Online Astronomy eText: Satellites (Moons)
The Satellites (Moons) of Saturn: Titan Link for sharing this page on Facebook
(a mixture of material written before and after the Cassini spacecraft reached Saturn)
Page last updated Nov 19, 2019

Voyager 1 image of Titan taken in 1980 Titan as viewed by Voyager 1 in 1980. Thick orange haze prevents any visible-light view of the surface. (Image credit Voyager Project, JPL, NASA, Calvin Hamilton, Solarviews)

  Titan is one of the largest moons in the Solar System. In fact for many years it was thought to be the largest of all the moons. However, it has a thick atmosphere, and that atmosphere makes it appear a little larger than it actually is. The way in which radio signals from Voyager 1 were cut off as it passed behind Titan in 1980 showed that Titan is actually slighter smaller than Ganymede, making it only the second largest moon in the Solar System.
  Despite this demotion, if Titan were orbiting the Sun on its own it would be a respectable planet. With a diameter of 3200 miles it is over twice the size and ten times the mass of Pluto. In fact it is even larger than Mercury, although only 40% as massive because it is made of ice and rock, whereas Mercury is made of iron and rock.
  Titan is unique among the moons of the Solar System in having a thick atmosphere. Its atmosphere contains about ten times as much gas per square foot of surface as the Earth's atmosphere, and even though its surface gravity is only about one-seventh of the Earth's gravity, the surface pressure (which is equal to the weight of the atmosphere, or the amount of gas in the atmosphere multiplied by the surface gravity) is about one and a half times greater than that of the Earth's atmosphere. Because of the low gravity and the large amount of gas, the atmosphere extends about ten times further into space than ours.

Voyager 1 image of blue and orange haze in the upper atmosphere of Titan as observed in 1980
Thin blue haze in the upper atmosphere of Titan lies above thick orange haze (false-color image)
(Image Credit NASA/JPL)

Cassini false-color ultraviolet image of 2nd haze layer above Titan's atmosphere
The atmosphere and haze layers extend more than 300 miles above the surface
(Ultraviolet image showing second haze layer, converted to false-color visual image)
(Image Credit NASA/JPL/Space Science Institute)

  Titan's atmosphere is over 90% nitrogen, but also contains a few percent of methane and some argon. Chemical reactions driven by absorption of ultraviolet radiation change the nitrogen and methane into various smog-like hydrocarbons which completely block our view of the surface, at least in visible light. Most of the orangish photochemical haze lies a little under 200 miles above the surface of Titan, but there is a thinner layer of blue haze another 100 miles out, and droplets of hydrocarbon compounds probably drip from the lower haze layer toward the surface, probably covering it with a tarry residue of organic compounds. There are also clouds, most likely of methane or ethane, a half dozen miles above the surface, and there may be ethane or methane oceans on the surface, although the glint characteristic of sunlight falling on lakes and oceans was not been observed in early infrared surveys of the surface by the Cassini spacecraft. Infrared observations indicate that there are lighter and darker areas on the surface, so it is not likely that the entire surface is covered by hydrocarbons. (Note: More recent Cassini observations show that there are intermittent lakes presumably made of liquid methane, and strong winds occasionally pile up "sand dunes" probably made of a mixture of methane and water ice.)

Winds and Dunes on Titan
 Large portions of Titan's equatorial regions are covered by "sand" dunes. The sand is probably grains of hydrocarbon compounds which are piled into dunes by the prevailing winds (though recent observations show than some dunes can form and change in very short periods of time, presumably as a result of much stronger than usual winds). As on the Earth the Coriolis effect due to the rotation of Titan creates zones parallel to the Equator in which the prevailing winds blow one way or another. On both Earth and Titan winds near the Equator primarily blow toward the west, and at higher latitudes winds primarily blow toward the east. Because the Earth is larger, it has an additional region of westward winds nearer the poles, and on the even larger Jovian planets, there are several additional regions of eastward and westward winds; but on Titan only the two patterns of major wind circulation exist.
 Given the westward motion of the atmosphere near the equator it would be expected that dunes would be sculpted accordingly; but rather oddly the dunes appear as though they were sculpted by eastward-blowing winds. Until very recently, this was a mystery. But a new theory based on seasonal changes in the direction and strength of the winds seems to explain the matter.
 Since Titan is very cold and rotates very slowly (only once in each orbit around Saturn, just as our Moon only rotates once in each orbit around the Earth), the winds driven by normal Coriolis effects are relatively slow -- less than two miles per hour -- and are apparently unable to shift the tiny grains of sand. But during Saturn's equinoxes (which, thanks to Titan's synchronous rotation, are also Titan's equinoxes), the greater heating of the equatorial regions reverses the equatorial wind direction and produces stronger winds -- two to four miles per hour -- which are able to shift the sand grains. Thus, most of the dunes are essentially stable for periods of 15 years (the time from one equinox to another), then slightly shift toward the east during the year or two nearest an equinox. (Although, as noted above, more recent observations have shown much more dramatic changes at irregular intervals, presumably due to much faster winds.)
Cassini map of winds on Titan
 The image above (Image credit NASA/JPL/Space Science Institute/Planetary Photojournal) presents a map based on Cassini observations of equinoctial winds. Note that the winds are toward the east rather than westward, as is the normal case near Titan's equator.
 The image below (Image credit JPL, JSC, ESA, NASA, Cassini Radar Mapper, apod100810) is a cropped and contrast-enhanced portion of an image of Titan's sand dunes. Individual dunes are about 300 feet high, half a mile wide and stretch for hundreds of miles nearly parallel to Titan's equator. Huge swaths of such dunes cover about 20% of Titan's surface, mostly in the region within 30 degrees of its equator.
Cropped, enlarged and contrast-enhanced portion of an image of Titan's sand dunes
Below, a much wider view of multiple dunes and hummocks in Xanadu (see geologic map, below)
(Image Credit NASA/JPL-Caltech/ASI/Universite Paris-Diderot) Cassini image of sand dunes and hummocks in Xanadu

