The Rosetta spacecraft is currently in hibernation, but is heading back towards the inner Solar System – getting warmer and happier! Despite having large solar panels to collect the Sun’s light and turn it into electrical energy, at it’s farthest from the Sun Rosetta just doesn’t get enough juice to keep all of the on-board systems running. To get around this, the spacecraft was all but switched off for the coldest and loneliest part of the journey.
Although we’re out of contact with the spacecraft, unless something unexpected has happened we are pretty sure we know where it is! ESA have produced this nice app to show the entire trajectory from launch until the end of mission – that’s a journey of 10 years! Unfortunately it seems to be only available in German, but hopefully it’s still clear. On the left side of the app “Ereignis” lets you choose an event – by default the app shows “Jetzt” – now – and gives you the up-to-date position of the spacecraft.
Along the bottom you can re-centre the view on various objects – for now the comet and spacecraft are the most interesting! Finally you can change the zoom level at the top, and hit the play button to run an animation forward in time. As you can see we’re almost at the comet!
All being well, Rosetta will wake up on schedule on Monday 20th January 2014, call home, and let us know that everything is fine. Then it’s all systems go as the spacecraft trajectory is adjusted to put us on our final intercept course to intercept and land on a comet!
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The images that comets and asteroids bring to mind are quite different – we typically think of comets as being bright objects with long tails, and asteroids as being dead lumps of rock. But in fact at closer inspection the differences are not as great as you might think! Comets and asteroids typically have different orbits – this is one of their key defining parameters. And of course comets, which typically spend much of their time in the outer reaches of the Solar System, undergo dramatic changes each time they pass close to the Sun.
As comets heat up, ices present underneath the surface sublimate (that is they transform directly from solid ice to a gas) and stream out from the comet, dragging along ice and dust particles from the surface. Once free, these dust grains suddenly find themselves being pushed this way and that by a variety of forces – the gravitational field of the comet, the gas flux, and even the tiny but incessant force of sunlight. Over time these particles evolve into the “coma”, the long tail of the comet which can span half the Solar System, with the heart of the comet (the “nucleus”) being reduced to an invisible spot hidden by the bright coma.
Looking at a nucleus far from the Sun, however, shows a quiet different picture. The old picture of comets was that of a dirty snowball, as shown in the picture to the left. However, all of our recent spacecraft flybys have shown that the comet nucleus is in fact dark and hot – and even when active, this activity is confined to only a small fraction of the surface. In fact the images of inactive comets and asteroids are so similar that you would be hard pressed to tell the difference from a picture alone. This of course raises the question of whether or not there really are two distinct classes of object, asteroids and comets, or merely a single broad family of objects, some with more ice, some with less, some in cometary orbits, and others captured and bound to the inner Solar System. In fact there is a session dedicated to just this question (“The asteroid-comet continuum“) at this year’s EPSC (European Planetary Science Congress). You can see for yourself by taking a look at this neat picture produced by Emily Lakdawalla showing all of the comets and asteroids so far visited by spacecraft:
It is immediately clear that amongst the small bodies we have visited, the asteroids are larger; indeed the largest comets we know are considerably smaller than the largest asteroids. But a close up of either reveals very little difference – or, rather, many differences (since every asteroid and comet shows a unique surface), but very little to distinguish the two classes of object.
What I find really interesting here is that the existence (or not!) of the cometary coma, an object that can be enormous, and has been a potent symbol for cultures through the ages, depends critically on the very outer layer of the already rather small cometary nucleus. For a comet to be active, heat has to penetrate through the dust crust (the hot, dry, outer layer of the comet) to the pristine ice, during the small time window when the comet is close to the Sun. Typical comet models, like the one shown (from this paper), assume that during each passage the ice “front” retreats deeper in to the nucleus, and a fraction of the overall mass is loss as gas, dust and ice emissions. It used to be thought that this ice front, or equivalently the thickness of the dust (“mantle”) layer, was at some tens to hundreds of metres depth. However, recent observations – in particular the NASA mission Deep Impact – have suggested that ice can be found only a few centimetres below the surface. So now the story is really interesting! The existence of the coma, which can evolve to billions of kilometres in length, depends on a covering of dust a mere few centimetres thick! If the dust mantle is thick enough, heat doesn’t penetrate to the ice layer at all, and the comet can become dormant – effectively looking like an asteroid.
