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Wiens RC, Udry A, Beyssac O, Quantin-Nataf C, Mangold N, Cousin A, Mandon L, Bosak T, Forni O, McLennan SM, Sautter V, Brown A, Benzerara K, Johnson JR, Mayhew L, Maurice S, Anderson RB, Clegg SM, Crumpler L, Gabriel TSJ, Gasda P, Hall J, Horgan BHN, Kah L, Legett C, Madariaga JM, Meslin PY, Ollila AM, Poulet F, Royer C, Sharma SK, Siljeström S, Simon JI, Acosta-Maeda TE, Alvarez-Llamas C, Angel SM, Arana G, Beck P, Bernard S, Bertrand T, Bousquet B, Castro K, Chide B, Clavé E, Cloutis E, Connell S, Dehouck E, Dromart G, Fischer W, Fouchet T, Francis R, Frydenvang J, Gasnault O, Gibbons E, Gupta S, Hausrath EM, Jacob X, Kalucha H, Kelly E, Knutsen E, Lanza N, Laserna J, Lasue J, Le Mouélic S, Leveille R, Lopez Reyes G, Lorenz R, Manrique JA, Martinez-Frias J, McConnochie T, Melikechi N, Mimoun D, Montmessin F, Moros J, Murdoch N, Pilleri P, Pilorget C, Pinet P, Rapin W, Rull F, Schröder S, Shuster DL, Smith RJ, Stott AE, Tarnas J, Turenne N, Veneranda M, Vogt DS, Weiss BP, Willis P, Stack KM, Williford KH, Farley KA. Compositionally and density stratified igneous terrain in Jezero crater, Mars. SCIENCE ADVANCES 2022; 8:eabo3399. [PMID: 36007007 PMCID: PMC9410274 DOI: 10.1126/sciadv.abo3399] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 02/07/2022] [Accepted: 05/31/2022] [Indexed: 06/15/2023]
Abstract
Before Perseverance, Jezero crater's floor was variably hypothesized to have a lacustrine, lava, volcanic airfall, or aeolian origin. SuperCam observations in the first 286 Mars days on Mars revealed a volcanic and intrusive terrain with compositional and density stratification. The dominant lithology along the traverse is basaltic, with plagioclase enrichment in stratigraphically higher locations. Stratigraphically lower, layered rocks are richer in normative pyroxene. The lowest observed unit has the highest inferred density and is olivine-rich with coarse (1.5 millimeters) euhedral, relatively unweathered grains, suggesting a cumulate origin. This is the first martian cumulate and shows similarities to martian meteorites, which also express olivine disequilibrium. Alteration materials including carbonates, sulfates, perchlorates, hydrated silicates, and iron oxides are pervasive but low in abundance, suggesting relatively brief lacustrine conditions. Orbital observations link the Jezero floor lithology to the broader Nili-Syrtis region, suggesting that density-driven compositional stratification is a regional characteristic.
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Affiliation(s)
- Roger C. Wiens
- Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA
| | - Arya Udry
- Department of Geoscience, University of Nevada Las Vegas, Las Vegas, NV, USA
| | - Olivier Beyssac
- Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, Muséum National d’Histoire Naturelle, Paris, France
| | - Cathy Quantin-Nataf
- Laboratoire de Géologie de Lyon, Université de Lyon, Université Claude Bernard Lyon1, Ecole Normale Supérieure de Lyon, Université Jean Monnet Saint Etienne, CNRS, Villeurbanne, France
| | - Nicolas Mangold
- Laboratoire de Planétologie et Géosciences, CNRS UMR 6112, Nantes Université, Université d’Angers, Université du Mans, Nantes, France
| | - Agnès Cousin
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse 3 Paul Sabatier, UPS, CNRS, CNES, Toulouse, France
| | - Lucia Mandon
- Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris-PSL, CNRS, Sorbonne Université, Université de Paris Cité, Meudon, France
| | - Tanja Bosak
- Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Olivier Forni
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse 3 Paul Sabatier, UPS, CNRS, CNES, Toulouse, France
| | | | - Violaine Sautter
- Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, Muséum National d’Histoire Naturelle, Paris, France
| | | | - Karim Benzerara
- Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, Muséum National d’Histoire Naturelle, Paris, France
| | - Jeffrey R. Johnson
- Space Exploration Sector, Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | - Lisa Mayhew
- Department of Geological Sciences, University of Colorado, Boulder, CO, USA
| | - Sylvestre Maurice
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse 3 Paul Sabatier, UPS, CNRS, CNES, Toulouse, France
| | - Ryan B. Anderson
- U.S. Geological Survey Astrogeology Science Center, Flagstaff, AZ, USA
| | - Samuel M. Clegg
- Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA
| | - Larry Crumpler
- New Mexico Museum of Natural History, Albuquerque, NM, USA
| | | | - Patrick Gasda
- Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA
| | - James Hall
- Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Briony H. N. Horgan
- Earth, Atmospheric, and Planetary Sciences, Purdue University, West Lafayette, IN, USA
| | - Linda Kah
- Earth and Planetary Sciences, University of Tennessee, Knoxville, TN, USA
| | - Carey Legett
- Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA
| | | | - Pierre-Yves Meslin
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse 3 Paul Sabatier, UPS, CNRS, CNES, Toulouse, France
| | - Ann M. Ollila
- Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA
| | - Francois Poulet
- Institut d’Astrophysique Spatiale, CNRS, Univ. Paris-Saclay, Orsay, France
| | - Clement Royer
- Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris-PSL, CNRS, Sorbonne Université, Université de Paris Cité, Meudon, France
| | | | | | - Justin I. Simon
- Center for Isotope Cosmochemistry and Geochronology, NASA Johnson Space Center, Houston, TX, USA
| | | | | | - S. Michael Angel
- Department of Chemistry and Biochemistry, University of South Carolina, Columbia, SC, USA
| | - Gorka Arana
- University of Basque Country, UPV/EHU, Leioa, Bilbao, Spain
| | - Pierre Beck
- Institut de Planétologie et d’Astrophysique de Grenoble, CNRS, Université Grenoble Alpes, Grenoble, France
| | - Sylvain Bernard
- Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, CNRS, Sorbonne Université, Muséum National d’Histoire Naturelle, Paris, France
| | - Tanguy Bertrand
- Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris-PSL, CNRS, Sorbonne Université, Université de Paris Cité, Meudon, France
| | - Bruno Bousquet
- Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France
| | - Kepa Castro
- University of Basque Country, UPV/EHU, Leioa, Bilbao, Spain
| | - Baptiste Chide
- Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA
| | - Elise Clavé
- Centre Lasers Intenses et Applications, CNRS, CEA, Université de Bordeaux, Bordeaux, France
| | - Ed Cloutis
- University of Winnipeg, Winnipeg, MB, Canada
| | | | - Erwin Dehouck
- Laboratoire de Géologie de Lyon, Université de Lyon, Université Claude Bernard Lyon1, Ecole Normale Supérieure de Lyon, Université Jean Monnet Saint Etienne, CNRS, Villeurbanne, France
| | - Gilles Dromart
- Laboratoire de Géologie de Lyon, Université de Lyon, Université Claude Bernard Lyon1, Ecole Normale Supérieure de Lyon, Université Jean Monnet Saint Etienne, CNRS, Villeurbanne, France
| | | | - Thierry Fouchet
- Laboratoire d’Etudes Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris-PSL, CNRS, Sorbonne Université, Université de Paris Cité, Meudon, France
| | - Raymond Francis
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | | | - Olivier Gasnault
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse 3 Paul Sabatier, UPS, CNRS, CNES, Toulouse, France
| | | | - Sanjeev Gupta
- Department of Earth Science and Engineering, Imperial College London, London, UK
| | | | - Xavier Jacob
- Institut de Mécanique des Fluides, Université de Toulouse 3 Paul Sabatier, Institut National Polytechnique de Toulouse, Toulouse, France
| | | | - Evan Kelly
- University of Hawai‘i, Honolulu, HI, USA
| | - Elise Knutsen
- Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Université Paris Saclay, Sorbonne Université, Guyancourt, France
| | - Nina Lanza
- Space and Planetary Exploration Team, Los Alamos National Laboratory, Los Alamos, NM, USA
| | | | - Jeremie Lasue
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse 3 Paul Sabatier, UPS, CNRS, CNES, Toulouse, France
| | - Stéphane Le Mouélic
- Laboratoire de Planétologie et Géosciences, CNRS UMR 6112, Nantes Université, Université d’Angers, Université du Mans, Nantes, France
| | | | | | - Ralph Lorenz
- Space Exploration Sector, Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA
| | | | | | | | - Noureddine Melikechi
- Department of Physics and Applied Physics, Kennedy College of Sciences, University of Massachusetts, Lowell, MA, USA
| | - David Mimoun
- Institut Supérieur de l’Aéronautique et de l’Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France
| | - Franck Montmessin
- Laboratoire Atmosphères, Milieux, Observations Spatiales, CNRS, Université Saint-Quentin-en-Yvelines, Université Paris Saclay, Sorbonne Université, Guyancourt, France
| | | | - Naomi Murdoch
- Institut Supérieur de l’Aéronautique et de l’Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France
| | - Paolo Pilleri
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse 3 Paul Sabatier, UPS, CNRS, CNES, Toulouse, France
| | - Cedric Pilorget
- Institut d’Astrophysique Spatiale, CNRS, Univ. Paris-Saclay, Orsay, France
| | - Patrick Pinet
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse 3 Paul Sabatier, UPS, CNRS, CNES, Toulouse, France
| | - William Rapin
- Institut de Recherche en Astrophysique et Planetologie (IRAP), Université de Toulouse 3 Paul Sabatier, UPS, CNRS, CNES, Toulouse, France
| | - Fernando Rull
- Research Group ERICA, Universidad de Valladolid, Valladolid, Spain
| | - Susanne Schröder
- Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany
| | - David L. Shuster
- Department of Earth and Planetary Science, University of California, Berkeley, CA, USA
| | | | - Alexander E. Stott
- Institut Supérieur de l’Aéronautique et de l’Espace (ISAE-SUPAERO), Université de Toulouse, Toulouse, France
| | - Jesse Tarnas
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | | | - Marco Veneranda
- Research Group ERICA, Universidad de Valladolid, Valladolid, Spain
| | - David S. Vogt
- Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institute of Optical Sensor Systems, Berlin, Germany
| | - Benjamin P. Weiss
- Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Peter Willis
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Kathryn M. Stack
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Kenneth H. Williford
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
- Blue Marble Space Institute of Science, Seattle, WA, USA
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Enya K, Yamagishi A, Kobayashi K, Yoshimura Y. Comparative study of methods for detecting extraterrestrial life in exploration mission of Mars and the solar system. LIFE SCIENCES IN SPACE RESEARCH 2022; 34:53-67. [PMID: 35940690 DOI: 10.1016/j.lssr.2022.07.001] [Citation(s) in RCA: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/12/2022] [Revised: 06/16/2022] [Accepted: 07/07/2022] [Indexed: 06/15/2023]
Abstract
The detection and analysis of extraterrestrial life are important issues of space science. Mars is among the most important planets to explore for extraterrestrial life, owing both to its physical properties and to its ancient and present environments as revealed by previous exploration missions. In this paper, we present a comparative study of methods for detecting extraterrestrial life and life-related substances. To this end, we have classified and summarized the characteristics targeted for the detection of extraterrestrial life in solar system exploration mission and the methods used to evaluate them. A summary table is presented. We conclude that at this moment (i) there is no realistic single detection method capable of concluding the discovery of extraterrestrial life, (ii) no single method has an advantage over the others in all respects, and (iii) there is no single method capable of distinguishing extraterrestrial life from terrestrial life. Therefore, a combination of complementary methods is essential. We emphasize the importance of endeavoring to detect extraterrestrial life without overlooking possible alien life forms, even at the cost of tolerating false positives. Summaries of both the targets and the detection methods should be updated continuously, and comparative studies of both should be pursued. Although this study assumes Mars to be a model site for the primary environment for life searches, both the targets and detection methods described herein will also be useful for searching for extraterrestrial life in any celestial environment and for the initial inspection of returned samples.
