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1. Volatile and organic compositions of sedimentary rocks in Yellowknife Bay, Gale crater, Mars.

Author

Ming DW, Archer PD Jr, 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 3rd, 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, and Yingst RA

Subjects
Bays, Carbon Dioxide analysis, Carbon Dioxide chemistry, Geologic Sediments analysis, Geologic Sediments chemistry, Oxygen analysis, Oxygen chemistry, Sulfides analysis, Sulfides chemistry, Water analysis, Water chemistry, Exobiology, Extraterrestrial Environment chemistry, Hydrocarbons, Chlorinated analysis, Mars, Volatile Organic Compounds analysis
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.

Published
2014
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2. Isotope ratios of H, C, and O in CO2 and H2O of the martian atmosphere.

Author

Webster CR, Mahaffy PR, Flesch GJ, Niles PB, Jones JH, Leshin LA, Atreya SK, Stern JC, Christensen LE, Owen T, Franz H, Pepin RO, Steele A, Achilles C, Agard C, Alves Verdasca JA, Anderson R, Anderson R, Archer D, Armiens-Aparicio C, Arvidson R, Atlaskin E, Aubrey A, Baker B, Baker M, Balic-Zunic T, Baratoux D, Baroukh J, Barraclough B, Bean K, Beegle L, Behar A, Bell J, Bender S, Benna M, Bentz J, Berger G, Berger J, Berman D, Bish D, Blake DF, Blanco Avalos JJ, Blaney D, Blank J, Blau H, Bleacher L, Boehm E, Botta O, Böttcher S, Boucher T, Bower H, Boyd N, Boynton B, Breves E, Bridges J, Bridges N, Brinckerhoff W, Brinza D, Bristow T, Brunet C, Brunner A, Brunner W, Buch A, Bullock M, Burmeister S, Cabane M, Calef F, Cameron J, Campbell J, Cantor B, Caplinger M, Caride Rodríguez J, Carmosino M, Carrasco Blázquez I, Charpentier A, Chipera S, Choi D, Clark B, Clegg S, Cleghorn T, Cloutis E, Cody G, Coll P, Conrad P, Coscia D, Cousin A, Cremers D, Crisp J, Cros A, Cucinotta F, d'Uston C, Davis S, Day M, de la Torre Juarez M, DeFlores L, DeLapp D, DeMarines J, DesMarais D, Dietrich W, Dingler R, Donny C, Downs B, Drake D, Dromart G, Dupont A, Duston B, Dworkin J, Dyar MD, Edgar L, Edgett K, Edwards C, Edwards L, Ehlmann B, Ehresmann B, Eigenbrode J, Elliott B, Elliott H, Ewing R, Fabre C, Fairén A, Farley K, Farmer J, Fassett C, Favot L, Fay D, Fedosov F, Feldman J, Feldman S, Fisk M, Fitzgibbon M, Floyd M, Flückiger L, Forni O, Fraeman A, Francis R, François P, Freissinet C, French KL, Frydenvang J, Gaboriaud A, Gailhanou M, Garvin J, Gasnault O, Geffroy C, Gellert R, Genzer M, Glavin D, Godber A, Goesmann F, Goetz W, Golovin D, Gómez Gómez F, Gómez-Elvira J, Gondet B, Gordon S, Gorevan S, Grant J, Griffes J, Grinspoon D, Grotzinger J, Guillemot P, Guo J, Gupta S, Guzewich S, Haberle R, Halleaux D, Hallet B, Hamilton V, Hardgrove C, Harker D, Harpold D, Harri AM, Harshman K, Hassler D, Haukka H, Hayes A, Herkenhoff K, Herrera P, Hettrich S, Heydari E, Hipkin V, Hoehler T, Hollingsworth J, Hudgins J, Huntress W, Hurowitz J, Hviid S, Iagnemma K, Indyk S, Israël G, Jackson R, Jacob S, Jakosky B, Jensen E, Jensen JK, Johnson J, Johnson M, Johnstone S, Jones A, Joseph J, Jun I, Kah L, Kahanpää H, Kahre M, Karpushkina N, Kasprzak W, Kauhanen J, Keely L, Kemppinen O, Keymeulen D, Kim MH, Kinch K, King P, Kirkland L, Kocurek G, Koefoed A, Köhler J, Kortmann O, Kozyrev A, Krezoski J, Krysak D, Kuzmin R, Lacour JL, Lafaille V, Langevin Y, Lanza N, Lasue J, Le Mouélic S, Lee EM, Lee