radio Wave". ESA Cassini-Huygens web site. June 1, 2007. Retrieved March 25, 2010.
- ^ Shiga, David Titan's changing spin hints at hidden ocean, New Scientist, March 20, 2008
- ^ DLR Interior Structure of Planetary Bodies DLR Radius to Density The natural satellites of the giant outer planets...
- ^ "Wind or Rain or Cold of Titan's Night?". Astrobiology Magazine. March 11, 2005. Archived from the original on July 17, 2007. Retrieved August 24, 2007.
- ^ Coustenis, p. 130
- ^ Zubrin, Robert (1999). Entering Space: Creating a Spacefaring Civilization. Section: Titan: Tarcher/Putnam. pp. 163–166. ISBN 1-58542-036-0.
- ^ Turtle, Elizabeth P. (2007). "Exploring the Surface of Titan with Cassini–Huygens". Smithsonian. Retrieved April 18, 2009.
- ^ Schröder, S. E.; Tomasko; Keller (2005). "The reflectance spectrum of Titan's surface as determined by Huygens". American Astronomical Society, DPS meeting No. 37, #46.15; Bulletin of the American Astronomical Society. 37 (726): 726. Bibcode:2005DPS....37.4615S.
{{cite journal}}
: Unknown parameter|coauthors=
ignored (|author=
suggested) (help); Unknown parameter|month=
ignored (help) - ^ de Selding, Petre (January 21, 2005). "Huygens Probe Sheds New Light on Titan". SPACE.com. Retrieved March 28, 2005.
- ^ Waite; J. H.; Cravens, T. E.; Coates, A. J.; Crary, F. J.; Magee, B.; Westlake, J. (2007). "The Process of Tholin Formation in Titan's Upper Atmosphere". Science. 316 (5826): 870. Bibcode:2007Sci...316..870W. doi:10.1126/science.1139727. PMID 17495166.
{{cite journal}}
: More than one of|pages=
and|page=
specified (help) - ^ C.P. McKay, J. B. Pollack, R. Courtin (1991). "The greenhouse and antigreenhouse effects on Titan". Science. 253 (5024): 1118–1121. doi:10.1126/science.11538492. PMID 11538492.
{{cite journal}}
: CS1 maint: multiple names: authors list (link) - ^ Titan: A World Much Like Earth. Space.com (2009-08-06). Retrieved on 2012-04-02.
- ^ "Titan Has More Oil Than Earth". February 13, 2008. Retrieved February 13, 2008.
- ^ Lakdawalla, Emily (January 21, 2004). "Titan: Arizona in an Icebox?". The Planetary Society. Retrieved March 28, 2005.
- ^ Emily L., Schaller (2006). "A large cloud outburst at Titan's south pole" (PDF). Icarus. 182 (182): 224–229. Bibcode:2006Icar..182..224S. doi:10.1016/j.icarus.2005.12.021. Retrieved August 23, 2007.
{{cite journal}}
: Unknown parameter|coauthors=
ignored (|author=
suggested) (help) - ^ "The Way the Wind Blows on Titan". Jet Propulsion Laboratory. June 1, 2007. Retrieved June 2, 2007.
- ^ Shiga, David (2006). "Huge ethane cloud discovered on Titan". New Scientist. 313: 1620. Retrieved August 7, 2007.
- ^ Mahaffy, Paul R. (May 13, 2005). "Intensive Titan Exploration Begins". Science. 308 (5724): 969–970. Bibcode:2005Sci...308..969M. doi:10.1126/science.1113205. PMID 15890870.
- ^ a b c d e Jennifer Chu (July 2012). "River networks on Titan point to a puzzling geologic history". MIT Research. Retrieved July 24, 2012.
- ^ "Titan, Saturn's largest moon is finally unravelled in detail". News Pakistan. March 12, 2012. Retrieved March 12, 2012.