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Affiliation(s)
- Keigo Enya
- Institute of Space & Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuou, Sagamihara, Kanagawa 252-5210, Japan.
| | - Akihiko Yamagishi
- School of Life Science, Tokyo University of Pharmacy and Life Science, 1432-1 Horinouchi, Hachioji, Tokyo 192-0392, Japan
| | - Kensei Kobayashi
- Department of Chemistry, Yokohama National University, 79-5 Tokiwadai, Hodogaya, Yokohama 240-8501, Japan
| | - Yoshitaka Yoshimura
- Department of Life Science, Tamagawa University, 6-1-1 Tamagawagakuen, Machida, Tokyo 194-8610, Japan
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Leask EK, Ehlmann BL, Greenberger RN, Pinet P, Daydou Y, Ceuleneer G, Kelemen P. Tracing Carbonate Formation, Serpentinization, and Biological Materials With Micro-/Meso-Scale Infrared Imaging Spectroscopy in a Mars Analog System, Samail Ophiolite, Oman. EARTH AND SPACE SCIENCE (HOBOKEN, N.J.) 2021; 8:e2021EA001637. [PMID: 34820479 PMCID: PMC8596454 DOI: 10.1029/2021ea001637] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/03/2021] [Revised: 09/14/2021] [Accepted: 09/20/2021] [Indexed: 05/25/2023]
Abstract
Visible-shortwave infrared (VSWIR) imaging spectrometers map composition remotely with spatial context, typically at many meters-scale from orbital and airborne data. Here, we evaluate VSWIR imaging spectroscopy capabilities at centimeters to sub-millimeter scale at the Samail Ophiolite, Oman, where mafic and ultramafic lithologies and their alteration products, including serpentine and carbonates, are exposed in a semi-arid environment, analogous to similar mineral associations observed from Mars orbit that will be explored by the Mars-2020 rover. At outcrop and hand specimen scales, VSWIR spectroscopy (a) identifies cross-cutting veins of calcite, dolomite, magnesite, serpentine, and chlorite that record pathways and time-order of multiple alteration events of changing fluid composition; (b) detects small-scale, partially altered remnant pyroxenes and localized epidote and prehnite that indicate protolith composition and temperatures and pressures of multiple generations of faulting and alteration, respectively; and (c) discriminates between spectrally similar carbonate and serpentine phases and carbonate solid solutions. In natural magnesite veins, minor amounts of ferrous iron can appear similar to olivine's strong 1-μm absorption, though no olivine is present. We also find that mineral identification for carbonate and serpentine in mixtures with each other is strongly scale- and texture-dependent; ∼40 area% dolomite in mm-scale veins at one serpentinite outcrop and ∼18 area% serpentine in a calcite-rich travertine outcrop are not discriminated until spatial scales of <∼1-2 cm/pixel. We found biological materials, for example bacterial mats versus vascular plants, are differentiated using wavelengths <1 μm while shortwave infrared wavelengths >1 μm are required to identify most organic materials and distinguish most mineral phases.
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Affiliation(s)
- Ellen K. Leask
- Division of Geological & Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
- Now at Johns Hopkins University/Applied Physics LaboratoryLaurelMDUSA
| | - Bethany L. Ehlmann
- Division of Geological & Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Rebecca N. Greenberger
- Division of Geological & Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - Patrick Pinet
- Institut de Recherche en Astrophysique et Planétologie (IRAP)Université de ToulouseCNRSUPSCNESToulouseFrance
| | - Yves Daydou
- Institut de Recherche en Astrophysique et Planétologie (IRAP)Université de ToulouseCNRSUPSCNESToulouseFrance
| | - Georges Ceuleneer
- Geosciences Environnement Toulouse (GET)Université de ToulouseCNRSUPSToulouseFrance
| | - Peter Kelemen
- Department of Earth & Environmental SciencesColumbia UniversityLamont Doherty Earth ObservatoryPalisadesNYUSA
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Yang M, Schatz GC. Quasiclassical Trajectory Study of the O( 3P) + CO 2( 1Σ g+) Reaction at Hyperthermal Energies. J Phys Chem A 2021; 125:8626-8634. [PMID: 34585571 DOI: 10.1021/acs.jpca.1c05836] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/28/2022]
Abstract
This paper presents the reaction mechanism, cross sections, and product energy partitioning for the O + CO2 reaction, calculated using Born-Oppenheimer molecular dynamics simulations with the quasiclassical trajectory (BOMD-QCT) method. At collision energies up to 9.5 eV, three reactions, oxygen exchange (above ∼1.5 eV), abstraction (above ∼5.5 eV), and dissociation (above ∼7.5 eV) occur, with abstraction and dissociation involving either an insertion-elimination mechanism or a stripping mechanism. The insertion-elimination mechanism involves the formation of a planar CO3 intermediate which lies 0.52 eV above the ground-state CO2; the energetic barrier for oxygen abstraction via this mechanism is 3.52 eV. Interestingly, the insertion-elimination mechanism predominately contributes to the cross sections at collision energies just above the effective energetic threshold for the abstraction and dissociation reactions; at higher collision energies, the contribution from the stripping mechanism increases and eventually dominates. At a collision energy of 9.5 eV, the cross sections for oxygen exchange, abstraction, and dissociation are 4.17 a02, 1.58 a02, and 0.68 a02, respectively. The lower reaction cross sections, higher effective reaction barrier, and product energy distribution of the stripping mechanism were attributed to the short lifetime (28 fs) of the OCOO species compared with that of the CO3 species (45 fs) that arises in the insertion-elimination mechanism. For the exchange reaction, it is found that roughly 40% of the reactant translational energy ends up in CO2 vibration, which provides a single-collision mechanism to produce highly excited CO2. We also studied intersystem crossing effects using trajectory surface hopping calculations and find no changes compared to single surface (triplet) calculations at energies below 7.5 eV; however, at 7.5 eV and higher the abstraction cross sections are changed by as much as 20%, and the (very small) dissociation cross sections are changed by factors of four or more.
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Affiliation(s)
- Muwen Yang
- Department of Chemistry and Applied Physics, Northwestern University, 2145 Sheridan Road, Evanston, Illinois 60208-3113, United States
| | - George C Schatz
- Department of Chemistry and Applied Physics, Northwestern University, 2145 Sheridan Road, Evanston, Illinois 60208-3113, United States
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YOSHIMURA Y, ENYA K, KOBAYASHI K, SASAKI S, YAMAGISHI A. Life Explorations for Biosignatures in Space. BUNSEKI KAGAKU 2021. [DOI: 10.2116/bunsekikagaku.70.309] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/23/2022]
Affiliation(s)
- Yoshitaka YOSHIMURA
- Department of Advanced Food Sciences, College of Agriculture, Tamagawa University
| | - Keigo ENYA
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency
| | - Kensei KOBAYASHI
- Graduate School of Engineering Science, Yokohama National University
| | - Satoshi SASAKI
- School of Bioscience and Biotechnology, Tokyo University of Technology
| | - Akihiko YAMAGISHI
- Department of Applied Life Sciences, School of Life Sciences, Tokyo University of Pharmacy and Life Sciences
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Abstract
Transverse aeolian ridges (TARs) are poorly understood relict aeolian Martian surface features. Processes that create TARs are not well-constrained, and understanding their formation is complicated since they appear to share some features of ripples, megaripples, and dunes. While some evidence of multi-stage TAR formation has been documented in Nirgal Vallis, here we present additional evidence for this process at nine locations on Mars using cratering superposition between different ridge morphologies. Most occurrences of multistage evolution will not preserve the precise series of cratering and formation events documented here, which potentially means that this formative process may have been more common than even these new widespread observations suggest. This formative process can help determine the relative similarity of TARs to ripples, megaripples and dunes. Based on our observations, we conclude that primary TAR forms are most like megaripples, and that subsequent ridges formed like aqueous ripple spurs.
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Thermodynamic Constraints on Smectite and Iron Oxide Formation at Gale Crater, Mars: Insights into Potential Free Energy from Aerobic Fe Oxidation in Lake Water–Groundwater Mixing Zone. MINERALS 2021. [DOI: 10.3390/min11040341] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
The presence of saponite and iron oxides in Sheepbed mudstone of Yellowknife Bay at Gale crater on Mars is considered as evidence of a habitable fluvio-lacustrine environment for chemolithoautotrophy. However, the energetic availability for metabolic reactions is poorly constrained. Herein, we propose the possible mixing of surface water and groundwater that (i) explains the formation of magnetite and hematite detected in Sheepbed mudstone and (ii) may work as a potential habitable zone for aerobic Fe2+-oxidizing microbes. Our thermodynamic modeling of water–rock reactions revealed that the formation of abundant saponite in Sheepbed mudstone may occur under various conditions of water-to-rock mass ratios, temperatures (5–200 °C), and initial fluid compositions. In contrast, the formation of iron oxides in the mudstone can be explained only by the mixing of Fe2+-rich groundwater and more oxidized surface waters, where the Fe2+-rich groundwater can be generated by the low-temperature water–rock reactions with a CO2-bearing initial fluid. The calculated bioavailable energy of aerobic Fe2+ oxidation in the fluid-mixing zone on Mars is similar to that estimated for a fluid-mixing zone on Earth actually inhabited by aerobic Fe2+-oxidizing microbes. The findings will contribute to a better understanding of potential habitability on Mars.
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Aerts JW, Riedo A, Melton DJ, Martini S, Flahaut J, Meierhenrich UJ, Meinert C, Myrgorodska I, Lindner R, Ehrenfreund P. Biosignature Analysis of Mars Soil Analogs from the Atacama Desert: Challenges and Implications for Future Missions to Mars. ASTROBIOLOGY 2020; 20:766-784. [PMID: 32167834 DOI: 10.1089/ast.2019.2063] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
The detection of biosignatures on Mars is of outstanding interest in the current field of astrobiology and drives various fields of research, ranging from new sample collection strategies to the development of more sensitive detection techniques. Detailed analysis of the organic content in Mars analog materials collected from extreme environments on Earth improves the current understanding of biosignature preservation and detection under conditions similar to those of Mars. In this article, we examined the biological fingerprint of several locations in the Atacama Desert (Chile), which include different wet and dry, and intermediate to high elevation salt flats (also named salars). Liquid chromatography and multidimensional gas chromatography mass spectrometry measurement techniques were used for the detection and analysis of amino acids extracted from the salt crusts and sediments by using sophisticated extraction procedures. Illumina 16S amplicon sequencing was used for the identification of microbial communities associated with the different sample locations. Although amino acid load and organic carbon and nitrogen quantities were generally low, it was found that most of the samples harbored complex and versatile microbial communities, which were dominated by (extremely) halophilic microorganisms (most notably by species of the Archaeal family Halobacteriaceae). The dominance of salts (i.e., halites and sulfates) in the investigated samples leaves its mark on the composition of the microbial communities but does not appear to hinder the potential of life to flourish since it can clearly adapt to the higher concentrations. Although the Atacama Desert is one of the driest and harshest environments on Earth, it is shown that there are still sub-locations where life is able to maintain a foothold, and, as such, salt flats could be considered as interesting targets for future life exploration missions on Mars.
