1
|
Fraeman AA, Edgar LA, Rampe EB, Thompson LM, Frydenvang J, Fedo CM, Catalano JG, Dietrich WE, Gabriel TSJ, Vasavada AR, Grotzinger JP, L'Haridon J, Mangold N, Sun VZ, House CH, Bryk AB, Hardgrove C, Czarnecki S, Stack KM, Morris RV, Arvidson RE, Banham SG, Bennett KA, Bridges JC, Edwards CS, Fischer WW, Fox VK, Gupta S, Horgan BHN, Jacob SR, Johnson JR, Johnson SS, Rubin DM, Salvatore MR, Schwenzer SP, Siebach KL, Stein NT, Turner SMR, Wellington DF, Wiens RC, Williams AJ, David G, Wong GM. Evidence for a Diagenetic Origin of Vera Rubin Ridge, Gale Crater, Mars: Summary and Synthesis of Curiosity's Exploration Campaign. J Geophys Res Planets 2020; 125:e2020JE006527. [PMID: 33520561 PMCID: PMC7818385 DOI: 10.1029/2020je006527] [Citation(s) in RCA: 9] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/13/2020] [Revised: 07/16/2020] [Accepted: 07/20/2020] [Indexed: 05/13/2023]
Abstract
This paper provides an overview of the Curiosity rover's exploration at Vera Rubin ridge (VRR) and summarizes the science results. VRR is a distinct geomorphic feature on lower Aeolis Mons (informally known as Mount Sharp) that was identified in orbital data based on its distinct texture, topographic expression, and association with a hematite spectral signature. Curiosity conducted extensive remote sensing observations, acquired data on dozens of contact science targets, and drilled three outcrop samples from the ridge, as well as one outcrop sample immediately below the ridge. Our observations indicate that strata composing VRR were deposited in a predominantly lacustrine setting and are part of the Murray formation. The rocks within the ridge are chemically in family with underlying Murray formation strata. Red hematite is dispersed throughout much of the VRR bedrock, and this is the source of the orbital spectral detection. Gray hematite is also present in isolated, gray-colored patches concentrated toward the upper elevations of VRR, and these gray patches also contain small, dark Fe-rich nodules. We propose that VRR formed when diagenetic event(s) preferentially hardened rocks, which were subsequently eroded into a ridge by wind. Diagenesis also led to enhanced crystallization and/or cementation that deepened the ferric-related spectral absorptions on the ridge, which helped make them readily distinguishable from orbit. Results add to existing evidence of protracted aqueous environments at Gale crater and give new insight into how diagenesis shaped Mars' rock record.
Collapse
Affiliation(s)
- A. A. Fraeman
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - L. A. Edgar
- U.S. Geological Survey Astrogeology Science CenterFlagstaffAZUSA
| | | | - L. M. Thompson
- Planetary and Space Science CentreUniversity of New BrunswickFrederictonNew BrunswickCanada
| | - J. Frydenvang
- Global InstituteUniversity of CopenhagenCopenhagenDenmark
| | - C. M. Fedo
- Department of Earth and Planetary SciencesUniversity of Tennessee, KnoxvilleKnoxvilleTNUSA
| | - J. G. Catalano
- Department of Earth and Planetary SciencesWashington University in St. LouisSt. LouisMOUSA
| | - W. E. Dietrich
- Department of Earth and Planetary ScienceUniversity of CaliforniaBerkeleyCAUSA
| | - T. S. J. Gabriel
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | - A. R. Vasavada
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - J. P. Grotzinger
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - J. L'Haridon
- Laboratoire de Planétologie et Géodynamique de Nantes, UMR6112 CNRSUniversité de Nantes, Université d'AngersNantesFrance
| | - N. Mangold
- Laboratoire de Planétologie et Géodynamique de Nantes, UMR6112 CNRSUniversité de Nantes, Université d'AngersNantesFrance
| | - V. Z. Sun
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - C. H. House
- Department of GeosciencesPennsylvania State UniversityUniversity ParkPAUSA
| | - A. B. Bryk
- Department of Earth and Planetary ScienceUniversity of CaliforniaBerkeleyCAUSA
| | - C. Hardgrove
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | - S. Czarnecki
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | - K. M. Stack
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | | | - R. E. Arvidson
