Tag: Mars

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Cool image time! The picture to the left, cropped, reduced, and sharpened to post here, was taken on April 25, 2024 by the high resolution camera on Mars Reconnaissance Orbiter (MRO).

It shows what the science team labels a “scour pit island,” an area about 13 miles long and 3.5 miles wide where the ground is covered by these pits.

Your eye may play tricks on you, reversing the elevations. These are all pits, with most having a central peak or ridgeline. To help, note that the sunlight is coming from the west. The arrow on the center left of the picture sits on a plateau above these pits.

According to this paper [pdf], the pits are slowly dug out by the wind coming from the southeast blowing to the northwest, as indicated by the arrows. The central peaks or ridges are thought to be a hint of the original topography, with the wind only able to pull ash from the terrain around these peaks.
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For original images go here and here.

Today’s two cool images above provide a nice sense of the massive nature of many Martian landslides. Scientists often call this kind of slide “mass wasting,” because rather than it occurring because a single rock propagates a larger flow of rocks as it starts rolling downhill, this slide occurs because a large section of the hillside suddenly breaks free and moves downward as a unit, carving a path as it goes.

Mars has a lot of these kinds of slides, likely caused partly by its lower gravity, 39% that of Earth’s.

The overview map to the right marks the location of both slides by their numbers. Number one took place on the eastern interior rim of a 56-mile-wide and 7,000-foot-deep unnamed crater the dry tropics of Mars. The slide dropped about 3,000 feet, beginning about halfway down from the top of the rim and not quite reaching the crater floor. The picture was taken by the high resolution camera on Mars Reconnaissance Orbiter (MRO) on March 31, 2024.

Number two occurred on the western interior rim of a 32-mile-wide and 6,500-foot-deep unnamed crater in the mid-latitudes where near-surface ice and glacial features are often found. In this case the slide fell downward about 3,500 feet. The picture was taken by MRO’s high resolution camera on March 14, 2024.

Despite the different latitudes and thus different climates and geological settings, both landslides look similar. It is possible they occurred under similar conditions, but at very different times. Or it is also possible that the Mars gravity and general environment promotes these mass wasting events everywhere.

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Cool image time! The picture to the right, rotated, cropped, reduced, and sharpened to post here, was taken on April 25, 2024 by the high resolution camera on Mars Reconnaissance Orbiter (MRO).

The scientists label this layered deposits, but that hardly describes what we are looking at. This slope, as shown in the overview map above, is the north flank of the central ridgeline inside the giant enclosed canyon depression dubbed Hebes Chasma, located just north of the main canyon of Valles Marineris, the largest known canyon in the solar system.

From floor to peak the ridge is around 16,000 feet high. Yet, its peak sits more than 6,000 feet below the plateau that surrounds Hebes. In this one picture the drop from high to low is only 5,700 feet, with thousands of feet of cliff unseen below and above.

Yet every single foot of these gigantic cliffs is layered. Based on close-up data obtained by Curiosity on the slopes of Mount Sharp in Gale Crater on the other side of the planet, the layers we can see here only represent the most coarse sedimentary boundaries. Within these layers are likely thousands upon thousands of thin additional layers, each likely representing some cyclical climate proces on Mars, even down to individual years.

Note too that the lower slopes in this picture (near the top) suggest some form of erosion flowing downhill. What caused that erosion process however remains unknown. It could have been liquid water, or glaciers, or some other process unique to Mars that we still haven’t uncovered.

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Today’s cool image is another example of how little we really understand the geology of Mars. The picture to the right, rotated, cropped, reduced, and enhanced to post here, was taken on February 22, 2024 by the high resolution camera on Mars Reconnaissance Orbiter (MRO).

The focus of the image is the eastern end of a large and very distinct dune field inside 31-mile-wide Matera Crater, as shown by the white rectangle in the overview map above. The field fills an area 10 by 11 miles inside the floor of the crater. On that eastern end is a very pronounced drainage gully dropping downhill about 2,000 feet to the east.

Gullies on Martian slopes, especially on the interior rims of craters, are not unusual. Though their true cause is not yet confirmed, the theories behind their existence all relate to some form of water/ice process, mostly relating to the seasonal freeze-thaw cycle.