{{cite news}}
:|first=
missing|last=
(help) - ^ Battersby, Stephen (October 29, 2004). "Titan's complex and strange world revealed". New Scientist. Retrieved August 31, 2007.
- ^ "Spacecraft: Cassini Orbiter Instruments, RADAR". Cassini–Huygens Mission to Saturn & Titan. NASA, Jet Propulsion Laboratory. Retrieved August 31, 2007.
- ^ Lorenz, R. D.; Callahan; Gim, Y.; Alberti, G.; Flamini, E.; Seu, R.; Picardi, G.; Orosei, R.; Zebker, H. (2007). "Titan's Shape, Radius and Landscape from Cassini Radar Altimetry" (PDF). Lunar and Planetary Science Conference. 38: 1329. Bibcode:2007LPI....38.1329L. Retrieved August 27, 2007.
- ^ "Cassini Reveals Titan's Xanadu Region To Be An Earth-Like Land". Science Daily. July 23, 2006. Retrieved August 27, 2007.
- ^ Barnes, Jason W.; Brown, Robert H.; Soderblom, Laurence; Buratti, Bonnie J.; Sotin, Christophe; Rodriguez, Sebastien; Le Mouèlic, Stephane; Baines, Kevin H.; Clark, Roger (2006). "Global-scale surface spectral variations on Titan seen from Cassini/VIMS" (PDF). Icarus. 186 (1): 242. Bibcode:2007Icar..186..242B. doi:10.1016/j.icarus.2006.08.021. Retrieved August 27, 2007.
- ^ Dermott, S. F. and Sagan, C. (1995). "Tidal effects of disconnected hydrocarbon seas on Titan". Nature. 374 (6519): 238–240. Bibcode:1995Natur.374..238D. doi:10.1038/374238a0. PMID 7885443.
{{cite journal}}
: CS1 maint: multiple names: authors list (link) - ^ Bortman, Henry (November 2, 2004). "Titan: Where's the Wet Stuff?". Astrobiology Magazine. Retrieved August 28, 2007.
- ^ Lakdawalla, Emily (June 28, 2005). "Dark Spot Near the South Pole: A Candidate Lake on Titan?". The Planetary Society. Retrieved October 14, 2006.
- ^ "NASA Confirms Liquid Lake On Saturn Moon". NASA. 2008. Retrieved December 20, 2009.
- ^ "NASA Cassini Radar Images Show Dramatic Shoreline on Titan" (Press release). Jet Propulsion Laboratory. September 16, 2005. Retrieved October 14, 2006.
- ^ a b "PIA08630: Lakes on Titan". NASA Planetary Photojournal. NASA/JPL. Retrieved October 14, 2006.
- ^ "Titan Has Liquid Lakes, Scientists Report in Nature". NASA/JPL. January 3, 2007. Retrieved January 8, 2007.
- ^ "River networks on Titan point to a puzzling geologic history". MIT. July 20, 2012. Retrieved July 23, 2012.
- ^ Hecht, Jeff (July 11, 2011). "Ethane lakes in a red haze: Titan's uncanny moonscape". New Scientist. Retrieved July 25, 2011.
- ^ "Tropical Methane Lakes on Saturn's Moon Titan". saturntoday.com. 2012. Retrieved June 16, 2012.
- ^ Hadhazy, Adam (2008). "Scientists Confirm Liquid Lake, Beach on Saturn's Moon Titan". Scientific American. Retrieved July 30, 2008.
- ^ Grossman, Lisa (August 21, 2009). "Saturn moon's mirror-smooth lake 'good for skipping rocks'". New Scientist. Retrieved November 25, 2009.
- ^ Wye, L. C. (2009). "Smoothness of Titan's Ontario Lacus: Constraints from Cassini RADAR specular reflection data". Geophysical Research Letters. 36 (16): L16201. Bibcode:2009GeoRL..3616201W. doi:10.1029/2009GL039588.
