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Clarke JT, Mayyasi M, Bhattacharyya D, Chaufray JY, Schneider N, Jakosky B, Yelle R, Montmessin F, Chaffin M, Curry S, Deighan J, Jain S, Bertaux JL, Cangi E, Crismani M, Evans S, Gupta S, Lefevre F, Holsclaw G, Lo D, McClintock W, Stevens M, Stewart I, Stone S, Mahaffy P, Benna M, Elrod M. Martian atmospheric hydrogen and deuterium: Seasonal changes and paradigm for escape to space. SCIENCE ADVANCES 2024; 10:eadm7499. [PMID: 39058782 PMCID: PMC11277398 DOI: 10.1126/sciadv.adm7499] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/03/2023] [Accepted: 06/25/2024] [Indexed: 07/28/2024]
Abstract
Mars' water history is fundamental to understanding Earth-like planet evolution. Water escapes to space as atoms, and hydrogen atoms escape faster than deuterium giving an increase in the residual D/H ratio. The present ratio reflects the total water Mars has lost. Observations with the Mars Atmosphere and Volatile Evolution (MAVEN) and Hubble Space Telescope (HST) spacecraft provide atomic densities and escape rates for H and D. Large increases near perihelion observed each martian year are consistent with a strong upwelling of water vapor. Short-term changes require processes in addition to thermal escape, likely from atmospheric dynamics and superthermal atoms. Including escape from hot atoms, both H and D escape rapidly, and the escape fluxes are limited by resupply from the lower atmosphere. In this paradigm for the escape of water, the D/H ratio of the escaping atoms and the enhancement in water are determined by upwelling water vapor and atmospheric dynamics rather than by the specific details of atomic escape.
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Affiliation(s)
- John T. Clarke
- Center for Space Physics, Boston University, Boston, MA, USA
| | - Majd Mayyasi
- Center for Space Physics, Boston University, Boston, MA, USA
| | - Dolon Bhattacharyya
- Center for Space Physics, Boston University, Boston, MA, USA
- LASP, University of Colorado, Boulder, CO, USA
| | | | | | | | - Roger Yelle
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | | | | | - Shannon Curry
- Space Sciences Laboratory, University of California, Berkeley, CA, USA
| | | | - Sonal Jain
- LASP, University of Colorado, Boulder, CO, USA
| | | | - Erin Cangi
- LASP, University of Colorado, Boulder, CO, USA
| | | | | | | | | | | | - Daniel Lo
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | | | - Michael Stevens
- Space Science Division, Naval Research Laboratory, Washington, DC, USA
| | - Ian Stewart
- LASP, University of Colorado, Boulder, CO, USA
| | - Shane Stone
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - Paul Mahaffy
- NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - Mehdi Benna
- University of Maryland Baltimore County, Baltimore County, MD, USA
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2
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Ciesielczuk J, Fabiańska MJ, Gaidzik K, Nádudvari Á, Misz-Kennan M, Abramowicz A. Botryoidal and spherulitic hematite as experimental evidence of highly acidic conditions in burning coal-waste dumps and potentially on Mars. THE SCIENCE OF THE TOTAL ENVIRONMENT 2024; 932:172759. [PMID: 38670352 DOI: 10.1016/j.scitotenv.2024.172759] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/18/2023] [Revised: 04/02/2024] [Accepted: 04/23/2024] [Indexed: 04/28/2024]
Abstract
In the extreme setting of burning coal-waste dumps in the Upper Silesian Coal Basin in Poland, botryoidal and spherulitic hematite occurs in association with sulphates and chlorides. A series of simple experiments aimed at replicating the conditions leading to the formation of hematite spherules on the burning dumps are described. Goethite synthesised in the laboratory, mixed with various combinations of other reactants, was heated in a heating chamber or a tubular furnace. Temperature, duration of heating, water and oxygen access, and pH were experimental variables. The results show that hematite may form spherules from goethite where access to oxygen is limited and where conditions are strongly acidic. The spherulitic shape of hematite produced due to dynamically changing physicochemical conditions in the burning dumps can be an indicator of an extremely acidic environment during the closing stages of coal-waste self-heating. The conditions of hematitic-spherule formation on burning coal-waste dumps may apply in a variety of other unrelated settings, e.g., waning volcanism, sulphuric acid speleologenesis and even the formation of blueberries on Mars.
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Affiliation(s)
- Justyna Ciesielczuk
- Institute of Earth Sciences, Faculty of Natural Sciences, University of Silesia in Katowice, Będzińska 60, 41-200 Sosnowiec, Poland.
| | - Monika J Fabiańska
- Institute of Earth Sciences, Faculty of Natural Sciences, University of Silesia in Katowice, Będzińska 60, 41-200 Sosnowiec, Poland
| | - Krzysztof Gaidzik
- Institute of Earth Sciences, Faculty of Natural Sciences, University of Silesia in Katowice, Będzińska 60, 41-200 Sosnowiec, Poland
| | - Ádám Nádudvari
- Institute of Earth Sciences, Faculty of Natural Sciences, University of Silesia in Katowice, Będzińska 60, 41-200 Sosnowiec, Poland
| | - Magdalena Misz-Kennan
- Institute of Earth Sciences, Faculty of Natural Sciences, University of Silesia in Katowice, Będzińska 60, 41-200 Sosnowiec, Poland
| | - Anna Abramowicz
- Institute of Earth Sciences, Faculty of Natural Sciences, University of Silesia in Katowice, Będzińska 60, 41-200 Sosnowiec, Poland
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3
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Styczinski MJ, Cooper ZS, Glaser DM, Lehmer O, Mierzejewski V, Tarnas J. Chapter 7: Assessing Habitability Beyond Earth. ASTROBIOLOGY 2024; 24:S143-S163. [PMID: 38498826 DOI: 10.1089/ast.2021.0097] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 03/20/2024]
Abstract
All known life on Earth inhabits environments that maintain conditions between certain extremes of temperature, chemical composition, energy availability, and so on (Chapter 6). Life may have emerged in similar environments elsewhere in the Solar System and beyond. The ongoing search for life elsewhere mainly focuses on those environments most likely to support life, now or in the past-that is, potentially habitable environments. Discussion of habitability is necessarily based on what we know about life on Earth, as it is our only example. This chapter gives an overview of the known and presumed requirements for life on Earth and discusses how these requirements can be used to assess the potential habitability of planetary bodies across the Solar System and beyond. We first consider the chemical requirements of life and potential feedback effects that the presence of life can have on habitable conditions, and then the planetary, stellar, and temporal requirements for habitability. We then review the state of knowledge on the potential habitability of bodies across the Solar System and exoplanets, with a particular focus on Mars, Venus, Europa, and Enceladus. While reviewing the case for the potential habitability of each body, we summarize the most prominent and impactful studies that have informed the perspective on where habitable environments are likely to be found.
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Affiliation(s)
- M J Styczinski
- University of Washington, Seattle, Washington, USA
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - Z S Cooper
- University of Washington, Seattle, Washington, USA
| | - D M Glaser
- School of Molecular Sciences, Arizona State University, Tempe, Arizona, USA
| | - O Lehmer
- NASA Ames Research Center, Moffett Field, California, USA
| | - V Mierzejewski
- School of Earth and Space Exploration, Arizona State University, Arizona, USA
| | - J Tarnas
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
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4
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Schaible MJ, Szeinbaum N, Bozdag GO, Chou L, Grefenstette N, Colón-Santos S, Rodriguez LE, Styczinski MJ, Thweatt JL, Todd ZR, Vázquez-Salazar A, Adams A, Araújo MN, Altair T, Borges S, Burton D, Campillo-Balderas JA, Cangi EM, Caro T, Catalano E, Chen K, Conlin PL, Cooper ZS, Fisher TM, Fos SM, Garcia A, Glaser DM, Harman CE, Hermis NY, Hooks M, Johnson-Finn K, Lehmer O, Hernández-Morales R, Hughson KHG, Jácome R, Jia TZ, Marlow JJ, McKaig J, Mierzejewski V, Muñoz-Velasco I, Nural C, Oliver GC, Penev PI, Raj CG, Roche TP, Sabuda MC, Schaible GA, Sevgen S, Sinhadc P, Steller LH, Stelmach K, Tarnas J, Tavares F, Trubl G, Vidaurri M, Vincent L, Weber JM, Weng MM, Wilpiszeki RL, Young A. Chapter 1: The Astrobiology Primer 3.0. ASTROBIOLOGY 2024; 24:S4-S39. [PMID: 38498816 DOI: 10.1089/ast.2021.0129] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 03/20/2024]
Abstract
The Astrobiology Primer 3.0 (ABP3.0) is a concise introduction to the field of astrobiology for students and others who are new to the field of astrobiology. It provides an entry into the broader materials in this supplementary issue of Astrobiology and an overview of the investigations and driving hypotheses that make up this interdisciplinary field. The content of this chapter was adapted from the other 10 articles in this supplementary issue and thus represents the contribution of all the authors who worked on these introductory articles. The content of this chapter is not exhaustive and represents the topics that the authors found to be the most important and compelling in a dynamic and changing field.
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Affiliation(s)
- Micah J Schaible
- School of Chemistry and Biochemistry, Georgia Institute of Technology, Atlanta, Georgia, USA
| | - Nadia Szeinbaum
- School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA
| | - G Ozan Bozdag
- School of Biological Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA
| | - Luoth Chou
- NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
- Center for Space Sciences and Technology, University of Maryland, Baltimore, Maryland, USA
- Georgetown University, Washington DC, USA
| | - Natalie Grefenstette
- Santa Fe Institute, Santa Fe, New Mexico, USA
- Blue Marble Space Institute of Science, Seattle, Washington, USA
| | - Stephanie Colón-Santos
- Wisconsin Institute for Discovery, University of Wisconsin-Madison, Wisconsin, USA
- Department of Botany, University of Wisconsin-Madison, Wisconsin, USA
| | - Laura E Rodriguez
- Lunar and Planetary Institute, Universities Space Research Association, Houston, Texas, USA
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - M J Styczinski
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
- University of Washington, Seattle, Washington, USA
| | - Jennifer L Thweatt
- Department of Biochemistry and Molecular Biology, Penn State University, University Park, Pennsylvania, USA
| | - Zoe R Todd
- Department of Earth and Space Sciences, University of Washington, Seattle, Washington, USA
| | - Alberto Vázquez-Salazar
- Departamento de Biología Evolutiva, Facultad de Ciencias, Universidad Nacional Autónoma de México, Mexico City, Mexico
- Department of Chemical and Biomolecular Engineering, University of California Los Angeles, California, USA
| | - Alyssa Adams
- Center for Space Sciences and Technology, University of Maryland, Baltimore, Maryland, USA
| | - M N Araújo
- Biochemistry Department, University of São Paulo, São Carlos, Brazil
| | - Thiago Altair
- Institute of Chemistry of São Carlos, Universidade de São Paulo, São Carlos, Brazil
- Department of Chemistry, College of the Atlantic, Bar Harbor, Maine, USA
| | | | - Dana Burton
- Department of Anthropology, George Washington University, Washington DC, USA
| | | | - Eryn M Cangi
- Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Boulder, Colorado, USA
| | - Tristan Caro
- Department of Geological Sciences, University of Colorado Boulder, Boulder, Colorado, USA
| | - Enrico Catalano
- Sant'Anna School of Advanced Studies, The BioRobotics Institute, Pisa, Italy
| | - Kimberly Chen
- School of Biological Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA
| | - Peter L Conlin
- School of Biological Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA
| | - Z S Cooper
- Department of Earth and Space Sciences, University of Washington, Seattle, Washington, USA
| | - Theresa M Fisher
- School of Earth and Space Exploration, Arizona State University, Tempe, Arizona, USA
| | - Santiago Mestre Fos
- School of Chemistry and Biochemistry, Georgia Institute of Technology, Atlanta, Georgia, USA
| | - Amanda Garcia
- Department of Bacteriology, University of Wisconsin-Madison, Wisconsin, USA
| | - D M Glaser
- Arizona State University, Tempe, Arizona, USA
| | - Chester E Harman
- Departamento de Biología Evolutiva, Facultad de Ciencias, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - Ninos Y Hermis
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
- Department of Physics and Space Sciences, University of Granada, Granada, Spain
| | - M Hooks
- NASA Johnson Space Center, Houston, Texas, USA
| | - K Johnson-Finn
- Earth-Life Science Institute, Tokyo Institute of Technology, Ookayama, Meguro-ku, Tokyo, Japan
- Rensselaer Polytechnic Institute, Troy, New York, USA
| | - Owen Lehmer
- Department of Earth and Space Sciences, University of Washington, Seattle, Washington, USA
| | - Ricardo Hernández-Morales
- Departamento de Biología Evolutiva, Facultad de Ciencias, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - Kynan H G Hughson
- School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA
| | - Rodrigo Jácome
- Departamento de Biología Evolutiva, Facultad de Ciencias, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - Tony Z Jia
- Blue Marble Space Institute of Science, Seattle, Washington, USA
- Earth-Life Science Institute, Tokyo Institute of Technology, Ookayama, Meguro-ku, Tokyo, Japan
| | - Jeffrey J Marlow
- Department of Biology, Boston University, Boston, Massachusetts, USA
| | - Jordan McKaig
- School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA
| | - Veronica Mierzejewski
- School of Earth and Space Exploration, Arizona State University, Tempe, Arizona, USA
| | - Israel Muñoz-Velasco
- Departamento de Biología Evolutiva, Facultad de Ciencias, Universidad Nacional Autónoma de México, Mexico City, Mexico
- Departamento de Biología Celular, Facultad de Ciencias, Universidad Nacional Autónoma de México, Mexico City, Mexico
| | - Ceren Nural
- Istanbul Technical University, Istanbul, Turkey
| | - Gina C Oliver
- Department of Geology, San Bernardino Valley College, San Bernardino, California, USA
| | - Petar I Penev
- School of Biological Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA
| | - Chinmayee Govinda Raj
- School of Chemistry and Biochemistry, Georgia Institute of Technology, Atlanta, Georgia, USA
| | - Tyler P Roche
- School of Chemistry and Biochemistry, Georgia Institute of Technology, Atlanta, Georgia, USA
| | - Mary C Sabuda
- Department of Earth and Environmental Sciences, University of Minnesota-Twin Cities, Minneapolis, Minnesota, USA
- Biotechnology Institute, University of Minnesota-Twin Cities, St. Paul, Minnesota, USA
| | - George A Schaible
- Department of Chemistry and Biochemistry, Montana State University, Bozeman, Montana, USA
| | - Serhat Sevgen
- Blue Marble Space Institute of Science, Seattle, Washington, USA
- Institute of Marine Sciences, Middle East Technical University, Erdemli, Mersin, Turkey
| | - Pritvik Sinhadc
- BEYOND: Center For Fundamental Concepts in Science, Arizona State University, Arizona, USA
- Dubai College, Dubai, United Arab Emirates
| | - Luke H Steller
- Australian Centre for Astrobiology, and School of Biological, Earth and Environmental Sciences, University of New South Wales, Kensington, Australia
| | - Kamil Stelmach
- Department of Chemistry, University of Virginia, Charlottesville, Virginia, USA
| | - J Tarnas
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - Frank Tavares
- Space Enabled Research Group, MIT Media Lab, Cambridge, Massachusetts, USA
| | - Gareth Trubl
- Physical and Life Sciences Directorate, Lawrence Livermore National Laboratory, Livermore, California, USA
| | - Monica Vidaurri
- Center for Space Sciences and Technology, University of Maryland, Baltimore, Maryland, USA
- Department of Physics and Astronomy, Howard University, Washington DC, USA
| | - Lena Vincent
- Wisconsin Institute for Discovery, University of Wisconsin-Madison, Wisconsin, USA
| | - Jessica M Weber
- NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | | | | | - Amber Young
- NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
- Northern Arizona University, Flagstaff, Arizona, USA
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Koyama S, Kamada A, Furukawa Y, Terada N, Nakamura Y, Yoshida T, Kuroda T, Vandaele AC. Atmospheric formaldehyde production on early Mars leading to a potential formation of bio-important molecules. Sci Rep 2024; 14:2397. [PMID: 38336798 PMCID: PMC10858170 DOI: 10.1038/s41598-024-52718-9] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/08/2023] [Accepted: 01/23/2024] [Indexed: 02/12/2024] Open
Abstract
Formaldehyde (H2CO) is a critical precursor for the abiotic formation of biomolecules, including amino acids and sugars, which are the building blocks of proteins and RNA. Geomorphological and geochemical evidence on Mars indicates a temperate environment compatible with the existence of surface liquid water during its early history at 3.8-3.6 billion years ago (Ga), which was maintained by the warming effect of reducing gases, such as H2. However, it remains uncertain whether such a temperate and weakly reducing surface environment on early Mars was suitable for producing H2CO. In this study, we investigated the atmospheric production of H2CO on early Mars using a 1-D photochemical model assuming a thick CO2-dominated atmosphere with H2 and CO. Our results show that a continuous supply of atmospheric H2CO can be used to form various organic compounds, including amino acids and sugars. This could be a possible origin for the organic matter observed on the Martian surface. Given the previously reported conversion rate from H2CO into ribose, the calculated H2CO deposition flux suggests a continuous supply of bio-important sugars on early Mars, particularly during the Noachian and early Hesperian periods.
