After a decade-long journey by the New Horizons spacecraft through our solar system, we can finally add Pluto and its main moon Charon to the roster of large icy bodies whose landscapes we have seen. And it was worth the wait. The first detailed images are surprising, showing a remarkable lack of impact craters on both Pluto and Charon.
NASA’s probe passed within 14,000 km of Pluto on July 14, and – after a nervous 12-hour wait for its call home – has begun to send back its trove of data, which includes images revealing details as small as 100 metres across.
The most detailed image of part of Pluto (see lead image) is truly staggering. Not a single impact crater is to be seen in this regiopn, so the surface must be very young – reshaped by some sort of geological activity such as faulting or icy volcanism.
It is rather early to speculate, but maybe Pluto captured Charon only a few hundred million years ago (rather than billions), and we are seeing the effect of the very strong tidal interactions that would have ensued. Pluto could, in fact, even be geologically active today. I watched this image come in via a NASA press conference with a group of colleagues, and we were both amazed and mystified.
Pluto – which has a diameter of 2,370km – shares its orbital space with many comparable-sized bodies and crosses the orbit of the giant planet Neptune, which is why it does not qualify as a planet. Nevertheless, it is a fascinating world, as indeed is Charon (1,208km diameter).
Both are bodies whose rocky interiors are deeply buried by ice of various kinds. There is probably water-ice at depth on Pluto, but the surface ice is a mixture of frozen methane, ethane, carbon monoxide and nitrogen.
Charon, with its weaker gravity, has lost the substances that can turn to vapour and escape more easily, and is mostly water-ice tainted by ammonia. That much we already knew. But New Horizons has been gathering data that will show us how these ices are arranged across each surface – and may find traces of other constituents.
adapted from multiple datasets via http://www.nasa.gov/mission_pages/newhorizons/main/index.html, Author provided
Already the images are throwing up new questions. The composite image above, compiled from various images during New Horizons' approach, shows slightly enhanced colour views of Pluto and Charon. Pluto is notable for patches of both bright and dark material in a belt straddling its equator. What are these? Is the bright, heart-shaped patch some kind of nitrogen frost or snow deposit? Is the dark stuff carbon or tar of some kind? (We know that solar ultraviolet radiation turn methane into tar). Charon, unique among known worlds, has a dark polar cap. Is that old, radiation-damaged methane, whereas the greyer equatorial region is cleaner water-ice?
An Open University PhD student has already made a preliminary photogeologic map of the half of Pluto seen during approach (see below). It shows the “heart”, the dark patches and other units in different colours – representing different terrains. Several impact craters have also been marked in green, and a few wrinkles on the surface.
Peter Fawden, Open University, Author provided
Then there are the tectonic features, the faulting or other deformation of the outer layer of a planet, to consider. These are better seen in black-and-white images. For example in the next image, just inside the eastern (right-hand) edge of the disk, the surface is cut by a fracture deep enough to cast shadows.
Charon has similar fractures too. These are also known on several icy moons, such as Ariel and Titania at Uranus, and Tethys at Saturn, where they are described as chasmata (Latin for chasms). The image below shows Charon and Uranus’s moon Titania at the correct relative scale. They both have fractures visible near their right-hand edges, which could be a remnant of a time when the surface became broken, perhaps by tidal forces.
Scientists are eagerly awaiting more data from New Horizons' onboard memory, which is now nearly full, that will take a total of 16 months to transmit to Earth. This is because at a range of more than 4.6 billion km from Earth the signal is so weak that it has to be transmitted at a slow rate of about 1 kilobit per second (you may be reading this via wi-fi operating at tens or hundreds of megabits per second). Although we may have to wait a while before we see the best of the pictures, what we already have already seen is enough to greatly intrigue planetary scientists such as myself.
David Rothery is author of Planets: A Very Short Introduction (Oxford University Press, 2010) and Moons: A Very Short Introduction (Oxford University Press, in press). He receives funding from the UK Space Agency and the Science & Technology Facilities Council for work related to Mercury and the European Space Agency's Mercury orbiter BepiColombo.
Authors: The Conversation