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51. Martian dust storms impact on atmospheric H2O and D/H observed by ExoMars Trace Gas Orbiter

Author

Vandaele, Ann Carine, Korablev, Oleg, Daerden, Frank, Aoki, Shohei, Thomas, Ian R., Altieri, Francesca, López-Valverde, Miguel, Villanueva, Geronimo L., Liuzzi, Giuliano, Smith, Michael D., Erwin, Justin T., Trompet, Loïc, Fedorova, Anna A., Montmessin, Franck, Trokhimovskiy, Alexander, Belyaev, Denis A., Ignatiev, Nikolay I., Luginin, Mikhail, Olsen, Kevin S., Baggio, Lucio, Alday, Juan, Bertaux, Jean-Loup, Betsis, Daria, Bolsée, David, Clancy, Todd, Cloutis, Edward, Depiesse, Cédric, Funke, Bernd, Garcia-Comas, Maia, Gérard, Jean-Claude, Giuranna, Marco, Gonzalez-Galindo, Francisco, Grigoriev, Alexey V., Ivanov, Yuriy S., Kaminski, Jacek, Karatekin, Ozgur, Lefèvre, Franck, Lewis, Stephen S.P., López-Puertas, Manuel, Mahieux, Arnaud, Maslov, Igor, Mason, Jon, Mumma, Michael J., Neary, Lori, Neefs, Eddy, Patrakeev, Andrey, Patsaev, Dmitry, Ristic, Bojan, Robert, Séverine, Schmidt, Frédéric, Shakun, Alexey, Teanby, Nicholas A., Viscardy, Sébastien, Willame, Yannick, Whiteway, James J.A., Wilquet, Valérie, Wolff, Michael J., Bellucci, Giancarlo, Patel, Manish R., López-Moreno, Jose-Juan, Forget, Francois, Wilson, Colin F., Svedhem, Håkan, Vago, Jorge L., Rodionov, Daniel, Alonso-Rodrigo, G., Bauduin, Sophie, Carrozzo, Giacomo, Crismani, Matteo, Da Pieve, Fabiana, D'Aversa, Emiliano, Etiope, Giuseppe, Fussen, Didier, Geminale, A., Gkouvelis, Leo, Holmes, James, Hubert, B., Kasaba, Y., Kass, David, Kleinböhl, A., Lanciano, Orietta, Nakagawa, Hiromu, Novak, Robert E., Oliva, Fabrizio, Piccialli, A., Renotte, E., Ritter, Birgit, Schneider, N., Sindoni, G., Thiemann, Ed, Vander Auwera, Jean, Wolkenberg, Paulina, Yelle, R., Anufreychik, Konstantin, Arnold, Gabriele, Duxbury, Natalia, Fouchet, Thierry, Grassi, Davide, Guerlet, Sandrine, Hartogh, Paul, Khatuntsev, Igor, Kokonkov, Nikita, Krasnopolsky, Vladimir, Kuzmin, Ruslan, Lacombe, Gaétan, Lellouch, Emmanuel, Määttänen, Anni A, Marcq, E., Martin-Torres, Javier, Medvedev, Alexander, Moshkin, Boris, Quantin-Nata, Cathy, Rodin, AM, Shematovich, Valery, Thomas, Nicolas Le, Vazquez, Luis, Vincendon, Matthieu, Zasova, Ludmila, Zelenyi, Lev, Zorzano, M. P., Vandaele, Ann Carine, Korablev, Oleg, Daerden, Frank, Aoki, Shohei, Thomas, Ian R., Altieri, Francesca, López-Valverde, Miguel, Villanueva, Geronimo L., Liuzzi, Giuliano, Smith, Michael D., Erwin, Justin T., Trompet, Loïc, Fedorova, Anna A., Montmessin, Franck, Trokhimovskiy, Alexander, Belyaev, Denis A., Ignatiev, Nikolay I., Luginin, Mikhail, Olsen, Kevin S., Baggio, Lucio, Alday, Juan, Bertaux, Jean-Loup, Betsis, Daria, Bolsée, David, Clancy, Todd, Cloutis, Edward, Depiesse, Cédric, Funke, Bernd, Garcia-Comas, Maia, Gérard, Jean-Claude, Giuranna, Marco, Gonzalez-Galindo, Francisco, Grigoriev, Alexey V., Ivanov, Yuriy S., Kaminski, Jacek, Karatekin, Ozgur, Lefèvre, Franck, Lewis, Stephen S.P., López-Puertas, Manuel, Mahieux, Arnaud, Maslov, Igor, Mason, Jon, Mumma, Michael J., Neary, Lori, Neefs, Eddy, Patrakeev, Andrey, Patsaev, Dmitry, Ristic, Bojan, Robert, Séverine, Schmidt, Frédéric, Shakun, Alexey, Teanby, Nicholas A., Viscardy, Sébastien, Willame, Yannick, Whiteway, James J.A., Wilquet, Valérie, Wolff, Michael J., Bellucci, Giancarlo, Patel, Manish R., López-Moreno, Jose-Juan, Forget, Francois, Wilson, Colin F., Svedhem, Håkan, Vago, Jorge L., Rodionov, Daniel, Alonso-Rodrigo, G., Bauduin, Sophie, Carrozzo, Giacomo, Crismani, Matteo, Da Pieve, Fabiana, D'Aversa, Emiliano, Etiope, Giuseppe, Fussen, Didier, Geminale, A., Gkouvelis, Leo, Holmes, James, Hubert, B., Kasaba, Y., Kass, David, Kleinböhl, A., Lanciano, Orietta, Nakagawa, Hiromu, Novak, Robert E., Oliva, Fabrizio, Piccialli, A., Renotte, E., Ritter, Birgit, Schneider, N., Sindoni, G., Thiemann, Ed, Vander Auwera, Jean, Wolkenberg, Paulina, Yelle, R., Anufreychik, Konstantin, Arnold, Gabriele, Duxbury, Natalia, Fouchet, Thierry, Grassi, Davide, Guerlet, Sandrine, Hartogh, Paul, Khatuntsev, Igor, Kokonkov, Nikita, Krasnopolsky, Vladimir, Kuzmin, Ruslan, Lacombe, Gaétan, Lellouch, Emmanuel, Määttänen, Anni A, Marcq, E., Martin-Torres, Javier, Medvedev, Alexander, Moshkin, Boris, Quantin-Nata, Cathy, Rodin, AM, Shematovich, Valery, Thomas, Nicolas Le, Vazquez, Luis, Vincendon, Matthieu, Zasova, Ludmila, Zelenyi, Lev, and Zorzano, M. P.