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Affiliation(s)
- Shungo Koyama
- Graduate School of Science, Tohoku University, Sendai, Miyagi, 980-8578, Japan.
| | - Arihiro Kamada
- Graduate School of Science, Tohoku University, Sendai, Miyagi, 980-8578, Japan
| | - Yoshihiro Furukawa
- Graduate School of Science, Tohoku University, Sendai, Miyagi, 980-8578, Japan
| | - Naoki Terada
- Graduate School of Science, Tohoku University, Sendai, Miyagi, 980-8578, Japan
| | - Yuki Nakamura
- Graduate School of Science, The University of Tokyo, Tokyo, Japan
| | - Tatsuya Yoshida
- Graduate School of Science, Tohoku University, Sendai, Miyagi, 980-8578, Japan
| | - Takeshi Kuroda
- Graduate School of Science, Tohoku University, Sendai, Miyagi, 980-8578, Japan
- Division for the Establishment of Frontier Sciences of Organization for Advanced Studies, Tohoku University, Sendai, Japan
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6
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Clodoré L, Foucher F, Hickman-Lewis K, Sorieul S, Jouve J, Réfrégiers M, Collet G, Petoud S, Gratuze B, Westall F. Multi-Technique Characterization of 3.45 Ga Microfossils on Earth: A Key Approach to Detect Possible Traces of Life in Returned Samples from Mars. ASTROBIOLOGY 2024; 24:190-226. [PMID: 38393828 DOI: 10.1089/ast.2023.0089] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 02/25/2024]
Abstract
The NASA Mars 2020 Perseverance rover is actively exploring Jezero crater to conduct analyses on igneous and sedimentary rock targets from outcrops located on the crater floor (Máaz and Séítah formations) and from the delta deposits, respectively. The rock samples collected during this mission will be recovered during the Mars Sample Return mission, which plans to bring samples back to Earth in the 2030s to conduct in-depth studies using sophisticated laboratory instrumentation. Some of these samples may contain traces of ancient martian life that may be particularly difficult to detect and characterize because of their morphological simplicity and subtle biogeochemical expressions. Using the volcanic sediments of the 3.45 Ga Kitty's Gap Chert (Pilbara, Australia), containing putative early life forms (chemolithotrophs) and considered as astrobiological analogues for potential early Mars organisms, we document the steps required to demonstrate the syngenicity and biogenicity of such biosignatures using multiple complementary analytical techniques to provide information at different scales of observation. These include sedimentological, petrological, mineralogical, and geochemical analyses to demonstrate macro- to microscale habitability. New approaches, some unavailable at the time of the original description of these features, are used to verify the syngenicity and biogenicity of the purported fossil chemolithotrophs. The combination of elemental (proton-induced X-ray emission spectrometry) and molecular (deep-ultraviolet and Fourier transform infrared) analyses of rock slabs, thin sections, and focused ion beam sections reveals that the carbonaceous matter present in the samples is enriched in trace metals (e.g., V, Cr, Fe, Co) and is associated with aromatic and aliphatic molecules, which strongly support its biological origin. Transmission electron microscopy observations of the carbonaceous matter documented an amorphous nanostructure interpreted to correspond to the degraded remains of microorganisms and their by-products (extracellular polymeric substances, filaments…). Nevertheless, a small fraction of carbonaceous particles has signatures that are more metamorphosed. They probably represent either reworked detrital biological or abiotic fragments of mantle origin. This study serves as an example of the analytical protocol that would be needed to optimize the detection of fossil traces of life in martian rocks.
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Affiliation(s)
- Laura Clodoré
- CNRS-Centre de Biophysique Moléculaire, Orléans, France
| | - Frédéric Foucher
- CNRS-Centre de Biophysique Moléculaire, Orléans, France
- CNRS-Conditions Extrêmes et Matériaux: Haute Température et Irradiation, Orléans, France
| | - Keyron Hickman-Lewis
- Natural History Museum, London, United Kingdom
- Dipartimento BiGeA, Università di Bologna, Bologna, Italy
| | | | - Jean Jouve
- University of Bordeaux, CNRS, IN2P3, CENBG, Gradignan, France
| | | | - Guillaume Collet
- CNRS-Centre de Biophysique Moléculaire, Orléans, France
- Chair of Cosmetology, AgroParisTech Innovation, Orléans, France
| | | | - Bernard Gratuze
- CNRS-Institut de Recherche sur les ArchéoMATériaux, Orléans, France
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7
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Magnuson E, Altshuler I, Freyria NJ, Leveille RJ, Whyte LG. Sulfur-cycling chemolithoautotrophic microbial community dominates a cold, anoxic, hypersaline Arctic spring. MICROBIOME 2023; 11:203. [PMID: 37697305 PMCID: PMC10494364 DOI: 10.1186/s40168-023-01628-5] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/12/2023] [Accepted: 07/19/2023] [Indexed: 09/13/2023]
Abstract
BACKGROUND Gypsum Hill Spring, located in Nunavut in the Canadian High Arctic, is a rare example of a cold saline spring arising through thick permafrost. It perennially discharges cold (~ 7 °C), hypersaline (7-8% salinity), anoxic (~ 0.04 ppm O2), and highly reducing (~ - 430 mV) brines rich in sulfate (2.2 g.L-1) and sulfide (9.5 ppm), making Gypsum Hill an analog to putative sulfate-rich briny habitats on extraterrestrial bodies such as Mars. RESULTS Genome-resolved metagenomics and metatranscriptomics were utilized to describe an active microbial community containing novel metagenome-assembled genomes and dominated by sulfur-cycling Desulfobacterota and Gammaproteobacteria. Sulfate reduction was dominated by hydrogen-oxidizing chemolithoautotrophic Desulfovibrionaceae sp. and was identified in phyla not typically associated with sulfate reduction in novel lineages of Spirochaetota and Bacteroidota. Highly abundant and active sulfur-reducing Desulfuromusa sp. highly transcribed non-coding RNAs associated with transcriptional regulation, showing potential evidence of putative metabolic flexibility in response to substrate availability. Despite low oxygen availability, sulfide oxidation was primarily attributed to aerobic chemolithoautotrophic Halothiobacillaceae. Low abundance and transcription of photoautotrophs indicated sulfur-based chemolithoautotrophy drives primary productivity even during periods of constant illumination. CONCLUSIONS We identified a rare surficial chemolithoautotrophic, sulfur-cycling microbial community active in a unique anoxic, cold, hypersaline Arctic spring. We detected Mars-relevant metabolisms including hydrogenotrophic sulfate reduction, sulfur reduction, and sulfide oxidation, which indicate the potential for microbial life in analogous S-rich brines on past and present Mars. Video Abstract.
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Affiliation(s)
- Elisse Magnuson
- Natural Resource Sciences, McGill University, Ste-Anne-de-Bellevue, QC Canada
| | - Ianina Altshuler
- MACE Laboratory, ALPOLE, School of Architecture, Civil and Environmental Engineering (ENAC), Ecole Polytechnique Fédérale de Lausanne, Lausanne, Switzerland
| | - Nastasia J. Freyria
- Natural Resource Sciences, McGill University, Ste-Anne-de-Bellevue, QC Canada
| | - Richard J. Leveille
- Department of Earth and Planetary Sciences, McGill University, Montreal, QC Canada
- Geosciences Department, John Abbott College, Ste-Anne-de-Bellevue, QC Canada
| | - Lyle G. Whyte
- Natural Resource Sciences, McGill University, Ste-Anne-de-Bellevue, QC Canada
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8
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Diloreto Z, Ahmad MS, Al Saad Al-Kuwari H, Sadooni F, Bontognali TRR, Dittrich M. Raman Spectroscopic and Microbial Study of Biofilms Hosted Gypsum Deposits in the Hypersaline Wetlands: Astrobiological Perspective. ASTROBIOLOGY 2023; 23:991-1005. [PMID: 37672713 DOI: 10.1089/ast.2023.0003] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 09/08/2023]
Abstract
Gypsum (CaSO4·2H2O) has been identified at the surface of Mars, by both orbiters and rovers. Because gypsum mostly forms in the presence of liquid water as an essential element for sustaining microbial life and has a low porosity, which is ideal for preserving organic material, it is a promising target to look for signs of past microbial life. In this article, we studied organic matter preservation within gypsum that precipitates in a salt flat or a so-called coastal sabkha located in Qatar. Sabkha's ecosystem is considered a modern analog to evaporitic environments that may have existed on early Mars. We collected the sediment cores in the areas where gypsum is formed and performed DNA analysis to characterize the community of extremophilic microorganisms that is present at the site of gypsum formation. Subsequently, we applied Raman spectroscopy, a technique available on several rovers that are currently exploring Mars, to evaluate which organic molecules can be detected through the translucent gypsum crystals. We showed that organic material can be encapsulated into evaporitic gypsum and detected via Raman microscopy with simple, straightforward sample preparation. The molecular biology data proved useful for assessing to what extent complex Raman spectra can be linked to the original microbial community, dominated by Halobacteria and methanogenic archaea, providing a reference for a signal that may be detected on Mars.
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Affiliation(s)
- Zach Diloreto
- Department of Physical and Environmental Sciences, University of Toronto, Scarborough, Toronto, Ontario, Canada
| | - Mirza Shaharyar Ahmad
- Department of Physical and Environmental Sciences, University of Toronto, Scarborough, Toronto, Ontario, Canada
| | | | | | - Tomaso R R Bontognali
- Space Exploration Institute, Neuchâtel, Switzerland
- Department of Environmental Sciences, University of Basel, Basel, Switzerland
| | - Maria Dittrich
- Department of Physical and Environmental Sciences, University of Toronto, Scarborough, Toronto, Ontario, Canada
- Department of Earth Sciences, University of Toronto, Toronto, Ontario, Canada
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Rapin W, Dromart G, Clark BC, Schieber J, Kite ES, Kah LC, Thompson LM, Gasnault O, Lasue J, Meslin PY, Gasda PJ, Lanza NL. Sustained wet-dry cycling on early Mars. Nature 2023; 620:299-302. [PMID: 37558847 DOI: 10.1038/s41586-023-06220-3] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/08/2022] [Accepted: 05/15/2023] [Indexed: 08/11/2023]
Abstract
The presence of perennially wet surface environments on early Mars is well documented1,2, but little is known about short-term episodicity in the early hydroclimate3. Post-depositional processes driven by such short-term fluctuations may produce distinct structures, yet these are rarely preserved in the sedimentary record4. Incomplete geological constraints have led global models of the early Mars water cycle and climate to produce diverging results5,6. Here we report observations by the Curiosity rover at Gale Crater indicating that high-frequency wet-dry cycling occurred in early Martian surface environments. We observe exhumed centimetric polygonal ridges with sulfate enrichments, joined at Y-junctions, that record cracks formed in fresh mud owing to repeated wet-dry cycles of regular intensity. Instead of sporadic hydrological activity induced by impacts or volcanoes5, our findings point to a sustained, cyclic, possibly seasonal, climate on early Mars. Furthermore, as wet-dry cycling can promote prebiotic polymerization7,8, the Gale evaporitic basin may have been particularly conducive to these processes. The observed polygonal patterns are physically and temporally associated with the transition from smectite clays to sulfate-bearing strata, a globally distributed mineral transition1. This indicates that the Noachian-Hesperian transition (3.8-3.6 billion years ago) may have sustained an Earth-like climate regime and surface environments favourable to prebiotic evolution.
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Affiliation(s)
- W Rapin
- Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France.
| | | | - B C Clark
- Space Science Institute, Boulder, CO, USA
| | - J Schieber
- Indiana University, Bloomington, IN, USA
| | - E S Kite
- University of Chicago, Chicago, IL, USA
| | - L C Kah
- University of Tennessee, Knoxville, TN, USA
| | - L M Thompson
- University of New Brunswick, Fredericton, NB, Canada
| | - O Gasnault
- Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France
| | - J Lasue
- Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France
| | - P-Y Meslin
- Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse 3 Paul Sabatier, CNRS, CNES, Toulouse, France
| | - P J Gasda
- Los Alamos National Laboratory, Los Alamos, NM, USA
| | - N L Lanza
- Los Alamos National Laboratory, Los Alamos, NM, USA
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10
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Boulesteix D, Buch A, Samson J, Millan M, Jomaa J, Coscia D, Moulay V, McIntosh O, Freissinet C, Stern JC, Szopa C. Influence of pH and salts on DMF-DMA derivatization for future Space Applications. Anal Chim Acta 2023; 1266:341270. [PMID: 37244655 DOI: 10.1016/j.aca.2023.341270] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/30/2023] [Revised: 03/24/2023] [Accepted: 04/23/2023] [Indexed: 05/29/2023]
Abstract
For gas chromatography - mass spectrometry (GC-MS) analyses performed in situ, pH and salts (e.g., chlorides, sulfates) may enhance or inhibit the detection of targeted molecules of interest for astrobiology (e.g. amino acids, fatty acids, nucleobases). Obviously, salts influence the ionic strength of the solutions, the pH value, and the salting effect. But the presence of salts may also produce complexes or mask ions in the sample (masking effect on hydroxide ion, ammonia, etc.). For future space missions, wet chemistry will be conducted before GC-MS analyses to detect the full organic content of a sample. The defined organic targets for space GC-MS instrument requirements are generally strongly polar or refractory organic compounds, such as amino acids playing a role in the protein production and metabolism regulations for life on Earth, nucleobases essential for DNA and RNA formation and mutation, and fatty acids that composed most of the eukaryote and prokaryote membranes on Earth and resist to environmental stress long enough to still be observed on Mars or ocean worlds in geological well-preserved records. The wet-chemistry chemical treatment consists of reacting an organic reagent with the sample to extract and volatilize polar or refractory organic molecules (i.e. dimethylformamide dimethyl acetal (DMF-DMA) in this study). DMF-DMA derivatizes functional groups with labile H in organics, without modifying their chiral conformation. The influence of pH and salt concentration of extraterrestrial materials on the DMF-DMA derivatization remains understudied. In this research, we studied the influence of different salts and pHs on the derivatization of organic molecules of astrobiological interest with DMF-DMA, such as amino acids, carboxylic acids, and nucleobases. Results show that salts and pH influence the derivatization yield, and that their effect depend on the nature of the organics and the salts studied. Second, monovalent salts lead to a higher or similar organic recovery compared to divalent salts regardless of pH below 8. However, a pH above 8 inhibits the DMF-DMA derivatization influencing the carboxylic acid function to become an anionic group without labile H. Overall, considering the negative effect of the salts on the detection of organic molecules, future space missions may have to consider a desalting step prior to derivatization and GC-MS analyses.
