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An Ancient Meteorite Is The First Chemical Evidence of Volcanic Convection on Mars

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For many years, we thought Mars was dead. A dusty, dry, barren planet, where nothing moves but the howling wind. Recently, however, pieces of evidence have started to emerge, hinting that Mars is both volcanically and geologically active.


Well, the idea of a volcanically active Mars just got a little more real. A meteorite that formed deep within the belly of Mars has just provided the first solid chemical proof of magma convection within the Martian mantle, scientists say. 

Crystals of olivine in the Tissint meteorite that fell to Earth in 2011 could only have formed in changing temperatures as it was rapidly swirled about in magma convection currents – showing that the planet was volcanically active when the crystals formed around 574 to 582 million years ago – and it could still be intermittently so today.

“There was no previous evidence of convection on Mars, but the question ‘Is Mars a still volcanically active planet?’ was previously investigated using different methods,” explained planetary geologist Nicola Mari of the University of Glasgow to ScienceAlert.

“However, this is the first study that proves activity in the Mars interior from a purely chemical point of view, on real Martian samples.”

Olivine, a magnesium iron silicate, isn’t rare. It crystallises from cooling magma, and it’s very common in Earth’s mantle; in fact, the olivine group dominates Earth’s mantle, usually as part of a rock mass. On Earth’s surface, it’s found in igneous rock.


It’s fairly common in meteorites. And olivine is also fairly common on Mars. In fact, the presence of olivine on the surface of Mars has previously been taken as evidence of the planet’s dryness, since the mineral weathers rapidly in the presence of water.

But when Mari and his team started studying the olivine crystals in the Tissint meteorite to try to understand the magma chamber where it formed, they noticed something strange. The crystals had irregularly spaced phosphorus-rich bands.

We know of this phenomenon on Earth – it’s a process called solute trapping. But it was a surprise to find it on Mars.

magma olivine(Mari et al., Meteoritics & Planetary Science, 2020)

“This occurs when the rate of crystal growth exceeds the rate at which phosphorus can diffuse through the melt, thus the phosphorus is obliged to enter the crystal structure instead of ‘swimming’ in the liquid magma,” Mari said.

“In the magma chamber that generated the lava that I studied, the convection was so vigorous that the olivines were moved from the bottom of the chamber (hotter) to the top (cooler) very rapidly – to be precise, this likely generated cooling rates of 15-30 degrees Celsius per hour for the olivines.”


The larger of the olivine crystals were also revealing. Traces of nickel and cobalt are in agreement with previous findings that they originated from deep under the Martian crust, a depth of 40 to 80 kilometres (25 to 50 miles).

This supplied the pressure at which they formed; along with the equilibration temperature of olivine, the team could now perform thermodynamic calculations to discover the temperature in the mantle at which the crystals formed.

They found that the Martian mantle probably had a temperature of around 1,560 degrees Celsius in the Martian Late Amazonian period when the olivine formed. This is very close to the ambient mantle temperature of Earth of 1,650 degrees Celsius during the Archean Eon, 4 to 2.5 billion years ago.

That doesn’t mean Mars is just like an early Earth. But it does mean that Mars could have retained quite a bit of heat under its mantle; it’s thought that, because it lacks the plate tectonics that help to dissipate heat on Earth, Mars may cool more slowly.

“I really think that Mars could be a still volcanically active world today, and these new results point toward this,” Mari told ScienceAlert.

“We may not see a volcanic eruption on Mars for the next 5 million years, but this doesn’t mean that the planet is inactive. It could just mean that the timing between eruptions between Mars and Earth is different, and instead of seeing one or more eruptions per day (as on Earth) we could see a Martian eruption every n-millions of years.”

We’ll need more research to confidently say this hypothesis checks out. But these results also mean that previous interpretations of the planet’s dryness based on surface olivine may need to be revisited. (Although let us be clear, Mars is still extremely dry.)

The ongoing NASA InSight mission that recently found evidence of Marsquakes, measures – among other things – the heat flux from the Martian crust. If Mars is still volcanically active, we may know more about it really soon.

The research has been published in Meteoritics & Planetary Science.


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It Hasn’t Rained on Mars For a Long Time, But These Sand Dunes Look Like Raindrops

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Mars is well-known for being a dry and arid place, where dusty red sand dunes are prevalent and water exists almost entirely in the form of ice and permafrost.

An upside to this, however, is the fact that these conditions are the reason why Mars’ many surface features are so well preserved. And as missions like the Mars Reconnaissance Orbiter (MRO) have shown, this allows for some pretty interesting finds.


Consider the picture recently taken by Curiosity’s High Resolution Imaging Science Experiment (HiRISE) instrument while orbiting above the Copernicus Crater on Mars.

