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Headshot of Emily Lakdawalla

GSA 2014: The puzzle of Gale crater's basaltic sedimentary rocks

Posted by Emily Lakdawalla

23-10-2014 19:31 CDT

Topics: mineralogy and petrology, geology, explaining science, Mars, Curiosity (Mars Science Laboratory)

I've just come back from a quick trip to Vancouver to attend two days of the annual Geological Society of America (GSA) conference. I went to it specifically to hear the latest Curiosity results, and saw the first indications of how Curiosity is going to be changing our view of Martian geology. It's a subtle but important shift in how we imagine ancient Mars. It relates to water, of course.

There are two main unifying points to the Curiosity results I saw at GSA. First: Every rock that Curiosity has seen is sedimentary. Second: nearly all of those sedimentary rocks have the bulk composition of an igneous rock called basalt. If you're a geologist, those two statements almost seem contradictory. Sedimentary rocks say "Mars was wet." Basaltic composition says "Mars was dry." Let me explain why, and then I'll try to explain where we go from here.

At GSA, several presenters described a diverse array of sedimentary rocks seen by Curiosity. Linda Kah, presenting on behalf of Becky Williams, talked about seeing "a series of spectacular sedimentary deposits" including "interbedded and very well lithified conglomerates, fluvial sands, sheet sands, and other, varied sedimentary environments." Conglomerates are made of large rock chunks, which need fast-moving water to form. "Fluvial" means a river environment -- sediments laid down by water running in channels, building up and tearing down sand bars. Sand sheets form in windy environments. Here are a couple of examples of different types of sedimentary rocks that showed up over and over in talks, some of the greatest hits of Curiosity's Mars Hand Lens Imager (MAHLI), in order of largest grain size to smallest:

Altar Mountain


Altar Mountain
Curiosity investigated a spot called Altar Mountain at the Darwin waypoint on sol 394. This MAHLI image, taken of a mostly shadowed spot on the outcrop, shows that Bardin Bluffs is a poorly sorted pebble conglomerate. Most of the grains are subangular, with gravel measuring 4 to 10 millimeters across. The poor sorting and disorganization suggests it was deposited rapidly.
Bardin Bluffs


Bardin Bluffs
Curiosity investigated a spot called Bardin Bluffs at the Darwin waypoint on sol 394. This MAHLI image, taken of a shadowed spot on the outcrop, shows that Bardin Bluffs is a pebbly sandstone. It is gravel-rich, with a sandy matrix and granule- to pebble-sized clasts that are subrounded to rounded in shape. The way that the grains touch each other indicates they were deposited by water. Grains are lumpy and pock-marked, indicating that they collided with each other as they were being transported.
MAHLI view of


MAHLI view of "Gillespie Lake," a coarse sandstone on the edge of Yellowknife Bay, sol 132
Curiosity held its MAHLI camera within 3 centimeters of a ledge on sol 132 to examine its grains up close. The investigation revealed the rock to be a coarse sandstone, made up of cemented grains of a range of sizes. The biggest grains at lower left are about 2 millimeters long, which is larger than sand; technically, they are classified as "granules." The whole view is about 4.3 centimeters wide; at full resolution, it is about 26.1 microns per pixel.
Aillik, Curiosity sol 322


Aillik, Curiosity sol 322
Curiosity imaged a target named Aillik on the Shaler outcrop on sol 322. There are no visible pebbles; Shaler is a very well-sorted sandstone.
Wernecke, Curiosity sol 169


Wernecke, Curiosity sol 169
Curiosity brushed and then imaged a target called Wernecke with its MAHLI camera on sol 169, as the rover was preparing to drill for the first time. MAHLI was able to pose within only 1 centimeter of the surface of Wernecke, and so achieved its highest resolution of about 10 microns per pixel. MAHLI cannot resolve individual grains within the rock, so the grain size is smaller than fine sand. The rock does have small nodules, informally called "measles" by the team. Some team members think they were once gas bubbles within the wet sediment, some (but not all) of which later filled with minerals. You can also see that the brush has scratched the surface, indicating that the rock is soft.