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Affiliation(s)
- D Boulesteix
- Laboratoire Génie des Procédés et Matériaux, CentraleSupélec, University Paris-Saclay, 8-10 Rue Joliot-Curie, 91190, Gif-sur-Yvette, France.
| | - A Buch
- Laboratoire Génie des Procédés et Matériaux, CentraleSupélec, University Paris-Saclay, 8-10 Rue Joliot-Curie, 91190, Gif-sur-Yvette, France.
| | - J Samson
- Laboratoire Génie des Procédés et Matériaux, CentraleSupélec, University Paris-Saclay, 8-10 Rue Joliot-Curie, 91190, Gif-sur-Yvette, France
| | - M Millan
- LATMOS/IPSL, UVSQ University Paris-Saclay, Sorbonne University, CNRS, 11 Bd d'Alembert, 78280, Guyancourt, France
| | - J Jomaa
- Planetary Environments Laboratory (Code 699), NASA Goddard Space Flight Center, Greenbelt, MD, 20771, USA; School of Medicine, Wayne State University, 42 W. Warren Ave, Detroit, MI, 48202, USA
| | - D Coscia
- LATMOS/IPSL, UVSQ University Paris-Saclay, Sorbonne University, CNRS, 11 Bd d'Alembert, 78280, Guyancourt, France
| | - V Moulay
- LATMOS/IPSL, UVSQ University Paris-Saclay, Sorbonne University, CNRS, 11 Bd d'Alembert, 78280, Guyancourt, France
| | - O McIntosh
- LATMOS/IPSL, UVSQ University Paris-Saclay, Sorbonne University, CNRS, 11 Bd d'Alembert, 78280, Guyancourt, France
| | - C Freissinet
- LATMOS/IPSL, UVSQ University Paris-Saclay, Sorbonne University, CNRS, 11 Bd d'Alembert, 78280, Guyancourt, France
| | - J C Stern
- Space Science Exploration Division (Code 690), NASA, Goddard Space Flight Center, Greenbelt, MD, 20771, USA
| | - C Szopa
- LATMOS/IPSL, UVSQ University Paris-Saclay, Sorbonne University, CNRS, 11 Bd d'Alembert, 78280, Guyancourt, France
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11
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Meyer MJ, Milliken RE, Hurowitz JE, Robertson KM. Ancient Siliciclastic-Evaporites as Seen by Remote Sensing Instrumentation with Implications for the Rover-Scale Exploration of Sedimentary Environments on Mars. ASTROBIOLOGY 2023; 23:477-495. [PMID: 36944138 DOI: 10.1089/ast.2022.0103] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/04/2023]
Abstract
Accurate interpretation of the martian sedimentary rock record-and by extension that planet's paleoenvironmental history and potential habitability-relies heavily on rover-based acquisition of textural and compositional data and researchers to properly interpret those data. However, the degree to which this type of remotely sensed information can be unambiguously resolved and accurately linked to geological processes in ancient sedimentary systems warrants further study. In this study, we characterize Mars-relevant siliciclastic-evaporite samples by traditional laboratory-based geological methods (thin section petrography, X-ray diffraction [XRD], backscattered electron imaging, microprobe chemical analyses) and remote sensing methods relevant to martian rover payloads (visible-near-mid infrared reflectance spectroscopy, X-ray fluorescence mapping, XRD). We assess each method's ability to resolve primary and secondary sedimentologic features necessary for the accurate interpretation of paleoenvironmental processes. While the most dominant textures and associated compositions (i.e., bedded gypsum evaporite) of the sample suite are readily identified by a combination of remote sensing techniques, equally important, although more subtle, components (i.e., interbedded windblown silt, meniscus cements) are not resolved unambiguously in bulk samples. However, rover-based techniques capable of coordinating spatially resolved compositional measurements with textural imaging reveal important features not readily detected using traditional assessments (i.e., subtle clay-organic associations, microscale diagenetic nodules). Our findings demonstrate the improved generational capacity of rovers to explore ancient sedimentary environments on Mars while also highlighting the complexities in extracting comprehensive paleoenvironmental information when limited to currently available rover-based techniques. Complete and accurate interpretation of ancient martian sedimentary environments, and by extension the habitability of those environments, likely requires sample return or in situ human exploration. Plain Language Summary Only when correctly translated can the ancient martian sedimentary rock record reveal the environmental evolution of the planet's surface through time. In this case study, we characterize Mars-relevant sedimentary rocks and evaluate the degree to which a comprehensive geological picture can be resolved unambiguously when limited to microscale remote sensing methods relevant to rovers on Mars. While the most dominant textural features and associated compositions of the sample suite are readily identified by a combination of remote sensing techniques, equally important but more subtle components are not resolved unambiguously in bulk samples. However, rover-based techniques capable of coordinating spatially resolved compositional measurements with textural imaging, such as Perseverance Rover's Planetary Instrument for X-Ray Lithochemistry instrument, reveal important features not readily detected by more traditional methods. We demonstrate that rovers have, generationally, improved in their capacity to resolve a true geological picture in ancient sedimentary environments, likely owing to an improved ability to coordinate spatially resolved compositional measurements with textural imaging at the microscale. However, our work also highlights the complexities involved in extracting subtle environmental information when limited to currently available rover-based techniques and suggests that comprehensive interpretation of ancient martian sedimentary systems likely requires sample return or in situ human exploration. Key Points Mars-relevant samples are characterized using both traditional laboratory and microscale rover-based remote sensing techniques to assess each method's ability to recognize features necessary for accurate paleoenvironmental process interpretation. While some key paleoenvironmental processes can reasonably be inferred via remote sensing methods, others cannot be resolved unambiguously. Perseverance Rover's Planetary Instrument for X-Ray Lithochemistry instrument reveals diagenetic features that would otherwise remain unseen by traditional thin section petrography.
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Affiliation(s)
- Melissa J Meyer
- Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, Rhode Island, USA
| | - Ralph E Milliken
- Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, Rhode Island, USA
| | - Joel E Hurowitz
- Department of Geosciences, Stony Brook University, Stony Brook, New York, USA
| | - Kevin M Robertson
- Department of Earth, Environmental, and Planetary Sciences, Brown University, Providence, Rhode Island, USA
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12
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Perron A, Stalport F, Dupraz S, Person A, Coll P, Szopa C, Navarro-González R, Glavin D, Vaulay MJ, Ménez B. Thermal Stability of (Bio)Carbonates: A Potential Signature for Detecting Life on Mars? ASTROBIOLOGY 2023; 23:359-371. [PMID: 37017440 DOI: 10.1089/ast.2021.0202] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/19/2023]
Abstract
The environmental conditions that prevail on the surface of Mars (i.e., high levels of radiation and oxidants) are not favorable for the long-term preservation of organic compounds on which all strategies for finding life on Mars have been based to date. Since life commonly produces minerals that are considered more resilient, the search for biominerals could constitute a promising alternative approach. Carbonates are major biominerals on Earth, and although they have not been detected in large amounts at the martian surface, recent observations show that they could constitute a significant part of the inorganic component in the martian soil. Previous studies have shown that calcite and aragonite produced by eukaryotes thermally decompose at temperatures 15°C lower than those of their abiotic counterparts. By using carbonate concretions formed by microorganisms, we find that natural and experimental carbonates produced by prokaryotes decompose at 28°C below their abiotic counterparts. The study of this sample set serves as a proof of concept for the differential thermal analysis approach to distinguish abiotic from bio-related carbonates. This difference in carbonate decomposition temperature can be used as a first physical evidence of life on Mars to be searched by in situ space exploration missions with the resolution and the technical constraints of the available onboard instruments.
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Affiliation(s)
- Alexandra Perron
- Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA), CNRS UMR 7583, Université Paris Est Créteil et Université Paris Cité, Institut Pierre Simon Laplace (IPSL), Créteil, France
- Université Paris Cité, Institut de physique du globe de Paris, CNRS UMR 7154, Paris, France
| | - Fabien Stalport
- Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA), CNRS UMR 7583, Université Paris Est Créteil et Université Paris Cité, Institut Pierre Simon Laplace (IPSL), Créteil, France
| | - Sébastien Dupraz
- Université Paris Cité, Institut de physique du globe de Paris, CNRS UMR 7154, Paris, France
| | - Alain Person
- Laboratoire de Biominéralisations et Paléoenvironnements, Sorbonne Université, Paris, France
| | - Patrice Coll
- Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA), CNRS UMR 7583, Université Paris Est Créteil et Université Paris Cité, Institut Pierre Simon Laplace (IPSL), Créteil, France
| | - Cyril Szopa
- Laboratoire Atmosphères, Milieux, Observations Spatiales, Institut Pierre Simon Laplace (IPSL), CNRS UMR 8190, UVSQ Université Paris-Saclay, Sorbonne Université, Guyancourt, France
| | - Rafael Navarro-González
- Laboratorio de Química de Plasmas y Estudios Planetarios, Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de Mexico, Mexico
| | - Daniel Glavin
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, Maryland, USA
| | - Marie Josèphe Vaulay
- Laboratoire Interfaces Traitements Organisation et DYnamique des Systèmes (ITODYS), CNRS UMR 7086, Université Paris Cité, Paris, France
| | - Bénédicte Ménez
- Université Paris Cité, Institut de physique du globe de Paris, CNRS UMR 7154, Paris, France
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13
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Bennett KA, Fox VK, Bryk A, Dietrich W, Fedo C, Edgar L, Thorpe MT, Williams AJ, Wong GM, Dehouck E, McAdam A, Sutter B, Millan M, Banham SG, Bedford CC, Bristow T, Fraeman A, Vasavada AR, Grotzinger J, Thompson L, O’Connell‐Cooper C, Gasda P, Rudolph A, Sullivan R, Arvidson R, Cousin A, Horgan B, Stack KM, Treiman A, Eigenbrode J, Caravaca G. The Curiosity Rover's Exploration of Glen Torridon, Gale Crater, Mars: An Overview of the Campaign and Scientific Results. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2023; 128:e2022JE007185. [PMID: 37034460 PMCID: PMC10078523 DOI: 10.1029/2022je007185] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/18/2022] [Revised: 05/10/2022] [Accepted: 05/12/2022] [Indexed: 06/16/2023]
Abstract
The Mars Science Laboratory rover, Curiosity, explored the clay mineral-bearing Glen Torridon region for 1 Martian year between January 2019 and January 2021, including a short campaign onto the Greenheugh pediment. The Glen Torridon campaign sought to characterize the geology of the area, seek evidence of habitable environments, and document the onset of a potentially global climatic transition during the Hesperian era. Curiosity roved 5 km in total throughout Glen Torridon, from the Vera Rubin ridge to the northern margin of the Greenheugh pediment. Curiosity acquired samples from 11 drill holes during this campaign and conducted the first Martian thermochemolytic-based organics detection experiment with the Sample Analysis at Mars instrument suite. The lowest elevations within Glen Torridon represent a continuation of lacustrine Murray formation deposits, but overlying widespread cross bedded sandstones indicate an interval of more energetic fluvial environments and prompted the definition of a new stratigraphic formation in the Mount Sharp group called the Carolyn Shoemaker formation. Glen Torridon hosts abundant phyllosilicates yet remains compositionally and mineralogically comparable to the rest of the Mount Sharp group. Glen Torridon samples have a great diversity and abundance of sulfur-bearing organic molecules, which are consistent with the presence of ancient refractory organic matter. The Glen Torridon region experienced heterogeneous diagenesis, with the most striking alteration occurring just below the Siccar Point unconformity at the Greenheugh pediment. Results from the pediment campaign show that the capping sandstone formed within the Stimson Hesperian aeolian sand sea that experienced seasonal variations in wind direction.
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Affiliation(s)
| | - Valerie K. Fox
- Department of Earth and Environmental SciencesUniversity of MinnesotaMinneapolisMNUSA
- Division of Geologic and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - Alex Bryk
- Department of Earth and Planetary ScienceUniversity of California, BerkeleyBerkeleyCAUSA
| | - William Dietrich
- Department of Earth and Planetary ScienceUniversity of California, BerkeleyBerkeleyCAUSA
| | - Christopher Fedo
- Department of Earth and Planetary SciencesUniversity of TennesseeKnoxvilleTNUSA
| | - Lauren Edgar
- Astrogeology Science CenterU.S. Geological SurveyFlagstaffAZUSA
| | | | - Amy J. Williams
- Department of Geological SciencesUniversity of FloridaGainesvilleFLUSA
| | - Gregory M. Wong
- Department of GeosciencesThe Pennsylvania State UniversityUniversity ParkPAUSA
| | - Erwin Dehouck
- Université de LyonUCBLENSLUJMCNRSLGL‐TPEVilleurbanneFrance
| | - Amy McAdam
- NASA Goddard Space Flight CenterGreenbeltMDUSA
| | - Brad Sutter
- Jacobs TechnologyHoustonTXUSA
- NASA Johnson Space CenterHoustonTXUSA
| | - Maëva Millan
- NASA Goddard Space Flight CenterGreenbeltMDUSA
- Department of BiologyGeorgetown UniversityWashingtonDCUSA
- Laboratoire Atmosphère, Observations Spatiales (LATMOS), LATMOS/IPSLUVSQ Université Paris‐Saclay, Sorbonne Université, CNRSGuyancourtFrance
| | - Steven G. Banham
- Department of Earth Sciences and EngineeringImperial College LondonLondonUK
| | - Candice C. Bedford
- NASA Johnson Space CenterHoustonTXUSA
- Lunar and Planetary InstituteHoustonTXUSA
| | | | - Abigail Fraeman
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Ashwin R. Vasavada
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - John Grotzinger
- Division of Geologic and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - Lucy Thompson
- Planetary and Space Science CentreUniversity of New BrunswickFrederictonNBCanada
| | | | | | - Amanda Rudolph
- Earth Atmosphere and Planetary SciencePurdue UniversityWest LafayetteINUSA
| | | | - Ray Arvidson
- Department of Earth and Planetary SciencesWashington University in St. LouisSt. LouisMOUSA
| | - Agnes Cousin
- IRAPUniversité de ToulouseCNRSCNESToulouseFrance
| | - Briony Horgan
- Earth Atmosphere and Planetary SciencePurdue UniversityWest LafayetteINUSA
| | - Kathryn M. Stack
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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14
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Liu L, Liu H, Zhang W, Chen Y, Shen J, Li Y, Pan Y, Lin W. Microbial diversity and adaptive strategies in the Mars-like Qaidam Basin, North Tibetan Plateau, China. ENVIRONMENTAL MICROBIOLOGY REPORTS 2022; 14:873-885. [PMID: 35925018 DOI: 10.1111/1758-2229.13111] [Citation(s) in RCA: 8] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/07/2022] [Accepted: 07/15/2022] [Indexed: 06/17/2023]
Abstract
The Qaidam Basin on the northern Tibetan Plateau, China, is one of the driest deserts at high elevations, and it has been considered a representative Mars analogue site. Despite recent advances in the diversity of microbial communities in the Qaidam Basin, our understanding of their genomic information, functional potential and adaptive strategies remains very limited. Here, we conducted a combination of physicochemical and metagenomic analyses to investigate the taxonomic composition and adaptive strategies of microbial life in the regolith across the Qaidam Basin. 16S ribosomal RNA (rRNA) gene-based and metagenomic analyses both reveal that microbial communities in the Qaidam Basin are dominated by the bacterial phylum Actinobacteria. The low levels of moisture and organic carbon contents appear to have essential constraints on microbial biomass and diversity. A total of 50 high-quality metagenome-assembled genomes were reconstructed and analysed. Our results reveal the potential of microorganisms to use ambient trace gases to meet energy and carbon needs in this nutrient-limited desert. Furthermore, we find that DNA repair mechanisms and protein protection are likely essential for microbial life in response to stressors of hyperaridity, intense ultraviolet radiation and tremendous temperature fluctuations in this Mars analogue. These findings shed light on the diversity and survival strategies of microbial life inhabiting Mar-like environments, which provide implications for potential life on early Mars.
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Affiliation(s)
- Li Liu
- Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
- College of Earth and Planetary Sciences, University of Chinese Academy of Sciences, Beijing, China
| | - Haiyun Liu
- Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
- School of Life Sciences, Fudan University, Shanghai, China
| | - Wensi Zhang
- Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
| | - Yan Chen
- Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
| | - Jianxun Shen
- Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
| | - Yiliang Li
- Department of Earth Sciences, The University of Hong Kong, Hong Kong, China
| | - Yongxin Pan
- Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
- College of Earth and Planetary Sciences, University of Chinese Academy of Sciences, Beijing, China
| | - Wei Lin
- Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
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15
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Bonnet Gibet V, Michaut C, Wieczorek M, Lognonné P. A Positive Feedback Between Crustal Thickness and Melt Extraction for the Origin of the Martian Dichotomy. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2022; 127:e2022JE007472. [PMID: 37033153 PMCID: PMC10078261 DOI: 10.1029/2022je007472] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 07/25/2022] [Revised: 10/20/2022] [Accepted: 11/17/2022] [Indexed: 06/19/2023]
Abstract
A North/South difference in crustal thickness is likely at the origin of the Martian dichotomy in topography. Recent crustal thickness maps were obtained by inversion of topography and gravity data seismically anchored at the InSight station. On average, the Martian crust is 51-71 km thick with a southern crust thicker by 18-28 km than the northern one. The origin of this crustal dichotomy is still debated although the hypothesis of a large impact is at present very popular. Here, we propose a new mechanism for the formation of this dichotomy that involves a positive feedback between crustal growth and mantle melting. As the crust is enriched in heat-producing elements, the lid of a one-plate planet is hotter and thinner where the crust is thicker, inducing a larger amount of partial melt below the lid and hence a larger rate of melt extraction and crustal growth. We first demonstrate analytically that larger wavelength perturbations, that is, hemispherical perturbations, grow faster because smaller wavelengths are more attenuated by thermal diffusion. We then use a parameterized thermal evolution model with a well-mixed mantle topped by two different lids characterized by their thermal structures and thicknesses to study the growth of the crust in the two hemispheres. Our results demonstrate that this positive feedback can generate a significant crustal dichotomy.