- Department of Earth and Planetary SciencesWashington University in St. LouisSt. LouisMOUSA
| | - S. G. Banham
- Department of Earth Science and EngineeringImperial College LondonLondonUK
| | - K. A. Bennett
- U.S. Geological Survey Astrogeology Science CenterFlagstaffAZUSA
| | - J. C. Bridges
- Space Research Centre, School of Physics and AstronomyUniversity of LeicesterLeicesterUK
| | - C. S. Edwards
- Department of Astronomy and Planetary ScienceNorthern Arizona UniversityFlagstaffAZUSA
| | - W. W. Fischer
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - V. K. Fox
- Department of Earth SciencesUniversity of Minnesota, Twin CitiesMinneapolisMNUSA
| | - S. Gupta
- Department of Earth Science and EngineeringImperial College LondonLondonUK
| | - B. H. N. Horgan
- Department of Earth, Atmospheric, and Planetary SciencesPurdue UniversityWest LafayetteINUSA
| | - S. R. Jacob
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | - J. R. Johnson
- Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | - S. S. Johnson
- Department of Biology, Science, Technology, and International Affairs ProgramGeorgetown UniversityWashingtonDCUSA
| | - D. M. Rubin
- Department of Earth and Planetary SciencesUniversity of CaliforniaSanta CruzCAUSA
| | - M. R. Salvatore
- Department of Astronomy and Planetary ScienceNorthern Arizona UniversityFlagstaffAZUSA
| | | | - K. L. Siebach
- Department of Earth, Environmental, and Planetary SciencesRice UniversityHoustonTXUSA
| | - N. T. Stein
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | | | - D. F. Wellington
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | - R. C. Wiens
- Los Alamos National LaboratoryLos AlamosNMUSA
| | - A. J. Williams
- Department of Geological SciencesUniversity of FloridaGainesvilleFLUSA
| | - G. David
- L'Institut de Recherche en Astrophysique et PlanétologieToulouseFrance
| | - G. M. Wong
- Department of GeosciencesPennsylvania State UniversityUniversity ParkPAUSA
| |
Collapse
|
2
|
Jacob SR, Wellington DF, Bell JF, Achilles C, Fraeman AA, Horgan B, Johnson JR, Maurice S, Peters GH, Rampe EB, Thompson LM, Wiens RC. Spectral, Compositional, and Physical Properties of the Upper Murray Formation and Vera Rubin Ridge, Gale Crater, Mars. J Geophys Res Planets 2020; 125:e2019JE006290. [PMID: 33282613 PMCID: PMC7685153 DOI: 10.1029/2019je006290] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/27/2019] [Revised: 08/20/2020] [Accepted: 08/21/2020] [Indexed: 05/20/2023]
Abstract
During 2018 and 2019, the Mars Science Laboratory Curiosity rover investigated the chemistry, morphology, and stratigraphy of Vera Rubin ridge (VRR). Using orbital data from the Compact Reconnaissance Imaging Spectrometer for Mars, scientists attributed the strong 860 nm signal associated with VRR to the presence of red crystalline hematite. However, Mastcam multispectral data and CheMin X-ray diffraction (XRD) measurements show that the depth of the 860 nm absorption is negatively correlated with the abundance of red crystalline hematite, suggesting that other mineralogical or physical parameters are also controlling the 860 nm absorption. Here, we examine Mastcam and ChemCam passive reflectance spectra from VRR and other locations to link the depth, position, and presence or absence of iron-related mineralogic absorption features to the XRD-derived rock mineralogy. Correlating CheMin mineralogy to spectral parameters showed that the ~860 nm absorption has a strong positive correlation with the abundance of ferric phyllosilicates. New laboratory reflectance measurements of powdered mineral mixtures can reproduce trends found in Gale crater. We hypothesize that variations in the 860 nm absorption feature in Mastcam and ChemCam observations of VRR materials are a result of three factors: (1) variations in ferric phyllosilicate abundance due to its ~800-1,000 nm absorption; (2) variations in clinopyroxene abundance because of its band maximum at ~860 nm; and (3) the presence of red crystalline hematite because of its absorption centered at 860 nm. We also show that relatively small changes in Ca-sulfate abundance is one potential cause of the erosional resistance and geomorphic expression of VRR.
