Geochemical diversity in first rocks examined by the Curiosity Rover in Gale Crater: Evidence for and significance of an alkali and volatile‐rich igneous source
Mariek E. Schmidt,John Campbell,Ralf Gellert,G. M. Perrett,Allan H. Treiman,Diana L. Blaney,A. Olilla,Fred Calef,Lauren A. Edgar,B. Elliott,John P. Grotzinger,John P. Grotzinger,Joel A. Hurowitz,Penelope L. King,Michelle E. Minitti,Violaine Sautter,K. M. Stack,Jeff A. Berger,John Bridges,Bethany L. Ehlmann,Bethany L. Ehlmann,Olivier Forni,L. A. Leshin,Kevin W. Lewis,Scott M. McLennan,D. W. Ming,Horton E. Newsom,I. Pradler,S. W. Squyres,Edward M. Stolper,Lucy M. Thompson,Scott VanBommel,Roger C. Wiens +32 more
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The first four rocks examined by the Mars Science Laboratory Alpha Particle X-ray Spectrometer indicate that Curiosity landed in a lithologically diverse region of Mars as discussed by the authors, collectively dubbed the Bradbury assemblage, were studied along an eastward traverse.Abstract:
The first four rocks examined by the Mars Science Laboratory Alpha Particle X-ray Spectrometer indicate that Curiosity landed in a lithologically diverse region of Mars. These rocks, collectively dubbed the Bradbury assemblage, were studied along an eastward traverse (sols 46–102). Compositions range from Na- and Al-rich mugearite Jake_Matijevic to Fe-, Mg-, and Zn-rich alkali-rich basalt/hawaiite Bathurst_Inlet and span nearly the entire range in FeO* and MnO of the data sets from previous Martian missions and Martian meteorites. The Bradbury assemblage is also enriched in K and moderately volatile metals (Zn and Ge). These elements do not correlate with Cl or S, suggesting that they are associated with the rocks themselves and not with salt-rich coatings. Three out of the four Bradbury rocks plot along a line in elemental variation diagrams, suggesting mixing between Al-rich and Fe-rich components. ChemCam analyses give insight to their degree of chemical heterogeneity and grain size. Variations in trace elements detected by ChemCam suggest chemical weathering (Li) and concentration in mineral phases (e.g., Rb and Sr in feldspars). We interpret the Bradbury assemblage to be broadly volcanic and/or volcaniclastic, derived either from near the Gale crater rim and transported by the Peace Vallis fan network, or from a local volcanic source within Gale Crater. High Fe and Fe/Mn in Et_Then likely reflect secondary precipitation of Fe^(3+) oxides as a cement or rind. The K-rich signature of the Bradbury assemblage, if igneous in origin, may have formed by small degrees of partial melting of metasomatized mantle.read more
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In situ evidence for continental crust on early Mars
V. Sautter,M. Toplis,Roger C. Wiens,Agnes Cousin,Cécile Fabre,Olivier Gasnault,Sylvestre Maurice,Olivier Forni,Jérémie Lasue,Ann Ollila,John Bridges,Nicolas Mangold,S. Le Mouélic,Martin R. Fisk,P. Y. Meslin,Pierre Beck,Patrick Pinet,L. Le Deit,William Rapin,Edward M. Stolper,H. E. Newsom,D. Dyar,Nina Lanza,David T. Vaniman,Samuel M. Clegg,James J. Wray +25 more
TL;DR: In this article, the authors present geochemical data and images of 22 specimens analysed by Curiosity that demonstrate that these light-toned materials are feldspar-rich magmatic rocks.
Journal ArticleDOI
Mineralogy, provenance, and diagenesis of a potassic basaltic sandstone on Mars: CheMin X-ray diffraction of the Windjana sample (Kimberley area, Gale Crater)
Allan H. Treiman,David L. Bish,David T. Vaniman,Steve J. Chipera,David F. Blake,D. W. Ming,Richard V. Morris,Thomas F. Bristow,Shaunna M. Morrison,Michael B. Baker,Elizabeth B. Rampe,Robert T. Downs,Justin Filiberto,Allen F. Glazner,Ralf Gellert,Lucy M. Thompson,Mariek E. Schmidt,Laetitia Le Deit,Roger C. Wiens,Amy McAdam,Cherie N. Achilles,Kenneth S. Edgett,Jack D. Farmer,Kim V. Fendrich,John P. Grotzinger,Sanjeev Gupta,John Michael Morookian,M. E. Newcombe,Melissa S. Rice,John G. Spray,Edward M. Stolper,Dawn Y. Sumner,Ashwin R. Vasavada,Albert S. Yen +33 more
TL;DR: The presence of sediment from many igneous sources, in concert with Curiosity's identifications of other igneous materials (e.g., mugearite), implies that the northern rim of Gale Crater exposes a diverse igneous complex, at least as diverse as that found in similar‐age terranes on Earth.
Journal ArticleDOI
Evolved gas analyses of sedimentary rocks and eolian sediment in Gale Crater, Mars: Results of the Curiosity rover's sample analysis at Mars instrument from Yellowknife Bay to the Namib Dune
Brad Sutter,Amy McAdam,Paul R. Mahaffy,D. W. Ming,Kenneth S. Edgett,E. B. Rampe,J. L. Eigenbrode,Heather B. Franz,Caroline Freissinet,John P. Grotzinger,Andrew Steele,Christopher H. House,P. D. Archer,Charles Malespin,Rafael Navarro-González,J. C. Stern,James F. Bell,Fred Calef,R. Gellert,Daniel P. Glavin,Lucy M. Thompson,Albert S. Yen +21 more
TL;DR: The Sample Analysis at Mars instrument evolved gas analyzer (SAM-EGA) has detected evolved water, H2, SO2, H 2S, NO, CO2, CO, O2 and HCl from two eolian sediments and nine sedimentary rocks from Gale Crater.
Journal ArticleDOI
Recalibration of the Mars Science Laboratory ChemCam instrument with an expanded geochemical database
Samuel M. Clegg,Roger C. Wiens,Ryan B. Anderson,Olivier Forni,Jens Frydenvang,Jérémie Lasue,Agnes Cousin,Valerie Payre,T. Boucher,M. Darby Dyar,Scott M. McLennan,Richard V. Morris,Trevor G. Graff,Stanley A. Mertzman,Bethany L. Ehlmann,Ines Belgacem,Horton E. Newsom,B. C. Clark,Noureddine Melikechi,A. Mezzacappa,Rhonda E. McInroy,Ronald Martinez,Patrick J. Gasda,Olivier Gasnault,Sylvestre Maurice +24 more
TL;DR: This article used a combination of partial least squares (PLS1) and independent component analysis (ICA) algorithms, together with a calibration transfer matrix to minimize differences between the conditions under which the standards were analyzed in the laboratory and the conditions on Mars.
Journal ArticleDOI
Diagenesis and clay mineral formation at Gale Crater, Mars
John Bridges,Susanne P. Schwenzer,Richard Leveille,Frances Westall,Roger C. Wiens,N. Mangold,Thomas F. Bristow,P. Edwards,Gilles Berger +8 more
TL;DR: In this paper, the Sheepbed mudstones of Yellowknife bay were modeled using thermochemical modeling to constrain the formation conditions of its secondary mineral assemblages. But the results of the modeling were not yet available.
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