16 October 2013
WASHINGTON, DC—Earth’s most eminent emissary to Mars has just proven that those rare Martian visitors that sometimes drop in on Earth — a.k.a. Martian meteorites — really are from the Red Planet. A key new measurement of Mars’ atmosphere by NASA’s Curiosity rover provides the most definitive evidence yet of the origins of Mars meteorites while at the same time providing a way to rule out Martian origins of other meteorites.
The new measurement is a high-precision count of two forms of argon gas—Argon-36 and Argon-38–accomplished by the Sample Analysis at Mars (SAM) instrument on Curiosity. These lighter and heavier forms, or isotopes, of argon exist naturally throughout the solar system. But on Mars the ratio of light to heavy argon is skewed because a lot of that planet’s original atmosphere was lost to space, with the lighter form of argon being taken away more readily because it rises to the top of the atmosphere more easily and requires less energy to escape. That’s left the Martian atmosphere relatively enriched in the heavier Argon-38.
Years of past analyses by Earth-bound scientists of gas bubbles trapped inside Martian meteorites had already narrowed the Martian argon ratio to between 3.6 and 4.5 (that is 3.6 to 4.5 atoms of Argon-36 to every one Argon-38) with the supposed Martian “atmospheric” value near four. Measurements by NASA’s Viking landers in the 1970’s put the Martian atmospheric ratio in the range of four to seven. The new SAM direct measurement on Mars now pins down the correct argon ratio at 4.2.
“We really nailed it,” said Sushil Atreya of the University of Michigan, Ann Arbor, the lead author of a paper reporting the finding today in Geophysical Research Letters, a journal of the American Geophysical Union. “This direct reading from Mars settles the case with all Martian meteorites,” he said.
One of the reasons scientists have been so interested in the argon ratio in Martian meteorites is that it was – before Curiosity – the best measure of how much atmosphere Mars has lost since the planet’s earlier, wetter, warmer days billions of years ago. Figuring out the planet’s atmospheric loss would enable scientists to better understand how Mars transformed from a once water-rich planet more like our own to the today’s drier, colder and less hospitable world.
Had Mars held onto its entire atmosphere and its original argon, Atreya explained, its ratio of the gas would be the same as that of the Sun and Jupiter. They have so much gravity that isotopes can’t preferentially escape, so their argon ratio – which is 5.5 – represents that of the primordial solar system.
While argon comprises only a tiny fraction of the gases lost to space from Mars, it is special because it’s a noble gas. That means the gas is inert, not reacting with other elements or compounds, and therefore a more straightforward tracer of the history of the Martian atmosphere.
“Other isotopes measured by SAM on Curiosity also support the loss of atmosphere, but none so directly as argon,” said Atreya. “Argon is the clearest signature of atmospheric loss because it’s chemically inert and does not interact or exchange with the Martian surface or the interior. This was a key measurement that we wanted to carry out on SAM.”
NASA’s Jet Propulsion Laboratory, Pasadena, Calif., manages the Curiosity mission for NASA’s Science Mission Directorate, Washington. The SAM investigation on the rover is managed by NASA Goddard Space Flight Center, Greenbelt, Md.
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“Primordial argon isotope fractionation in the atmosphere of Mars measured by the SAM instrument on Curiosity, and implications for atmospheric loss”
Sushil K. Atreya and Michael H. Wong
Department of Atmospheric, Oceanic and Space Sciences, The University of Michigan, Ann Arbor, Mich.;
Melissa G. Trainer, Heather B. Franz, Charles A. Malespin, Paul R. Mahaffy, Pamela G. Conrad and Anna E.
Goddard Space Flight Center, Greenbelt, Md.;
Concordia College, Moorhead, Minn.;
Laurie A. Leshin
School of Science, Rensselaer Polytechnic Institute, Troy, N.Y.;
John H. Jones
NASA Johnson Space Center, Houston, Tx.;
Christopher R. Webster
Jet Propulsion Laboratory, California Institute of Technology, Pasadena, Calif.;
Tobias C. Owen
University of Hawaii, Honolulu, Hawaii;
Robert O. Pepin
University of Minnesota, Minneapolis, Minn.;
Universidad Nacional Autónoma de México, Ciudad Universitaria, Apartado, México.
Contact information for the authors:
Sushil Atreya, Phone: +1 (734) 936-0489, Email: email@example.com