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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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2
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Sephton MA, Freeman K, Hays L, Thiessen F, Benison K, Carrier B, Dworkin JP, Glamoclija M, Gough R, Onofri S, Peterson R, Quinn R, Russell S, Stüeken EE, Velbel M, Zolotov M. Thresholds of Temperature and Time for Mars Sample Return: Final Report of the Mars Sample Return Temperature-Time Tiger Team. ASTROBIOLOGY 2024; 24:443-488. [PMID: 38768433 DOI: 10.1089/ast.2023.0098] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/22/2024]
Affiliation(s)
- Mark A Sephton
- Imperial College London, Earth Science and Engineering, South Kensington Campus, London, UK
| | - Kate Freeman
- The Pennsylvania State University, Geosciences, University Park, Pennsylvania, USA
| | - Lindsay Hays
- NASA Headquarters, Mars Sample Return Program, Washington, DC, USA
| | - Fiona Thiessen
- European Space Research and Technology Centre, Noordwijk, South Holland, Netherlands
| | - Kathleen Benison
- West Virginia University, Department of Geology and Geography, Morgantown, West Virginia, USA
| | - Brandi Carrier
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California, USA
| | - Jason P Dworkin
- NASA Goddard Space Flight Center, Astrochemistry, Greenbelt, Maryland, USA
| | - Mihaela Glamoclija
- Rutgers University Newark College of Arts and Sciences, Earth and Environmental Sciences, Newark, New Jersey, USA
| | - Raina Gough
- University of Colorado, Department of Chemistry and Biochemistry, Boulder, Colorado, USA
| | - Silvano Onofri
- University of Tuscia, Department of Ecological and Biological Sciences, Largo dell'Università snc Viterbo, Italy
| | | | - Richard Quinn
- NASA Ames Research Center, Moffett Field, California, USA
| | - Sara Russell
- Natural History Museum, Department of Earth Sciences, London, UK
| | - Eva E Stüeken
- University of St Andrews, School of Earth and Environmental Sciences, St Andrews, Fife, UK
| | - Michael Velbel
- Michigan State University, Earth and Environmental Sciences, East Lansing, Michigan, USA
- Smithsonian Institution, Department of Mineral Sciences, National Museum of Natural History, Washington, DC, USA
| | - Mikhail Zolotov
- Arizona State University, School of Earth and Space Exploration, Tempe, Arizona, USA
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3
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Qin X, Ren X, Wang X, Liu J, Wu H, Zeng X, Sun Y, Chen Z, Zhang S, Zhang Y, Chen W, Liu B, Liu D, Guo L, Li K, Zeng X, Huang H, Zhang Q, Yu S, Li C, Guo Z. Modern water at low latitudes on Mars: Potential evidence from dune surfaces. SCIENCE ADVANCES 2023; 9:eadd8868. [PMID: 37115933 PMCID: PMC10146874 DOI: 10.1126/sciadv.add8868] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Indexed: 05/03/2023]
Abstract
Landforms on the Martian surface are critical to understanding the nature of surface processes in the recent past. However, modern hydroclimatic conditions on Mars remain enigmatic, as explanations for the formation of observed landforms are ambiguous. We report crusts, cracks, aggregates, and bright polygonal ridges on the surfaces of hydrated salt-rich dunes of southern Utopia Planitia (~25°N) from in situ exploration by the Zhurong rover. These surface features were inferred to form after 1.4 to 0.4 million years ago. Wind and CO2 frost processes can be ruled out as potential mechanisms. Instead, involvement of saline water from thawed frost/snow is the most likely cause. This discovery sheds light on more humid conditions of the modern Martian climate and provides critical clues to future exploration missions searching for signs of extant life, particularly at low latitudes with comparatively warmer, more amenable surface temperatures.
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Affiliation(s)
- Xiaoguang Qin
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
- Corresponding author. (X.Q.); (X.R.); (X.W.); (J.L.)
| | - Xin Ren
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- Corresponding author. (X.Q.); (X.R.); (X.W.); (J.L.)
| | - Xu Wang
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
- Corresponding author. (X.Q.); (X.R.); (X.W.); (J.L.)
| | - Jianjun Liu
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- Corresponding author. (X.Q.); (X.R.); (X.W.); (J.L.)
| | - Haibin Wu
- Key Laboratory of Cenozoic Geology and Environment, 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
| | - Xingguo Zeng
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Yong Sun
- Institute of Atmospheric Physics, Chinese Academy of Sciences, Beijing, China
| | - Zhaopeng Chen
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Shihao Zhang
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
| | - Yizhong Zhang
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Wangli Chen
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Bin Liu
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Dawei Liu
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Lin Guo
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Kangkang Li
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
| | - Xiangzhao Zeng
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Hai Huang
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Qing Zhang
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Songzheng Yu
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Chunlai Li
- Key Laboratory of Lunar and Deep Space Exploration, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Zhengtang Guo
- Key Laboratory of Cenozoic Geology and Environment, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
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Abstract
Off-Earth drilling may be assumed as the second phase of space exploration to discover the unrevealed subsurface on the planetary bodies. It accelerates future space objectives such as in-situ propellant production, mineral exploitation, and space tourism. Owing to the rampant progress in modern technology, the new drill tools mounted on the sophisticated robots are capable to drill the planetary regolith dispersed on the celestial objects; however, formidable obstacles such as microgravity, vacuum condition, and temperature fluctuation as well as the weight limitation, lack of real-time drilling analysis, and remote robot-operator communication impose pressing restrictions on the quick development of space drilling tools. In this study, research on the past and present aspects of off-Earth drilling has been implemented to illuminate the horizon of this technology in the near-term future. The context encompasses a detailed description of the limitations, applications and mechanisms of the different drilling techniques adopted for planetary bodies. A particular emphasis is put on the hydraulic power systems which have not been satisfactorily deployed in off-Earth drilling yet. The research strives to glance over the pivotal aspects of off-Earth drilling to contribute to the future drilling programs planned by the national and private space agencies.
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Noffke N. Microbially Induced Sedimentary Structures in Clastic Deposits: Implication for the Prospection for Fossil Life on Mars. ASTROBIOLOGY 2021; 21:866-892. [PMID: 34042490 PMCID: PMC8262410 DOI: 10.1089/ast.2021.0011] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Download PDF] [Figures] [Subscribe] [Scholar Register] [Received: 01/22/2021] [Accepted: 04/08/2021] [Indexed: 06/12/2023]
Abstract
Abundant and well-preserved fossil microbenthos occurs in siliciclastic deposits of all Earth ages, from the early Archean to today. Studies in modern settings show how microbenthos responds to sediment dynamics by baffling and trapping, binding, biostabilization, and growth. Results of this microbial-sediment interaction are microbially induced sedimentary structures (MISS). Successful prospection for rich MISS occurrences in the terrestrial lithological record requires unraveling genesis and taphonomy of MISS, both of which are defined only by a narrow range of specific conditions. These conditions have to coincide with high detectability which is a function of outcrop quality, bedding character, and rock type. Assertions on biogenicity of MISS morphologies must be based on the presence of microbially induced sedimentary textures (MIST), which are MISS-internal textures comprising replacement minerals arranged into microscopic biological morphologies, ancient carbonaceous matter, trace fossils, and geochemical signals. MISS serve as possible templates for the decryption of ancient life-processes on Mars. This article closes with a perspective on selected deposits and ancient environments in Meridiani Planum, Gale Crater, and Jezero Crater, Mars, regarding their potential for MISS occurrences. The earlier hypothesis of structures on Mars as potentially being MISS is revised.