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Affiliation(s)
- Valentin Bonnet Gibet
- Laboratoire de Géologie de LyonTerre, Planètes, EnvironnementEcole Normale Supérieure de LyonCNRSUniversité de LyonUniversité Claude Bernard Lyon 1Université Jean MonetLyonFrance
| | - Chloé Michaut
- Laboratoire de Géologie de LyonTerre, Planètes, EnvironnementEcole Normale Supérieure de LyonCNRSUniversité de LyonUniversité Claude Bernard Lyon 1Université Jean MonetLyonFrance
- Institut Universitaire de FranceParisFrance
| | - Mark Wieczorek
- Laboratoire LagrangeObservatoire de la Côte d’AzurCNRSUniversité Côte d’AzurNiceFrance
| | - Philippe Lognonné
- CNRSInstitut de physique du globe de ParisUniversité de ParisParisFrance
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16
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Mitrofanov IG, Nikiforov SY, Djachkova MV, Lisov DI, Litvak ML, Sanin AB, Vasavada AR. Water and Chlorine in the Martian Subsurface Along the Traverse of NASA's Curiosity Rover: 1. DAN Measurement Profiles Along the Traverse. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2022; 127:e2022JE007327. [PMID: 36588803 PMCID: PMC9788246 DOI: 10.1029/2022je007327] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 04/06/2022] [Revised: 10/28/2022] [Accepted: 11/06/2022] [Indexed: 06/17/2023]
Abstract
This paper presents estimates of the water and chlorine contents in the subsurface of Gale crater based on the measurements by the Dynamic Albedo of Neutrons (DAN) instrument onboard the NASA Curiosity rover. It is Part 1 of a two-paper series. Data derived both from DAN active and passive measurements are presented in discrete surface areas (pixels) assuming a homogeneous distribution of water within the DAN sensing depth (60 cm) along the traverse of the rover. It is shown that the content of hydrogen, reported as Water Equivalent Hydrogen, varies between almost zero and a maximum of (6.1 ± 0.7) wt.%. The content of absorption equivalent chlorine varies between almost zero and (2.6 ± 0.2) wt.%. Such variations are thought to be related to the different geological processes and environmental conditions present in the strata along the traverse during the evolutionary history of Gale crater. The second paper (Part 2) studies particular properties of water and abundances of neutron absorbing elements at distinct geological regions, that the rover crossed on its way.
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Affiliation(s)
- I. G. Mitrofanov
- Space Research Institute of the Russian Academy of Sciences (IKI)MoscowRussia
| | - S. Y. Nikiforov
- Space Research Institute of the Russian Academy of Sciences (IKI)MoscowRussia
| | - M. V. Djachkova
- Space Research Institute of the Russian Academy of Sciences (IKI)MoscowRussia
| | - D. I. Lisov
- Space Research Institute of the Russian Academy of Sciences (IKI)MoscowRussia
| | - M. L. Litvak
- Space Research Institute of the Russian Academy of Sciences (IKI)MoscowRussia
| | - A. B. Sanin
- Space Research Institute of the Russian Academy of Sciences (IKI)MoscowRussia
| | - A. R. Vasavada
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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17
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Khan SY, Stack KM, Yingst RA, Bergmann K. Characterization of Clasts in the Glen Torridon Region of Gale Crater Observed by the Mars Science Laboratory Curiosity Rover. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2022; 127:e2021JE007095. [PMID: 36588802 PMCID: PMC9788136 DOI: 10.1029/2021je007095] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/26/2021] [Revised: 10/18/2022] [Accepted: 10/23/2022] [Indexed: 06/16/2023]
Abstract
The morphology and composition of clasts have the potential to reveal the nature and extent of erosional processes acting in a region. Dense accumulations of granule- to pebble-sized clasts covering the ground throughout the Glen Torridon region of Gale crater on Mars were studied using data acquired by the Mars Science Laboratory Curiosity rover between sols 2300 and 2593. In this study, measurements of shape, size, texture, and elemental abundance of unconsolidated granules and pebbles within northern Glen Torridon were compiled. Nine primary clast types were identified through stepwise hierarchical clustering, all of which are sedimentary and can be compositionally linked to local bedrock, suggesting relatively short transport distances. Several clast types display features associated with fragmentation along bedding planes and existing cracks in bedrock. These results indicate that Glen Torridon clasts are primarily the product of in-situ physical weathering of local bedrock.
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Affiliation(s)
- Sabrina Y. Khan
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyCAPasadenaUSA
- Department of Earth, Atmospheric, and Planetary SciencesMassachusetts Institute of TechnologyMACambridgeUSA
- Department of Earth and Planetary SciencesJohns Hopkins UniversityMDBaltimoreUSA
| | - Kathryn M. Stack
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyCAPasadenaUSA
| | | | - Kristin Bergmann
- Department of Earth, Atmospheric, and Planetary SciencesMassachusetts Institute of TechnologyMACambridgeUSA
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18
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Nikitczuk MP, Bebout GE, Geiger CA, Ota T, Kunihiro T, Mustard JF, Halldórsson SA, Nakamura E. Nitrogen Incorporation in Potassic and Micro- and Meso-Porous Minerals: Potential Biogeochemical Records and Targets for Mars Sampling. ASTROBIOLOGY 2022; 22:1293-1309. [PMID: 36074082 PMCID: PMC9618379 DOI: 10.1089/ast.2021.0158] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 10/01/2021] [Accepted: 06/27/2022] [Indexed: 06/15/2023]
Abstract
We measured the N concentrations and isotopic compositions of 44 samples of terrestrial potassic and micro- and meso-porous minerals and a small number of whole-rocks to determine the extent to which N is incorporated and stored during weathering and low-temperature hydrothermal alteration in Mars surface/near-surface environments. The selection of these minerals and other materials was partly guided by the study of altered volcanic glass from Antarctica and Iceland, in which the incorporation of N as NH4+ in phyllosilicates is indicated by correlated concentrations of N and the LILEs (i.e., K, Ba, Rb, Cs), with scatter likely related to the presence of exchanged, occluded/trapped, or encapsulated organic/inorganic N occurring within structural cavities (e.g., in zeolites). The phyllosilicates, zeolites, and sulfates analyzed in this study contain between 0 and 99,120 ppm N and have δ15Nair values of -34‰ to +65‰. Most of these minerals, and the few siliceous hydrothermal deposits that were analyzed, have δ15N consistent with the incorporation of biologically processed N during low-temperature hydrothermal or weathering processes. Secondary ion mass spectrometry on altered hyaloclastites demonstrates the residency of N in smectites and zeolites, and silica. We suggest that geological materials known on Earth to incorporate and store N and known to be abundant at, or near, the surface of Mars should be considered targets for upcoming Mars sample return with the intent to identify any signs of ancient or modern life.
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Affiliation(s)
- Matthew P. Nikitczuk
- Department of Earth and Environmental Sciences, Lehigh University, Bethlehem, Pennsylvania, USA
| | - Gray E. Bebout
- Department of Earth and Environmental Sciences, Lehigh University, Bethlehem, Pennsylvania, USA
- Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Japan
| | - Charles A. Geiger
- Universität Salzburg, Fachbereich Chemie und Physik der Materialien, Salzburg, Austria
| | - Tsutomu Ota
- Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Japan
| | - Takuya Kunihiro
- Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Japan
| | - John F. Mustard
- Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, Rhode Island, USA
| | - Sæmundur A. Halldórsson
- Nordic Volcanological Center, Institute of Earth Sciences, University of Iceland, Reykjavík, Iceland
| | - Eizo Nakamura
- Pheasant Memorial Laboratory for Geochemistry and Cosmochemistry, Institute for Planetary Materials, Okayama University, Misasa, Japan
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19
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Ritter B, Diederich-Leicher JL, Binnie SA, Stuart FM, Wennrich V, Bolten A, Dunai TJ. Impact of CaSO 4-rich soil on Miocene surface preservation and Quaternary sinuous to meandering channel forms in the hyperarid Atacama Desert. Sci Rep 2022; 12:17951. [PMID: 36289432 PMCID: PMC9606260 DOI: 10.1038/s41598-022-22787-9] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/23/2022] [Accepted: 10/19/2022] [Indexed: 01/24/2023] Open
Abstract
The Atacama Desert is the driest and oldest desert on Earth. Despite the abundance evidence for long-term landscape stability, there are subtle signs of localised fluvial erosion and deposition since the onset of hyperaridity in the rock record. In the dry core of the Atacama Desert, pluvial episodes allowed antecedent drainage to incise into uplifting fault scarps, which in turn generated sinuous to meandering channels. Incision of ancient alluvial fan surfaces occurred during intermittent fluvial periods, albeit without signs of surface erosion. Fluvial incision during predominantly hyperarid climate periods is evident from these channels in unconsolidated alluvium. The absence of dense vegetation to provide bank stability and strength led us to investigate the potential role of regionally ubiquitous CaSO4-rich surface cover. This has enabled the preservation of Miocene surfaces and we hypothesize that it provided the required bank stability by adding strength to the upper decimetre to meter of incised alluvium to allow high sinuosity of stream channels to form during pluvial episodes in the Quaternary.
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Affiliation(s)
- Benedikt Ritter
- grid.6190.e0000 0000 8580 3777Institute of Geology & Mineralogy, University of Cologne, Cologne, Germany
| | - Julia L. Diederich-Leicher
- grid.6190.e0000 0000 8580 3777Institute of Geology & Mineralogy, University of Cologne, Cologne, Germany
| | - Steven A. Binnie
- grid.6190.e0000 0000 8580 3777Institute of Geology & Mineralogy, University of Cologne, Cologne, Germany
| | - Finlay M. Stuart
- grid.224137.10000 0000 9762 0345Isotope Geosciences Unit, Scottish Universities Environmental Research Centre, East Kilbride, UK
| | - Volker Wennrich
- grid.6190.e0000 0000 8580 3777Institute of Geology & Mineralogy, University of Cologne, Cologne, Germany
| | - Andreas Bolten
- grid.6190.e0000 0000 8580 3777Institute of Geography, University of Cologne, Cologne, Germany
| | - Tibor J. Dunai
- grid.6190.e0000 0000 8580 3777Institute of Geology & Mineralogy, University of Cologne, Cologne, Germany
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20
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Wu JH, McGenity TJ, Rettberg P, Simões MF, Li WJ, Antunes A. The archaeal class Halobacteria and astrobiology: Knowledge gaps and research opportunities. Front Microbiol 2022; 13:1023625. [PMID: 36312929 PMCID: PMC9608585 DOI: 10.3389/fmicb.2022.1023625] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/20/2022] [Accepted: 09/07/2022] [Indexed: 09/19/2023] Open
Abstract
Water bodies on Mars and the icy moons of the outer solar system are now recognized as likely being associated with high levels of salt. Therefore, the study of high salinity environments and their inhabitants has become increasingly relevant for Astrobiology. Members of the archaeal class Halobacteria are the most successful microbial group living in hypersaline conditions and are recognized as key model organisms for exposure experiments. Despite this, data for the class is uneven across taxa and widely dispersed across the literature, which has made it difficult to properly assess the potential for species of Halobacteria to survive under the polyextreme conditions found beyond Earth. Here we provide an overview of published data on astrobiology-linked exposure experiments performed with members of the Halobacteria, identifying clear knowledge gaps and research opportunities.
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Affiliation(s)
- Jia-Hui Wu
- State Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology (MUST), Taipa, Macau SAR, China
- China National Space Administration (CNSA), Macau Center for Space Exploration and Science, Taipa, Macau SAR, China
| | - Terry J. McGenity
- School of Life Sciences, University of Essex, Colchester, United Kingdom
| | - Petra Rettberg
- German Aerospace Center (DLR), Institute of Aerospace Medicine, Köln, Germany
| | - Marta F. Simões
- State Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology (MUST), Taipa, Macau SAR, China
- China National Space Administration (CNSA), Macau Center for Space Exploration and Science, Taipa, Macau SAR, China
| | - Wen-Jun Li
- State Key Laboratory of Biocontrol, Guangdong Provincial Key Laboratory of Plant Resources and Southern Marine Science and Engineering Guangdong Laboratory (Zhuhai), School of Life Sciences, Sun Yat-sen University, Guangzhou, China
| | - André Antunes
- State Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology (MUST), Taipa, Macau SAR, China
- China National Space Administration (CNSA), Macau Center for Space Exploration and Science, Taipa, Macau SAR, China
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21
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Demaret L, Hutchinson IB, Ingley R, Edwards HGM, Fagel N, Compere P, Javaux EJ, Eppe G, Malherbe C. Fe-Rich Fossil Vents as Mars Analog Samples: Identification of Extinct Chimneys in Miocene Marine Sediments Using Raman Spectroscopy, X-Ray Diffraction, and Scanning Electron Microscopy-Energy Dispersive X-Ray Spectroscopy. ASTROBIOLOGY 2022; 22:1081-1098. [PMID: 35704291 DOI: 10.1089/ast.2021.0128] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/15/2023]
Abstract
On Earth, the circulation of Fe-rich fluids in hydrothermal environments leads to characteristic iron mineral deposits, reflecting the pH and redox chemical conditions of the hydrothermal system, and is often associated with chemotroph microorganisms capable of deriving energy from chemical gradients. On Mars, iron-rich hydrothermal sites are considered to be potentially important astrobiological targets for searching evidence of life during exploration missions, such as the Mars 2020 and the ExoMars 2022 missions. In this study, an extinct hydrothermal chimney from the Jaroso hydrothermal system (SE Spain), considered an interesting geodynamic and mineralogical terrestrial analog for Mars, was analyzed using Raman spectroscopy, X-ray diffraction, and scanning electron microscopy coupled with energy dispersive X-ray spectroscopy. The sample consists of a fossil vent in a Miocene shallow-marine sedimentary deposit composed of a marl substrate, an iron-rich chimney pipe, and a central space filled with backfilling deposits and vent condensates. The iron crust is particularly striking due to the combined presence of molecular and morphological indications of a microbial colonization, including mineral microstructures (e.g., stalks, filaments), iron oxyhydroxide phases (altered goethite, ferrihydrite), and organic signatures (carotenoids, organopolymers). The clear identification of pigments by resonance Raman spectroscopy and the preservation of organics in association with iron oxyhydroxides by Raman microimaging demonstrate that the iron crust was indeed colonized by microbial communities. These analyses confirm that Raman spectroscopy is a powerful tool for documenting the habitability of such historical hydrothermal environments. Finally, based on the results obtained, we propose that the ancient iron-rich hydrothermal pipes should be recognized as singular terrestrial Mars analog specimens to support the preparatory work for robotic in situ exploration missions to Mars, as well as during the subsequent interpretation of data returned by those missions.
