Ligeia Mare from a false-color mosaic of synthetic aperture radar images of Titan's north polar region.
|Diameter||500 km[note 1]|
Ligeia Mare / / is a lake in the north polar region of Titan, the planet Saturn's largest moon. It is the second largest body of liquid on the surface of Titan, after Kraken Mare. Larger than Lake Superior on Earth, it is mostly composed of liquid methane, with unknown but lesser components of dissolved nitrogen and ethane, as well as other organic compounds. It is located at 78° N, 249° W, and has been fully imaged by the Cassini spacecraft. Measuring roughly 420 km (260 mi) by 350 km (217 mi) across, it has a surface area of about 126,000 km2, and a shoreline over 2000 km (1240 mi) in length. The lake may be hydrologically connected to the larger Kraken Mare. Its namesake is Ligeia, one of the sirens in Greek mythology.
Ligeia Mare has two predominant types of coastline, "crenulated" and "subdued". The former is characterized by hummocky, eroded terrain, the latter by lower, smoother topography and the presence of more numerous and longer channels. Crenulated terrain predominates on the eastern and southern sides of the lake; subdued terrain to the west and north. Except in the southeast where the rough topography extends to the coast, hummocky terrain tends to be separated from the shoreline by a more subdued bench. The coast has numerous bays that appear to be flooded river mouths (rias), and unlike at Ontario Lacus there are no visible subaerial delta deposits, possible evidence of a recent sea level rise. In the northeast and northwest sections of the mare, along about a quarter of the total shoreline, there are extensive areas where the depth is less than 5 m, shallow enough for imaging radar to penetrate to the bottom. 2013 radar measurements by Cassini indicate parts of the lake are 170 m deep which implies the liquid must be very pure methane since the radar signal was able to pass right through it. The surface of the lake appears very smooth on radar; it is flat within a few millimeters, suggesting very light surface winds.
The average depth is on the order of 50 m, while the maximum depth is probably > 200 m. The total volume is likely to be > 7000 km3.
The reasons for Ligeia Mare's nearly pure methane composition are still not entirely clear. Until studies showed otherwise, it had been assumed that ethane would be the primary constituent of Titan's seas, as it is produced in Titan's upper atmosphere by the following reaction:
- 2 CH4 -> H2 + C2H6
The lack of ethane is an open question awaiting further investigation. Theories include it migrating into the undersea crust or perhaps into Kraken Mare, whose composition has as of yet not been as well studied. In the latter case, ethane-poor liquid hydrocarbon would be the equivalent of terrestrial freshwater (Titanian precipitation is mainly methane).
In addition to ethane, Titan's atmosphere produces a wide range of more complex photochemical products, such as nitriles and benzene. These are believed to precipitate out and flow into Titan's seas. Radar data suggests that Ligeia Mare's seabed is likely covered in a thick layer of these organic compounds.
Temperature readings from the shoreline of Ligeia Mare suggest that it is porous and highly saturated with hydrocarbons. The shorelines of Ligeia Mare and other north polar lakes and maria have been stable over the period of observation by Cassini, in contrast to south polar Ontario Lacus, where there has been significant shoreline recession. However, transient phenomena have been observed including a 260 square kilometre feature dubbed "Magic Island" by Cassini scientists. The "Magic Island" area only appeared in 2014 and may be waves, bubbles or subsurface ice rising to the surface as the lake warms up during spring, or possibly silt like material suspended in the liquid hydrocarbon sea.
The Titan Mare Explorer (TiME) is a lake-lander proposed in 2009 to splash down on and then drift about the lake. It was selected for a Phase-A design study in 2011 as a candidate mission for the 12th NASA Discovery Program opportunity, but was not selected for flight.
|[[File:PIA16197 Titan river.jpg|thumb|40px|Vid Flumina, a river over 400 km long that empties into Ligeia Mare (in the lower center of the image at the top of the page). Radar measurements say that it is a network of hundred meters deep canyons.|
- The USGS web site gives the size as a "diameter", but it is actually the length in the longest dimension.
- New Century Cyclopedia of Names
- "Titan maria". Gazetteer of Planetary Nomenclature. USGS Astrogeology Science Center. Retrieved 2012-03-16.
- "Cassini Spacecraft Reveals Clues About Titan". SpaceRef. December 12, 2013. Retrieved 2013-12-18.
- "Cassini Explores a Methane Sea on Titan". Jet Propulsion Laboratory News. 2016-04-26.
- Le Gall, A.; Malaska, M. J.; Lorenz, R. D.; Janssen, M. A.; Tokano, T.; Hayes, A. G.; Mastrogiuseppe, M.; Lunine, J. I.; Veyssière, G.; Encrenaz, P.; Karatekin, O. (2016-02-25). "Composition, seasonal change, and bathymetry of Ligeia Mare, Titan, derived from its microwave thermal emission". Journal of Geophysical Research: Planets. 121 (2): 233–251. Bibcode:2016JGRE..121..233L. doi:10.1002/2015JE004920.
- Stofan, E. R.,; Lunine, J. I.; Lorenz, R. D.; Kirk, R. L.; Aharonson, O.; Hayes, A. G.; Lucas, A.; Turtle, E. P.; Wall, S. D.; Wood, C. A.; Cassini Radar Team (2012). Shorelines of Ligeia Mare, Titan - 43rd Lunar and Planetary Science Conference (PDF). Lunar and Planetary Institute. Retrieved 2012-03-20.
- Marco Mastrogiuseppe, Valerio Poggiali, Alexander Hayes, Ralph Lorenz, Jonathan Lunine, Giovanni Picardi, Roberto Seu, Enrico Flamini, Giuseppe Mitri, Claudia Notarnicola, Philippe Paillou, and Howard Zebker, The bathymetry of a Titan sea", 4 March 2014.
- "Cassini Finds a Lake On Titan That's Almost Completely Methane". Astronomy Magazine. 2016-04-27. Retrieved 2016-04-27.
- "Cassini explores the depths of a methane sea on Titan". Cosmos Magazine. 2016-04-27. Retrieved 2016-04-27.
- Turtle, E. P.; Perry, J. E.; Hayes, A. G.; McEwen, A. S. (2011-02-15). "Shoreline retreat at Titan's Ontario Lacus and Arrakis Planitia from Cassini Imaging Science Subsystem observations". Icarus. 212 (2): 957–959. Bibcode:2011Icar..212..957T. doi:10.1016/j.icarus.2011.02.005. Retrieved 2012-03-25.
- Staff (23 June 2014). "Planetary Scientists Discover Mysterious Geologic Object on Titan". Sci-News.com. Retrieved 2014-10-11.
- Stofan, Ellen (25 August 2009). "Titan Mare Explorer (TiME): The First Exploration of an Extra-Terrestrial Sea" (PDF). Retrieved 2009-11-03.. Also available as Stofan, E., Titan Mare Explorer (TiME): First Exploration of an Extraterrestrial Sea. Retrieved 13 June 2017.
- NASA Discovery Program office, NASA Announces Three New Mission Candidates Archived 2016-11-18 at the Wayback Machine. May 5, 2011. Accessed 13 June 2017.
- Let's go sailing on lakes of Titan! (November 1, 2009)
- Landau, Elizabeth (2012). "Probe would set sail on a Saturn moon". Retrieved 2012-10-09.
- Hall, Loura (May 30, 2014). "Titan Submarine: Exploring the Depths of Kraken".
- "NASA Funds Titan Submarine, Other Far-Out Space Exploration Ideas".
- "Vid Flumina". USGS planetary nomenclature page. USGS. Retrieved 2014-01-01.