Titan (Moon)

Titan
Titan in true color. The color is of Titan's hazy atmosphere.[1]
Date of discovery	March 25, 1655[2][3]
Name of discoverer	Christiaan Huygens[2][3][4]
Name origin	First generation of Greco-Roman gods
Orbital characteristics
Primary	Saturn
Order from primary	20
Perikrone	1,186,680 km[5]
Apokrone	1,257,060 km[5]
Semi-major axis	1,221,870 km[6]
Orbital eccentricity	0.0288[6]
Sidereal month	15.85 da[6]
Avg. orbital speed	5.58 km/s[3]
Inclination	0.34854° to Saturn's equator
Rotational characteristics
Sidereal day	15.85 da[3]
Axial tilt	0°
Physical characteristics
Mass	1.34553 * 1023 kg (2.25157% earth)[5]
Density	1,880 kg/m³[7]
Mean radius	2,575.5 km[7]
Surface gravity	1.3535 m/s² (0.13802 g)[5]
Escape speed	2.6405 km/s[5]
Surface area	83,355,253 km² (16.352% earth)[5]
Mean temperature	95 K[3]
Composition	Rock, water ice, and hydrocarbons
Color	Orange[1]
Albedo	0.21[7]

Titan (Greek Τῑτάν first-generation god), or Saturn VI, is the largest satellite of Saturn, the second-largest planetary satellite in the solar system (after Ganymede), and the only body other than Earth to have bodies of liquid on its surface for any length of time. Until recently most astronomers believed that Titan was the only celestial body other than Earth to have a dense atmosphere. Titan is twentieth in order from Saturn and the sixth satellite of dwarf planet size (consistent with its official IAU catalog designation as "Saturn VI").

The most exciting finds on Titan to date are the liquid hydrocarbon "seas," containing among them more hydrocarbons than the entire proved reserves of oil and natural gas on earth.^[8]

Discovery and naming[edit]

The Dutch astronomer Christiaan Huygens^[4] first discovered Titan on March 25, 1655. He used a telescope far more refined than the one that Galileo Galilei had earlier used to discover four of the moons of Jupiter.^[9] This was the first of Saturn's moons to be discovered, so Huygens named the object he found Saturni Luna (Latin for "Saturn's moon"). Giovanni Domenico Cassini and other astronomers would eventually discover eight more moons of Saturn, including at least five inside of Titan. With Cassini's discoveries of the first four of these, Titan's name was changed to "Saturn IV." Titan now bears the catalog designation of "Saturn VI," the identifier that the International Astronomical Union has now assigned it. Recent deep-space robotic missions have discovered that a total of nineteen moons orbit inside Titan, and another forty outside it.^[10]

Titan got its common name from John Herschel (son of the astronomer William Herschel). He gave Titan a generic name for the Titans of mythology, and also named the other seven moons then known after specific deities among the Titans.^[11]

Orbital and rotational characteristics[edit]

Titan follows a slightly eccentric orbit at a mean distance of 1.22 million kilometers from Saturn's center (or rather, the barycenter of the Saturnine system). Its sidereal month is 15.85 Julian days, as is the length of its sidereal day. Astronomers therefore consider it in tidal lock with Saturn.

Titan is also in a 3:4 orbital resonance with the satellite Hyperion, the next farther satellite in the Saturnian system.

Physical characteristics[edit]

Titan is slightly larger in radius than Mercury (and Earth's Moon), and is more massive than any of the dwarf planets Eris, Pluto, and Ceres by one to two orders of magnitude. Titan was once thought to be the broadest of all satellites, but the Voyager 1 probe showed that Titan's large apparent diameter was due to its atmosphere, and in fact Ganymede is slightly larger in radius than is Titan.^[12]

Titan's bulk is probably half water ice and half rock, in several layers with a rock center and several layers of various crystalline forms of ice.^[12]

Magnetometric experiments have not shown any appreciable magnetic dipole moment on Titan at present.^[13]

Atmosphere[edit]

The atmosphere of Titan is probably its most salient distinguishing feature. Its pressure at the surface is 1.6 times that at sea level on Earth, or roughly the pressure at the depth of an average swimming pool.^[14] This atmosphere is composed chiefly of nitrogen and various hydrocarbon compounds that give Titan its orange color.^[3]