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Affiliation(s)
- Lucas Demaret
- Mass Spectrometry Laboratory, MolSys Research Unit, University of Liege, Liege, Belgium
- Early Life Traces & Evolution-Astrobiology, UR Astrobiology, University of Liege, Liege, Belgium
| | - Ian B Hutchinson
- Department of Physics and Astronomy, University of Leicester, Leicester, United Kingdom
| | - Richard Ingley
- Department of Physics and Astronomy, University of Leicester, Leicester, United Kingdom
| | - Howell G M Edwards
- Department of Physics and Astronomy, University of Leicester, Leicester, United Kingdom
| | - Nathalie Fagel
- Laboratory Argiles, Géochimie et Environnements Sédimentaires, University of Liege, Liege, Belgium
| | - Philippe Compere
- Laboratory of Functional and Evolutionary Morphology, UR FOCUS, and Centre for Applied Research and Education in Microscopy (CAREM), University of Liege, Liege, Belgium
| | - Emmanuelle J Javaux
- Early Life Traces & Evolution-Astrobiology, UR Astrobiology, University of Liege, Liege, Belgium
| | - Gauthier Eppe
- Mass Spectrometry Laboratory, MolSys Research Unit, University of Liege, Liege, Belgium
| | - Cédric Malherbe
- Mass Spectrometry Laboratory, MolSys Research Unit, University of Liege, Liege, Belgium
- Early Life Traces & Evolution-Astrobiology, UR Astrobiology, University of Liege, Liege, Belgium
- Department of Physics and Astronomy, University of Leicester, Leicester, United Kingdom
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22
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Understanding redox processes during iron precipitation in standing water: implications in formation of iron oxides minerals in the terrestrial planetary environment (especially Mars). PROCEEDINGS OF THE INDIAN NATIONAL SCIENCE ACADEMY 2022. [DOI: 10.1007/s43538-022-00092-3] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/15/2022]
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23
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Bonales LJ, Muñoz-Iglesias V, Prieto-Ballesteros O, Mateo-Martí E. Preservation of glycine coordination compounds under a gamma radiation dose representative of natural mars radioactivity. Sci Rep 2022; 12:13677. [PMID: 35953504 PMCID: PMC9372174 DOI: 10.1038/s41598-022-17802-y] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/22/2021] [Accepted: 07/31/2022] [Indexed: 11/09/2022] Open
Abstract
The Martian subsurface is more favorable for organic preservation than its surface because of the shielding effect of rocks from cosmic rays and UV radiation with increasing depth. Nevertheless, the natural radioactivity on Mars owing to U, Th, and K must be considered to study the possible extant and/or extinct life. Here, we demonstrate the importance of natural radiation on the amino acid glycine in two different chemical environments, GlyFeSO4 5H2O and GlyMgSO4 5H2O, which are coordination compounds considered relevant to Mars. The results show that after a 600 kGy dose of gamma radiation, glycine was more stable when it bonded to Mg in the GlyMgSO4 5H2O coordination compound, it was less stable when it bonded to Fe in the GlyFeSO4 5H2O compound. Studies on the effects of gamma radiation on preservation of organic molecules bound to minerals and other potential compounds on Mars are significantly important in the search for biosignatures.
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Affiliation(s)
- Laura J Bonales
- Departamento de Evolución Molecular, Spanish Centre for Astrobiology, (CAB-CSIC), Instituto Nacional de Técnica Aeroespacial (INTA), Carretera de Ajalvir km 4, Torrejón de Ardoz, 28850, Madrid, Spain.
| | - Victoria Muñoz-Iglesias
- Departamento de Evolución Molecular, Spanish Centre for Astrobiology, (CAB-CSIC), Instituto Nacional de Técnica Aeroespacial (INTA), Carretera de Ajalvir km 4, Torrejón de Ardoz, 28850, Madrid, Spain
- Departamento de Planetología y habitabilidad, Spanish Centre for Astrobiology, (CAB-CSIC), Instituto Nacional de Técnica Aeroespacial (INTA), Carretera de Ajalvir km 4, Torrejón de Ardoz, 28850, Madrid, Spain
| | - Olga Prieto-Ballesteros
- Departamento de Evolución Molecular, Spanish Centre for Astrobiology, (CAB-CSIC), Instituto Nacional de Técnica Aeroespacial (INTA), Carretera de Ajalvir km 4, Torrejón de Ardoz, 28850, Madrid, Spain
- Departamento de Planetología y habitabilidad, Spanish Centre for Astrobiology, (CAB-CSIC), Instituto Nacional de Técnica Aeroespacial (INTA), Carretera de Ajalvir km 4, Torrejón de Ardoz, 28850, Madrid, Spain
| | - Eva Mateo-Martí
- Departamento de Evolución Molecular, Spanish Centre for Astrobiology, (CAB-CSIC), Instituto Nacional de Técnica Aeroespacial (INTA), Carretera de Ajalvir km 4, Torrejón de Ardoz, 28850, Madrid, Spain
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24
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Concept and Design of Martian Far-IR ORE Spectrometer (MIRORES). REMOTE SENSING 2022. [DOI: 10.3390/rs14122799] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
Sulfide ores are a major source of noble (Au, Ag, and Pt) and base (Cu, Pb, Zn, Sn, Co, Ni, etc.) metals and will, therefore, be vital for the self-sustainment of future Mars colonies. Martian meteorites are rich in sulfides, which is reflected in recent findings for surface Martian rocks analyzed by the Spirit and Curiosity rovers. However, the only high-resolution (18 m/pixel) infrared (IR) spectrometer orbiting Mars, the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM), onboard the Mars Reconnaissance Orbiter (MRO), is not well-suited for detecting sulfides on the Martian surface. Spectral interference with silicates impedes sulfide detection in the 0.4–3.9 μm CRISM range. In contrast, at least three common hydrothermal sulfides on Earth and Mars (pyrite, chalcopyrite, marcasite) have prominent absorption peaks in a narrow far-IR (FIR) wavelength range of 23–28 μm. Identifying the global distribution and chemical composition of sulfide ore deposits would help in choosing useful targets for future Mars exploration missions. Therefore, we have designed a new instrument suitable for measuring sulfides in the FIR range called the Martian far-IR Ore Spectrometer (MIRORES). MIRORES will measure radiation in six narrow bands (~0.3 µm in width), including three bands centered on the sulfide absorption bands (23.2, 24.3 and 27.6 µm), two reference bands (21.5 and 26.1) and one band for clinopyroxene interference (29.0 µm). Focusing on sulfides only will make it possible to adapt the instrument size (32 × 32 × 42 cm) and mass (<10 kg) to common microsatellite requirements. The biggest challenges related to this design are: (1) the small field of view conditioned by the high resolution required for such a study (<20 m/pixel), which, in limited space, can only be achieved by the use of the Cassegrain optical system; and (2) a relatively stable measurement temperature to maintain radiometric accuracy and enable precise calibration.
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25
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Stack KM, Dietrich WE, Lamb MP, Sullivan RJ, Christian JR, Newman CE, O’Connell‐Cooper CD, Sneed JW, Day M, Baker M, Arvidson RE, Fedo CM, Khan S, Williams RME, Bennett KA, Bryk AB, Cofield S, Edgar LA, Fox VK, Fraeman AA, House CH, Rubin DM, Sun VZ, Van Beek JK. Orbital and In-Situ Investigation of Periodic Bedrock Ridges in Glen Torridon, Gale Crater, Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2022; 127:e2021JE007096. [PMID: 35865672 PMCID: PMC9286800 DOI: 10.1029/2021je007096] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 10/18/2021] [Revised: 05/03/2022] [Accepted: 05/07/2022] [Indexed: 06/15/2023]
Abstract
Gale crater, the field site for NASA's Mars Science Laboratory Curiosity rover, contains a diverse and extensive record of aeolian deposition and erosion. This study focuses on a series of regularly spaced, curvilinear, and sometimes branching bedrock ridges that occur within the Glen Torridon region on the lower northwest flank of Aeolis Mons, the central mound within Gale crater. During Curiosity's exploration of Glen Torridon between sols ∼2300-3080, the rover drove through this field of ridges, providing the opportunity for in situ observation of these features. This study uses orbiter and rover data to characterize ridge morphology, spatial distribution, compositional and material properties, and association with other aeolian features in the area. Based on these observations, we find that the Glen Torridon ridges are consistent with an origin as wind-eroded bedrock ridges, carved during the exhumation of Mount Sharp. Erosional features like the Glen Torridon ridges observed elsewhere on Mars, termed periodic bedrock ridges (PBRs), have been interpreted to form transverse to the dominant wind direction. The size and morphology of the Glen Torridon PBRs are consistent with transverse formative winds, but the orientation of nearby aeolian bedforms and bedrock erosional features raise the possibility of PBR formation by a net northeasterly wind regime. Although several formation models for the Glen Torridon PBRs are still under consideration, and questions persist about the nature of PBR-forming paleowinds, the presence of PBRs at this site provides important constraints on the depositional and erosional history of Gale crater.
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Affiliation(s)
- Kathryn M. Stack
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - William E. Dietrich
- Department of Earth and Planetary ScienceUniversity of California, BerkeleyBerkeleyCAUSA
| | - Michael P. Lamb
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - Robert J. Sullivan
- Cornell Center for Astrophysics & Planetary ScienceCornell UniversityIthacaNYUSA
| | - John R. Christian
- Department of Earth and Planetary SciencesWashington University in St. LouisSt. LouisMOUSA
| | | | | | - Jonathan W. Sneed
- Department of Earth, Planetary, and Space SciencesUniversity of California, Los AngelesLos AngelesCAUSA
| | - Mackenzie Day
- Department of Earth, Planetary, and Space SciencesUniversity of California, Los AngelesLos AngelesCAUSA
| | - Mariah Baker
- Center for Earth & Planetary StudiesNational Air & Space MuseumSmithsonian InstitutionWashingtonDCUSA
| | - Raymond E. Arvidson
- Department of Earth and Planetary SciencesWashington University in St. LouisSt. LouisMOUSA
| | - Christopher M. Fedo
- Department of Earth and Planetary SciencesUniversity of Tennessee, KnoxvilleKnoxvilleTNUSA
| | - Sabrina Khan
- Department of Earth, Atmospheric, and Planetary SciencesMassachusetts Institute of TechnologyCambridgeMAUSA
| | | | | | - Alexander B. Bryk
- Department of Earth and Planetary ScienceUniversity of California, BerkeleyBerkeleyCAUSA
| | - Shannon Cofield
- U.S. Department of the InteriorBureau of Ocean Energy ManagementWashingtonDCUSA
| | - Lauren A. Edgar
- Astrogeology Science CenterU.S. Geological SurveyFlagstaffAZUSA
| | - Valerie K. Fox
- Earth and Environmental SciencesUniversity of MinnesotaMinneapolisMNUSA
| | - Abigail A. Fraeman
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | - David M. Rubin
- Earth and Planetary SciencesUniversity of California, Santa CruzSanta CruzCAUSA
| | - Vivian Z. Sun
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - Jason K. Van Beek
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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26
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Liu Y, Wu X, Zhao YYS, Pan L, Wang C, Liu J, Zhao Z, Zhou X, Zhang C, Wu Y, Wan W, Zou Y. Zhurong reveals recent aqueous activities in Utopia Planitia, Mars. SCIENCE ADVANCES 2022; 8:eabn8555. [PMID: 35544566 PMCID: PMC9094648 DOI: 10.1126/sciadv.abn8555] [Citation(s) in RCA: 2] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/15/2023]
Abstract
The Mars' climate is cold and dry in the most recent epoch, and liquid water activities are considered extremely limited. Previous orbital data only show sporadic hydrous minerals in the northern lowlands of Mars excavated by large impacts. Using the short-wave infrared spectral data obtained by the Zhurong rover of China's Tianwen-1 mission, which landed in southern Utopia Planitia on Mars, we identify hydrated sulfate/silica materials on the Amazonian terrain at the landing site. These hydrated minerals are associated with bright-toned rocks, interpreted to be duricrust developed locally. The lithified duricrusts suggest that formation with substantial liquid water originates by either groundwater rising or subsurface ice melting. In situ evidence for aqueous activities identified at Zhurong's landing site indicates a more active Amazonian hydrosphere for Mars than previously thought.
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Affiliation(s)
- Yang Liu
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China
- Center for Excellence in Comparative Planetology, Chinese Academy of Sciences, Hefei 200083, China
- Corresponding author.
| | - Xing Wu
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China
| | - Yu-Yan Sara Zhao
- Center for Excellence in Comparative Planetology, Chinese Academy of Sciences, Hefei 200083, China
- Center for Lunar and Planetary Sciences, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang 550081, China
| | - Lu Pan
- Center for Star and Planet Formation, GLOBE Institute, University of Copenhagen, Copenhagen, Denmark
| | - Chi Wang
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China
| | - Jia Liu
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China
| | - Zhenxing Zhao
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China
- University of Chinese Academy of Sciences, Beijing 100049, China
| | - Xiang Zhou
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China
- University of Chinese Academy of Sciences, Beijing 100049, China
| | - Chaolin Zhang
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China
- University of Chinese Academy of Sciences, Beijing 100049, China
| | - Yuchun Wu
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China
- University of Chinese Academy of Sciences, Beijing 100049, China
| | - Wenhui Wan
- State Key Laboratory of Remote Sensing Science, Aerospace Information Research Institute, Chinese Academy of Sciences, Beijing 100101, China
| | - Yongliao Zou
- State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China
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27
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Vasavada AR. Mission Overview and Scientific Contributions from the Mars Science Laboratory Curiosity Rover After Eight Years of Surface Operations. SPACE SCIENCE REVIEWS 2022; 218:14. [PMID: 35399614 PMCID: PMC8981195 DOI: 10.1007/s11214-022-00882-7] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 03/20/2021] [Accepted: 03/21/2022] [Indexed: 06/14/2023]
Abstract
UNLABELLED NASA's Mars Science Laboratory mission, with its Curiosity rover, has been exploring Gale crater (5.4° S, 137.8° E) since 2012 with the goal of assessing the potential of Mars to support life. The mission has compiled compelling evidence that the crater basin accumulated sediment transported by marginal rivers into lakes that likely persisted for millions of years approximately 3.6 Ga ago in the early Hesperian. Geochemical and mineralogical assessments indicate that environmental conditions within this timeframe would have been suitable for sustaining life, if it ever were present. Fluids simultaneously circulated in the subsurface and likely existed through the dry phases of lake bed exposure and aeolian deposition, conceivably creating a continuously habitable subsurface environment that persisted to less than 3 Ga in the early Amazonian. A diversity of organic molecules has been preserved, though degraded, with evidence for more complex precursors. Solid samples show highly variable isotopic abundances of sulfur, chlorine, and carbon. In situ studies of modern wind-driven sediment transport and multiple large and active aeolian deposits have led to advances in understanding bedform development and the initiation of saltation. Investigation of the modern atmosphere and environment has improved constraints on the timing and magnitude of atmospheric loss, revealed the presence of methane and the crater's influence on local meteorology, and provided measurements of high-energy radiation at Mars' surface in preparation for future crewed missions. Rover systems and science instruments remain capable of addressing all key scientific objectives. Emphases on advance planning, flexibility, operations support work, and team culture have allowed the mission team to maintain a high level of productivity in spite of declining rover power and funding. SUPPLEMENTARY INFORMATION The online version contains supplementary material available at 10.1007/s11214-022-00882-7.
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Affiliation(s)
- Ashwin R. Vasavada
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA USA
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Chirality in Organic and Mineral Systems: A Review of Reactivity and Alteration Processes Relevant to Prebiotic Chemistry and Life Detection Missions. Symmetry (Basel) 2022. [DOI: 10.3390/sym14030460] [Citation(s) in RCA: 10] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/01/2023] Open
Abstract
Chirality is a central feature in the evolution of biological systems, but the reason for biology’s strong preference for specific chiralities of amino acids, sugars, and other molecules remains a controversial and unanswered question in origins of life research. Biological polymers tend toward homochiral systems, which favor the incorporation of a single enantiomer (molecules with a specific chiral configuration) over the other. There have been numerous investigations into the processes that preferentially enrich one enantiomer to understand the evolution of an early, racemic, prebiotic organic world. Chirality can also be a property of minerals; their interaction with chiral organics is important for assessing how post-depositional alteration processes could affect the stereochemical configuration of simple and complex organic molecules. In this paper, we review the properties of organic compounds and minerals as well as the physical, chemical, and geological processes that affect organic and mineral chirality during the preservation and detection of organic compounds. We provide perspectives and discussions on the reactions and analytical techniques that can be performed in the laboratory, and comment on the state of knowledge of flight-capable technologies in current and future planetary missions, with a focus on organics analysis and life detection.
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Kloprogge JT(T, Hartman H. Clays and the Origin of Life: The Experiments. Life (Basel) 2022; 12:259. [PMID: 35207546 PMCID: PMC8880559 DOI: 10.3390/life12020259] [Citation(s) in RCA: 9] [Impact Index Per Article: 4.5] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/16/2021] [Revised: 01/08/2022] [Accepted: 02/01/2022] [Indexed: 12/15/2022] Open
Abstract
There are three groups of scientists dominating the search for the origin of life: the organic chemists (the Soup), the molecular biologists (RNA world), and the inorganic chemists (metabolism and transient-state metal ions), all of which have experimental adjuncts. It is time for Clays and the Origin of Life to have its experimental adjunct. The clay data coming from Mars and carbonaceous chondrites have necessitated a review of the role that clays played in the origin of life on Earth. The data from Mars have suggested that Fe-clays such as nontronite, ferrous saponites, and several other clays were formed on early Mars when it had sufficient water. This raised the question of the possible role that these clays may have played in the origin of life on Mars. This has put clays front and center in the studies on the origin of life not only on Mars but also here on Earth. One of the major questions is: What was the catalytic role of Fe-clays in the origin and development of metabolism here on Earth? First, there is the recent finding of a chiral amino acid (isovaline) that formed on the surface of a clay mineral on several carbonaceous chondrites. This points to the formation of amino acids on the surface of clay minerals on carbonaceous chondrites from simpler molecules, e.g., CO2, NH3, and HCN. Additionally, there is the catalytic role of small organic molecules, such as dicarboxylic acids and amino acids found on carbonaceous chondrites, in the formation of Fe-clays themselves. Amino acids and nucleotides adsorb on clay surfaces on Earth and subsequently polymerize. All of these observations and more must be subjected to strict experimental analysis. This review provides an overview of what has happened and is now happening in the experimental clay world related to the origin of life. The emphasis is on smectite-group clay minerals, such as montmorillonite and nontronite.
