Jun 11, 1999
Unearthing Clues to Martian Fossils
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Unearthing clues to Martian fossils
The hunt for signs of ancient life on Mars
leads scientists to Mono Lake, CA
First you would die, either from asphyxiation or hypothermia. Mars's carbon dioxide atmosphere is 100 times less dense than Earth's and the average surface temperature is -60 deg C. The exact cause of death would depend on the season, the time of day (Martian temperatures fluctuate as much as 100 degrees from dawn to dusk), and the latitude of your surprise landing site.
Next you would begin to dry out. There is no liquid water on the surface of Mars and little, if any, water vapor in the atmosphere. Your lifeless body would become dessicated like an Egyptian mummy.
Finally, not that it would matter terribly, you would contract a very nasty sunburn. The Red Planet's rarefied atmosphere does a poor job blocking UV rays from the sun (there is no protective ozone layer in the atmosphere). Radiation levels are so intense that they probably sterilize the uppermost layers of Martian soil.
The next time you visit Mars, take a space suit.
December 3: Mars Polar Lander nears touchdown
December 2: What next, Leonids?
November 30: Polar Lander Mission Overview
November 30: Learning how to make a clean sweep in space
The reality of this picture is somewhat controversial, but if it is true, it seems likely to many scientists that early Mars could have teemed with simple forms of life.
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Farmer (formerly of NASA/Ames) along with his collaborators at ASU, is a pioneer in the new scientific discipline called exopaleontology -- the search for signs of primeval life on other planets.
"Mars may harbor the best preserved rocks in the solar system," he continued. "For example, the Allan Hills meteorite [an ancient potato-sized rock from Mars that crashed into Antarctica 13,000 years ago] is nearly 4.6 billion years old. The fossil record on Mars might go all the way back to the earliest history of the planet."
Farmer says he wouldn't mind visiting Mars to prospect for fossils in person, but an unmanned probe is likely to be the first exopalentologist on the Red Planet. Where should a Mars lander set down to seek out the elusive fossil record? The answer to that question may be found here on Earth in an other-worldly place called Mono Lake.
"Mono Lake lies in a lifeless, hideous desert ... This solemn, silent, sailless sea - this lonely tenant of the loneliest spot on earth - is little graced with the picturesque."Mono Lake in California is nearly 700,000 years old, making it one of the oldest lakes in North America. Throughout its long existence, salts and minerals have washed into the lake from Eastern Sierra streams, but there is no outlet. Fresh water evaporating leaves behind salts and minerals so that now Mono Lake is about 2 1/2 times as salty and 80 times as alkaline as the ocean. Swimmers in the lake find that they literally cannot sink (dissolved carbonates, chlorides and sulfates make floating easy) but their skin does tend to bleach and burn in the alkaline water.
Mark Twain, Roughing It, 1875
Left: Mars Global Surveyor image of Gusev Crater and Ma'adim Valles. More images and information.
There is almost certainly no life in places like Gusev Crater today. All the ancient ponds and lakes on Mars are now bone dry and scorched by solar UV radiation. Nevertheless, there could be fossils of life forms that thrived billions of years ago, and a curious geological feature of Mono Lake may be telling us where and how to look for them.
At first glance the most striking aspect of Mono Lake are the weird mineral spires called tufa, a type of freshwater limestone. They are formed when calcium-rich spring water bubbles up through the alkaline lake, which is rich in bicarbonate. The calcium and bicarbonate combine, precipitating out as limestone. Tufa towers only grow while underwater, but at Mono Lake they can be seen towering as much as 12 feet above the surface. That's because the lake level has been lowered in recent years to supply water to Los Angeles, 360 miles to the south.
"Whenever you have minerals that precipitate rapidly as they do around the springs in Mono Lake, microorganisms become entombed," says Farmer. "The fossils of soft-bodied microbes formed by this process could be preserved for billions of years."
Farmer has spent many years studying the tufa at Mono Lake as an analog of carbonate deposits that might one day be discovered on Mars.