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Affiliation(s)
- Joost W Aerts
- Molecular Cell Biology, Faculty of Science, VU University Amsterdam, Amsterdam, The Netherlands
| | - Andreas Riedo
- Astrobiology Laboratory, Sackler Laboratory for Astrophysics, Leiden Observatory, Leiden University, Leiden, The Netherlands
| | - Daniel J Melton
- Astrobiology Laboratory, Sackler Laboratory for Astrophysics, Leiden Observatory, Leiden University, Leiden, The Netherlands
| | - Simone Martini
- Astrobiology Laboratory, Sackler Laboratory for Astrophysics, Leiden Observatory, Leiden University, Leiden, The Netherlands
| | - Jessica Flahaut
- CRPG, CNRS/University of Lorraine, Vandoeuvre-les-Nancy, France
| | - Uwe J Meierhenrich
- CNRS, Institut de Chimie de Nice UMR 7272, Université Côte d'Azur, Nice, France
| | - Cornelia Meinert
- CNRS, Institut de Chimie de Nice UMR 7272, Université Côte d'Azur, Nice, France
| | | | - Robert Lindner
- Life Support and Physical Sciences Instrumentation Section, European Space Agency, ESTEC, Noordwijk, The Netherlands
| | - Pascale Ehrenfreund
- Astrobiology Laboratory, Sackler Laboratory for Astrophysics, Leiden Observatory, Leiden University, Leiden, The Netherlands
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Brown AJ, Viviano CE, Goudge TA. Olivine-Carbonate Mineralogy of the Jezero Crater Region. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2020; 125:e2019JE006011. [PMID: 33123452 PMCID: PMC7592698 DOI: 10.1029/2019je006011] [Citation(s) in RCA: 23] [Impact Index Per Article: 5.8] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/24/2019] [Accepted: 12/18/2019] [Indexed: 05/28/2023]
Abstract
A well-preserved, ancient delta deposit, in combination with ample exposures of carbonate outcrops, makes Jezero Crater in Nili Fossae a compelling astrobiological site. We use Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) observations to characterize the surface mineralogy of the crater and surrounding watershed. Previous studies have documented the occurrence of olivine and carbonates in the Nili Fossae region. We focus on correlations between these two well-studied lithologies in the Jezero crater watershed. We map the position and shape of the olivine 1 μm absorption band and find that carbonates are found in association with olivine which displays a 1 μm band shifted to long wavelengths. We then use Thermal Emission Imaging Spectrometer (THEMIS) coverage of Nili Fossae and perform tests to investigate whether the long wavelength shifted (redshifted) olivine signature is correlated with high thermal inertia outcrops. We find that there is no consistent correlation between thermal inertia and the unique olivine signature. We discuss a range of formation scenarios for the olivine and carbonate associations, including the possibility that these lithologies are products of serpentinization reactions on early Mars. These lithologies provide an opportunity for deepening our understanding of early Mars and, given their antiquity, may provide a framework to study the timing of valley networks and the thermal history of the Martian crust and interior from the early Noachian to today.
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Affiliation(s)
| | - C. E. Viviano
- Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA
| | - T. A. Goudge
- Department of Geological Sciences, Jackson School of Geosciences, The University of Texas at Austin, Austin, TX, USA
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10
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Seto M, Noguchi K, Cappellen PV. Potential for Aerobic Methanotrophic Metabolism on Mars. ASTROBIOLOGY 2019; 19:1187-1195. [PMID: 31173512 PMCID: PMC6785171 DOI: 10.1089/ast.2018.1943] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 08/20/2018] [Accepted: 05/07/2019] [Indexed: 06/09/2023]
Abstract
Observational evidence supports the presence of methane (CH4) in the martian atmosphere on the order of parts per billion by volume (ppbv). Here, we assess whether aerobic methanotrophy is a potentially viable metabolism in the martian upper regolith, by calculating metabolic energy gain rates under assumed conditions of martian surface temperature, pressure, and atmospheric composition. Using kinetic parameters for 19 terrestrial aerobic methanotrophic strains, we show that even under the imposed low temperature and pressure extremes (180-280 K and 6-11 hPa), methane oxidation by oxygen (O2) should in principle be able to generate the minimum energy production rate required to support endogenous metabolism (i.e., cellular maintenance). Our results further indicate that the corresponding metabolic activity would be extremely low, with cell doubling times in excess of 4000 Earth years at the present-day ppbv-level CH4 mixing ratios in the atmosphere of Mars. Thus, while aerobic methanotrophic microorganisms similar to those found on Earth could theoretically maintain their vital functions, they are unlikely to constitute prolific members of hypothetical martian soil communities.
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Affiliation(s)
- Mayumi Seto
- Department of Chemistry, Biology, and Environmental Sciences, Faculty of Science, Nara Women's University, Nara, Japan
| | - Katsuyuki Noguchi
- Department of Chemistry, Biology, and Environmental Sciences, Faculty of Science, Nara Women's University, Nara, Japan
| | - Philippe Van Cappellen
- Ecohydrology Research Group, Department of Earth and Environmental Sciences, Water Institute, University of Waterloo, Waterloo, Canada
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11
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Aerts JW, van Spanning RJM, Flahaut J, Molenaar D, Bland PA, Genge MJ, Ehrenfreund P, Martins Z. Microbial Communities in Sediments From Four Mildly Acidic Ephemeral Salt Lakes in the Yilgarn Craton (Australia) - Terrestrial Analogs to Ancient Mars. Front Microbiol 2019; 10:779. [PMID: 31133990 PMCID: PMC6512757 DOI: 10.3389/fmicb.2019.00779] [Citation(s) in RCA: 10] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/05/2018] [Accepted: 03/27/2019] [Indexed: 11/24/2022] Open
Abstract
The Yilgarn Craton in Australia has a large number of naturally occurring shallow ephemeral lakes underlain by a dendritic system of paleodrainage channels. Processes like evaporation, flooding, erosion, as well as inflow of saline, often acidic and ion-rich groundwater contribute to the (dynamic) nature of the lakes and the composition of the sediments. The region has previously been described as an analog environment for early Mars due to its geological and geophysical similarities. Here, we investigated sediment samples of four lake environments aimed at getting a fundamental understanding of the native microbial communities and the mineralogical and (bio)chemical composition of the sediments they are associated with. The dominant mineral phases in the sediments were quartz, feldspars and amphiboles, while halite and gypsum were the only evaporites detected. Element analysis revealed a rich and complex image, in which silicon, iron, and aluminum were the dominant ions, but relative high concentrations of trace elements such as strontium, chromium, zirconium, and barium were also found. The concentrations of organic carbon, nitrogen, and phosphorus were generally low. 16S amplicon sequencing on the Illumina platform showed the presence of diverse microbial communities in all four lake environments. We found that most of the communities were dominated by extremely halophilic Archaea of the Halobacteriaceae family. The dynamic nature of these lakes appears to influence the biological, biochemical, and geological components of the ecosystem to a large effect. Inter- and intra-lake variations in the distributions of microbial communities were significant, and could only to a minor degree be explained by underlying environmental conditions. The communities are likely significantly influenced by small scale local effects caused by variations in geological settings and dynamic interactions caused by aeolian transport and flooding and evaporation events.
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Affiliation(s)
- Joost W Aerts
- Department of Molecular Cell Biology, Vrije Universiteit Amsterdam, Amsterdam, Netherlands
| | - Rob J M van Spanning
- Department of Molecular Cell Biology, Vrije Universiteit Amsterdam, Amsterdam, Netherlands
| | - Jessica Flahaut
- Centre de Recherches Pétrographiques et Géochimiques, Centre National de la Recherche Scientifique/Université de Lorraine, Vandœuvre-lès-Nancy, France
| | - Douwe Molenaar
- Department of Molecular Cell Biology, Vrije Universiteit Amsterdam, Amsterdam, Netherlands
| | - Phil A Bland
- Department of Applied Geology, Curtin University, Perth, WA, Australia
| | - Matt J Genge
- Department of Earth Science and Engineering, Faculty of Engineering, Imperial College London, London, United Kingdom
| | - Pascale Ehrenfreund
- Leiden Observatory, Leiden University, Leiden, Netherlands.,Space Policy Institute, Elliott School of International Affairs, George Washington University, Washington, DC, United States
| | - Zita Martins
- Centro de Química-Física Molecular-Institute of Nanoscience and Nanotechnology (CQFM-IN), Institute for Bioengineering and Biosciences (iBB), Departamento de Engenharia Química, Instituto Superior Técnico (IST), Universidade de Lisboa, Lisbon, Portugal
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12
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Tosca NJ, Ahmed IA, Tutolo BM, Ashpitel A, Hurowitz JA. Magnetite Authigenesis and the Warming of Early Mars. NATURE GEOSCIENCE 2018; 11:635-639. [PMID: 30123317 PMCID: PMC6092749 DOI: 10.1038/s41561-018-0203-8] [Citation(s) in RCA: 13] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/12/2018] [Accepted: 07/10/2018] [Indexed: 05/14/2023]
Abstract
The Curiosity rover has documented lacustrine sediments at Gale Crater, but how liquid water became physically stable on the early Martian surface is a matter of significant debate. To constrain the composition of the early Martian atmosphere during sediment deposition, we experimentally investigated the nucleation and growth kinetics of authigenic Fe-minerals in Gale Crater mudstones. Experiments show that pH variations within anoxic basaltic waters trigger a series of mineral transformations that rapidly generate magnetite and H2(aq). Magnetite continues to form through this mechanism despite high PCO2 and supersaturation with respect to Fe-carbonate minerals. Reactive transport simulations that incorporate these experimental data show that groundwater infiltration into a lake equilibrated with a CO2-rich atmosphere can trigger the production of both magnetite and H2(aq) in the mudstones. H2(aq), generated at concentrations that would readily exsolve from solution, is capable of increasing annual mean surface temperatures above freezing in CO2-dominated atmospheres. We therefore suggest that magnetite authigenesis could have provided a short-term feedback for stabilizing liquid water, as well as a principal feedstock for biologically relevant chemical reactions, at the early Martian surface.
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Affiliation(s)
- Nicholas J. Tosca
- Dept. of Earth Sciences, University of Oxford, South Parks Road, Oxford, OX1 3AN, UK
| | - Imad A.M. Ahmed
- Dept. of Earth Sciences, University of Oxford, South Parks Road, Oxford, OX1 3AN, UK
| | - Benjamin M. Tutolo
- Department of Geoscience, University of Calgary, Calgary, AB, T2N 1N4, Canada
| | - Alice Ashpitel
- Dept. of Earth Sciences, University of Oxford, South Parks Road, Oxford, OX1 3AN, UK
| | - Joel A. Hurowitz
- Department of Geosciences, Stony Brook University, Stony Brook, NY 11794-2100, USA
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14
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Abstract
The habitable zone (HZ) is the circular region around a star(s) where standing bodies of water could exist on the surface of a rocky planet. Space missions employ the HZ to select promising targets for follow-up habitability assessment. The classical HZ definition assumes that the most important greenhouse gases for habitable planets orbiting main-sequence stars are CO2 and H2O. Although the classical HZ is an effective navigational tool, recent HZ formulations demonstrate that it cannot thoroughly capture the diversity of habitable exoplanets. Here, I review the planetary and stellar processes considered in both classical and newer HZ formulations. Supplementing the classical HZ with additional considerations from these newer formulations improves our capability to filter out worlds that are unlikely to host life. Such improved HZ tools will be necessary for current and upcoming missions aiming to detect and characterize potentially habitable exoplanets.
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15
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Foley BJ, Smye AJ. Carbon Cycling and Habitability of Earth-Sized Stagnant Lid Planets. ASTROBIOLOGY 2018; 18:873-896. [PMID: 30035642 DOI: 10.1089/ast.2017.1695] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/08/2023]
Abstract
Models of thermal evolution, crustal production, and CO2 cycling are used to constrain the prospects for habitability of rocky planets, with Earth-like size and composition, in the stagnant lid regime. Specifically, we determine the conditions under which such planets can maintain rates of CO2 degassing large enough to prevent global surface glaciation but small enough so as not to exceed the upper limit on weathering rates provided by the supply of fresh rock, a situation which would lead to runaway atmospheric CO2 accumulation and an inhospitably hot climate. The models show that stagnant lid planets with initial radiogenic heating rates of 100-250 TW, and with total CO2 budgets ranging from ∼10-2 to 1 times Earth's estimated CO2 budget, can maintain volcanic outgassing rates suitable for habitability for ≈1-5 Gyr; larger CO2 budgets result in uninhabitably hot climates, while smaller budgets result in global glaciation. High radiogenic heat production rates favor habitability by sustaining volcanism and CO2 outgassing longer. Thus, the results suggest that plate tectonics may not be required for establishing a long-term carbon cycle and maintaining a stable, habitable climate. The model is necessarily highly simplified, as the uncertainties with exoplanet thermal evolution and outgassing are large. Nevertheless, the results provide some first-order guidance for future exoplanet missions, by predicting the age at which habitability becomes unlikely for a stagnant lid planet as a function of initial radiogenic heat budget. This prediction is powerful because both planet heat budget and age can potentially be constrained from stellar observations. Key Words: Exoplanets-Habitability-Stagnant lid tectonics-Carbon cycle-Volcanism. Astrobiology 18, 873-896.