Grain size tells you something about the energy of the fluid that was transporting the sediment grains. But MAHLI and Mastcam can also see larger-scale sedimentary structures in the way that the rocks are put together. In separate talks, Dave Rubin and Melissa Rice identified a diverse array of geologic settings in which these sedimentary rocks were deposited. Rubin pointed out aeolian (windblown) sands at Shaler, but said there were also examples of compound cross bedding, which is what you get in fluvial (river) settings.

Shaler outcrop, Curiosity sol 316


Shaler outcrop, Curiosity sol 316
Shaler is an outcrop of cross-bedded, light-toned, well-sorted sands, located above the Yellowknife Bay area. It likely represents a fluvial (river) environment, with minor reworking of the sediments by wind when it dried out.

Rubin also spent quite a while talking about the south-dipping beds at the Kimberley, as did Melissa Rice. She talked about how they these stacks of south-dipping bedded sandstones climbed upward, up elevation, toward the south. Really the only way to do that is if they represent the toe of what she called an "aggradational system" -- essentially, a river delta, where a faster-moving body of water, which can carry larger sediment grains, meets a slow-moving or still body of water. The bigger sediment gets dropped, building out a deposit of sands. It's a pretty big deposit, too; the "striated unit" at the Kimberley that represents these south-dipping beds covers an area of two square kilometers.

The north edge of Kimberley, Curiosity sol 580

NASA / JPL / MSSS / Doug Ellison

The north edge of Kimberley, Curiosity sol 580
While parked about 4 meters from the north edge of Kimberley, Curiosity took almost 250 images of the outcrop with the higher-resolution Mastcam. The rock layers are tilted gently away from the rover. In places, windblown sand has piled up against the rock. Small cascades of loose material disturb the drifted sand in places.

Water interacted with all of these rocks more than once. Many of these rocks -- mudstones, siltstones, and sandstones -- contain fractures with mineral fills, evidence for mineral-rich water fracturing the existing rocks and precipitating out mineral deposits -- and yet, despite all that water running around, these rocks still have a basaltic composition.

So I guess it's a good time to talk about basalt. Here, have some basalt.


Imperial College Rock Library

Basalt is one of the most common types of rock on planetary surfaces. It is a dark-colored, igneous rock that usually contains the minerals olivine, pyroxene, and feldspar. This basalt came from Mauna Loa, Hawaii. To learn much more about this rock, visit the Imperial College Rock Library.

All the terrestrial planets -- Earth, Mars, Venus, Mercury, and the honorary terrestrial planets the Moon, Io, and Vesta -- have vast regions that are covered with basalt. Basalt is an igneous rock, meaning it solidified from a melt, so is made of mineral crystals that are intergrown with each other. Basalt is very dark in color, and typically has three main minerals: green olivine and black pyroxene (both of which are rich in iron and magnesium), plus dark gray feldspar (which bears calcium and sodium). Relative to many other interesting kinds of rocks that you find on Earth, basalt is high in iron, magnesium, and calcium, and low in silicon, aluminum, and potassium.

Basalt is common in the solar system, but it doesn't get along with water very well. Water chemically attacks the crystal structure of olivine, pyroxene, and feldspar. It weathers those primary igneous minerals into other minerals that have tons of water stuffed into their crystal structures, such as clay minerals. Water oxidizes the abundant iron and in basalt, turning rocks from dark gray or green to red. If the water can flow away from the rock it's attacking, it can leach out and remove iron, magnesium, and calcium, leaving behind a rock that's relatively enriched in silicon and aluminum.

Chemical weathering of basalt happens fast, in geologic terms. It goes even faster if you bust up a piece of basalt into lots of tiny little pieces, making a large surface area for water to work on. So if you take a basalt, fracture it up, and then get it wet -- which is what you need to do to make a sedimentary rock out of basalt -- you would expect the resulting rock not to look very much like basalt.

Sedimentary rocks that have a basaltic mineral composition are not common on Earth. If you start with a basalt, and break it up due to physical or chemical weathering, and then you transport it somewhere in a river and deposit it in a lake or ocean, water will act on the basaltic rock fragments, carry away their iron and magnesium, and leave behind a much more silicon- and aluminum-rich sedimentary rock. Instead, it would be made of clays.