{{cite journal}}
: Unknown parameter|coauthors=
ignored (|author=
suggested) (help) - ^ Cook, J.-R. C. (December 17, 2009). "Glint of Sunlight Confirms Liquid in Northern Lake District of Titan". NASA web site Cassini mission page. NASA. Retrieved December 18, 2009.
- ^ Lakdawalla, E. (December 17, 2009). "Cassini VIMS sees the long-awaited glint off a Titan lake". The Planetary Society Blog. Planetary Society. Retrieved December 17, 2009.
- ^ a b Wall, Mike (December 17, 2010). "Saturn Moon's 'Lake Ontario': Shallow and Virtually Wave-free". Space.Com web site. Retrieved December 19, 2010.
- ^ a b "Tides turn on Titan". Nature. June 28, 2012. Retrieved June 29, 2012.
{{cite news}}
:|first=
missing|last=
(help) - ^ Puiu, Tibi (June 29, 2012). "Saturn's moon Titan most likely harbors a subsurface ocean of water". zmescience.com web site. Retrieved June 29, 2012.
- ^ a b c d Wood, C. A. (September 6, 2009). "Impact craters on Titan". Icarus. 206 (1). Elsevier: 334–344. Bibcode:2010Icar..206..334L. doi:10.1016/j.icarus.2009.08.021.
{{cite journal}}
:|access-date=
requires|url=
(help); Unknown parameter|coauthors=
ignored (|author=
suggested) (help) - ^ "PIA07365: Circus Maximus". NASA Planetary Photojournal. Retrieved May 4, 2006.
- ^ "PIA07368: Impact Crater with Ejecta Blanket". NASA Planetary Photojournal. Retrieved May 4, 2006.
- ^ "PIA08737: Crater Studies on Titan". NASA Planetary Photojournal. Retrieved September 15, 2006.
- ^ "PIA08425: Radar Images the Margin of Xanadu". NASA Planetary Photojournal. Retrieved September 26, 2006.
- ^ "PIA08429: Impact Craters on Xanadu". NASA Planetary Photojournal. Retrieved September 26, 2006.
- ^ Ivanov, B. A. (1997). "Atmospheric entry of large meteoroids: implication to Titan". Planetary and Space Science. 45 (8): 993–1007. Bibcode:1997P&SS...45..993I. doi:10.1016/S0032-0633(97)00044-5.
{{cite journal}}
: Unknown parameter|coauthors=
ignored (|author=
suggested) (help) - ^ Artemieva, Natalia (2003). "Cratering on Titan: impact melt, ejecta, and the fate of surface organics". Icarus. 164 (2): 471–480. Bibcode:2003Icar..164..471A. doi:10.1016/S0019-1035(03)00148-9.
{{cite journal}}
: Unknown parameter|coauthors=
ignored (|author=
suggested) (help) - ^ Owen, Tobias (2005). "Planetary science: Huygens rediscovers Titan". Nature. 438 (7069): 756–757. Bibcode:2005Natur.438..756O. doi:10.1038/438756a. PMID 16363022.
- ^ Media Relations Office: Cassini Imaging Central Laboratory For Operations (2009). "Cassini Finds Hydrocarbon Rains May Fill The Lakes". Space Science Institute, Boulder, Colorado. Retrieved January 29, 2009.
- ^ a b Moore, J.M.; Pappalardo (2008). "Titan: Callisto With Weather?". American Geophysical Union. 11. American Geophysical Union, Fall Meeting 2008: 06. Bibcode:2008AGUFM.P11D..06M.
{{cite journal}}
: More than one of|work=
and|journal=
specified (help); Unknown parameter|coauthors=
ignored (|author=
suggested) (help) - ^ Neish, C.D.; Lorenz, R.D. and O'Brien, D.P. (2005). "Shape and thermal modeling of the possible cryovolcanic dome Ganesa Macula on Titan: Astrobiological implications". Lunar and Planetary Laboratory, University of Arizona, Observatoire de la Cote d'Azur. Archived from the original on August 14, 2007. Retrieved August 27, 2007.