The ease with which heat flows through a material is described by its thermal conductivity – materials with low conductivity are good insulators, whereas highly conductive materials allow heat to flow easily. Thermal conductivity is a straightforward parameter to measure for large lumps of material; it’s a little harder for granular materials, which conduct heat in a variety of ways non-uniformly! And of course to do this remotely on a spacecraft is even more tricky. Nevertheless, it is a parameter that cannot easily be estimated remotely. Infrared measurements of the surface temperature can help, but you really need to get down and dirty with the comet to get a good measure of conductivity!
Measuring thermal conductivity in-situ on the surface of 67P /C-G is one of primary goals of the MUPUS instrument onboard the Philae lander, part of the Rosetta mission. To do this, MUPUS carries a rather large nail which will be remotely hammered into the surface of the nucleus. With a combination of temperature measurements, and actively heating the surrounding material, MUPUS should be able to study how well heat flows through these vitally important outer layers of a comet. I’ll save the details of that for another post, but you can get a sneak preview in this neat animation produced by the Space Research Institute of the Polish Academy of Sciences (audio in Polish):
So, in summary, comets and asteroids have more in common than first thought – at least from studying their surfaces. How deep these similarities go, and whether we really have an asteroid-comet continuum, or if we just wrongly identify dormant comets as asteroids, remains to be seen! At least with Rosetta we have the chance to study one cometary nucleus in more detail, and to get below the surface as well. One thing is for sure, we will have enough data from Rosetta to keep us happy for at least a few years 😉
As promised in my last blog entry, having talked a little about why I am interested in simulating granular material (i.e. materials made up of distinct particles), I want to talk a little now about some of the tools I’m using. Of course all are free and open source – so you can download them and give it a try yourself!
Granular materials are oddities – sometimes they can behave like solids, and form stable structures, and sometimes they behave like liquids, and flow and pour. And sometimes they transition readily between the two! Because of this wide ranging behaviour, we don’t (yet!) have a nice set of equations to describe their bulk behaviour (as we for do, say, for gases). Instead, it is possible to build numerical models of granular systems by modelling the behaviour of individual particles, their interactions with other particles, walls, etc. This may sound complex, but much of the complexity is in how to computationally deal with tracking enough particles to be useful, not in the underlying physics. So if we can correctly describe the interactions of a pair of particles, we should be able to describe a system of billions of such particles – providing we have enough time and computing power!
This technique is called the Discrete Element Method (DEM) and is an extension of molecular dynamics to deal with larger particles which have a finite size and a rotational degree of freedom. There are several open source codes available which you might like to look into – I have played with three: ESyS-Particle, YADE and LIGGGHTS. Each has its own advantages, and in fact I ended up using bits of each (a geometry building module from ESyS called LSMGenGeo, some YADE scripts to build ballistic aggregates, and LIGGGHTS for my “grunt work”). In this post I’ll focus mainly on LIGGGHTS, since it is the engine at the heart of most of the calculations I’m working on right now.
LIGGGHTS is a fork of the popular molecular dynamics code LAMMPS with enhancements to better deal with the macroscopic particles used in granular mechanics simulations. As such, the computational complexity of stably integrating the equations of motions for millions of particles, and figuring out which particles are interacting, is already well-validated by the many LAMMPS users. The enhancements made by the LIGGGHTS team focus on the contact models (the physics of two particles interacting), linking the DEM model to a fluid dynamics code (OpenFOAM), allowing importing of CAD meshes for greater flexibility, and a host of utilities to enable generating of complex particle packings, support for non-spherical particles and so on. You can check out a recent presentation by the LIGGGHTS team [PDF] for more details!