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Affiliation(s)
- Bradford J Foley
- Department of Geosciences, Pennsylvania State University, University Park , Pennsylvania
| | - Andrew J Smye
- Department of Geosciences, Pennsylvania State University, University Park , Pennsylvania
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16
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Hao J, Giovenco E, Pedreira-Segade U, Montagnac G, Daniel I. Compatibility of Amino Acids in Ice Ih: Implications for the Origin of Life. ASTROBIOLOGY 2018; 18:381-392. [PMID: 29620923 DOI: 10.1089/ast.2017.1735] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/08/2023]
Abstract
Icy environments may have been common on early Earth due to the faint young sun. Previous studies have proposed that the formation of large icy bodies in the early ocean could concentrate the building blocks of life in eutectic fluids and, therefore, facilitate the polymerization of monomers. This hypothesis is based on the untested assumption that organic molecules are virtually incompatible in ice Ih (hexagonal ice). In this study, we conducted freezing experiments to explore the partitioning behavior of selected amino acids (AAs; glycine, l-alanine, l-proline, and l-phenylalanine) between ice Ih and aqueous solutions analogous to seawater. We allowed ice crystals to grow slowly from a few seeds in equilibrium with the solution and used Raman spectroscopy to analyze in situ the relative concentrations of AAs in the ice and aqueous solution. During freezing, there was no precipitation of AA crystals, indicating that the concentrations in solution never reached their solubility limit, even when the droplet was mostly frozen. Analyses of the Raman spectra of the ice and eutectic solution suggested that considerable amounts of AAs existed in the ice phase with partition coefficients varying between 0.2 and 0.5. These observations imply little incompatibility of AAs in ice Ih during the freezing of the solutions, rendering the concentration hypothesis in a eutectic system unwarranted. However, incorporation into ice Ih could protect AAs from decomposition or racemization and significantly improve the efficiency of extraterrestrial transport of small organics. Therefore, this study supports the hypothesis of extraterrestrial delivery of organic molecules in icy comets and asteroids to the primitive Earth as suggested by an increasing number of independent observations. Key Words: Ice Ih-Partition coefficient-Amino acids-Polymerization-Extraterrestrial transport of organics. Astrobiology 18, 381-392.
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Affiliation(s)
- Jihua Hao
- Univ Lyon, Université Lyon 1 , Ens de Lyon, CNRS, UMR 5276 LGL-TPE, Villeurbanne, France
| | - Elena Giovenco
- Univ Lyon, Université Lyon 1 , Ens de Lyon, CNRS, UMR 5276 LGL-TPE, Villeurbanne, France
| | - Ulysse Pedreira-Segade
- Univ Lyon, Université Lyon 1 , Ens de Lyon, CNRS, UMR 5276 LGL-TPE, Villeurbanne, France
| | - Gilles Montagnac
- Univ Lyon, Université Lyon 1 , Ens de Lyon, CNRS, UMR 5276 LGL-TPE, Villeurbanne, France
| | - Isabelle Daniel
- Univ Lyon, Université Lyon 1 , Ens de Lyon, CNRS, UMR 5276 LGL-TPE, Villeurbanne, France
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17
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Jakosky BM, Slipski M, Benna M, Mahaffy P, Elrod M, Yelle R, Stone S, Alsaeed N. Mars' atmospheric history derived from upper-atmosphere measurements of 38Ar/ 36Ar. Science 2017; 355:1408-1410. [PMID: 28360326 DOI: 10.1126/science.aai7721] [Citation(s) in RCA: 155] [Impact Index Per Article: 22.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/09/2016] [Accepted: 03/06/2017] [Indexed: 11/02/2022]
Abstract
The history of Mars' atmosphere is important for understanding the geological evolution and potential habitability of the planet. We determine the amount of gas lost to space through time using measurements of the upper-atmospheric structure made by the Mars Atmosphere and Volatile Evolution (MAVEN) spacecraft. We derive the structure of 38Ar/36Ar between the homopause and exobase altitudes. Fractionation of argon occurs as a result of loss of gas to space by pickup-ion sputtering, which preferentially removes the lighter atom. The measurements require that 66% of the atmospheric argon has been lost to space. Thus, a large fraction of Mars' atmospheric gas has been lost to space, contributing to the transition in climate from an early, warm, wet environment to today's cold, dry atmosphere.
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Affiliation(s)
| | - M Slipski
- University of Colorado, Boulder, CO, USA
| | - M Benna
- NASA/Goddard Spaceflight Center, Greenbelt, MD, USA
| | - P Mahaffy
- NASA/Goddard Spaceflight Center, Greenbelt, MD, USA
| | - M Elrod
- NASA/Goddard Spaceflight Center, Greenbelt, MD, USA
| | - R Yelle
- University of Arizona, Tucson, AZ, USA
| | - S Stone
- University of Arizona, Tucson, AZ, USA
| | - N Alsaeed
- University of Colorado, Boulder, CO, USA.,American University of Sharjah, Sharjah, United Arab Emirates
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18
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Beblo-Vranesevic K, Bohmeier M, Perras AK, Schwendner P, Rabbow E, Moissl-Eichinger C, Cockell CS, Pukall R, Vannier P, Marteinsson VT, Monaghan EP, Ehrenfreund P, Garcia-Descalzo L, Gómez F, Malki M, Amils R, Gaboyer F, Westall F, Cabezas P, Walter N, Rettberg P. The responses of an anaerobic microorganism, Yersinia intermedia MASE-LG-1 to individual and combined simulated Martian stresses. PLoS One 2017; 12:e0185178. [PMID: 29069099 PMCID: PMC5656303 DOI: 10.1371/journal.pone.0185178] [Citation(s) in RCA: 10] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Abstract] [MESH Headings] [Grants] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/03/2017] [Accepted: 09/07/2017] [Indexed: 11/18/2022] Open
Abstract
The limits of life of aerobic microorganisms are well understood, but the responses of anaerobic microorganisms to individual and combined extreme stressors are less well known. Motivated by an interest in understanding the survivability of anaerobic microorganisms under Martian conditions, we investigated the responses of a new isolate, Yersinia intermedia MASE-LG-1 to individual and combined stresses associated with the Martian surface. This organism belongs to an adaptable and persistent genus of anaerobic microorganisms found in many environments worldwide. The effects of desiccation, low pressure, ionizing radiation, varying temperature, osmotic pressure, and oxidizing chemical compounds were investigated. The strain showed a high tolerance to desiccation, with a decline of survivability by four orders of magnitude during a storage time of 85 days. Exposure to X-rays resulted in dose-dependent inactivation for exposure up to 600 Gy while applied doses above 750 Gy led to complete inactivation. The effects of the combination of desiccation and irradiation were additive and the survivability was influenced by the order in which they were imposed. Ionizing irradiation and subsequent desiccation was more deleterious than vice versa. By contrast, the presence of perchlorates was not found to significantly affect the survival of the Yersinia strain after ionizing radiation. These data show that the organism has the capacity to survive and grow in physical and chemical stresses, imposed individually or in combination that are associated with Martian environment. Eventually it lost its viability showing that many of the most adaptable anaerobic organisms on Earth would be killed on Mars today.
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Affiliation(s)
- Kristina Beblo-Vranesevic
- Radiation Biology Department, Institute of Aerospace Medicine, German Aerospace Center (DLR), Cologne, Germany
- * E-mail:
| | - Maria Bohmeier
- Radiation Biology Department, Institute of Aerospace Medicine, German Aerospace Center (DLR), Cologne, Germany
| | - Alexandra K. Perras
- Department of Internal Medicine, Medical University of Graz, Graz, Austria
- Department of Microbiology and Archaea, University of Regensburg, Regensburg, Germany
| | - Petra Schwendner
- School of Physics and Astronomy, UK Center for Astrobiology, University of Edinburgh, Edinburgh, United Kingdom
| | - Elke Rabbow
- Radiation Biology Department, Institute of Aerospace Medicine, German Aerospace Center (DLR), Cologne, Germany
| | - Christine Moissl-Eichinger
- Department of Internal Medicine, Medical University of Graz, Graz, Austria
- BioTechMed Graz, Graz, Austria
| | - Charles S. Cockell
- School of Physics and Astronomy, UK Center for Astrobiology, University of Edinburgh, Edinburgh, United Kingdom
| | - Rüdiger Pukall
- German Collection of Microorganisms and Cell Cultures, Leibniz Institute DSMZ, Braunschweig, Germany
| | | | - Viggo T. Marteinsson
- MATIS—Prokaria, Reykjavík, Iceland
- Faculty of Food Science and Nutrition, University of Iceland, Reykjavík, Iceland
| | | | - Pascale Ehrenfreund
- Leiden Observatory, Universiteit Leiden, Leiden, Netherland
- Space Policy Institute, George Washington University, Washington DC, United States of America
| | - Laura Garcia-Descalzo
- Instituto Nacional de Técnica Aeroespacial—Centro de Astrobiología (INTA-CAB), Madrid, Spain
| | - Felipe Gómez
- Instituto Nacional de Técnica Aeroespacial—Centro de Astrobiología (INTA-CAB), Madrid, Spain
| | | | | | - Frédéric Gaboyer
- Centre de Biophysique Moléculaire, Centre National de la Recherche Scientifique (CNRS), Orléans, France
| | - Frances Westall
- Centre de Biophysique Moléculaire, Centre National de la Recherche Scientifique (CNRS), Orléans, France
| | | | | | - Petra Rettberg
- Radiation Biology Department, Institute of Aerospace Medicine, German Aerospace Center (DLR), Cologne, Germany
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19
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Mickol RL, Page JL, Schuerger AC. Magnesium Sulfate Salt Solutions and Ices Fail to Protect Serratia liquefaciens from the Biocidal Effects of UV Irradiation under Martian Conditions. ASTROBIOLOGY 2017; 17:401-412. [PMID: 28459604 DOI: 10.1089/ast.2015.1448] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/07/2023]
Abstract
The growth of Serratia liquefaciens has been demonstrated under martian conditions of 0.7 kPa (7 mbar), 0°C, and CO2-enriched anoxic atmospheres (Schuerger et al., 2013, Astrobiology 13:115-131), but studies into the survivability of cells under hypersaline conditions that are likely to be encountered on Mars are lacking. Serratia liquefaciens cells were suspended in aqueous MgSO4 solutions, or frozen brines, and exposed to terrestrial (i.e., 101.3 kPa, 24°C, O2/N2-normal atmosphere) or martian (i.e., 0.7 kPa, -25°C, CO2-anoxic atmosphere) conditions to assess the roles of MgSO4 and UV irradiation on the survival of S. liquefaciens. Four solutions were tested for their capability to attenuate martian UV irradiation in both liquid and frozen forms: sterile deionized water (SDIW), 10 mM PO4 buffer, 5% MgSO4, and 10% MgSO4. None of the solutions in either liquid or frozen forms provided enhanced protection against martian UV irradiation. Sixty minutes of UV irradiation reduced cell densities from 2.0 × 106 cells/mL to less than 10 cells/mL for both liquid and frozen solutions. In contrast, 3-4 mm of a Mars analog soil were sufficient to attenuate 100% of UV irradiation. Results suggest that terrestrial microorganisms may not survive on Sun-exposed surfaces on Mars, even if the cells are embedded in frozen martian brines composed of MgSO4. However, if dispersed microorganisms can be covered by only a few millimeters of dust or regolith, long-term survival is probable. Key Words: Hypobaria-Mars-Planetary protection-Brines. Astrobiology 17, 401-412.