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Affiliation(s)
- Jacob Teunis (Theo) Kloprogge
- School of Earth and Environmental Sciences, The University of Queensland, Brisbane, QLD 4072, Australia
- Department of Chemistry, College of Arts and Sciences, University of the Philippines Visayas, Miagao 5023, Philippines
| | - Hyman Hartman
- Department of Earth Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA
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Abstract
The current Martian climate is not habitable and far from Earth’s climate. At the same time that life spread on Earth (3 Gy ago), the Red Planet was possibly more similar to our Blue Planet. Our model includes a coupled model with dynamic ocean and atmosphere including a hydrological cycle and a simplified glacier mass flux scheme. We show that an ocean is stable in agreement with interpretations of the surface geological records. What was the nature of the Late Hesperian climate, warm and wet or cold and dry? Formulated this way the question leads to an apparent paradox since both options seem implausible. A warm and wet climate would have produced extensive fluvial erosion but few valley networks have been observed at the age of the Late Hesperian. A too cold climate would have kept any northern ocean frozen most of the time. A moderate cold climate would have transferred the water from the ocean to the land in the form of snow and ice. But this would prevent tsunami formation, for which there is some evidence. Here, we provide insights from numerical climate simulations in agreement with surface geological features to demonstrate that the Martian climate could have been both cold and wet. Using an advanced general circulation model (GCM), we demonstrate that an ocean can be stable, even if the Martian mean surface temperature is lower than 0 °C. Rainfall is moderate near the shorelines and in the ocean. The southern plateau is mostly covered by ice with a mean temperature below 0 °C and a glacier return flow back to the ocean. This climate is achieved with a 1-bar CO2-dominated atmosphere with 10% H2. Under this scenario of 3 Ga, the geologic evidence of a shoreline and tsunami deposits along the ocean/land dichotomy are compatible with ice sheets and glacial valleys in the southern highlands.
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Cockell CS. Bridging the gap between microbial limits and extremes in space: space microbial biotechnology in the next 15 years. Microb Biotechnol 2022; 15:29-41. [PMID: 34534397 PMCID: PMC8719799 DOI: 10.1111/1751-7915.13927] [Citation(s) in RCA: 7] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [Abstract] [MESH Headings] [Grants] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/05/2021] [Accepted: 09/05/2021] [Indexed: 12/01/2022] Open
Abstract
The establishment of a permanent human settlement in space is one of humanity's ambitions. To achieve this, microorganisms will be used to carry out many functions such as recycling, food and pharmaceutical production, mining and other processes. However, the physical and chemical extremes in all locations beyond Earth exceed known growth limits of microbial life. Making microbes more tolerant of a greater range of extraterrestrial extremes will not produce organisms that can grow in unmodified extraterrestrial environments since in many of them not even liquid water can exist. However, by narrowing the gap, the engineering demands on bioindustrial processes can be reduced and greater robustness can be incorporated into the biological component. I identify and describe these required microbial biotechnological modifications and speculate on long-term possibilities such as microbial biotechnology on Saturn's moon Titan to support a human presence in the outer Solar System and bioprocessing of asteroids. A challenge for space microbial biotechnology in the coming decades is to narrow the microbial gap by systemically identifying the genes required to do this and incorporating them into microbial systems that can be used to carry out bioindustrial processes of interest.
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Affiliation(s)
- Charles S. Cockell
- UK Centre for AstrobiologySchool of Physics and AstronomyUniversity of EdinburghEdinburghUK
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Williams RM, Irwin RP, Noe Dobrea EZ, Howard AD, Dietrich WE, Cawley J. Inverted channel variations identified on a distal portion of a bajada in the central Atacama Desert, Chile. GEOMORPHOLOGY (AMSTERDAM, NETHERLANDS) 2021; 393:107925. [PMID: 34785830 PMCID: PMC8587680 DOI: 10.1016/j.geomorph.2021.107925] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
In deserts, the interplay between occasional fluvial events and persistent aeolian erosion can form composite modern and relict surfaces, especially on the distal portion of alluvial fans. There, relief inversion of alluvial deposits by differential erosion can form longitudinal ridges. We identified two distinct ridge types formed by relief inversion on converging alluvial fans in the hyperarid Chilean Atacama Desert. Although they are co-located and similar in scale, the ridge types have different ages and formation histories that apparently correspond to minor paleoclimate variations. Gravel-armored ridges are remnants of deflated alluvial deposits with a bimodal sediment distribution (gravel and sand) dated to a minor pluvial phase at the end of the Late Pleistocene (~12 kyr). In contrast, younger (~9 kyr) sulfate-capped ridges formed during a minor arid phase with evaporite deposition in a pre-existing channel that armored the underlying deposits. Collectively, inverted channels at Salar de Llamara resulted from multiple episodes of surface overland flow and standing water spanning several thousand years. Based on ridge relief and age, the minimum long-term deflation rate is 0.1-0.2 m/kyr, driven primarily by wind erosion. This case study is an example of the equifinality concept whereby different processes lead to similar landforms. The complex history of the two ridge types can only be generally constrained in remotely sensed data. In situ observations are required to discern the specifics of the aqueous history, including the flow type, magnitude, sequence, and paleoenvironment. These findings have relevance for interpreting similar landforms on Mars.
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Affiliation(s)
- Rebecca M.E. Williams
- Planetary Science Institute, 1700 E. Fort Lowell, Suite 106, Tucson, AZ 85719, United States of America
| | - Rossman P. Irwin
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, PO Box 37012, MRC 315, Washington, DC 20013-7012, United States of America
| | - Eldar Z. Noe Dobrea
- Planetary Science Institute, 1700 E. Fort Lowell, Suite 106, Tucson, AZ 85719, United States of America
| | - Alan D. Howard
- Planetary Science Institute, 1700 E. Fort Lowell, Suite 106, Tucson, AZ 85719, United States of America
| | - William E. Dietrich
- Earth & Planetary Science, University of California—Berkeley, 307 McCone Hall, Berkeley, CA 94720, United States of America
| | - J.C. Cawley
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, PO Box 37012, MRC 315, Washington, DC 20013-7012, United States of America
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Ye T, Wang B, Li C, Bian P, Chen L, Wang G. Exposure of cyanobacterium Nostoc sp. to the Mars-like stratosphere environment. JOURNAL OF PHOTOCHEMISTRY AND PHOTOBIOLOGY B-BIOLOGY 2021; 224:112307. [PMID: 34649187 DOI: 10.1016/j.jphotobiol.2021.112307] [Citation(s) in RCA: 8] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/26/2021] [Revised: 08/25/2021] [Accepted: 09/09/2021] [Indexed: 01/19/2023]
Abstract
During the HH-19-2 flight mission of the Chinese Scientific Experimental System, dried Nostoc sp. cells were exposed to the stratosphere environment (32,508 m altitude) for 3 h and 22 min. The atmospheric pressure, temperature, relative humidity, and ionizing and non-ionizing radiation levels at that altitude are similar to those on the surface of Mars. Although analyses revealed decreased photosynthetic activity, a decline in autofluorescence, and damage to the cellular morphology in the flight-exposed sample, the death rate was low (28%). Physiological changes were not obvious after the exposure to the Mars-like vacuum conditions. The ground-exposed samples showed a similar trend to the flight-exposed samples, but the damage was relatively slight. RNA-sequencing data revealed a number of affected metabolic pathways: photosynthetic system and CO2 fixation function, activation of antioxidant systems, heat shock protein, DNA repair, and protein synthesis. Results suggest that Nostoc sp. has the potential to survive in a Mars-like environment and that it may be a suitable pioneer species to colonize Mars in the future in closed life-support systems (base) or in localities with relatively suitable conditions for life, such as localities with water available.
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Affiliation(s)
- Tong Ye
- Key Laboratory of Algal Biology, Institute of Hydrobiology, Chinese Academy of Sciences, Wuhan 430072, China; University of Chinese Academy of Sciences, Beijing 100049, China
| | - Bo Wang
- Key Laboratory of Algal Biology, Institute of Hydrobiology, Chinese Academy of Sciences, Wuhan 430072, China; University of Chinese Academy of Sciences, Beijing 100049, China
| | - Caiyan Li
- Key Laboratory of Algal Biology, Institute of Hydrobiology, Chinese Academy of Sciences, Wuhan 430072, China; University of Chinese Academy of Sciences, Beijing 100049, China
| | - Po Bian
- Key Laboratory of Ion Beam Bio-engineering, Hefei Institutes of Physical Science, Chinese Academy of Sciences and Anhui Province, Hefei, Anhui 230031, China
| | - Lanzhou Chen
- School of Resource & Environmental Sciences, Wuhan University, Wuhan 430079, PR China
| | - Gaohong Wang
- Key Laboratory of Algal Biology, Institute of Hydrobiology, Chinese Academy of Sciences, Wuhan 430072, China; University of Chinese Academy of Sciences, Beijing 100049, China.
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Merging Perspectives on Secondary Minerals on Mars: A Review of Ancient Water-Rock Interactions in Gale Crater Inferred from Orbital and In-Situ Observations. MINERALS 2021. [DOI: 10.3390/min11090986] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 01/20/2023]
Abstract
Phyllosilicates, sulfates, and Fe oxides are the most prevalent secondary minerals detected on Mars from orbit and the surface, including in the Mars Science Laboratory Curiosity rover’s field site at Gale crater. These records of aqueous activity have been investigated in detail in Gale crater, where Curiosity’s X-ray diffractometer allows for direct observation and detailed characterization of mineral structure and abundance. This capability provides critical ground truthing to better understand how to interpret Martian mineralogy inferred from orbital datasets. Curiosity is about to leave behind phyllosilicate-rich strata for more sulfate-rich terrains, while the Mars 2020 Perseverance rover is in its early exploration of ancient sedimentary strata in Jezero crater. It is thus an appropriate time to review Gale crater’s mineral distribution from multiple perspectives, utilizing the range of chemical, mineralogical, and spectral measurements provided by orbital and in situ observations. This review compares orbital predictions of composition in Gale crater with higher fidelity (but more spatially restricted) in situ measurements by Curiosity, and we synthesize how this information contributes to our understanding of water-rock interaction in Gale crater. In the context of combining these disparate spatial scales, we also discuss implications for the larger understanding of martian surface evolution and the need for a wide range of data types and scales to properly reconstruct ancient geologic processes using remote methods.
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A Review of the Phyllosilicates in Gale Crater as Detected by the CheMin Instrument on the Mars Science Laboratory, Curiosity Rover. MINERALS 2021. [DOI: 10.3390/min11080847] [Citation(s) in RCA: 10] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/20/2022]
Abstract
Curiosity, the Mars Science Laboratory (MSL) rover, landed on Mars in August 2012 to investigate the ~3.5-billion-year-old (Ga) fluvio-lacustrine sedimentary deposits of Aeolis Mons (informally known as Mount Sharp) and the surrounding plains (Aeolis Palus) in Gale crater. After nearly nine years, Curiosity has traversed over 25 km, and the Chemistry and Mineralogy (CheMin) X-ray diffraction instrument on-board Curiosity has analyzed 30 drilled rock and three scooped soil samples to date. The principal strategic goal of the mission is to assess the habitability of Mars in its ancient past. Phyllosilicates are common in ancient Martian terrains dating to ~3.5–4 Ga and were detected from orbit in some of the lower strata of Mount Sharp. Phyllosilicates on Earth are important for harboring and preserving organics. On Mars, phyllosilicates are significant for exploration as they are hypothesized to be a marker for potential habitable environments. CheMin data demonstrate that ancient fluvio-lacustrine rocks in Gale crater contain up to ~35 wt. % phyllosilicates. Phyllosilicates are key indicators of past fluid–rock interactions, and variation in the structure and composition of phyllosilicates in Gale crater suggest changes in past aqueous environments that may have been habitable to microbial life with a variety of possible energy sources.
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36
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Adams D, Luo Y, Wong ML, Dunn P, Christensen M, Dong C, Hu R, Yung Y. Nitrogen Fixation at Early Mars. ASTROBIOLOGY 2021; 21:968-980. [PMID: 34339294 DOI: 10.1089/ast.2020.2273] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
The Mars Science Laboratory (MSL) recently discovered nitrates in Gale Crater (e.g., Stern et al., 2015; Sutter et al., 2017). One possible mechanism for ancient nitrate deposition on Mars is through HNOx formation and rain out in the atmosphere, for which lightning-induced NO is likely the fundamental source. This study investigates nitrogen (N2) fixation in early Mars' atmosphere, with implications for early Mars' habitability. We consider a 1 bar atmosphere of background CO2, with abundance of N2, hydrogen, and methane varied from 1% to 10% to explore a swath of potential early Mars climates. We derive lightning-induced thermochemical equilibrium fluxes of NO and HCN by coupling the lightning-rate parametrization from the study of Romps et al. (2014) with chemical equilibrium with applications, and we use a Geant4 simulation platform to estimate the effect of solar energetic particle events. These fluxes are used as input into KINETICS, the Caltech/JPL coupled photochemistry and transport code, which models the chemistry of 50 species linked by 495 reactions to derive rain-out fluxes of HNOx and HCN. We compute equilibrium concentrations of cyanide and nitrate in a putative northern ocean at early Mars, assuming hydrothermal vent circulation and photoreduction act as the dominant loss mechanisms. We find average oceanic concentrations of ∼0.1-2 nM nitrate and ∼0.01-2 mM cyanide. HCN is critical for protein synthesis at concentrations >0.01 M (e.g., Holm and Neubeck, 2009), and our result is astrobiologically significant if secondary local concentration mechanisms occurred. Nitrates may act as high-potential electron acceptors for early metabolisms, although the minimum concentration required is unknown. Our study derives concentrations that will be useful for future laboratory studies to investigate the habitability at early Mars. The aqueous nitrate concentrations correspond to surface nitrate precipitates of ∼1-8 × 10-4 wt % that may have formed after the evaporation of surface waters, and these values roughly agree with recent MSL measurements.
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Affiliation(s)
- Danica Adams
- Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA
| | - Yangcheng Luo
- Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA
| | - Michael L Wong
- Department of Astronomy and Astrobiology Program, University of Washington, Seattle, Washington, USA
- Virtual Planet Laboratory, University of Washington, Seattle, Washington, USA
| | - Patrick Dunn
- Space Sciences Laboratory, University of California, Berkeley, Berkeley, California, USA
| | - Madeline Christensen
- Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA
- Bellarmine Preparatory, Tacoma, Washington, USA
| | - Chuanfei Dong
- Department of Astrophysical Sciences, Princeton University, Princeton, California, USA
| | - Renyu Hu
- Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - Yuk Yung
- Department of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
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Dundas CM, Becerra P, Byrne S, Chojnacki M, Daubar IJ, Diniega S, Hansen CJ, Herkenhoff KE, Landis ME, McEwen AS, Portyankina G, Valantinas A. Active Mars: A Dynamic World. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2021; 126:e2021JE006876. [PMID: 35845553 PMCID: PMC9285055 DOI: 10.1029/2021je006876] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 02/24/2021] [Revised: 06/17/2021] [Accepted: 06/21/2021] [Indexed: 06/15/2023]
Abstract
Mars exhibits diverse surface changes at all latitudes and all seasons. Active processes include impact cratering, aeolian sand and dust transport, a variety of slope processes, changes in polar ices, and diverse effects of seasonal CO2 frost. The extent of surface change has been surprising and indicates that the present climate is capable of reshaping the surface. Activity has important implications for the Amazonian history of Mars: understanding processes is a necessary step before we can understand their implications and variations over time.