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Affiliation(s)
- Nora Noffke
- Old Dominion University, Department of Ocean and Earth Sciences, Norfolk, Virginia, USA
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6
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Bell JF, Maki JN, Mehall GL, Ravine MA, Caplinger MA, Bailey ZJ, Brylow S, Schaffner JA, Kinch KM, Madsen MB, Winhold A, Hayes AG, Corlies P, Tate C, Barrington M, Cisneros E, Jensen E, Paris K, Crawford K, Rojas C, Mehall L, Joseph J, Proton JB, Cluff N, Deen RG, Betts B, Cloutis E, Coates AJ, Colaprete A, Edgett KS, Ehlmann BL, Fagents S, Grotzinger JP, Hardgrove C, Herkenhoff KE, Horgan B, Jaumann R, Johnson JR, Lemmon M, Paar G, Caballo-Perucha M, Gupta S, Traxler C, Preusker F, Rice MS, Robinson MS, Schmitz N, Sullivan R, Wolff MJ. The Mars 2020 Perseverance Rover Mast Camera Zoom (Mastcam-Z) Multispectral, Stereoscopic Imaging Investigation. SPACE SCIENCE REVIEWS 2021; 217:24. [PMID: 33612866 PMCID: PMC7883548 DOI: 10.1007/s11214-020-00755-x] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.7] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/22/2020] [Accepted: 09/25/2020] [Indexed: 05/16/2023]
Abstract
Mastcam-Z is a multispectral, stereoscopic imaging investigation on the Mars 2020 mission's Perseverance rover. Mastcam-Z consists of a pair of focusable, 4:1 zoomable cameras that provide broadband red/green/blue and narrowband 400-1000 nm color imaging with fields of view from 25.6° × 19.2° (26 mm focal length at 283 μrad/pixel) to 6.2° × 4.6° (110 mm focal length at 67.4 μrad/pixel). The cameras can resolve (≥ 5 pixels) ∼0.7 mm features at 2 m and ∼3.3 cm features at 100 m distance. Mastcam-Z shares significant heritage with the Mastcam instruments on the Mars Science Laboratory Curiosity rover. Each Mastcam-Z camera consists of zoom, focus, and filter wheel mechanisms and a 1648 × 1214 pixel charge-coupled device detector and electronics. The two Mastcam-Z cameras are mounted with a 24.4 cm stereo baseline and 2.3° total toe-in on a camera plate ∼2 m above the surface on the rover's Remote Sensing Mast, which provides azimuth and elevation actuation. A separate digital electronics assembly inside the rover provides power, data processing and storage, and the interface to the rover computer. Primary and secondary Mastcam-Z calibration targets mounted on the rover top deck enable tactical reflectance calibration. Mastcam-Z multispectral, stereo, and panoramic images will be used to provide detailed morphology, topography, and geologic context along the rover's traverse; constrain mineralogic, photometric, and physical properties of surface materials; monitor and characterize atmospheric and astronomical phenomena; and document the rover's sample extraction and caching locations. Mastcam-Z images will also provide key engineering information to support sample selection and other rover driving and tool/instrument operations decisions.
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Affiliation(s)
| | | | | | - M. A. Ravine
- Malin Space Science Systems, Inc., San Diego, CA USA
| | | | | | - S. Brylow
- Malin Space Science Systems, Inc., San Diego, CA USA
| | | | | | | | | | | | | | - C. Tate
- Cornell Univ., Ithaca, NY USA
| | | | | | - E. Jensen
- Malin Space Science Systems, Inc., San Diego, CA USA
| | - K. Paris
- Arizona State Univ., Tempe, AZ USA
| | | | - C. Rojas
- Arizona State Univ., Tempe, AZ USA
| | | | | | | | - N. Cluff
- Arizona State Univ., Tempe, AZ USA
| | | | - B. Betts
- The Planetary Society, Pasadena, CA USA
| | | | - A. J. Coates
- Mullard Space Science Laboratory, Univ. College, London, UK
| | - A. Colaprete
- NASA/Ames Research Center, Moffett Field, CA USA
| | - K. S. Edgett
- Malin Space Science Systems, Inc., San Diego, CA USA
| | - B. L. Ehlmann
- JPL/Caltech, Pasadena, CA USA
- Caltech, Pasadena, CA USA
| | | | | | | | | | | | - R. Jaumann
- Inst. of Geological Sciences, Free University Berlin, Berlin, Germany
| | | | - M. Lemmon
- Space Science Inst., Boulder, CO USA
| | - G. Paar
- Joanneum Research, Graz, Austria
| | | | | | | | - F. Preusker
- DLR/German Aerospace Center, Berlin, Germany
| | - M. S. Rice
- Western Washington Univ., Bellingham, WA USA
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7
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Chan MA, Bowen BB, Corsetti FA, Farrand WH, Law ES, Newsom HE, Perl SM, Spear JR, Thompson DR. Exploring, Mapping, and Data Management Integration of Habitable Environments in Astrobiology. Front Microbiol 2019; 10:147. [PMID: 30891006 PMCID: PMC6412026 DOI: 10.3389/fmicb.2019.00147] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/24/2018] [Accepted: 01/21/2019] [Indexed: 11/17/2022] Open
Abstract
New approaches to blending geoscience, planetary science, microbiology-geobiology/ecology, geoinformatics and cyberinfrastructure technology disciplines in a holistic effort can be transformative to astrobiology explorations. Over the last two decades, overwhelming orbital evidence has confirmed the abundance of authigenic (in situ, formed in place) minerals on Mars. On Earth, environments where authigenic minerals form provide a substrate for the preservation of microbial life. Similarly, extraterrestrial life is likely to be preserved where crustal minerals can record and preserve the biochemical mechanisms (i.e., biosignatures). The search for astrobiological evidence on Mars has focused on identifying past or present habitable environments - places that could support some semblance of life. Thus, authigenic minerals represent a promising habitable environment where extraterrestrial life could be recorded and potentially preserved over geologic time scales. Astrobiology research necessarily takes place over vastly different scales; from molecules to viruses and microbes to those of satellites and solar system exploration, but the differing scales of analyses are rarely connected quantitatively. The mismatch between the scales of these observations- from the macro- satellite mineralogical observations to the micro- microbial observations- limits the applicability of our astrobiological understanding as we search for records of life beyond Earth. Each-scale observation requires knowledge of the geologic context and the environmental parameters important for assessing habitability. Exploration efforts to search for extraterrestrial life should attempt to quantify both the geospatial context and the temporal/spatial relationships between microbial abundance and diversity within authigenic minerals at multiple scales, while assimilating resolutions from satellite observations to field measurements to microscopic analyses. Statistical measures, computer vision, and the geospatial synergy of Geographic Information Systems (GIS), can allow analyses of objective data-driven methods to locate, map, and predict where the "sweet spots" of habitable environments occur at multiple scales. This approach of science information architecture or an "Astrobiology Information System" can provide the necessary maps to guide researchers to discoveries via testing, visualizing, documenting, and collaborating on significant data relationships that will advance explorations for evidence of life in our solar system and beyond.
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Affiliation(s)
- Marjorie A. Chan
- Department of Geology and Geophysics, The University of Utah, Salt Lake City, UT, United States
| | - Brenda B. Bowen
- Department of Geology and Geophysics, The University of Utah, Salt Lake City, UT, United States
| | - Frank A. Corsetti
- Department of Earth Sciences, University of Southern California, Los Angeles, CA, United States
| | | | - Emily S. Law
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, United States
| | - Horton E. Newsom
- Department Earth and Planetary Sciences, University of New Mexico, Albuquerque, NM, United States
| | - Scott M. Perl
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, United States
| | - John R. Spear
- Department of Civil and Environmental Engineering, Colorado School of Mines, Golden, CO, United States
| | - David R. Thompson
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, United States
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Shkolyar S, Farmer JD. Biosignature Preservation Potential in Playa Evaporites: Impacts of Diagenesis and Implications for Mars Exploration. ASTROBIOLOGY 2018; 18:1460-1478. [PMID: 30124326 DOI: 10.1089/ast.2018.1849] [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: 06/08/2023]
Abstract
Assessing biosignature preservation potential (BPP) in ancient habitable environments on Mars is a top NASA priority. We address this goal through the study of Miocene-Pliocene evaporites of the Verde Formation (central Arizona). We assessed the effects of diagenesis on BPP, integrating outcrop-scale observations with six lab analyses: thin-section petrography, X-ray diffraction, Raman spectroscopy, total organic carbon (TOC), electron probe microanalysis (EPMA), and visible to near-infrared (VNIR) reflectance spectroscopy. We recognized five facies and their diagenetic pathways. Two facies included mudstones which contain clusters of displacive growth gypsum (DGG). Early DGG was altered during diagenesis by dissolution forming crystal cavities and later underwent recrystallization, cation substitution, and sulfate dehydration. Another facies was identified by lenticular beds dominated by halite and late diagenetic thenardite (Na2SO4). These pods are overlain by a sequence of interbedded gray and red mudstones which record cyclic oxidation and Fe-oxide cementation. During the Pleistocene, a lacustrine environment developed, accompanied by magnesite cementation of playa mudstones. TOC analyses were used as a proxy for inferring the BPP in each facies. The highest BPP was associated with both red and gray mudstone facies. This study provides a taphonomic framework for playa environments on Earth that record the impacts of diagenesis on BPP, with potential applications to Mars sample return (MSR) missions.