Collapse
Affiliation(s)
- S. R. Jacob
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | - D. F. Wellington
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | - J. F. Bell
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | - C. Achilles
- NASA Goddard Space Flight CenterGreenbeltMDUSA
| | - A. A. Fraeman
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - B. Horgan
- Department of Earth, Atmospheric, and Planetary SciencesPurdue UniversityWest LafayetteINUSA
| | - J. R. Johnson
- Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | - S. Maurice
- Institut de Recherche en Astrophysique et PlanetologieToulouseFrance
| | - G. H. Peters
- NASA Neil A. Armstrong Flight Research CenterEdwardsCAUSA
| | | | - L. M. Thompson
- Planetary and Space Science CentreUniversity of New BrunswickCanada
| | - R. C. Wiens
- Los Alamos National LaboratoryLos AlamosNMUSA
| |
Collapse
|
3
|
Fraeman AA, Johnson JR, Arvidson RE, Rice MS, Wellington DF, Morris RV, Fox VK, Horgan BHN, Jacob SR, Salvatore MR, Sun VZ, Pinet P, Bell JF, Wiens RC, Vasavada AR. Synergistic Ground and Orbital Observations of Iron Oxides on Mt. Sharp and Vera Rubin Ridge. J Geophys Res Planets 2020; 125:e2019JE006294. [PMID: 33042722 PMCID: PMC7539960 DOI: 10.1029/2019je006294] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/26/2019] [Revised: 07/21/2020] [Accepted: 07/23/2020] [Indexed: 05/04/2023]
Abstract
Visible/short-wave infrared spectral data from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) show absorptions attributed to hematite at Vera Rubin ridge (VRR), a topographic feature on northwest Mt. Sharp. The goals of this study are to determine why absorptions caused by ferric iron are strongly visible from orbit at VRR and to improve interpretation of CRISM data throughout lower Mt. Sharp. These goals are achieved by analyzing coordinated CRISM and in situ spectral data along the Curiosity Mars rover's traverse. VRR bedrock within areas that have the deepest ferric absorptions in CRISM data also has the deepest ferric absorptions measured in situ. This suggests strong ferric absorptions are visible from orbit at VRR because of the unique spectral properties of VRR bedrock. Dust and mixing with basaltic sand additionally inhibit the ability to measure ferric absorptions in bedrock stratigraphically below VRR from orbit. There are two implications of these findings: (1) Ferric absorptions in CRISM data initially dismissed as noise could be real, and ferric phases are more widespread in lower Mt. Sharp than previously reported. (2) Patches with the deepest ferric absorptions in CRISM data are, like VRR, reflective of deeper absorptions in the bedrock. One model to explain this spectral variability is late-stage diagenetic fluids that changed the grain size of ferric phases, deepening absorptions. Curiosity's experience highlights the strengths of using CRISM data for spectral absorptions and associated mineral detections and the caveats in using these data for geologic interpretations and strategic path planning tools.
Collapse
Affiliation(s)
- A. A. Fraeman
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - J. R. Johnson
- Johns Hopkins University Applied Physics LaboratoryLaurelMDUSA
| | - R. E. Arvidson
- Department of Earth and Planetary SciencesWashington UniversitySt. LouisMOUSA
| | - M. S. Rice
- Geology Department, Physics and Astronomy DepartmentWestern Washington UniversityBellinghamWAUSA
| | - D. F. Wellington
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | | | - V. K. Fox
- Division of Geological and Planetary SciencesCalifornia Institute of TechnologyPasadenaCAUSA
| | - B. H. N. Horgan
- Department of Earth, Atmospheric, and Planetary SciencesPurdue UniversityWest LafayetteINUSA
| | - S. R. Jacob
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | - M. R. Salvatore
- Department of Astronomy and Planetary ScienceNorthern Arizona UniversityFlagstaffAZUSA
| | - V. Z. Sun
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| | - P. Pinet
- Institut de Recherche en Astrophysique et PlanétologieUniversité de Toulouse, CNRS, UPS, CNESToulouseFrance
| | - J. F. Bell
- School of Earth and Space ExplorationArizona State UniversityTempeAZUSA
| | - R. C. Wiens
- Los Alamos National LaboratoryLos AlamosNMUSA
| | - A. R. Vasavada
- Jet Propulsion LaboratoryCalifornia Institute of TechnologyPasadenaCAUSA
| |
Collapse
|
4
|
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.
Collapse
|
5
|
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
|