Pluto is just 3.5 pixels across in the latest images from the New Horizons spacecraft. That’s nine square pixels. You can’t do much with nine pixels. You might be able to see crude patterns of light and dark, but you probably wouldn’t call it a map. Still, it’s a start.
In a few months, this will all change. Craters, mountains and other landforms will take shape before our eyes. When New Horizons flies past Pluto in July, we will see a new, alien landscape in stark detail. At that point, we will have a lot to talk about. The only way we can talk about it is if those features, whatever they turn out to be, have names.
Today we are beginning a campaign called “Our Pluto”. The goal is to gather together the names that we will eventually use to label the maps of Pluto and its large moon, Charon. After discussions with the International Astronomical Union (IAU), we have defined a set of broad themes for these names, related to mythology, literature and history.
The New Horizons science team is doing something unprecedented. Naming campaigns have been held before, but on a different scale. Today, the entire landscapes of Pluto and Charon is open to the public. We have called the campaign “Our Pluto” because we think that everyone should have a say in the names we use on those strange and distant worlds. At ourpluto.seti.org, you can vote for your favorite names, talk about them, and nominate names that we might have overlooked.
After the campaign ends, the New Horizons science team will select your best ideas and pitch them to the IAU. The IAU will have final say over the names on the maps of Pluto and Charon.
Let the conversation begin!
A Piece of Mars: With all due apologies to followers of the show Coupling, I have to call these things “melty dunes”. This link shows what a crisp dune should look like. The dunes in this 600×450 m (0.37×0.28 mi) scene, however, have rounded crests and sand that seems to have ponded around the bottom of the dunes. These are common at high southern latitudes on Mars. (HiRISE ESP_039610_1150, NASA/JPL/Univ. of Arizona)
A piece of Mars: Ripples form endless chevrons in this 600×450 m (0.37×0.30 mi) scene. It’s really the crest of a dune that connects all the vertices in the chevrons, making that straight line that runs nearly vertical through the center. Wind from the south (bottom) is deflected by this crest and other local topography just out of the scene. This pattern has been there for at least 3 Mars years. How long will it last? (HiRISE ESP_013785_1300, NASA/JPL/Univ. of Arizona)
No one is ever excited when the topic of “dust” is brought up. Usually dust is a hindrance – something you sweep away during spring-cleaning, or an annoyance because your allergies can’t handle it. But for astronomers, finding dust around another star – i.e., circumstellar dust – is like finding the next piece of an interstellar puzzle. That’s because circumstellar dust holds clues to understanding not only the origins of planets outside of our solar system, but also gives us a leg up in figuring out our place in the Universe. (more…)
A piece of Mars: Most dunes on Mars are dark, like these and these. So why is this one bright? It’s adjacent to a more typical, dark dune. It’s possible that there are two populations of sand here that are different enough in size or density, and so they respond to different winds – thus producing remarkably different dunes in the same location. (HiRISE ESP_039568_1120, NASA/JPL/Univ. of Arizona)
A piece of Mars: The smooth areas are eroded dunes, separated by fields of boulders (the scene is 1.51×1.14 km or 0.93×0.71 mi). The largest boulder near the center is 7.5 m (25 ft) across, the size of a small RV. The interesting wave patterns on the lower sides of the smooth dunes… well, I don’t know. My best guess is it’s another type of bedform created from the sand of the smooth dunes. Do you know? (HiRISE ESP_039595_1230, NASA/JPL/Univ. of Arizona)
A piece of Mars: What happens to dunes as they move over rough terrain? This is what a barchan looks like on a relatively flat surface. If the hills are smaller than the dune, then it does its best to pretend they don’t exist, like the one in this image. It’s 175m (574ft) wide and 190m (623ft) long, with a slipface indicating overall migration to the northeast. (HiRISE ESP_039524_1445, NASA/JPL/Univ. of Arizona)
A piece of Mars: This scene (600×450 m or 1969×1476 ft) is covered in small craters, formed by the splash of a larger crater nearby. They cover everything, even the bright ripples visible on the right. So the ripples were there before the impact that formed all these little craters. And yet… there are itsy little gray ripples on the upper right, merging with the crater rims – these are new ripples, younger than the craters. On Mars, it’s the wind that wins in the end. (HiRISE ESP_039057_1485, NASA/JPL/Univ. of Arizona)
A piece of Mars: The curving ridge of a mountain has signs of many small landslides. Mantled on top of these is an older set of landslides that has been partially eroded away. The rippled edge of this older deposit suggests that it is wind that has done the erosion. So the history here goes: mountains, then landslides, then wind erosion, then new smaller landslides. (HiRISE ESP_039195_1755 NASA/JPL/Univ. of Arizona)
A piece of Mars: This 600×450 m (1969×1476 ft) scene has a complex sedimentary history. How are bearded craters and dunes formed? They weren’t always bearded. At some point, a deposit of bright material accumulated on this surface, and was then eroded so that all that remains of it is what is protected by topography (anything that pokes up like dunes or crater rims). Can you find the boulder that has tumbled downslope (it too has a beard!). (HiRISE ESP_038826_1700, NASA/JPL/Univ. of Arizona)