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Affiliation(s)
- Svetlana Shkolyar
- School of Earth and Space Exploration, Arizona State University , Tempe, Arizona
| | - Jack D Farmer
- School of Earth and Space Exploration, Arizona State University , Tempe, Arizona
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9
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Kereszturi A, Bradak B, Chatzitheodoridis E, Ujvari G. Indicators and Methods to Understand Past Environments from ExoMars Rover Drills. ORIGINS LIFE EVOL B 2016; 46:435-454. [PMID: 27029794 DOI: 10.1007/s11084-016-9492-3] [Citation(s) in RCA: 16] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/28/2015] [Accepted: 01/15/2016] [Indexed: 11/26/2022]
Abstract
Great advances are expected during the analysis of drilled material acquired from 2 m depth by ExoMars rover, supported by the comparison to local context, and the joint use of different instruments. Textural information might be less detailed relatively to what is usually obtained at outcrops during classical geological field work on the Earth, partly because of the lack of optical imaging of the borehole wall and also because the collected samples are crushed. However sub-mm scale layering and some other sedimentary features might be identified in the borehole wall observations, or in the collected sample prior to crushing, and also at nearby outcrops. The candidate landing sites provide different targets and focus for research: Oxia Planum requires analysis of phyllosilicates and OH content, at Mawrth Vallis the layering of various phyllosilicates and the role of shallow-subsurface leaching should be emphasized. At Aram Dorsum the particle size and fluvial sedimentary features will be interesting. Hydrated perchlorates and sulphates are ideal targets possibly at every landing sites because of OH retention, especially if they are mixed with smectites, thus could point to even ancient wet periods. Extensive use of information from the infrared wall scanning will be complemented for geological context by orbital and rover imaging of nearby outcrops. Information from the context is especially useful to infer the possible action of past H2O. Separation of the ice and liquid water effects will be supported by cation abundance and sedimentary context. Shape of grains also helps here, and composition of transported grains points to the weathering potential of the environment in general. The work on Mars during the drilling and sample analysis will provide brand new experience and knowledge for future missions.
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Affiliation(s)
- A Kereszturi
- Research Centre for Astronomy and Earth Sciences, Budapest, Hungary.
| | - B Bradak
- Research Centre for Astronomy and Earth Sciences, Budapest, Hungary
- Department of Planetology, Kobe University, Kobe, Japan
| | | | - G Ujvari
- Research Centre for Astronomy and Earth Sciences, Budapest, Hungary
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10
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Núñez JI, Farmer JD, Sellar RG, Swayze GA, Blaney DL. Science applications of a multispectral microscopic imager for the astrobiological exploration of Mars. ASTROBIOLOGY 2014; 14:132-69. [PMID: 24552233 PMCID: PMC3929460 DOI: 10.1089/ast.2013.1079] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/23/2013] [Accepted: 01/15/2014] [Indexed: 05/30/2023]
Abstract
Future astrobiological missions to Mars are likely to emphasize the use of rovers with in situ petrologic capabilities for selecting the best samples at a site for in situ analysis with onboard lab instruments or for caching for potential return to Earth. Such observations are central to an understanding of the potential for past habitable conditions at a site and for identifying samples most likely to harbor fossil biosignatures. The Multispectral Microscopic Imager (MMI) provides multispectral reflectance images of geological samples at the microscale, where each image pixel is composed of a visible/shortwave infrared spectrum ranging from 0.46 to 1.73 μm. This spectral range enables the discrimination of a wide variety of rock-forming minerals, especially Fe-bearing phases, and the detection of hydrated minerals. The MMI advances beyond the capabilities of current microimagers on Mars by extending the spectral range into the infrared and increasing the number of spectral bands. The design employs multispectral light-emitting diodes and an uncooled indium gallium arsenide focal plane array to achieve a very low mass and high reliability. To better understand and demonstrate the capabilities of the MMI for future surface missions to Mars, we analyzed samples from Mars-relevant analog environments with the MMI. Results indicate that the MMI images faithfully resolve the fine-scale microtextural features of samples and provide important information to help constrain mineral composition. The use of spectral endmember mapping reveals the distribution of Fe-bearing minerals (including silicates and oxides) with high fidelity, along with the presence of hydrated minerals. MMI-based petrogenetic interpretations compare favorably with laboratory-based analyses, revealing the value of the MMI for future in situ rover-mediated astrobiological exploration of Mars.
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Affiliation(s)
- Jorge I. Núñez
- School of Earth and Space Exploration, Arizona State University, Tempe, Arizona
| | - Jack D. Farmer
- School of Earth and Space Exploration, Arizona State University, Tempe, Arizona
| | - R. Glenn Sellar
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
| | | | - Diana L. Blaney
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California
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11
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Planning for Mars returned sample science: final report of the MSR End-to-End International Science Analysis Group (E2E-iSAG). ASTROBIOLOGY 2012; 12:175-230. [PMID: 22468886 DOI: 10.1089/ast.2011.0805] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/31/2023]
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12
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Summers DP, Basa RCB, Khare B, Rodoni D. Abiotic nitrogen fixation on terrestrial planets: reduction of NO to ammonia by FeS. ASTROBIOLOGY 2012; 12:107-114. [PMID: 22283408 DOI: 10.1089/ast.2011.0646] [Citation(s) in RCA: 10] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/31/2023]
Abstract
Understanding the abiotic fixation of nitrogen and how such fixation can be a supply of prebiotic nitrogen is critical for understanding both the planetary evolution of, and the potential origin of life on, terrestrial planets. As nitrogen is a biochemically essential element, sources of biochemically accessible nitrogen, especially reduced nitrogen, are critical to prebiotic chemistry and the origin of life. Loss of atmospheric nitrogen can result in loss of the ability to sustain liquid water on a planetary surface, which would impact planetary habitability and hydrological processes that shape the surface. It is known that NO can be photochemically converted through a chain of reactions to form nitrate and nitrite, which can be subsequently reduced to ammonia. Here, we show that NO can also be directly reduced, by FeS, to ammonia. In addition to removing nitrogen from the atmosphere, this reaction is particularly important as a source of reduced nitrogen on an early terrestrial planet. By converting NO directly to ammonia in a single step, ammonia is formed with a higher product yield (~50%) than would be possible through the formation of nitrate/nitrite and subsequent conversion to ammonia. In conjunction with the reduction of NO, there is also a catalytic disproportionation at the mineral surface that converts NO to NO₂ and N₂O. The NO₂ is then converted to ammonia, while the N₂O is released back in the gas phase, which provides an abiotic source of nitrous oxide.
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Affiliation(s)
- David P Summers
- Carl Sagan Center, SETI Institute, c/o NASA Ames Research Center, Moffett Field, CA 94035-1000, USA.
