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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. JOURNAL OF GEOPHYSICAL RESEARCH. 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] [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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2
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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 P, 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. JOURNAL OF GEOPHYSICAL RESEARCH. PLANETS 2017; 122:2510-2543. [PMID: 29497589 PMCID: PMC5815393 DOI: 10.1002/2017je005267] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/16/2017] [Revised: 05/18/2017] [Accepted: 05/19/2017] [Indexed: 05/31/2023]
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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3
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Susko D, Karunatillake S, Kodikara G, Skok JR, Wray J, Heldmann J, Cousin A, Judice T. A record of igneous evolution in Elysium, a major martian volcanic province. Sci Rep 2017; 7:43177. [PMID: 28233797 PMCID: PMC5324095 DOI: 10.1038/srep43177] [Citation(s) in RCA: 11] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/25/2016] [Accepted: 01/22/2017] [Indexed: 11/30/2022] Open
Abstract
A major knowledge gap exists on how eruptive compositions of a single martian volcanic province change over time. Here we seek to fill that gap by assessing the compositional evolution of Elysium, a major martian volcanic province. A unique geochemical signature overlaps with the southeastern flows of this volcano, which provides the context for this study of variability of martian magmatism. The southeastern lava fields of Elysium Planitia show distinct chemistry in the shallow subsurface (down to several decimeters) relative to the rest of the martian mid-to-low latitudes (average crust) and flows in northwest Elysium. By impact crater counting chronology we estimated the age of the southeastern province to be 0.85 ± 0.08 Ga younger than the northwestern fields. This study of the geochemical and temporal differences between the NW and SE Elysium lava fields is the first to demonstrate compositional variation within a single volcanic province on Mars. We interpret the geochemical and temporal differences between the SE and NW lava fields to be consistent with primary magmatic processes, such as mantle heterogeneity or change in depth of melt formation within the martian mantle due to crustal loading.
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Affiliation(s)
- David Susko
- Department of Geology and Geophysics, Louisiana State University, Louisiana, USA
| | - Suniti Karunatillake
- Department of Geology and Geophysics, Louisiana State University, Louisiana, USA
| | - Gayantha Kodikara
- Department of Oceanography and Marine Geology, Faculty of Fisheries and Marine Sciences &Technology, University of Rahuna, Matara, Sri Lanka
| | | | - James Wray
- School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, GA, USA
| | | | - Agnes Cousin
- Institut de Recherche en Astrophysique et Planétologie, Toulouse, France
| | - Taylor Judice
- Department of Geology and Geophysics, Louisiana State University, Louisiana, USA
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Lasne J, Noblet A, Szopa C, Navarro-González R, Cabane M, Poch O, Stalport F, François P, Atreya SK, Coll P. Oxidants at the Surface of Mars: A Review in Light of Recent Exploration Results. ASTROBIOLOGY 2016; 16:977-996. [PMID: 27925795 DOI: 10.1089/ast.2016.1502] [Citation(s) in RCA: 15] [Impact Index Per Article: 1.9] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/06/2023]
Abstract
In 1976, the Viking landers carried out the most comprehensive search for organics and microbial life in the martian regolith. Their results indicate that Mars' surface is lifeless and, surprisingly, depleted in organics at part-per-billion levels. Several biology experiments on the Viking landers gave controversial results that have since been explained by the presence of oxidizing agents on the surface of Mars. These oxidants may degrade abiotic or biological organics, resulting in their nondetection in the regolith. As several exploration missions currently focus on the detection of organics on Mars (or will do so in the near future), knowledge of the oxidative state of the surface is fundamental. It will allow for determination of the capability of organics to survive on a geological timescale, the most favorable places to seek them, and the best methods to process the samples collected at the surface. With this aim, we review the main oxidants assumed to be present on Mars, their possible formation pathways, and those laboratory studies in which their reactivity with organics under Mars-like conditions has been evaluated. Among the oxidants assumed to be present on Mars, only four have been detected so far: perchlorate ions (ClO4-) in salts, hydrogen peroxide (H2O2) in the atmosphere, and clays and metal oxides composing surface minerals. Clays have been suggested as catalysts for the oxidation of organics but are treated as oxidants in the following to keep the structure of this article straightforward. This work provides an insight into the oxidizing potential of the surface of Mars and an estimate of the stability of organic matter in an oxidizing environment. Key Words: Mars surface-Astrobiology-Oxidant-Chemical reactions. Astrobiology 16, 977-996.
