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Cycil LM, Hausrath EM, Ming DW, Adcock CT, Raymond J, Remias D, Ruemmele WP. Investigating the Growth of Algae Under Low Atmospheric Pressures for Potential Food and Oxygen Production on Mars. Front Microbiol 2021; 12:733244. [PMID: 34867849 PMCID: PMC8633435 DOI: 10.3389/fmicb.2021.733244] [Citation(s) in RCA: 7] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/30/2021] [Accepted: 09/28/2021] [Indexed: 11/13/2022] Open
Abstract
With long-term missions to Mars and beyond that would not allow resupply, a self-sustaining Bioregenerative Life Support System (BLSS) is essential. Algae are promising candidates for BLSS due to their completely edible biomass, fast growth rates and ease of handling. Extremophilic algae such as snow algae and halophilic algae may also be especially suited for a BLSS because of their ability to grow under extreme conditions. However, as indicated from over 50 prior space studies examining algal growth, little is known about the growth of algae at close to Mars-relevant pressures. Here, we explored the potential for five algae species to produce oxygen and food under low-pressure conditions relevant to Mars. These included Chloromonas brevispina, Kremastochrysopsis austriaca, Dunaliella salina, Chlorella vulgaris, and Spirulina plantensis. The cultures were grown in duplicate in a low-pressure growth chamber at 670 ± 20 mbar, 330 ± 20 mbar, 160 ± 20 mbar, and 80 ± 2.5 mbar pressures under continuous light exposure (62-70 μmol m-2 s-1). The atmosphere was evacuated and purged with CO2 after sampling each week. Growth experiments showed that D. salina, C. brevispina, and C. vulgaris were the best candidates to be used for BLSS at low pressure. The highest carrying capacities for each species under low pressure conditions were achieved by D. salina at 160 mbar (30.0 ± 4.6 × 105 cells/ml), followed by C. brevispina at 330 mbar (19.8 ± 0.9 × 105 cells/ml) and C. vulgaris at 160 mbar (13.0 ± 1.5 × 105 cells/ml). C. brevispina, D. salina, and C. vulgaris all also displayed substantial growth at the lowest tested pressure of 80 mbar reaching concentrations of 43.4 ± 2.5 × 104, 15.8 ± 1.3 × 104, and 57.1 ± 4.5 × 104 cells per ml, respectively. These results indicate that these species are promising candidates for the development of a Mars-based BLSS using low pressure (∼200-300 mbar) greenhouses and inflatable structures that have already been conceptualized and designed.
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Affiliation(s)
- Leena M Cycil
- Department of Geoscience, University of Nevada, Las Vegas, Las Vegas, NV, United States
| | - Elisabeth M Hausrath
- Department of Geoscience, University of Nevada, Las Vegas, Las Vegas, NV, United States
| | | | - Christopher T Adcock
- Department of Geoscience, University of Nevada, Las Vegas, Las Vegas, NV, United States
| | - James Raymond
- School of Life Sciences, University of Nevada, Las Vegas, Las Vegas, NV, United States
| | - Daniel Remias
- School of Engineering, University of Applied Sciences Upper Austria, Wels, Austria
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2
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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] [What about the content of this article? (0)] [Affiliation(s)] [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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3
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Morrison SM, Downs RT, Blake DF, Vaniman DT, Ming DW, Treiman AH, Achilles CN, Hazen RM, Yen AS, Morris RV, Rampe EB, Bristow TF, Chipera SJ, Castle N, Tu V, Walroth R. Predicting Martian mineral compositions in situ: crystal chemical techniques. Acta Crystallogr A Found Adv 2019. [DOI: 10.1107/s0108767319098015] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022] Open
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4
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Affiliation(s)
- Douglas W. Ming
- National Aeronautics and Space Administration; Johnson Space Center; Houston Texas
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5
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Peretyazhko TS, Niles PB, Sutter B, Morris RV, Agresti DG, Le L, Ming DW. Smectite formation in the presence of sulfuric acid: Implications for acidic smectite formation on early Mars. Geochim Cosmochim Acta 2018; 220:248-260. [PMID: 32801388 PMCID: PMC7427815 DOI: 10.1016/j.gca.2017.10.004] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/19/2023]
Abstract
The excess of orbital detection of smectite deposits compared to carbonate deposits on the martian surface presents an enigma because smectite and carbonate formations are both favored alteration products of basalt under neutral to alkaline conditions. We propose that Mars experienced acidic events caused by sulfuric acid (H2SO4) that permitted phyllosilicate, but inhibited carbonate, formation. To experimentally verify this hypothesis, we report the first synthesis of smectite from Mars-analogue glass-rich basalt simulant (66 wt% glass, 32 wt% olivine, 2 wt% chromite) in the presence of H2SO4 under hydrothermal conditions (~200 °C). Smectites were analyzed by X-ray diffraction, Mossbauer spectroscopy, visible and near-infrared reflectance spectroscopy and electron microprobe to characterize mineralogy and chemical composition. Solution chemistry was determined by Inductively Coupled Plasma Mass Spectrometry. Basalt simulant suspensions in 11-42 mM H2SO4 were acidic with pH ≤ 2 at the beginning of incubation and varied from acidic (pH 1.8) to mildly alkaline (pH 8.4) at the end of incubation. Alteration of glass phase during reaction of the basalt simulant with H2SO4 led to formation of the dioctahedral smectite at final pH ~3 and trioctahedral smectite saponite at final pH ~4 and higher. Anhydrite and hematite formed in the final pH range from 1.8 to 8.4 while natroalunite was detected at pH 1.8. Hematite was precipitated as a result of oxidative dissolution of olivine present in Adirondack basalt simulant. Formation of secondary phases, including smectite, resulted in release of variable amounts of Si, Mg, Na and Ca while solubilization of Al and Fe was low. Comparison of mineralogical and solution chemistry data indicated that the type of smectite (i.e., dioctahedral vs trioctahedral) was likely controlled by Mg leaching from altering basalt and substantial Mg loss created favorable conditions for formation of dioctahedral smectite. We present a model for global-scale smectite formation on Mars via acid-sulfate conditions created by the volcanic outgassing of SO2 in the Noachian and early Hesperian.
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Affiliation(s)
| | - P B Niles
- NASA Johnson Space Center, Houston, TX 77058
| | - B Sutter
- Jacobs, NASA Johnson Space Center, Houston, TX 77058
| | - R V Morris
- NASA Johnson Space Center, Houston, TX 77058
| | - D G Agresti
- University of Alabama at Birmingham, Birmingham, AL 35294
| | - L Le
- Jacobs, NASA Johnson Space Center, Houston, TX 77058
| | - D W Ming
- NASA Johnson Space Center, Houston, TX 77058
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6
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Ehlmann BL, Edgett KS, Sutter B, Achilles CN, Litvak ML, Lapotre MGA, Sullivan R, Fraeman AA, Arvidson RE, Blake DF, Bridges NT, Conrad PG, Cousin A, Downs RT, Gabriel TSJ, Gellert R, Hamilton VE, Hardgrove C, Johnson JR, Kuhn S, Mahaffy PR, Maurice S, McHenry M, Meslin PY, Ming DW, Minitti ME, Morookian JM, Morris RV, O'Connell-Cooper CD, Pinet PC, Rowland SK, Schröder S, Siebach KL, Stein NT, Thompson LM, Vaniman DT, Vasavada AR, Wellington DF, Wiens RC, Yen AS. Chemistry, mineralogy, and grain properties at Namib and High dunes, Bagnold dune field, Gale crater, Mars: A synthesis of Curiosity rover observations. J Geophys Res Planets 2017; 122:2510-2543. [PMID: 29497589 DOI: 10.1002/2016je005225] [Citation(s) in RCA: 26] [Impact Index Per Article: 3.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/16/2017] [Revised: 05/18/2017] [Accepted: 05/19/2017] [Indexed: 05/25/2023]
Abstract
The Mars Science Laboratory Curiosity rover performed coordinated measurements to examine the textures and compositions of aeolian sands in the active Bagnold dune field. The Bagnold sands are rounded to subrounded, very fine to medium sized (~45-500 μm) with ≥6 distinct grain colors. In contrast to sands examined by Curiosity in a dust-covered, inactive bedform called Rocknest and soils at other landing sites, Bagnold sands are darker, less red, better sorted, have fewer silt-sized or smaller grains, and show no evidence for cohesion. Nevertheless, Bagnold mineralogy and Rocknest mineralogy are similar with plagioclase, olivine, and pyroxenes in similar proportions comprising >90% of crystalline phases, along with a substantial amorphous component (35% ± 15%). Yet Bagnold and Rocknest bulk chemistry differ. Bagnold sands are Si enriched relative to other soils at Gale crater, and H2O, S, and Cl are lower relative to all previously measured Martian soils and most Gale crater rocks. Mg, Ni, Fe, and Mn are enriched in the coarse-sieved fraction of Bagnold sands, corroborated by visible/near-infrared spectra that suggest enrichment of olivine. Collectively, patterns in major element chemistry and volatile release data indicate two distinctive volatile reservoirs in Martian soils: (1) amorphous components in the sand-sized fraction (represented by Bagnold) that are Si-enriched, hydroxylated alteration products and/or H2O- or OH-bearing impact or volcanic glasses and (2) amorphous components in the fine fraction (<40 μm; represented by Rocknest and other bright soils) that are Fe, S, and Cl enriched with low Si and adsorbed and structural H2O.
