This sequence of seven images from the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter shows wind-caused changes in the parachute of NASA's Mars Science Laboratory spacecraft as the chute lay on the Martian ground during months after its use in safe landing of the Curiosity rover. Image credit: NASA/JPL-Caltech/Univ. of Arizona.
How cool is this? An animation of seven images from the HiRISE camera on the Mars Reconnaissance Orbiter show a “flapping” of the parachute that allowed the Curiosity rover to descend safely through Mars atmosphere images. The chute, imaged as it lay on the ground following the rover’s safe landing, was blown about by the Martian breeze! The images were acquired by HiRISE between August 12, 2012 and January 13, 2013. The different images show distinct changes in the parachute, which is attached to the backshell that encompassed the rover during launch, flight and descent.
The HiRISE team explains the animation:
In the first four images there are only subtle changes, perhaps explained by differences in viewing and illumination geometry.
Sometime between September 8, 2012 and November 30, 2012, there was a major change in which the parachute extension to the southeast (lower right) was moved inward, so the parachute covers a smaller area. In the same time interval some of the dark ejecta around the backshell brightened, perhaps from deposition of airborne dust.
Another change happened between December 16, 2012 and January 13, 2013, when the parachute shifted a bit to the southeast. This type of motion may kick off dust and keep parachutes on the surface bright, to help explain why the parachute from Viking 1 (landed in 1976) remains detectable.
The Mars Science Laboratory’s parachute flaps in the wind on Mars. Images by the HiRISE camera on the Mars Reconnaissance Orbiter, animation by Doug Ellison.
And here’s a look at how big the chute really is (note the people for scale):
MSL parachutte tested in a wind tunnel. Credit: JPL.
The Dunes of 'Inca City.' Credit: NASA/JPL/University of Arizona.
These pictures require you to grab the 3-D glasses you have handy by your desk (if you don’t have a pair, here’s some great options for buying some) and get a “you-are-there” experience from the HiRISE camera on the Mars Reconnaissance Orbiter. Here, you can virtually tumble down crater walls, hover over steep cliffs, and see how layered bedrock appears from above.
Our lead image is of an area referred to as “Inca City,” the informal name given by Mariner 9 scientists in 1972 to a set of intersecting, rectilinear ridges, which some people thought looked like structures or streets. Even back then scientists thought they might be dunes, but that didn’t keep people from going off the deep end about this region. But the power of HiRISE has revealed these truly are dunes, and in this image you can see some of the seasonal processes as the region goes from winter to spring. As the carbon dioxide frost and ice on the dunes warms, small areas warm and sublimate (turn from solid to gas) faster, creating a speckled surface.
Fresh 4-Kilometer Rayed Crater Northeast of Chimbote Crater. Credit: NASA/JPL/University of Arizona.Cliff with Columnar Jointing. Credit: NASA/JPL/University of Arizona.Central Uplift of a Large Impact Crater. Credit: NASA/JPL/University of Arizona.Buttes and craters: Compositional Diversity in Northern Hellas Region. Credit: NASA/JPL/University of Arizona.Well-Preserved 4-Kilometer impact Crater. Credit: NASA/JPL/University of Arizona.Flow Boundary in Elysium Planitia. Credit: NASA/JPL/University of Arizona.A fissure on Mars named Cerberus Fossae. Credit: NASA/JPL/University of Arizona.Possible Gullies in Graben. Credit: NASA/JPL/University of Arizona.Layered Bedrock on Crater Floor. Credit: NASA/JPL/University of Arizona.
Tracks from the Curiosity rover were imaged by the HiRISE camera on the Mars Reconnaissance Orbiter on January 2, 2012. Credit: NASA/JPL/University of Arizona.
Look closely and see where the Curiosity rover has been roving about inside Gale Crater on Mars, from “Bradbury Landing” to its current location in “Yellowknife Bay.” This shot was taken by the HiRISE camera on board the Mars Reconnaissance Orbiter on January 2, 2013.
“This image shows the entire distance traveled from the landing site (dark smudge at left) to its location as of 2 January 2013 (the rover is bright feature at right),” wrote HiRISE principal investigator Alfred McEwen on the HiRISE website. “The tracks are not seen where the rover has recently driven over the lighter-toned surface, which may be more indurated [hardened] than the darker soil.”
You can compare this image to one taken on September 8, 2012 to see how much the rover has driven in Gale Crater:
Curiosity rover tracks seen from orbit by HiRISE on September 8, 2012. Credit: NASA/JPL/University of Arizona.
