By studying the chemical elements on Mars today — including carbon and oxygen — scientists can work backwards to piece together the history of a planet that once had the conditions necessary to support life.
Weaving this story, element by element, from roughly 140 million miles (225 million kilometers) away is a painstaking process. But scientists aren’t the type to be easily deterred. Orbiters and rovers at Mars have confirmed that the planet once had liquid water, thanks to clues that include dry riverbeds, ancient shorelines, and salty surface chemistry. Using NASA’s Curiosity Rover, scientists have found evidence for long-lived lakes. They’ve also dug up organic compounds, or life’s chemical building blocks. The combination of liquid water and organic compounds compels scientists to keep searching Mars for signs of past — or present — life.
Despite the tantalizing evidence found so far, scientists’ understanding of Martian history is still unfolding, with several major questions open for debate. For one, was the ancient Martian atmosphere thick enough to keep the planet warm, and thus wet, for the amount of time necessary to sprout and nurture life? And the organic compounds: are they signs of life — or of chemistry that happens when Martian rocks interact with water and sunlight?
In a recent Nature Astronomy report on a multi-year experiment conducted in the chemistry lab inside Curiosity’s belly, called Sample Analysis at Mars (SAM), a team of scientists offers some insights to help answer these questions. The team found that certain minerals in rocks at Gale Crater may have formed in an ice-covered lake. These minerals may have formed during a cold stage sandwiched between warmer periods, or after Mars lost most of its atmosphere and began to turn permanently cold.
Gale is a crater the size of Connecticut and Rhode Island combined. It was selected as Curiosity’s 2012 landing site because it had signs of past water, including clay minerals that might help trap and preserve ancient organic molecules. Indeed, while exploring the base of a mountain in the center of the crater, called Mount Sharp, Curiosity found a layer of sediments 1,000 feet (304 meters) thick that was deposited as mud in ancient lakes. To form that much sediment an incredible amount of water would have flowed down into those lakes for millions to tens of millions of warm and humid years, some scientists say. But some geological features in the crater also hint at a past that included cold, icy conditions.
“At some point, Mars’ surface environment must have experienced a transition from being warm and humid to being cold and dry, as it is now, but exactly when and how that occurred is still a mystery,” says Heather Franz, a NASA geochemist based at NASA’s Goddard Space Flight Center in Greenbelt, Maryland.
Franz, who led the SAM study, notes that factors such as changes in Mars’ obliquity and the amount of volcanic activity could have caused the Martian climate to alternate between warm and cold over time. This idea is supported by chemical and mineralogical changes in Martian rocks showing that some layers formed in colder environments and others formed in warmer ones.
In any case, says Franz, the array of data collected by Curiosity so far suggests that the team is seeing evidence for Martian climate change recorded in rocks.
Carbon and oxygen star in the Martian climate story
Franz’s team found evidence for a cold ancient environment after the SAM lab extracted the gases carbon dioxide, or CO2, and oxygen from 13 dust and rock samples. Curiosity collected these samples over the course of five Earth years.
CO2 is a molecule of one carbon atom bonded with two oxygen atoms, with carbon serving as a key witness in the case of the mysterious Martian climate. In fact, this simple yet versatile element is as critical as water in the search for life elsewhere. On Earth, carbon flows continuously through the air, water, and surface in a well-understood cycle that hinges on life. For example, plants absorb carbon from the atmosphere in the form of CO2. In return, they produce oxygen, which humans and most other life forms use for respiration in a process that ends with the release of carbon back into the air, again via CO2, or into the Earth’s crust as life forms die and are buried.
Scientists are finding there’s also a carbon cycle on Mars and they’re working to understand it. With little water or abundant surface life on the Red Planet for at least the past 3 billion years, the carbon cycle is much different than Earth’s.
“Nevertheless, the carbon cycling is still happening and is still important because it’s not only helping reveal information about Mars’ ancient climate,” says Paul Mahaffy, principal investigator on SAM and director of the Solar System Exploration Division at NASA Goddard. “It’s also showing us that Mars is a dynamic planet that’s circulating elements that are the buildings blocks of life as we know it.”
The gases build a case for a chilly period
After Curiosity fed rock and dust samples into SAM, the lab heated each one to nearly 1,650 degrees Fahrenheit (900 degrees Celsius) to liberate the gases inside. By looking at the oven temperatures that released the CO2 and oxygen, scientists could tell what kind of minerals the gases were coming from. This type of information helps them understand how carbon is cycling on Mars.
Various studies have suggested that Mars’ ancient atmosphere, containing mostly CO2, may have been thicker than Earth’s is today. Most of it has been lost to space, but some may be stored in rocks at the planet’s surface, particularly in the form of carbonates, which are minerals made of carbon and oxygen. On Earth, carbonates are produced when CO2 from the air is absorbed in the oceans and other bodies of water and then mineralized into rocks. Scientists think the same process happened on Mars and that it could help explain what happened to some of the Martian atmosphere.
Yet, missions to Mars haven’t found enough carbonates in the surface to support a thick atmosphere.