Geologic map of Titan compiled from over 100 Cassini passages by the moon
Geologic map of Titan compiled from over 100 Cassini passages by the moon
Click on the image for a much larger version
(Image Credit NASA/JPL-Caltech/ASU)

The left side of the Cassini geologic map of Titan
The left side of the geologic map of Titan; click on the image to see a larger full version
(Image Credit NASA/JPL-Caltech/ASU)

The right side of the Cassini geologic map of Titan
The right side of the geologic map of Titan; click on the image to see a larger full version
(Image Credit NASA/JPL-Caltech/ASU)

2006 Cassini radar images of methane lakes near Titan's north pole
  July 21, 2006 radar observations of the polar regions of Titan by the Cassini spacecraft show a number of large, dark, exceptionally smooth areas (two separate areas, each about 10 degrees from Titan's North Pole, and about 250 by 90 miles in size, are shown above). The simplest explanation of thse features is that they are lakes of liquid ethane or methane, both of which are stable as liquids at the low temperatures and high pressures found near Titan's poles. They certainly cannot be water, which is a rock-like solid at such temperatures. Later observations confirmed the existence of intermittent lakes on Titan, making it only the second Solar System object (after the Earth) known to have lakes of any sort. (Image Credit NASA, JPL, Cassini Spacecraft Team, Planetary Photojournal)

2006 Cassini radar image of methane lakes near Titan's north pole; colorized high-contrast portion of first image
  A colorized high-contrast radar image which includes the upper left portion of the image above, and the area to its left (west). Areas which reflect radar poorly (smoother areas) are shown in blue and areas which reflect radar well (usually rougher areas) in tan, simulating lakes and land areas, respectively. It is thought that below-ground methane is leaking into the lower-lying areas, particularly in cooler regions, then evaporates into the atmosphere (leaving "dry" lakebeds when the temperature rises). When it reaches the upper stratosphere, ultraviolet radiation transforms it into complex hydrocarbons which gradually drift down to the surface, and hydrogen which escapes into space. (Image Credit NASA, JPL, Cassini Spacecraft Team, Planetary Photojournal)

Landing on Titan
Fisheye view of Titan's surface, taken by Huygens probe en route to landing
  A panoramic (fisheye) view of Titan, as viewed from three miles (5 km) above the surface of the moon by the Huygens probe after passing through higher-laying clouds that completely obscure the surface from space. The probe's landing site was just right of center, in the large dark area which dominates the view. This relatively dark basin appears to be a "dry" lakebed, surrounded by lighter colored hills (to the right) and plateaus filled with streambeds and canyons (above). Although at the time the image was taken this part of the surface appeared to be essentially devoid of liquids, infrequent flash floods of liquid methane are thought to carve out the icy surface in a way similar to flash floods of water carving out desert sediments on the Earth. (Image Credit ESA, NASA, Descent Imager/Spectral Radiometer Team (LPL))

First color image of the surface of Titan, taken at the Huygens landing site on Jan 14, 2005
  The first color image of the surface of Titan at the Huygens landing site, taken Jan 14, 2005. Ice boulders lie scattered across a surface of a wet-sand or soft clay consistency mixture of rock-hard ice and liquid methane. (Image Credit ESA, NASA, Descent Imager/Spectral Radiometer Team (LPL))