Abstract

info:eu-repo/semantics/published

Published
2019

52. The potential science and engineering value of samples delivered to Earth by Mars sample return

Author

Beaty, David D.W., Grady, Monica, McSween, H. Y., Sefton-Nash, E., Carrier, B., Altieri, F., Ammannito, E., Amelin, Yuri, Anand, Mahesh, Benning, Liane G, Bishop, J. L., Borg, L. E., Boucher, D., Brucato, John Robert, Buseman, H., Campbell, K., Czaja, A. D., Debaille, Vinciane, Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, Andrea A. D., Hausrath, E. M., Herd, C. D. K., Horgan, B., Humayun, M., Kleine, Thorsten, Kleinhenz, J., Mangold, Nicolas, Mayhew, L. E., McCoy, Tim, McCubbin, Francis M., McLennan, Scott M., Moser, Desmond, Moynier, Frédéric, Mustard, John Fraser, Niles, P. B., Ori, G. G., Raulin, F., Rettberg, Petra, Rucker, M. A., Schmitz, Nicole, Schwenzer, Susanne P., Septhon, M. A., Shaheen, R., Sharp, Z. D., Shuster, D. L., Siljeström, S., Smith, Caroline L., Spry, J. A., Steele, Andrew, Swindle, T. D., Ten Kate, Inge Loes, Tosca, N. J., Usui, Tomohiro, Van Kranendonk, M. J., Wadhwa, Meenakshi, Weiss, Benjamin P., Werner, Stephanie C., Westall, Frances, Wheeler, R. M., Zipfel, Jutta, Zorzano, M. P., Beaty, David D.W., Grady, Monica, McSween, H. Y., Sefton-Nash, E., Carrier, B., Altieri, F., Ammannito, E., Amelin, Yuri, Anand, Mahesh, Benning, Liane G, Bishop, J. L., Borg, L. E., Boucher, D., Brucato, John Robert, Buseman, H., Campbell, K., Czaja, A. D., Debaille, Vinciane, Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, Andrea A. D., Hausrath, E. M., Herd, C. D. K., Horgan, B., Humayun, M., Kleine, Thorsten, Kleinhenz, J., Mangold, Nicolas, Mayhew, L. E., McCoy, Tim, McCubbin, Francis M., McLennan, Scott M., Moser, Desmond, Moynier, Frédéric, Mustard, John Fraser, Niles, P. B., Ori, G. G., Raulin, F., Rettberg, Petra, Rucker, M. A., Schmitz, Nicole, Schwenzer, Susanne P., Septhon, M. A., Shaheen, R., Sharp, Z. D., Shuster, D. L., Siljeström, S., Smith, Caroline L., Spry, J. A., Steele, Andrew, Swindle, T. D., Ten Kate, Inge Loes, Tosca, N. J., Usui, Tomohiro, Van Kranendonk, M. J., Wadhwa, Meenakshi, Weiss, Benjamin P., Werner, Stephanie C., Westall, Frances, Wheeler, R. M., Zipfel, Jutta, and Zorzano, M. P.

Abstract

Executive summary provided in lieu of abstract., SCOPUS: no.j, info:eu-repo/semantics/published

Published
2019

53. The Atmospheric Chemistry Suite (ACS) of three spectrometers for the ExoMars 2016 Trace Gas Orbiter

Author

Korablev, O., Montmessin, F., Trokhimovskiy, A., Fedorova, A. A., Shakun, A. V., Grigoriev, A. V., Moshkin, B. E., Ignatiev, N. I., Forget, F., Lefèvre, F., Anufreychik, K., Dzuban, I., Ivanov, Y. S., Kalinnikov, Y. K., Kozlova, T. O., Kungurov, A., Makarov, V., Martynovich, F., Maslov, I., Merzlyakov, D., Moiseev, P. P., Nikolskiy, Y., Patrakeev, A., Patsaev, D., Santos-Skripko, A., Sazonov, O., Semena, N., Semenov, A., Shashkin, V., Sidorov, A., Stepanov, A. V., Stupin, I., Timonin, D., Titov, A. Y., Viktorov, A., Zharkov, A., Altieri, F., Arnold, G., Belyaev, D. A., Bertaux, J. L., Betsis, D. S., Duxbury, N., Encrenaz, T., Fouchet, T., Gérard, J.-C., Grassi, D., Guerlet, S., Hartogh, P., Kasaba, Y., Khatuntsev, I., Krasnopolsky, V. A., Kuzmin, R. O., Lellouch, E., Lopez-Valverde, M. A., Luginin, M., Määttänen, A., Marcq, E., Martin Torres, J., Medvedev, A. S., Millour, E., Olsen, K. S., Patel, M. R., Quantin-Nataf, C., Rodin, A. V., Shematovich, V. I., Thomas, I., Thomas, N., Vazquez, L., Vincendon, M., Wilquet, V., Wilson, C. F., Zasova, L. V., Zelenyi, L. M., Zorzano, M. P., Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Main Astronomical Observatory of NAS of Ukraine (MAO), National Academy of Sciences of Ukraine (NASU), National Research Institute for Physical-technical and Radiotechnical Measurements (VNIIFTRI), Scientific Production Enterprise Astron Electronics, Faculty of Physics [MSU, Moscow], Lomonosov Moscow State University (MSU), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Tohoku University [Sendai], Moscow Institute of Physics and Technology [Moscow] (MIPT), Catholic University of America, Vernadsky Institute of Geochemistry and Analytical Chemistry (GEOKHI), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Department of Computer Science [Kiruna], Luleå University of Technology (LUT), Instituto Andaluz de Ciencias de la Tierra (IACT), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Universidad de Granada (UGR), The Open University [Milton Keynes] (OU), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Institute of Astronomy of the Russian Academy of Sciences (INASAN), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Universität Bern [Bern], Facultad de Informática [Madrid], Universidad Complutense de Madrid [Madrid] (UCM), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Oxford], University of Oxford [Oxford], Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), PLANETO - LATMOS, Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad de Granada (UGR), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad de Granada = University of Granada (UGR), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Universität Bern [Bern] (UNIBE), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), University of Oxford, and Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)

Subjects
Cross-dispersion, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Atmosphere, 520 Astronomy, Mars, Echelle, Fourier-spectrometer, 620 Engineering, High-resolution spectrometer, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph]
Abstract

International audience; The Atmospheric Chemistry Suite (ACS) package is an element of the Russian contribution to the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission. ACS consists of three separate infrared spectrometers, sharing common mechanical, electrical, and thermal interfaces. This ensemble of spectrometers has been designed and developed in response to the Trace Gas Orbiter mission objectives that specifically address the requirement of high sensitivity instruments to enable the unambiguous detection of trace gases of potential geophysical or biological interest. For this reason, ACS embarks a set of instruments achieving simultaneously very high accuracy (ppt level), very high resolving power (>10,000) and large spectral coverage (0.7 to 17 μm—the visible to thermal infrared range). The near-infrared (NIR) channel is a versatile spectrometer covering the 0.7–1.6 μm spectral range with a resolving power of ∼20,000. NIR employs the combination of an echelle grating with an AOTF (Acousto-Optical Tunable Filter) as diffraction order selector. This channel will be mainly operated in solar occultation and nadir, and can also perform limb observations. The scientific goals of NIR are the measurements of water vapor, aerosols, and dayside or night side airglows. The mid-infrared (MIR) channel is a cross-dispersion echelle instrument dedicated to solar occultation measurements in the 2.2–4.4 μm range. MIR achieves a resolving power of >50,000. It has been designed to accomplish the most sensitive measurements ever of the trace gases present in the Martian atmosphere. The thermal-infrared channel (TIRVIM) is a 2-inch double pendulum Fourier-transform spectrometer encompassing the spectral range of 1.7–17 μm with apodized resolution varying from 0.2 to 1.3 cm−1. TIRVIM is primarily dedicated to profiling temperature from the surface up to ∼60 km and to monitor aerosol abundance in nadir. TIRVIM also has a limb and solar occultation capability. The technical concept of the instrument, its accommodation on the spacecraft, the optical designs as well as some of the calibrations, and the expected performances for its three channels are described.