My aim is ultimately to come up with a validated model of a cometary surface which accounts for low gravity, the various inter-particle forces, and the surface environment. But before one can run, one has to learn to walk – hence I’ve been playing with LIGGGHTS and trying to make a set of simulations that demonstrate the main features I want to include in my model. So for the the next few posts, I’m going to link a few YouTube videos showing output from LIGGGHTS and talk a little about them. If you want a sneak preview, you can jump to the YouTube playlist of these videos!
One of my current research interests is in low gravity regoliths, and in particular the dynamics of ice and dust particles in the upper layers of a cometary nucleus. One of the main reasons for this is preparation for the Rosetta spacecraft’s arrival at comet 67P / Churyumov–Gerasimenko (for a summary, see the video I posted about previously). We have a fair bit of evidence now that cometary nucleii are covered with granular material – most probably volatile-depleted dust particles that do not get lifted from the surface by the escape of sublimating ices. Various landforms have been imaged by spacecraft that could be formed by flow or erosional processes that also imply a granular surface. But to fully understand such features, we need to better understand how granular material behaves under comet-like conditions.
The first port of call in trying to answer such questions is usually the lab – for example in our comet simulation lab at the Space Research Institute we have a vacuum chamber into which we can put various ice and dust mixtures, cool them down with either liquid nitrogen or a closed loop cooler, and switch on the pumps to remove the air. By shining a simulated Sun on the surface, and monitoring temperatures and pressures, it is possible to simulate some of the suspected surface processes taking place on a comet. Such experiments are vital to understand questions such as how gas and heat flow through a porous medium under vacuum. However, they do not capture the dynamics of a real cometary surface, where the low gravity plays an important role.
Just how important is it? Well, first consider that the surface gravity on 67P is something like 30,000 times less than on Earth. This means that the Philae lander, which has a mass of 96 kg on the Earth, will weigh only a few grams on the comet – hence it has screws built into the feet and 2 harpoons to secure itself, and even these operate only when a “holddown” thruster is firing to give some extra force. The same calculation can be applied to the weight of an individual dust particle at the surface. To see what happens to such a particle, not only weight, but other forces need to be considered – for example adhesion (“sticky”) forces, or the force of escaping gasses trying to drag the particle away from the surface. Each of these forces scale differently with the particle size. Under Earth gravity, for example, we only notice the adhesion forces when we are dealing with very small particles; since weight decreases more rapidly than adhesion as we move to smaller particles, at some point it dominates. This explains why flour acts differently from dry sand when you try to pour it.
Ground flour is mostly micron sized (a millionth of a metre), whereas sand can have grains up to a millimetre in size. Because individual flour grains are so small, adhesive forces make them cling to each other, and any container they’re in. This means that they don’t flow well and are called cohesive. Coarse dry sand, on the other hand, typically flows very readily – in this case the particles are heavier and their own weight and momentum governs their motion. Now compare the situation on Earth to that on a comet – a sand grain would experience a similar adhesive force as on Earth (there are differences due to temperature and surface cleanliness, but we’ll leave that for another post!), but it would weight 30,000 times less! So even larger particles on a comet might be expected to behave like tiny particles on the Earth. In fact from such calculations alone one can expect that even centimetre sized particles could behave cohesively under certain conditions – very different from our every day experience!
However, understanding how a few particles behave is very different from understanding the complexity created when millions of such particles interact. Experiments under low gravity are certainly possible – using drop towers (think of a tall tower, pumped free of air, with your experiment dropped from the top – see the schematic above!), parabolic flights (the so-called “vomit comet”), sounding rockets, or of course experiments on orbit. But these are either of limited duration (e.g. until your payload hits the bucket of polystyrene beads at the bottom of the drop tower!), or very expensive (e.g. flying onboard the International Space Station). Instead one can use computer simulations. Modern computers and clusters of computers can simulate the collective behaviour of millions, if not billions of particles. Making sure that the physics holds still requires experiments to validate the models, but it’s often a lot quicker and cheaper than running hundreds of experiments, and it allows access to regimes that are hard to simulate on Earth!
So that’s a little about the “why?” of running such simulations – in my next post I’ll show the software I’ve been using and explain a bit of the “how?”.