Nonetheless, the few carbonates that SAM did detect revealed something interesting about the Martian climate through the isotopes of carbon and oxygen stored in them. Isotopes are versions of each element that have different masses. Because different chemical processes, from rock formation to biological activity, use these isotopes in different proportions, the ratios of heavy to light isotopes in a rock provide scientists with clues to how the rock formed.
In some of the carbonates SAM found, scientists noticed that the oxygen isotopes were lighter than those in the Martian atmosphere. This suggests that the carbonates did not form long ago simply from atmospheric CO2 absorbed into a lake. If they had, the oxygen isotopes in the rocks would have been slightly heavier than the ones in the air.
While it’s possible that the carbonates formed very early in Mars’ history, when the atmospheric composition was a bit different than it is today, Franz and her colleagues suggest that the carbonates more likely formed in a freezing lake. In this scenario, the ice could have sucked up heavy oxygen isotopes and left the lightest ones to form carbonates later. Other Curiosity scientists have also presented evidence suggesting that ice-covered lakes could have existed in Gale Crater.
So where is all the carbon?
The low abundance of carbonates on Mars is puzzling, scientists say. If there aren’t many of these minerals at Gale Crater, perhaps the early atmosphere was thinner than predicted. Or maybe something else is storing the missing atmospheric carbon.
Based on their analysis, Franz and her colleagues suggest that some carbon could be sequestered in other minerals, such as oxalates, which store carbon and oxygen in a different structure than carbonates. Their hypothesis is based on the temperatures at which CO2 was released from some samples inside SAM — too low for carbonates, but just right for oxalates — and on the different carbon and oxygen isotope ratios than the scientists saw in the carbonates.
Oxalates are the most common type of organic mineral produced by plants on Earth. But oxalates also can be produced without biology. One way is through the interaction of atmospheric CO2 with surface minerals, water, and sunlight, in a process known as abiotic photosynthesis. This type of chemistry is hard to find on Earth because there’s abundant life here, but Franz’s team hopes to create abiotic photosynthesis in the lab to figure out if it actually could be responsible for the carbon chemistry they’re seeing in Gale Crater.
On Earth, abiotic photosynthesis may have paved the way for photosynthesis among some of the first microscopic life forms, which is why finding it on other planets interests astrobiologists.
Even if it turns out that abiotic photosynthesis locked some carbon from the atmosphere into rocks at Gale Crater, Franz and her colleagues would like to study soil and dust from different parts of Mars to understand if their results from Gale Crater reflect a global picture. They may one day get a chance to do so. NASA’s Perseverance Mars rover, due to launch to Mars between July and August 2020, plans to pack up samples in Jezero Crater for possible return to labs on Earth.
- “Indigenous and exogenous organics and surface–atmosphere cycling inferred from carbon and oxygen isotopes at Gale crater” by H. B. Franz, P. R. Mahaffy, C. R. Webster, G. J. Flesch, E. Raaen, C. Freissinet, S. K. Atreya, C. H. House, A. C. McAdam, C. A. Knudson, P. D. Archer Jr., J. C. Stern, A. Steele, B. Sutter, J. L. Eigenbrode, D. P. Glavin, J. M. T. Lewis, C. A. Malespin, M. Millan, D. W. Ming, R. Navarro-González and R. E. Summons, 27 January 2020, Nature Astronomy.
- “Deposition, exhumation, and paleoclimate of an ancient lake deposit, Gale crater, Mars” by J. P. Grotzinger, S. Gupta, M. C. Malin, D. M. Rubin, J. Schieber, K. Siebach, D. Y. Sumner, K. M. Stack, A. R. Vasavada, R. E. Arvidson, F. Calef III, L. Edgar, W. F. Fischer, J. A. Grant, J. Griffes, L. C. Kah, M. P. Lamb, K. W. Lewis, N. Mangold, M. E. Minitti, M. Palucis, M. Rice, R. M. E. Williams, R. A. Yingst, D. Blake, D. Blaney, P. Conrad, J. Crisp, W. E. Dietrich, G. Dromart, K. S. Edgett, R. C. Ewing, R. Gellert, J. A. Hurowitz, G. Kocurek, P. Mahaffy, M. J. McBride, S. M. McLennan, M. Mischna, D. Ming, R. Milliken, H. Newsom, D. Oehler, T. J. Parker, D. Vaniman, R. C. Wiens and S. A. Wilson, 9 October 2015, Science.
- “Chemical alteration of fine-grained sedimentary rocks at Gale crater” by N. Mangolda, E. Dehouck, C. Fedo, O. Forni, C. Achilles, T. Bristow, R. T. Downs, J. Frydenvang, O. Gasnault, J. L’Haridon, L. Le Deit, S. Maurice, S. M. McLennan, P.-Y. Meslin, S. Morrison, H. E. Newsom, E. Rampe, W. Rapin, F. Rivera-Hernandez, M. Salvatore and R. C. Wiens, 17 November 2018, Icarus.
- “Subsistence of ice-covered lakes during the Hesperian at Gale crater, Mars” by Alexandre M. Kling, Robert M. Haberle, Christopher P. McKay, Thomas F. Bristow and Frances Rivera-Hernández, 9 November 2019, Icarus.