And here’s a map of Curiosity’s travels that NASA released yesterday:
Mission scientists said at a briefing yesterday (January 15, 2013) that between Sol (Martian day) 120 and Sol 121 of the mission — which equates to Dec. 7 and Dec. 8, 2012 — Curiosity crossed over a terrain boundary into lighter-toned rocks that correspond to high thermal inertia values observed by NASA’s Mars Odyssey orbiter. The green dashed line marks the boundary between the terrain types.
The inset graphs the range in ground temperature recorded each day by the Rover Environmental Monitoring Station (REMS) on Curiosity. Note that the arrival onto the lighter-toned terrain corresponds with an abrupt shift in the range of daily ground temperatures to a consistently smaller spread in values. This independently signals the same transition seen from orbit, and marks the arrival at well-exposed, stratified bedrock.
Sol 124 (Dec. 11, 2012) marked the arrival into an area called “Yellowknife Bay,” where sulfate-filled veins and concretions were discovered, along with much finer-grained sediments providing evidence of past water interacting with the surface.
Here’s the Mars weather report provided by REMS for Sol 158 (January 15, 2013):
Yep, you really want to click on this link to see the full color version of this great oblique view of Mt. Sharp (a.k.a. Aeolis Mons) in Gale Crater, taken by the HiRISE camera on the Mars Reconnaissance Orbiter. Or you can click here to see the full “raw” strip from the spacecraft.
“The viewing angle is 45 degrees, like looking out an airplane window,” wrote HiRISE Principal Investigator Alfred McEwen on the HiRISE website. McEwen noted that this color version doesn’t show the Curiosity rover or the hardware left over from the landing on Mars, but it does provide a great view of Gale Crater’s central mound.
So how “true” is the color in this image?
“It may be close, but not true,” Christian Schaller from the HiRISE team told Universe Today. Schaller pointed out the description (pdf) of color in HiRISE images from the HiRISE team:
It isn’t natural color, as seen by normal human eyes, because the IR, RED, and BG channels are displayed in red, green, and blue colors. For the Extras products, each color band is individually stretched to maximize contrast, so the colors are enhanced differently for each image based on the color and brightness of each scene. Scenes with dark shadows and bright sunlit slopes or with both bright and dark materials are stretched less, so the colors are less enhanced than is the case over bland scenes.
Jim Bell, the lead scientist for the Pancam color imaging system on the Mars Exploration Rovers, said he likes to use the term “approximate true color” because the MER panoramic camera images are estimates of what humans would see if they were on Mars. Other colleagues, Bell said, use “natural color.”
“We actually try to avoid the term ‘true color’ because nobody really knows precisely what the ‘truth’ is on Mars,” Bell told Universe Today in 2007 for an article about the art of extraterrestrial photography. In fact, Bell pointed out, on Mars, as well as Earth, color changes all the time: whether it’s cloudy or clear, the Sun is high or low, or if there are variations in how much dust is in the atmosphere. “Colors change from moment to moment. It’s a dynamic thing. We try not to draw the line that hard by saying ‘this is the truth!’”
Several gorgeous images are in this week’s update from the HiRISE camera on board the Mars Reconnaissance Orbiter. This lovely image shows the cliffs at the edges of huge ice sheet at the North Pole of Mars. These cliffs are about 800 meters (2,600 feet) high, and the ice sheet is several kilometers thick at its center. This is a great spot to look for ice avalanches that HiRISE has captured previously. The HiRISE team said that the slopes of these cliffs are almost vertical, plus dense networks of cracks cover the icy cliff faces making it easier for material to break free. The team regularly monitors sites like this to check for new blocks that have fallen. You can look for yourself to see if any avalanches have occurred since the last image was taken of this area, almost exactly one Martian year ago.
The HiRISE scientists monitor these regions to help in understand the climatic record stored in the ice sheet itself.
What else did HiRISE see this week?
These cool-looking dunes look reminiscent of Pac-Man, and they might even be moving across the surface of Mars! They are approximately 100 meters across and are traversing a bumpy, hard terrain, pushed across the surface by the winds on Mars. The HiRISE team will take more images of this dune field in subsequent passes to determine whether these dunes are really moving.
This image shows a gullied crater in the Southern mid-latitudes with light-toned deposits near the center of its floor, and two areas of collapsed terrain at the northern and southern edges of the crater floor.
For more information on each of these images, click on them to see the original page on the HiRISE website, or go to the HiRISE website to see all the wonderful images from Mars.
Outflow channel in the Tharsis region on Mars. Credit: NASA/JPL/University of Arizona
Large features on Mars called outflow channels have been a point of contention among planetary scientists. “Most Mars scientists accept that outflow channels were carved by water, but alternate hypotheses persist, especially that lava carved the outflow channels,” said Alfred McEwen Principal Investigator of the HiRISE camera on the Mars Reconnaissance Orbiter. McEwen said that water is still the preferred mechanism and he doubts that all the channels could have been created by lava flows.