Published
2018
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54. Martian Eolian Dust Probed by ChemCam

Author

Lasue, J., primary, Cousin, A., additional, Meslin, P.‐Y., additional, Mangold, N., additional, Wiens, R. C., additional, Berger, G., additional, Dehouck, E., additional, Forni, O., additional, Goetz, W., additional, Gasnault, O., additional, Rapin, W., additional, Schroeder, S., additional, Ollila, A., additional, Johnson, J., additional, Le Mouélic, S., additional, Maurice, S., additional, Anderson, R., additional, Blaney, D., additional, Clark, B., additional, Clegg, S. M., additional, d'Uston, C., additional, Fabre, C., additional, Lanza, N., additional, Madsen, M. B., additional, Martin‐Torres, J., additional, Melikechi, N., additional, Newsom, H., additional, Sautter, V., additional, and Zorzano, M. P., additional

Published
2018
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55. Spatiotemporal patterns driven by autocatalytic internal reaction noise.

Author

Hochberg, David, Zorzano, M.-P., and Morán, Federico

Subjects
SOLID solutions, LANGEVIN equations, CONTINUUM mechanics, DIFFERENTIAL equations, SEMICONDUCTOR doping, STOCHASTIC differential equations
Abstract

The influence that intrinsic local-density fluctuations can have on solutions of mean-field reaction-diffusion models is investigated numerically by means of the spatial patterns arising from two species that react and diffuse in the presence of strong internal reaction noise. The dynamics of the Gray–Scott (GS) model [P. Gray and S. K. Scott, Chem. Eng. Sci. 38, 29 (1983); and ibid.39, 1087 (1984); and J. Phys. Chem. 89, 22 (1985)] with a constant external source is first cast in terms of a continuum field theory representing the corresponding master equation. We then derive a Langevin description of the field theory and use these stochastic differential equations in our simulations. The nature of the multiplicative noise is specified exactly without recourse to assumptions and turns out to be of the same order as the reaction itself, and thus cannot be treated as a small perturbation. Many of the complex patterns obtained in the absence of noise for the GS model are completely obliterated by these strong internal fluctuations, but we find novel spatial patterns induced by this reaction noise in the regions of parameter space that otherwise correspond to homogeneous solutions when fluctuations are not included. [ABSTRACT FROM AUTHOR]

Published
2005
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56. Martian Eolian Dust Probed by ChemCam

Author

Lasue, J., Cousin, A., Meslin, P. -Y., Mangold, N., Wiens, R. C., Berger, G., Dehouck, E., Forni, O., Goetz, W., Gasnault, O., Rapin, W., Schroeder, S., Ollila, A., Johnson, J., Le Mouelic, S., Maurice, S., Anderson, R., Blaney, D., Clark, B., Clegg, S. M., d'Uston, C., Fabre, C., Lanza, N., Madsen, M. B., Martin-Torres, J., Melikechi, N., Newsom, H., Sautter, V., Zorzano, M. P., Lasue, J., Cousin, A., Meslin, P. -Y., Mangold, N., Wiens, R. C., Berger, G., Dehouck, E., Forni, O., Goetz, W., Gasnault, O., Rapin, W., Schroeder, S., Ollila, A., Johnson, J., Le Mouelic, S., Maurice, S., Anderson, R., Blaney, D., Clark, B., Clegg, S. M., d'Uston, C., Fabre, C., Lanza, N., Madsen, M. B., Martin-Torres, J., Melikechi, N., Newsom, H., Sautter, V., and Zorzano, M. P.

Published
2018

57. Convective vortices and dust devils at the MSL landing site

Author

Kahanpää, Henrik, Newman, C., Moores, J., Zorzano, M. -P., Martin-Torres, J., Navarro, S., Lepinette, A., Cantor, B., Lemmon, M. T., Valentin-Serrano, P., Ullan, A., Schmidt, W., School common, ELEC, Ashima Research, York University, Centro de Astrobiología, Luleå University of Technology, Malin Space Science Systems, Texas A&M University, Instituto Andaluz de Ciencias de la Tierra, University of Alcalá, Finnish Meteorological Institute, Department of Radio Science and Engineering, Department of Electronics and Nanoengineering, Aalto-yliopisto, and Aalto University

Subjects
MARTIAN ATMOSPHERE, PLANETARY BOUNDARY-LAYER, MARS PATHFINDER, STATISTICAL DISTRIBUTION, RESOLUTION STEREO CAMERA, GALE CRATER, LARGE-EDDY SIMULATIONS, SCIENCE LABORATORY MISSION, GENERAL-CIRCULATION MODEL, INTERANNUAL VARIABILITY
Abstract

Two hundred fifty-two transient drops in atmospheric pressure, likely caused by passing convective vortices, were detected by the Rover Environmental Monitoring Station instrument during the first Martian year of the Mars Science Laboratory (MSL) landed mission. These events resembled the vortex signatures detected by the previous Mars landers Pathfinder and Phoenix; however, the MSL observations contained fewer pressure drops greater than 1.5 Pa and none greater than 3.0 Pa. Apparently, these vortices were generally not lifting dust as only one probable dust devil has been observed visually by MSL. The obvious explanation for this is the smaller number of strong vortices with large central pressure drops since according to Arvidson et al. [2014] ample dust seems to be present on the surface. The annual variation in the number of detected convective vortices followed approximately the variation in Dust Devil Activity (DDA) predicted by the MarsWRF numerical climate model. This result does not prove, however, that the amount of dust lifted by dust devils would depend linearly on DDA, as is assumed in several numerical models of the Martian atmosphere, since dust devils are only the most intense fraction of all convective vortices on Mars, and the amount of dust that can be lifted by a dust devil depends on its central pressure drop. Sol-to-sol variations in the number of vortices were usually small. However, on 1 Martian solar day a sudden increase in vortex activity, related to a dust storm front, was detected.

Published
2016

58. Oxidation of manganese in an ancient aquifer, Kimberley formation, Gale crater, Mars

Author

Lanza, N., Wiens, R. C., Arvidson, R.E., Clark, B., Fischer, W.W., Gellert, R., Grotzinger, J., Hurowitz, J., McLennan, S M, Morris, R. V., Rice, M., Bell, J F, Berger, Jeff A., Blaney, D., Bridges, N., Calef, F., Campbell, J. L., Clegg, S., Cousin, A., Edgett, K., Fabre, C., Fisk, M., Forni, O., Frydenfang, Jens, Hardy, K., Hardgrove, C., Johnson, J., Lasue, J., Le Mouelic, S., Malin, M., Mangold, N., Martin-Torres, J., Maurice, S., McBride, M., Ming, D., Newsom, H., Ollila, A., Sautter, V., Schröder, Susanne, Thompson, L., Treiman, A., Van Bommel, S., Vaniman, D., Zorzano, M.-P., Los Alamos National Laboratory (LANL), Department of Earth and Planetary Sciences [St Louis], Washington University in Saint Louis (WUSTL), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Department of Physics [Guelph], University of Guelph, Stony Brook University [SUNY] (SBU), State University of New York (SUNY), Department of Geosciences, State University of New York (SUNY)-State University of New York (SUNY), Department of Primary Care and Population Health [London] (PCPH), University College of London [London] (UCL), The Alan Turing Institute, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Department of Mathematics and Statistics [Toronto], York University [Toronto], Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Malin Space Science Systems (MSSS), GeoRessources, Institut national des sciences de l'Univers (INSU - CNRS)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Oregon State University (OSU), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Computer Science, Electrical and Space Engineering [Luleå], Luleå University of Technology (LUT), NASA Johnson Space Center (JSC), NASA, Institute of Meteoritics [Albuquerque] (IOM), The University of New Mexico [Albuquerque], Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Centre National de la Recherche Scientifique (CNRS), Justus-Liebig-Universität Gießen = Justus Liebig University (JLU), University of Gothenburg (GU), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), and Justus-Liebig-Universität Gießen (JLU)