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7
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Niles PB, Michalski J, Ming DW, Golden DC. Elevated olivine weathering rates and sulfate formation at cryogenic temperatures on Mars. Nat Commun 2017; 8:998. [PMID: 29044111 PMCID: PMC5647339 DOI: 10.1038/s41467-017-01227-7] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/20/2017] [Accepted: 08/31/2017] [Indexed: 11/12/2022] Open
Abstract
Large Hesperian-aged (~3.7 Ga) layered deposits of sulfate-rich sediments in the equatorial regions of Mars have been suggested to be evidence for ephemeral playa environments. But early Mars may not have been warm enough to support conditions similar to what occurs in arid environments on Earth. Instead cold, icy environments may have been widespread. Under cryogenic conditions sulfate formation might be blocked, since kinetics of silicate weathering are typically strongly retarded at temperatures well below 0 °C. But cryo-concentration of acidic solutions may counteract the slow kinetics. Here we show that cryo-concentrated acidic brines rapidly chemically weather olivine minerals and form sulfate minerals at temperatures as low as −60 °C. These experimental results demonstrate the viability of sulfate formation under current Martian conditions, even in the polar regions. An ice-hosted sedimentation and weathering model may provide a compelling description of the origin of large Hesperian-aged layered sulfate deposits on Mars. Sulphate-rich sediments have been taken as evidence of surface water on Mars. Here, the authors show that cryo-concentrated brines chemically weather olivine minerals forming sulfate minerals at up to −60 °C, showing that cryogenic weathering and sulfate formation can occur under current Martian conditions.
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Affiliation(s)
- Paul B Niles
- Astromaterials Research and Exploration Science Division, NASA Johnson Space Center, Houston, TX, 77058, USA.
| | - Joseph Michalski
- Department of Earth Sciences and Laboratory for Space Research, University of Hong Kong, Hong Kong, China
| | - Douglas W Ming
- Astromaterials Research and Exploration Science Division, NASA Johnson Space Center, Houston, TX, 77058, USA
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8
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Hurowitz JA, Grotzinger JP, Fischer WW, McLennan SM, Milliken RE, Stein N, Vasavada AR, Blake DF, Dehouck E, Eigenbrode JL, Fairén AG, Frydenvang J, Gellert R, Grant JA, Gupta S, Herkenhoff KE, Ming DW, Rampe EB, Schmidt ME, Siebach KL, Stack-Morgan K, Sumner DY, Wiens RC. Redox stratification of an ancient lake in Gale crater, Mars. Science 2017; 356:356/6341/eaah6849. [PMID: 28572336 DOI: 10.1126/science.aah6849] [Citation(s) in RCA: 171] [Impact Index Per Article: 24.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/31/2016] [Accepted: 04/19/2017] [Indexed: 11/02/2022]
Abstract
In 2012, NASA's Curiosity rover landed on Mars to assess its potential as a habitat for past life and investigate the paleoclimate record preserved by sedimentary rocks inside the ~150-kilometer-diameter Gale impact crater. Geological reconstructions from Curiosity rover data have revealed an ancient, habitable lake environment fed by rivers draining into the crater. We synthesize geochemical and mineralogical data from lake-bed mudstones collected during the first 1300 martian solar days of rover operations in Gale. We present evidence for lake redox stratification, established by depth-dependent variations in atmospheric oxidant and dissolved-solute concentrations. Paleoclimate proxy data indicate that a transition from colder to warmer climate conditions is preserved in the stratigraphy. Finally, a late phase of geochemical modification by saline fluids is recognized.
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Affiliation(s)
- J A Hurowitz
- Department of Geosciences, Stony Brook University, Stony Brook, NY 11794-2100, USA.
| | - J P Grotzinger
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
| | - W W Fischer
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
| | - S M McLennan
- Department of Geosciences, Stony Brook University, Stony Brook, NY 11794-2100, USA
| | - R E Milliken
- Department of Geological Sciences, Brown University, Providence, RI 02912, USA
| | - N Stein
- Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
| | - A R Vasavada
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - D F Blake
- Department of Space Sciences, NASA Ames Research Center, Moffett Field, CA 94035, USA
| | - E Dehouck
- Institut de Recherche en Astrophysique et Planétologie, University Paul Sabatier, 31028 Toulouse, France
| | - J L Eigenbrode
- NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - A G Fairén
- Centro de Astrobiología, Consejo Superior de Investigaciones Científicas-Instituto Nacional de Técnica Aeroespacial (CSIC-INTA), 28850 Madrid, Spain.,Department of Astronomy, Cornell University, Ithaca, NY 14853, USA
| | - J Frydenvang
- Space Remote Sensing, Los Alamos National Laboratory, Los Alamos, NM 87544, USA.,University of Copenhagen, 1350 Copenhagen, Denmark
| | - R Gellert
- Department of Physics, University of Guelph, Guelph, Ontario N1G 2W1, Canada
| | - J A Grant
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20560, USA
| | - S Gupta
- Department of Earth Science and Engineering, Imperial College London, London SW7 2AZ, UK
| | | | - D W Ming
- Astromaterials Research and Exploration Science Division, NASA Johnson Space Center, Houston, TX 77058, USA
| | - E B Rampe
- NASA Johnson Space Center, Houston, TX 77058, USA
| | - M E Schmidt
- Department of Earth Sciences, Brock University, St. Catharines, Ontario L2S 3A1, Canada
| | - K L Siebach
- Department of Geosciences, Stony Brook University, Stony Brook, NY 11794-2100, USA.,Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA
| | - K Stack-Morgan
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
| | - D Y Sumner
- Department of Earth and Planetary Sciences, University of California-Davis, Davis, CA 95616, USA
| | - R C Wiens
- Space Remote Sensing, Los Alamos National Laboratory, Los Alamos, NM 87544, USA
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9
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Freissinet C, Glavin DP, Mahaffy PR, Miller KE, Eigenbrode JL, Summons RE, Brunner AE, Buch A, Szopa C, Archer PD, Franz HB, Atreya SK, Brinckerhoff WB, Cabane M, Coll P, Conrad PG, Des Marais DJ, Dworkin JP, Fairén AG, François P, Grotzinger JP, Kashyap S, ten Kate IL, Leshin LA, Malespin CA, Martin MG, Martin-Torres FJ, McAdam AC, Ming DW, Navarro-González R, Pavlov AA, Prats BD, Squyres SW, Steele A, Stern JC, Sumner DY, Sutter B, Zorzano MP. Organic molecules in the Sheepbed Mudstone, Gale Crater, Mars. J Geophys Res Planets 2015; 120:495-514. [PMID: 26690960 PMCID: PMC4672966 DOI: 10.1002/2014je004737] [Citation(s) in RCA: 149] [Impact Index Per Article: 16.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/03/2014] [Revised: 01/12/2015] [Accepted: 02/13/2015] [Indexed: 05/04/2023]
Abstract
UNLABELLED The Sample Analysis at Mars (SAM) instrument on board the Mars Science Laboratory Curiosity rover is designed to conduct inorganic and organic chemical analyses of the atmosphere and the surface regolith and rocks to help evaluate the past and present habitability potential of Mars at Gale Crater. Central to this task is the development of an inventory of any organic molecules present to elucidate processes associated with their origin, diagenesis, concentration, and long-term preservation. This will guide the future search for biosignatures. Here we report the definitive identification of chlorobenzene (150-300 parts per billion by weight (ppbw)) and C2 to C4 dichloroalkanes (up to 70 ppbw) with the SAM gas chromatograph mass spectrometer (GCMS) and detection of chlorobenzene in the direct evolved gas analysis (EGA) mode, in multiple portions of the fines from the Cumberland drill hole in the Sheepbed mudstone at Yellowknife Bay. When combined with GCMS and EGA data from multiple scooped and drilled samples, blank runs, and supporting laboratory analog studies, the elevated levels of chlorobenzene and the dichloroalkanes cannot be solely explained by instrument background sources known to be present in SAM. We conclude that these chlorinated hydrocarbons are the reaction products of Martian chlorine and organic carbon derived from Martian sources (e.g., igneous, hydrothermal, atmospheric, or biological) or exogenous sources such as meteorites, comets, or interplanetary dust particles. KEY POINTS First in situ evidence of nonterrestrial organics in Martian surface sediments Chlorinated hydrocarbons identified in the Sheepbed mudstone by SAM Organics preserved in sample exposed to ionizing radiation and oxidative condition.
