Help Shape the Future of Space Exploration

Join The Planetary Society Now  arrow.png

Join our eNewsletter for updates & action alerts

    Please leave this field empty
Blogs

Headshot of Emily Lakdawalla

Titan's lakes: The basics

Posted by Emily Lakdawalla

15-03-2014 10:30 CDT

Topics: Huygens, pretty pictures, Cassini, Titan, explaining science, Saturn's moons

Since Seth MacFarlane tweeted that this weekend's episode of Cosmos was going to include a segment on lakes on Titan, I thought I'd write a post about the basics of Titan lakes.

Titan is Saturn's largest moon. It's larger than all other moons in the solar system except Jupiter's Ganymede. Indeed, it's bigger than Mercury. If you read in old (pre-Voyager) books about Titan, you'll see that we used to think Titan was the biggest moon in the solar system, because it wears a thick cloak of an atmosphere that makes it basically impossible to see its surface, at least with un-augmented vision. Titan doesn't give up its secrets easily. This is what it looked like to Voyager 2.

Voyager 2 approach image of Titan

NASA / JPL / Gordan Ugarkovic

Voyager 2 approach image of Titan
Voyager 2 took the images for this natural color composite on August 23, 1981, as it approached for its flyby of Saturn.

If we had a hard time seeing Titan's surface, at least we could see its atmosphere. And its atmosphere contains something surprising: methane. Now, methane is common in the solar system. Methane is what makes the atmospheres of Uranus and Neptune blue. Methane is in Pluto's atmosphere, and it's frozen to the surface of other big Kuiper belt objects like Eris and Makemake. But compared to these places, Titan is positively balmy and much closer to the Sun.

Methane is made of one carbon atom bonded to four hydrogen atoms. At Titan's distance from the Sun, solar ultraviolet radiation destroys methane rapidly, breaking it into bits -- loose hydrogen atoms, and carbons bonded to a couple hydrogens. When these molecule pieces come back together, they don't always rearrange into methane. Carbons stick together, making bigger molecules with more carbons. Then those get broken up, and even bigger pieces stick together. Sometimes they combine with nitrogen from the atmosphere. This is more or less the same process that makes smog on Earth, and is one reason it's so hard to see through Titan's atmosphere. Some of the loose hydrogens combine into molecular hydrogen gas. Physics says the lightweight hydrogen gas should escape Titan entirely. This all happens pretty rapidly; methane is just not stable at Titan, not over the age of the solar system.

So how is there methane still around for us to see it? One possibility is that it's just a freak sudden event that released a bunch of methane into Titan's atmosphere at the moment in the solar system's four-billion-year history that we happened to develop the tools to be able to detect methane on Titan. That's possible, but relatively unlikely. Or, there's a reservoir of methane at the surface or inside Titan that resupplies the atmosphere. At one point, we thought Titan might be covered in a global ocean of methane. ESA even designed the Huygens lander to float, just in case it landed in a methane ocean; we really didn't know what we'd find down there when we launched Cassini in 1997.

When Huygens landed on Titan in 2005, it actually found itself in a dry plain, but one that clearly showed that a fluid had flowed there. It's clear from the shapes of the rocks: they're rounded. These "rocks" are actually composed of water ice; the fluid must have been methane maybe mixed with ethane.

Huygens view of Titan's surface (colorized)

NASA / JPL / ESA / UA

Huygens view of Titan's surface (colorized)
Huygens returned this photo after landing on Titan on January 14, 2005. It has been colorized based upon spectral data. The round objects in this image are pebbles and cobbles composed of ice. The surface is darker than originally expected, consisting of a mixture of water and hydrocarbon ice. There is also evidence of erosion at the base of these objects, indicating possible fluvial activity.

Huygens also clearly demonstrated that fluids flow across Titan's surface, at least sometimes, because there's really no other way you can make branching channels that look like this:

Panorama of the

ESA / NASA / JPL / UA; image processing and panorama: René Pascal

Panorama of the "Shoreline" on Titan
Panorama of the "Shoreline" on Titan, stitched from Huygens DISR Side-Looking and Medium-Resolution Imager raw data.