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Amils R, González-Toril E, Aguilera A, Rodríguez N, Fernández-Remolar D, Gómez F, García-Moyano A, Malki M, Oggerin M, Sánchez-Andrea I, Sanz J. From Río Tinto to Mars: the terrestrial and extraterrestrial ecology of acidophiles. ADVANCES IN APPLIED MICROBIOLOGY 2011; 77:41-70. [PMID: 22050821 DOI: 10.1016/b978-0-12-387044-5.00002-9] [Citation(s) in RCA: 14] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 10/27/2022]
Abstract
The recent geomicrobiological characterization of Río Tinto, Iberian Pyrite Belt (IPB), has proven the importance of the iron cycle, not only in generating the extreme conditions of the habitat (low pH, high concentration of toxic heavy metals) but also in maintaining the high level of microbial diversity, both prokaryotic and eukaryotic, detected in the water column and the sediments. The extreme conditions of the Tinto basin are not the product of industrial contamination but the consequence of the presence of an underground bioreactor that obtains its energy from the massive sulfide minerals of the IPB. To test this hypothesis, a drilling project was carried out to intersect ground waters that interact with the mineral ore in order to provide evidence of subsurface microbial activities and the potential resources to support these activities. The oxidants that drive the system appear to come from the rock matrix, contradicting conventional acid mine drainage models. These resources need only groundwater to launch microbial metabolism. There are several similarities between the vast deposits of sulfates and iron oxides on Mars and the main sulfide-containing iron bioleaching products found in the Tinto. Firstly, the short-lived methane detected both in Mars' atmosphere and in the sediments and subsurface of the IPB and secondly, the abundance of iron, common to both. The physicochemical properties of iron make it a source of energy, a shield against radiation and oxidative stress as well as a natural pH controller. These similarities have led to Río Tinto's status as a Mars terrestrial analogue.
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Shkrob IA, Chemerisov SD, Marin TW. Photocatalytic decomposition of carboxylated molecules on light-exposed martian regolith and its relation to methane production on Mars. ASTROBIOLOGY 2010; 10:425-436. [PMID: 20528197 DOI: 10.1089/ast.2009.0433] [Citation(s) in RCA: 13] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/29/2023]
Abstract
We propose that the paucity of organic compounds in martian soil can be accounted for by efficient photocatalytic decomposition of carboxylated molecules due to the occurrence of the photo-Kolbe reaction at the surface of particulate iron(III) oxides that are abundant in the martian regolith. This photoreaction is initiated by the absorption of UVA light, and it readily occurs even at low temperature. The decarboxylation is observed for miscellaneous organic carboxylates, including the nonvolatile products of kerogen oxidation (that are currently thought to accumulate in the soil) as well as alpha-amino acids and peptides. Our study indicates that there may be no "safe haven" for these organic compounds on Mars; oxidation by reactive radicals, such as hydroxyl, is concerted with photocatalytic reactions on the oxide particles. Acting together, these two mechanisms result in mineralization of the organic component. The photooxidation of acetate (the terminal product of radical oxidation of the aliphatic component of kerogen) on the iron(III) oxides results in the formation of methane; this reaction may account for seasonably variable production of methane on Mars. The concomitant reduction of Fe(III) in the regolith leads to the formation of highly soluble ferrous ions that contribute to weathering of the soil particles.
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Affiliation(s)
- Ilya A Shkrob
- Chemical Sciences and Engineering Division, Argonne National Laboratory, Argonne, Illinois 60439, USA.
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15
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The Mars Astrobiology Explorer-Cacher (MAX-C): a potential rover mission for 2018. Final report of the Mars Mid-Range Rover Science Analysis Group (MRR-SAG) October 14, 2009. ASTROBIOLOGY 2010; 10:127-163. [PMID: 20298148 DOI: 10.1089/ast.2010.0462] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/29/2023]
Abstract
This report documents the work of the Mid-Range Rover Science Analysis Group (MRR-SAG), which was assigned to formulate a concept for a potential rover mission that could be launched to Mars in 2018. Based on programmatic and engineering considerations as of April 2009, our deliberations assumed that the potential mission would use the Mars Science Laboratory (MSL) sky-crane landing system and include a single solar-powered rover. The mission would also have a targeting accuracy of approximately 7 km (semimajor axis landing ellipse), a mobility range of at least 10 km, and a lifetime on the martian surface of at least 1 Earth year. An additional key consideration, given recently declining budgets and cost growth issues with MSL, is that the proposed rover must have lower cost and cost risk than those of MSL--this is an essential consideration for the Mars Exploration Program Analysis Group (MEPAG). The MRR-SAG was asked to formulate a mission concept that would address two general objectives: (1) conduct high priority in situ science and (2) make concrete steps toward the potential return of samples to Earth. The proposed means of achieving these two goals while balancing the trade-offs between them are described here in detail. We propose the name Mars Astrobiology Explorer-Cacher(MAX-C) to reflect the dual purpose of this potential 2018 rover mission.
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Hausrath EM, Treiman AH, Vicenzi E, Bish DL, Blake D, Sarrazin P, Hoehler T, Midtkandal I, Steele A, Brantley SL. Short- and long-term olivine weathering in Svalbard: implications for Mars. ASTROBIOLOGY 2008; 8:1079-1092. [PMID: 19191538 DOI: 10.1089/ast.2007.0195] [Citation(s) in RCA: 8] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/27/2023]
Abstract
Liquid water is essential to life as we know it on Earth; therefore, the search for water on Mars is a critical component of the search for life. Olivine, a mineral identified as present on Mars, has been proposed as an indicator of the duration and characteristics of water because it dissolves quickly, particularly under low-pH conditions. The duration of olivine persistence relative to glass under conditions of aqueous alteration reflects the pH and temperature of the reacting fluids. In this paper, we investigate the utility of 3 methodologies to detect silicate weathering in a Mars analog environment (Sverrefjell volcano, Svalbard). CheMin, a miniature X-ray diffraction instrument developed for flight on NASA's upcoming Mars Science Laboratory, was deployed on Svalbard and was successful in detecting olivine and weathering products. The persistence of olivine and glass in Svalbard rocks was also investigated via laboratory observations of weathered hand samples as well as an in situ burial experiment. Observations of hand samples are consistent with the inference that olivine persists longer than glass at near-zero temperatures in the presence of solutions at pH approximately 7-9 on Svalbard, whereas in hydrothermally altered zones, glass has persisted longer than olivine in the presence of fluids at similar pH at approximately 50 degrees C. Analysis of the surfaces of olivine and glass samples, which were buried on Sverrefjell for 1 year and then retrieved, documented only minor incipient weathering, though these results suggest the importance of biological impacts. The 3 types of observations (CheMin, laboratory observations of hand samples, burial experiments) of weathering of olivine and glass at Svalbard show promise for interpretation of weathering on Mars. Furthermore, the weathering relationships observed on Svalbard are consistent with laboratory-measured dissolution rates, which suggests that relative mineral dissolution rates in the laboratory, in concert with field observations, can be used to yield valuable information regarding the pH and temperature of reacting martian fluids.
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Affiliation(s)
- E M Hausrath
- Department of Geosciences, Pennsylvania State University, University Park, PA, USA.