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Affiliation(s)
- C Freissinet
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
- NASA Postdoctoral Program, Oak Ridge Associated UniversitiesOak Ridge, Tennessee, USA
- Correspondence to:
C. Freissinet and P. R. Mahaffy,, ,
| | - D P Glavin
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - P R Mahaffy
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
- Correspondence to:
C. Freissinet and P. R. Mahaffy,, ,
| | - K E Miller
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of TechnologyCambridge, Massachusetts, USA
| | - J L Eigenbrode
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - R E Summons
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of TechnologyCambridge, Massachusetts, USA
| | - A E Brunner
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
- Center for Research and Exploration in Space Science & Technology, University of MarylandCollege Park, Maryland, USA
| | - A Buch
- Laboratoire de Génie des Procédés et Matériaux, Ecole Centrale ParisChâtenay-Malabry, France
| | - C Szopa
- Laboratoire Atmosphères, Milieux, Observations Spatiales, Pierre and Marie Curie University, Université de Versailles Saint-Quentin-en-Yvelines, and CNRSParis, France
| | - P D Archer
- Jacobs, NASA Johnson Space CenterHouston, Texas, USA
| | - H B Franz
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
- Center for Research and Exploration in Space Science & Technology, University of Maryland, Baltimore CountyBaltimore, Maryland, USA
| | - S K Atreya
- Department of Atmospheric, Oceanic and Space Sciences, University of MichiganAnn Arbor, Michigan, USA
| | - W B Brinckerhoff
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - M Cabane
- Laboratoire Atmosphères, Milieux, Observations Spatiales, Pierre and Marie Curie University, Université de Versailles Saint-Quentin-en-Yvelines, and CNRSParis, France
| | - P Coll
- Laboratoire Interuniversitaire des Systèmes Atmosphériques, Université Paris-Est Créteil, Paris VII–Denis Diderot University, and CNRSCréteil, France
| | - P G Conrad
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - D J Des Marais
- Exobiology Branch, NASA Ames Research CenterMoffett Field, California, USA
| | - J P Dworkin
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - A G Fairén
- Department of Astronomy, Cornell UniversityIthaca, New York, USA
- Centro de Astrobiología, INTA-CSICMadrid, Spain
| | - P François
- Department of Atmospheric, Oceanic and Space Sciences, University of MichiganAnn Arbor, Michigan, USA
| | - J P Grotzinger
- Division of Geological and Planetary Sciences, California Institute of TechnologyPasadena, California, USA
| | - S Kashyap
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
- Center for Research and Exploration in Space Science & Technology, University of Maryland, Baltimore CountyBaltimore, Maryland, USA
| | - I L ten Kate
- Earth Sciences Department, Utrecht UniversityUtrecht, Netherlands
| | - L A Leshin
- Department of Earth and Environmental Sciences and School of Science, Rensselaer Polytechnic InstituteTroy, New York, USA
| | - C A Malespin
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
- Goddard Earth Sciences and Technologies and Research, Universities Space Research AssociationColumbia, Maryland, USA
| | - M G Martin
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
- Department of Chemistry, Catholic University of AmericaWashington, District of Columbia, USA
| | - F J Martin-Torres
- Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR)Granada, Spain
- Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of TechnologyKiruna, Sweden
| | - A C McAdam
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - D W Ming
- Astromaterials Research and Exploration Science Directorate, NASA Johnson Space CenterHouston, Texas, USA
| | - R Navarro-González
- Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Ciudad UniversitariaMéxico City, Mexico
| | - A A Pavlov
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - B D Prats
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - S W Squyres
- Department of Astronomy, Cornell UniversityIthaca, New York, USA
| | - A Steele
- Geophysical Laboratory, Carnegie Institution of WashingtonWashington, District of Columbia, USA
| | - J C Stern
- Solar System Exploration Division, NASA Goddard Space Flight CenterGreenbelt, Maryland, USA
| | - D Y Sumner
- Department of Earth and Planetary Sciences, University of CaliforniaDavis, California, USA
| | - B Sutter
- Jacobs, NASA Johnson Space CenterHouston, Texas, USA
| | - M-P Zorzano
- Centro de Astrobiologia (INTA-CSIC)Madrid, Spain
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10
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Freissinet C, Glavin DP, Mahaffy PR, Miller KE, Eigenbrode JL, Summons RE, Brunner AE, Buch A, Szopa C, Archer PD, Franz HB, Atreya SK, Brinckerhoff WB, Cabane M, Coll P, Conrad PG, Des Marais DJ, Dworkin JP, Fairén AG, François P, Grotzinger JP, Kashyap S, Ten Kate IL, Leshin LA, Malespin CA, Martin MG, Martin-Torres FJ, McAdam AC, Ming DW, Navarro-González R, Pavlov AA, Prats BD, Squyres SW, Steele A, Stern JC, Sumner DY, Sutter B, Zorzano MP. Organic molecules in the Sheepbed Mudstone, Gale Crater, Mars. J Geophys Res Planets 2015; 120:495-514. [PMID: 26690960 DOI: 10.1002/2015je004884.received] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Subscribe] [Scholar Register] [Received: 10/03/2014] [Revised: 01/12/2015] [Accepted: 02/13/2015] [Indexed: 05/25/2023]
Abstract
UNLABELLED The Sample Analysis at Mars (SAM) instrument on board the Mars Science Laboratory Curiosity rover is designed to conduct inorganic and organic chemical analyses of the atmosphere and the surface regolith and rocks to help evaluate the past and present habitability potential of Mars at Gale Crater. Central to this task is the development of an inventory of any organic molecules present to elucidate processes associated with their origin, diagenesis, concentration, and long-term preservation. This will guide the future search for biosignatures. Here we report the definitive identification of chlorobenzene (150-300 parts per billion by weight (ppbw)) and C2 to C4 dichloroalkanes (up to 70 ppbw) with the SAM gas chromatograph mass spectrometer (GCMS) and detection of chlorobenzene in the direct evolved gas analysis (EGA) mode, in multiple portions of the fines from the Cumberland drill hole in the Sheepbed mudstone at Yellowknife Bay. When combined with GCMS and EGA data from multiple scooped and drilled samples, blank runs, and supporting laboratory analog studies, the elevated levels of chlorobenzene and the dichloroalkanes cannot be solely explained by instrument background sources known to be present in SAM. We conclude that these chlorinated hydrocarbons are the reaction products of Martian chlorine and organic carbon derived from Martian sources (e.g., igneous, hydrothermal, atmospheric, or biological) or exogenous sources such as meteorites, comets, or interplanetary dust particles. KEY POINTS First in situ evidence of nonterrestrial organics in Martian surface sediments Chlorinated hydrocarbons identified in the Sheepbed mudstone by SAM Organics preserved in sample exposed to ionizing radiation and oxidative condition.