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Affiliation(s)
- Rebecca L Mickol
- 1 Center for Space and Planetary Sciences, University of Arkansas , Fayetteville, Arkansas
| | - Jessica L Page
- 2 Department of Physics and Space Science, Florida Institute of Technology , Melbourne, Florida
| | - Andrew C Schuerger
- 3 Department of Plant Pathology, University of Florida , Gainesville, Florida
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20
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Colangelo-Lillis J, Eicken H, Carpenter SD, Deming JW. Evidence for marine origin and microbial-viral habitability of sub-zero hypersaline aqueous inclusions within permafrost near Barrow, Alaska. FEMS Microbiol Ecol 2016; 92:fiw053. [PMID: 26976841 DOI: 10.1093/femsec/fiw053] [Citation(s) in RCA: 23] [Impact Index Per Article: 2.9] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Accepted: 03/05/2016] [Indexed: 11/12/2022] Open
Abstract
Cryopegs are sub-surface hypersaline brines at sub-zero temperatures within permafrost; their global extent and distribution are unknown. The permafrost barrier to surface and groundwater advection maintains these brines as semi-isolated systems over geological time. A cryopeg 7 m below ground near Barrow, Alaska, was sampled for geochemical and microbiological analysis. Sub-surface brines (in situtemperature of -6 °C, salinity of 115 ppt), and an associated sediment-infused ice wedge (melt salinity of 0.04 ppt) were sampled using sterile technique. Major ionic concentrations in the brine corresponded more closely to other (Siberian) cryopegs than to Standard seawater or the ice wedge. Ionic ratios and stable isotope analysis of water conformed to a marine or brackish origin with subsequent Rayleigh fractionation. The brine contained ∼1000× more bacteria than surrounding ice, relatively high viral numbers suggestive of infection and reproduction, and an unusually high ratio of particulate to dissolved extracellular polysaccharide substances. A viral metagenome indicated a high frequency of temperate viruses and limited viral diversity compared to surface environments, with closest similarity to low water activity environments. Interpretations of the results underscore the isolation of these underexplored microbial ecosystems from past and present oceans.
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Affiliation(s)
- J Colangelo-Lillis
- School of Oceanography and Astrobiology Program, University of Washington, Seattle, WA, 98195, USA
| | - H Eicken
- International Arctic Research Center, University of Alaska Fairbanks, Fairbanks, AK, 99775, USA
| | - S D Carpenter
- School of Oceanography and Astrobiology Program, University of Washington, Seattle, WA, 98195, USA
| | - J W Deming
- School of Oceanography and Astrobiology Program, University of Washington, Seattle, WA, 98195, USA
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Read PL, Lewis SR, Mulholland DP. The physics of Martian weather and climate: a review. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2015; 78:125901. [PMID: 26534887 DOI: 10.1088/0034-4885/78/12/125901] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/16/2023]
Abstract
The planet Mars hosts an atmosphere that is perhaps the closest in terms of its meteorology and climate to that of the Earth. But Mars differs from Earth in its greater distance from the Sun, its smaller size, its lack of liquid oceans and its thinner atmosphere, composed mainly of CO(2). These factors give Mars a rather different climate to that of the Earth. In this article we review various aspects of the martian climate system from a physicist's viewpoint, focusing on the processes that control the martian environment and comparing these with corresponding processes on Earth. These include the radiative and thermodynamical processes that determine the surface temperature and vertical structure of the atmosphere, the fluid dynamics of its atmospheric motions, and the key cycles of mineral dust and volatile transport. In many ways, the climate of Mars is as complicated and diverse as that of the Earth, with complex nonlinear feedbacks that affect its response to variations in external forcing. Recent work has shown that the martian climate is anything but static, but is almost certainly in a continual state of transient response to slowly varying insolation associated with cyclic variations in its orbit and rotation. We conclude with a discussion of the physical processes underlying these long- term climate variations on Mars, and an overview of some of the most intriguing outstanding problems that should be a focus for future observational and theoretical studies.
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Affiliation(s)
- P L Read
- Atmospheric, Oceanic & Planetary Physics, University of Oxford, Clarendon Laboratory, Parks Road, Oxford, OX1 3PU, UK
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22
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Baker VR, Hamilton CW, Burr DM, Gulick VC, Komatsu G, Luo W, Rice JW, Rodriguez J. Fluvial geomorphology on Earth-like planetary surfaces: A review. GEOMORPHOLOGY (AMSTERDAM, NETHERLANDS) 2015; 245:149-182. [PMID: 29176917 PMCID: PMC5701759 DOI: 10.1016/j.geomorph.2015.05.002] [Citation(s) in RCA: 8] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/07/2023]
Abstract
Morphological evidence for ancient channelized flows (fluvial and fluvial-like landforms) exists on the surfaces of all of the inner planets and on some of the satellites of the Solar System. In some cases, the relevant fluid flows are related to a planetary evolution that involves the global cycling of a volatile component (water for Earth and Mars; methane for Saturn's moon Titan). In other cases, as on Mercury, Venus, Earth's moon, and Jupiter's moon Io, the flows were of highly fluid lava. The discovery, in 1972, of what are now known to be fluvial channels and valleys on Mars sparked a major controversy over the role of water in shaping the surface of that planet. The recognition of the fluvial character of these features has opened unresolved fundamental questions about the geological history of water on Mars, including the presence of an ancient ocean and the operation of a hydrological cycle during the earliest phases of planetary history. Other fundamental questions posed by fluvial and fluvial-like features on planetary bodies include the possible erosive action of large-scale outpourings of very fluid lavas, such as those that may have produced the remarkable canali forms on Venus; the ability of exotic fluids, such as methane, to create fluvial-like landforms, as observed on Saturn's moon, Titan; and the nature of sedimentation and erosion under different conditions of planetary surface gravity. Planetary fluvial geomorphology also illustrates fundamental epistemological and methodological issues, including the role of analogy in geomorphological/geological inquiry.
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Affiliation(s)
- Victor R. Baker
- Department of Hydrology and Water Resources, University of Arizona, Tucson, AZ 85721, USA
- Lunar and Planetary Laboratory, Department of Planetary Sciences, University of Arizona, Tucson, AZ 85721, USA
| | - Christopher W. Hamilton
- Lunar and Planetary Laboratory, Department of Planetary Sciences, University of Arizona, Tucson, AZ 85721, USA
| | - Devon M. Burr
- Earth and Planetary Sciences Department, University of Tennessee-Knoxville, Knoxville, TN 37996-1410, USA
| | - Virginia C. Gulick
- SETI Institute, Mountain View, CA 94043, USA
- NASA Ames Research Center, MS 239-20, Moffett Field, CA 94035, USA
| | - Goro Komatsu
- International Research School of Planetary Sciences, Università d’Annunzio, Viale Pindaro 42, 65127 Pescara, Italy
| | - Wei Luo
- Department of Geography, Northern Illinois University, DeKalb, IL 60115, USA
| | | | - J.A.P. Rodriguez
- NASA Ames Research Center, MS 239-20, Moffett Field, CA 94035, USA
- Planetary Science Institute, Tucson, AZ 85719, USA
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Misra A, Krissansen-Totton J, Koehler MC, Sholes S. Transient Sulfate Aerosols as a Signature of Exoplanet Volcanism. ASTROBIOLOGY 2015; 15:462-477. [PMID: 26053611 DOI: 10.1089/ast.2014.1204] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/04/2023]
Abstract
Geological activity is thought to be important for the origin of life and for maintaining planetary habitability. We show that transient sulfate aerosols could be a signature of exoplanet volcanism and therefore of a geologically active world. A detection of transient aerosols, if linked to volcanism, could thus aid in habitability evaluations of the exoplanet. On Earth, subduction-induced explosive eruptions inject SO2 directly into the stratosphere, leading to the formation of sulfate aerosols with lifetimes of months to years. We demonstrate that the rapid increase and gradual decrease in sulfate aerosol loading associated with these eruptions may be detectable in transit transmission spectra with future large-aperture telescopes, such as the James Webb Space Telescope (JWST) and European Extremely Large Telescope (E-ELT), for a planetary system at a distance of 10 pc, assuming an Earth-like atmosphere, bulk composition, and size. Specifically, we find that a signal-to-noise ratio of 12.1 and 7.1 could be achieved with E-ELT (assuming photon-limited noise) for an Earth analogue orbiting a Sun-like star and M5V star, respectively, even without multiple transits binned together. We propose that the detection of this transient signal would strongly suggest an exoplanet volcanic eruption, if potential false positives such as dust storms or bolide impacts can be ruled out. Furthermore, because scenarios exist in which O2 can form abiotically in the absence of volcanic activity, a detection of transient aerosols that can be linked to volcanism, along with a detection of O2, would be a more robust biosignature than O2 alone.
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Affiliation(s)
- Amit Misra
- 1 Department of Astronomy, University of Washington , Seattle, Washington
- 2 University of Washington Astrobiology Program, University of Washington , Seattle, Washington
| | - Joshua Krissansen-Totton
- 2 University of Washington Astrobiology Program, University of Washington , Seattle, Washington
- 3 Department of Earth and Space Sciences, University of Washington , Seattle, Washington
| | - Matthew C Koehler
- 2 University of Washington Astrobiology Program, University of Washington , Seattle, Washington
- 3 Department of Earth and Space Sciences, University of Washington , Seattle, Washington
| | - Steven Sholes
- 2 University of Washington Astrobiology Program, University of Washington , Seattle, Washington
- 3 Department of Earth and Space Sciences, University of Washington , Seattle, Washington
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Aerts JW, Röling WFM, Elsaesser A, Ehrenfreund P. Biota and biomolecules in extreme environments on Earth: implications for life detection on Mars. Life (Basel) 2014; 4:535-65. [PMID: 25370528 PMCID: PMC4284457 DOI: 10.3390/life4040535] [Citation(s) in RCA: 23] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/07/2014] [Revised: 09/08/2014] [Accepted: 09/16/2014] [Indexed: 11/24/2022] Open
Abstract
The three main requirements for life as we know it are the presence of organic compounds, liquid water, and free energy. Several groups of organic compounds (e.g., amino acids, nucleobases, lipids) occur in all life forms on Earth and are used as diagnostic molecules, i.e., biomarkers, for the characterization of extant or extinct life. Due to their indispensability for life on Earth, these biomarkers are also prime targets in the search for life on Mars. Biomarkers degrade over time; in situ environmental conditions influence the preservation of those molecules. Nonetheless, upon shielding (e.g., by mineral surfaces), particular biomarkers can persist for billions of years, making them of vital importance in answering questions about the origins and limits of life on early Earth and Mars. The search for organic material and biosignatures on Mars is particularly challenging due to the hostile environment and its effect on organic compounds near the surface. In support of life detection on Mars, it is crucial to investigate analogue environments on Earth that resemble best past and present Mars conditions. Terrestrial extreme environments offer a rich source of information allowing us to determine how extreme conditions affect life and molecules associated with it. Extremophilic organisms have adapted to the most stunning conditions on Earth in environments with often unique geological and chemical features. One challenge in detecting biomarkers is to optimize extraction, since organic molecules can be low in abundance and can strongly adsorb to mineral surfaces. Methods and analytical tools in the field of life science are continuously improving. Amplification methods are very useful for the detection of low concentrations of genomic material but most other organic molecules are not prone to amplification methods. Therefore, a great deal depends on the extraction efficiency. The questions “what to look for”, “where to look”, and “how to look for it” require more of our attention to ensure the success of future life detection missions on Mars.