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Herkenhoff KE, Grotzinger J, Knoll AH, McLennan SM, Weitz C, Yingst A, Anderson R, Archinal BA, Arvidson RE, Barrett JM, Becker KJ, Bell JF, Budney C, Chapman MG, Cook D, Ehlmann B, Franklin B, Gaddis LR, Galuszka DM, Garcia PA, Geissler P, Hare TM, Howington-Kraus E, Johnson JR, Keszthelyi L, Kirk RL, Lanagan P, Lee EM, Leff C, Maki JN, Mullins KF, Parker TJ, Redding BL, Rosiek MR, Sims MH, Soderblom LA, Spanovich N, Springer R, Squyres SW, Stolper D, Sucharski RM, Sucharski T, Sullivan R, Torson JM. Surface processes recorded by rocks and soils on Meridiani Planum, Mars: Microscopic Imager observations during Opportunity's first three extended missions. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2008je003100] [Citation(s) in RCA: 26] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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18
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Zent AP, Ichimura AS, Quinn RC, Harding HK. The formation and stability of the superoxide radical (O2−) on rock-forming minerals: Band gaps, hydroxylation state, and implications for Mars oxidant chemistry. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003001] [Citation(s) in RCA: 21] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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19
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20
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Knoll AH, Jolliff BL, Farrand WH, Bell III JF, Clark BC, Gellert R, Golombek MP, Grotzinger JP, Herkenhoff KE, Johnson JR, McLennan SM, Morris R, Squyres SW, Sullivan R, Tosca NJ, Yen A, Learner Z. Veneers, rinds, and fracture fills: Relatively late alteration of sedimentary rocks at Meridiani Planum, Mars. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je002949] [Citation(s) in RCA: 49] [Impact Index Per Article: 3.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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21
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Moissl C, Bruckner JC, Venkateswaran K. Archaeal diversity analysis of spacecraft assembly clean rooms. ISME JOURNAL 2007; 2:115-9. [DOI: 10.1038/ismej.2007.98] [Citation(s) in RCA: 44] [Impact Index Per Article: 2.6] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Cabrol NA, Wettergreen D, Warren-Rhodes K, Grin EA, Moersch J, Diaz GC, Cockell CS, Coppin P, Demergasso C, Dohm JM, Ernst L, Fisher G, Glasgow J, Hardgrove C, Hock AN, Jonak D, Marinangeli L, Minkley E, Ori GG, Piatek J, Pudenz E, Smith T, Stubbs K, Thomas G, Thompson D, Waggoner A, Wagner M, Weinstein S, Wyatt M. Life in the Atacama: Searching for life with rovers (science overview). ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006jg000298] [Citation(s) in RCA: 35] [Impact Index Per Article: 2.1] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Nathalie A. Cabrol
- Space Sciences Division; NASA Ames Research Center; Moffett Field California USA
- SETI Institute; Mountain View California USA
| | - David Wettergreen
- Robotics Institute; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Kim Warren-Rhodes
- Space Sciences Division; NASA Ames Research Center; Moffett Field California USA
- SETI Institute; Mountain View California USA
| | - Edmond A. Grin
- Space Sciences Division; NASA Ames Research Center; Moffett Field California USA
- SETI Institute; Mountain View California USA
| | - Jeffrey Moersch
- Department of Earth and Planetary Sciences; University of Tennessee; Knoxville Tennessee USA
| | | | - Charles S. Cockell
- Planetary and Space Sciences Research Institute; Open University; Milton Keynes UK
| | - Peter Coppin
- Robotics Institute; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | | | - James M. Dohm
- Hydrology and Water Resources Department; University of Arizona; Tucson Arizona USA
| | - Lauren Ernst
- Department of Biology; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Gregory Fisher
- Department of Biology; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Justin Glasgow
- Department of Industrial Engineering; University of Iowa; Iowa City Iowa USA
| | - Craig Hardgrove
- Department of Earth and Planetary Sciences; University of Tennessee; Knoxville Tennessee USA
| | - Andrew N. Hock
- Department of Earth and Space Sciences; University of California; Los Angeles California USA
| | - Dominic Jonak
- Robotics Institute; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | | | - Edwin Minkley
- Department of Biology; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | | | - Jennifer Piatek
- Department of Earth and Planetary Sciences; University of Tennessee; Knoxville Tennessee USA
| | - Erin Pudenz
- Department of Industrial Engineering; University of Iowa; Iowa City Iowa USA
| | - Trey Smith
- Robotics Institute; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Kristen Stubbs
- Robotics Institute; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Geb Thomas
- Department of Industrial Engineering; University of Iowa; Iowa City Iowa USA
| | - David Thompson
- Robotics Institute; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Alan Waggoner
- Department of Biology; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Michael Wagner
- Robotics Institute; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Shmuel Weinstein
- Department of Biology; Carnegie Mellon University; Pittsburgh Pennsylvania USA
| | - Michael Wyatt
- Department of Earth and Planetary Sciences; University of Tennessee; Knoxville Tennessee USA
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Glotch TD, Rogers AD. Evidence for aqueous deposition of hematite- and sulfate-rich light-toned layered deposits in Aureum and Iani Chaos, Mars. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002863] [Citation(s) in RCA: 66] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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24
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Minitti ME, Weitz CM, Lane MD, Bishop JL. Morphology, chemistry, and spectral properties of Hawaiian rock coatings and implications for Mars. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002839] [Citation(s) in RCA: 65] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Farrand WH, Bell JF, Johnson JR, Jolliff BL, Knoll AH, McLennan SM, Squyres SW, Calvin WM, Grotzinger JP, Morris RV, Soderblom J, Thompson SD, Watters WA, Yen AS. Visible and near-infrared multispectral analysis of rocks at Meridiani Planum, Mars, by the Mars Exploration Rover Opportunity. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002773] [Citation(s) in RCA: 46] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Summers DP, Khare B. Nitrogen fixation on early Mars and other terrestrial planets: experimental demonstration of abiotic fixation reactions to nitrite and nitrate. ASTROBIOLOGY 2007; 7:333-41. [PMID: 17480164 DOI: 10.1089/ast.2006.0032] [Citation(s) in RCA: 18] [Impact Index Per Article: 1.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/15/2023]
Abstract
Understanding the abiotic fixation of nitrogen is critical to understanding planetary evolution and the potential origin of life on terrestrial planets. Nitrogen, an essential biochemical element, is certainly necessary for life as we know it to arise. The loss of atmospheric nitrogen can result in an incapacity to sustain liquid water and impact planetary habitability and hydrological processes that shape the surface. However, our current understanding of how such fixation may occur is almost entirely theoretical. This work experimentally examines the chemistry, in both gas and aqueous phases, that would occur from the formation of NO and CO by the shock heating of a model carbon dioxide/nitrogen atmosphere such as is currently thought to exist on early terrestrial planets. The results show that two pathways exist for the abiotic fixation of nitrogen from the atmosphere into the crust: one via HNO and another via NO(2). Fixation via HNO, which requires liquid water, could represent fixation on a planet with liquid water (and hence would also be a source of nitrogen for the origin of life). The pathway via NO(2) does not require liquid water and shows that fixation could occur even when liquid water has been lost from a planet's surface (for example, continuing to remove nitrogen through NO(2) reaction with ice, adsorbed water, etc.).
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Affiliation(s)
- David P Summers
- SETI Institute, c/o NASA Ames Research Center, Moffett Field, California 94035-1000, USA.
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27
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Developing luminescence dating for extraterrestrial applications: Characterization of martian simulants and minerals. RADIAT MEAS 2007. [DOI: 10.1016/j.radmeas.2007.01.038] [Citation(s) in RCA: 8] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/23/2022]
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28
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Johnson JR, Grundy WM, Lemmon MT, Bell JF, Johnson MJ, Deen R, Arvidson RE, Farrand WH, Guinness E, Hayes AG, Herkenhoff KE, Seelos F, Soderblom J, Squyres S. Spectrophotometric properties of materials observed by Pancam on the Mars Exploration Rovers: 2. Opportunity. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002762] [Citation(s) in RCA: 24] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
| | | | - Mark T. Lemmon
- Department of Atmospheric Sciences; Texas A&M University; College Station Texas USA
| | - James F. Bell
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - Miles J. Johnson
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - Robert Deen
- Jet Propulsion Laboratory; Pasadena California USA
| | - R. E. Arvidson
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | | | - E. Guinness
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - Alexander G. Hayes
- Lincoln Laboratory; Massachusetts Institute of Technology; Boston Massachusetts USA
| | - K. E. Herkenhoff
- Astrogeology Team; U.S. Geological Survey; Flagstaff Arizona USA
| | - F. Seelos
- Applied Physics Laboratory; Johns Hopkins University; Laurel Maryland USA
| | - J. Soderblom
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - S. Squyres
- Department of Astronomy; Cornell University; Ithaca New York USA