Subjects
Manganese, LIBS, ChemCam, [SDU]Sciences of the Universe [physics], Mars, MSL, Mars Science Laboratory, ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2016
Full Text
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59. Organic molecules in the Sheepbed Mudstone, Gale Crater, Mars

Author

Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Miller, Kristen, Summons, Roger E, Freissinet, C., Glavin, D. P., Mahaffy, P. R., Eigenbrode, J. L., Brunner, A. E., Buch, A., Szopa, C., Archer, P. D., Franz, H. B., Atreya, S. K., Brinckerhoff, W. B., Cabane, M., Coll, P., Conrad, P. G., Des Marais, D. J., Dworkin, J. P., Fairén, A. G., François, P., Grotzinger, J. P., Kashyap, S., ten Kate, I. L., Leshin, L. A., Malespin, C. A., Martin, M. G., Martin-Torres, F. J., McAdam, A. C., Ming, D. W., Navarro-González, R., Pavlov, A. A., Prats, B. D., Squyres, S. W., Steele, A., Stern, J. C., Sumner, D. Y., Sutter, B., Zorzano, M.-P., Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Miller, Kristen, Summons, Roger E, Freissinet, C., Glavin, D. P., Mahaffy, P. R., Eigenbrode, J. L., Brunner, A. E., Buch, A., Szopa, C., Archer, P. D., Franz, H. B., Atreya, S. K., Brinckerhoff, W. B., Cabane, M., Coll, P., Conrad, P. G., Des Marais, D. J., Dworkin, J. P., Fairén, A. G., François, P., Grotzinger, J. P., Kashyap, S., ten Kate, I. L., Leshin, L. A., Malespin, C. A., Martin, M. G., Martin-Torres, F. J., McAdam, A. C., Ming, D. W., Navarro-González, R., Pavlov, A. A., Prats, B. D., Squyres, S. W., Steele, A., Stern, J. C., Sumner, D. Y., Sutter, B., and Zorzano, M.-P.

Abstract

The Sample Analysis at Mars (SAM) instrument on board the Mars Science Laboratory Curiosity rover is designed to conduct inorganic and organic chemical analyses of the atmosphere and the surface regolith and rocks to help evaluate the past and present habitability potential of Mars at Gale Crater. Central to this task is the development of an inventory of any organic molecules present to elucidate processes associated with their origin, diagenesis, concentration, and long-term preservation. This will guide the future search for biosignatures. Here we report the definitive identification of chlorobenzene (150–300 parts per billion by weight (ppbw)) and C2 to C4 dichloroalkanes (up to 70 ppbw) with the SAM gas chromatograph mass spectrometer (GCMS) and detection of chlorobenzene in the direct evolved gas analysis (EGA) mode, in multiple portions of the fines from the Cumberland drill hole in the Sheepbed mudstone at Yellowknife Bay. When combined with GCMS and EGA data from multiple scooped and drilled samples, blank runs, and supporting laboratory analog studies, the elevated levels of chlorobenzene and the dichloroalkanes cannot be solely explained by instrument background sources known to be present in SAM. We conclude that these chlorinated hydrocarbons are the reaction products of Martian chlorine and organic carbon derived from Martian sources (e.g., igneous, hydrothermal, atmospheric, or biological) or exogenous sources such as meteorites, comets, or interplanetary dust particles.

Published
2017

61. Highlights from the Rover Environmental Monitoring Station (REMS) on Board the Mars Science Laboratory: New Windows for Atmospheric Research on Mars

Author

Martin-Torres, Javier, Zorzano, M.-P., Armiens, C., Carrasco, I., Delgado-Bonal, A., Genzer, M., Gómez, F., Gómez-Elvira, J., Haberle, R., Hamilton, V.E., Harri, A.-M., Kahanpää, H., Kemppinen, O., Lemmon, M.T., Lepinette, A., Soler, J. Martín, Martínez-Frías, J., Mischna, M., Mora, L., Navarro, S., Newman, C., de Pablo, M.A., Pla-García, J., Peinado, V., Polkko, J., and Vasavada, A.R.

Subjects
Rymd- och flygteknik, Aerospace Engineering
Abstract

Upprättat; 2014; 20150629 (ninhul)

Published
2014

62. Results from the Rover Environmental Monitoring Station (REMS) on Board the Mars Science Laboratory

Author

Mischna, M.A., Gómez-Elvira, J., Armiens, C., Carrasco, I., Genzer, M., Gómez, F., Haberle, R., Hamilton, V.E., Harri, A.-M., Kahanpää, H., Kemppinen, O., Lepinette, A., Soler, J. Martín, Martin-Torres, Javier, Martínez-Frías, J., Mora, L., Navarro, S., Newman, C., Pablo, M.A. de, Peinado, V., Polkko, J., Rafkin, S.C.R., Ramos, M., Rennó, N.O., Richardson, M., and Zorzano, M.-P.

Subjects
Rymd- och flygteknik, Aerospace Engineering
Abstract

Upprättat; 2014; 20150629 (ninhul)

Published
2014

63. Preliminary Interpretation of the Meteorological Environment Through Mars Science Laboratory Rover Environmental Monitoring Station Observations and Mesoscale Modeling

Author

Pla-García, J., Rafkin, S., Martin-Torres, Javier, Zorzano, M.-P., and Elvira-Gómez, J.

Subjects
Rymd- och flygteknik, Aerospace Engineering
Abstract

In this study the Mars Regional AtmosphericModeling System (MRAMS) has been applied to theGale Crater region, the landing site of the Mars ScienceLaboratory (MSL) Rover Curiosity. The landingsite is at one of the lowest elevations in Gale,between the crater rim and the ~4 km high centralmound known as Mt. Sharp. As Curiosity headstoward its long term target of Mt. Sharp, the meteorologicalconditions are expected to change due to theincreasing influence of topographically-inducedthermal circulations that have been predicted by numerousprevious studies [1, 2, 3, 4]. The types ofperturbations of pressure, air and ground temperatureand wind measured by the Rover EnvironmentalMonitoring Station (REMS) [5] have never beenobserved at other locations and these data provide agreat opportunity to test the models at the most meteorologicalinteresting area measured to date. Weprovide a comparison of MRAMS predictions (pressure,air temperature, winds and ground temperature)to the REMS data available at the location of theRover for sols 21-25 (when first regular REMSmeasurements were obtained, Ls=163), sols 51-55(Ls=180), sol 215 (Ls=270) and sols 348-352 (Ls=0),in order to provide a baseline of model performance. Upprättat; 2014; 20150602 (ninhul)

Published
2014

64. REMS Instrument Design and Operation Status : Monitoring the Environment from a Moving Hot Exploration Rover on Mars

Author

Zorzano, M.-P., Martin-Torres, Javier, Armiens, C., Carrasco, I., Genzer, M., Gómez, F., Gómez-Elvira, J., Haberle, R., Hamilton, V.E., Harri, A.-M., Kahanpää, H., Kemppinen, O., Lepinette, A., Soler, J. Martín, Martínez-Frías, J., Mischna, M., Mora, L., Navarro, S., Newman, C., Pablo, M.A. de, Pla, J., Peinado, V., Polkko, J., Rafkin, S.C.R., Ramos, M., and Vasavada, A.R.