To flow with liquid, those river valleys must have been filled with methane that came from higher elevations; it had to rain methane on Titan. Rainfall runs off, and then what? It must pool somewhere.

What we learned from the Cassini orbiter at Saturn is that there are lakes on Titan. The first lake was spotted near the south pole by Cassini's camera, peering at Titan in an infrared wavelength invisible to human eyes. It turns out there's only one lake at the south pole.

Lake on Titan

NASA / JPL / SSI

Lake on Titan
The footprint-like feature in the upper left corner of this image is Ontario Lacus, a hydrocarbon lake. It is roughly 234 kilometers long by 73 kilometers wide, about the size of Lake Ontario (a lake on the U.S.-Canadian border). The red cross below center identifies the location of Titan's south pole.

But the most dramatic pictures of lakes on Titan came from Cassini's radar instrument. Radar imagers see the landscape differently from cameras. You're looking at a picture of surface roughness. Rocky surfaces are rough, and look bright. Smoother surfaces, like, say, sandy ones -- look dark. Liquid surfaces, smooth as glass, look black black black. This is what the radar instrument saw at the north pole.

Titan's rivers and lakes

NASA / JPL

Titan's rivers and lakes
A Cassini RADAR swath across Titan's north polar regions passed over numerous methane-ethane lakes and river channels that feed them. There is not any evidence that any of the channels were actually running with flowing liquid when Cassini took the image; it's more likely that they are dry washes like those in Earth's deserts, and that they appear dark because a layer of fine sediment is deposited along their bottoms. The data are from flyby T28, April 10, 2007.
The Shores of Kraken Mare

NASA/JPL/ASI

The Shores of Kraken Mare
Radar image of Kraken Mare, a sea of liquid methane and ethane on Saturn's moon Titan, as observed by the Cassini spacecraft. The data indicates the depth here exceeds tens of meters. The image covers an area about 270 kilometers wide.

We can now map and name Titan's lakes. The smaller ones are named for similar-sized lakes on Earth. There are 32 named lakes on Titan. All but three of them are near Titan's north pole. There one near Titan's south pole is called Ontario Lacus, named for the lake bordering the U.S. and Canada. They've found two (so far) in Titan's southern temperate regions, named Sionascaig and Urmia for lakes in Scotland and Iran, respectively. There are three big ones, big enough to be called seas or "mare," named for mythical sea creatures: Kraken, Ligeia, and Punga mare.

Bird's eye view of Titan's Land of Lakes (annotated version)

NASA / JPL-Caltech / SSI / JHUAPL / University of Arizona

Bird's eye view of Titan's Land of Lakes (annotated version)

Rainfall, river runoff, lakes, evaporation into clouds, rainfall again. Cassini has seen clouds make storms on Titan. We have seen the whole cycle -- it's just like Earth's water cycle, but with a completely different substance, and much, much colder.

Since Cassini arrived in 2004, we've learned a lot about Titan and its lakes. For instance, we may be seeing the southern lake district changing over time. And we're still learning. On Monday, I'll be in Houston for a huge annual meeting of planetary scientists called the Lunar and Planetary Science Conference. There's a whole session devoted to the lakes on Titan (PDF). Scientists are figuring out just how much liquid is in the lakes. They're discovering new lakes in northern temperate latitudes. They're finding very low waves on some of the lakes. They're using laboratory experiments to figure out what other stuff is dissolved in the methane and ethane. They're figuring out what happens when lakes evaporate. They're even watching water currents in the lakes, and discovering "mysterious new islands" that seemed to appear out of nowhere. I'll be filing a report after I attend that session, bringing you the latest science from Titan.

The Cassini mission will only last a few more years before it runs out of fuel and ends its life with a plunge into Saturn's atmosphere. These dynamic lakes on Titan are so exciting, it would be wonderful to return to Titan with a dedicated mission to study them more, either from orbit or by actually floating a boat in a lake and letting it drift with the currents. We were close to getting such a mission on the books, but NASA didn't select it for development.

