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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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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.
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Grotzinger JP, Gupta S, Malin MC, Rubin DM, Schieber J, Siebach K, Sumner DY, Stack KM, Vasavada AR, Arvidson RE, Calef F, Edgar L, Fischer WF, Grant JA, Griffes J, Kah LC, Lamb MP, Lewis KW, Mangold N, Minitti ME, Palucis M, Rice M, Williams RME, Yingst RA, Blake D, Blaney D, Conrad P, Crisp J, Dietrich WE, Dromart G, Edgett KS, Ewing RC, Gellert R, Hurowitz JA, Kocurek G, Mahaffy P, McBride MJ, McLennan SM, Mischna M, Ming D, Milliken R, Newsom H, Oehler D, Parker TJ, Vaniman D, Wiens RC, Wilson SA. Deposition, exhumation, and paleoclimate of an ancient lake deposit, Gale crater, Mars. Science 2015; 350:aac7575. [DOI: 10.1126/science.aac7575] [Citation(s) in RCA: 399] [Impact Index Per Article: 44.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
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Stolper EM, Baker MB, Newcombe ME, Schmidt ME, Treiman AH, Cousin A, Dyar MD, Fisk MR, Gellert R, King PL, Leshin L, Maurice S, McLennan SM, Minitti ME, Perrett G, Rowland S, Sautter V, Wiens RC, Kemppinen O, Bridges N, Johnson JR, Cremers D, Bell JF, Edgar L, Farmer J, Godber A, Wadhwa M, Wellington D, McEwan I, Newman C, Richardson M, Charpentier A, Peret L, Blank J, Weigle G, Li S, Milliken R, Robertson K, Sun V, Edwards C, Ehlmann B, Farley K, Griffes J, Grotzinger J, Miller H, Pilorget C, Rice M, Siebach K, Stack K, Brunet C, Hipkin V, Léveillé R, Marchand G, Sánchez PS, Favot L, Cody G, Steele A, Flückiger L, Lees D, Nefian A, Martin M, Gailhanou M, Westall F, Israël G, Agard C, Baroukh J, Donny C, Gaboriaud A, Guillemot P, Lafaille V, Lorigny E, Paillet A, Pérez R, Saccoccio M, Yana C, Armiens‐Aparicio C, Rodríguez JC, Blázquez IC, Gómez FG, Gómez-Elvira J, Hettrich S, Malvitte AL, Jiménez MM, Martínez-Frías J, Martín-Soler J, Martín-Torres FJ, Jurado AM, Mora-Sotomayor L, Caro GM, López SN, Peinado-González V, Pla-García J, Manfredi JAR, Romeral-Planelló JJ, Fuentes SAS, Martinez ES, Redondo JT, Urqui-O'Callaghan R, Mier MPZ, Chipera S, Lacour JL, Mauchien P, Sirven JB, Manning H, Fairén A, Hayes A, Joseph J, Squyres S, Sullivan R, Thomas P, Dupont A, Lundberg A, Melikechi N, Mezzacappa A, DeMarines J, Grinspoon D, Reitz G, Prats B, Atlaskin E, Genzer M, Harri AM, Haukka H, Kahanpää H, Kauhanen J, Kemppinen O, Paton M, Polkko J, Schmidt W, Siili T, Fabre C, Wray J, Wilhelm MB, Poitrasson F, Patel K, Gorevan S, Indyk S, Paulsen G, Gupta S, Bish D, Schieber J, Gondet B, Langevin Y, Geffroy C, Baratoux D, Berger G, Cros A, d’Uston C, Forni O, Gasnault O, Lasue J, Lee QM, Meslin PY, Pallier E, Parot Y, Pinet P, Schröder S, Toplis M, Lewin É, Brunner W, Heydari E, Achilles C, Oehler D, Sutter B, Cabane M, Coscia D, Israël G, Szopa C, Teinturier S, Dromart G, Robert F, Le Mouélic S, Mangold N, Nachon M, Buch A, Stalport F, Coll P, François P, Raulin F, Cameron J, Clegg S, DeLapp D, Dingler R, Jackson RS, Johnstone S, Lanza N, Little C, Nelson T, Williams RB, Kirkland L, Baker B, Cantor B, Caplinger M, Davis S, Duston B, Edgett K, Fay D, Hardgrove C, Harker D, Herrera P, Jensen E, Kennedy MR, Krezoski G, Krysak D, Lipkaman L, Malin M, McCartney E, McNair S, Nixon B, Posiolova L, Ravine M, Salamon A, Saper L, Stoiber K, Supulver K, Van Beek J, Van Beek T, Zimdar R, French KL, Iagnemma K, Miller K, Summons R, Goesmann F, Goetz W, Hviid S, Johnson M, Lefavor M, Lyness E, Breves E, Fassett C, Blake DF, Bristow T, DesMarais D, Edwards L, Haberle R, Hoehler T, Hollingsworth J, Kahre M, Keely L, McKay C, Wilhelm MB, Bleacher L, Brinckerhoff W, Choi D, Conrad P, Dworkin JP, Eigenbrode J, Floyd