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Affiliation(s)
- J Lasne
- 1 LISA, Universités Paris-Est Créteil and Paris Diderot, Institut Pierre Simon Laplace , CNRS UMR 7583, Créteil, France
| | - A Noblet
- 1 LISA, Universités Paris-Est Créteil and Paris Diderot, Institut Pierre Simon Laplace , CNRS UMR 7583, Créteil, France
| | - C Szopa
- 2 LATMOS, UPMC Université Paris 06, Université Versailles St Quentin , CNRS, Guyancourt, France
| | - R Navarro-González
- 3 Laboratorio de Química de Plasmas y Estudios Planetarios, Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México , Ciudad de México, México
| | - M Cabane
- 2 LATMOS, UPMC Université Paris 06, Université Versailles St Quentin , CNRS, Guyancourt, France
| | - O Poch
- 1 LISA, Universités Paris-Est Créteil and Paris Diderot, Institut Pierre Simon Laplace , CNRS UMR 7583, Créteil, France
- 4 NCCR PlanetS, Physikalisches Institut, Universität Bern , Bern, Switzerland
| | - F Stalport
- 1 LISA, Universités Paris-Est Créteil and Paris Diderot, Institut Pierre Simon Laplace , CNRS UMR 7583, Créteil, France
| | - P François
- 1 LISA, Universités Paris-Est Créteil and Paris Diderot, Institut Pierre Simon Laplace , CNRS UMR 7583, Créteil, France
- 5 IC2MP, Equipe Eau Géochimie Santé, Université de Poitiers , CNRS UMR 7285, Poitiers, France
| | - S K Atreya
- 6 Department of Climate and Space Sciences, University of Michigan , Ann Arbor, Michigan, USA
| | - P Coll
- 1 LISA, Universités Paris-Est Créteil and Paris Diderot, Institut Pierre Simon Laplace , CNRS UMR 7583, Créteil, France
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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] [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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Meslin PY, Gasnault O, Forni O, Schröder S, Cousin A, Berger G, Clegg SM, Lasue J, Maurice S, Sautter V, Le Mouélic S, Wiens RC, Fabre C, Goetz W, Bish D, Mangold N, Ehlmann B, Lanza N, Harri AM, Anderson R, Rampe E, McConnochie TH, Pinet P, Blaney D, Léveillé R, Archer D, Barraclough B, Bender S, Blake D, Blank JG, Bridges N, Clark BC, DeFlores L, Delapp D, Dromart G, Dyar MD, Fisk M, Gondet B, Grotzinger J, Herkenhoff K, Johnson J, Lacour JL, Langevin Y, Leshin L, Lewin E, Madsen MB, Melikechi N, Mezzacappa A, Mischna MA, Moores JE, Newsom H, Ollila A, Perez R, Renno N, Sirven JB, Tokar R, de la Torre M, d'Uston L, Vaniman D, Yingst A. Soil diversity and hydration as observed by ChemCam at Gale crater, Mars. Science 2013; 341:1238670. [PMID: 24072924 DOI: 10.1126/science.1238670] [Citation(s) in RCA: 190] [Impact Index Per Article: 17.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
The ChemCam instrument, which provides insight into martian soil chemistry at the submillimeter scale, identified two principal soil types along the Curiosity rover traverse: a fine-grained mafic type and a locally derived, coarse-grained felsic type. The mafic soil component is representative of widespread martian soils and is similar in composition to the martian dust. It possesses a ubiquitous hydrogen signature in ChemCam spectra, corresponding to the hydration of the amorphous phases found in the soil by the CheMin instrument. This hydration likely accounts for an important fraction of the global hydration of the surface seen by previous orbital measurements. ChemCam analyses did not reveal any significant exchange of water vapor between the regolith and the atmosphere. These observations provide constraints on the nature of the amorphous phases and their hydration.
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Affiliation(s)
- P-Y Meslin
- Université de Toulouse, UPS-OMP, IRAP, 31028 Toulouse, France.
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Riedo A, Bieler A, Neuland M, Tulej M, Wurz P. Performance evaluation of a miniature laser ablation time-of-flight mass spectrometer designed for in situ investigations in planetary space research. JOURNAL OF MASS SPECTROMETRY : JMS 2013; 48:1-15. [PMID: 23303743 DOI: 10.1002/jms.3104] [Citation(s) in RCA: 18] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/04/2012] [Revised: 09/02/2012] [Accepted: 09/05/2012] [Indexed: 06/01/2023]
Abstract
Key performance features of a miniature laser ablation time-of-flight mass spectrometer designed for in situ investigations of the chemical composition of planetary surfaces are presented. This mass spectrometer is well suited for elemental and isotopic analysis of raw solid materials with high sensitivity and high spatial resolution. In this study, ultraviolet laser radiation with irradiances suitable for ablation (< 1 GW/cm(2)) is used to achieve stable ion formation and low sample consumption. In comparison to our previous laser ablation studies at infrared wavelengths, several improvements to the experimental setup have been made, which allow accurate control over the experimental conditions and good reproducibility of measurements. Current performance evaluations indicate significant improvements to several instrumental figures of merit. Calibration of the mass scale is performed within a mass accuracy (Δm/m) in the range of 100 ppm, and a typical mass resolution (m/Δm) ~600 is achieved at the lead mass peaks. At lower laser irradiances, the mass resolution is better, about (m/Δm) ~900 for lead, and limited by the laser pulse duration of 3 ns. The effective dynamic range of the instrument was enhanced from about 6 decades determined in previous study up to more than 8 decades at present. Current studies show high sensitivity in detection of both metallic and non-metallic elements. Their abundance down to tens of ppb can be measured together with their isotopic patterns. Due to strict control of the experimental parameters, e.g. laser characteristics, ion-optical parameters and sample position, by computer control, measurements can be performed with high reproducibility.
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Affiliation(s)
- A Riedo
- Space Research and Planetary Sciences, Physics Institute, University of Bern, Sidlerstrasse 5, 3012, Bern, Switzerland.
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Planning for Mars returned sample science: final report of the MSR End-to-End International Science Analysis Group (E2E-iSAG). ASTROBIOLOGY 2012; 12:175-230. [PMID: 22468886 DOI: 10.1089/ast.2011.0805] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/31/2023]
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9
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McGlynn IO, Fedo CM, McSween HY. Soil mineralogy at the Mars Exploration Rover landing sites: An assessment of the competing roles of physical sorting and chemical weathering. ACTA ACUST UNITED AC 2012. [DOI: 10.1029/2011je003861] [Citation(s) in RCA: 39] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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