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Affiliation(s)
- C Freissinet
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA ; NASA Postdoctoral Program, Oak Ridge Associated Universities Oak Ridge, Tennessee, USA
| | - D P Glavin
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - P R Mahaffy
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - K E Miller
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology Cambridge, Massachusetts, USA
| | - J L Eigenbrode
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - R E Summons
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology Cambridge, Massachusetts, USA
| | - A E Brunner
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA ; Center for Research and Exploration in Space Science & Technology, University of Maryland College Park, Maryland, USA
| | - A Buch
- Laboratoire de Génie des Procédés et Matériaux, Ecole Centrale Paris Châtenay-Malabry, France
| | - C Szopa
- Laboratoire Atmosphères, Milieux, Observations Spatiales, Pierre and Marie Curie University, Université de Versailles Saint-Quentin-en-Yvelines, and CNRS Paris, France
| | - P D Archer
- Jacobs, NASA Johnson Space Center Houston, Texas, USA
| | - H B Franz
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA ; Center for Research and Exploration in Space Science & Technology, University of Maryland, Baltimore County Baltimore, Maryland, USA
| | - S K Atreya
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan Ann Arbor, Michigan, USA
| | - W B Brinckerhoff
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - M Cabane
- Laboratoire Atmosphères, Milieux, Observations Spatiales, Pierre and Marie Curie University, Université de Versailles Saint-Quentin-en-Yvelines, and CNRS Paris, France
| | - P Coll
- Laboratoire Interuniversitaire des Systèmes Atmosphériques, Université Paris-Est Créteil, Paris VII-Denis Diderot University, and CNRS Créteil, France
| | - P G Conrad
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - D J Des Marais
- Exobiology Branch, NASA Ames Research Center Moffett Field, California, USA
| | - J P Dworkin
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - A G Fairén
- Department of Astronomy, Cornell University Ithaca, New York, USA ; Centro de Astrobiología, INTA-CSIC Madrid, Spain
| | - P François
- Department of Atmospheric, Oceanic and Space Sciences, University of Michigan Ann Arbor, Michigan, USA
| | - J P Grotzinger
- Division of Geological and Planetary Sciences, California Institute of Technology Pasadena, California, USA
| | - S Kashyap
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA ; Center for Research and Exploration in Space Science & Technology, University of Maryland, Baltimore County Baltimore, Maryland, USA
| | - I L Ten Kate
- Earth Sciences Department, Utrecht University Utrecht, Netherlands
| | - L A Leshin
- Department of Earth and Environmental Sciences and School of Science, Rensselaer Polytechnic Institute Troy, New York, USA
| | - C A Malespin
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA ; Goddard Earth Sciences and Technologies and Research, Universities Space Research Association Columbia, Maryland, USA
| | - M G Martin
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA ; Department of Chemistry, Catholic University of America Washington, District of Columbia, USA
| | - F J Martin-Torres
- Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR) Granada, Spain ; Division of Space Technology, Department of Computer Science, Electrical and Space Engineering, Luleå University of Technology Kiruna, Sweden
| | - A C McAdam
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - D W Ming
- Astromaterials Research and Exploration Science Directorate, NASA Johnson Space Center Houston, Texas, USA
| | - R Navarro-González
- Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Ciudad Universitaria México City, Mexico
| | - A A Pavlov
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - B D Prats
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - S W Squyres
- Department of Astronomy, Cornell University Ithaca, New York, USA
| | - A Steele
- Geophysical Laboratory, Carnegie Institution of Washington Washington, District of Columbia, USA
| | - J C Stern
- Solar System Exploration Division, NASA Goddard Space Flight Center Greenbelt, Maryland, USA
| | - D Y Sumner
- Department of Earth and Planetary Sciences, University of California Davis, California, USA
| | - B Sutter
- Jacobs, NASA Johnson Space Center Houston, Texas, USA
| | - M-P Zorzano
- Centro de Astrobiologia (INTA-CSIC) Madrid, Spain
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Vaniman DT, Bish DL, Ming DW, Bristow TF, Morris RV, Blake DF, Chipera SJ, Morrison SM, Treiman AH, Rampe EB, Rice M, Achilles CN, Grotzinger JP, McLennan SM, Williams J, Bell JF, Newsom HE, Downs RT, Maurice S, Sarrazin P, Yen AS, Morookian JM, Farmer JD, Stack K, Milliken RE, Ehlmann BL, Sumner DY, Berger G, Crisp JA, Hurowitz JA, Anderson R, Des Marais DJ, Stolper EM, Edgett KS, Gupta S, Spanovich N. Mineralogy of a mudstone at Yellowknife Bay, Gale crater, Mars. Science 2014. [PMID: 24324271 DOI: 10.1126/science1243480] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 05/10/2023]
Abstract
Sedimentary rocks at Yellowknife Bay (Gale crater) on Mars include mudstone sampled by the Curiosity rover. The samples, John Klein and Cumberland, contain detrital basaltic minerals, calcium sulfates, iron oxide or hydroxides, iron sulfides, amorphous material, and trioctahedral smectites. The John Klein smectite has basal spacing of ~10 angstroms, indicating little interlayer hydration. The Cumberland smectite has basal spacing at both ~13.2 and ~10 angstroms. The larger spacing suggests a partially chloritized interlayer or interlayer magnesium or calcium facilitating H2O retention. Basaltic minerals in the mudstone are similar to those in nearby eolian deposits. However, the mudstone has far less Fe-forsterite, possibly lost with formation of smectite plus magnetite. Late Noachian/Early Hesperian or younger age indicates that clay mineral formation on Mars extended beyond Noachian time.
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Affiliation(s)
- D T Vaniman
- Planetary Science Institute, Tucson, AZ 85719, USA
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12
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McLennan SM, Anderson RB, Bell JF, Bridges JC, Calef F, Campbell JL, Clark BC, Clegg S, Conrad P, Cousin A, Des Marais DJ, Dromart G, Dyar MD, Edgar LA, Ehlmann BL, Fabre C, Forni O, Gasnault O, Gellert R, Gordon S, Grant JA, Grotzinger JP, Gupta S, Herkenhoff KE, Hurowitz JA, King PL, Le Mouélic S, Leshin LA, Léveillé R, Lewis KW, Mangold N, Maurice S, Ming DW, Morris RV, Nachon M, Newsom HE, Ollila AM, Perrett GM, Rice MS, Schmidt ME, Schwenzer SP, Stack K, Stolper EM, Sumner DY, Treiman AH, VanBommel S, Vaniman DT, Vasavada A, Wiens RC, Yingst RA. Elemental geochemistry of sedimentary rocks at Yellowknife Bay, Gale crater, Mars. Science 2013; 343:1244734. [PMID: 24324274 DOI: 10.1126/science.1244734] [Citation(s) in RCA: 214] [Impact Index Per Article: 19.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Sedimentary rocks examined by the Curiosity rover at Yellowknife Bay, Mars, were derived from sources that evolved from an approximately average martian crustal composition to one influenced by alkaline basalts. No evidence of chemical weathering is preserved, indicating arid, possibly cold, paleoclimates and rapid erosion and deposition. The absence of predicted geochemical variations indicates that magnetite and phyllosilicates formed by diagenesis under low-temperature, circumneutral pH, rock-dominated aqueous conditions. Analyses of diagenetic features (including concretions, raised ridges, and fractures) at high spatial resolution indicate that they are composed of iron- and halogen-rich components, magnesium-iron-chlorine-rich components, and hydrated calcium sulfates, respectively. Composition of a cross-cutting dike-like feature is consistent with sedimentary intrusion. The geochemistry of these sedimentary rocks provides further evidence for diverse depositional and diagenetic sedimentary environments during the early history of Mars.
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Affiliation(s)
- S M McLennan
- Department of Geosciences, State University of New York, Stony Brook, NY 11794, USA
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13
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Ming DW, Archer PD, Glavin DP, Eigenbrode JL, Franz HB, Sutter B, Brunner AE, Stern JC, Freissinet C, McAdam AC, Mahaffy PR, Cabane M, Coll P, Campbell JL, Atreya SK, Niles PB, Bell JF, Bish DL, Brinckerhoff WB, Buch A, Conrad PG, Des Marais DJ, Ehlmann BL, Fairén AG, Farley K, Flesch GJ, Francois P, Gellert R, Grant JA, Grotzinger JP, Gupta S, Herkenhoff KE, Hurowitz JA, Leshin LA, Lewis KW, McLennan SM, Miller KE, Moersch J, Morris RV, Navarro-González R, Pavlov AA, Perrett GM, Pradler I, Squyres SW, Summons RE, Steele A, Stolper EM, Sumner DY, Szopa C, Teinturier S, Trainer MG, Treiman AH, Vaniman DT, Vasavada AR, Webster CR, Wray JJ, Yingst RA. Volatile and organic compositions of sedimentary rocks in Yellowknife Bay, Gale crater, Mars. Science 2013; 343:1245267. [PMID: 24324276 DOI: 10.1126/science.1245267] [Citation(s) in RCA: 135] [Impact Index Per Article: 12.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
H2O, CO2, SO2, O2, H2, H2S, HCl, chlorinated hydrocarbons, NO, and other trace gases were evolved during pyrolysis of two mudstone samples acquired by the Curiosity rover at Yellowknife Bay within Gale crater, Mars. H2O/OH-bearing phases included 2:1 phyllosilicate(s), bassanite, akaganeite, and amorphous materials. Thermal decomposition of carbonates and combustion of organic materials are candidate sources for the CO2. Concurrent evolution of O2 and chlorinated hydrocarbons suggests the presence of oxychlorine phase(s). Sulfides are likely sources for sulfur-bearing species. Higher abundances of chlorinated hydrocarbons in the mudstone compared with Rocknest windblown materials previously analyzed by Curiosity suggest that indigenous martian or meteoritic organic carbon sources may be preserved in the mudstone; however, the carbon source for the chlorinated hydrocarbons is not definitively of martian origin.
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Affiliation(s)
- D W Ming
- Astromaterials Research and Exploration Science Directorate, NASA Johnson Space Center, Houston, TX 77058, USA
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14
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Bish DL, Blake DF, Vaniman DT, Chipera SJ, Morris RV, Ming DW, Treiman AH, Sarrazin P, Morrison SM, Downs RT, Achilles CN, Yen AS, Bristow TF, Crisp JA, Morookian JM, Farmer JD, Rampe EB, Stolper EM, Spanovich N. X-ray diffraction results from Mars Science Laboratory: mineralogy of Rocknest at Gale crater. Science 2013; 341:1238932. [PMID: 24072925 DOI: 10.1126/science.1238932] [Citation(s) in RCA: 278] [Impact Index Per Article: 25.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/03/2022]
Abstract
The Mars Science Laboratory rover Curiosity scooped samples of soil from the Rocknest aeolian bedform in Gale crater. Analysis of the soil with the Chemistry and Mineralogy (CheMin) x-ray diffraction (XRD) instrument revealed plagioclase (~An57), forsteritic olivine (~Fo62), augite, and pigeonite, with minor K-feldspar, magnetite, quartz, anhydrite, hematite, and ilmenite. The minor phases are present at, or near, detection limits. The soil also contains 27 ± 14 weight percent x-ray amorphous material, likely containing multiple Fe(3+)- and volatile-bearing phases, including possibly a substance resembling hisingerite. The crystalline component is similar to the normative mineralogy of certain basaltic rocks from Gusev crater on Mars and of martian basaltic meteorites. The amorphous component is similar to that found on Earth in places such as soils on the Mauna Kea volcano, Hawaii.
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Affiliation(s)
- D L Bish
- Department of Geological Sciences, Indiana University, Bloomington, IN 47405, USA.