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Squyres SW, Arvidson RE, Bollen D, Bell JF, Brückner J, Cabrol NA, Calvin WM, Carr MH, Christensen PR, Clark BC, Crumpler L, Des Marais DJ, d'Uston C, Economou T, Farmer J, Farrand WH, Folkner W, Gellert R, Glotch TD, Golombek M, Gorevan S, Grant JA, Greeley R, Grotzinger J, Herkenhoff KE, Hviid S, Johnson JR, Klingelhöfer G, Knoll AH, Landis G, Lemmon M, Li R, Madsen MB, Malin MC, McLennan SM, McSween HY, Ming DW, Moersch J, Morris RV, Parker T, Rice JW, Richter L, Rieder R, Schröder C, Sims M, Smith M, Smith P, Soderblom LA, Sullivan R, Tosca NJ, Wänke H, Wdowiak T, Wolff M, Yen A. Overview of the Opportunity Mars Exploration Rover Mission to Meridiani Planum: Eagle Crater to Purgatory Ripple. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2006je002771] [Citation(s) in RCA: 126] [Impact Index Per Article: 7.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- S. W. Squyres
- Department of Astronomy; Cornell University, Space Sciences Building; Ithaca New York USA
| | - R. E. Arvidson
- Department Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - D. Bollen
- Department of Astronomy; Cornell University, Space Sciences Building; Ithaca New York USA
| | - J. F. Bell
- Department of Astronomy; Cornell University, Space Sciences Building; Ithaca New York USA
| | - J. Brückner
- Max Planck Institut für Chemie, Kosmochemie; Mainz Germany
| | - N. A. Cabrol
- NASA Ames/SETI Institute; Moffett Field California USA
| | - W. M. Calvin
- Department of Geological Sciences; University of Nevada, Reno; Reno Nevada USA
| | - M. H. Carr
- U.S. Geological Survey; Menlo Park California USA
| | - P. R. Christensen
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - B. C. Clark
- Lockheed Martin Corporation; Littleton Colorado USA
| | - L. Crumpler
- New Mexico Museum of Natural History and Science; Albuquerque New Mexico USA
| | | | - C. d'Uston
- Centre d'Etude Spatiale des Rayonnements; Toulouse France
| | - T. Economou
- Enrico Fermi Institute; University of Chicago; Chicago Illinois USA
| | - J. Farmer
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | | | - W. Folkner
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - R. Gellert
- Department of Physics; University of Guelph; Guelph, Ontario Canada
| | - T. D. Glotch
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - M. Golombek
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | | | - J. A. Grant
- Center for Earth and Planetary Studies; Smithsonian Institution; Washington, D. C. USA
| | - R. Greeley
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - J. Grotzinger
- Division of Geological and Planetary Sciences; California Institute of Technology; Pasadena California USA
| | | | - S. Hviid
- Max Planck Institut für Sonnensystemforschung; Katlenburg-Lindau Germany
| | | | - G. Klingelhöfer
- Institut für Anorganische und Analytische Chemie; Johannes Gutenberg-Universität; Mainz Germany
| | - A. H. Knoll
- Botanical Museum; Harvard University; Cambridge Massachusetts USA
| | - G. Landis
- NASA Glenn Research Center; Cleveland Ohio USA
| | - M. Lemmon
- Department of Atmospheric Sciences; Texas A&M University; College Station Texas USA
| | - R. Li
- Department of Civil and Environmental Engineering and Geodetic Science; Ohio State University; Columbus Ohio USA
| | - M. B. Madsen
- Niels Bohr Institute; Ørsted Laboratory; Copenhagen Denmark
| | - M. C. Malin
- Malin Space Science Systems; San Diego California USA
| | - S. M. McLennan
- Department of Geosciences; State University of New York; Stony Brook New York USA
| | - H. Y. McSween
- Department of Earth and Planetary Sciences; University of Tennessee; Knoxville Tennessee USA
| | - D. W. Ming
- NASA Johnson Space Center; Houston Texas USA
| | - J. Moersch
- Department of Earth and Planetary Sciences; University of Tennessee; Knoxville Tennessee USA
| | | | - T. Parker
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - J. W. Rice
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - L. Richter
- DLR Institute of Space Simulation; Cologne Germany
| | - R. Rieder
- Max Planck Institut für Chemie, Kosmochemie; Mainz Germany
| | - C. Schröder
- Institut für Anorganische und Analytische Chemie; Johannes Gutenberg-Universität; Mainz Germany
| | - M. Sims
- NASA Ames Research Center; Moffett Field California USA
| | - M. Smith
- NASA Goddard Space Flight Center; Greenbelt Maryland USA
| | - P. Smith
- Lunar and Planetary Laboratory; University of Arizona; Tucson Arizona USA
| | | | - R. Sullivan
- Department of Astronomy; Cornell University, Space Sciences Building; Ithaca New York USA
| | - N. J. Tosca
- Department of Geosciences; State University of New York; Stony Brook New York USA
| | - H. Wänke
- Max Planck Institut für Chemie, Kosmochemie; Mainz Germany
| | - T. Wdowiak
- Department of Physics; University of Alabama at Birmingham; Birmingham Alabama USA
| | - M. Wolff
- Space Science Institute; Martinez Georgia USA
| | - A. Yen
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
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Glotch TD, Bandfield JL. Determination and interpretation of surface and atmospheric Miniature Thermal Emission Spectrometer spectral end-members at the Meridiani Planum landing site. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002671] [Citation(s) in RCA: 41] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Timothy D. Glotch
- Division of Geological and Planetary Science; California Institute of Technology; Pasadena California USA
| | - Joshua L. Bandfield
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
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Weitz CM, Anderson RC, Bell JF, Farrand WH, Herkenhoff KE, Johnson JR, Jolliff BL, Morris RV, Squyres SW, Sullivan RJ. Soil grain analyses at Meridiani Planum, Mars. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002541] [Citation(s) in RCA: 69] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
- C. M. Weitz
- Planetary Science Institute; Tucson Arizona USA
| | | | - J. F. Bell
- Department of Astronomy; Cornell University; Ithaca New York USA
| | | | | | | | - B. L. Jolliff
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | | | - S. W. Squyres
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - R. J. Sullivan
- Department of Astronomy; Cornell University; Ithaca New York USA
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32
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Glotch TD, Bandfield JL, Christensen PR, Calvin WM, McLennan SM, Clark BC, Rogers AD, Squyres SW. Mineralogy of the light-toned outcrop at Meridiani Planum as seen by the Miniature Thermal Emission Spectrometer and implications for its formation. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002672] [Citation(s) in RCA: 86] [Impact Index Per Article: 4.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
- Timothy D. Glotch
- Division of Geological and Planetary Sciences; California Institute of Technology; Pasadena California USA
| | - Joshua L. Bandfield
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | | | - Wendy M. Calvin
- Department of Geological Sciences; University of Nevada; Reno Nevada USA
| | - Scott M. McLennan
- Department of Geosciences; State University of New York; Stony Brook New York USA
| | | | - A. Deanne Rogers
- Division of Geological and Planetary Sciences; California Institute of Technology; Pasadena California USA
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Souza-Egipsy V, Ormö J, Beitler Bowen B, Chan MA, Komatsu G. Ultrastructural study of iron oxide precipitates: implications for the search for biosignatures in the Meridiani hematite concretions, Mars. ASTROBIOLOGY 2006; 6:527-45. [PMID: 16916280 DOI: 10.1089/ast.2006.6.527] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/11/2023]
Abstract
Two terrestrial environments that have been proposed as analogs for the iron oxide precipitation in the Meridiani Planum region of Mars include the Rio Tinto precipitates and southern Utah marble concretions. Samples of two typical Utah iron oxide concretions and iron oxide precipitates in contact with biofilms from Rio Tinto have been studied to determine whether evidence could be found for biomediation in the precipitation process and to identify likely locations for fossil microorganisms. Scanning electron microscopy, energy dispersive X-ray, and gas chromatography-mass spectrometry (GC-MS) were used to search for biosignatures in the Utah marbles. The precipitation of iron oxides resembles known biosignatures, though organic compounds could not be confirmed with GC-MS analysis. In contrast, textural variations induced by biological activity are abundant in the modern Rio Tinto samples. Although no compelling evidence of direct or indirect biomediation was found in the Utah marbles, the ultrastructure of the iron oxide cement in the concretion suggests an inward growth during concretion precipitation from an initially spherical redox front. No indication for growth from a physical nucleus was found.
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Affiliation(s)
- Virginia Souza-Egipsy
- Centro de Astrobiología, Instituto Nacional de Técnica Aeroespacial, Torrejón de Ardoz, Madrid, Spain.
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34
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Kendrick MG, Kral TA. Survival of methanogens during desiccation: implications for life on Mars. ASTROBIOLOGY 2006; 6:546-51. [PMID: 16916281 DOI: 10.1089/ast.2006.6.546] [Citation(s) in RCA: 16] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/11/2023]
Abstract
The relatively recent discoveries that liquid water likely existed on the surface of past Mars and that methane currently exists in the martian atmosphere have fueled the possibility of extant or extinct life on Mars. One possible explanation for the existence of the methane would be the presence of methanogens in the subsurface. Methanogens are microorganisms in the domain Archaea that can metabolize molecular hydrogen as an energy source and carbon dioxide as a carbon source and produce methane. One factor of importance is the arid nature of Mars, at least at the surface. If one is to assume that life exists below the surface, then based on the only example of life that we know, liquid water must be present. Realistically, however, that liquid water may be seasonal just as it is at some locations on our home planet. Here we report on research designed to determine how long certain species of methanogens can survive desiccation on a Mars soil simulant, JSC Mars-1. Methanogenic cells were grown on JSC Mars-1, transferred to a desiccator within a Coy anaerobic environmental chamber, and maintained there for varying time periods. Following removal from the desiccator and rehydration, gas chromatographic measurements of methane indicated survival for varying time periods. Methanosarcina barkeri survived desiccation for 10 days, while Methanobacterium formicicum and Methanothermobacter wolfeii were able to survive for 25 days.