TiME Floating on Titan

NASA

Titan Mare Explorer (TiME)

And with the problems in NASA's budget that we're following closely at The Planetary Society, it's looking less and less likely that we're going to follow up on what Cassini discovered at Titan any time soon -- not for many decades, at least. If this disturbs you, I hope you'll consider joining The Planetary Society and writing to your representatives to tell them that Titan -- and the rest of the outer solar system -- deserves great new missions that will follow the tradition of discovery that has led from Pioneers, to Voyagers, to Galileo, to Cassini, to Juno.

Once the operating missions die out at the end of 2017, NASA has nothing following them to the giant planets. Nothing under construction now means that there will be no active giant planet mission for at least a decade, probably longer, even if we started developing one today. At least Europe is filling the breach with their JUICE mission, and because solar system exploration has always been international, American scientists are involved with it. But Europe still can't go beyond Jupiter. For now, if we want to follow up at Saturn or Uranus or Neptune, only the U.S. can do it. And I, for one, think we should!

 
See other posts from March 2014

 

Or read more blog entries about: Huygens, pretty pictures, Cassini, Titan, explaining science, Saturn's moons

Comments:

Jonathan Ursin: 03/15/2014 06:18 CDT

A Neptune orbiter would so cool! I just finished reading the book "Titan Unveiled" It was also... so cool! The book did leave me with the unaddressed question... Is it possible that the source of methane on Titan is from life in an under-ice environment like what people hypothesise with Europa? Maybe this will be addressed in Cosmos Episode 2

Artur: 03/16/2014 09:09 CDT

With E-sail (http://arxiv.org/abs/1312.6554) Europe will be able go far beyond Jupiter.

Enzo: 03/17/2014 05:08 CDT

@Artur, The problem for Europe is that they do not have a way to power probes beyond Jupiter because they do not have RTGs, only solar power. They are addressing this. Their other limitation is probably less resilience to high radiation that limits where they can go. In fact they are going to orbit Ganymede with JUICE while they could go to the much more interesting Europa if it wasn't for the radiation environment,

Mike Malaska: 03/18/2014 08:18 CDT

A couple clarifications: There are a few other lakes in the south polar terrain, but they are much smaller than Ontario Lacus. There are also hints that there may have been larger lakes in the past in the south, but that they evaporated as Titan's climate cycled. Also, there is not much evidence that the cobbles and sands seen in the Huygens surface image are water ice. Many atmospheric chemistry models predict meters of organic stuff covering the surface. Those rocks and sands could just as easily be some type of organic material. We really don't know exactly what most of Titan's surface is made of just yet - it is one of the most exciting mysteries of Solar System exploration. This makes a very compelling reason to send another mission to Titan.

Artur: 03/18/2014 02:42 CDT

@Enzo, Europe (UK) is trying to build radioisotope power source that uses Am-241, although it is difficult to find information on the current status of the project.

Enzo: 03/18/2014 07:15 CDT

@Artur, I know, that's what I meant by "they are addressing this". Fairly recent article here : http://www.world-nuclear-news.org/ON-Positive_results_from_space_battery_work-2607135.html

Kalle Centergren: 03/22/2014 06:10 CDT

interesting.. using Am241 might give the posibility to do very long lifed missions with a half-life of 432.2 years. the normal TEGs with Pu-238 have a half life of "only" 87.7 years. on the down side, you will probably need more mas per Watt outputt with Am241

Leave a Comment:

You must be logged in to submit a comment. Log in now.
Facebook Twitter Email RSS AddThis

Blog Search

LightSail - Flight by Light

Support LightSail!

In 2016, The Planetary Society’s LightSail program will take the technology a step further.

I want to help!

Featured Images

The Face of a Comet

Antares
Hayabusa 2 and DCAM3
Hayabusa 2 at Gate Position
More Images

Featured Video

View Larger »

Space in Images

Pretty pictures and
awe-inspiring science.

See More

Join the New Millennium Committee

Let’s invent the future together!

Become a Member

Connect With Us

Facebook! Twitter! Google+ and more…
Continue the conversation with our online community!