Subjects
Rymd- och flygteknik, Aerospace Engineering
Abstract

Upprättat; 2014; 20150629 (ninhul)

Published
2014

65. Convective Vortices at the MSL Landing Site

Author

Kahanpää, H., Juarez, M. de la Torre, Moores, J., Rennó, N., Navarro, S., Haberle, R., Zorzano, M-P., Martin-Torres, Javier, Verdasca, J., Lepinette, A., Rodríguez-Manfredi, J.A., and Gomez-Elvira, J.

Subjects
Rymd- och flygteknik, Aerospace Engineering
Abstract

Upprättat; 2014; 20150603 (ninhul)

Published
2014

67. Organic molecules in the Sheepbed Mudstone, Gale Crater, Mars

Author

Freissinet, C., Glavin, D. P., Mahaffy, P. R., Miller, K. E., Eigenbrode, J. L., Summons, R. E., Brunner, A. E., Buch, A., Szopa, C., Archer, P. D., Franz, H. B., Atreya, S. K., Brinckerhoff, W. B., Cabane, M., Coll, P., Conrad, P. G., Des Marais, D. J., Dworkin, J. P., Fairén, A. G., François, P., Grotzinger, J. P., Kashyap, S., ten Kate, I. L., Leshin, L. A., Malespin, C. A., Martin, M. G., Martin-Torres, F. J., Mcadam, A. C., Ming, D. W., Navarro-González, R., Pavlov, A. A., Prats, B. D., Squyres, S. W., Steele, A., Stern, J. C., Sumner, D. Y., Sutter, B., Zorzano, M. P., the MSL Science Team, Freissinet, C., Glavin, D. P., Mahaffy, P. R., Miller, K. E., Eigenbrode, J. L., Summons, R. E., Brunner, A. E., Buch, A., Szopa, C., Archer, P. D., Franz, H. B., Atreya, S. K., Brinckerhoff, W. B., Cabane, M., Coll, P., Conrad, P. G., Des Marais, D. J., Dworkin, J. P., Fairén, A. G., François, P., Grotzinger, J. P., Kashyap, S., ten Kate, I. L., Leshin, L. A., Malespin, C. A., Martin, M. G., Martin-Torres, F. J., Mcadam, A. C., Ming, D. W., Navarro-González, R., Pavlov, A. A., Prats, B. D., Squyres, S. W., Steele, A., Stern, J. C., Sumner, D. Y., Sutter, B., Zorzano, M. P., and the MSL Science Team

Abstract

The Sample Analysis at Mars (SAM) instrument on board the Mars Science Laboratory Curiosity rover is designed to conduct inorganic and organic chemical analyses of the atmosphere and the surface regolith and rocks to help evaluate the past and present habitability potential of Mars at Gale Crater. Central to this task is the development of an inventory of any organic molecules present to elucidate processes associated with their origin, diagenesis, concentration, and long-term preservation. This will guide the future search for biosignatures. Here we report the definitive identification of chlorobenzene (150-300 parts per billion by weight (ppbw)) and C2 to C4 dichloroalkanes (up to 70ppbw) with the SAM gas chromatograph mass spectrometer (GCMS) and detection of chlorobenzene in the direct evolved gas analysis (EGA) mode, in multiple portions of the fines from the Cumberland drill hole in the Sheepbed mudstone at Yellowknife Bay. When combined with GCMS and EGA data from multiple scooped and drilled samples, blank runs, and supporting laboratory analog studies, the elevated levels of chlorobenzene and the dichloroalkanes cannot be solely explained by instrument background sources known to be present in SAM. We conclude that these chlorinated hydrocarbons are the reaction products of Martian chlorine and organic carbon derived from Martian sources (e.g., igneous, hydrothermal, atmospheric, or biological) or exogenous sources such as meteorites, comets, or interplanetary dust particles.

Published
2015

68. Organic molecules in the Sheepbed Mudstone, Gale Crater, Mars

Author

Petrology, Freissinet, C., Glavin, D. P., Mahaffy, P. R., Miller, K. E., Eigenbrode, J. L., Summons, R. E., Brunner, A. E., Buch, A., Szopa, C., Archer, P. D., Franz, H. B., Atreya, S. K., Brinckerhoff, W. B., Cabane, M., Coll, P., Conrad, P. G., Des Marais, D. J., Dworkin, J. P., Fairén, A. G., François, P., Grotzinger, J. P., Kashyap, S., ten Kate, I. L., Leshin, L. A., Malespin, C. A., Martin, M. G., Martin-Torres, F. J., Mcadam, A. C., Ming, D. W., Navarro-González, R., Pavlov, A. A., Prats, B. D., Squyres, S. W., Steele, A., Stern, J. C., Sumner, D. Y., Sutter, B., Zorzano, M. P., the MSL Science Team, Petrology, Freissinet, C., Glavin, D. P., Mahaffy, P. R., Miller, K. E., Eigenbrode, J. L., Summons, R. E., Brunner, A. E., Buch, A., Szopa, C., Archer, P. D., Franz, H. B., Atreya, S. K., Brinckerhoff, W. B., Cabane, M., Coll, P., Conrad, P. G., Des Marais, D. J., Dworkin, J. P., Fairén, A. G., François, P., Grotzinger, J. P., Kashyap, S., ten Kate, I. L., Leshin, L. A., Malespin, C. A., Martin, M. G., Martin-Torres, F. J., Mcadam, A. C., Ming, D. W., Navarro-González, R., Pavlov, A. A., Prats, B. D., Squyres, S. W., Steele, A., Stern, J. C., Sumner, D. Y., Sutter, B., Zorzano, M. P., and the MSL Science Team

Published
2015

69. Mars Science Laboratory relative humidity observations: Initial results

Author

Harri, A.‐M., primary, Genzer, M., additional, Kemppinen, O., additional, Gomez‐Elvira, J., additional, Haberle, R., additional, Polkko, J., additional, Savijärvi, H., additional, Rennó, N., additional, Rodriguez‐Manfredi, J. A., additional, Schmidt, W., additional, Richardson, M., additional, Siili, T., additional, Paton, M., additional, Torre‐Juarez, M. De La, additional, Mäkinen, T., additional, Newman, C., additional, Rafkin, S., additional, Mischna, M., additional, Merikallio, S., additional, Haukka, H., additional, Martin‐Torres, J., additional, Komu, M., additional, Zorzano, M.‐P., additional, Peinado, V., additional, Vazquez, L., additional, and Urqui, R., additional

Published
2014
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70. An Examination of Soil Crusts on the Floor of Jezero Crater, Mars

Author

Hausrath, E. M., Adcock, C. T., Bechtold, A., Beck, P., Benison, K., Brown, A., Cardarelli, E. L., Carman, N. A., Chide, B., Christian, J., Clark, B. C., Cloutis, E., Cousin, A., Forni, O., Gabriel, T. S. J., Gasnault, O., Golombek, M., Gómez, F., Hecht, M. H., Henley, T. L. J., Huidobro, J., Johnson, J., Jones, M. W. M., Kelemen, P., Knight, A., Lasue, J. A., Le Mouélic, S., Madariaga, J. M., Maki, J., Mandon, L., Martinez, G., Martínez‐Frías, J., McConnochie, T. H., Meslin, P.‐Y., Zorzano, M.‐P., Newsom, H., Paar, G., Randazzo, N., Royer, C., Siljeström, S., Schmidt, M. E., Schröder, S., Sephton, M. A., Sullivan, R., Turenne, N., Udry, A., VanBommel, S., Vaughan, A., Wiens, R. C., and Williams, N.