QM, Lees D, Lefavor M, Lemmon M, Lepinette Malvitte A, Léveillé R, Lewin-Carpintier É, Lewis K, Li S, Lipkaman L, Little C, Litvak M, Lorigny E, Lugmair G, Lundberg A, Lyness E, Madsen M, Maki J, Malakhov A, Malespin C, Malin M, Mangold N, Manhes G, Manning H, Marchand G, Marín Jiménez M, Martín García C, Martin D, Martin M, Martínez-Frías J, Martín-Soler J, Martín-Torres FJ, Mauchien P, Maurice S, McAdam A, McCartney E, McConnochie T, McCullough E, McEwan I, McKay C, McLennan S, McNair S, Melikechi N, Meslin PY, Meyer M, Mezzacappa A, Miller H, Miller K, Milliken R, Ming D, Minitti M, Mischna M, Mitrofanov I, Moersch J, Mokrousov M, Molina Jurado A, Moores J, Mora-Sotomayor L, Morookian JM, Morris R, Morrison S, Mueller-Mellin R, Muller JP, Muñoz Caro G, Nachon M, Navarro López S, Navarro-González R, Nealson K, Nefian A, Nelson T, Newcombe M, Newman C, Newsom H, Nikiforov S, Nixon B, Noe Dobrea E, Nolan T, Oehler D, Ollila A, Olson T, de Pablo Hernández MÁ, Paillet A, Pallier E, Palucis M, Parker T, Parot Y, Patel K, Paton M, Paulsen G, Pavlov A, Pavri B, Peinado-González V, Peret L, Perez R, Perrett G, Peterson J, Pilorget C, Pinet P, Pla-García J, Plante I, Poitrasson F, Polkko J, Popa R, Posiolova L, Posner A, Pradler I, Prats B, Prokhorov V, Purdy SW, Raaen E, Radziemski L, Rafkin S, Ramos M, Rampe E, Raulin F, Ravine M, Reitz G, Rennó N, Rice M, Richardson M, Robert F, Robertson K, Rodriguez Manfredi JA, Romeral-Planelló JJ, Rowland S, Rubin D, Saccoccio M, Salamon A, Sandoval J, Sanin A, Sans Fuentes SA, Saper L, Sarrazin P, Sautter V, Savijärvi H, Schieber J, Schmidt M, Schmidt W, Scholes D, Schoppers M, Schröder S, Schwenzer S, Sebastian Martinez E, Sengstacken A, Shterts R, Siebach K, Siili T, Simmonds J, Sirven JB, Slavney S, Sletten R, Smith M, Sobrón Sánchez P, Spanovich N, Spray J, Squyres S, Stack K, Stalport F, Stein T, Stewart N, Stipp SL, Stoiber K, Stolper E, Sucharski B, Sullivan R, Summons R, Sumner D, Sun V, Supulver K, Sutter B, Szopa C, Tan F, Tate C, Teinturier S, ten Kate I, Thomas P, Thompson L, Tokar R, Toplis M, Torres Redondo J, Trainer M, Treiman A, Tretyakov V, Urqui-O'Callaghan R, Van Beek J, Van Beek T, VanBommel S, Vaniman D, Varenikov A, Vasavada A, Vasconcelos P, Vicenzi E, Vostrukhin A, Voytek M, Wadhwa M, Ward J, Weigle E, Wellington D, Westall F, Wiens RC, Wilhelm MB, Williams A, Williams J, Williams R, Williams RB, Wilson M, Wimmer-Schweingruber R, Wolff M, Wong M, Wray J, Wu M, Yana C, Yen A, Yingst A, Zeitlin C, Zimdar R, and Zorzano Mier MP

Abstract

Stable isotope ratios of H, C, and O are powerful indicators of a wide variety of planetary geophysical processes, and for Mars they reveal the record of loss of its atmosphere and subsequent interactions with its surface such as carbonate formation. We report in situ measurements of the isotopic ratios of D/H and (18)O/(16)O in water and (13)C/(12)C, (18)O/(16)O, (17)O/(16)O, and (13)C(18)O/(12)C(16)O in carbon dioxide, made in the martian atmosphere at Gale Crater from the Curiosity rover using the Sample Analysis at Mars (SAM)'s tunable laser spectrometer (TLS). Comparison between our measurements in the modern atmosphere and those of martian meteorites such as ALH 84001 implies that the martian reservoirs of CO2 and H2O were largely established ~4 billion years ago, but that atmospheric loss or surface interaction may be still ongoing.