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35
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Fergason RL, Christensen PR, Bell JF, Golombek MP, Herkenhoff KE, Kieffer HH. Physical properties of the Mars Exploration Rover landing sites as inferred from Mini-TES-derived thermal inertia. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002583] [Citation(s) in RCA: 114] [Impact Index Per Article: 6.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Robin L. Fergason
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | | | - James F. Bell
- Department of Astronomy, Space Science Building; Cornell University; Ithaca New York USA
| | - Matthew P. Golombek
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
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36
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Grant JA, Arvidson RE, Crumpler LS, Golombek MP, Hahn B, Haldemann AFC, Li R, Soderblom LA, Squyres SW, Wright SP, Watters WA. Crater gradation in Gusev crater and Meridiani Planum, Mars. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002465] [Citation(s) in RCA: 57] [Impact Index Per Article: 3.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- J. A. Grant
- Center for Earth and Planetary Studies; National Air and Space Museum, Smithsonian Institution; Washington, DC USA
| | - R. E. Arvidson
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - L. S. Crumpler
- New Mexico Museum of Natural History and Science; Albuquerque New Mexico USA
| | - M. P. Golombek
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - B. Hahn
- Department of Geosciences; State University of New York; Stony Brook New York USA
| | - A. F. C. Haldemann
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | - R. Li
- Department of Civil and Environmental Engineering and Geodetic Science; Ohio State University; Columbus Ohio USA
| | | | - S. W. Squyres
- Department of Astronomy; Cornell University; Ithaca New York USA
| | - S. P. Wright
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - W. A. Watters
- Department of Earth, Atmospheric, and Planetary Sciences; Massachusetts Institute of Technology; Cambridge Massachusetts USA
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37
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Nunes DC, Phillips RJ. Radar subsurface mapping of the polar layered deposits on Mars. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002609] [Citation(s) in RCA: 57] [Impact Index Per Article: 3.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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38
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McCollom TM, Hynek BM. A volcanic environment for bedrock diagenesis at Meridiani Planum on Mars. Nature 2005; 438:1129-31. [PMID: 16372002 DOI: 10.1038/nature04390] [Citation(s) in RCA: 29] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/28/2005] [Accepted: 10/28/2005] [Indexed: 11/08/2022]
Abstract
Exposed bedrocks at Meridiani Planum on Mars display chemical and mineralogical evidence suggesting interaction with liquid water. On the basis of morphological observations as well as high abundances of haematite and sulphate minerals, the rocks have been interpreted as sediments that were deposited in a shallow body of briny water with subsequent evaporation leaving behind the sulphate minerals. The iron-sulphur mineralization at Meridiani has also been inferred to be analogous to that produced during oxidative weathering of metal sulphide minerals, such as occurs at acid mine drainage sites. Neither of these interpretations, however, is consistent with the chemical composition of the rocks. Here we propose an alternative model for diagenesis of Meridiani bedrock that involves deposition of volcanic ash followed by reaction with condensed sulphur dioxide- and water-bearing vapours emitted from fumaroles. This scenario does not require prolonged interaction with a standing body of surface water and may have occurred at high temperatures. Consequently, the model invokes an environment considerably less favourable for biological activity on Mars than previously proposed interpretations.
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Affiliation(s)
- Thomas M McCollom
- Center for Astrobiology, University of Colorado, Boulder, Colorado 80309, USA.
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39
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Sullivan R, Banfield D, Bell JF, Calvin W, Fike D, Golombek M, Greeley R, Grotzinger J, Herkenhoff K, Jerolmack D, Malin M, Ming D, Soderblom LA, Squyres SW, Thompson S, Watters WA, Weitz CM, Yen A. Aeolian processes at the Mars Exploration Rover Meridiani Planum landing site. Nature 2005; 436:58-61. [PMID: 16001061 DOI: 10.1038/nature03641] [Citation(s) in RCA: 213] [Impact Index Per Article: 11.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/23/2004] [Accepted: 04/12/2005] [Indexed: 11/09/2022]
Abstract
The martian surface is a natural laboratory for testing our understanding of the physics of aeolian (wind-related) processes in an environment different from that of Earth. Martian surface markings and atmospheric opacity are time-variable, indicating that fine particles at the surface are mobilized regularly by wind. Regolith (unconsolidated surface material) at the Mars Exploration Rover Opportunity's landing site has been affected greatly by wind, which has created and reoriented bedforms, sorted grains, and eroded bedrock. Aeolian features here preserve a unique record of changing wind direction and wind strength. Here we present an in situ examination of a martian bright wind streak, which provides evidence consistent with a previously proposed formational model for such features. We also show that a widely used criterion for distinguishing between aeolian saltation- and suspension-dominated grain behaviour is different on Mars, and that estimated wind friction speeds between 2 and 3 m s(-1), most recently from the northwest, are associated with recent global dust storms, providing ground truth for climate model predictions.
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Affiliation(s)
- R Sullivan
- Jet Propulsion Laboratory, California Institute of Technology, USA.
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Golombek MP, Arvidson RE, Bell JF, Christensen PR, Crisp JA, Crumpler LS, Ehlmann BL, Fergason RL, Grant JA, Greeley R, Haldemann AFC, Kass DM, Parker TJ, Schofield JT, Squyres SW, Zurek RW. Assessment of Mars Exploration Rover landing site predictions. Nature 2005; 436:44-8. [PMID: 16001058 DOI: 10.1038/nature03600] [Citation(s) in RCA: 85] [Impact Index Per Article: 4.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Abstract
Comprehensive analyses of remote sensing data during the three-year effort to select the Mars Exploration Rover landing sites at Gusev crater and at Meridiani Planum correctly predicted the atmospheric density profile during entry and descent and the safe and trafficable surfaces explored by the two rovers. The Gusev crater site was correctly predicted to be a low-relief surface that was less rocky than the Viking landing sites but comparably dusty. A dark, low-albedo, flat plain composed of basaltic sand and haematite with very few rocks was expected and found at Meridiani Planum. These results argue that future efforts to select safe landing sites based on existing and acquired remote sensing data will be successful. In contrast, geological interpretations of the sites based on remote sensing data were less certain and less successful, which emphasizes the inherent ambiguities in understanding surface geology from remotely sensed data and the uncertainty in predicting exactly what materials will be available for study at a landing site.
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Affiliation(s)
- M P Golombek
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA.
