slideshow about

You are here

IAG Planetary Geomorphology Working Group

Featured images for December 2011:

Evaporites on Titan

Images and caption contributed 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 theywere 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 -- different from Earth's 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 (Image of the Month, March 2010).

Therefore the evaporites on Titan have an unusual nature relative 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.

Image 1
Image 1:  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.

Image 2

Image 2:  Close-up of Atacama Lacuna, Titan.  This dry lake in the center shows evaporite deposits, but neighboring lakes to the east do not.

Image 3

Image 3:  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.

 

Recommended Reading:

Aharonson, O. et al., 2009. An asymmetric distribution of lakes on Titan as a possible consequence of orbital forcing Nature Geoscience 2, 851.854.  

Barnes, J.W.  et al.,  (2011). Organic Sedimentary Deposits in Titan's Dry Lakebeds: Probable Evaporite, Icarus 216, pp136-140, doi:10.1016/j.icarus.2011.08.022

Barnes, J.W. et al., (2009). Shoreline features of Titan's Ontario Lacus from Cassini/VIMS observations. Icarus 201, 217.225.  

Brown, R.H. et al., 2008. The identification of liquid ethane in Titan.s Ontario Lacus. Nature 454, 607.610.

Cordier, D. et al., 2009. An estimate of the chemical composition of Titan’s lakes. Astrophys. J. 707, L128.L131.

Hayes, A. et al., 2008. Hydrocarbon lakes on Titan: Distribution and interaction with a porous regolith. Geophys. Res. Lett., 35, L09204.

Hayes, A.G. et al., 2011. Transient surface liquid in Titan’s polar regions from Cassini. Icarus 211, 655.671.

McCord, T.B. et al., 2008. Titan’s surface: Search for spectral diversity and composition using the Cassini VIMS investigation. Icarus 194, 212.242

Moore, J.M., Howard, A.D., 2010. Are the basins of Titan’s Hotei Regio and Tui Regio sites of former low latitude seas? Geophys. Res. Lett. 37, L22205.

Turtle, E.P. et al., 2011. Shoreline Retreat at Titan.s Ontario Lacus and Arrakis Planitia from Cassini Imaging Science Subsystem Observations. Icarus 212, 957. 959.

Past Images

PSI, a Nonprofit Corporation 501(c)(3), and an Equal Opportunity/M/F/Vet/Disabled/Affirmative Action Employer.
1700 East Fort Lowell, Suite 106 * Tucson, AZ 85719-2395 * 520-622-6300 * FAX: 520-622-8060
Copyright © 2014 . All Rights Reserved.