Trapped Ar isotopes in meteorite ALH 84001 indicate Mars did not have a thick ancient atmosphere
Water is not currently stable in liquid form on the martian surface due to the present mean atmospheric pressure of ∼7 mbar and mean global temperature of ∼220 K. However, geomorphic features and hydrated mineral assemblages suggest that Mars’ climate was once warmer and liquid water flowed on the s...
| Main Authors: | , , , |
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| Format: | Article |
| Language: | en_US |
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Elsevier
2017
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| Online Access: | http://hdl.handle.net/1721.1/110477 https://orcid.org/0000-0003-3113-3415 |
| _version_ | 1811092880033316864 |
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| author | Cassata, William S. Shuster, David L. Renne, Paul R. Weiss, Benjamin P. |
| author2 | Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences |
| author_facet | Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences Cassata, William S. Shuster, David L. Renne, Paul R. Weiss, Benjamin P. |
| author_sort | Cassata, William S. |
| collection | MIT |
| description | Water is not currently stable in liquid form on the martian surface due to the present mean atmospheric pressure of ∼7 mbar and mean global temperature of ∼220 K. However, geomorphic features and hydrated mineral assemblages suggest that Mars’ climate was once warmer and liquid water flowed on the surface. These observations may indicate a substantially more massive atmosphere in the past, but there have been few observational constraints on paleoatmospheric pressures. Here we show how the [superscript 40]Ar/[superscript 36]Ar ratios of trapped gases within martian meteorite ALH 84001 constrain paleoatmospheric pressure on Mars during the Noachian era [∼4.56–3.8 billion years (Ga)]. Our model indicates that atmospheric pressures did not exceed ∼1.5 bar during the first 400 million years (Ma) of the Noachian era, and were <400 mbar by 4.16 Ga. Such pressures of CO[subscript 2] are only sufficient to stabilize liquid water on Mars’ surface at low latitudes during seasonally warm periods. Other greenhouse gases like SO[superscript 2] and water vapor may have played an important role in intermittently stabilizing liquid water at higher latitudes following major volcanic eruptions or impact events. |
| first_indexed | 2024-09-23T15:32:20Z |
| format | Article |
| id | mit-1721.1/110477 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T15:32:20Z |
| publishDate | 2017 |
| publisher | Elsevier |
| record_format | dspace |
| spelling | mit-1721.1/1104772024-05-15T02:11:15Z Trapped Ar isotopes in meteorite ALH 84001 indicate Mars did not have a thick ancient atmosphere Cassata, William S. Shuster, David L. Renne, Paul R. Weiss, Benjamin P. Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences Weiss, Michael Weiss, Benjamin P Water is not currently stable in liquid form on the martian surface due to the present mean atmospheric pressure of ∼7 mbar and mean global temperature of ∼220 K. However, geomorphic features and hydrated mineral assemblages suggest that Mars’ climate was once warmer and liquid water flowed on the surface. These observations may indicate a substantially more massive atmosphere in the past, but there have been few observational constraints on paleoatmospheric pressures. Here we show how the [superscript 40]Ar/[superscript 36]Ar ratios of trapped gases within martian meteorite ALH 84001 constrain paleoatmospheric pressure on Mars during the Noachian era [∼4.56–3.8 billion years (Ga)]. Our model indicates that atmospheric pressures did not exceed ∼1.5 bar during the first 400 million years (Ma) of the Noachian era, and were <400 mbar by 4.16 Ga. Such pressures of CO[subscript 2] are only sufficient to stabilize liquid water on Mars’ surface at low latitudes during seasonally warm periods. Other greenhouse gases like SO[superscript 2] and water vapor may have played an important role in intermittently stabilizing liquid water at higher latitudes following major volcanic eruptions or impact events. United States. National Aeronautics and Space Administration. Mars Fundamental Research Program (Grant MFRP05-0108) Ann and Gordon Getty Foundation 2017-07-05T20:44:21Z 2017-07-05T20:44:21Z 2012-05 2012-04 Article http://purl.org/eprint/type/JournalArticle 0019-1035 http://hdl.handle.net/1721.1/110477 Cassata, William S. et al. “Trapped Ar Isotopes in Meteorite ALH 84001 Indicate Mars Did Not Have a Thick Ancient Atmosphere.” Icarus 221.1 (2012): 461–465. https://orcid.org/0000-0003-3113-3415 en_US http://dx.doi.org/10.1016/j.icarus.2012.05.005 Icarus Creative Commons Attribution-NonCommercial-NoDerivs License http://creativecommons.org/licenses/by-nc-nd/4.0/ application/pdf Elsevier Prof. Weiss via Michael Noga |
| spellingShingle | Cassata, William S. Shuster, David L. Renne, Paul R. Weiss, Benjamin P. Trapped Ar isotopes in meteorite ALH 84001 indicate Mars did not have a thick ancient atmosphere |
| title | Trapped Ar isotopes in meteorite ALH 84001 indicate Mars did not have a thick ancient atmosphere |
| title_full | Trapped Ar isotopes in meteorite ALH 84001 indicate Mars did not have a thick ancient atmosphere |
| title_fullStr | Trapped Ar isotopes in meteorite ALH 84001 indicate Mars did not have a thick ancient atmosphere |
| title_full_unstemmed | Trapped Ar isotopes in meteorite ALH 84001 indicate Mars did not have a thick ancient atmosphere |
| title_short | Trapped Ar isotopes in meteorite ALH 84001 indicate Mars did not have a thick ancient atmosphere |
| title_sort | trapped ar isotopes in meteorite alh 84001 indicate mars did not have a thick ancient atmosphere |
| url | http://hdl.handle.net/1721.1/110477 https://orcid.org/0000-0003-3113-3415 |
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