{{cite web}}
: CS1 maint: multiple names: authors list (link) - ^ Lakdawalla, Emily (2008). "Genesa Macula Isn't A Dome". The Planetary Society. Retrieved January 30, 2009.
- ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1038/nature03596, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with
|doi=10.1038/nature03596
instead. - ^ LeCorre, L.; LeMouélic, S.; Sotin, C. (2008). "Cassini/VIMS observations of cryo-volcanic features on Titan" (PDF). Lunar and Planetary Science. XXXIX.
- ^ Shiga, David (March 28, 2009). "Giant 'ice flows' bolster case for Titan's volcanoes". NewScientist.
- ^ "Mountain range spotted on Titan". BBC News. December 12, 2006. Retrieved August 6, 2007.
- ^ Mountains Discovered on Saturn’s Largest Moon Newswise, Retrieved on July 2, 2008.
- ^ Richard A. Lovett (2010). "Saturn Moon Has Ice Volcano—And Maybe Life?". National Geographic. Retrieved December 19, 2010.
- ^ Fortes, A. D. (2007). "Ammonium sulfate on Titan: Possible origin and role in cryovolcanism". Icarus. 188 (1): 139–153. Bibcode:2007Icar..188..139F. doi:10.1016/j.icarus.2006.11.002.
{{cite journal}}
: Unknown parameter|coauthors=
ignored (|author=
suggested) (help); Unknown parameter|month=
ignored (help) - ^ Lakdawalla, Emily. (December 17, 2008). "AGU: Titan: Volcanically active world, or "Callisto with weather?". The Planetary Society. Retrieved October 11, 2010.
- ^ Roe; H. G. (2004). "A new 1.6-micron map of Titan's surface". Geophys. Res. Lett. 31 (17): L17S03. Bibcode:2004GeoRL..3117S03R. doi:10.1029/2004GL019871.
- ^ Lorenz, R. (2003). "The Glitter of Distant Seas". Science. 302 (5644): 403–404. doi:10.1126/science.1090464. PMID 14526089.
- ^ a b Goudarzi, Sara (May 4, 2006). "Saharan Sand Dunes Found on Saturn's Moon Titan". SPACE.com. Retrieved August 6, 2007.
- ^ Lorenz, R. D. (July 30, 2010). "Winds of Change on Titan". Science. 329 (5991): 519–20. Bibcode:2010Sci...329..519L. doi:10.1126/science.1192840. PMID 20671175.
- ^ a b Lorenz, RD; Wall, S; Radebaugh, J; Boubin, G; Reffet, E; Janssen, M; Stofan, E; Lopes, R; Kirk, R (2006). "The sand seas of Titan: Cassini RADAR observations of longitudinal dunes". Science. 312 (5774): 724–727. Bibcode:2006Sci...312..724L. doi:10.1126/science.1123257. PMID 16675695.
- ^ Lancaster, N. (2006). "Linear Dunes on Titan". Science. 312 (5774): 702–703. doi:10.1126/science.1126292. PMID 16675686.
- ^ "Titan's Smoggy Sand Grains". JPL. 2008. Retrieved May 6, 2008.
- ^ Benton, Julius L. Jr. (2005). Saturn and How to Observe It. Springer London. pp. 141–146. ISBN 978-1-84628-045-0.
- ^ a b "Planetary Satellite Physical Parameters". JPL (Solar System Dynamics). April 3, 2009. Retrieved June 29, 2010.
- ^ Näränen, Jyri. "The Atmosphere of Titan". University of Helsinki, Department of Astronomy. Retrieved August 19, 2007.
- ^ "The Pioneer Missions". Pioneer Project. NASA, Jet Propulsion Laboratory. March 26, 2007. Retrieved August 19, 2007.
