David Catling

David Catling is a Professor in Earth and Space Sciences at the University of Washington. He is a planetary scientist and astrobiologist whose research focuses on understanding the differences between the evolution of planets, their atmospheres, and their potential for life. He has participated in NASA’s Mars exploration program[1] and contributed research to help find life elsewhere in the solar system and on planets orbiting other stars.[2][3] He is also known for his work on the evolution of Earth’s atmosphere and biosphere, particularly how Earth’s atmosphere became rich in oxygen[4] and allowed complex life to evolve.[5][6]

Biography

David Catling completed a D.Phil. in the Department of Atmospheric, Oceanic and Planetary Physics at the University of Oxford in 1994. After working as a postdoctoral scholar and then research scientist at NASA’s Ames Research Center from 1995-2001, he became a professor at the University of Washington in 2001. Since 2012, he has been a full professor at the University of Washington.

Research

In the area of the evolution of the Earth’s atmosphere, Catling is known for a theory explaining how the Earth’s crust accumulated large quantities of oxidized minerals and how the atmosphere became rich in oxygen.[7] Geological records show that oxygen flooded the atmosphere in a Great Oxidation Event (GOE) about 2.4 billion years ago, even though bacteria that produced oxygen likely evolved hundreds of millions of years earlier. Catling’s theory proposes that biological oxygen was initially used by reactions with chemicals in the environment; gradually, however, Earth’s environment shifted to a tipping point where oxygen flooded the air. Atmospheric methane is the key part of this theory. Before oxygen was abundant, methane gas could reach concentrations hundreds of times greater than today’s 1.8 parts per million. Ultraviolet light decomposes methane molecules in the upper atmosphere, causing hydrogen gas to escape into space. Over time, the irreversible atmospheric escape of hydrogen– a powerful reducing agent -caused Earth to oxidize and reach the GOE tipping point.[8]

Other studies about Earth’s atmospheric oxygen have considered its second increase around 600 million years ago that acted as a precursor to the rise of animal life. Catling proposed looking at oxygen-sensitive variations in stable isotopes of selenium to trace atmospheric and seawater oxygen, and the results of such a study showed that Earth's second increase in oxygen occurred in fits and starts spread over about 100 million years.[9][10]

Catling also contributed to the first measurements of Earth’s atmospheric thickness billions of years ago. He helped pioneer two techniques: using fossil raindrop imprints to set an upper limit on air density, which was applied to fossil imprints from 2.7 billion years ago,[11][12] and using fossil bubbles in ancient lava flows, which suggests that air pressure 2.7 billion years ago was less than half that of the modern atmosphere.[13][14]

Catling has also researched the evolution of the atmosphere and surface of Mars.[15] In the 1990s, he pioneered research on how the types of salts from dried-up lakes or seas on Mars could indicate the past environment and whether Mars was habitable.[16] Since then, the discovery of salts and clays from former lakebeds has been a key success of missions to Mars by NASA and ESA. Catling was on the Science Team for NASA’s Phoenix Lander mission, which in 2008 was the first spacecraft to land in the ice-rich high latitudes of Mars. Catling contributed to research that included the first scoops by a lander of water ice from below the surface of Mars[17] and the first measurement of soluble salts in martian soil, including the soil pH.[18] In experimental work with Jonathan Toner to examine low temperature solutions of perchlorate salts, as found on Mars, Toner and Catling discovered that such solutions supercool and never crystallize.[19] The perchlorates form glasses (amorphous solids) around -120 °C. Glasses are known to be far better for preserving microbes and biological molecules than crystalline salts, which could be relevant to the search for life on Mars, Jupiter’s moon Europa, and Saturn’s moon Enceladus.

In the field of planetary atmospheres, David Catling and Tyler Robinson have proposed a general explanation for a curious observation: the minimum air temperature between the troposphere (the lowest atmospheric layer where temperature declines with altitude) and stratosphere (where temperature increases with altitude in an 'inversion') occurs a pressure of about 0.1 bar on Earth, Titan, Jupiter, Saturn, Uranus and Neptune. This level is the tropopause. Robinson and Catling used the physics of radiation to explain why the tropopause temperature minimum in these extremely different atmospheres occurs at a common pressure.[20] They propose that a pressure around 0.1 bar could be a fairly general rule for planets with stratospheric temperature inversions. This rule could constrain the atmospheric structure on exoplanets and hence their surface temperature and habitability.