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15
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Blake DF, Morris RV, Kocurek G, Morrison SM, Downs RT, Bish D, Ming DW, Edgett KS, Rubin D, Goetz W, Madsen MB, Sullivan R, Gellert R, Campbell I, Treiman AH, McLennan SM, Yen AS, Grotzinger J, Vaniman DT, Chipera SJ, Achilles CN, Rampe EB, Sumner D, Meslin PY, Maurice S, Forni O, Gasnault O, Fisk M, Schmidt M, Mahaffy P, Leshin LA, Glavin D, Steele A, Freissinet C, Navarro-González R, Yingst RA, Kah LC, Bridges N, Lewis KW, Bristow TF, Farmer JD, Crisp JA, Stolper EM, Des Marais DJ, Sarrazin P. Curiosity at Gale crater, Mars: characterization and analysis of the Rocknest sand shadow. Science 2013; 341:1239505. [PMID: 24072928 DOI: 10.1126/science.1239505] [Citation(s) in RCA: 231] [Impact Index Per Article: 21.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/03/2022]
Abstract
The Rocknest aeolian deposit is similar to aeolian features analyzed by the Mars Exploration Rovers (MERs) Spirit and Opportunity. The fraction of sand <150 micrometers in size contains ~55% crystalline material consistent with a basaltic heritage and ~45% x-ray amorphous material. The amorphous component of Rocknest is iron-rich and silicon-poor and is the host of the volatiles (water, oxygen, sulfur dioxide, carbon dioxide, and chlorine) detected by the Sample Analysis at Mars instrument and of the fine-grained nanophase oxide component first described from basaltic soils analyzed by MERs. The similarity between soils and aeolian materials analyzed at Gusev Crater, Meridiani Planum, and Gale Crater implies locally sourced, globally similar basaltic materials or globally and regionally sourced basaltic components deposited locally at all three locations.
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Affiliation(s)
- D F Blake
- National Aeronautics and Space Administration Ames Research Center, Moffett Field, CA 94035, USA.
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16
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Archer PD, Ming DW, Sutter B. The effects of instrument parameters and sample properties on thermal decomposition: interpreting thermal analysis data from Mars. ACTA ACUST UNITED AC 2013. [DOI: 10.1186/2191-2521-2-2] [Citation(s) in RCA: 22] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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17
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Niles PB, Boynton WV, Hoffman JH, Ming DW, Hamara D. Stable Isotope Measurements of Martian Atmospheric CO
2
at the Phoenix Landing Site. Science 2010; 329:1334-7. [PMID: 20829484 DOI: 10.1126/science.1192863] [Citation(s) in RCA: 12] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- Paul B. Niles
- Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA
| | - William V. Boynton
- Department of Planetary Sciences, University of Arizona, Tucson, AZ 85721, USA
| | - John H. Hoffman
- Physics Department, University of Texas, Dallas, TX 75080, USA
| | - Douglas W. Ming
- Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058, USA
| | - Dave Hamara
- Department of Planetary Sciences, University of Arizona, Tucson, AZ 85721, USA
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18
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Morris RV, Ruff SW, Gellert R, Ming DW, Arvidson RE, Clark BC, Golden DC, Siebach K, Klingelhöfer G, Schröder C, Fleischer I, Yen AS, Squyres SW. Identification of carbonate-rich outcrops on Mars by the Spirit rover. Science 2010; 329:421-4. [PMID: 20522738 DOI: 10.1126/science.1189667] [Citation(s) in RCA: 85] [Impact Index Per Article: 6.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Decades of speculation about a warmer, wetter Mars climate in the planet's first billion years postulate a denser CO2-rich atmosphere than at present. Such an atmosphere should have led to the formation of outcrops rich in carbonate minerals, for which evidence has been sparse. Using the Mars Exploration Rover Spirit, we have now identified outcrops rich in magnesium-iron carbonate (16 to 34 weight percent) in the Columbia Hills of Gusev crater. Its composition approximates the average composition of the carbonate globules in martian meteorite ALH 84001. The Gusev carbonate probably precipitated from carbonate-bearing solutions under hydrothermal conditions at near-neutral pH in association with volcanic activity during the Noachian era.
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Seelos KD, Arvidson RE, Jolliff BL, Chemtob SM, Morris RV, Ming DW, Swayze GA. Silica in a Mars analog environment: Ka'u Desert, Kilauea Volcano, Hawaii. ACTA ACUST UNITED AC 2010. [DOI: 10.1029/2009je003347] [Citation(s) in RCA: 28] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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20
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Kounaves SP, Stroble ST, Anderson RM, Moore Q, Catling DC, Douglas S, McKay CP, Ming DW, Smith PH, Tamppari LK, Zent AP. Discovery of natural perchlorate in the Antarctic Dry Valleys and its global implications. Environ Sci Technol 2010; 44:2360-2364. [PMID: 20155929 DOI: 10.1021/es9033606] [Citation(s) in RCA: 81] [Impact Index Per Article: 5.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/28/2023]
Abstract
In the past few years, it has become increasingly apparent that perchlorate (ClO(4)(-)) is present on all continents, except the polar regions where it had not yet been assessed, and that it may have a significant natural source. Here, we report on the discovery of perchlorate in soil and ice from several Antarctic Dry Valleys (ADVs) where concentrations reach up to 1100 microg/kg. In the driest ADV, perchlorate correlates with atmospherically deposited nitrate. Far from anthropogenic activity, ADV perchlorate provides unambiguous evidence that natural perchlorate is ubiquitous on Earth. The discovery has significant implications for the origin of perchlorate, its global biogeochemical interactions, and possible interactions with the polar ice sheets. The results support the hypotheses that perchlorate is produced globally and continuously in the Earth's atmosphere, that it typically accumulates in hyperarid areas, and that it does not build up in oceans or other wet environments most likely because of microbial reduction on a global scale.
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Affiliation(s)
- Samuel P Kounaves
- Department of Chemistry, Tufts University, Medford, Massachusetts 02155, USA.
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Mellon MT, Arvidson RE, Sizemore HG, Searls ML, Blaney DL, Cull S, Hecht MH, Heet TL, Keller HU, Lemmon MT, Markiewicz WJ, Ming DW, Morris RV, Pike WT, Zent AP. Ground ice at the Phoenix Landing Site: Stability state and origin. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2009je003417] [Citation(s) in RCA: 140] [Impact Index Per Article: 9.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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22
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Boynton WV, Ming DW, Kounaves SP, Young SMM, Arvidson RE, Hecht MH, Hoffman J, Niles PB, Hamara DK, Quinn RC, Smith PH, Sutter B, Catling DC, Morris RV. Evidence for calcium carbonate at the Mars Phoenix landing site. Science 2009; 325:61-4. [PMID: 19574384 DOI: 10.1126/science.1172768] [Citation(s) in RCA: 75] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Carbonates are generally products of aqueous processes and may hold important clues about the history of liquid water on the surface of Mars. Calcium carbonate (approximately 3 to 5 weight percent) has been identified in the soils around the Phoenix landing site by scanning calorimetry showing an endothermic transition beginning around 725 degrees C accompanied by evolution of carbon dioxide and by the ability of the soil to buffer pH against acid addition. Based on empirical kinetics, the amount of calcium carbonate is most consistent with formation in the past by the interaction of atmospheric carbon dioxide with liquid water films on particle surfaces.
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Affiliation(s)
- W V Boynton
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA.
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23
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Smith PH, Tamppari LK, Arvidson RE, Bass D, Blaney D, Boynton WV, Carswell A, Catling DC, Clark BC, Duck T, Dejong E, Fisher D, Goetz W, Gunnlaugsson HP, Hecht MH, Hipkin V, Hoffman J, Hviid SF, Keller HU, Kounaves SP, Lange CF, Lemmon MT, Madsen MB, Markiewicz WJ, Marshall J, McKay CP, Mellon MT, Ming DW, Morris RV, Pike WT, Renno N, Staufer U, Stoker C, Taylor P, Whiteway JA, Zent AP. H2O at the Phoenix landing site. Science 2009; 325:58-61. [PMID: 19574383 DOI: 10.1126/science.1172339] [Citation(s) in RCA: 100] [Impact Index Per Article: 6.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Phoenix mission investigated patterned ground and weather in the northern arctic region of Mars for 5 months starting 25 May 2008 (solar longitude between 76.5 degrees and 148 degrees ). A shallow ice table was uncovered by the robotic arm in the center and edge of a nearby polygon at depths of 5 to 18 centimeters. In late summer, snowfall and frost blanketed the surface at night; H(2)O ice and vapor constantly interacted with the soil. The soil was alkaline (pH = 7.7) and contained CaCO(3), aqueous minerals, and salts up to several weight percent in the indurated surface soil. Their formation likely required the presence of water.
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Affiliation(s)
- P H Smith
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA.