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Affiliation(s)
- Joost W Aerts
- Molecular Cell Physiology, Faculty of Earth and Life Sciences, VU University Amsterdam, de Boelelaan 1085, 1081 HV Amsterdam, The Netherlands.
| | - Wilfred F M Röling
- Molecular Cell Physiology, Faculty of Earth and Life Sciences, VU University Amsterdam, de Boelelaan 1085, 1081 HV Amsterdam, The Netherlands.
| | - Andreas Elsaesser
- Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands.
| | - Pascale Ehrenfreund
- Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands.
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Tomkinson T, Lee MR, Mark DF, Smith CL. Sequestration of Martian CO2 by mineral carbonation. Nat Commun 2014; 4:2662. [PMID: 24149494 PMCID: PMC4354006 DOI: 10.1038/ncomms3662] [Citation(s) in RCA: 17] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/11/2013] [Accepted: 09/24/2013] [Indexed: 12/03/2022] Open
Abstract
Carbonation is the water-mediated replacement of silicate minerals, such as olivine, by carbonate, and is commonplace in the Earth’s crust. This reaction can remove significant quantities of CO2 from the atmosphere and store it over geological timescales. Here we present the first direct evidence for CO2 sequestration and storage on Mars by mineral carbonation. Electron beam imaging and analysis show that olivine and a plagioclase feldspar-rich mesostasis in the Lafayette meteorite have been replaced by carbonate. The susceptibility of olivine to replacement was enhanced by the presence of smectite veins along which CO2-rich fluids gained access to grain interiors. Lafayette was partially carbonated during the Amazonian, when liquid water was available intermittently and atmospheric CO2 concentrations were close to their present-day values. Earlier in Mars’ history, when the planet had a much thicker atmosphere and an active hydrosphere, carbonation is likely to have been an effective mechanism for sequestration of CO2. The mechanism by which Mars lost its early dense and carbon dioxide-rich atmosphere remains relatively unknown. Here, via mineralogical analysis of the Lafayette Martian meteorite, Tomkinson et al. infer that carbonation was an effective carbon dioxide sequestration mechanism on an early, water-rich Mars.
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Affiliation(s)
- Tim Tomkinson
- Scottish Universities Environmental Research Centre, Rankine Avenue, Scottish Enterprise Technology Park, East Kilbride G75 0QF, UK
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Groemer G, Foresta L, Turetschek T, Bothe C, Boyd A, Dinkelaker A, Dissertori M, Fasching D, Fischer M, Föger D, Frischauf N, Fritsch L, Fuchs H, Gautsch C, Gerard S, Goetzloff L, Gołebiowska I, Gorur P, Groemer G, Groll P, Haider C, Haider O, Hauth E, Hauth S, Hettrich S, Jais W, Jones N, Taj-Eddine K, Karl A, Kauerhoff T, Khan MS, Kjeldsen A, Klauck J, Losiak A, Luger M, Luger T, Luger U, McArthur J, Moser L, Neuner J, Orgel C, Ori GG, Paternesi R, Peschier J, Pfeil I, Prock S, Radinger J, Ragonig C, Ramirez B, Ramo W, Rampey M, Sams A, Sams E, Sams S, Sandu O, Sans A, Sansone P, Scheer D, Schildhammer D, Scornet Q, Sejkora N, Soucek A, Stadler A, Stummer F, Stumptner W, Taraba M, Tlustos R, Toferer E, Winter E, Zanella-Kux K. A case for using ground-based thermal inertia measurements to detect Martian caves. ASTROBIOLOGY 2014; 14:431-437. [PMID: 24823802 DOI: 10.1089/ast.2013.1063] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/03/2023]
Abstract
Martian caves are regarded as one of the most interesting locations in which to search for life on the planet. Data obtained during the MARS2013 expedition at Hamar Laghdad Ridge in the Tafilalt region of Morocco indicate that even small cavities can display thermal behavior that is characteristic for caves. For example, temperature in a cavity equaled 14°C±0.1°C before sunrise, which was higher than the temperature of the ambient air (10°C±0.1°C) and proximate rocks (9°C±0.1°C) at the same time. Within 30 min after sunrise, when the temperature of surrounding rocks corresponded to 15°C, this thermal relationship reversed. Measurements were conducted under simulated spaceflight conditions, including near-real-time interpretation of data that were acquired in a complex flight planning environment. We conclude that using ground-based thermal contrast measurements, in 7-14 μm band before and after sunset, is an effective method for Mars astronauts to identify caves, possibly superior to usage of space-based or ground-penetrating data.
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Affiliation(s)
- Gernot Groemer
- 1 Austrian Space Forum, Innsbruck Office , Innsbruck, Austria
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Forget F, Leconte J. Possible climates on terrestrial exoplanets. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2014; 372:20130084. [PMID: 24664919 DOI: 10.1098/rsta.2013.0084] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/03/2023]
Abstract
What kind of environment may exist on terrestrial planets around other stars? In spite of the lack of direct observations, it may not be premature to speculate on exoplanetary climates, for instance, to optimize future telescopic observations or to assess the probability of habitable worlds. To begin with, climate primarily depends on (i) the atmospheric composition and the volatile inventory; (ii) the incident stellar flux; and (iii) the tidal evolution of the planetary spin, which can notably lock a planet with a permanent night side. The atmospheric composition and mass depends on complex processes, which are difficult to model: origins of volatiles, atmospheric escape, geochemistry, photochemistry, etc. We discuss physical constraints, which can help us to speculate on the possible type of atmosphere, depending on the planet size, its final distance for its star and the star type. Assuming that the atmosphere is known, the possible climates can be explored using global climate models analogous to the ones developed to simulate the Earth as well as the other telluric atmospheres in the solar system. Our experience with Mars, Titan and Venus suggests that realistic climate simulators can be developed by combining components, such as a 'dynamical core', a radiative transfer solver, a parametrization of subgrid-scale turbulence and convection, a thermal ground model and a volatile phase change code. On this basis, we can aspire to build reliable climate predictors for exoplanets. However, whatever the accuracy of the models, predicting the actual climate regime on a specific planet will remain challenging because climate systems are affected by strong positive feedbacks. They can drive planets with very similar forcing and volatile inventory to completely different states. For instance, the coupling among temperature, volatile phase changes and radiative properties results in instabilities, such as runaway glaciations and runaway greenhouse effect.
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Affiliation(s)
- F Forget
- Laboratoire de Météorologie Dynamique, IPSL, Paris, France
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Craddock RA, Maxwell TA. Geomorphic evolution of the Martian highlands through ancient fluvial processes. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/92je02508] [Citation(s) in RCA: 194] [Impact Index Per Article: 16.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Scott VJ, Tse M, Shearn MJ, Siegel PH, Amashukeli X. An RF-powered micro-reactor for the detection of astrobiological target molecules on planetary bodies. THE REVIEW OF SCIENTIFIC INSTRUMENTS 2012; 83:084102. [PMID: 22938313 DOI: 10.1063/1.4746994] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/01/2023]
Abstract
We describe a sample-processing micro-reactor that utilizes 60 GHz RF radiation with approximately 730 mW of output power. The instrument design and performance characterization are described and then illustrated with modeling and experimental studies. The micro-reactor's efficiency on affecting hydrolysis of chemical bonds similar to those within large complex molecules was demonstrated: a disaccharide-sucrose-was hydrolyzed completely under micro-reactor conditions. The products of the micro-reactor-facilitated hydrolysis were analyzed using mass spectroscopy and proton nuclear magnetic resonance analytical techniques.
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Affiliation(s)
- Valerie J Scott
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA
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Kereszturi A. Review of wet environment types on Mars with focus on duration and volumetric issues. ASTROBIOLOGY 2012; 12:586-600. [PMID: 22794300 DOI: 10.1089/ast.2011.0686] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/01/2023]
Abstract
The astrobiological significance of certain environment types on Mars strongly depends on the temperature, duration, and chemistry of liquid water that was present there in the past. Recent works have focused on the identification of signs of ancient water on Mars, as it is more difficult to estimate the above-mentioned parameters. In this paper, two important factors are reviewed, the duration and the volume of water at different environment types on past and present Mars. Using currently available information, we can only roughly estimate these values, but as environment types show characteristic differences in this respect, it is worth comparing them and the result may have importance for research in astrobiology. Impact-induced and geothermal hydrothermal systems, lakes, and valley networks were in existence on Mars over the course of from 10(2) to 10(6) years, although they would have experienced substantially different temperature regimes. Ancient oceans, as well as water in outflow channels and gullies, and at the microscopic scale as interfacial water layers, would have had inherently different times of duration and overall volume: oceans may have endured from 10(4) to 10(6) years, while interfacial water would have had the smallest volume and residence time of liquid phase on Mars. Martian wet environments with longer residence times of liquid water are believed to have existed for that amount of time necessary for life to develop on Earth between the Late Heavy Bombardment and the age of the earliest fossil record. The results of this review show the necessity for more detailed analysis of conditions within geothermal heat-induced systems to reconstruct the conditions during weathering and mineral alteration, as well as to search for signs of reoccurring wet periods in ancient crater lakes.
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Affiliation(s)
- Akos Kereszturi
- Konkoly Thege Miklos Astronomical Institute, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, Budapest, Hungary.
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Direito SOL, Marees A, Röling WFM. Sensitive life detection strategies for low-biomass environments: optimizing extraction of nucleic acids adsorbing to terrestrial and Mars analogue minerals. FEMS Microbiol Ecol 2012; 81:111-23. [PMID: 22329626 DOI: 10.1111/j.1574-6941.2012.01325.x] [Citation(s) in RCA: 48] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/30/2011] [Revised: 01/19/2012] [Accepted: 01/31/2012] [Indexed: 11/29/2022] Open
Abstract
The adsorption of nucleic acids to mineral matrixes can result in low extraction yields and negatively influences molecular microbial ecology studies, in particular for low-biomass environments on Earth and Mars. We determined the recovery of nucleic acids from a range of minerals relevant to Earth and Mars. Clay minerals, but also other silicates and nonsilicates, showed very low recovery (< 1%). Consequently, optimization of DNA extraction was directed towards clays. The high temperatures and acidic conditions used in some methods to dissolve mineral matrices proved to destruct DNA. The most efficient method comprised a high phosphate solution (P/EtOH; 1 M phosphate, 15% ethanol buffer at pH 8) introduced at the cell-lysing step in DNA extraction, to promote chemical competition with DNA for adsorption sites. This solution increased DNA yield from clay samples spiked with known quantities of cells up to nearly 100-fold. DNA recovery was also enhanced from several mineral samples retrieved from an aquifer, while maintaining reproducible DGGE profiles. DGGE profiles were obtained for a clay sample for which no profile could be generated with the standard DNA isolation protocol. Mineralogy influenced microbial community composition. The method also proved suitable for the recovery of low molecular weight DNA (< 1.5 kb).
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Affiliation(s)
- Susana O L Direito
- Molecular Cell Physiology, Faculty of Earth and Life Sciences, VU University Amsterdam, Amsterdam, The Netherlands
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Schuttlefield JD, Sambur JB, Gelwicks M, Eggleston CM, Parkinson BA. Photooxidation of chloride by oxide minerals: implications for perchlorate on Mars. J Am Chem Soc 2011; 133:17521-3. [PMID: 21961793 DOI: 10.1021/ja2064878] [Citation(s) in RCA: 55] [Impact Index Per Article: 4.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/28/2022]
Abstract
We show that highly oxidizing valence band holes, produced by ultraviolet (UV) illumination of naturally occurring semiconducting minerals, are capable of oxidizing chloride ion to perchlorate in aqueous solutions at higher rates than other known natural perchlorate production processes. Our results support an alternative to atmospheric reactions leading to the formation of high concentrations of perchlorate on Mars.