Abstract

Martian soils are critically important for understanding the history of Mars, past potentially habitable environments, returned samples, and future human exploration. This study examines soil crusts on the floor of Jezero crater encountered during initial phases of the Mars 2020 mission. Soil surface crusts have been observed on Mars at other locations, starting with the two Viking Lander missions. Rover observations show that soil crusts are also common across the floor of Jezero crater, revealed in 45 of 101 locations where rover wheels disturbed the soil surface, two out of seven helicopter flights that crossed the wheel tracks, and four of eight abrasion/drilling sites. Most soils measured by the SuperCam laser‐induced breakdown spectroscopy (LIBS) instrument show high hydrogen content at the surface, and fine‐grained soils also show a visible/near infrared (VISIR) 1.9 μm H2O absorption feature. The Planetary Instrument for X‐ray Lithochemistry (PIXL) and SuperCam observations suggest the presence of salts at the surface of rocks and soils. The correlation of S and Cl contents with H contents in SuperCam LIBS measurements suggests that the salts present are likely hydrated. On the “Naltsos” target, magnesium and sulfur are correlated in PIXL measurements, and Mg is tightly correlated with H at the SuperCam points, suggesting hydrated Mg‐sulfates. Mars Environmental Dynamics Analyzer (MEDA) observations indicate possible frost events and potential changes in the hydration of Mg‐sulfate salts. Jezero crater soil crusts may therefore form by salts that are hydrated by changes in relative humidity and frost events, cementing the soil surface together. Martian soils are important for understanding the history of Mars as well as future sample return and human exploration. Soil crusts in Jezero crater, which are also broadly found across Mars, can be observed when they are disturbed, such as by rover wheels or coring/abrasion activities. Jezero crater soil crusts are examined using images from the Perseverance and Ingenuity cameras, as well as using data from the SuperCam, PIXL, Mastcam‐Z, and MEDA instruments. Soil crusts are common in Jezero crater and show characteristics including hydration at the surface and the presence of salts that might contain water. MEDA instrument measurements indicate that changes in the hydration state of salts may result during conditions measured at Jezero crater. Jezero crater soil crusts may therefore form by salts that are present on the surface that can add or lose water during changes in relative atmospheric humidity and frost events. These changes in the amount of water present in the salts may result in soil surfaces that are cemented together, forming the crusts observed at Jezero crater. A better understanding of Mars soil crusts will help in the understanding of samples returned to Earth from Mars, as well as future human exploration. Soil crusts are prevalent across the Jezero crater floorSoil surfaces are largely hydratedSoil crusts likely contain salts and may form during changes in atmospheric relative humidity at the surface Soil crusts are prevalent across the Jezero crater floor Soil surfaces are largely hydrated Soil crusts likely contain salts and may form during changes in atmospheric relative humidity at the surface

Published
2023
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71. Intrabeam scattering and the coasting beam in the HERA proton ring

Author

Zorzano, M. P. and Wanzenberg, R.

Subjects
Physics::Accelerator Physics, High Energy Physics::Experiment, Accelerators and Storage Rings
Abstract

Undesired coasting beam of protons has been detected in the HERA proton ring in high energy storage operation. This mainly disturbs the operation of the HERA-B experiment, and can have some impact on H1 and ZEUS where it generates background spikes (depending also on the collimator settings). In this work we present a collection of data and facts, to be taken as starting point for further theoretical and experimental studies. We propose Intra Beam Scattering as a possible physical mechanism for creating the coasting beam and discuss the implications of this longitudinal dynamics model on observables such as the bunch length, energy spread, dc current and reaction rate at the HERA-B wires. The results seem to be in qualitative agreement with the measurements.

Published
2000
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73. Possible physical and thermodynamical evidence for liquid water at the Phoenix landing site

Author

Rennó, Nilton O., primary, Bos, Brent J., additional, Catling, David, additional, Clark, Benton C., additional, Drube, Line, additional, Fisher, David, additional, Goetz, Walter, additional, Hviid, Stubbe F., additional, Keller, Horst Uwe, additional, Kok, Jasper F., additional, Kounaves, Samuel P., additional, Leer, Kristoffer, additional, Lemmon, Mark, additional, Madsen, Morten Bo, additional, Markiewicz, Wojciech J., additional, Marshall, John, additional, McKay, Christopher, additional, Mehta, Manish, additional, Smith, Miles, additional, Zorzano, M. P., additional, Smith, Peter H., additional, Stoker, Carol, additional, and Young, Suzanne M. M., additional

Published
2009
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84. Fluids, evaporation and precipitates at Gale Crater

Author

Schwenzer, S. P., Bridges, J. C., Leveille, R., Wiens, R. C., Mangold, N., McAdam, A., Conrad, P., Kelley, S. P., Westall, F., Martín-Torres, F., and Zorzano, M.-P.

Abstract

The Mars Science Laboratory (MSL) mission landed in Gale Crater, Mars, on 6th August 2012, and has explored the Yellowknife Bay area. The detailed mineralogical and sedimentological studies provide a unique opportunity to characterise the secondary fluids associated with this habitable environment.

85. Martian Eolian Dust Analyzed by ChemCam

Author

Lasue, J., Cousin, A., Meslin, P. Y., Mangold, N., Wiens, R. C., Berger, G., Dehouck, E., Forni, O., Goetz, W., Gasnault, O., William Rapin, Schröder, S., Ollila, A., Johnson, J., Le Mouélic, S., Maurice, S., Anderson, R., Blaney, D., Clark, B., Clegg, S. M., Uston, C. D., Fabre, C., Lanza, N., Madsen, M. B., Martín-Torres, J., Melikechi, N., Newsom, H., Sautter, V., Zorzano, M. P., Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Institute of Meteoritics [Albuquerque] (IOM), and The University of New Mexico [Albuquerque]

Subjects
[SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology
Abstract

International audience; The martian eolian dust chemical composition is homogeneous at the sub-mm scale. It is different from the Aeolis Palus soils and Bagnold sands with a larger content of FeO, TiO2 and lower hydration.