"There are lots of microfossils here and there in the tufa, formed where the rapid precipitation of carbonates captured microorganisms," continued Farmer. "I've seen larval casings of alkaline flies and cyanobacteria fossils, also things that look like algae (simple multicellular plants). I haven't yet found any fossils of brine shrimp, but I'm still looking."
"In thin sections of tufa I've also found clumps of decayed organic material called kerogen, which may contain chemofossil signatures. Chemofossils are the chemicals produced by the breakdown of cell walls. For example, Mono Lake diatoms have a hard shell with an organic coating that protects them from the alkaline water. When they die, the coating dissolves and so does the diatom. All that's left of this organic material is trace chemicals. It is possible to relate such products to specific organisms like diatoms or algae, but its not always easy. You have to become a Sherlock Holmes and piece together what the community must have been like from clues (both chemical and fossil) that are preserved."
"In evaporative basins, there's a lot of variation in chemistry from basin to basin, and throughout the history of the lake," Farmer continued. "What's beautiful about Mono Lake is that we have an active system of tufa-formation and mineral precipitation. Other paleo lake basins in Western North America are now dry because the climate has changed and evaporation now dominates inflow."
In Search of Mono Lake -- on Mars?Finding microfossils on Mars won't be easy, even if life once existed there. After all Mars is a big planet and fossils are not likely to be found just anywhere. No one knows for sure, but Farmer and collaborators think that a good starting point might be evaporative basins with carbonate deposits where microbial fossils could be entombed, in other words, places that were once like Mono Lake.
The chemical mixture in an evaporative basin depends on what kinds of rocks are in the vicinity. When water flows into a lake, it flows over rocks and dissolves minerals and ions such as sodium, chloride ions, pottasium, calcium -- all the salts commonly found in the Western Salt Lakes. In an evaporative basin the salts and minerals become concentrated, and the lake naturally becomes alkaline with ph > 9. The detailed chemical balance depends on the details of the terrain. This general picture is true on both Mars and Earth.
"Compared to Earth, Mars has a much different set of source rocks," explains Farmer. "On Mars the crust is more like the ocean floor on Earth, featuring basalts, iron, magnesium, and silicate-poor rocks. Rocks in the Mono Basin are enriched in silica, sodium and potassium. Because water was less abundant, it took longer to build up briney water on Mars through evaporation. But the waters there would be richer in calcium, magnesium, and iron. In spite of these chemical differences, the basic picture is still the same: rapid precipitation of minerals would have been an important process in these ancient martian basins, and if microorganisms were there, their fossils would have been entombed."
Phil Christensen, one of Farmer's collaborators, is using the Thermal Emission Spectrograph (TES) on Mars Global Surveyor to search out places on Mars with tufa-like carbonate formations in evaporated lake beds. Carbonates have specific kinds of absorption features in mid-infrared spectra that should be easy to identify. Unfortunately, the resolution of the TES is only 3 km/pixel, which would make smaller carbonate deposits like those at Mono Lake difficult to detect. In March 2001 an Arizona State University instrument called THEMIS (Thermal Emission Imaging System) is scheduled for launch on NASA's Mars Surveyor 2001 orbiter. With a spatial resolution of 100m per pixel, the ASU spectrometer could easily detect the signature of carbonate deposits at the scale of the Mono Lake tufas.
Above: Sample carbonate absorption spectra in the mid-infrared. More information from the USGS.