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Kounaves SP, Hecht MH, West SJ, Morookian JM, Young SMM, Quinn R, Grunthaner P, Wen X, Weilert M, Cable CA, Fisher A, Gospodinova K, Kapit J, Stroble S, Hsu PC, Clark BC, Ming DW, Smith PH. The MECA Wet Chemistry Laboratory on the 2007 Phoenix Mars Scout Lander. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003084] [Citation(s) in RCA: 42] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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25
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Schmidt ME, Ruff SW, McCoy TJ, Farrand WH, Johnson JR, Gellert R, Ming DW, Morris RV, Cabrol N, Lewis KW, Schroeder C. Hydrothermal origin of halogens at Home Plate, Gusev Crater. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2007je003027] [Citation(s) in RCA: 62] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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26
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Goetz W, Leer K, Gunnlaugsson HP, Bartlett P, Basso B, Bell J, Bertelsen P, Binau CS, Chu PC, Gorevan S, Hansen MF, Hviid SF, Kinch KM, Klingelhöfer G, Kusack A, Madsen MB, Ming DW, Morris RV, Mumm E, Myrick T, Olsen M, Squyres SW, Wilson J, Yen A. Search for magnetic minerals in Martian rocks: Overview of the Rock Abrasion Tool (RAT) magnet investigation on Spirit and Opportunity. ACTA ACUST UNITED AC 2008. [DOI: 10.1029/2006je002819] [Citation(s) in RCA: 9] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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27
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Lichtenberg KA, Arvidson RE, Poulet F, Morris RV, Knudson A, Bell JF, Bellucci G, Bibring JP, Farrand WH, Johnson JR, Ming DW, Pinet PC, Rogers AD, Squyres SW. Coordinated analyses of orbital and Spirit Rover data to characterize surface materials on the cratered plains of Gusev Crater, Mars. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002850] [Citation(s) in RCA: 25] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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28
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Guinness EA, Arvidson RE, Jolliff BL, Seelos KD, Seelos FP, Ming DW, Morris RV, Graff TG. Hyperspectral reflectance mapping of cinder cones at the summit of Mauna Kea and implications for equivalent observations on Mars. ACTA ACUST UNITED AC 2007. [DOI: 10.1029/2006je002822] [Citation(s) in RCA: 15] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- Edward A. Guinness
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - Raymond E. Arvidson
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - Bradley L. Jolliff
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - Kim D. Seelos
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - Frank P. Seelos
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | | | | | - Trevor G. Graff
- School of Earth and Space Exploration; Arizona State University; Tempe Arizona USA
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29
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Squyres SW, Aharonson O, Clark BC, Cohen BA, Crumpler L, de Souza PA, Farrand WH, Gellert R, Grant J, Grotzinger JP, Haldemann AFC, Johnson JR, Klingelhöfer G, Lewis KW, Li R, McCoy T, McEwen AS, McSween HY, Ming DW, Moore JM, Morris RV, Parker TJ, Rice JW, Ruff S, Schmidt M, Schröder C, Soderblom LA, Yen A. Pyroclastic activity at Home Plate in Gusev Crater, Mars. Science 2007; 316:738-42. [PMID: 17478719 DOI: 10.1126/science.1139045] [Citation(s) in RCA: 150] [Impact Index Per Article: 8.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Home Plate is a layered plateau in Gusev crater on Mars. It is composed of clastic rocks of moderately altered alkali basalt composition, enriched in some highly volatile elements. A coarsegrained lower unit lies under a finer-grained upper unit. Textural observations indicate that the lower strata were emplaced in an explosive event, and geochemical considerations favor an explosive volcanic origin over an impact origin. The lower unit likely represents accumulation of pyroclastic materials, whereas the upper unit may represent eolian reworking of the same pyroclastic materials.
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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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30
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Squyres SW, Arvidson RE, Blaney DL, Clark BC, Crumpler L, Farrand WH, Gorevan S, Herkenhoff KE, Hurowitz J, Kusack A, McSween HY, Ming DW, Morris RV, Ruff SW, Wang A, Yen A. Rocks of the Columbia Hills. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002562] [Citation(s) in RCA: 129] [Impact Index Per Article: 7.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
Affiliation(s)
| | - Raymond E. Arvidson
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - Diana L. Blaney
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
| | | | - Larry Crumpler
- New Mexico Museum of Natural History and Science; Albuquerque New Mexico USA
| | | | | | | | - Joel Hurowitz
- Department of Geosciences; State University of New York; Stony Brook New York USA
| | | | - Harry Y. McSween
- Department of Earth and Planetary Sciences; University of Tennessee; Knoxville Tennessee USA
| | | | | | - Steven W. Ruff
- Department of Geological Sciences; Arizona State University; Tempe Arizona USA
| | - Alian Wang
- Department of Earth and Planetary Sciences; Washington University; St. Louis Missouri USA
| | - Albert Yen
- Jet Propulsion Laboratory; California Institute of Technology; Pasadena California USA
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31
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Yen AS, Gellert R, Schröder C, Morris RV, Bell JF, Knudson AT, Clark BC, Ming DW, Crisp JA, Arvidson RE, Blaney D, Brückner J, Christensen PR, DesMarais DJ, de Souza PA, Economou TE, Ghosh A, Hahn BC, Herkenhoff KE, Haskin LA, Hurowitz JA, Joliff BL, Johnson JR, Klingelhöfer G, Madsen MB, McLennan SM, McSween HY, Richter L, Rieder R, Rodionov D, Soderblom L, Squyres SW, Tosca NJ, Wang A, Wyatt M, Zipfel J. An integrated view of the chemistry and mineralogy of martian soils. Nature 2005; 436:49-54. [PMID: 16001059 DOI: 10.1038/nature03637] [Citation(s) in RCA: 300] [Impact Index Per Article: 15.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/20/2004] [Accepted: 04/08/2005] [Indexed: 11/09/2022]
Abstract
The mineralogical and elemental compositions of the martian soil are indicators of chemical and physical weathering processes. Using data from the Mars Exploration Rovers, we show that bright dust deposits on opposite sides of the planet are part of a global unit and not dominated by the composition of local rocks. Dark soil deposits at both sites have similar basaltic mineralogies, and could reflect either a global component or the general similarity in the compositions of the rocks from which they were derived. Increased levels of bromine are consistent with mobilization of soluble salts by thin films of liquid water, but the presence of olivine in analysed soil samples indicates that the extent of aqueous alteration of soils has been limited. Nickel abundances are enhanced at the immediate surface and indicate that the upper few millimetres of soil could contain up to one per cent meteoritic material.
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Affiliation(s)
- Albert S Yen
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA.
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32
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Haskin LA, Wang A, Jolliff BL, McSween HY, Clark BC, Des Marais DJ, McLennan SM, Tosca NJ, Hurowitz JA, Farmer JD, Yen A, Squyres SW, Arvidson RE, Klingelhöfer G, Schröder C, de Souza PA, Ming DW, Gellert R, Zipfel J, Brückner J, Bell JF, Herkenhoff K, Christensen PR, Ruff S, Blaney D, Gorevan S, Cabrol NA, Crumpler L, Grant J, Soderblom L. Water alteration of rocks and soils on Mars at the Spirit rover site in Gusev crater. Nature 2005; 436:66-9. [PMID: 16001063 DOI: 10.1038/nature03640] [Citation(s) in RCA: 206] [Impact Index Per Article: 10.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/18/2004] [Accepted: 04/08/2005] [Indexed: 11/08/2022]
Abstract
Gusev crater was selected as the landing site for the Spirit rover because of the possibility that it once held a lake. Thus one of the rover's tasks was to search for evidence of lake sediments. However, the plains at the landing site were found to be covered by a regolith composed of olivine-rich basaltic rock and windblown 'global' dust. The analyses of three rock interiors exposed by the rock abrasion tool showed that they are similar to one another, consistent with having originated from a common lava flow. Here we report the investigation of soils, rock coatings and rock interiors by the Spirit rover from sol (martian day) 1 to sol 156, from its landing site to the base of the Columbia hills. The physical and chemical characteristics of the materials analysed provide evidence for limited but unequivocal interaction between water and the volcanic rocks of the Gusev plains. This evidence includes the softness of rock interiors that contain anomalously high concentrations of sulphur, chlorine and bromine relative to terrestrial basalts and martian meteorites; sulphur, chlorine and ferric iron enrichments in multilayer coatings on the light-toned rock Mazatzal; high bromine concentration in filled vugs and veins within the plains basalts; positive correlations between magnesium, sulphur and other salt components in trench soils; and decoupling of sulphur, chlorine and bromine concentrations in trench soils compared to Gusev surface soils, indicating chemical mobility and separation.