This image showed raindrop-like features that are actually signs of sand dunes that are rich in olivine. These same types of dunes exist on Earth but are very rare since this mineral weathers quickly and turns to clay in wet environments.

Olivine is used by geologists to describe a group of rock-forming minerals that are typically found in igneous rocks. This mineral is so-named because of its green color, which is due to its chemical composition – silicate-based (SiO4) and bonded with either Magnesium or Iron (Mg2SiO4; Fe2SiO4).

On Earth, it is generally found in dark-colored igneous rocks and is one of the first minerals to crystalize during the slow cooling of magma.

ESP 031221 1315 RED.browse 768x1080(NASA/JPL/University of Arizona)

However, it is a rare thing to find so many sand dunes that are rich in olivine deposits on Earth, as was imaged by the MRO. The reason for this is because olivine is one of the weaker common minerals on Earth’s surface and quickly turns into a combination of clay minerals, iron oxides and ferrihydrites (iddingsite) in the presence of water.

However, deposits of olivine have been found in meteorites, on the Moon, Mars, and even on the asteroid Itokawa (which was visited by the Japanese Hayabusa mission in 2005). Since asteroids and meteorites are essentially leftover material from the formation of the Solar System, this would suggest that olivine minerals were present at the time.


In addition, the presence of iddingsite on Mars and the Moon is a strong indication that liquid water once existed there. By studying deposits of olivine and it’s by-products, scientists might be able to determine when Mars made the transition from having liquid water on its surface to the very dry place that it is today.

In the meantime, the discovery of these many dunes on Mars is a testament to how well certain features have been preserved over time. If there was indeed wind and water erosion on Mars as their is on Earth, the Copernicus Crater would have become a clay-rich region very quickly.

As always, Mars dazzles us with unique combination of similarities and differences to Earth!

This article was originally published by Universe Today. Read the original article.


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This Mysterious Feature on Mars Might Finally Have an Explanation

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A strange feature on the surface of Mars has kept scientists guessing about its origin. It’s a surface deposit of a mineral which is more common in the interiors of planets. A new study shows that this interior mineral was probably brought to the surface by an ancient explosive volcano.


Nili Fossae is located in the Syrtis Major region on Mars. It’s near the Isidis Planitia, a huge plain inside an impact basin on Mars.

Nili Fossae is interesting because of the mineral deposits in the area, and what those deposits tell us about Mars. Specifically, it contains a large deposit of the mineral olivine, which is typically found in the interior of planets.

The question this study tried to answer is how did the olivine find its way to the surface?


The Olivine Within

Olivine itself is not rare or remarkable. In fact, it’s the primary component of the Earth’s mantle. It’s not rare on Mars either. The word olivine actually covers a group of minerals that are very similar. For one, they’re all greenish, which explains the “olive” in olivine.

They’re found in igneous rocks, which are basically cooled, solidified lava.

With that in mind, the explanation may seem rather obvious. Of course this deposit of olivine came from a volcano. How else could it have gotten to the surface from the mantle?


But science is all about the details. When, exactly, in Martian history was this olivine deposited by a volcano? In what context did it happen, and was it part of larger events that shaped Mars? What type of volcanic event created it?

Those questions, and the size of the olivine deposit in question, are what make this study interesting.

The study is from Brown University, in Providence, Rhode Island. The authors are grad students Christopher Kremer and Michael Bramble, and John Mustard, from Brown University’s Department of Earth, Environmental and Planetary Sciences.

The paper is called A widespread olivine-rich ash deposit on Mars and is published in the journal Geology.

Olivine grains from Hawaiin lava (Wilson44691/Wikimedia/CC0)Olivine grains from Hawaiin lava (Wilson44691/Wikimedia/CC0)

Mineral Nerds

There exists a certain type of person who is extremely interested in minerals. Far from being an unusual, anti-social obsession pursued in a distant corner of a university campus, the study of minerals is a building block of planetary science.

Without our understanding of minerals, we have no hope of piecing together the history of Earth. We would also be ignorant about all the other planets in our Solar System, and about asteroids and meteorites, too.


When it comes to Mars, the importance of understanding minerals cannot be over-emphasized. The types of minerals we see, where we see them, and how they got there, are all clues to understanding Mars.

And when scientists spot an unusual deposit of minerals there, they want to know how it got there.

Martian Jigsaw Puzzle

Mars is a jigsaw puzzle. We’re nowhere near completing it, but piece by piece we’re beginning to understand the history of that planet. Specifically, we want to know if it was ever habitable, and if it might yet be home to some microscopic life.

Those questions can’t really be answered directly: they have to be revealed by completing the Martian jigsaw puzzle.

This unusual deposit of olivine is one of the pieces of the puzzle.

This olivine deposit was first discovered in 2003 and presented in a paper in Science. That paper announced the discovery of a 30,000 square kilometer area with about 30 percent olivine.