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Affiliation(s)
- Colin M. Dundas
- U.S. Geological SurveyAstrogeology Science CenterFlagstaffAZUSA
| | | | - Shane Byrne
- Lunar and Planetary LaboratoryUniversity of ArizonaTucsonAZUSA
| | | | - Ingrid J. Daubar
- Department of Earth, Environmental, and Planetary SciencesBrown UniversityProvidenceRIUSA
| | - Serina Diniega
- Jet Propulsion Laboratory/California Institute of TechnologyPasadenaCAUSA
| | | | | | - Margaret E. Landis
- Laboratory for Atmospheric and Space PhysicsUniversity of ColoradoBoulderCOUSA
| | | | - Ganna Portyankina
- Laboratory for Atmospheric and Space PhysicsUniversity of ColoradoBoulderCOUSA
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Bristow TF, Grotzinger JP, Rampe EB, Cuadros J, Chipera SJ, Downs GW, Fedo CM, Frydenvang J, McAdam AC, Morris RV, Achilles CN, Blake DF, Castle N, Craig P, Des Marais DJ, Downs RT, Hazen RM, Ming DW, Morrison SM, Thorpe MT, Treiman AH, Tu V, Vaniman DT, Yen AS, Gellert R, Mahaffy PR, Wiens RC, Bryk AB, Bennett KA, Fox VK, Millken RE, Fraeman AA, Vasavada AR. Brine-driven destruction of clay minerals in Gale crater, Mars. Science 2021; 373:198-204. [PMID: 34244410 DOI: 10.1126/science.abg5449] [Citation(s) in RCA: 20] [Impact Index Per Article: 6.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/24/2021] [Accepted: 05/28/2021] [Indexed: 11/02/2022]
Abstract
Mars' sedimentary rock record preserves information on geological (and potential astrobiological) processes that occurred on the planet billions of years ago. The Curiosity rover is exploring the lower reaches of Mount Sharp, in Gale crater on Mars. A traverse from Vera Rubin ridge to Glen Torridon has allowed Curiosity to examine a lateral transect of rock strata laid down in a martian lake ~3.5 billion years ago. We report spatial differences in the mineralogy of time-equivalent sedimentary rocks <400 meters apart. These differences indicate localized infiltration of silica-poor brines, generated during deposition of overlying magnesium sulfate-bearing strata. We propose that destabilization of silicate minerals driven by silica-poor brines (rarely observed on Earth) was widespread on ancient Mars, because sulfate deposits are globally distributed.
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Affiliation(s)
- T F Bristow
- Eobiology Branch, NASA Ames Research Center, Moffett Field, CA 94035, USA.
| | - J P Grotzinger
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
| | - E B Rampe
- Astromaterials Research and Exploration Science Division, NASA Johnson Space Center, Houston, TX 77058, USA
| | - J Cuadros
- Department of Earth Sciences, Natural History Museum, London SW7 5BD, UK
| | - S J Chipera
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - G W Downs
- Department of Geosciences, University of Arizona, Tucson, AZ 85721, USA
| | - C M Fedo
- Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996, USA
| | - J Frydenvang
- Globe Institute, University of Copenhagen, Copenhagen, Denmark
| | - A C McAdam
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - R V Morris
- Astromaterials Research and Exploration Science Division, NASA Johnson Space Center, Houston, TX 77058, USA
| | - C N Achilles
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - D F Blake
- Eobiology Branch, NASA Ames Research Center, Moffett Field, CA 94035, USA
| | - N Castle
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - P Craig
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - D J Des Marais
- Eobiology Branch, NASA Ames Research Center, Moffett Field, CA 94035, USA
| | - R T Downs
- Department of Geosciences, University of Arizona, Tucson, AZ 85721, USA
| | - R M Hazen
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - D W Ming
- Astromaterials Research and Exploration Science Division, NASA Johnson Space Center, Houston, TX 77058, USA
| | - S M Morrison
- Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA
| | - M T Thorpe
- Jacobs Technology-Jacobs JETS Contract, Astromaterials Research and Exploration Science Division, at NASA Johnson Space Center, Houston, TX 77058, USA
| | - A H Treiman
- Lunar and Planetary Institute, Universities Space Research Association, Houston, TX 77058, USA
| | - V Tu
- Jacobs Technology-Jacobs JETS Contract, Astromaterials Research and Exploration Science Division, at NASA Johnson Space Center, Houston, TX 77058, USA
| | - D T Vaniman
- Planetary Science Institute, Tucson, AZ 85719, USA
| | - A S Yen
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - R Gellert
- Department of Physics, University of Guelph, Guelph, Ontario N1G 2W1, Canada
| | - P R Mahaffy
- Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - R C Wiens
- Los Alamos National Laboratory, Los Alamos, NM 87545, USA
| | - A B Bryk
- Department of Earth and Planetary Science, University of California Berkeley, Berkeley, CA 94720, USA
| | - K A Bennett
- U.S. Geological Survey, Astrogeology Science Center, Flagstaff, AZ 86001, USA
| | - V K Fox
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
| | - R E Millken
- Department of Earth, Environmental Sciences and Planetary Sciences, Brown University, Providence, RI 02912, USA
| | - A A Fraeman
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - A R Vasavada
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
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Scheller EL, Swindle C, Grotzinger J, Barnhart H, Bhattacharjee S, Ehlmann BL, Farley K, Fischer WW, Greenberger R, Ingalls M, Martin PE, Osorio-Rodriguez D, Smith BP. Formation of Magnesium Carbonates on Earth and Implications for Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2021; 126:e2021JE006828. [PMID: 34422534 PMCID: PMC8378241 DOI: 10.1029/2021je006828] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/25/2021] [Accepted: 05/29/2021] [Indexed: 05/20/2023]
Abstract
Magnesium carbonates have been identified within the landing site of the Perseverance rover mission. This study reviews terrestrial analog environments and textural, mineral assemblage, isotopic, and elemental analyses that have been applied to establish formation conditions of magnesium carbonates. Magnesium carbonates form in five distinct settings: ultramafic rock-hosted veins, the matrix of carbonated peridotite, nodules in soil, alkaline lake, and playa deposits, and as diagenetic replacements within lime-and dolostones. Dominant textures include fine-grained or microcrystalline veins, nodules, and crusts. Microbial influences on formation are recorded in thrombolites, stromatolites, crinkly, and pustular laminites, spheroids, and filamentous microstructures. Mineral assemblages, fluid inclusions, and carbon, oxygen, magnesium, and clumped isotopes of carbon and oxygen have been used to determine the sources of carbon, magnesium, and fluid for magnesium carbonates as well as their temperatures of formation. Isotopic signatures in ultramafic rock-hosted magnesium carbonates reveal that they form by either low-temperature meteoric water infiltration and alteration, hydrothermal alteration, or metamorphic processes. Isotopic compositions of lacustrine magnesium carbonate record precipitation from lake water, evaporation processes, and ambient formation temperatures. Assessment of these features with similar analytical techniques applied to returned Martian samples can establish whether carbonates on ancient Mars were formed at high or low temperature conditions in the surface or subsurface through abiotic or biotic processes. The timing of carbonate formation processes could be constrained by 147Sm-143Nd isochron, U-Pb concordia, 207Pb-206Pb isochron radiometric dating as well as 3He, 21Ne, 22Ne, or 36Ar surface exposure dating of returned Martian magnesium carbonate samples.
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Affiliation(s)
- Eva L Scheller
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - Carl Swindle
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - John Grotzinger
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - Holly Barnhart
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - Surjyendu Bhattacharjee
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - Bethany L Ehlmann
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
| | - Ken Farley
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - Woodward W Fischer
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - Rebecca Greenberger
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - Miquela Ingalls
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
- Department of Geosciences, Pennsylvania State University, State College, PA, USA
| | - Peter E Martin
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
- Geological Sciences Department, University of Colorado Boulder, Boulder, CO, USA
| | - Daniela Osorio-Rodriguez
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
| | - Ben P Smith
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA
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Clark BC, Kolb VM, Steele A, House CH, Lanza NL, Gasda PJ, VanBommel SJ, Newsom HE, Martínez-Frías J. Origin of Life on Mars: Suitability and Opportunities. Life (Basel) 2021; 11:539. [PMID: 34207658 PMCID: PMC8227854 DOI: 10.3390/life11060539] [Citation(s) in RCA: 9] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/22/2021] [Revised: 05/28/2021] [Accepted: 06/01/2021] [Indexed: 02/07/2023] Open
Abstract
Although the habitability of early Mars is now well established, its suitability for conditions favorable to an independent origin of life (OoL) has been less certain. With continued exploration, evidence has mounted for a widespread diversity of physical and chemical conditions on Mars that mimic those variously hypothesized as settings in which life first arose on Earth. Mars has also provided water, energy sources, CHNOPS elements, critical catalytic transition metal elements, as well as B, Mg, Ca, Na and K, all of which are elements associated with life as we know it. With its highly favorable sulfur abundance and land/ocean ratio, early wet Mars remains a prime candidate for its own OoL, in many respects superior to Earth. The relatively well-preserved ancient surface of planet Mars helps inform the range of possible analogous conditions during the now-obliterated history of early Earth. Continued exploration of Mars also contributes to the understanding of the opportunities for settings enabling an OoL on exoplanets. Favoring geochemical sediment samples for eventual return to Earth will enhance assessments of the likelihood of a Martian OoL.
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Affiliation(s)
| | - Vera M. Kolb
- Department of Chemistry, University of Wisconsin—Parkside, Kenosha, WI 53141, USA;
| | - Andrew Steele
- Earth and Planetary Laboratory, Carnegie Institution for Science, Washington, DC 20015, USA;
| | - Christopher H. House
- Department of Biochemistry and Molecular Biology, Pennsylvania State University, State College, PA 16807, USA;
| | - Nina L. Lanza
- Los Alamos National Laboratory, Los Alamos, NM 87545, USA; (N.L.L.); (P.J.G.)
| | - Patrick J. Gasda
- Los Alamos National Laboratory, Los Alamos, NM 87545, USA; (N.L.L.); (P.J.G.)
| | - Scott J. VanBommel
- Department of Earth and Planetary Sciences, Washington University in St. Louis, St. Louis, MO 63130, USA;
| | - Horton E. Newsom
- Institute of Meteoritics, Department of Earth and Planetary Sciences, University of New Mexico, Albuquerque, NM 88033, USA;
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Viennet JC, Bernard S, Le Guillou C, Sautter V, Grégoire B, Jambon A, Pont S, Beyssac O, Zanda B, Hewins R, Remusat L. Martian Magmatic Clay Minerals Forming Vesicles: Perfect Niches for Emerging Life? ASTROBIOLOGY 2021; 21:605-612. [PMID: 33684326 DOI: 10.1089/ast.2020.2345] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
Mars was habitable in its early history, but the consensus is that it is quite inhospitable today, in particular because its modern climate cannot support stable liquid water at the surface. Here, we report the presence of magmatic Fe/Mg clay minerals within the mesostasis of the martian meteorite NWA 5790, an unaltered 1.3 Ga nakhlite archetypal of the martian crust. These magmatic clay minerals exhibit a vesicular texture that forms a network of microcavities or pockets, which could serve as microreactors and allow molecular crowding, a necessary step for the emergence of life. Because their formation does not depend on climate, such niches for emerging life may have been generated on Mars at many periods throughout its history, regardless of the stability or availability of liquid water at the surface.
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Affiliation(s)
- Jean-Christophe Viennet
- Muséum National d'Histoire Naturelle, Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS UMR 7590, Sorbonne Université, CNRS, Paris, France
| | - Sylvain Bernard
- Muséum National d'Histoire Naturelle, Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS UMR 7590, Sorbonne Université, CNRS, Paris, France
| | - Corentin Le Guillou
- Université Lille, CNRS, INRA, ENSCL, UMR 8207 - UMET - Unité Matériaux et Transformations, Lille, France
| | - Violaine Sautter
- Muséum National d'Histoire Naturelle, Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS UMR 7590, Sorbonne Université, CNRS, Paris, France
| | - Brian Grégoire
- Centre National de la Recherche Scientifique (CNRS), Université de Poitiers, UMR 7285 IC2MP-Hydrasa, Poitiers, France
| | - Albert Jambon
- Muséum National d'Histoire Naturelle, Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS UMR 7590, Sorbonne Université, CNRS, Paris, France
| | - Sylvain Pont
- Muséum National d'Histoire Naturelle, Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS UMR 7590, Sorbonne Université, CNRS, Paris, France
| | - Olivier Beyssac
- Muséum National d'Histoire Naturelle, Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS UMR 7590, Sorbonne Université, CNRS, Paris, France
| | - Brigitte Zanda
- Muséum National d'Histoire Naturelle, Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS UMR 7590, Sorbonne Université, CNRS, Paris, France
| | - Roger Hewins
- Muséum National d'Histoire Naturelle, Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS UMR 7590, Sorbonne Université, CNRS, Paris, France
| | - Laurent Remusat
- Muséum National d'Histoire Naturelle, Institut de Minéralogie, Physique des Matériaux et Cosmochimie, CNRS UMR 7590, Sorbonne Université, CNRS, Paris, France
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Mojarro A, Jin L, Szostak JW, Head JW, Zuber MT. In search of the RNA world on Mars. GEOBIOLOGY 2021; 19:307-321. [PMID: 33565260 PMCID: PMC8248371 DOI: 10.1111/gbi.12433] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/02/2020] [Revised: 01/22/2021] [Accepted: 01/23/2021] [Indexed: 05/17/2023]
Abstract
Advances in origins of life research and prebiotic chemistry suggest that life as we know it may have emerged from an earlier RNA World. However, it has been difficult to reconcile the conditions used in laboratory experiments with real-world geochemical environments that may have existed on the early Earth and hosted the origin(s) of life. This challenge is due to geologic resurfacing and recycling that have erased the overwhelming majority of the Earth's prebiotic history. We therefore propose that Mars, a planet frozen in time, comprised of many surfaces that have remained relatively unchanged since their formation > 4 Gya, is the best alternative to search for environments consistent with geochemical requirements imposed by the RNA world. In this study, we synthesize in situ and orbital observations of Mars and modeling of its early atmosphere into solutions containing a range of pHs and concentrations of prebiotically relevant metals (Fe2+ , Mg2+ , and Mn2+ ) spanning various candidate aqueous environments. We then experimentally determine RNA degradation kinetics due to metal-catalyzed hydrolysis (cleavage) and evaluate whether early Mars could have been permissive toward the accumulation of long-lived RNA polymers. Our results indicate that a Mg2+ -rich basalt sourcing metals to a slightly acidic (pH 5.4) environment mediates the slowest rates of RNA cleavage, though geologic evidence and basalt weathering models suggest aquifers on Mars would be near neutral (pH ~ 7). Moreover, the early onset of oxidizing conditions on Mars has major consequences regarding the availability of oxygen-sensitive metals (i.e., Fe2+ and Mn2+ ) due to increased RNA degradation rates and precipitation. Overall, (a) low pH decreases RNA cleavage at high metal concentrations; (b) acidic to neutral pH environments with Fe2+ or Mn2+ cleave more RNA than Mg2+ ; and (c) alkaline environments with Mg2+ dramatically cleaves more RNA while precipitates were observed for Fe2+ and Mn2+ .
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Affiliation(s)
- Angel Mojarro
- Department of Earth, Atmospheric and Planetary SciencesMassachusetts Institute of TechnologyCambridgeMAUSA
| | - Lin Jin
- Department of Molecular Biology, and Center for Computational and Integrative BiologyMassachusetts General HospitalBostonMAUSA
| | - Jack W. Szostak
- Department of Molecular Biology, and Center for Computational and Integrative BiologyMassachusetts General HospitalBostonMAUSA
| | - James W. Head
- Department of Earth, Environmental and Planetary SciencesBrown UniversityProvidenceRIUSA
| | - Maria T. Zuber
- Department of Earth, Atmospheric and Planetary SciencesMassachusetts Institute of TechnologyCambridgeMAUSA
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43
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Cockell CS, Wordsworth R, Whiteford N, Higgins PM. Minimum Units of Habitability and Their Abundance in the Universe. ASTROBIOLOGY 2021; 21:481-489. [PMID: 33513037 DOI: 10.1089/ast.2020.2350] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
Although the search for habitability is a much-vaunted objective in the study of planetary environments, the material requirements for an environment to be habitable can be met with relatively few ingredients. In this hypothesis paper, the minimum material requirements for habitability are first re-evaluated, necessarily based on life "as we know it." From this vantage point, we explore examples of the minimum number of material requirements for habitable conditions to arise in a planetary environment, which we illustrate with "minimum habitability diagrams." These requirements raise the hypothesis that habitable conditions may be common throughout the universe. If the hypothesis was accepted, then the discovery of life would remain an important discovery, but habitable conditions on their own would be an unremarkable feature of the material universe. We discuss how minimum units of habitability provide a parsimonious way to consider the minimum number of geological inferences about a planetary body, and the minimum number of atmospheric components that must be measured, for example in the case of exoplanets, to be able to make assessments of habitability.