The constituents of Titan's atmosphere are listed in this table:^[15]

Name	Formula	Concentration
Major constituents		Percent
Nitrogen	N2	87-99
Argon	Ar	0-6
Methane	CH4	1-6
Minor constituents		ppm
Hydrogen	H2	2000
Ethane	CH3CH3	20
Acetylene	HC#CH	4
Ethylene	H2C=CH2	1
Propane	CH3CH2CH3	1
Methylacetylene	H3CC#CH	0.03
Diacetylene	HC#C-C#CH	0.02
Hydrogen cyanide	HC#N	1
Cyanogen	N#C-C#N	0.02
Cyanoacetylene	HC#C-C#N	0.03
Acetonitrile	H3C-C#N	0.003
Carbon monoxide	C=O	50
Carbon dioxide	O=C=O	0.01

The argon finding is significant because much of it is ⁴⁰Ar, an isotope usually associated with volcanism. The currently favored interpretation is that Titan has multiple "cryovolcanos" that erupt with water ice and ammonia.^[16]

The atmosphere is not of uniform composition. Clouds, presumably of methane, do form. Furthermore, Huygens' images of the surface show clear signs of erosion and formations that look like dry riverbeds, a sign that rain occurs—though the rain is of methane, not water.^[12] However, the data do not indicate the looked-for "ocean" of methane, but rather indicate something akin to the seasonal rivers and lakes seen on earth.^[12][16]

Until 2005, Titan was regarded as the only natural satellite in the solar system to have a true atmosphere. But the Cassini-Huygens Mission has already demonstrated that Saturn's inner moon Enceladus also has an atmosphere, believed composed of ionized water vapor from repeated eruptions from volcanoes and/or geysers on its surface. This "atmosphere" is constantly escaping from Enceladus, perhaps to persist as the E ring of Saturn's ring system. Thus it requires a continuous source of replenishment. The theories of Enceladus' volcanic and/or geothermal activity are an attempt to explain this replenishment.^[17]

Liquid Hydrocarbons on Titan[edit]

Until the Cassini spacecraft arrived at Saturn, most astronomers understood that Titan's atmosphere had methane as a significant component, and speculated that this methane must derive from a surface ocean of methane. Yet initial observations of Titan's south pole disclosed no such ocean,^[18] and indeed not more than two small lakes.^[19] But observations of the north pole revealed vast liquid hydrocarbon deposits in the form of multiple lakes and streams, rather than a world-covering ocean.^[19][20] These findings easily surpass all the known hydrocarbon reserves on Earth. Yet Lorenz et al. note that while the liquid lakes appear adequate in the short term to replenish methane lost through photolysis, they could not keep the atmosphere supplied with methane over deep time.

The Prebiotic-Abiotic Controversy[edit]

Before the launch of the Cassini-Huygens Mission (see below), speculations on whether Titan had the required elements for abiogenesis were rife.^[3] Specifically, scientists believed that the methane in Titan's atmosphere would combine photochemically to yield ethane, ethylene (ethene), acetylene (ethyne), and hydrogen cyanide, and thus form amino acids.^[3][14]

The Huygens lander has thus far found no biological process, though it has found the suspected constituents, and more. But gas-chromatograph mass spectrophotometric findings have also shown that the bulk of the methane on Titan is actually ¹³C methane—not the ¹²C methane that one would normally expect from biological processes.^[21] Scientists at the Goddard Space Flight Center conclude that this methane is vented to the surface from a supply that was somehow trapped deep beneath the surface when Titan was formed. Furthermore, this lends further support to Thomas Gold's 1998 hypothesis that Earth's own supplies of oil and natural gas are in fact abiotic in origin.^[22]

This latest finding militates against the speculation that life might exist on Titan. Many scientists believe that Titan's chemistry and physical features are of a type that could have given rise to the earliest chemicals required for life, had Titan been much closer to the Sun than it actually is. That speculation predates the Cassini-Huygens mission and includes a model suggesting that Titan harbored a vast underground reservoir of ammonia solution.^[23] That particular model depended on the methane and the cyanide being biogenic, but as has been noted above, the methane certainly is not biogenic.

