22 December 2009
AGU 2009: Day 4 – Enceladus and Exoplanets
Posted by Ryan Anderson
Thursday at AGU started with a tough choice. At 8 am there was a talk about methane on Mars, and a special lecture about the water plumes on Enceladus, and plate tectonics on Venus! In the end I decided to go to the Enceladus lecture, given by Sue Kieffer. She explained that there are two primary models for how the Enceladus plumes form. The first is dubbed the “cold faithful” model, and involves pure water coming into contact with the vacuum of space, perhaps in an underground cavern, and boiling to create a plume of vapor and ice particles. (remember, if the pressure is low enough it doesn’t need to be hot for water to boil) The problem with this model is that gases detected in the plume would have to also be in the water, and when exposed to the vacuum they would come out of solution, much like a shaken can of pop, and so the amount of ice in the plume would be different from observations.
The other model, which Kieffer prefers, is the “frigid faithful” model, which relies on “clathrates” – gas molecules trapped in cages of water ice. In this model, dense fractures in the subsurface ice act as conduits for gases, including water vapor, released from the clathrates due to the geothermal heating in the crust. In this scenario the fractures are constantly sealing themselves as ice condenses in the mouth of the vent, but re-open as tidal stresses fracture the crust.
The enceladus lecture finished with a long question and discussion session. Some of the concerns with the “frigid faithful” model were that it is hard to explain how the observed sodium got into the vapor plume. Also, it looks like argon is concentrated in the plume, which is best done with liquid water. Kieffer admitted that this was “troublesome” but another commenter pointed out that radioactive potassium in the ice could decay to provide the Argon. There is still the problem that the amount of argon coming out with the plume is way more than could be continually produced, suggesting that argon built up for a long time and is now being released. That would mean we are seeing a “special” event, and scientists are always hesitant to invoke special circumstances to explain an observation.
After Enceladus, I headed over to the session on planetary interiors. This session talked about all sorts of different objects, including everyone’s favorite two-faced moon of Saturn, Iapetus. Iapetus has a bizarre ring of mountains encircling its equator and a couple of talks tried to explain why that might be. Previous theories suggested that the ridge could be due to Iapetus changing shape as it began to spin slower, but Mikael Beuthe said that scenario wouldn’t produce the right kind of faults in the crust. He suggested that a better explanation would be if the crust was slightly thinner at the equator and Iapetus shrank as it cooled, causing the crust to buckle along the equator. A second talk by David Sandwell suggested the somewhat strange idea that the ridge was formed when the planet contracted due to melting of the interior ice, causing the outer spherical shell to collapse in two hemispherical halves. After these talks, there was some discussion and several scientists pointed out that it’s hard to explain massive faults right along the equator but nowhere else. Those people favored an origin related to material accreted from the rings.
The other reason that I attended the planetary interiors session was that several talks speculated about “super-earth” exoplanets. C. Sotin (I didn’t catch his full first name) addressed the question of whether super-Earths would be more or less likely to have plate tectonics than the Earth. One paper, based on scaling up the equations that govern the process on Earth, suggested that super-earths would have plate tectonics, but a different paper based on simulations said exactly the opposite. Sotin took a look at both sides and concluded that it’s not just a simple function of the mass of the planet. Lots of unknown factors like water content, changes of phase deep in the mantle, and the degree to which the primordial crust is fractured all play a role.
Another talk by Peter Driscol took a look at how to get “optimal” geodynamos in rocky exoplanets. He showed that, to get the maximum magnetic field from an Earth-sized planet, it should be slightly hotter than the Earth, but that Earth is still pretty darn good. He also said that it could be possible to detect the radiation from charged particles in the stellar wind spiraling through the planet’s magnetic field! The observation would have to be made from above earth’s ionosphere, and the most likely candidate would be a planet with a big convecting core (and therefore a powerful magnetic field) orbiting a nearby star which has a strong stellar wind.
One of the comments after Driscol’s talk, directed at everyone working on super-earth dynamics struck me as extremely significant. I didn’t catch the person’s name, but he pointed out that everyone assumes that the mantles of super-earths behave like the earth’s mantle, but in actuality, under the enormous heat and pressure silicates would actually break down and behave like a metal, much the same way that hydrogen becomes metallic inside Jupiter and Saturn! If Si really does become metallic in super-earths, then that would have lots of bizarre consequences, likely powering much stronger magnetic fields and possibly changing the heat-flow out of the planet.
Finally, Linda Elkins-Tanton talked about what the mantle convection would be like on a tidally-locked rocky planet. Such a planet would always have one side facing its star while the other would be in constant darkness. Elkins-Tanoton and her student Sarah Goldman found that the powerful heating on one side of the planet and cooling on the other side would drive a continuous upwelling plume on the hot side of the planet and a matching downwelling plume on the cold side. In extreme cases, this could lead to the presence of “magma ponds” on the sunlit side of the planet, which are constantly spilling away from the hottest point and eventually freezing. That sort of mass redistribution could make the planet want to re-orient itself. They have not yet considered what an atmosphere would do to the magma ponds, but likely it would transfer the heat away more effectively, making the ponds more prone to freezing.
I have always loved the idea of a tidally-locked terrestrial planet, particularly since there might be a sweet-spot near the terminator where the surface temperature is habitable. I’ve even started a short story set on such a world. It might be time to dig that back up…
Been a while since I have had the time to have a look at your blog. Very informative summary for some one like me – interested in the field but not professionally involved! There are so many interesting things happening (data!) that it’s hard to keep up.
Have a great Christams. 🙂
Thanks! I’m glad you find the conference summaries informative! I always worry that I am summarizing to the point that it only makes sense to someone in the field…
Happy new year!
Would be nice to see some illustrations of magma ponds 🙂
Unfortunately, there isn’t much in the way of illustrations for the work being done on tidally-locked planets… yet. 🙂
Hah I am honestly the only reply to this incredible post!