1
|
Thomas NH, Ehlmann BL, Rapin W, Rivera‐Hernández F, Stein NT, Frydenvang J, Gabriel T, Meslin P, Maurice S, Wiens RC. Hydrogen Variability in the Murray Formation, Gale Crater, Mars. J Geophys Res Planets 2020; 125:e2019JE006289. [PMID: 32999802 PMCID: PMC7507757 DOI: 10.1029/2019je006289] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/22/2019] [Revised: 03/04/2020] [Accepted: 03/09/2020] [Indexed: 05/16/2023]
Abstract
The Mars Science Laboratory (MSL) Curiosity rover is exploring the Murray formation, a sequence of heterolithic mudstones and sandstones recording fluvial deltaic and lake deposits that comprise over 350 m of sedimentary strata within Gale crater. We examine >4,500 Murray formation bedrock points, employing recent laboratory calibrations for ChemCam laser-induced breakdown spectroscopy H measurements at millimeter scale. Bedrock in the Murray formation has an interquartile range of 2.3-3.1 wt.% H2O, similar to measurements using the Dynamic Albedo of Neutrons and Sample Analysis at Mars instruments. However, specific stratigraphic intervals include high H targets (6-18 wt.% H2O) correlated with Si, Mg, Ca, Mn, or Fe, indicating units with opal, hydrated Mg sulfates, hydrated Ca sulfates, Mn-enriched units, and akageneite or other iron oxyhydroxides, respectively. One stratigraphic interval with higher hydrogen is the Sutton Island unit and Blunts Point unit contact, where higher hydrogen is associated with Fe-rich, Ca-rich, and Mg-rich points. A second interval with higher hydrogen occurs in the Vera Rubin ridge portion of the Murray formation, where higher hydrogen is associated with Fe-rich, Ca-rich, and Si-rich points. We also observe trends in the H signal with grain size, separate from chemical variation, whereby coarser-grained rocks have higher hydrogen. Variability in the hydrogen content of rocks points to a history of water-rock interaction at Gale crater that included changes in lake water chemistry during Murray formation deposition and multiple subsequent groundwater episodes.
Collapse
Affiliation(s)
- N. H. Thomas
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - B. L. Ehlmann
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - W. Rapin
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | | | - N. T. Stein
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - J. Frydenvang
- Natural History MuseumUniversity of CopenhagenCopenhagenDenmark
| | - T. Gabriel
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | - P.‐Y. Meslin
- Institut de Recherche en Astrophysique et PlanétologieUniversité de Toulouse, CNRS, UPS, CNESToulouseFrance
| | - S. Maurice
- Institut de Recherche en Astrophysique et PlanétologieUniversité de Toulouse, CNRS, UPS, CNESToulouseFrance
| | - R. C. Wiens
- Los Alamos National LaboratoryLos AlamosNMUSA
| |
Collapse
|
2
|
Thomas NH, Ehlmann BL, Meslin P, Rapin W, Anderson DE, Rivera‐Hernández F, Forni O, Schröder S, Cousin A, Mangold N, Gellert R, Gasnault O, Wiens RC. Mars Science Laboratory Observations of Chloride Salts in Gale Crater, Mars. Geophys Res Lett 2019; 46:10754-10763. [PMID: 31894167 PMCID: PMC6919417 DOI: 10.1029/2019gl082764] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/18/2019] [Revised: 07/15/2019] [Accepted: 07/18/2019] [Indexed: 05/09/2023]
Abstract
The Mars Science Laboratory Curiosity rover is traversing a sequence of stratified sedimentary rocks in Gale crater that contain varied eolian, fluviodeltaic, and lake deposits, with phyllosilicates, iron oxides, and sulfate salts. Here, we report the chloride salt distribution along the rover traverse. Chlorine is detected at low levels (<3 wt.%) in soil and rock targets with multiple MSL instruments. Isolated fine-scale observations of high chlorine (up to ≥15 wt.% Cl), detected using the ChemCam instrument, are associated with elevated Na2O and interpreted as halite grains or cements in bedrock. Halite is also interpreted at the margins of veins and in nodular, altered textures. We have not detected halite in obvious evaporitic layers. Instead, its scattered distribution indicates that chlorides emplaced earlier in particular members of the Murray formation were remobilized and reprecipitated by later groundwaters within Murray formation mudstones and in diagenetic veins and nodules.
Collapse
Affiliation(s)
- N. H. Thomas
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - B. L. Ehlmann
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - P.‐Y. Meslin
- Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, UPS, CNESToulouseFrance
| | - W. Rapin
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - D. E. Anderson
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | | | - O. Forni
- Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, UPS, CNESToulouseFrance
| | | | - A. Cousin
- Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, UPS, CNESToulouseFrance
| | - N. Mangold
- Laboratoire de Planétologie et Géodynamique, UMR6112, CNRS, Université de NantesNantesFrance
| | - R. Gellert
- Department of PhysicsUniversity of GulephGulephOntarioCanada
| | - O. Gasnault
- Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, UPS, CNESToulouseFrance
| | - R. C. Wiens
- Los Alamos National LaboratoryLos AlamosNMUSA
| |
Collapse
|
3
|
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. J Geophys Res 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] [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: 05/31/2023]
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.
Collapse
|
4
|
Meslin P, Renoux MC, Manin C, Wendremaire P, Rosselini D, Tambat A, Tiprez C, Akhdar M. Une fièvre boutonneuse méditerranéenne chez un nourrisson de 2 mois. Arch Pediatr 2014; 21:772-5. [DOI: 10.1016/j.arcped.2014.04.022] [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] [Received: 09/29/2013] [Revised: 10/31/2013] [Accepted: 04/18/2014] [Indexed: 11/16/2022]
|