Possible Subsurface Ammonia Ocean[edit]

The ammonia-water "aquifer" might yet exist, however, as a vast subsurface ocean. The ⁴⁰Ar findings certainly suggest this.^[16] But recently Cassini's controllers carefully mapped fifty of Titan's landmarks and then discovered an apparent shift of all fifty landmarks by as much as 30 km (less than 20 miles). This finding suggests that the moon's crust is somehow decoupled from its core and is floating on top of a liquid layer. Astronomers believe that this layer lies 100 km (over 60 miles) deep to the rocky surface.^[24]

Problems for Uniformitarian Theories[edit]

The most serious problem that Titan poses for uniformitarian theories is that astronomers still have not found the vast reserves of methane that would be necessary to maintain the current level of methane in the atmosphere over deep time. Lorenz and his colleagues state flatly that Titan must be subject to drastic climate change unless an as-yet unaccounted-for internal source of methane is replenishing the atmosphere "at exactly the right rate" (emphasis added).^[20]

Yet the findings suggesting an ammonia aquifer 100 km deep to the surface make such an internal source much more difficult to explain. This is especially so if, as suspected, the entire surface of Titan floats on the ammonia ocean beneath it with no connection to the core.

Observation and Exploration[edit]

In the 300-plus years since its discovery, the only study of Titan was by observation with Earth-based telescopes. Pioneer 11 made a brief flyby of Saturn in 1979 and took several low-quality images. Voyager 1 and Voyager 2 were next to visit Saturn in 1980 and 1981; Voyager 1 did make a close flyby of Titan, but its instruments could not penetrate the thick haze of the Titanian atmosphere.^[3]

In 1994 the Hubble Space Telescope took photographs of an apparent "continent" on the Saturnian face of Titan.^[14]

The first truly comprehensive study of that system is the Cassini-Huygens Mission, which launched on October 15, 1997 and arrived in the Saturnian system on July 1, 2004.^[3] The major innovation of this mission was the use of radar equipment aboard the orbiter and the lander, to penetrate the haze.

Huygens was designed to land, and to study the atmosphere and the surface in detail on the way down. Huygens landed fully functional on Titan on January 14, 2005. It remained functional for three hours while it sent back many images and much data on the composition, including the carbon-isotopic ratio, of the Titanian atmosphere.

Cassini continues to study Titan and the rest of the Saturnine system. Its mission was originally scheduled to run for four years, ending in July 2008, but NASA has announced a two-year extension with multiple rendezvous with Titan and additional rendezvous with Enceladus, Rhea, Dione, and Helene. Mission planners also suggest that after two years, Cassini might still have enough fuel for another two-year extension, and speak hopefully of specific future missions to Titan and Enceladus.^[25]

In fiction[edit]

Titan was a frequent staple of science fiction in the 1950s and 1960s. Specifically:

• Robert A. Heinlein conceived of Titan as an ideal location for a cold-regions field-testing laboratory for emergency survival equipment.
• Carey Rockwell conceived of Titan as a mining colony. He never made clear exactly what sort of mineral wealth Titan might possess, but the hydrocarbons alone (and in a reducing atmosphere) might have been a good candidate, had Mr. Rockwell known then what NASA and the ESA know today.
• Larry Niven envisioned Titan as an exclusive and expensive resort destination. He conceived of a resort built on Titan's Saturnine face, where guests could gaze at Saturn and its rings. He wrote this concept, of course, before Voyager 1 made its flyby and was unable to photograph the surface of Titan through the haze. Moreover, Titan's orbit is only slightly inclined with respect to the ring plane, so that even had the atmosphere been clear, the view might not have been as spectacular as Mr. Niven might have imagined.

Gallery[edit]

• 

  Titan transits Saturn just south of the ring plane

• 

  Titan's hazy atmosphere in ultraviolet light

• 

  Three false-color mosaics of Titan showing changes in its atmosphere within three months

• 

  Surface of Titan from 17 to 8 km up, from Huygens lander as it descended

• 

  Surface of Titan from 7 to 0.5 km up, from Huygens lander as it descended

• 

  Surface of Titan, from Huygens lander after it landed

• 

  Surface of Titan, in color, from Huygens lander

References[edit]

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