- ^ "Pioneer XI". Photo Index. NASA. Retrieved August 19, 2007.
- ^ Richardson, J; Lorenz, Ralph D.; McEwen, Alfred (2004). "Titan's Surface and Rotation: New Results from Voyager 1 Images". Icarus. 170 (1): 113–124. Bibcode:2004Icar..170..113R. doi:10.1016/j.icarus.2004.03.010. verified 2005-03-28.
- ^ Lingard, Steve (2005). "How To Land on Titan" (23). Ingenia. Retrieved January 11, 2009.
{{cite journal}}
: Cite journal requires|journal=
(help); Unknown parameter|coauthors=
ignored (|author=
suggested) (help); Unknown parameter|month=
ignored (help) - ^ "Cassini at Saturn: Introduction". NASA, Jet Propulsion Laboratory. Retrieved September 6, 2007.
- ^ "Cassini Equinox Mission: Titan Flyby (T-70) – June 21, 2010". NASA/JPL. Retrieved July 8, 2010.
- ^ "Huygens Exposes Titan's Surface". Spacetoday. Retrieved August 19, 2007.
- ^ a b "Seeing, touching and smelling the extraordinarily Earth-like world of Titan". ESA News, European Space Agency. January 21, 2005. Retrieved March 28, 2005.
- ^ "Huygens landing site to be named after Hubert Curien". ESA. March 5, 2007. Retrieved August 6, 2007.
- ^ "Mission Summary: TANDEM/TSSM Titan and Enceladus Mission". ESA. 2009. Retrieved January 30, 2009.
- ^ Rincon, Paul (February 18, 2009). "Jupiter in space agencies' sights". BBC News.
- ^ Stofan, Ellen (2010). "TiME: Titan Mare Explorer" (PDF). Caltech. Retrieved August 17, 2011.
- ^ "NASA picks project shortlist for next Discovery mission". TG Daily. May 9, 2011. Retrieved May 20, 2011.
{{cite news}}
:|first=
missing|last=
(help) - ^ Greenfieldboyce, Nell (September 16, 2009). "Exploring A Moon By Boat". National Public Radio (NPR). Retrieved November 8, 2009.
- ^ a b Raulin, F. (2005). "Exo-astrobiological aspects of Europa and Titan: From observations to speculations". Space Science Review. 116 (1–2): 471–487. Bibcode:2005SSRv..116..471R. doi:10.1007/s11214-005-1967-x.
- ^ Staff (October 4, 2010). "Lakes on Saturn's Moon Titan Filled With Liquid Hydrocarbons Like Ethane and Methane, Not Water". ScienceDaily. Retrieved October 5, 2010.
- ^ a b Raulin F., Owen T. (2002). "Organic chemistry and exobiology on Titan". Space Science Review. 104 (1–2): 377–394. Bibcode:2002SSRv..104..377R. doi:10.1023/A:1023636623006.
- ^ Staff (October 8, 2010). "Titan's haze may hold ingredients for life". Astronomy. Retrieved October 14, 2010.
- ^ Artemivia N., Lunine J, (2003). "Cratering on Titan: impact melt, ejecta, and the fate of surface organics". Icarus. 164 (2): 471–480. Bibcode:2003Icar..164..471A. doi:10.1016/S0019-1035(03)00148-9.
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: CS1 maint: extra punctuation (link) CS1 maint: multiple names: authors list (link) - ^ Richard A. Lovett Saturn Moon Titan May Have Underground Ocean, National Geographic, March 20, 2008
- ^ a b c d McKay, C. P.; Smith, H. D. (2005). "Possibilities for methanogenic life in liquid methane on the surface of Titan". Icarus. 178 (1): 274–276. Bibcode:2005Icar..178..274M. doi:10.1016/j.icarus.2005.05.018.