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Morris RV, Ruff SW, Gellert R, Ming DW, Arvidson RE, Clark BC, Golden DC, Siebach K, Klingelhöfer G, Schröder C, Fleischer I, Yen AS, Squyres SW. Identification of carbonate-rich outcrops on Mars by the Spirit rover. Science 2010; 329:421-4. [PMID: 20522738 DOI: 10.1126/science.1189667] [Citation(s) in RCA: 85] [Impact Index Per Article: 6.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Decades of speculation about a warmer, wetter Mars climate in the planet's first billion years postulate a denser CO2-rich atmosphere than at present. Such an atmosphere should have led to the formation of outcrops rich in carbonate minerals, for which evidence has been sparse. Using the Mars Exploration Rover Spirit, we have now identified outcrops rich in magnesium-iron carbonate (16 to 34 weight percent) in the Columbia Hills of Gusev crater. Its composition approximates the average composition of the carbonate globules in martian meteorite ALH 84001. The Gusev carbonate probably precipitated from carbonate-bearing solutions under hydrothermal conditions at near-neutral pH in association with volcanic activity during the Noachian era.
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Fendrihan S, Musso M, Stan-Lotter H. Raman spectroscopy as a potentialmethod for the detection of extremely halophilic archaea embedded in halite in terrestrial and possibly extraterrestrial samples. JOURNAL OF RAMAN SPECTROSCOPY : JRS 2009; 40:1996-2003. [PMID: 22058585 PMCID: PMC3207228 DOI: 10.1002/jrs.2357] [Citation(s) in RCA: 21] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/03/2023]
Abstract
Evidence for the widespread occurrence of extraterrestrial halite, particularly on Mars, has led to speculations on the possibility of halophilic microbial forms of life; these ideas have been strengthened by reports of viable haloarchaea from sediments of geological age (millions of years). Raman spectroscopy, being a sensitive detection method for future astrobiological investigations onsite, has been used in the current study for the detection of nine different extremely halophilic archaeal strains which had been embedded in laboratory-made halite crystals in order to simulate evaporitic conditions. The cells accumulated preferentially in tiny fluid inclusions, in simulation of the precipitation of salt in natural brines. FT-Raman spectroscopy using laser excitation at 1064 nm and dispersive micro Raman spectroscopy at 514.5 nm were applied. The spectra showed prominent peaks at 1507, 1152 and 1002 cm(-1) which are attributed to haloarchaeal C(50) carotenoid compounds (mainly bacterioruberins). Their intensity varied from strain to strain at 1064-nm laser excitation. Other distinguishable features were peaks due to peptide bonds (amide I, amide III) and to nucleic acids. No evidence for fatty acids was detected, consistent with their general absence in all archaea.These results contribute to a growing database on Raman spectra of terrestrial microorganisms from hypersaline environments and highlight the influence of the different macromolecular composition of diverse strains on these spectra.
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Affiliation(s)
- Sergiu Fendrihan
- Department of Molecular Biology, Division of Microbiology, University of Salzburg, Billrothstrasse 11, A-5020 Salzburg, Austria
| | - Maurizio Musso
- Department of Materials Engineering and Physics, Division of Physics and Biophysics, University of Salzburg, Hellbrunnerstrasse 34, A-5020 Salzburg, Austria
| | - Helga Stan-Lotter
- Department of Molecular Biology, Division of Microbiology, University of Salzburg, Billrothstrasse 11, A-5020 Salzburg, Austria
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McKeown NK, Bishop JL, Noe Dobrea EZ, Ehlmann BL, Parente M, Mustard JF, Murchie SL, Swayze GA, Bibring JP, Silver EA. Characterization of phyllosilicates observed in the central Mawrth Vallis region, Mars, their potential formational processes, and implications for past climate. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003301] [Citation(s) in RCA: 89] [Impact Index Per Article: 5.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Halevy I, Pierrehumbert RT, Schrag DP. Radiative transfer in CO2-rich paleoatmospheres. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009jd011915] [Citation(s) in RCA: 53] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Boynton WV, Ming DW, Kounaves SP, Young SMM, Arvidson RE, Hecht MH, Hoffman J, Niles PB, Hamara DK, Quinn RC, Smith PH, Sutter B, Catling DC, Morris RV. Evidence for calcium carbonate at the Mars Phoenix landing site. Science 2009; 325:61-4. [PMID: 19574384 DOI: 10.1126/science.1172768] [Citation(s) in RCA: 75] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Carbonates are generally products of aqueous processes and may hold important clues about the history of liquid water on the surface of Mars. Calcium carbonate (approximately 3 to 5 weight percent) has been identified in the soils around the Phoenix landing site by scanning calorimetry showing an endothermic transition beginning around 725 degrees C accompanied by evolution of carbon dioxide and by the ability of the soil to buffer pH against acid addition. Based on empirical kinetics, the amount of calcium carbonate is most consistent with formation in the past by the interaction of atmospheric carbon dioxide with liquid water films on particle surfaces.
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Affiliation(s)
- W V Boynton
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA.
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Poulet F, Beaty DW, Bibring JP, Bish D, Bishop JL, Noe Dobrea E, Mustard JF, Petit S, Roach LH. Key scientific questions and key investigations from the first international conference on Martian phyllosilicates. ASTROBIOLOGY 2009; 9:257-267. [PMID: 19400732 DOI: 10.1089/ast.2009.0335] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/27/2023]
Abstract
Minerals and their occurrences can tell us about the chemistry, pressure, and temperatures of past environments on Mars and thus allow inferences about the potential for habitability. Thanks to recent space exploration, a new vision is emerging wherein Mars hosted environmental conditions of potential astrobiological relevance. This epoch is identified by the presence of phyllosilicate-bearing deposits, which are generally contained in very ancient basement rocks. In October 2008, over 100 planetary scientists representing 11 countries met in Paris to assess and discuss the relevance of martian phyllosilicates. The conference was structured to promote the discussion and debate of key scientific questions and key essential investigations. The purpose of this report is to document the current state of knowledge related to martian phyllosilicates and to ascertain which questions remain to be addressed: What are the basic characteristics of the phyllosilicate minerals on Mars? What are the genetic mechanisms by which phyllosilicate minerals have formed on Mars? What is the relationship between the phyllosilicate minerals observed in martian meteorites and those detected from orbit? What are the implications of phyllosilicate-bearing rocks for the development of prebiotic chemistry and the preservation of biosignatures? The most promising investigations to address these questions are presented.
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Affiliation(s)
- François Poulet
- Institut d'Astrophysique Spatiale, CNRS/Université Paris-Sud, Orsay, France.
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Ehlmann BL, Mustard JF, Murchie SL, Poulet F, Bishop JL, Brown AJ, Calvin WM, Clark RN, Marais DJD, Milliken RE, Roach LH, Roush TL, Swayze GA, Wray JJ. Orbital identification of carbonate-bearing rocks on Mars. Science 2009; 322:1828-32. [PMID: 19095939 DOI: 10.1126/science.1164759] [Citation(s) in RCA: 122] [Impact Index Per Article: 8.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Geochemical models for Mars predict carbonate formation during aqueous alteration. Carbonate-bearing rocks had not previously been detected on Mars' surface, but Mars Reconnaissance Orbiter mapping reveals a regional rock layer with near-infrared spectral characteristics that are consistent with the presence of magnesium carbonate in the Nili Fossae region. The carbonate is closely associated with both phyllosilicate-bearing and olivine-rich rock units and probably formed during the Noachian or early Hesperian era from the alteration of olivine by either hydrothermal fluids or near-surface water. The presence of carbonate as well as accompanying clays suggests that waters were neutral to alkaline at the time of its formation and that acidic weathering, proposed to be characteristic of Hesperian Mars, did not destroy these carbonates and thus did not dominate all aqueous environments.
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Affiliation(s)
- Bethany L. Ehlmann
- Department of Geological Sciences, Brown University, Providence, RI02912, USA
- Johns Hopkins University/Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA
- Institut d'Astrophysique Spatiale, Université Paris Sud 11, 91405 Orsay, France
- SETI Institute and NASA Ames Research Center, 515 North Whisman Road, Mountain View, CA 94043, USA
- Department of Geological Sciences and Engineering, University of Nevada, MS 172, 1664 North Virginia Street, Reno, NV 89557, USA
| | - John F. Mustard
- Department of Geological Sciences, Brown University, Providence, RI02912, USA
- Johns Hopkins University/Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA
- Institut d'Astrophysique Spatiale, Université Paris Sud 11, 91405 Orsay, France
- SETI Institute and NASA Ames Research Center, 515 North Whisman Road, Mountain View, CA 94043, USA
- Department of Geological Sciences and Engineering, University of Nevada, MS 172, 1664 North Virginia Street, Reno, NV 89557, USA
| | - Scott L. Murchie
- Department of Geological Sciences, Brown University, Providence, RI02912, USA
- Johns Hopkins University/Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA
- Institut d'Astrophysique Spatiale, Université Paris Sud 11, 91405 Orsay, France
- SETI Institute and NASA Ames Research Center, 515 North Whisman Road, Mountain View, CA 94043, USA
- Department of Geological Sciences and Engineering, University of Nevada, MS 172, 1664 North Virginia Street, Reno, NV 89557, USA
| | - Francois Poulet
- Department of Geological Sciences, Brown University, Providence, RI02912, USA
- Johns Hopkins University/Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA
- Institut d'Astrophysique Spatiale, Université Paris Sud 11, 91405 Orsay, France
- SETI Institute and NASA Ames Research Center, 515 North Whisman Road, Mountain View, CA 94043, USA
- Department of Geological Sciences and Engineering, University of Nevada, MS 172, 1664 North Virginia Street, Reno, NV 89557, USA
| | - Janice L. Bishop
- Department of Geological Sciences, Brown University, Providence, RI02912, USA
- Johns Hopkins University/Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA
- Institut d'Astrophysique Spatiale, Université Paris Sud 11, 91405 Orsay, France
- SETI Institute and NASA Ames Research Center, 515 North Whisman Road, Mountain View, CA 94043, USA
- Department of Geological Sciences and Engineering, University of Nevada, MS 172, 1664 North Virginia Street, Reno, NV 89557, USA
| | - Adrian J. Brown
- Department of Geological Sciences, Brown University, Providence, RI02912, USA
- Johns Hopkins University/Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA
- Institut d'Astrophysique Spatiale, Université Paris Sud 11, 91405 Orsay, France
- SETI Institute and NASA Ames Research Center, 515 North Whisman Road, Mountain View, CA 94043, USA
- Department of Geological Sciences and Engineering, University of Nevada, MS 172, 1664 North Virginia Street, Reno, NV 89557, USA
| | - Wendy M. Calvin
- Department of Geological Sciences, Brown University, Providence, RI02912, USA
- Johns Hopkins University/Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA
- Institut d'Astrophysique Spatiale, Université Paris Sud 11, 91405 Orsay, France
- SETI Institute and NASA Ames Research Center, 515 North Whisman Road, Mountain View, CA 94043, USA
- Department of Geological Sciences and Engineering, University of Nevada, MS 172, 1664 North Virginia Street, Reno, NV 89557, USA
| | - Roger N. Clark
- Department of Geological Sciences, Brown University, Providence, RI02912, USA
- Johns Hopkins University/Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA
- Institut d'Astrophysique Spatiale, Université Paris Sud 11, 91405 Orsay, France
- SETI Institute and NASA Ames Research Center, 515 North Whisman Road, Mountain View, CA 94043, USA
- Department of Geological Sciences and Engineering, University of Nevada, MS 172, 1664 North Virginia Street, Reno, NV 89557, USA
| | - David J. Des Marais
- Department of Geological Sciences, Brown University, Providence, RI02912, USA
- Johns Hopkins University/Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA
- Institut d'Astrophysique Spatiale, Université Paris Sud 11, 91405 Orsay, France
- SETI Institute and NASA Ames Research Center, 515 North Whisman Road, Mountain View, CA 94043, USA
- Department of Geological Sciences and Engineering, University of Nevada, MS 172, 1664 North Virginia Street, Reno, NV 89557, USA
| | - Ralph E. Milliken
- Department of Geological Sciences, Brown University, Providence, RI02912, USA
- Johns Hopkins University/Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA
- Institut d'Astrophysique Spatiale, Université Paris Sud 11, 91405 Orsay, France
- SETI Institute and NASA Ames Research Center, 515 North Whisman Road, Mountain View, CA 94043, USA