"I'm optimistic," concludes Farmer. "Eventually I believe we're going to find carbonate deposits on Mars -- places that remind us of Mono Lake -- and when we do we'll have strong arguments for a landing site for exobiology. It's just a matter of time." Related Links Related Stories:
The Red Planet in 3D -- New data from Mars Global Surveyor reveal the topography of Mars better than many continental regions on Earth. May 27, 1999 NASA NASA Science News
Search for life on Mars will start in Siberia -- Russian and NASA scientists will look for life forms in the inhospitable realm of Siberian permafrost. May 27, 1999 NASA NASA Science News
Stormy weather on Mars -- During the recent close approach of Mars to Earth, NASA's Hubble Space Telescope spotted a gigantic storm swirling near the Red Planet's north pole. May 19, 1999 NASA NASA Science News
Mars unveils a magnetic personality -- Plate tectonics on the Red Planet might have important consequences for ancient Martian life. Apr 30, 1999 NASA NASA Science News
Plate tectonics on Mars? -- Magnetic stripes on the surface of Mars are similar to fields in the sea floors of Earth. Apr 29, 1999 NASA NASA Science News
A close encounter with the Red Planet -- Mars makes its closest approach to Earth in 1999. Apr 23, 1999 NASA NASA Science News
A new face on Mars has scientists smiling -- MGS beams back pictures of the "Happy Face Crater". Mar. 12, 1999 NASA NASA Science News
Related Web Links:
Gusev Crater and Ma'adim Vallis -- Global Surveyor images
Mars weather, climate, and life FAQ -- from NASA/Ames
www.MonoLake.org -- Mono Lake home page
What would happen to a dead body on Mars? -- NASA/Ames Quest Ask-a-Scientist query
Mars Surveyor 2001 -- home page at JPL
Mars Global Surveyor -- home page at JPL
THEMIS -- Thermal Emission Imaging System from ASU
ASU Planetary Exploration Lab -- Thermal Emission Imaging System from ASU
NASA Astrobiology -- an excellent website from NASA/Ames
Appendix: Where did all the water go?There may have once been ponds and lakes on Mars, but they're dry now. Physical conditions on the surface of Mars, namely low atmospheric pressure and low temperature, conspire to make liquid water unstable. The average atmospheric pressure on Mars is only about 6 millibars compared to the Earth's average pressure of 1013 millibars. The average surface temperature on Mars is about -60 deg C compared to the Earth's 15 deg C. At certain locations and times on Mars, when the air pressure is high enough and the temperature is above freezing (greater than 0 deg C), liquid water is theoretically possible; but the rate of evaporation would be so great that liquid water (if it were present) would rapidly vaporize.
Nevertheless, there is widespread evidence of dried-up valleys and channels thought to have been eroded by liquid water. Many Martian outflow channels strongly resemble flood channels on Eath, like those in eastern Washington in the USA. On Mars they may have formed when groundwater or subsurface slush was catastrophically brought to the surface, perhaps triggered by large impacts or "marsquakes". On the other hand, geological studies of the valley networks suggest that these must have been gradually eroded by running water: some show morphology suggesting formation by groundwater sapping (i.e. when a river is fed by a spring and the valley grows by headward erosion); others seem to have been produced by precipitation runoff. The valley networks are almost completely (but not quite) restricted to ancient upper highlands, dated as 3.5 to 4.0 billion years old from the quantity of impact craters, so it is postulated that environmental conditions on Mars must have been conducive to liquid water at this time.
Right: High resolution Mars Global Surveyor images were combined with Viking Orbiter color data to produce this stunning, detailed view of a Martian canyon's edge. The area pictured is about 6 miles wide and represents a tiny part of the northern edge of the canyon Valles Marineris, whose total length is about 2,500 miles. Details 20 to 30 feet across can be seen in the high resolution data. What processes caused the well-defined layers in the steep canyon walls? In the Grand Canyon on planet Earth, sedimentary processes have resulted in spectacular rock layers. But similar layers of rock in canyons of the Hawaiian Islands were created by volcanoes. Regardless of the origin of layering on Mars, its extent suggests that early Mars was geologically active and complex. More information.
The upper limit on the present amount of water on the martian surface is 800,000 to 1.2 million cubic miles (3.2 to 4.7 million cubic kilometers), or about 1.5 times the amount of ice covering Greenland. If both caps are composed completely of water, the combined volumes are equivalent to a global layer 66 to 100 feet (22 to 33 meters) deep, about one-third the minimum volume of a proposed ancient ocean on Mars.