Emily LakdawallaMar 16, 2010

Titan: Callisto with weather

It's the second time I've posted with this provocative title. The first time, I was just reposting the title of a talk given by Jeff Moore at the 2008 meeting of the American Geophysical Union. This time, it's in response to a new paper published last week in Science by Luciano Iess and his coauthors.

The paper concerned measurements of Titan's gravity. Cassini has flown past Titan more than 50 times. On a few of those occasions, the closest-approach period of the flyby has been given over to precise tracking of Cassini's radio beacon: Cassini points its radio dish at Earth and broadcasts its carrier signal as several gigantic radio telescopes tune in and listen. As Cassini flies through the sway of Titan's gravity, it accelerates and then decelerates. The radio telescopes on Earth measure Cassini's "range rate," that is, the component of Cassini's speed in the direction measured along the Earth-Cassini line. The radio tracking is so precise, Iess says in his paper, that they can determine Cassini's speed to a precision of better than a tenth of a millimeter per second. (They also have to take into account things like the minute acceleration imparted to Cassini by radiation from its radioisotope thermal generators; all these factors are modeled and corrected for.)

How does this probe Titan's gravity? Cassini's acceleration as it flies past Titan is sensitive to how mass is distributed within Titan. Titan's a solid object, so how can mass be distributed unevenly within it? Consider Earth, which has a highly anisotropic mass distribution. Earth has a metal core with a density of upwards of 20 grams per cubic centimeter; all the way up where we stand on the crust, its density is barely more than 2.5 grams per cubic centimeter. Titan is made of the same stuff Earth is, though in different proportions: it started out its existence with more water ice and less metal than Earth, so overall it has a lower density than our planet does. But knowing its overall density doesn't tell us whether it's internally stratified, like Earth is, or mostly not, like Callisto. Until recently, it's been assumed that great big Titan is internally stratified into a core of metal, then a layer of rock, then ice, then very likely a bit of ocean, followed by its ice shell and its atmosphere.

Why do we care if Titan is internally stratified? Because internal stratification goes hand-in-hand with internal geologic activity. If Titan is an active world -- as would seem to be the case, given its youthful-looking surface lacking many craters -- then it's natural to assume it's internally stratified. And numerous peer-reviewed papers have been published on volcanic edifices on Titan -- even on active volcanism on Titan.

Not so fast, Jeff argued. Here's a bit from that 2008 post on his talk: "The only unambiguously identified features on Titan are exogenic -- fluvial, aeolian, and impact. There are no unambiguously identified features that are endogenic -- tectonic or volcanic." That is, we have very strong evidence that the surface is shaped by processes that result from the atmosphere, things like rain and wind. But so far the jury's out on whether there are internal processes going on. To be fair, Jeff pointed out, it may just be that the data isn't good enough yet. He asserted that despite the accomplishments of Cassini's four years at Saturn, "the state of imaging on Titan is similar to state of understanding of Mars after Mariner 6 and 7." Imaging is similar in extent and resolution; after Mariner 6 and 7, the jury was out on whether anything besides cratering had shaped Mars' surface.

Still, Jeff said, "When you look at features on Galilean satellites that are of similar size, they don't look very much like Titanian features -- even on Callisto." He compared images of large craters on the Galilean moons to the largest ones observed on Titan. The Galilean moons' craters were flat and degraded, a result of relaxation of a relatively mobile icy crust. By contrast, Titan's biggest craters have much steeper topography. "This implies Titan's lithosphere is stiffer than the Galileans'. In fact, the only similar-sized and -shaped crater features are on Dione and Tethys."

So what the gravity data says about Titan's internal structure is really important. And what does it say? The Iess et al. paper states that Titan's shape is the one that you would expect from an icy body responding passively to the forces of Saturnian tides and its own rotation, and that its mass is not concentrated in the center as it is for Earth or even Ganymede. Titan's mass is more concentrated toward its center than it is for Callisto, but still it appears that if there has been any separation of Titan's icy component from its rocky component, such separation (known as "differentiation" among geophysicists) is incomplete, and that there is either "imperfect separation of rock from ice or a core in which a large amount of water remains chemically bound in silicates."

Here's the picture of what people have been thinking Titan looked like inside, in a 3D view very helpfully generated by Doug Ellison:

Titan's internal structure [DEPRECATED]
Titan's internal structure [DEPRECATED] A computer-generated view exposes Titan's internal structure: layers of ice (containing an internal ocean), rock, and a metal core.Image: Doug Ellison, based on a model from Hussmann et al., 2006

And here's what the Iess paper suggests it actually looks like inside:

Titan's internal structure
Titan's internal structure Studies of Titan's gravity have shown that Titan is very likely only incompletely differentiated, meaning that its component materials (ice, rock, metal) are not separated into layers according to their density. The distribution of its internal mass is intermediate between Callisto's (which is not differentiated) and Ganymede's (which is).Image: Doug Ellison, based on an internal model from Mitri et al., 2010

So Jeff Moore's question -- is Titan just Callisto with weather? -- may have an affirmative answer. Underneath that youthful surface shaped by wind, rain, rivers, even seas of methane and ethane may lie a geologically quiescent world. Here, then, is a current view of how Titan's interior structure stacks up against those of other icy bodies in the solar system. (Keep in mind that there is much more data backing up these cartoons for the moons of Saturn and Jupiter than there is for the more distant moons, not to speak of the lack of data other than mass and surface composition for the Kuiper belt objects.)

Interiors of icy bodies in the solar system (as of 2010)
Interiors of icy bodies in the solar system (as of 2010) Many bodies in our solar system may contain oceans. Jupiter's ice-coated moons (Europa, Ganymede, and Callisto) probably contain internal saltwater oceans. The more distant large and medium-sized icy moons, the icy dwarf planets, and tiny Enceladus may contain colder ammonia-water oceans. Oceans in icy satellites could be a common feature throughout the universe, while Earth's surface ocean may be the more unusual case. These interior models were developed by many geophysicists from data about the sizes, densities, and orbital characteristics of each body.Image: Doug Ellison, Emily Lakdawalla, and Bob Pappalardo. Internal models based mostly on Hauke Hussmann, Frank Sohl, and Tilman Spohn, 2006, except for Titan (Giuseppi Mitri et al., 2010) and the Galilean moons (Bob Pappalardo, personal communication).

As I was composing this entry, I got another email from Bob Pappalardo pointing me to a new paper in press that's relevant to this subject, by Francis Nimmo and Bruce Bills. They look at Titan's topography and find it to be a bit higher than they'd expect for an icy world (as Jeff More also pointed out), suggesting it has a thick, rigid outer ice shell that is not presently convecting. Convection -- in which warm material from depth rises, flowing in the solid state, while cool material from the surface sinks -- is the engine that drives geologic activity on Earth and presumably other worlds as well. So, "not convecting" implies "not geologically active."

These will be fighting words to some researchers, of course. It's a good thing Cassini will be at Saturn for more than seven more years! There's a lot yet to be learned.

I want to take this moment to issue some congratulations. Bob Pappalardo has been leading the Cassini mission as its Project Scientist for a short time, only 20 months. As of today, he is leaving Cassini, moving on to a full time position as the project scientist for the Europa Jupiter System Mission currently under development at the Jet Propulsion Laboratory. Bob will be replaced on Cassini by Linda Spilker, who has been Deputy Project Scientist, who's steered Cassini's science from its beginning. So, congratulations to Bob and best wishes that he'll see the Europa mission through development, launch, arrival, and science mission at Jupiter; and congratulations, too, to Linda, for rising to the scientific helm of NASA's outer planet flagship.

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