Published
2013
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3. Mineralogy at Meridiani Planum from the Mini-TES Experiment on the Opportunity Rover.

Author

Christensen PR, Wyatt MB, Glotch TD, Rogers AD, Anwar S, Arvidson RE, Bandfield JL, Blaney DL, Budney C, Calvin WM, Fallacaro A, Fergason RL, Gorelick N, Graff TG, Hamilton VE, Hayes AG, Johnson JR, Knudson AT, McSween HY Jr, Mehall GL, Mehall LK, Moersch JE, Morris RV, Smith MD, Squyres SW, Ruff SW, and Wolff MJ

Subjects
Calcium Sulfate, Extraterrestrial Environment, Ferric Compounds, Geologic Sediments, Iron Compounds, Magnesium Compounds, Magnesium Sulfate, Silicates, Spacecraft, Sulfates, Water, Mars, Minerals
Abstract

The Miniature Thermal Emission Spectrometer (Mini-TES) on Opportunity investigated the mineral abundances and compositions of outcrops, rocks, and soils at Meridiani Planum. Coarse crystalline hematite and olivine-rich basaltic sands were observed as predicted from orbital TES spectroscopy. Outcrops of aqueous origin are composed of 15 to 35% by volume magnesium and calcium sulfates [a high-silica component modeled as a combination of glass, feldspar, and sheet silicates (approximately 20 to 30%)], and hematite; only minor jarosite is identified in Mini-TES spectra. Mini-TES spectra show only a hematite signature in the millimeter-sized spherules. Basaltic materials have more plagioclase than pyroxene, contain olivine, and are similar in inferred mineral composition to basalt mapped from orbit. Bounce rock is dominated by clinopyroxene and is close in inferred mineral composition to the basaltic martian meteorites. Bright wind streak material matches global dust. Waterlain rocks covered by unaltered basaltic sands suggest a change from an aqueous environment to one dominated by physical weathering.

Published
2004
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4. The Opportunity Rover's Athena science investigation at Meridiani Planum, Mars.

Author

Squyres SW, Arvidson RE, Bell JF 3rd, Brückner J, Cabrol NA, Calvin W, Carr MH, Christensen PR, Clark BC, Crumpler L, 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 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 Jr, Richter L, Rieder R, Sims M, Smith M, Smith P, Soderblom LA, Sullivan R, Wänke H, Wdowiak T, Wolff M, and Yen A

Subjects
Atmosphere, Evolution, Planetary, Extraterrestrial Environment, Ferric Compounds, Geologic Sediments, Minerals, Silicates, Spacecraft, Water, Wind, Mars
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.

Published
2004
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5. Surficial deposits at Gusev Crater along Spirit Rover traverses.

Author

Grant JA, Arvidson R, Bell JF 3rd, 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 Jr, Ruff S, Richter L, Squyres S, Sullivan R, and Weitz C

Subjects
Extraterrestrial Environment, Geologic Sediments, Minerals, Silicates, Volcanic Eruptions, Water, Mars
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.

Published
2004
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6. Initial results from the Mini-TES experiment in Gusev Crater from the Spirit Rover.

Author

Christensen PR, Ruff SW, Fergason RL, Knudson AT, Anwar S, Arvidson RE, Bandfield JL, Blaney DL, Budney C, Calvin WM, Glotch TD, Golombek MP, Gorelick N, Graff TG, Hamilton VE, Hayes A, Johnson JR, McSween HY Jr, Mehall GL, Mehall LK, Moersch JE, Morris RV, Rogers AD, Smith MD, Squyres SW, Wolff MJ, and Wyatt MB

Subjects
Carbonates, Geologic Sediments, Interferometry, Iron Compounds, Magnesium Compounds, Oxides, Silicates, Spectrum Analysis, Temperature, Water, Mars, Minerals
Abstract

The Miniature Thermal Emission Spectrometer (Mini-TES) on Spirit has studied the mineralogy and thermophysical properties at Gusev crater. Undisturbed soil spectra show evidence for minor carbonates and bound water. Rocks are olivinerich basalts with varying degrees of dust and other coatings. Dark-toned soils observed on disturbed surfaces may be derived from rocks and have derived mineralogy (+/-5 to 10%) of 45% pyroxene (20% Ca-rich pyroxene and 25% pigeonite), 40% sodic to intermediate plagioclase, and 15% olivine (forsterite 45% +/-5 to 10). Two spectrally distinct coatings are observed on rocks, a possible indicator of the interaction of water, rock, and airfall dust. Diurnal temperature data indicate particle sizes from 40 to 80 microm in hollows to approximately 0.5 to 3 mm in soils.