M, Freissinet C, Garvin J, Glavin D, Harpold D, Mahaffy P, Martin DK, McAdam A, Pavlov A, Raaen E, Smith MD, Stern J, Tan F, Trainer M, Meyer M, Posner A, Voytek M, Anderson RC, Aubrey A, Beegle LW, Behar A, Blaney D, Brinza D, Calef F, Christensen L, Crisp J, DeFlores L, Ehlmann B, Feldman J, Feldman S, Flesch G, Hurowitz J, Jun I, Keymeulen D, Maki J, Mischna M, Morookian JM, Parker T, Pavri B, Schoppers M, Sengstacken A, Simmonds JJ, Spanovich N, Juarez MDLT, Vasavada A, Webster CR, Yen A, Archer PD, Cucinotta F, Jones JH, Ming D, Morris RV, Niles P, Rampe E, Nolan T, Radziemski L, Barraclough B, Bender S, Berman D, Dobrea EN, Tokar R, Vaniman D, Williams RME, Yingst A, Lewis K, Cleghorn T, Huntress W, Manhès G, Hudgins J, Olson T, Stewart N, Sarrazin P, Grant J, Vicenzi E, Wilson SA, Bullock M, Ehresmann B, Hamilton V, Hassler D, Peterson J, Rafkin S, Zeitlin C, Fedosov F, Golovin D, Karpushkina N, Kozyrev A, Litvak M, Malakhov A, Mitrofanov I, Mokrousov M, Nikiforov S, Prokhorov V, Sanin A, Tretyakov V, Varenikov A, Vostrukhin A, Kuzmin R, Clark B, Wolff M, Botta O, Drake D, Bean K, Lemmon M, Schwenzer SP, Anderson RB, Herkenhoff K, Lee EM, Sucharski R, Hernández MÁDP, Ávalos JJB, Ramos M, Jones A, Kim MH, Malespin C, Plante I, Muller JP, Navarro-González R, Ewing R, Boynton W, Downs R, Fitzgibbon M, Harshman K, Morrison S, Dietrich W, Kortmann O, Palucis M, Sumner DY, Williams A, Lugmair G, Wilson MA, Rubin D, Jakosky B, Balic-Zunic T, Frydenvang J, Jensen JK, Kinch K, Koefoed A, Madsen MB, Stipp SLS, Boyd N, Campbell JL, Pradler I, VanBommel S, Jacob S, Owen T, Atlaskin E, Savijärvi H, Boehm E, Böttcher S, Burmeister S, Guo J, Köhler J, García CM, Mueller-Mellin R, Wimmer-Schweingruber R, Bridges JC, McConnochie T, Benna M, Franz H, Bower H, Brunner A, Blau H, Boucher T, Carmosino M, Atreya S, Elliott H, Halleaux D, Rennó N, Wong M, Pepin R, Elliott B, Spray J, Thompson L, Gordon S, Newsom H, Ollila A, Williams J, Vasconcelos P, Bentz J, Nealson K, Popa R, Kah LC, Moersch J, Tate C, Day M, Kocurek G, Hallet B, Sletten R, Francis R, McCullough E, Cloutis E, ten Kate IL, Kuzmin R, Arvidson R, Fraeman A, Scholes D, Slavney S, Stein T, Ward J, Berger J, Moores JE. The Petrochemistry of Jake_M: A Martian Mugearite. Science 2013; 341:1239463. [DOI: 10.1126/science.1239463] [Citation(s) in RCA: 115] [Impact Index Per Article: 10.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/03/2022]
Affiliation(s)
| | | | | | - M. E. Schmidt
- Brock University, St. Catharines, Ontario L2T 3V8, Canada
| | - A. H. Treiman
- Lunar and Planetary Institute, Houston, TX 77058, USA
| | - A. Cousin
- Los Alamos National Laboratory, Los Alamos, NM 87545, USA
- Institut de Recherches en Astrophysique et Planétologie, 31028 Toulouse, France
| | - M. D. Dyar
- Mount Holyoke College, South Hadley, MA 01075, USA
| | - M. R. Fisk
- Oregon State University, Corvallis, OR 97331, USA
| | - R. Gellert
- University of Guelph, Guelph, Ontario N1G 2W1, Canada
| | - P. L. King
- Research School of Earth Sciences, Australian National University, Acton, ACT 0200, Australia
| | - L. Leshin
- Rensselaer Polytechnic Institute, Troy, NY 12180, USA
| | - S. Maurice
- Institut de Recherches en Astrophysique et Planétologie, 31028 Toulouse, France
| | - S. M. McLennan
- The State University of New York, Stony Brook, NY 11794, USA
| | - M. E. Minitti
- Applied Physics Laboratory, The Johns Hopkins University, Baltimore, MD 20723, USA
| | - G. Perrett
- University of Guelph, Guelph, Ontario N1G 2W1, Canada
| | - S. Rowland
- University of Hawaii, Honolulu, HI 96822, USA
| | - V. Sautter
- Laboratoire de Minéralogie et Cosmochimie du Muséum, 75005 Paris, France
| | - R. C. Wiens
- Los Alamos National Laboratory, Los Alamos, NM 87545, USA
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