But Curiosity's rocks have a basaltic composition -- rich in iron and magnesium, less so in aluminum and silicon. They do have high potassium for basaltic rocks, which has had the scientists scratching their heads. And there is at least one rock that does contain a fair amount of clay, the one they drilled into at Yellowknife Bay. But it's still pretty puzzling that so many of Curiosity's rocks are sedimentary, and yet they're basaltic in composition. In fact, there's only one rock that members of the Curiosity team have specifically identified as being a basalt -- not a sedimentary rock of basalt composition, but an actual basaltic lava rock. They've even written a paper about it and published it in Science: Jake Matijevic, the Martian mugearite. It's the first rock they examined with the robotic arm:

The rock

NASA / JPL / MSSS / Damia Bouic

The rock "Jake Matijevic" in context
A montage of images of Jake Matijevic on Mars, from a wide angle view to a MAHLI closeup.

Except, it turns out, Jake Matijevic is not an igneous rock. Oops!

In one of his three GSA talks, Ken Edgett dropped the surprising statement that Jake Matijevic is actually a sedimentary rock. Ken (who is the principal investigator on the MAHLI camera) explained that over the course of the primary mission, as Curiosity examined a wide variety of rocks up close, he and the MAHLI team began to notice similarities among certain classes of rocks. Rock localities that really puzzled them early on in the mission started to become comprehensible as they saw more and more examples of Gale crater rocks and the team -- as Ken put it -- "calibrated our brains" to be able to see clearly what the rock types actually were. They saw Jake Matijevic on sol 47. More than an Earth year later, at an outcrop called Bungle Bungle, they saw another rock, Jum Jum, that is a dead ringer for Jake M. And it's not a lava rock, it's a sandstone. (Note: the idea that Jake M is a sedimentary, not igneous, rock is likely not the unanimous opinion of the Curiosity team. But the MAHLI team seems to be convinced.)

In retrospect, Ken said, he could look back at Mastcam images of Jake Matijevic and see pebbles sticking out of it. Now it's obvious, -- to him -- that it's a coarse-grained sandstone. But in the days after they landed, they didn't know that yet, didn't know what to expect to see, and they didn't see the dark, coarse-grained sandstone for what it was.

That realization has led Ken to what can only be described as a crisis in confidence that he (and, by extension, a large fraction of Mars geomorphologists) actually know what they're looking at on Mars. He explained this in another of his talks, focusing on what he can see in Mars Reconnaissance Orbiter Context Camera images. Back in 2000, Ken and Mike Malin published a paper in Science that first claimed that clastic sedimentary rocks were widespread on Mars. For more than a decade, Ken said, they thought they knew what sedimentary rocks on Mars looked like. They were light-toned and layered, and not very resistant to erosion. Opportunity confirmed that, examining the widespread soft-as-butter sulfate-rich bedrock of Meridiani planum.

Portrait of Marquette, Opportunity sol 2088

NASA / JPL-Caltech / Cornell / enhancement by Stuart Atkinson

Rock type contrasts

The bedrock at Opportunity's landing site is light-toned and very easily eroded, so that it forms a flat pavement everywhere, while other erratic igneous rocks like Marquette Island, shown here, perch on the surface, resistant to erosion. Marquette Island is thought to have come from deep beneath Mars' surface, thrown to Meridiani Planum in an impact.

But Curiosity's discovering something different. Curiosity is seeing rocks like those at Point Lake, which, Ken said, were the cause of long-term discussion about what they were. Were they dark-colored, massive sedimentary rocks, or dark-colored, massive volcanic flows? It's the most fundamental description of a rock you can make! And they couldn't figure it out. Not right away. But as time has gone on and Curiosity has seen other occurrences of similar rocks -- such as the Rensslaer rock at the Cooperstown science waypoint -- which are clearly sandstones, the Curiosity team has learned that Martian sedimentary rocks can have the composition of basalt and the color of basalt and be resistant to erosion like basalt and preserve impact craters like basaltic flows do and yet be sedimentary.