Work by Catling and his students is also the first to accurately quantity the thermodynamic disequilibrium in planetary atmospheres of the Solar System, which has been proposed a means to look for life remotely.[2]

Works

David Catling has authored over 100 scientific articles or book chapters. He is the author of the following books:

References

  1. ↑ Shapiro, Nina (April 2015). "As a New Space Race Heats Up, Mars Beckons Once Again". Seattle Weekly. Retrieved 2016-08-21.
  2. 1 2 Krissansen-Totton, J.; Bergsman, D. S.; Catling, D. C. (2016). "On detecting biospheres from chemical disequilibrium in planetary atmospheres". Astrobiology. 16: 39–67. doi:10.1089/ast.2015.1327.
  3. ↑ Krissansen-Totton, J.; Schwieterman, E.; Charnay, B.; Arney, G.; Robinson, T. D.; Meadows, V.; Catling, D. C. (2016). "Is the Pale Blue Dot unique? Optimized photometric bands for identifying Earth-like planets". Astrophysical Journal. 817: 31. doi:10.3847/0004-637X/817/1/31.
  4. ↑ Catling, D. C. (2014). "The Great Oxidation Event Transition". In Holland, H. D.; Turekian, K. K. Treatise on Geochemistry (Second ed.). Amsterdam: Elsevier. pp. 177–195. doi:10.1016/B978-0-08-095975-7.01307-3.
  5. ↑ Catling, D. C.; Glein, C. R.; Zahnle, K. J.; McKay, C. P. "Why O2 is required by complex life on habitable planets and the concept of planetary "oxygenation time". Astrobiology. 5: 415–438. doi:10.1089/ast.2005.5.415.
  6. ↑ Dorminey, Bruce (2012). "Why E.T. Would Also Breathe Oxygen". Forbes Magazine. Retrieved 2016-08-21.
  7. ↑ Catling, D. C.; Zahnle, K. J.; McKay, C. P. (2001). "Biogenic methane, hydrogen escape, and the irreversible oxidation of early Earth". Science. 293: 839–843. doi:10.1126/science.1061976.
  8. ↑ Zahnle, K. J.; Catling, D. C. "Waiting for oxygen". In Shaw, G. H. Special Paper 504: Earth's Early Atmosphere and Surface Environment. Geological Society of America. pp. 37–48.
  9. ↑ Pogge von Strandmann, P.; Stüeken, E. E.; Elliott, T.; Poulton, S. W.; Dehler, C. M.; Canfield, D. E.; Catling, D. C. (2015). "Selenium isotope evidence for post-glacial oxygenation trends in the Ediacaran ocean". Nature Communications. 6: 10157. doi:10.1038/ncomes10157.
  10. ↑ "Oxygen provided breath of life that allowed animals to evolve". Washington.edu. Retrieved January 31, 2016.
  11. ↑ Som, S. M.; Catling, D. C.; Harnmeijer, J. P.; Polivka, P. M.; Buick, R. (2012). "Air density 2.7 billion years ago limited to less than twice modern levels by fossil raindrop imprints". Nature. 484: 359–362. doi:10.1038/nature10890.
  12. ↑ Marder, Jenny (2012). "What a Baking Pan and Hairspray Taught Us About Earth's Ancient Atmosphere". PBS Newshour. Retrieved 2016-08-21.
  13. ↑ Som, S. M.; Buick, R.; Hagadorn, J. W.; Blake, T. S.; Perrault, J. M.; Harnmeijer, J. P.; Catling, D. C. (2012). "Earth's air pressure 2.7 billion years ago constrained to less than half of modern levels". Nature Geoscience. 9: 448–451. doi:10.1038/ngeo2713.
  14. ↑ "The curious lightness of an early atmosphere". The Economist. 419 (8989): 69–70. May 14–20, 2012.
  15. ↑ Catling, David C. "Mars Atmosphere: History and Surface Interactions". In Spohn, T.; Breuer, D.; Johnson, T. V. Encyclopedia of the Solar System (Third ed.). Amsterdam: Elsevier. pp. 343–357. ISBN 9780124158450.
  16. ↑ Catling, D. C. (1999). "A chemical model for evaporites on early Mars: Possible sedimentary tracers of the early climate and implications for exploration". Journal of Geophysical Research. 104: 16,453–16,470. doi:10.1029/1998JE001020.
  17. ↑ Smith, P. H.; Tamppari, L.; Arvidson, R. E.; Bass, D. S.; Blaney, D.; Boynton, W. V.; Carswell, A.; Catling, D. C.; et al. (2009). "H2O at the Phoenix landing site". Science. 325: 58–61. doi:10.1126/science.1172339.
  18. ↑ Hecht, M. H.; Kounaves, S. P.; Quinn, R. C.; West, S. J.; Young, S. M. M.; Ming, D. W.; Catling, D. C.; Clark, B. C.; Boynton, W. V.; Hoffman, J.; DeFlores, L. P.; Gospodinova, K.; Kapit, J.; Smith, P. H. (2009). "Detection of perchlorate and soluble chemistry of martian soil: Findings from the Phoenix Mars Lander". Science. 325: 64–67. doi:10.1126/science.1172466.
  19. ↑ Toner, J. D.; Catling, D. C.; Light, B. (2014). "The formation of supercooled brines, viscous liquids, and low-temperature glasses on Mars". Icarus. 233: 36–47. doi:10.1016/j.icarus.2014.01.018.
  20. ↑ Robinson, T. D.; Catling, D. C. (2014). "Common 0.1 bar tropopause in thick atmospheres set by pressure-dependent infrared transparency". Nature Geoscience. 7: 12–15. doi:10.1038/NGEO2020.
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