- Department of Geological Sciences and Engineering, University of Nevada, MS 172, 1664 North Virginia Street, Reno, NV 89557, USA
| | - Leah H. Roach
- Department of Geological Sciences, Brown University, Providence, RI02912, USA
- Johns Hopkins University/Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA
- Institut d'Astrophysique Spatiale, Université Paris Sud 11, 91405 Orsay, France
- SETI Institute and NASA Ames Research Center, 515 North Whisman Road, Mountain View, CA 94043, USA
- Department of Geological Sciences and Engineering, University of Nevada, MS 172, 1664 North Virginia Street, Reno, NV 89557, USA
| | - Ted L. Roush
- Department of Geological Sciences, Brown University, Providence, RI02912, USA
- Johns Hopkins University/Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA
- Institut d'Astrophysique Spatiale, Université Paris Sud 11, 91405 Orsay, France
- SETI Institute and NASA Ames Research Center, 515 North Whisman Road, Mountain View, CA 94043, USA
- Department of Geological Sciences and Engineering, University of Nevada, MS 172, 1664 North Virginia Street, Reno, NV 89557, USA
| | - Gregg A. Swayze
- Department of Geological Sciences, Brown University, Providence, RI02912, USA
- Johns Hopkins University/Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA
- Institut d'Astrophysique Spatiale, Université Paris Sud 11, 91405 Orsay, France
- SETI Institute and NASA Ames Research Center, 515 North Whisman Road, Mountain View, CA 94043, USA
- Department of Geological Sciences and Engineering, University of Nevada, MS 172, 1664 North Virginia Street, Reno, NV 89557, USA
| | - James J. Wray
- Department of Geological Sciences, Brown University, Providence, RI02912, USA
- Johns Hopkins University/Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD 20723, USA
- Institut d'Astrophysique Spatiale, Université Paris Sud 11, 91405 Orsay, France
- SETI Institute and NASA Ames Research Center, 515 North Whisman Road, Mountain View, CA 94043, USA
- Department of Geological Sciences and Engineering, University of Nevada, MS 172, 1664 North Virginia Street, Reno, NV 89557, USA
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Zahnle K, Haberle RM, Catling DC, Kasting JF. Photochemical instability of the ancient Martian atmosphere. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003160] [Citation(s) in RCA: 104] [Impact Index Per Article: 6.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 01/01/2023]
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Mangold N, Ansan V, Masson P, Quantin C, Neukum G. Geomorphic study of fluvial landforms on the northern Valles Marineris plateau, Mars. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002985] [Citation(s) in RCA: 58] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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44
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Johnson SS, Mischna MA, Grove TL, Zuber MT. Sulfur-induced greenhouse warming on early Mars. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002962] [Citation(s) in RCA: 76] [Impact Index Per Article: 4.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Schröder C, Rodionov DS, McCoy TJ, Jolliff BL, Gellert R, Nittler LR, Farrand WH, Johnson JR, Ruff SW, Ashley JW, Mittlefehldt DW, Herkenhoff KE, Fleischer I, Haldemann AFC, Klingelhöfer G, Ming DW, Morris RV, de Souza PA, Squyres SW, Weitz C, Yen AS, Zipfel J, Economou T. Meteorites on Mars observed with the Mars Exploration Rovers. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002990] [Citation(s) in RCA: 63] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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46
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Chevrier V, Poulet F, Bibring JP. Early geochemical environment of Mars as determined from thermodynamics of phyllosilicates. Nature 2007; 448:60-3. [PMID: 17611538 DOI: 10.1038/nature05961] [Citation(s) in RCA: 153] [Impact Index Per Article: 9.0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/29/2006] [Accepted: 05/22/2007] [Indexed: 11/09/2022]
Abstract
Images of geomorphological features that seem to have been produced by the action of liquid water have been considered evidence for wet surface conditions on early Mars. Moreover, the recent identification of large deposits of phyllosilicates, associated with the ancient Noachian terrains suggests long-timescale weathering of the primary basaltic crust by liquid water. It has been proposed that a greenhouse effect resulting from a carbon-dioxide-rich atmosphere sustained the temperate climate required to maintain liquid water on the martian surface during the Noachian. The apparent absence of carbonates and the low escape rates of carbon dioxide, however, are indicative of an early martian atmosphere with low levels of carbon dioxide. Here we investigate the geochemical conditions prevailing on the surface of Mars during the Noachian period using calculations of the aqueous equilibria of phyllosilicates. Our results show that Fe3+-rich phyllosilicates probably precipitated under weakly acidic to alkaline pH, an environment different from that of the following period, which was dominated by strongly acid weathering that led to the sulphate deposits identified on Mars. Thermodynamic calculations demonstrate that the oxidation state of the martian surface was already high, supporting early escape of hydrogen. Finally, equilibrium with carbonates implies that phyllosilicate precipitation occurs preferentially at a very low partial pressure of carbon dioxide. We suggest that the possible absence of Noachian carbonates more probably resulted from low levels of atmospheric carbon dioxide, rather than primary acidic conditions. Other greenhouse gases may therefore have played a part in sustaining a warm and wet climate on the early Mars.
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Affiliation(s)
- Vincent Chevrier
- W. M. Keck Laboratory for Space Simulation, Arkansas Center for Space and Planetary Sciences, MUSE 202, University of Arkansas, Fayetteville, Arkansas 72701, USA.
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47
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Gilichinsky DA, Wilson GS, Friedmann EI, McKay CP, Sletten RS, Rivkina EM, Vishnivetskaya TA, Erokhina LG, Ivanushkina NE, Kochkina GA, Shcherbakova VA, Soina VS, Spirina EV, Vorobyova EA, Fyodorov-Davydov DG, Hallet B, Ozerskaya SM, Sorokovikov VA, Laurinavichyus KS, Shatilovich AV, Chanton JP, Ostroumov VE, Tiedje JM. Microbial populations in Antarctic permafrost: biodiversity, state, age, and implication for astrobiology. ASTROBIOLOGY 2007; 7:275-311. [PMID: 17480161 DOI: 10.1089/ast.2006.0012] [Citation(s) in RCA: 80] [Impact Index Per Article: 4.7] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/15/2023]
Abstract
Antarctic permafrost soils have not received as much geocryological and biological study as has been devoted to the ice sheet, though the permafrost is more stable and older and inhabited by more microbes. This makes these soils potentially more informative and a more significant microbial repository than ice sheets. Due to the stability of the subsurface physicochemical regime, Antarctic permafrost is not an extreme environment but a balanced natural one. Up to 10(4) viable cells/g, whose age presumably corresponds to the longevity of the permanently frozen state of the sediments, have been isolated from Antarctic permafrost. Along with the microbes, metabolic by-products are preserved. This presumed natural cryopreservation makes it possible to observe what may be the oldest microbial communities on Earth. Here, we describe the Antarctic permafrost habitat and biodiversity and provide a model for martian ecosystems.
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Affiliation(s)
- D A Gilichinsky
- Institutes of Physicochemical and Biological Problems in Soil Science, Russian Academy of Sciences, Pushchino, Moscow Region, Russia. gilichin@online stack.net
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48
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Andrews-Hanna JC, Phillips RJ, Zuber MT. Meridiani Planum and the global hydrology of Mars. Nature 2007; 446:163-6. [PMID: 17344848 DOI: 10.1038/nature05594] [Citation(s) in RCA: 37] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/27/2006] [Accepted: 01/08/2007] [Indexed: 11/09/2022]
Abstract
The Opportunity Mars Exploration Rover found evidence for groundwater activity in the Meridiani Planum region of Mars in the form of aeolian and fluvial sediments composed of sulphate-rich grains. These sediments appear to have experienced diagenetic modification in the presence of a fluctuating water table. In addition to the extensive secondary aqueous alteration, the primary grains themselves probably derive from earlier playa evaporites. Little is known, however, about the hydrologic processes responsible for this environmental history-particularly how such extensive evaporite deposits formed in the absence of a topographic basin. Here we investigate the origin of these deposits, in the context of the global hydrology of early Mars, using numerical simulations, and demonstrate that Meridiani is one of the few regions of currently exposed ancient crust predicted to have experienced significant groundwater upwelling and evaporation. The global groundwater flow would have been driven primarily by precipitation-induced recharge and evaporative loss, with the formation of the Tharsis volcanic rise possibly playing a role through the burial of aquifers and induced global deformation. These results suggest that the deposits formed as a result of sustained groundwater upwelling and evaporation, rather than ponding within an enclosed basin. The evaporite formation coincided with a transition to more arid conditions that increased the relative impact of a deep-seated, global-scale hydrology on the surface evolution.
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Affiliation(s)
- Jeffrey C Andrews-Hanna
- McDonnell Center for the Space Sciences and the Department of Earth and Planetary Sciences, Washington University, St Louis, Missouri 63130, USA.
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49
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Abstract
One of the goals of the present Martian exploration is to search for evidence of extinct (or even extant) life. This could be redefined as a search for carbon. The carbon cycle (or, more properly, cycles) on Earth is a complex interaction among three reservoirs: the atmosphere; the hydrosphere; and the lithosphere. Superimposed on this is the biosphere, and its presence influences the fixing and release of carbon in these reservoirs over different time-scales. The overall carbon balance is kept at equilibrium on the surface by a combination of tectonic processes (which bury carbon), volcanism (which releases it) and biology (which mediates it). In contrast to Earth, Mars presently has no active tectonic system; neither does it possess a significant biosphere. However, these observations might not necessarily have held in the past. By looking at how Earth's carbon cycles have changed with time, as both the Earth's tectonic structure and a more sophisticated biology have evolved, and also by constructing a carbon cycle for Mars based on the carbon chemistry of Martian meteorites, we investigate whether or not there is evidence for a Martian biosphere.
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Affiliation(s)
- Monica M Grady
- Planetary and Space Sciences Research Institute, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK.
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50
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Quinn R, Zent AP, McKay CP. The photochemical stability of carbonates on Mars. ASTROBIOLOGY 2006; 6:581-91. [PMID: 16916284 DOI: 10.1089/ast.2006.6.581] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/11/2023]
Abstract
Carbonates, predominately MgCO3, have been spectroscopically identified at a level of 2-5% in martian dust. However, in spite of this observation, and a large number of climate studies that suggest 1 to several bars of CO2 should be sequestered in carbonate rocks, no outcrop-scale exposures of carbonate have been detected anywhere on Mars to date. To address one hypothesis for this long-standing puzzle, the effect of ultraviolet (UV) light on the stability of calcium carbonate in a simulated martian atmosphere was experimentally investigated. Using 13C-labeled calcite, we found no experimental evidence of the UV photodecomposition of calcium carbonate in a simulated martian atmosphere. Extrapolating the lower limit of detection of our experimental system to an upper limit of carbonate decomposition on Mars yields a quantum efficiency of 3.5 x 10(-8) molecules/photon over the wavelength interval of 190-390 nm and a maximum UV photodecomposition rate of 1.2 x 10(-13) kg m(-2) s(-1) from a calcite surface. The maximum loss of bulk calcite due to this process would be 2.5 nm year(-1) (Mars year). However, calcite is expected to be thermodynamically stable on the surface of Mars, and potential UV photodecomposition reaction mechanisms indicate that, though calcium carbonate may decompose under vacuum, it would be stable in a CO2 atmosphere. Given the expected stability of carbonate on Mars and our inability to detect carbonate decomposition, we conclude that it is unlikely that the apparent absence of extensive carbonate deposits on the martian surface is due to UV photodecomposition in the current environment.
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Affiliation(s)
- Richard Quinn
- SETI Institute, NASA Ames Research Center, Moffett Field, California 94039, USA.
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