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41
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Borg L. A review of meteorite evidence for the timing of magmatism and of surface or near-surface liquid water on Mars. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2005je002402] [Citation(s) in RCA: 91] [Impact Index Per Article: 4.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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42
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Golden DC, Ming DW, Morris RV, Mertzman SA. Laboratory-simulated acid-sulfate weathering of basaltic materials: Implications for formation of sulfates at Meridiani Planum and Gusev crater, Mars. ACTA ACUST UNITED AC 2005. [DOI: 10.1029/2005je002451] [Citation(s) in RCA: 53] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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43
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Chan MA, Beitler Bowen B, Parry W, Ormö J, Komatsu G. Red rock and red planet diagenesis: Comparisons of Earth and Mars concretions. ACTA ACUST UNITED AC 2005. [DOI: 10.1130/1052-5173(2005)015[4:rrarpd]2.0.co;2] [Citation(s) in RCA: 52] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/30/2022]
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44
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Squyres SW, Arvidson RE, Bell JF, Brückner J, Cabrol NA, Calvin W, Carr MH, Christensen PR, Clark BC, Crumpler L, Marais DJD, d'Uston C, Economou T, Farmer J, Farrand W, Folkner W, Golombek M, Gorevan S, Grant JA, Greeley R, Grotzinger J, Haskin L, Herkenhoff KE, Hviid S, Johnson J, Klingelhöfer G, Knoll AH, Landis G, Lemmon M, Li R, Madsen MB, Malin MC, McLennan SM, McSween HY, Ming DW, Moersch J, Morris RV, Parker T, Rice JW, Richter L, Rieder R, Sims M, Smith M, Smith P, Soderblom LA, Sullivan R, Wänke H, Wdowiak T, Wolff M, Yen A. The Opportunity Rover's Athena science investigation at Meridiani Planum, Mars. Science 2004; 306:1698-703. [PMID: 15576602 DOI: 10.1126/science.1106171] [Citation(s) in RCA: 130] [Impact Index Per Article: 6.5] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Mars Exploration Rover Opportunity has investigated the landing site in Eagle crater and the nearby plains within Meridiani Planum. The soils consist of fine-grained basaltic sand and a surface lag of hematite-rich spherules, spherule fragments, and other granules. Wind ripples are common. Underlying the thin soil layer, and exposed within small impact craters and troughs, are flat-lying sedimentary rocks. These rocks are finely laminated, are rich in sulfur, and contain abundant sulfate salts. Small-scale cross-lamination in some locations provides evidence for deposition in flowing liquid water. We interpret the rocks to be a mixture of chemical and siliciclastic sediments formed by episodic inundation by shallow surface water, followed by evaporation, exposure, and desiccation. Hematite-rich spherules are embedded in the rock and eroding from them. We interpret these spherules to be concretions formed by postdepositional diagenesis, again involving liquid water.
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Affiliation(s)
- S W Squyres
- Department of Astronomy, Space Sciences Building, Cornell University, Ithaca, NY 14853, USA.
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45
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Arvidson RE, Anderson RC, Bartlett P, Bell JF, Christensen PR, Chu P, Davis K, Ehlmann BL, Golombek MP, Gorevan S, Guinness EA, Haldemann AFC, Herkenhoff KE, Landis G, Li R, Lindemann R, Ming DW, Myrick T, Parker T, Richter L, Seelos FP, Soderblom LA, Squyres SW, Sullivan RJ, Wilson J. Localization and physical property experiments conducted by Opportunity at Meridiani Planum. Science 2004; 306:1730-3. [PMID: 15576608 DOI: 10.1126/science.1104211] [Citation(s) in RCA: 117] [Impact Index Per Article: 5.9] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The location of the Opportunity landing site was determined to better than 10-m absolute accuracy from analyses of radio tracking data. We determined Rover locations during traverses with an error as small as several centimeters using engineering telemetry and overlapping images. Topographic profiles generated from rover data show that the plains are very smooth from meter- to centimeter-length scales, consistent with analyses of orbital observations. Solar cell output decreased because of the deposition of airborne dust on the panels. The lack of dust-covered surfaces on Meridiani Planum indicates that high velocity winds must remove this material on a continuing basis. The low mechanical strength of the evaporitic rocks as determined from grinding experiments, and the abundance of coarse-grained surface particles argue for differential erosion of Meridiani Planum.
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Affiliation(s)
- R E Arvidson
- Department of Earth and Planetary Sciences, Washington University, St. Louis, MO 63130, USA.
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46
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Bell JF, Squyres SW, Arvidson RE, Arneson HM, Bass D, Calvin W, Farrand WH, Goetz W, Golombek M, Greeley R, Grotzinger J, Guinness E, Hayes AG, Hubbard MYH, Herkenhoff KE, Johnson MJ, Johnson JR, Joseph J, Kinch KM, Lemmon MT, Li R, Madsen MB, Maki JN, Malin M, McCartney E, McLennan S, McSween HY, Ming DW, Morris RV, Dobrea EZN, Parker TJ, Proton J, Rice JW, Seelos F, Soderblom JM, Soderblom LA, Sohl-Dickstein JN, Sullivan RJ, Weitz CM, Wolff MJ. Pancam multispectral imaging results from the Opportunity Rover at Meridiani Planum. Science 2004; 306:1703-9. [PMID: 15576603 DOI: 10.1126/science.1105245] [Citation(s) in RCA: 115] [Impact Index Per Article: 5.8] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Panoramic Camera (Pancam) images from Meridiani Planum reveal a low-albedo, generally flat, and relatively rock-free surface. Within and around impact craters and fractures, laminated outcrop rocks with higher albedo are observed. Fine-grained materials include dark sand, bright ferric iron-rich dust, angular rock clasts, and millimeter-size spheroidal granules that are eroding out of the laminated rocks. Spectra of sand, clasts, and one dark plains rock are consistent with mafic silicates such as pyroxene and olivine. Spectra of both the spherules and the laminated outcrop materials indicate the presence of crystalline ferric oxides or oxyhydroxides. Atmospheric observations show a steady decline in dust opacity during the mission. Astronomical observations captured solar transits by Phobos and Deimos and time-lapse observations of sunsets.
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Affiliation(s)
- J F Bell
- Department of Astronomy, Cornell University, Ithaca NY 14853, USA.
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47
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Squyres SW, Grotzinger JP, Arvidson RE, Bell JF, Calvin W, Christensen PR, Clark BC, Crisp JA, Farrand WH, Herkenhoff KE, Johnson JR, Klingelhöfer G, Knoll AH, McLennan SM, McSween HY, Morris RV, Rice JW, Rieder R, Soderblom LA. In situ evidence for an ancient aqueous environment at Meridiani Planum, Mars. Science 2004; 306:1709-14. [PMID: 15576604 DOI: 10.1126/science.1104559] [Citation(s) in RCA: 244] [Impact Index Per Article: 12.2] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Sedimentary rocks at Eagle crater in Meridiani Planum are composed of fine-grained siliciclastic materials derived from weathering of basaltic rocks, sulfate minerals (including magnesium sulfate and jarosite) that constitute several tens of percent of the rock by weight, and hematite. Cross-stratification observed in rock outcrops indicates eolian and aqueous transport. Diagenetic features include hematite-rich concretions and crystal-mold vugs. We interpret the rocks to be a mixture of chemical and siliciclastic sediments with a complex diagenetic history. The environmental conditions that they record include episodic inundation by shallow surface water, evaporation, and desiccation. The geologic record at Meridiani Planum suggests that conditions were suitable for biological activity for a period of time in martian history.
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Affiliation(s)
- S W Squyres
- Department of Astronomy, Cornell University, Ithaca, NY 14853, USA.
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48
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Soderblom LA, Anderson RC, Arvidson RE, Bell JF, Cabrol NA, Calvin W, Christensen PR, Clark BC, Economou T, Ehlmann BL, Farrand WH, Fike D, Gellert R, Glotch TD, Golombek MP, Greeley R, Grotzinger JP, Herkenhoff KE, Jerolmack DJ, Johnson JR, Jolliff B, Klingelhöfer G, Knoll AH, Learner ZA, Li R, Malin MC, McLennan SM, McSween HY, Ming DW, Morris RV, Rice JW, Richter L, Rieder R, Rodionov D, Schröder C, Seelos FP, Soderblom JM, Squyres SW, Sullivan R, Watters WA, Weitz CM, Wyatt MB, Yen A, Zipfel J. Soils of Eagle Crater and Meridiani Planum at the Opportunity Rover Landing Site. Science 2004; 306:1723-6. [PMID: 15576606 DOI: 10.1126/science.1105127] [Citation(s) in RCA: 138] [Impact Index Per Article: 6.9] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The soils at the Opportunity site are fine-grained basaltic sands mixed with dust and sulfate-rich outcrop debris. Hematite is concentrated in spherules eroded from the strata. Ongoing saltation exhumes the spherules and their fragments, concentrating them at the surface. Spherules emerge from soils coated, perhaps from subsurface cementation, by salts. Two types of vesicular clasts may represent basaltic sand sources. Eolian ripples, armored by well-sorted hematite-rich grains, pervade Meridiani Planum. The thickness of the soil on the plain is estimated to be about a meter. The flatness and thin cover suggest that the plain may represent the original sedimentary surface.
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50
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Opportunity: First 90 days on Mars. Nature 2004. [DOI: 10.1038/news041129-10] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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