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Affiliation(s)
- Larry A Haskin
- Department of Earth and Planetary Sciences, Washington University in Saint Louis, Missouri 63130, USA
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33
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Goetz W, Bertelsen P, Binau CS, Gunnlaugsson HP, Hviid SF, Kinch KM, Madsen DE, Madsen MB, Olsen M, Gellert R, Klingelhöfer G, Ming DW, Morris RV, Rieder R, Rodionov DS, de Souza PA, Schröder C, Squyres SW, Wdowiak T, Yen A. Indication of drier periods on Mars from the chemistry and mineralogy of atmospheric dust. Nature 2005; 436:62-5. [PMID: 16001062 DOI: 10.1038/nature03807] [Citation(s) in RCA: 110] [Impact Index Per Article: 5.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/23/2004] [Accepted: 04/29/2005] [Indexed: 11/08/2022]
Abstract
The ubiquitous atmospheric dust on Mars is well mixed by periodic global dust storms, and such dust carries information about the environment in which it once formed and hence about the history of water on Mars. The Mars Exploration Rovers have permanent magnets to collect atmospheric dust for investigation by instruments on the rovers. Here we report results from Mössbauer spectroscopy and X-ray fluorescence of dust particles captured from the martian atmosphere by the magnets. The dust on the magnets contains magnetite and olivine; this indicates a basaltic origin of the dust and shows that magnetite, not maghemite, is the mineral mainly responsible for the magnetic properties of the dust. Furthermore, the dust on the magnets contains some ferric oxides, probably including nanocrystalline phases, so some alteration or oxidation of the basaltic dust seems to have occurred. The presence of olivine indicates that liquid water did not play a dominant role in the processes that formed the atmospheric dust.
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Affiliation(s)
- Walter Goetz
- Max-Planck-Institut für Sonnensystemforschung, Katlenburg-Lindau, D-37191, Germany
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34
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Abstract
Micronutrient-substituted synthetic hydroxyapatite (SHA) is being evaluated by the National Aeronautics and Space Administration's (NASA) Advanced Life Support (ALS) Program for crop production on long-duration human missions to the International Space Station or for future Lunar or Martian outposts. The stirred-flow technique was utilized to characterize Ca, P, Fe, Mn, and Cu release characteristics from Fe-, Mn-, and Cu-containing SHA in deionized (DI) water, citric acid, and diethylene-triamine-pentaacetic acid (DTPA). Initially, Ca and P release rates decreased rapidly with time and were controlled by a non-SHA calcium phosphate phase(s) with low Ca/P solution molar ratios (0.91-1.51) relative to solid SHA ratios (1.56-1.64). At later times, Ca/P solution molar ratios (1.47-1.79) were near solid SHA ratios and release rates decreased slowly indicating that SHA controlled Ca and P release. Substituted SHA materials had faster dissolution rates relative to unsubstituted SHA. The initial metal release rate order was Mn >> Cu > Fe which followed metal-oxide/phosphate solubility suggesting that poorly crystalline metal-oxides/phosphates were dominating metal release. Similar metal release rates for all substituted SHA (approximately 0.01 cmol kg-1 min-1) at the end of the DTPA experiment indicated that SHA dissolution was supplying the metals into solution and that poorly crystalline metal-oxide/phosphates were not controlling metal release. Results indicate that non-SHA Ca-phosphate phases and poorly crystalline metal-oxide/phosphates will contribute Ca, P, and metals. After these phases have dissolved, substituted SHA will be the source of Ca, P, and metals for plants.
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Affiliation(s)
- B Sutter
- Dep. of Soil and Crop Sciences, Texas A&M Univ., College Station, TX 77843, USA.
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35
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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] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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36
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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] [What about the content of this article? (0)] [Affiliation(s)] [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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37
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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] [What about the content of this article? (0)] [Affiliation(s)] [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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38
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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] [What about the content of this article? (0)] [Affiliation(s)] [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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39
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Rieder R, Gellert R, Anderson RC, Brückner J, Clark BC, Dreibus G, Economou T, Klingelhöfer G, Lugmair GW, Ming DW, Squyres SW, d'Uston C, Wänke H, Yen A, Zipfel J. Chemistry of rocks and soils at Meridiani Planum from the Alpha Particle X-ray Spectrometer. Science 2004; 306:1746-9. [PMID: 15576611 DOI: 10.1126/science.1104358] [Citation(s) in RCA: 314] [Impact Index Per Article: 15.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Alpha Particle X-ray Spectrometer on the Opportunity rover determined major and minor elements of soils and rocks in Meridiani Planum. Chemical compositions differentiate between basaltic rocks, evaporite-rich rocks, basaltic soils, and hematite-rich soils. Although soils are compositionally similar to those at previous landing sites, differences in iron and some minor element concentrations signify the addition of local components. Rocky outcrops are rich in sulfur and variably enriched in bromine relative to chlorine. The interaction with water in the past is indicated by the chemical features in rocks and soils at this site.
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Affiliation(s)
- R Rieder
- Max-Planck-Institut für Chemie, J. J. Becher-Weg 27, D-55128 Mainz, Germany.
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40
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Herkenhoff KE, Squyres SW, Arvidson R, Bass DS, Bell JF, Bertelsen P, Ehlmann BL, Farrand W, Gaddis L, Greeley R, Grotzinger J, Hayes AG, Hviid SF, Johnson JR, Jolliff B, Kinch KM, Knoll AH, Madsen MB, Maki JN, McLennan SM, McSween HY, Ming DW, Rice JW, Richter L, Sims M, Smith PH, Soderblom LA, Spanovich N, Sullivan R, Thompson S, Wdowiak T, Weitz C, Whelley P. Evidence from Opportunity's Microscopic Imager for water on Meridiani Planum. Science 2004; 306:1727-30. [PMID: 15576607 DOI: 10.1126/science.1105286] [Citation(s) in RCA: 118] [Impact Index Per Article: 5.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Microscopic Imager on the Opportunity rover analyzed textures of soils and rocks at Meridiani Planum at a scale of 31 micrometers per pixel. The uppermost millimeter of some soils is weakly cemented, whereas other soils show little evidence of cohesion. Rock outcrops are laminated on a millimeter scale; image mosaics of cross-stratification suggest that some sediments were deposited by flowing water. Vugs in some outcrop faces are probably molds formed by dissolution of relatively soluble minerals during diagenesis. Microscopic images support the hypothesis that hematite-rich spherules observed in outcrops and soils also formed diagenetically as concretions.
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Affiliation(s)
- K E Herkenhoff
- U.S. Geological Survey Astrogeology Team, Flagstaff, AZ 86001, USA.
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41
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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] [What about the content of this article? (0)] [Affiliation(s)] [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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42
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Klingelhöfer G, Morris RV, Bernhardt B, Schröder C, Rodionov DS, de Souza PA, Yen A, Gellert R, Evlanov EN, Zubkov B, Foh J, Bonnes U, Kankeleit E, Gütlich P, Ming DW, Renz F, Wdowiak T, Squyres SW, Arvidson RE. Jarosite and Hematite at Meridiani Planum from Opportunity's Mössbauer Spectrometer. Science 2004; 306:1740-5. [PMID: 15576610 DOI: 10.1126/science.1104653] [Citation(s) in RCA: 193] [Impact Index Per Article: 9.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Mossbauer spectra measured by the Opportunity rover revealed four mineralogical components in Meridiani Planum at Eagle crater: jarosite- and hematite-rich outcrop, hematite-rich soil, olivine-bearing basaltic soil, and a pyroxene-bearing basaltic rock (Bounce rock). Spherules, interpreted to be concretions, are hematite-rich and dispersed throughout the outcrop. Hematitic soils both within and outside Eagle crater are dominated by spherules and their fragments. Olivine-bearing basaltic soil is present throughout the region. Bounce rock is probably an impact erratic. Because jarosite is a hydroxide sulfate mineral, its presence at Meridiani Planum is mineralogical evidence for aqueous processes on Mars, probably under acid-sulfate conditions.
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Affiliation(s)
- G Klingelhöfer
- Institut für Anorganische und Analytische Chemie, Johannes Gutenberg-Universität, Staudinger Weg 9, D-55128 Mainz, Germany.
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43
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Squyres SW, Arvidson RE, Bell JF, Brückner J, Cabrol NA, Calvin W, Carr MH, Christensen PR, Clark BC, Crumpler L, Des Marais DJ, 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 A, 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 Spirit Rover's Athena science investigation at Gusev Crater, Mars. Science 2004; 305:794-9. [PMID: 15297657 DOI: 10.1126/science.1100194] [Citation(s) in RCA: 25] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Mars Exploration Rover Spirit and its Athena science payload have been used to investigate a landing site in Gusev crater. Gusev is hypothesized to be the site of a former lake, but no clear evidence for lacustrine sedimentation has been found to date. Instead, the dominant lithology is basalt, and the dominant geologic processes are impact events and eolian transport. Many rocks exhibit coatings and other characteristics that may be evidence for minor aqueous alteration. Any lacustrine sediments that may exist at this location within Gusev apparently have been buried by lavas that have undergone subsequent impact disruption.
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Affiliation(s)
- S W Squyres
- Department of Astronomy, Cornell University, Ithaca, NY 14853, USA.
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44
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Arvidson RE, Anderson RC, Bartlett P, Bell JF, Blaney D, Christensen PR, Chu P, Crumpler L, Davis K, Ehlmann BL, Fergason R, Golombek MP, Gorevan S, Grant JA, Greeley R, Guinness EA, Haldemann AFC, Herkenhoff K, Johnson J, Landis G, Li R, Lindemann R, McSween H, Ming DW, Myrick T, Richter L, Seelos FP, Squyres SW, Sullivan RJ, Wang A, Wilson J. Localization and physical properties experiments conducted by Spirit at Gusev Crater. Science 2004; 305:821-4. [PMID: 15297662 DOI: 10.1126/science.1099922] [Citation(s) in RCA: 144] [Impact Index Per Article: 7.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The precise location and relative elevation of Spirit during its traverses from the Columbia Memorial station to Bonneville crater were determined with bundle-adjusted retrievals from rover wheel turns, suspension and tilt angles, and overlapping images. Physical properties experiments show a decrease of 0.2% per Mars solar day in solar cell output resulting from deposition of airborne dust, cohesive soil-like deposits in plains and hollows, bright and dark rock coatings, and relatively weak volcanic rocks of basaltic composition. Volcanic, impact, aeolian, and water-related processes produced the encountered landforms and materials.