Point Lake, Curiosity sol 302

NASA / JPL / MSSS / Emily Lakdawalla

Point Lake, Curiosity sol 302
Point Lake is a dark, massive unit of rock that caps the Shaler sandstone. Members of the Curiosity team have hotly debated whether Point Lake is an igneous rock (a lava flow) or a sedimentary rock (another sandstone, just darker and more erosion-resistant than the Shaler rock).

And that's made Ken go back to the drawing board with his interpretation of orbital photos. It used to be that he thought light-toned rocks that are not resistant to erosion so don't preserve craters well were sedimentary, and dark-toned rocks that did resist erosion and did preserve impact craters were igneous. But now that's been turned upside down. Sedimentary rocks can be dark. They can preserve craters. "Holy crap, what do we do now?" he asked. "I've reached a point where I'm not sure I can tell you on any given crater with a heavily cratered floor whether it's sedimentary or volcanic. I can't tell you. I don't know. If you don't see vents, I don't know." He gave this image as an example -- the more heavily cratered deposits within Elorza crater he would once have thought were lava flows, but he's no longer sure.

Cratered caprock within Elorza crater, Mars


Cratered caprock within Elorza crater, Mars
Elorza is a 45-kilometer crater located a bit east of Valles Marineris. Its floor contains several deposits of material with heavily cratered surfaces, overlying a less-cratered substrate. The heavily cratered material is more resistant to erosion and better able to preserve impact craters than the more easily eroded material that it lies on top of.

This particular talk of Ken's ended with several minutes to spare for questions and comments, and Mars mapper extraordinaire Tim Parker made a striking one. He talked about how the Hesperian age of Mars is distinguished by widespread lava flows -- or so we think. Aloud, he wondered: "Is the Hesperian system really a sedimentary system?" Ken didn't have a good answer to that -- except that he thought it was the right kind of question to be asking.

Curiosity, up there on Mars, is finding absolutely nothing but sedimentary rocks that still have a basaltic composition. It's kind of mind-boggling. It shouldn't be happening (based upon our understanding of Earth geology), so clearly there is something here that is not at all like Earth.

The first and arguably most important difference between Mars' sedimentary rocks as seen by Curiosity and sedimentary rocks investigated by geologists on Earth is their age. The rocks Curiosity is studying are more than 3.5 billion years old, possibly quite a bit older. When Earth was that old, it was a different place. It's very likely that Earth's rocks were predominantly basaltic then, too. Sedimentary rocks are made out of other source rocks. If all you have is basaltic rocks to work with, your sedimentary rocks are going to look more like basaltic rocks. There was an entertaining presentation by Ezat Heydari that showed that you can pretty much explain the entire diversity of rock compositions seen by Curiosity as a simple mix of two endmembers: chunks of broken-up basalt, and a finer-grained material that looks like the ash you'd get from explosive eruptions of very iron- and magnesium-rich komatiites. Nowadays, Earth makes its sedimentary rocks from all kinds of source rocks, most often from much more silicon- and aluminum-rich rocks that have experienced processing through Earth's active rock cycle multiple times. Mars hasn't had that luxury. In a sense, Mars is giving us a chance to look at what sedimentary rocks on Earth might once have looked like, 3.5 or more billion years ago.

But there's still the pesky problem of having rocks made of very fine-grained sediments that, ought not to have a basaltic composition, because the very water that is required to transport, deposit, and lithify sediments into rocks should've also attacked the basaltic minerals and turned them into something else -- a fact that Allan Treiman emphasized in his presentation on Curiosity CheMin results. That's telling us something important, too. For one thing, Allan said, it suggests that the way that Mars turned basaltic lava rock into sediments was not through the action of water -- that Mars broke basalt into basaltic grains through mechanical rather than chemical weathering. And then whatever water-related experience moved those sediments from their point of origin and deposited them into layers in Gale must have happened quite fast, with the water going away very quickly.