86. The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter

Author

Korablev, O., Montmessin, F., Trokhimovskiy, A., Fedorova, A. A., Shakun, A. V., Grigoriev, A. V., Moshkin, B. E., Ignatiev, N. I., Forget, F., Lefèvre, F., Anufreychik, K., Dzuban, I., Ivanov, Y. S., Kalinnikov, Y. K., Kozlova, T. O., Kungurov, A., Makarov, V., Martynovich, F., Maslov, I., Merzlyakov, D., Moiseev, P. P., Nikolskiy, Y., Patrakeev, A., Patsaev, D., Santos-Skripko, A., Sazonov, O., Semena, N., Semenov, A., Shashkin, V., Sidorov, A., Stepanov, A. V., Stupin, I., Timonin, D., Titov, A. Y., Viktorov, A., Zharkov, A., Altieri, F., Arnold, G., Belyaev, D. A., Bertaux, J. L., Betsis, D. S., Duxbury, N., Encrenaz, T., Fouchet, T., Gérard, J.-C., Grassi, D., Guerlet, S., Hartogh, P., Kasaba, Y., Khatuntsev, I., Krasnopolsky, V. A., Kuzmin, R. O., Lellouch, E., Lopez-Valverde, M. A., Luginin, M., Määttänen, A., Marcq, E., Martin Torres, J., Medvedev, A. S., Millour, E., Olsen, K. S., Patel, M. R., Quantin-Nataf, C., Rodin, A. V., Shematovich, V. I., Thomas, I., Thomas, Nicolas, Vazquez, L., Vincendon, M., Wilquet, V., Wilson, C. F., Zasova, L. V., Zelenyi, L. M., and Zorzano, M. P.

Subjects
520 Astronomy, 620 Engineering, 7. Clean energy
Abstract

The Atmospheric Chemistry Suite (ACS) package is an element of the Russian contribution to the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission. ACS consists of three separate infrared spectrometers, sharing common mechanical, electrical, and thermal interfaces. This ensemble of spectrometers has been designed and developed in response to the Trace Gas Orbiter mission objectives that specifically address the requirement of high sensitivity instruments to enable the unambiguous detection of trace gases of potential geophysical or biological interest. For this reason, ACS embarks a set of instruments achieving simultaneously very high accuracy (ppt level), very high resolving power (>10,000) and large spectral coverage (0.7 to 17 μm—the visible to thermal infrared range). The near-infrared (NIR) channel is a versatile spectrometer covering the 0.7–1.6 μm spectral range with a resolving power of ~20,000. NIR employs the combination of an echelle grating with an AOTF (Acousto-Optical Tunable Filter) as diffraction order selector. This channel will be mainly operated in solar occultation and nadir, and can also perform limb observations. The scientific goals of NIR are the measurements of water vapor, aerosols, and dayside or night side airglows. The mid-infrared (MIR) channel is a cross-dispersion echelle instrument dedicated to solar occultation measurements in the 2.2–4.4 μm range. MIR achieves a resolving power of >50,000. It has been designed to accomplish the most sensitive measurements ever of the trace gases present in the Martian atmosphere. The thermal-infrared channel (TIRVIM) is a 2-inch double pendulum Fourier-transform spectrometer encompassing the spectral range of 1.7–17 μm with apodized resolution varying from 0.2 to 1.3 cm⁻¹. TIRVIM is primarily dedicated to profiling temperature from the surface up to ~60 km and to monitor aerosol abundance in nadir. TIRVIM also has a limb and solar occultation capability. The technical concept of the instrument, its accommodation on the spacecraft, the optical designs as well as some of the calibrations, and the expected performances for its three channels are described.

93. The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter

Author

Korablev, O., Montmessin, F., Trokhimovskiy, A., Fedorova, A. A., Shakun, A. V., Grigoriev, A. V., Moshkin, B. E., Ignatiev, N. I., Forget, F., Lefèvre, F., Anufreychik, K., Dzuban, I., Ivanov, Y. S., Kalinnikov, Y. K., Kozlova, T. O., Kungurov, A., Makarov, V., Martynovich, F., Maslov, I., Merzlyakov, D., Moiseev, P. P., Nikolskiy, Y., Patrakeev, A., Patsaev, D., Santos-Skripko, A., Sazonov, O., Semena, N., Semenov, A., Shashkin, V., Sidorov, A., Stepanov, A. V., Stupin, I., Timonin, D., Titov, A. Y., Viktorov, A., Zharkov, A., Altieri, F., Arnold, G., Belyaev, D. A., Bertaux, J. L., Betsis, D. S., Duxbury, N., Encrenaz, T., Fouchet, T., Gérard, J.-C., Grassi, D., Guerlet, S., Hartogh, P., Kasaba, Y., Khatuntsev, I., Krasnopolsky, V. A., Kuzmin, R. O., Lellouch, E., Lopez-Valverde, M. A., Luginin, M., Määttänen, A., Marcq, E., Martin Torres, J., Medvedev, A. S., Millour, E., Olsen, K. S., Patel, M. R., Quantin-Nataf, C., Rodin, A. V., Shematovich, V. I., Thomas, I., Thomas, N., Vazquez, L., Vincendon, M., Wilquet, V., Wilson, C. F., Zasova, L. V., Zelenyi, L. M., Zorzano, M. P., Korablev, O., Montmessin, F., Trokhimovskiy, A., Fedorova, A. A., Shakun, A. V., Grigoriev, A. V., Moshkin, B. E., Ignatiev, N. I., Forget, F., Lefèvre, F., Anufreychik, K., Dzuban, I., Ivanov, Y. S., Kalinnikov, Y. K., Kozlova, T. O., Kungurov, A., Makarov, V., Martynovich, F., Maslov, I., Merzlyakov, D., Moiseev, P. P., Nikolskiy, Y., Patrakeev, A., Patsaev, D., Santos-Skripko, A., Sazonov, O., Semena, N., Semenov, A., Shashkin, V., Sidorov, A., Stepanov, A. V., Stupin, I., Timonin, D., Titov, A. Y., Viktorov, A., Zharkov, A., Altieri, F., Arnold, G., Belyaev, D. A., Bertaux, J. L., Betsis, D. S., Duxbury, N., Encrenaz, T., Fouchet, T., Gérard, J.-C., Grassi, D., Guerlet, S., Hartogh, P., Kasaba, Y., Khatuntsev, I., Krasnopolsky, V. A., Kuzmin, R. O., Lellouch, E., Lopez-Valverde, M. A., Luginin, M., Määttänen, A., Marcq, E., Martin Torres, J., Medvedev, A. S., Millour, E., Olsen, K. S., Patel, M. R., Quantin-Nataf, C., Rodin, A. V., Shematovich, V. I., Thomas, I., Thomas, N., Vazquez, L., Vincendon, M., Wilquet, V., Wilson, C. F., Zasova, L. V., Zelenyi, L. M., and Zorzano, M. P.