This picture was taken in the spring, exactly when seasonal changes might be spotted. In fact, scientists have been taking regular MRO images of this gully since 2007, when it was featured image. From that 2007 caption:
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Cool image time! The picture to the right, cropped, reduced, and sharpened to post here, was taken on February 26, 2024 by the high resolution camera on Mars Reconnaissance Orbiter (MRO). It shows what the scientists label as the “relation between flutes and flows”.

The flood lava plain in the northern part of this picture represents the flows. At some point in the distant past some event, either a volcanic eruption, or a large impact, caused lava to spew out across this terrain, leaving behind a smooth plain that has only partly been marked by later crater impacts.

The many parallel ridges pointing to the northeast in the southern part of the picture represent the flutes.

One other very important flow is not directly visible. The prevailing winds that blow to the southwest are what carved these flutes, slowly pushing the material southward while carving out the many gaps between the ridges.
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Sometimes the cool geological features I find in the Mars Reconnaissance Orbiter (MRO) image archive are so large they are difficult to present on this webpage. Today is an example. The picture to the right, cropped, reduced, and sharpened to post here, was taken on March 13, 2024 by the high resolution camera on MRO. It shows the distinct run-out of debris from a landslide that flowed downhill to the north as a single unit of material. Along the way it carved its track in the ground, almost like a ramp.

The full picture however suggested something much more spectacular. In that full image this landslide is merely a small side avalanche to a landslide many times larger. And that high resolution picture only shows what appears to be a small section of that giant slide. Obviously, this required a look at the global mosaic produced by MRO’s context camera to find out how far that avalanche actually extended.
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Cool image time! The picture to the right, rotated, cropped, reduced, and sharpened to post here, was taken on February 10, 2024 by the high resolution camera on Mars Reconnaissance Orbiter (MRO). It shows what the scientists label boringly “Lava Interactions with Landscape.”

What is the lava, and what is the landscape? Here’s is my initial guess, based simply on looking at this image alone. The mound in the middle is the landscape, the rounded top of a very ancient mountain or hill. The flat plain that surrounds it is flood lava, that in the far past poured in and mostly buried the mountain.

Everything here signals a very old terrain. To get this mountain worn so smooth from the thin Martian atmosphere has to have taken more than a billion years. And that flood lava has to also be as old, because of the number of craters on its surface. I don’t know the impact rate, but I know it takes time to accumulate this number of impacts.

The sense of age is further underlined by the moat that surrounds the hill. When that lava poured in, it would have flooded right up to the mountain slope. Over time the weakest section of lava, most prone to erosion, would be that contact point. To wear it away as we now see it must have taken many eons.

All these speculations are a very unreliable guesses. To get a better understanding of this terrain it is essential we look at more than this picture alone.
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Cool image time! The picture to the right, rotated, cropped, and enhanced to post here, was taken on December 17, 2023 by the high resolution camera on Mars Reconnaissance Orbiter (MRO). It shows what the scientists label “banded terrain and possible breached crater.”

Banded terrain is another name for a geological feature dubbed “taffy terrain” and only found on Mars, and furthermore only found there in Hellas Basin, the deepest giant impact basin on the red planet. This taffy terrain is considered very young, no than 3 billion years old, and formed from the flow of some form of viscous material, though what that material is remains unsolved.

This image however may help solve that mystery. The breached crater is just off frame to the upper right. The two-fingered flow coming down from the picture’s top is the flow coming out of the crater’s gap.
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Cool image time! The picture to the right, cropped, reduced, and sharpened to post here, was taken on February 25, 2024 by the high resolution camera on Mars Reconnaissance Orbiter (MRO). It shows a small spot of the floor of Mars’ giant canyon Valles Marineris, the largest such canyon known in the solar system, as indicated by the white dot on the overview map above.

This location is not actually at the very bottom of the canyon, but on a very large mountainous bench extending out about 20 miles from the canyon’s south rim. It seems there is a lot of dust and sand on this bench, producing many miles of swirling dunes. It also appears there are many terraced layers in the region as well, which also swirl in curves going in many different directions. Though it appears that most of the swirls in this picture are from layers in the bedrock, this conclusion is not certain. For example, are the curves on the top of the mesa dunes or bedrock layers? The answer is hardly clear.

For scale, the canyon at this location is about 80 to 90 miles wide. The northern rim rises five miles from the bottom to the top, while the south rises seven miles. And yet, though five to ten times larger than Earth’s Grand Canyon, this is only a small side spur of Valles Marineris.