All in all, the picture that Curiosity is painting is of a Mars where water played an important role in making nearly every rock that now covers the surface, and yet water's appearances in the geologic record were very, very brief. A Mars that has been mostly incredibly dry except for very rare occasions, concentrated mostly in Mars' earliest history. It makes sense, in a way, because a Mars where water was abundant would not preserve the record of ancient impact craters and landforms that Mars has. Yet it's still a little hard to understand how Mars could have enough water for every rock we see to be sedimentary, yet so little water that we can see a good geologic record of events that happened more than 3.5 billion years ago.

The Mars water pendulum is constantly swinging back and forth. Before the space age, Mars was wet. After Mariner and Viking, it was dry. After Mars Global Surveyor, it was wetter, and the recent orbiters have made it seem wetter yet, with their discoveries of clays and sulfates and carbonates and chlorides. With Curiosity's results, I feel like the "water on Mars" argument is bifurcating; Mars was never wet like Earth, but it is not dry like the Moon. Water is crucially important to Mars' story, and yet Mars is drier than the driest conceivable environment on Earth. In the end, it's just Mars, and it has its own unique story, different from all the other planets.

See other posts from October 2014


Or read more blog entries about: mineralogy and petrology, geology, explaining science, Mars, Curiosity (Mars Science Laboratory)


Brian: 10/24/2014 01:52 CDT

This shows why "ground truth" is the most important element of aerial photo interpretation. So, do these discoveries close the book on the possibility of a "habitable Mars"?

Stephen: 10/24/2014 03:43 CDT

Great article as always, Emily. I guess it just goes to show that geologists still have a-ways to go before they figure Mars out. At the moment every time they think they have, it goes and pulls a new rabbit from out of its bag of tricks! :-)

quayley: 10/24/2014 10:59 CDT

Another excellent and very interesting blog, you should be on the outreach payroll at nasa, to be honest their website updates are sporadic and short at best

Leila: 10/24/2014 11:20 CDT

Fascinating. It must have been hard to summarize such complex news and discussions so concisely, but you did it very well.

David Frankis: 10/24/2014 02:06 CDT

Obvious question: does the atmosphere within which the rock-water interaction takes place make a difference to the outcome or the speed of weathering? Earth's atmosphere (which dissolves in its water) is more oxidising than Mars's.

Ned: 10/24/2014 03:16 CDT

Great blog Emily. I wonder how much data is going to have to be reevaluated now or how many papers will need to be corrected now. Will be interesting to see how everything will be reinterpreted.

Beemer: 10/24/2014 03:29 CDT

I suppose we have to presume water is most often just another mineral in its frozen state? Surely, when frozen and in an non-oxygenating environment things appear stable until something happens, whether pressure or heat based melts it? The image you displayed off Ken showing craters in what was considered laval may have been mineral/water/CO2 based "lava". I'm constantly surprised by what looks like good solid geology from space is nothing more than a friable sand heap. This has to be from out gassing of our life giving "mineral" i.e., water. The glue and the spacer. Hey I may be wrong and if you think so, I'm all ears :)

Fred Thurber: 10/24/2014 03:30 CDT

This is sort of discouraging news. But there is a clay layer at the base of Mt Sharp which indicates a long-term aqueous environment, right? I assume that MSL is currently below that layer and will be working its way up to it.

Dougforworldsexplr: 10/24/2014 03:32 CDT

Very informative blog, Emily. You certainly came through with results after the conference. However I am sorry that the many basaltic rocks even though they are sedimentary could mean Mars have been less habitable than previously thought. How do these rock results co-ordinate with Vallis Marineris or other indications of ancient water on Mars and is it still possible considering all the main evidence that Mars was habitable with the ability to support liquid water and a substantial atmosphere for a considerable period of time?

