Emily Lakdawalla • Aug 17, 2009
Here's a little piece of eye candy for you. There is a canonical shot of Uranus taken by Voyager 2 as it departed the system, showing the apparently serene blue orb as a thin crescent:
Any time there's a gnarly old data set, image processor Ted Stryk has typically had a go at it. Here is his version of those five crescent moons. From left to right, they are Oberon, Titania, Umbriel, Ariel, and little Miranda. This photo won't win a beauty contest, but it's a view of these tiny dark worlds that almost no one has really seen before.
Not long after the Voyager encounters, in the late 1980's, dynamicists (mostly William Tittemore, Jack Wisdom, Stan Dermott, and Renu Malhotra) did a study of the Uranian satellite system to try to explain what was going on. In particular, some of the satellite surfaces were not primordial or were just plain weird (e.g. Miranda). But most interestingly, the inclinations of the satellites had Miranda sticking out like a sore thumb with an inclination of 4 degrees, an order of magnitude more than the other moons and unusual for any of the regular satellites of the outer planets. They were able to explain Miranda's inclination and some of the resurfacing events through models the dynamical evolution of the system [that is, how the orbits of the moons have shifted with time as they interact gravitationally with each other and Uranus].
Due to the tides from Uranus, the major satellites are moving outwards (just as our Moon is moving away from the Earth). Kepler's third law says that the size of the orbit is related to the orbital period, so this tidal evolution changes the orbital periods of all the satellites in different ways. Occasionally in this evolution, two of the satellites will cross a resonance (e.g. one satellite going around exactly 5 times when the other goes around exactly 3 times). These resonances powerfully affect the orbits and, combined with continued tidal evolution, can create Miranda's inclination and can also create eccentricities that lead to internal tidal heating and resurfacing. This isn't a recent result, but I thought it was pretty cool that the dynamical model does an excellent job of reproducing Miranda's anomalous post-resonant inclination, without a lot of parameter tuning.
The second interesting thing going on with Uranus right now is that the satellites are undergoing mutual events. (This is similar to the situation with the KBO I've been working on, Haumea, see haumea-namaka.blogspot.com). This is described on the Armagh Observatory website and there are a few recent (2007 and 2008) scientific papers that talk about some of the observations, and, in one case, modeling. They haven't gotten to the point where they'll use all the observations to refine the masses, radii, etc. of the system, but I would expect new updated physical properties of the Uranian moons in the next few years. I think it's also true that some of these event light curves will give us crude albedo properties of regions of the satellites not seen by Voyager.
Along these same lines, there's a recent observation of a stellar occultation of Titania that improved the error bars on Voyager's measurement of its radius by a factor of 3 and also put a pretty strong upper limit (10-8) atmospheres!) on any tenuous atmosphere that could exist (this limit shows that Titania does not have a Pluto-like atmosphere, which is at the 10-6 atmosphere level). The main author gave a presentation at the Division of Planetary Sciences meeting last fall (for which there is video) if it interests you. Looking at the abstract, I didn't realize that they were also able to constrain the size of the giant star that was occulted. Cool!
Anyway, just a few thoughts for someone interested in the Uranian moons. Although we aren't flying there anytime soon, we can still learn about the system through clever observations.
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