But in what could be seen as a type of compromise, he offered a new theory for the outflow channels, based on observations by HiRISE: the channels were originally carved by huge water flows on ancient Mars and later were partially filled in by lava.
“This sequence of events provides a better explanation,” McEwen said.
Large outflow channels can be 10 km or more in width and may be hundreds of kilometers long. From orbital images, they appear to be huge, dry river beds, carved by very large volumes of running water.
While these features are too large to have been caused by flooding from rainfall, other explanations have been offered. One model involves large amounts of water frozen as permafrost in the soil and when a major source of local heating occurred, such as volcanic activity, there was melting and catastrophic flooding.
However, other explanations don’t involve water at all, but suggest flowing lava created these channels.
Speaking at the 2012 Lunar and Planetary Science Conference last week, McEwen mentioned specifically one proponent of the lava hypothesis, David Leverington from Texas Tech University, who proposed last year that slippery, low-viscosity lavas created the channels. Leverington says the lava hypothesis offers a simpler explanation that fits well within a wider geological framework of Mars and compares well with similar channel-like features on the Moon and Venus.
“He makes some good points,” McEwen said, “and argues for a form of Occam’s Razor. But we have been searching extensively with HiRISE and finding things that satisfy Leverington’s challenges.”
McEwen said the abundant evidence of water carving the channels is too hard to dismiss. Several examples of outflow channels show deposits from water-based flooding that lava flow can’t explain; additionally, there is ample evidence of bedrock erosion by water on Mars.
McEwen also said crater dating areas of several outflow channels show that the channels themselves are older than the lava flow.
Part of Athabasca Valles, draped in lava. Credit: NASA/JPL/University of Arizona
“In the Athabasca Valles channels, MRO data showed that lava completely filled the channels and even overflow in places,” he said. “The lava can actually make channels look young.”
Uzboi Valles offers the best counterexample to Leverington’s hypothesis, McEwen said. “No lava fills in this highlands channel, and the channel preserves local layered alluvial deposits and shorelines. So that means we cannot explain all outflows channels from lava erosion.”
McEwen and his team suggest that large floods may have occurred in the Hesperian to early Amazonian, ending about 1 to 1.5 billion years ago, carving the channels. Then, later came the lava flows that formed Mars’ broad plains and sand dunes that we now see – which also filled in some of the outflow channels.
Bedrock Exposures in Uzboi Vallis. Credit: NASA/JPL/University of Arizona
But McEwen said the debate about these channels is good science. “Did water create these channels? That is a good question,” he said. “We shouldn’t just assume the answer is yes. But we propose water must have carved at least some of the channels, and that water outflow is the main mechanism. If you disagree with anything I’ve said, go to the HiRISE website’s “HiWish” page to suggest areas for further imaging of these features. I’ve been disappointed how few members of the science community have used this tool,” he said.
Clouds give a fuzzy view of ice-topped dunes on Mars. Credit: NASA/JPL/University of Arizona
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The science team from the HiRISE camera on the Mars Reconnaissance Orbiter wanted to take another look at a region of icy sand dunes on Mars to look for seasonal changes as spring is now arriving on the Red Planet’s northern hemisphere. But the view was obstructed by clouds, creating this unusual hazy view.
“This happens occasionally. We’ve found that weather forecasting on Mars is just as challenging — if not more — than on Earth,” said HiRISE team member Candy Hansen, who I nabbed in the hallway during the Lunar and Planetary Science Conference today, to ask about this unique image. “The clouds are likely made of water ice crystals, and the dunes have a coating of CO2 ice that is just starting to sublimate away as the Sun’s rays are getting stronger in this region.”
Hansen said these are dark barchan, or crescent-shaped dunes. During the winter, this region was completely covered with carbon dioxide ice, but now just the the tops of the dune have ice; also visible are what looks like white cracks, which is ice protected in shallow grooves on the ground. HiRISE will likely check back on this region later during the Martian summer to provide the science team with a seasonal sequence portfolio of images of the region, a benefit of having a mission in orbit for several years. MRO and HiRISE are workhorses, having been in orbit since March of 2006.
These barchan (crescent-shaped) sand dunes are found within the North Polar region of Mars. Credit: NASA/JPL/University of Arizona
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Say the word “dunes” and the image that likely comes to mind is the sort of features you’d see in the Sahara Desert; huge mounds of carmel-colored shifting sand. But on Mars, dunes take on an entirely different connotation, and with the orbital eyes of the HiRISE camera on the Mars Reconnaissance Orbiter, we’ve seen some pretty bizarre-looking dunes. Take the image above for example, a newly released photo of well-speckled dunes in Mars’ north polar region. In this image, taken during the northern spring season, the dunes and ground are still covered in seasonal frost. “The speckled appearance is due to the warming of the area — as the carbon dioxide frost and ice on the dunes warms, small areas warm and sublimate (turn from solid to gas) faster, creating small jets that expose/deposit dark sand and dust onto the surface,” writes Serina Diniega on the HiRISE website. “Notice that there are no spots on the ground between the dunes — that is because the ground stays more uniformly cold, unlike the darker dune sand.”