Margarita: 10/25/2014 09:19 CDT

Such an interesting blog, Emily, thanks so much. I didn't know what "sub angular" meant as I'm innocent of all geology education. For anyone else who is also in this position, this url has as useful Geology 101:

Torbjörn Larsson: 10/26/2014 07:57 CDT

Well, bummer. @Brian: "do these discoveries close the book on the possibility of a "habitable Mars"?" I don't see how they could. First, you would still have the possibility that live emerged in the crust. That is not how life emerged on Earth, our origin seems rooted in the interface between ocean and crust, so it would take longer. (For reasons of geochemistry or simply because the right conditions would not yet have appeared when oceans did here.) If life emerged that way, temporary hydrothermal systems around craters are not conducive enough for emergence of life. Second, the current evidence gives a Mars "never wet like Earth, but ... not dry like the Moon". That still leaves the opportunity for a shortlived ice/water ocean in the northern basin or large craters, with the likely required hot hydrothermal systems for the right chemical conditions. Life emergence is believed to happen on a time scale of 10 000 - 100 000 years, so that seems feasible. And such early life emerging in the crust/water interface would already be pretty much adapted to the initial (and perhaps still) refuge of a wet crustal environment. I'm a layman here, but I think the observations cut down on the likelihood for life. But they also concentrate the future search for life conditions to the crust in a more definitive way. At least they will, if Curiosity can't find anything interesting in the future investigation of Gale clays (if they are still believed to exist).

Thomas P Hopp: 10/26/2014 01:10 CDT

Emily, thanks for a superb report about Mars scientists' confusion over their findings. I think they may be misled by their mission directive to "follow the water" and look for habitable places. I have my doubts that they are looking at wind blown sediments or riverbeds, at all. The paradox of basaltic "sediments" not having been subject to chemical alteration by water goes away if you think what I think--that Mt. Sharp is a stupendous volcano similar to Mt. St. Helens here in Washington State. In the Curiosity images and chemistry data, I see nothing inconsistent with Mt. Sharp being a stratovolcano made of thousands of pyroclastic flows. The "sands" and "conglomerates" then just become different grades of fine or coarse volcanic ash or stones. Their chemistry is correct. Their "windblown" or "flow-deposited" nature become simply the results of red-hot pyroclastic flows. I drew some figures to illustrate my interpretation:

Nikolaus Kuhn: 10/29/2014 09:11 CDT

Dear Emily. thank you for your interesting and a well-written report. I think the conundrum of water and limited weathering has to be placed in a geomorphic context.Fairly coarse-grained Ssedimentary rocks in mountains do often not contain many secondary minerals or other traces of chemical weathering because the sorting during deposition leads to a fractionation by particle size. Products of chemical weathering move generally further than the remnants of physical breakdown. Looking for this finer sediments is therefore essential because they would give a better indication of the degree of weathering. They would also preserve traces of life, if there are any. However, locating these sites is tricky because straight forward analogies between sedimentary forms and deposition processes between Mars and Earth do not work. The reduced Martian gravity affects both flow hydraulics as well as sediment movement, leading e.g. to poorer sorting in a given flow of water. A key question in the search for traces of life as well as the analysis of sedimentary rocks is therefore an improved quantitative analysis and understanding of the Martian geomorphology.

mopterek: 10/30/2014 02:31 CDT

Congratulations Emily for this great report and blog. Writing this is not very original I know. Welcome to the realm of real geology, where no one would have the idea of identifying a rock from scratch using the CIPW norm like in the cited Science paper! I understand that probably not everyone agrees with Ken Edgett; nevertheless I would rather trust him if I were asked. Identifying rocks in very arid regions is not always easy even on Earth; I found myself like an idiot more than once when in front of an outcrop it took me a loooong time to determine whether it is a sandstone or an altered basalt, even after breaking it. New surprises of this kind are probably ahead if Curiosity lives long enough!

eyesoars: 11/10/2014 11:12 CST

@David Frankis The oxygen question is a big one; it certainly changes, substantially, the solubilities of iron and other minerals in water. Are there large reserves of oxygen-free water in Earth's lithosphere? How do they affect the rocks they saturate? We also have little idea what the early Martian atmosphere was like in terms of density and components. Methane? Carbon monoxide? HCN? It seems unlikely that the transporting fluid would be something other than water, although possible. Candidates might be CO2 (requires too much pressure to be liquid), methane/ethane/ammonia/... (too cold/requires too much pressure), &c.

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