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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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45
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Bell JF, Squyres SW, Arvidson RE, Arneson HM, Bass D, Blaney D, Cabrol N, Calvin W, Farmer J, Farrand WH, Goetz W, Golombek M, Grant JA, Greeley R, 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, Moersch JE, Morris RV, Dobrea EZN, Parker TJ, Proton J, Rice JW, Seelos F, Soderblom J, Soderblom LA, Sohl-Dickstein JN, Sullivan RJ, Wolff MJ, Wang A. Pancam multispectral imaging results from the Spirit Rover at Gusev Crater. Science 2004; 305:800-6. [PMID: 15297658 DOI: 10.1126/science.1100175] [Citation(s) in RCA: 130] [Impact Index Per Article: 6.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Panoramic Camera images at Gusev crater reveal a rock-strewn surface interspersed with high- to moderate-albedo fine-grained deposits occurring in part as drifts or in small circular swales or hollows. Optically thick coatings of fine-grained ferric iron-rich dust dominate most bright soil and rock surfaces. Spectra of some darker rock surfaces and rock regions exposed by brushing or grinding show near-infrared spectral signatures consistent with the presence of mafic silicates such as pyroxene or olivine. Atmospheric observations show a steady decline in dust opacity during the mission, and astronomical observations captured solar transits by the martian moons, Phobos and Deimos, as well as a view of Earth from the martian surface.
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Affiliation(s)
- J F Bell
- Cornell University, Ithaca, NY 14853-6801, USA.
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Morris RV, Klingelhöfer G, Bernhardt B, Schröder C, Rodionov DS, De Souza PA, Yen A, Gellert R, Evlanov EN, Foh J, Kankeleit E, Gütlich P, Ming DW, Renz F, Wdowiak T, Squyres SW, Arvidson RE. Mineralogy at Gusev Crater from the Mossbauer Spectrometer on the Spirit Rover. Science 2004; 305:833-6. [PMID: 15297666 DOI: 10.1126/science.1100020] [Citation(s) in RCA: 241] [Impact Index Per Article: 12.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Mössbauer spectra measured on Mars by the Spirit rover during the primary mission are characterized by two ferrous iron doublets (olivine and probably pyroxene) and a ferric iron doublet (tentatively associated to nanophase ferric iron oxide). Two sextets resulting from nonstoichiometric magnetite are also present, except for a coating on the rock Mazatzal, where a hematite-like sextet is present. Greater proportions of ferric-bearing phases are associated with undisturbed soils and rock surfaces as compared to fresh rock surfaces exposed by grinding. The ubiquitous presence of olivine in soil suggests that physical rather than chemical weathering processes currently dominate at Gusev crater.
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Affiliation(s)
- R V Morris
- NASA Johnson Space Center, Houston, TX, USA.
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Grant JA, Arvidson R, Bell JF, Cabrol NA, Carr MH, Christensen P, Crumpler L, Des Marais DJ, Ehlmann BL, Farmer J, Golombek M, Grant FD, Greeley R, Herkenhoff K, Li R, McSween HY, Ming DW, Moersch J, Rice JW, Ruff S, Richter L, Squyres S, Sullivan R, Weitz C. Surficial Deposits at Gusev Crater Along Spirit Rover Traverses. Science 2004; 305:807-10. [PMID: 15297659 DOI: 10.1126/science.1099849] [Citation(s) in RCA: 71] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The Mars Exploration Rover Spirit has traversed a fairly flat, rock-strewn terrain whose surface is shaped primarily by impact events, although some of the landscape has been altered by eolian processes. Impacts ejected basaltic rocks that probably were part of locally formed lava flows from at least 10 meters depth. Some rocks have been textured and/or partially buried by windblown sediments less than 2 millimeters in diameter that concentrate within shallow, partially filled, circular impact depressions referred to as hollows. The terrain traversed during the 90-sol (martian solar day) nominal mission shows no evidence for an ancient lake in Gusev crater.
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Affiliation(s)
- J A Grant
- Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, DC 20560, USA.
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48
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Gellert R, Rieder R, Anderson RC, Brückner J, Clark BC, Dreibus G, Economou T, Klingelhöfer G, Lugmair GW, Ming DW, Squyres SW, D'Uston C, Wänke H, Yen A, Zipfel J. Chemistry of Rocks and Soils in Gusev Crater from the Alpha Particle X-ray Spectrometer. Science 2004; 305:829-32. [PMID: 15297665 DOI: 10.1126/science.1099913] [Citation(s) in RCA: 254] [Impact Index Per Article: 12.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The alpha particle x-ray spectrometer on the Spirit rover determined major and minor elements of soils and rocks in Gusev crater in order to unravel the crustal evolution of planet Mars. The composition of soils is similar to those at previous landing sites, as a result of global mixing and distribution by dust storms. Rocks (fresh surfaces exposed by the rock abrasion tool) resemble volcanic rocks of primitive basaltic composition with low intrinsic potassium contents. High abundance of bromine (up to 170 parts per million) in rocks may indicate the alteration of surfaces formed during a past period of aqueous activity in Gusev crater.
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Affiliation(s)
- R Gellert
- Max-Planck-Institut für Chemie, J. J. Becher-Weg 27, D-55128 Mainz, Germany.
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49
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Bell JF, Squyres SW, Arvidson RE, Arneson HM, Bass D, Blaney D, Cabrol N, Calvin W, Farmer J, Farrand WH, Goetz W, Golombek M, Grant JA, Greeley R, 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, Moersch JE, Morris RV, Dobrea EZN, Parker TJ, Proton J, Rice JW, Seelos F, Soderblom J, Soderblom LA, Sohl-Dickstein JN, Sullivan RJ, Wolff MJ, Wang A. Pancam multispectral imaging results from the Spirit Rover at Gusev Crater. Science 2004. [PMID: 15297658 DOI: 10.1126/science.1100175,2004] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Panoramic Camera images at Gusev crater reveal a rock-strewn surface interspersed with high- to moderate-albedo fine-grained deposits occurring in part as drifts or in small circular swales or hollows. Optically thick coatings of fine-grained ferric iron-rich dust dominate most bright soil and rock surfaces. Spectra of some darker rock surfaces and rock regions exposed by brushing or grinding show near-infrared spectral signatures consistent with the presence of mafic silicates such as pyroxene or olivine. Atmospheric observations show a steady decline in dust opacity during the mission, and astronomical observations captured solar transits by the martian moons, Phobos and Deimos, as well as a view of Earth from the martian surface.
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Affiliation(s)
- J F Bell
- Cornell University, Ithaca, NY 14853-6801, USA.
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Sutter B, Ming DW, Clearfield A, Hossner LR. Mineralogical and chemical characterization of iron-, manganese-, and copper-containing synthetic hydroxyapatites. Soil Sci Soc Am J 2003; 67:1935-1942. [PMID: 14740607 DOI: 10.2136/sssaj2003.1935] [Citation(s) in RCA: 18] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/24/2023]
Abstract
The National Aeronautics and Space Administration's (NASA) Advanced Life Support (ALS) Program is evaluating the use of Fe-, Mn-, and Cu-containing synthetic hydroxyapatite (SHA) as a slow release fertilizer for crops that might be grown on the International Space Station or at Lunar and Martian outposts. Separate Fe-, Mn-, and Cu-containing SHA materials along with a transition-metal free SHA (pure-SHA) were synthesized using a precipitation method. Chemical and mineralogical analyses determined if and how Fe, Mn, and Cu were incorporated into the SHA structure. X-ray diffraction (XRD), Rietveld refinement, and transmission electron microscopy (TEM) confirmed that SHA materials with the apatite structure were produced. Chemical analyses indicated that the metal containing SHA materials were deficient in Ca relative to pure-SHA. The shift in the infrared PO4-mu 3 vibrations, smaller unit cell parameters, smaller particle size, and greater structural strain for Fe-, Mn-, and Cu-containing SHA compared with pure-SHA suggested that Fe, Mn, and Cu were incorporated into SHA structure. Rietveld analyses revealed that Fe, Mn, and Cu substituted into the Ca2 site of SHA. An Fe-rich phase was detected by TEM analyses and backscattered electron microscopy in the Fe-containing SHA material with the greatest Fe content. The substitution of metals into SHA suggests that metal-SHA materials are potential slow-release sources of micronutrients for plant uptake in addition to Ca and P.
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Affiliation(s)
- B Sutter
- Dep. of Soil and Crop Sciences, Texas A&M Univ., College Station, TX 77843, USA.
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