The area is notable for its geological formation. It’s an area of what are called grabens. Grabens are valleys with sharp escarpments on both sides, caused by the downward displacement of blocks of land.


In that initial paper, the authors said that “post-impact faulting of this area has exposed subsurface layers rich in olivine.” Over the years, other researchers have come up with other possible explanations.

Some have suggested effusive lava flow. Others have suggested that the olivine was dredged up by a massive impact. Perhaps the same impact that created the enormous Isidis Basin where the deposit is located.

This new study says that the olivine was deposited by explosive volcanism.

Grabens are valleys with sharp escarpments on both sides. (Horst_graben/US Geological Survey)Grabens are valleys with sharp escarpments on both sides. (Horst_graben/US Geological Survey)

Volcanic Explosions

For most of us, a volcano is a volcano. But there are different types. One type is called explosive volcanism.

“This is one of the most tangible pieces of evidence yet for the idea that explosive volcanism was more common on early Mars,” said Christopher Kremer, a graduate student at Brown University who led the work.

Explosive volcanism happens when magma contains dissolved gases like water vapour. That dissolved gas creates a lot of pressure in the magma, and when the overhead rock can’t withstand the pressure, it explodes. That explosion sends a massive amount of fiery ash and lava into the air.

Since explosive volcanism requires water vapour, scientists think that this type of volcanic explosion happened early in Mars’ life, when there was more water around.

Over time, Mars lost its water, and volcanic activity would have been less explosive. It would have been replaced by what’s called effusive volcanism, which is gentler and causes lava to flow across the surface, rather than explode into the air.

According to Kremer, there’s lots of evidence for this effusive volcanic phase in Martian history, whereas evidence for the earlier, explosive phase is not so easily discovered, especially with orbital instruments.

“Understanding how important explosive volcanism was on early Mars is ultimately important for understanding the water budget in Martian magma, groundwater abundance and the thickness of the atmosphere,” said Kremer.

Nili Fossae (NASA/Christopher Kremer/Brown)Nili Fossae (NASA/Christopher Kremer/Brown)

Orbital Eyes on Mars

For now, all scientists have to study this deposit with are orbital instruments. Kremer and his colleagues used high-resolution images from NASA’s Mars Reconnaissance Orbiter (MRO) to study the geology of the area in detail. As Kremer said in a press release, they took a different tack when studying the area.

“This work departed methodologically from what other folks have done by looking at the physical shape of the terrains that are composed of this bedrock,” Kremer said.

“What’s the geometry, the thickness and orientation of the layers that make it up. We found that the explosive volcanism and ashfall explanation ticks all the right boxes, while all of the alternative ideas for what this deposit might be disagree in several important respects with what we observe from orbit.”

One of the things that differentiate this deposit from other effusive lava flow areas is the distribution of the lava itself. While an effusive flow would basically spread liquid rock over the surface, where it would pool in low-lying areas, this deposit is in long continuous layers over valleys, craters, hills, and other features.

According to Kremer, that is much more consistent with ash settling from an explosive eruption than it is with lava flow.

The continuous deposit also rules out the impact scenario too. The Isidis impact that created the Isidis Basin cannot have created such a uniform layer of ash. Also, the ash is deposited on top of some of the features created by the Isidis impact.

The condition of the olivine itself also rules out the impact scenario. The olivine shows evidence of sustained and widespread contact with water. The olivine was altered by that contact, much more than other olivine on Mars.

The authors say that only makes sense of this olivine was from ash fall, since is ash is much more porous than other rocks, and would have allowed the water to contact the olivine.

Can a Rover Solve the Puzzle?

It’s difficult to be absolutely certain about something that you can only study from orbit. Luckily, a rover is headed that way.

In 2020, NASA’s Mars 2020 rover will be launched on its way to Mars. Its landing site? The Jezero Crater, which is inside the olivine deposit. There are exposed areas of olivine accessible to the rover, and it seems certain that the 2020 rover will study it.

“What’s exciting is that we’ll see very soon if I’m right or wrong,” Kremer said. “So that’s a little nerve wracking, but if it’s not an ashfall, it’s probably going to be something much stranger. That’s just as fun if not more so.”

“One of Mars 2020’s top 10 discoveries is going to be figuring out what this olivine-bearing unit is,” said Mustard, Kremer’s advisor. “That’s something people will be writing and talking about for a long time.”

Once we know how this olivine puzzle piece fits in, we’ll know something about the era of explosive volcanism on Mars. By extension, we’ll know something about ancient Martian water. By extension from that, we’ll know something about the ancient Martian atmosphere.

From there, we’ll know something about Martian habitability.

Aren’t puzzles fun?

This article was originally published by Universe Today. Read the original article.


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