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Cool image time! The picture to the right, cropped, reduced, and sharpened to post here, was taken on March 2, 2024 by the high resolution camera on Mars Reconnaissance Orbiter (MRO). It shows what the scientists label as “platy fractures.”

The ridges likely align with cracks that developed over time on this lava field, which then formed the ridges when magma oozed up from below. It is also possible that these events were closely linked, that the pressure from the magma below cracked this lava field, with the magma immediately oozing out. Because the pressure was evenly applied across the whole surface, it caused a network of cracks and plates, not a single vent or caldera. The even distribution of the pressure also caused only a small amount of lava to leak out to form the ridges.
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Cool image time! The picture to the right, cropped to post here, was taken on March 16, 2024 by the high resolution camera of Mars Reconnaissance Orbiter (MRO). It was released today as a captioned picture from MRO’s camera team. As noted in the caption, written by the camera’s principal investigator Alfred McEwen:

This image shows a field a sand dunes in the Martian springtime while the seasonal carbon dioxide frost is sublimating into the air. This sublimation process is not at all uniform, instead creating a pattern of dark spots.

In addition, the inter-dune areas are also striking, with bright frost persisting in the troughs of polygons. Our enhanced-color cutout is centered on a brownish-colored inter-dune area.

Each winter the carbon dioxide in the Martian atmosphere falls as snow, mantling the surface in the latitudes above 60 degrees with a clear coat of dry ice. When spring arrives the sunlight passes through the mantle to heat the ground below, which in turn causes the base of the dry ice mantle to sublimate into gas. When the pressure builds enough, the gas breaks through the mantle at its weak points, spewing out and bringing with it dust from below, which stains the mantle with the dark spots.
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The cool image to the right, cropped, reduced, and enhanced to post here, was taken on February 22, 2024 by the high resolution camera on Mars Reconnaissance Orbiter (MRO). It gives us another example the many-layered geological history of Mars, seen in numerous locations across the entire Martian surface.

This example shows many thin layers, going downhill about 450 feet from the mesa near the bottom of the picture to the low point near the picture’s top. At this resolution there appear to be roughly two dozen prominent layers in that descent, but a closer look suggests many more layers within those large layers. Like the terrain that Curiosity is traversing on Mount Sharp, the closer one gets the more layers one sees. And each layer signifies a different geological event, possibly even marking the annual seasons, each either adding or removing a layer of dust or ice, or placing down a new layer of lava.
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Cool image time! The picture to the right, rotated, cropped, reducedl, and enhanced to post here, was taken on February 24, 2024 by the high resolution camera on Mars Reconnaissance Orbiter (MRO). Dubbed a “terrain sample” by the camera team, it was likely taken not as part of any specific research project but to fill a gap in the camera’s schedule so as to maintain that camera’s proper temperature. When they have to do this, they try to pick interesting targets, though there is no guarantee the result will be very interesting.

In this case the camera team already knew this location would have intriguing geology, based on an earlier terrain sample taken a year ago only eight miles to the south. The landscape here is a flat plateaus surrounding flat depressions, some of which appear connected by drainage channels. Today’s picture shows one flat depression with a short tail-like channel flowing into it.

Note the pockmarked surface. The many holes could be impact craters, but they also could be holes caused when the near-surface ice at this location sublimated into gas and bubbled upward to escape. Now all we see is dry bedrock, the flat ground riddled with holes.
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Cool image time! The picture to the right, rotated, cropped, and reduced to post here, was taken on December 21, 2023 by the high resolution camera on Mars Reconnaissance Orbiter (MRO). It shows what the scientists label as an “inlet to a paleolake.” I have used this context camera lower resolution image taken January 14, 2023 to fill in the blank central strip caused by a failed filter on the high resolution camera.

The elevation difference between the plateau on the lower left and the lake bottom on the upper right is about 700 feet. The inlet channel floor is about 200 feet below the plateau. We know it is ancient because of the number of small craters within it as well as on the lakebed below. It has been a very long time since any water or ice flowed down this channel to drain into the lake to the north.

While a lot of analysis of orbital data has found numerous examples of paleolakes in the dry equatoral regions of Mars (see here, here, here, here, and here , this particular example is so obvious not much analysis is needed, as shown in the overview map below.
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