See below for more weird dunes on Mars.
Dunes in Aonia Terra on Mars. Credit: NASA/JPL/University of Arizona
These dunes look as through someone has thrown a rippled blue-toned cloth across Mars’ surface. HiRISE is monitoring these dunes in Aonia Terra for changes such as gullies, which form over the winter from the action of carbon dioxide frost. This image was taken on January 18, 2012 here on Earth, but the season in on Mars where this was taken was late fall in the Southern hemisphere. “Frost is just starting to accumulate here, and is concentrated on pole-facing slopes and in the troughs between the meter-scale ripples,” wrote HiRISE Principal Investigator Alfred McEwen.
Dunes in Russell Crater Dunes on Mars. Credit: NASA/JPL/University of ArizonaPink dunes with black polka-dot speckles. Credit: NASA/JPL/University of ArizonaA wide area of dunes in Terra Cimmeria look as if they are being viewed under water. Credit: NASA/JPL/University of ArizonaFans and polygons on Dunes. Credit: NASA/JPL/University of ArizonaDark sand dunes at high Northern latitudes on Mars are covered seasonally by a layer of condensed carbon dioxide (dry ice), visible in this image. Credit: NASA/JPL/University of Arizona
Chocolate dunes? Credit: NASA/JPL/University of Arizona
The Phoenix lander still visible at Mars north polar region, nearly 4 Earth years and 2 Mars years after the spacecraft landed on Mars. Credit: NASA/JPL/University of Arizona
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I spy Phoenix! said the HiRISE camera on board the Mars Reconnaissance Orbiter! This new image acquired on January 26, 2012 shows that the Phoenix lander and its backshell are still visible from Mars’ orbit. The parachute, seen in earlier images, is probably about 130 meters south of where this picture ends. This is one of a series of images to monitor frost patterns at the Phoenix landing site, said HiRISE Principal Investigator, Alfred McEwen, adding that this new images shows almost the same appearance of the hardware as 1 Mars years ago, in 2010. See larger versions of this image at the HiRISE website.
See below for comparison images from orbit from 2008, shortly after Phoenix landed and 2010, after the mission had ended.
Two images of the Phoenix Mars lander taken from Martian orbit in 2008 and 2010. The 2008 lander image shows two relatively blue spots on either side corresponding to the spacecraft's clean circular solar panels. In the 2010 image scientists see a dark shadow that could be the lander body and eastern solar panel, but no shadow from the western solar panel. Image credit: NASA/JPL-Caltech/University of Arizona
In these images, also from the Mars Reconnaissance Orbiter, signs of severe ice damage to the lander’s solar panels show up in the 2010 image, with one panel appearing to be completely gone. The Phoenix team says this is consistent with predictions of how Phoenix could be damaged by harsh winter conditions. It was anticipated that the weight of a carbon-dioxide ice buildup could bend or break the solar panels.
An avalanche on Mars captured by the HiRISE camera on the Mars Reconnaissance Orbiter on November 27, 2011. Credit: NASA/JPL/University of Arizona.
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Its avalanche season on Mars! And once again the HiRISE camera on the Mars Reconnaissance Orbiter has captured an avalanche taking place on a steep cliff or scarp in Mars’ north polar region. Back in 2008, the HiRISE team created quite a sensation when it captured an avalanche in action on Mars. The high resolution camera did it again in 2010 when springtime arrived once more. Now, another Mars year later, the team has been monitoring specific areas, looking for evidence of avalanches and they hit pay dirt – literally. This image of an avalanche taking place is from a large image “strip” from HiRISE taken in the extreme northern latitude of Mars, about 85 degrees north.
Dust, fine-grained ice and possibly large blocks of either regolith or rocks has detached from a steep, towering cliff and cascaded below. The HiRISE team say the occurrence of avalanches is spectacularly revealed by the accompanying clouds of fine material that continue to settle out of the air.
The avalanches are a result of carbon-dioxide frost that clings to the scarp in the darkness of winter, and when sunlight hits them in the spring they loosen up and fall.
These events happen mostly in the middle of spring, roughly equivalent to April to early May on Earth. And it seems this is a regular spring process at Mars’ north pole that may be expected every year.
This image is part of the latest PDS release from HiRISE.
