What Happened to Early Mars’ Atmosphere? New Study Eliminates One Theory

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A new analysis of the largest known deposit of carbonate minerals on Mars helps limit the range of possible answers about how and why Mars changed from a world with watery environments billions of years ago to the arid Red Planet of today.

A new analysis of the largest known deposit of carbonate minerals on Mars helps limit the range of possible answers about how and why Mars changed from a world with watery environments billions of years ago to the arid Red Planet of today.

The modern Martian atmosphere is too thin for liquid water to persist on the surface. A denser atmosphere on ancient Mars could have kept water from immediately evaporating. It could also have allowed parts of the planet to be warm enough to keep liquid water from freezing. But if the atmosphere was once thicker, what happened to it? The new detective work makes one suspected route for atmospheric loss look less likely.

Christopher Edwards, a former Caltech researcher now with the U.S. Geological Survey in Flagstaff, Arizona, and Bethany Ehlmann of the California Institute of Technology and NASA Jet Propulsion Laboratory reported the findings and analysis in a paper posted online this month by the journal Geology.

Carbon dioxide makes up most of the Martian atmosphere. That gas can be pulled out of the air and sequestered in the ground by chemical reactions with rocks to form carbonate minerals. Years before the series of successful Mars missions in the past two decades, many scientists expected to find large Martian deposits of carbonates holding much of the carbon from the planet's original atmosphere. Instead, these missions have found low concentrations of carbonate distributed widely, but only a few concentrated deposits. By far the largest known carbonate-rich deposit on Mars covers an area at least the size of Delaware, in an area called Nili Fossae. 

"The biggest carbonate deposit on Mars has, at most, twice as much carbon in it as the current Mars atmosphere," said Pasadena-based Ehlmann. "Even if you combined all known carbon reservoirs together, it is still nowhere near enough to sequester the thick atmosphere that has been proposed for the time when there were rivers flowing on the Martian surface."

Their estimate of how much carbon is locked into the Nili Fossae carbonate deposit uses observations from numerous Mars missions, including the Thermal Emission Spectrometer (TES) on NASA's Mars Global Surveyor orbiter, the mineral-mapping Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) and two telescopic cameras on NASA's Mars Reconnaissance Orbiter, and the Thermal Emission Imaging System (THEMIS) on NASA's Mars Odyssey orbiter.

Edwards and Ehlmann compare their tally of sequestered carbon at Nili Fossae to what would be needed to account for an early Mars atmosphere dense enough to sustain surface waters during the period when flowing rivers left their mark by cutting extensive river-valley networks. By their estimate, it would require more than 35 carbonate deposits the size of the one examined at Nili Fossae. They deem it unlikely that so many large deposits have been overlooked in numerous detailed orbiter surveys of the planet. While deposits from an even earlier time in Mars history could be deeper and better hidden, they don't help solve the thin-atmosphere conundrum at the time of valley network formation.

One possible explanation is that Mars did have a much denser atmosphere during its flowing-rivers period, and then lost most of it to outer space from the top of the atmosphere, rather than by sequestration in minerals. NASA's Curiosity Mars rover mission has found evidence for ancient top-of-atmosphere loss, based on the modern Mars atmosphere's ratio of heavier carbon to lighter carbon. Uncertainty remains about how much of that loss occurred before the period of valley formation; much may have happened earlier. NASA's MAVEN orbiter, examining the outer atmosphere of Mars since late 2014, may help reduce that uncertainty.

An alternative explanation, favored by Edwards and Ehlmann, is that the original Martian atmosphere had already lost most of its carbon dioxide by the era of valley formation.

"Maybe the atmosphere wasn't so thick by the time of valley network formation," Edwards said. "Instead of a Mars that was wet and warm, maybe it was cold and wet with an atmosphere that had already thinned. How warm would it need to have been for the valleys to form? Not very. In most locations, you could have had snow and ice instead of rain. You just have to nudge above the freezing point to get water to thaw and flow occasionally, and that doesn't require very much atmosphere." 

Arizona State University, Tempe, provided the TES and THEMIS instruments. The Johns Hopkins University Applied Physics Laboratory, Laurel, Maryland, provided CRISM. JPL, a division of Caltech, manages the Mars Reconnaissance Orbiter and Mars Odyssey project for NASA's Science Mission Directorate, Washington, and managed the Mars Global Surveyor project through its nine years of orbiter operations at Mars. Lockheed Martin Space Systems in Denver built the three orbiters.

For more information about USGS work with the Mars Reconnaissance Orbiter mission, visit the Astrogeology Science Center website

For more information about USGS work, visit the Mars Odyssey mission website.

imaging from Mars
Rocks Here Sequester Some of Mars' Early Atmosphere.This image combines data from two instruments (High Resolution Imaging Science Experiment and Compact Reconnaissance Imaging Spectrometer for Mars) onboard NASA’s Mars Reconnaissance Orbiter to map color-coded composition over the shape of the ground within the Nili Fossae plains region of Mars. Carbonate-rich deposits in this area (green hues) hold some carbon formerly in the atmosphere's carbon dioxide, while sand dunes (brown hues) are composed of olivine-bearing basalt and purple hues are basaltic in composition.
Imaging from Mars
Multiple Instruments Used for Mars Carbon Estimate.The left image of this pair presents data from the Thermal Emission imaging system onboard NASA’s Mars Odyssey orbiter. The color-coding indicates thermal inertia -- the physical property of how quickly a surface material heats up or cools off. Sand, for example (blue hues), cools off quicker after sundown than bedrock (red hues) does.The right images of this pair presents the regional composition from the Compact Reconnaissance Imaging Spectrometer for Mars onboard the NASA’s Mars Reconnaissance Orbiter. Green hues are consistent with carbonate-rich materials, while brown/yellow hues are olivine-bearing sands, and locations with purple hues are basaltic in composition. The gray-scale base map is a mosaic of daytime THEMIS infrared images.