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: CS1 maint: multiple names: authors list (link) - ^ "Have We Discovered Evidence For Life On Titan". Space Daily. June 8, 2010. Retrieved March 15, 2012.
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:|first=
missing|last=
(help) - ^ a b c Committee on the Limits of Organic Life in Planetary Systems, Committee on the Origins and Evolution of Life, National Research Council; The Limits of Organic Life in Planetary Systems; The National Academies Press, 2007; page 74.
- ^ a b c d e "What is Consuming Hydrogen and Acetylene on Titan?". NASA/JPL. 2010. Retrieved June 6, 2010.
- ^ Strobel, Darrell F. (2010). "Molecular hydrogen in Titan's atmosphere: Implications of the measured tropospheric and thermospheric mole fractions" (PDF). Icarus. 208 (2): 878–886. Bibcode:2010Icar..208..878S. doi:10.1016/j.icarus.2010.03.003.
- ^ "Saturn's Moon Titan: Prebiotic Laboratory". Astrobiology Magazine. August 11, 2004. Archived from the original on August 28, 2004. Retrieved August 11, 2004.
- ^ "Earth could seed Titan with life". BBC News. March 18, 2006. Retrieved March 10, 2007.
- ^ Gladman, Brett; Dones, Luke; Levinson, Harold F.; Burns, Joseph A. (2005). "Impact Seeding and Reseeding in the Inner Solar System". Astrobiology. 5 (4): 483–496. Bibcode:2005AsBio...5..483G. doi:10.1089/ast.2005.5.483. PMID 16078867.
{{cite journal}}
: CS1 maint: multiple names: authors list (link) - ^ Lunine, Jonathan (2008). [www.amphilsoc.org/sites/default/files/CCLunine1530402.pdf "Saturn's Titan: A Strict Test for Life's Cosmic Ubiquity"] (PDF). Proceedings of the American Philosophical Society. 153 (4): 403. arXiv:0908.0762. Bibcode:2009arXiv0908.0762L.
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: Check|url=
value (help) copy at archive.org - ^ Lorenz, Ralph D.; Lunine, Jonathan I. and McKay, Christopher P. (1997). "Titan under a red giant sun: A new kind of "habitable" moon" (PDF). NASA Ames Research Center, Lunar and Planetary Laboratory, Department of Planetary Sciences, University of Arizona. Retrieved March 21, 2008.
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: CS1 maint: multiple names: authors list (link)
Bibliography
- Coustenis, Athéna and Taylor, F. W. (2008). Titan: Exploring an Earthlike World. World Scientific. ISBN 978-981-270-501-3.
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: CS1 maint: multiple names: authors list (link)
Further reading
![](http://upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/30px-Commons-logo.svg.png)
- Lorenz, Ralph (2002). Lifting Titan's Veil: Exploring the Giant Moon of Saturn. Cambridge University Press. ISBN 0-521-79348-3.
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External links
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- Cassini–Huygens Mission To Saturn & Titan. Multimedia Feature Titan Virtual Tour
- Titan Profile at NASA's Solar System Exploration site
- Video of Huygens’ descent from the ESA
- Cassini Imaging Central Laboratory for Operations (CICLOPS) site Titan image search
- European Space Agency. (2005). ESA—Cassini-Huygens. Retrieved March 28, 2005.
- The Planetary Society (2005). TPS: Saturn's moon Titan. Retrieved March 28, 2005.
- University of Arizona Lunar and Planetary Lab (2005). Lunar and Planetary Lab The Descent Imager-Spectral Radiometer of the Cassini–Huygens Mission to Titan. Retrieved March 28, 2005.
- The Alien Noise. This recording is a laboratory reconstruction of the sounds heard by Huygens' microphones.
- Movie of Titan's rotation from the National Oceanic and Atmospheric Administration site
- AstronomyCast: Titan Fraser Cain and Pamela Gay, 2010.
- Titan nomenclature and Titan map with feature names from the USGS planetary nomenclature page
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