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Affiliation(s)
- Charles S Cockell
- UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh, Edinburgh, UK
| | - Robin Wordsworth
- Department of Earth and Planetary Sciences, Harvard University, Cambridge, Massachusetts, USA
| | - Niall Whiteford
- Institute for Astronomy, Royal Observatory, Blackford Hill, Edinburgh, UK
| | - Peter M Higgins
- UK Centre for Astrobiology, School of Physics and Astronomy, University of Edinburgh, Edinburgh, UK
- Institute for Astronomy, Royal Observatory, Blackford Hill, Edinburgh, UK
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44
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Rizzo V, Armstrong R, Hua H, Cantasano N, Nicolò T, Bianciardi G. Life on Mars: Clues, Evidence or Proof? SOLAR PLANETS AND EXOPLANETS [WORKING TITLE] 2021. [DOI: 10.5772/intechopen.95531] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/23/2023]
Abstract
The search for life on Mars is one of the main objectives of space missions. At “Pahrump Hills Field Site” (Gale Crater, Mojave target), inside the mudstones of the Murray lacustrine sequence, Curiosity rover found organic materials and lozenge shaped laths considered by NASA as pseudomorphic crystals. Besides it detected mineral assemblages suggesting both oxidizing (hematite) and reducing (magnetite) environments, as well as acidic (diagenetic and/or authigenic jarosite) and neutral (apatite) conditions, that might suggest bacterially mediated reactions. Our morphological and morphometrical investigations show that such diagenetic microstructures are unlikely to be lozenge shapes and, in addition to several converging features, they suggest the presence of remnants of complex algal-like biota, similar to terrestrial procaryotes and/or eukaryotes; possible microorganisms that, on the base of absolute dating criteria used by other scholars, lived on Mars about 2.12 +/−0.36 Ga ago.
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45
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Tan JS, Royle SH, Sephton MA. Artificial Maturation of Iron- and Sulfur-Rich Mars Analogues: Implications for the Diagenetic Stability of Biopolymers and Their Detection with Pyrolysis-Gas Chromatography-Mass Spectrometry. ASTROBIOLOGY 2021; 21:199-218. [PMID: 33226839 PMCID: PMC7876361 DOI: 10.1089/ast.2019.2211] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/17/2019] [Accepted: 09/29/2020] [Indexed: 05/04/2023]
Abstract
Acidic iron- and sulfur-rich streams are appropriate analogues for the late Noachian and early Hesperian periods of martian history, when Mars exhibited extensive habitable environments. Any past life on Mars may have left behind diagnostic evidence of life that could be detected at the present day. For effective preservation, these remains must have avoided the harsh radiation flux at the martian surface, survived geological storage for billions of years, and remained detectable within their geochemical environment by analytical instrument suites used on Mars today, such as thermal extraction techniques. We investigated the detectability of organic matter within sulfur stream sediments that had been subjected to artificial maturation by hydrous pyrolysis. After maturation, the samples were analyzed by pyrolysis-gas chromatography-mass spectrometry (py-GC-MS) to determine whether organic matter could be detected with this commonly used technique. We find that macromolecular organic matter can survive the artificial maturation process in the presence of iron- and sulfur-rich minerals but cannot be unambiguously distinguished from abiotic organic matter. However, if jarosite and goethite are present in the sulfur stream environment, they interfere with the py-GC-MS detection of organic compounds in these samples. Clay reduces the obfuscating effect of the oxidizing minerals by providing nondeleterious adsorption sites. We also find that after a simple alkali and acid leaching process that removes oxidizing minerals such as iron sulfates, oxides, and oxyhydroxides, the sulfur stream samples exhibit much greater organic responses during py-GC-MS in terms of both abundance and diversity of organic compounds, such as the detection of hopanes in all leached samples. Our results suggest that insoluble organic matter can be preserved over billions of years of geological storage while still retaining diagnostic organic information, but sample selection strategies must either avoid jarosite- and goethite-rich outcrops or conduct preparative chemistry steps to remove these oxidants prior to analysis by thermal extraction techniques.
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Affiliation(s)
- Jonathan S.W. Tan
- Impacts and Astromaterials Research Centre, Department of Earth Science and Engineering, Imperial College London, London, UK
| | - Samuel H. Royle
- Impacts and Astromaterials Research Centre, Department of Earth Science and Engineering, Imperial College London, London, UK
| | - Mark A. Sephton
- Impacts and Astromaterials Research Centre, Department of Earth Science and Engineering, Imperial College London, London, UK
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46
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Ertem G. The Role of Minerals in Events That Led to the Origin of Life. ASTROBIOLOGY 2021; 21:137-150. [PMID: 33544652 DOI: 10.1089/ast.2020.2245] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
The role of minerals in the events that led to the origin of life is discussed with regard to (1) their catalytic role for the formation of RNA-like oligomers from their monomers and (2) their protective role for organic molecules formed in space that were delivered to planetary surfaces. Results obtained in the laboratory demonstrate that minerals do catalyze the oligomerization of ribonucleic acid (RNA) monomers to produce short RNA chains. Furthermore, and more importantly, these synthetic RNA chains formed by mineral catalysis serve as a template for the formation of complementary RNA chains, which is a significant finding that demonstrates the role of minerals in the origin of life. Simulation experiments run under Mars-like conditions have also shown that Mars analog minerals can shield the precursors of RNA and proteins against the harmful effects of UV and gamma radiation at the martian surface and 5 cm below the surface.
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Affiliation(s)
- Gözen Ertem
- Carl Sagan Center, SETI Institute, Mountain View, California, USA
- University of Maryland, College Park, Maryland, USA
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47
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Azua-Bustos A, Fairén AG, Silva CG, Carrizo D, Fernández-Martínez MÁ, Arenas-Fajardo C, Fernández-Sampedro M, Gil-Lozano C, Sánchez-García L, Ascaso C, Wierzchos J, Rampe EB. Inhabited subsurface wet smectites in the hyperarid core of the Atacama Desert as an analog for the search for life on Mars. Sci Rep 2020; 10:19183. [PMID: 33154541 PMCID: PMC7645800 DOI: 10.1038/s41598-020-76302-z] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Grants] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/23/2020] [Accepted: 10/16/2020] [Indexed: 01/21/2023] Open
Abstract
The modern Martian surface is unlikely to be habitable due to its extreme aridity among other environmental factors. This is the reason why the hyperarid core of the Atacama Desert has been studied as an analog for the habitability of Mars for more than 50 years. Here we report a layer enriched in smectites located just 30 cm below the surface of the hyperarid core of the Atacama. We discovered the clay-rich layer to be wet (a phenomenon never observed before in this region), keeping a high and constant relative humidity of 78% (aw 0.780), and completely isolated from the changing and extremely dry subaerial conditions characteristic of the Atacama. The smectite-rich layer is inhabited by at least 30 halophilic species of metabolically active bacteria and archaea, unveiling a previously unreported habitat for microbial life under the surface of the driest place on Earth. The discovery of a diverse microbial community in smectite-rich subsurface layers in the hyperarid core of the Atacama, and the collection of biosignatures we have identified within the clays, suggest that similar shallow clay deposits on Mars may contain biosignatures easily reachable by current rovers and landers.
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Affiliation(s)
- Armando Azua-Bustos
- Centro de Astrobiología (CSIC-INTA), 28850, Madrid, Spain.
- Instituto de Ciencias Biomédicas, Facultad de Ciencias de la Salud, Universidad Autónoma de Chile, Santiago, Chile.
| | - Alberto G Fairén
- Centro de Astrobiología (CSIC-INTA), 28850, Madrid, Spain.
- Department of Astronomy, Cornell University, Ithaca, NY, 14853, USA.
| | | | - Daniel Carrizo
- Centro de Astrobiología (CSIC-INTA), 28850, Madrid, Spain
| | | | | | | | - Carolina Gil-Lozano
- Centro de Astrobiología (CSIC-INTA), 28850, Madrid, Spain
- Laboratory of Planetology and Geodynamics, Université de Nantes, 44322, Nantes, France
| | | | - Carmen Ascaso
- Museo Nacional de Ciencias Naturales (CSIC), 28006, Madrid, Spain
| | - Jacek Wierzchos
- Museo Nacional de Ciencias Naturales (CSIC), 28006, Madrid, Spain
| | - Elizabeth B Rampe
- Astromaterials Research and Exploration Science Division, NASA Johnson Space Center, Houston, TX, USA
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48
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Capacity of Chlorate to Oxidize Ferrous Iron: Implications for Iron Oxide Formation on Mars. MINERALS 2020. [DOI: 10.3390/min10090729] [Citation(s) in RCA: 11] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 02/05/2023]
Abstract
Chlorate is an important Cl-bearing species and a strong potential Fe(II) oxidant on Mars. Since the amount of oxychlorine species (perchlorate and chlorate) detected on Mars is limited (<~1 wt.%), the effectiveness of chlorate to produce iron oxides depends heavily on its oxidizing capacity. Decomposition of chlorate or intermediates produced during its reduction, before reaction with Fe(II) would decrease its effective capacity as an oxidant. We thus evaluated the capacity of chlorate to produce Fe(III) minerals in Mars-relevant fluids, via oxidation of dissolved Fe(II). Each chlorate ion can oxidize 6 Fe(II) ions under all conditions investigated. Mass balance demonstrated that 1 wt.% chlorate (as ClO3−) could produce approximately 6 to 12 wt.% Fe(III) or mixed valent mineral products, with the amount varying with the formula of the precipitating phase. The mineral products are primarily determined by the fluid type (chloride- or sulfate-rich), the solution pH, and the rate of Fe(II) oxidation. The pH at the time of initial mineral nucleation and the amount of residual dissolved Fe(II) in the system exert important additional controls on the final mineralogy. Subsequent diagenetic transformation of these phases would yield 5.7 wt.% hematite per wt.% of chlorate reacted, providing a quantitative constraint on the capacity of chlorate to generate iron oxides on Mars.
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49
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Schenk P, Scully J, Buczkowski D, Sizemore H, Schmidt B, Pieters C, Neesemann A, O'Brien D, Marchi S, Williams D, Nathues A, De Sanctis M, Tosi F, Russell CT, Castillo-Rogez J, Raymond C. Impact heat driven volatile redistribution at Occator crater on Ceres as a comparative planetary process. Nat Commun 2020; 11:3679. [PMID: 32778649 PMCID: PMC7417549 DOI: 10.1038/s41467-020-17184-7] [Citation(s) in RCA: 16] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/21/2019] [Accepted: 06/16/2020] [Indexed: 12/02/2022] Open
Abstract
Hydrothermal processes in impact environments on water-rich bodies such as Mars and Earth are relevant to the origins of life. Dawn mapping of dwarf planet (1) Ceres has identified similar deposits within Occator crater. Here we show using Dawn high-resolution stereo imaging and topography that Ceres' unique composition has resulted in widespread mantling by solidified water- and salt-rich mud-like impact melts with scattered endogenic pits, troughs, and bright mounds indicative of outgassing of volatiles and periglacial-style activity during solidification. These features are distinct from and less extensive than on Mars, indicating that Occator melts may be less gas-rich or volatiles partially inhibited from reaching the surface. Bright salts at Vinalia Faculae form thin surficial precipitates sourced from hydrothermal brine effusion at many individual sites, coalescing in several larger centers, but their ages are statistically indistinguishable from floor materials, allowing for but not requiring migration of brines from deep crustal source(s).
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Affiliation(s)
- P Schenk
- Lunar and Planetary Institute/USRA, Houston, TX, USA.
| | - J Scully
- Jet Propulsion Laboratory/Caltech, Pasadena, CA, USA
| | - D Buczkowski
- Johns Hopkins University-Applied Physics Laboratory, Laurel, MD, USA
| | - H Sizemore
- Planetary Science Institute, Tucson, AZ, USA
| | - B Schmidt
- Georgia Institute of Technology, Atlanta, GA, USA
| | - C Pieters
- Brown University Providence, Providence, RI, USA
| | | | - D O'Brien
- Planetary Science Institute, Tucson, AZ, USA
| | - S Marchi
- Southwest Research Institute, Boulder, CO, USA
| | - D Williams
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
| | - A Nathues
- Max Planck Institute for Solar System Research, Goettingen, Germany
| | - M De Sanctis
- Istituto di Astrofisica e Planetologia Spaziali, INAF, Rome, Italy
| | - F Tosi
- Istituto di Astrofisica e Planetologia Spaziali, INAF, Rome, Italy
| | - C T Russell
- University of California, Los Angeles, CA, USA
| | | | - C Raymond
- Jet Propulsion Laboratory/Caltech, Pasadena, CA, USA
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50
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Achilles CN, Rampe EB, Downs RT, Bristow TF, Ming DW, Morris RV, Vaniman DT, Blake DF, Yen AS, McAdam AC, Sutter B, Fedo CM, Gwizd S, Thompson LM, Gellert R, Morrison SM, Treiman AH, Crisp JA, Gabriel TSJ, Chipera SJ, Hazen RM, Craig PI, Thorpe MT, Des Marais DJ, Grotzinger JP, Tu VM, Castle N, Downs GW, Peretyazhko TS, Walroth RC, Sarrazin P, Morookian JM. Evidence for Multiple Diagenetic Episodes in Ancient Fluvial-Lacustrine Sedimentary Rocks in Gale Crater, Mars. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2020; 125:e2019JE006295. [PMID: 32999799 PMCID: PMC7507756 DOI: 10.1029/2019je006295] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/02/2019] [Revised: 06/17/2020] [Accepted: 06/22/2020] [Indexed: 05/13/2023]
Abstract
The Curiosity rover's exploration of rocks and soils in Gale crater has provided diverse geochemical and mineralogical data sets, underscoring the complex geological history of the region. We report the crystalline, clay mineral, and amorphous phase distributions of four Gale crater rocks from an 80-m stratigraphic interval. The mineralogy of the four samples is strongly influenced by aqueous alteration processes, including variations in water chemistries, redox, pH, and temperature. Localized hydrothermal events are evidenced by gray hematite and maturation of amorphous SiO2 to opal-CT. Low-temperature diagenetic events are associated with fluctuating lake levels, evaporative events, and groundwater infiltration. Among all mudstones analyzed in Gale crater, the diversity in diagenetic processes is primarily captured by the mineralogy and X-ray amorphous chemistry of the drilled rocks. Variations indicate a transition from magnetite to hematite and an increase in matrix-associated sulfates suggesting intensifying influence from oxic, diagenetic fluids upsection. Furthermore, diagenetic fluid pathways are shown to be strongly affected by unconformities and sedimentary transitions, as evidenced by the intensity of alteration inferred from the mineralogy of sediments sampled adjacent to stratigraphic contacts.
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Affiliation(s)
| | | | - R. T. Downs
- Department of GeosciencesUniversity of ArizonaTucsonAZUSA
| | | | | | | | | | | | - A. S. Yen
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | - B. Sutter
- Jacobs at NASA Johnson Space CenterHoustonTXUSA
| | - C. M. Fedo
- Department of Earth and Planetary SciencesUniversity of Tennessee, KnoxvilleKnoxvilleTNUSA
| | - S. Gwizd
- Department of Earth and Planetary SciencesUniversity of Tennessee, KnoxvilleKnoxvilleTNUSA
| | - L. M. Thompson
- Department of Earth SciencesUniversity of New BrunswickFrederictonNew BrunswickCanada
| | - R. Gellert
- Department of PhysicsUniversity of GuelphGuelphOntarioCanada
| | | | | | - J. A. Crisp
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - T. S. J. Gabriel
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | | | - R. M. Hazen
- Carnegie Institute for ScienceWashingtonDCUSA
| | | | | | | | - J. P. Grotzinger
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - V. M. Tu
- Jacobs at NASA Johnson Space CenterHoustonTXUSA
| | - N. Castle
- Planetary Science InstituteTucsonAZUSA
| | - G. W. Downs
- Department of GeosciencesUniversity of ArizonaTucsonAZUSA
| | | | | | | | - J. M. Morookian
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
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