Published
2004
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7. The Spirit Rover's Athena science investigation at Gusev Crater, Mars.

Author

Squyres SW, Arvidson RE, Bell JF 3rd, 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 Jr, Richter L, Rieder R, Sims M, Smith M, Smith P, Soderblom LA, Sullivan R, Wänke H, Wdowiak T, Wolff M, and Yen A

Subjects
Atmosphere, Extraterrestrial Environment, Geologic Sediments, Geological Phenomena, Geology, Magnetics, Minerals, Water, Wind, Mars
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.

Published
2004
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8. Pancam multispectral imaging results from the Spirit Rover at Gusev Crater.

Author

Bell JF 3rd, 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 MY, 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 Jr, Ming DW, Moersch JE, Morris RV, Dobrea EZ, Parker TJ, Proton J, Rice JW Jr, Seelos F, Soderblom J, Soderblom LA, Sohl-Dickstein JN, Sullivan RJ, Wolff MJ, and Wang A

Subjects
Atmosphere, Evolution, Planetary, Extraterrestrial Environment, Ferric Compounds, Geologic Sediments, Iron Compounds, Minerals, Silicates, Solar System, Spectrum Analysis, Water, Mars
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.

Published
2004
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9. Basaltic rocks analyzed by the Spirit Rover in Gusev Crater.

Author

McSween HY, Arvidson RE, Bell JF 3rd, Blaney D, Cabrol NA, Christensen PR, Clark BC, Crisp JA, Crumpler LS, Des Marais DJ, Farmer JD, Gellert R, Ghosh A, Gorevan S, Graff T, Grant J, Haskin LA, Herkenhoff KE, Johnson JR, Jolliff BL, Klingelhoefer G, Knudson AT, McLennan S, Milam KA, Moersch JE, Morris RV, Rieder R, Ruff SW, De Souza PA Jr, Squyres SW, Wänke H, Wang A, Wyatt MB, Yen A, and Zipfel J

Subjects
Extraterrestrial Environment, Geologic Sediments, Iron Compounds, Magnesium Compounds, Oxides, Spectroscopy, Mossbauer, Spectrum Analysis, Water, Mars, Minerals, Silicates
Abstract

The Spirit landing site in Gusev Crater on Mars contains dark, fine-grained, vesicular rocks interpreted as lavas. Pancam and Mini-Thermal Emission Spectrometer (Mini-TES) spectra suggest that all of these rocks are similar but have variable coatings and dust mantles. Magnified images of brushed and abraded rock surfaces show alteration rinds and veins. Rock interiors contain

Published
2004
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10. Wind-related processes detected by the Spirit Rover at Gusev Crater, Mars.

Author

Greeley R, Squyres SW, Arvidson RE, Bartlett P, Bell JF 3rd, Blaney D, Cabrol NA, Farmer J, Farrand B, Golombek MP, Gorevan SP, Grant JA, Haldemann AF, Herkenhoff KE, Johnson J, Landis G, Madsen MB, McLennan SM, Moersch J, Rice JW Jr, Richter L, Ruff S, Sullivan RJ, Thompson SD, Wang A, Weitz CM, and Whelley P

Subjects
Evolution, Planetary, Extraterrestrial Environment, Wind, Mars
Abstract

Wind-abraded rocks, ripples, drifts, and other deposits of windblown sediments are seen at the Columbia Memorial Station where the Spirit rover landed. Orientations of these features suggest formative winds from the north-northwest, consistent with predictions from atmospheric models of afternoon winds in Gusev Crater. Cuttings from the rover Rock Abrasion Tool are asymmetrically distributed toward the south-southeast, suggesting active winds from the north-northwest at the time (midday) of the abrasion operations. Characteristics of some rocks, such as a two-toned appearance, suggest that they were possibly buried and exhumed on the order of 5 to 60 centimeters by wind deflation, depending on location.

Published
2004
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