  The atmosphere of Titan is thought to be very similar to the early atmosphere of the Earth, and the presence of large amounts of complex organic compounds such as hydrogen cyanide, which is a precursor of life, makes scientists wonder whether Titan may harbor primitive lifeforms. Even though its very low temperature (discussed below) makes that somewhat unlikely, that is one of the exciting possibilities that was studied by the Huygens lander, which parachuted into Titan's atmosphere around the end of 2004. Radar imaging by the Cassini spacecraft and surface observations by the Huygens lander answered a few questions about the atmopshere and surface of the moon in the area near the landing, but raised more questions than they answered.
  Titan is able to have an atmosphere because it is relatively large and relatively cold, with surface temperatures around 290 degrees below zero Fahrenheit, and temperatures in the upper haze layers around 150 degrees below zero (the haze layers are warmer because of the heat that they absorb during the photochemical processes that produce the smog-like compounds). However, Ganymede and Callisto, the two largest moons of Jupiter, are about the same size as Titan and only about 30% warmer, so they are theoretically just as capable of holding onto an atmosphere, and neither of them has any substantial amount of gases. This makes us wonder why Titan has an atmosphere, while the other two moons don't.
  The most likely explanation of this difference is probably due to a difference in the composition of ices inside the moons. Because Jupiter formed closer to the Sun, where it was somewhat warmer, volatile ices would have been relatively rarer, and Ganymede and Callisto's ices are probably mostly water ice. Titan, forming around Saturn, which is twice as far from the Sun, in a region which was somewhat colder, although also containing substantial amounts of water ice, would have had a chance to accumulate large amounts of more volatile ices. During the early history of the Solar System, as radioactive materials contained within the rocky materials of various bodies began to heat them up and melt them, the evaporation of ammonia and methane ices would have produced a thick atmosphere of such gases. Over a period of time, absorption of ultraviolet radiation would have split off the hydrogen gas (ammonia is made of hydrogen and nitrogen, while methane is made of hydrogen and carbon), and as the hydrogen escaped into space (because anything smaller than a Jovian planet doesn't have enough gravity to hold onto such a light gas), what was left behind was the present atmosphere of nitrogen and argon, and a residue of carbon and hydrocarbon compounds. Since Ganymede and Callisto wouldn't have had nearly as much of the more volatile ices, they probably just didn't have the chance to form much of an atmosphere, and the fact that they could hold onto an atmosphere became irrelevant.
  One question about Titan's atmosphere is how it manages to maintain its concentration of methane. Theoretical calculations indicate that the loss of hydrogen gas to space and the chemical reactions which convert methane and nitrogen into heavier hydrocarbons which sink to the surface of the moon should remove all of the methane now in the atmosphere in a relatively short period of time (about ten million years, which seems like a long time, but is very short compared to the age of the Solar System). As a result there must be a continual replacement of the methane, presumably by the evaporation of methane ice from the interior.
  Titan's internal structure is unknown, but its density is almost twice that of water ice, which would imply a nearly equal mixture of ice and rocky materials. Heat generated by radioactivity within the rocky materials is probably responsible for the replenishment of methane gas in the atmosphere, but whether the heat was adequate to allow Titan to differentiate, like Ganymede, or whether Titan is more uniformly mixed, like Callisto, is not known. The Cassini spacecraft should resolve this uncertainty, but in any event Titan is not likely to have a substantially liquid region within its icy interior, because it does not have a magnetic field.
  As is true of many of the moons in the Solar System, Titan rotates synchronously, meaning that its rotation period is the same as its orbital period around Saturn (just under 16 Earth days), and it always keeps the same face towards Saturn.

Data for Titan

Discovered by Christian Huygens in 1655
Named after the Titans, the sons and daughters of Uranus and Gaea
Orbital size 1,221,800 km (approximately 760,000 miles)
Orbital eccentricity 3%
Orbital inclination 0.3 degrees
Orbital period 15.94542 days
Rotation period 15.94542 days (synchronous rotation, one side permanently facing Saturn)
Diameter 5150 km (3200 miles), bigger than Mercury, slightly smaller than Ganymede
Mass 0.0225 Earth masses (0.4 Mercury masses, 1.8 Moon masses, or 11 Pluto masses)
Surface gravity 1/7 of Earth, 6/7 of Earth's Moon
Density 1.9 times density of water (Composition probably about half ice, half rock)
Albedo (reflectivity) 20%
Surface temperature 290 Fahrenheit degrees below zero
Atmosphere 10 times mass of Earth's, 10 times depth of Earth's
Atmospheric surface pressure 1.6 times Earth's
Atmospheric composition more than 90% nitrogen, a few percent methane, some argon