Join Donate

Emily LakdawallaJanuary 12, 2012

Evaporites on Titan

The following was posted in December as a Planetary Geomorphology Image of the Month, a monthly Web feature provided by the Planetary Geomorphology Working Group of the International Association of Geomorphologists, and I thought it'd be of interest to you. --ESL


by Jason W. Barnes
Assistant Professor of Physics, University of Idaho

Evaporites form on planetary surfaces when dissolved chemical solids precipitate out of saturated solution as their liquid solvent evaporates. Until recently, they were known to exist on only two planets: Earth and Mars. On Earth there are a variety of evaporite constituents including carbonates (CaCO3), sulfates (CaSO4), and halides (NaCl), progressing in order of increasing solubility. NASA's rover Opportunity discovered evaporitic deposits on Mars that are primarily composed of sulfates. These are different from Earth's evaporites due to a highly acidic formation environment.

A third planetary instance of evaporite has now been discovered in an exotic location: Saturn's moon Titan. Being so far from the Sun, Titan has a low surface temperature of 90°K (-183°C), just warmer than liquid nitrogen. Hence all of Titan's water is permanently frozen. However, methane on Titan plays the same role that water does on Earth and Mars. Titan has methane clouds, methane rain, methane rivers, and methane lakes and seas.

Therefore, the evaporites on Titan have an unusual nature compared to those on rocky planets. Instead of water being the solvent, on Titan the solvent is methane. And instead of salts being the solute, on Titan organic molecules derived from ultraviolet photolysis of methane dissolve in rain, surface, and ground liquid. Those organics precipitate out of lakes when the liquid methane solute evaporates, becoming evaporite.

Titan lakes, wet and dry

NASA / JPL / UA

Titan lakes, wet and dry
Cassini VIMS/RADAR hybrid image of filled and dry lakes south of Titan's methane sea Ligeia Mare. The brightness of the image is determined by synthetic aperture radar which indicates roughness, and the colors by Cassini's Visual and Infrared Mapping Spectrometer indicate composition. Some of the small lakes in the image are filled (cyan arrows). Other lakes show lacustrine morphology, but no evidence for liquids. Some of those dry lakes have the same composition as the surrounding terrain, but others show evaporites in bright orange.

Atacama Lacuna, Titan

NASA / JPL / UA

Atacama Lacuna, Titan
Close-up of Atacama Lacuna, Titan. This dry lake in the center shows evaporite deposits, but neighboring lakes to the east do not.
Great Salt Lake and environs

Google maps

Great Salt Lake and environs
Google maps satellite view of the environs of the Great Salt Lake in the American state of Utah. The Great Salt Lake is the ultimate sink for surface runoff in the American west. It has no outlets, and thus its waters have high concentrations of dissolved salts. A large evaporite deposit surrounds the Great Salt Lake, marking its extent during the Pleistocene. However just south of the Great Salt Lake lies Utah Lake, which is freshwater. Utah lake maintains low salt content because it has an output stream that drains the lake of water and salt equally; hence it has no evaporite at the bottom. A similar effect may occur on Titan and explain why some dry lakes contain evaporite and others do not.

Read more: Titan, Earth, geology, Saturn's moons, Earth analogs

You are here:
Headshot of Emily Lakdawalla
Emily Lakdawalla

Senior Editor and Planetary Evangelist for The Planetary Society
Read more articles by Emily Lakdawalla

Comments & Sharing
MER
Let's Change the World

Become a member of The Planetary Society and together we will create the future of space exploration.

Join Today

Emily Lakdwalla
The Planetary Fund

Support enables our dedicated journalists to research deeply and bring you original space exploration articles.

Donate