Abstract

The Atmospheric Chemistry Suite (ACS) package is an element of the Russian contribution to the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission. ACS consists of three separate infrared spectrometers, sharing common mechanical, electrical, and thermal interfaces. This ensemble of spectrometers has been designed and developed in response to the Trace Gas Orbiter mission objectives that specifically address the requirement of high sensitivity instruments to enable the unambiguous detection of trace gases of potential geophysical or biological interest. For this reason, ACS embarks a set of instruments achieving simultaneously very high accuracy (ppt level), very high resolving power (>10,000) and large spectral coverage (0.7 to 17 μm—the visible to thermal infrared range). The near-infrared (NIR) channel is a versatile spectrometer covering the 0.7–1.6 μm spectral range with a resolving power of ∼20,000. NIR employs the combination of an echelle grating with an AOTF (Acousto-Optical Tunable Filter) as diffraction order selector. This channel will be mainly operated in solar occultation and nadir, and can also perform limb observations. The scientific goals of NIR are the measurements of water vapor, aerosols, and dayside or night side airglows. The mid-infrared (MIR) channel is a cross-dispersion echelle instrument dedicated to solar occultation measurements in the 2.2–4.4 μm range. MIR achieves a resolving power of >50,000. It has been designed to accomplish the most sensitive measurements ever of the trace gases present in the Martian atmosphere. The thermal-infrared channel (TIRVIM) is a 2-inch double pendulum Fourier-transform spectrometer encompassing the spectral range of 1.7–17 μm with apodized resolution varying from 0.2 to 1.3 cm−1. TIRVIM is primarily dedicated to profiling temperature from the surface up to ∼60 km and to monitor aerosol abundance in nadir. TIRVIM also has a limb and solar occultation capability. The technical concept of the instrum

94. The potential science and engineering value of samples delivered to Earth by Mars sample return

Author

Beaty, D. W., Grady, Monica, McSween, H. Y., Sefton-Nash, E., Carrier, B. L., Altieri, F., Amelin, Y., Ammannito, E., Anand, M., Benning, L. G., Bishop, J. L., Borg, L. E., Boucher, D., Brucato, J. R., Busemann, H., Campbell, K. A., Czaja, A. D., Debaille, V., Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, A. D., M. Hausrath, E., Herd, C. D. K., Horgan, B., Humanyun, M., Kleine, T., Kleinhenz, J., Mackelprang, R., Mangold, N., Mayhew, L. E., McCoy, J. T., McCubbin, F. M., McLennan, S. M., Moser, D. E., Moynier, F., Mustard, J. F., Niles, P. B., Ori, G. G., Raulin, F., Rettberg, P., Rucker, M. A., Schmitz, N., Schwenzer, S. P., Sephton, M. A., Shaheen, R., Sharp, Z. D., Schuster, D. L., Siljestrom, S., Smith, C. L., Spry, J. A., Steele, A., Swindle, T. D., ten Kate, I. L., Tosca, N. J., Usui, T., Van Kranendonk, M. J., Wadhwa, M., Weiss, B. P., Werner, S. C., Westall, F., Wheeler, R. M., Zipfel, J., Zorzano, M. P., Beaty, D. W., Grady, Monica, McSween, H. Y., Sefton-Nash, E., Carrier, B. L., Altieri, F., Amelin, Y., Ammannito, E., Anand, M., Benning, L. G., Bishop, J. L., Borg, L. E., Boucher, D., Brucato, J. R., Busemann, H., Campbell, K. A., Czaja, A. D., Debaille, V., Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, A. D., M. Hausrath, E., Herd, C. D. K., Horgan, B., Humanyun, M., Kleine, T., Kleinhenz, J., Mackelprang, R., Mangold, N., Mayhew, L. E., McCoy, J. T., McCubbin, F. M., McLennan, S. M., Moser, D. E., Moynier, F., Mustard, J. F., Niles, P. B., Ori, G. G., Raulin, F., Rettberg, P., Rucker, M. A., Schmitz, N., Schwenzer, S. P., Sephton, M. A., Shaheen, R., Sharp, Z. D., Schuster, D. L., Siljestrom, S., Smith, C. L., Spry, J. A., Steele, A., Swindle, T. D., ten Kate, I. L., Tosca, N. J., Usui, T., Van Kranendonk, M. J., Wadhwa, M., Weiss, B. P., Werner, S. C., Westall, F., Wheeler, R. M., Zipfel, J., and Zorzano, M. P.

95. Fluids during diagenesis and sulfate vein formation in sediments at Gale crater, Mars

Author

Schwenzer, S. P., Bridges, J. C., Wiens, R. C., Conrad, P. G., Kelley, S. P., Leveille, R., Mangold, N., Martin-Torres, J., McAdam, A., Newsom, H., Zorzano, M. P., Rapin, W., Spray, J., Treiman, A. H., Westall, F., Fairen, A. G., Meslin, P.-Y., Schwenzer, S. P., Bridges, J. C., Wiens, R. C., Conrad, P. G., Kelley, S. P., Leveille, R., Mangold, N., Martin-Torres, J., McAdam, A., Newsom, H., Zorzano, M. P., Rapin, W., Spray, J., Treiman, A. H., Westall, F., Fairen, A. G., and Meslin, P.-Y.

Abstract

We model the fluids involved in the alteration processes recorded in the Sheepbed Member mudstones of Yellowknife Bay (YKB), Gale crater, Mars, as revealed by the Mars Science Laboratory Curiosity rover investigations. We compare the Gale crater waters with fluids modeled for shergottites, nakhlites, and the ancient meteorite ALH 84001, as well as rocks analyzed by the Mars Exploration rovers, and with terrestrial ground and surface waters. The aqueous solution present during sediment alteration associated with phyllosilicate formation at Gale was high in Na, K, and Si; had low Mg, Fe, and Al concentrations—relative to terrestrial groundwaters such as the Deccan Traps and other modeled Mars fluids; and had near neutral to alkaline pH. Ca and S species were present in the 10−3 to 10−2 concentration range. A fluid local to Gale crater strata produced the alteration products observed by Curiosity and subsequent evaporation of this groundwater-type fluid formed impure sulfate- and silica-rich deposits—veins or horizons. In a second, separate stage of alteration, partial dissolution of this sulfate-rich layer in Yellowknife Bay, or beyond, led to the pure sulfate veins observed in YKB. This scenario is analogous to similar processes identified at a terrestrial site in Triassic sediments with gypsum veins of the Mercia Mudstone Group in Watchet Bay, UK.

96. Fluids, evaporation and precipitates at Gale Crater

Author

Schwenzer, S. P., Bridges, J. C., Leveille, R., Wiens, R. C., Mangold, N., McAdam, A., Conrad, P., Kelley, S. P., Westall, F., Martín-Torres, F., Zorzano, M.-P., Schwenzer, S. P., Bridges, J. C., Leveille, R., Wiens, R. C., Mangold, N., McAdam, A., Conrad, P., Kelley, S. P., Westall, F., Martín-Torres, F., and Zorzano, M.-P.

Abstract

The Mars Science Laboratory (MSL) mission landed in Gale Crater, Mars, on 6th August 2012, and has explored the Yellowknife Bay area. The detailed mineralogical and sedimentological studies provide a unique opportunity to characterise the secondary fluids associated with this habitable environment.

97. Report of the Science Community Workshop on the proposed First Sample Depot for the Mars Sample Return Campaign

Author

Czaja, A. D., Zorzano, M.‐P., Kminek, G., Meyer, M. A., Beaty, D. W., Sefton‐Nash, E., Carrier, B. L., Thiessen, F., Haltigin, T., Bouvier, A., Dauphas, N., French, K. L., Hallis, L. J., Harris, R. L., Hauber, E., Rodriguez, L. E., Schwenzer, S., Steele, A., Tait, K. T., Thorpe, M. T., Usui, T., Vanhomwegen, J., Velbel, M. A., Edwin, S., Farley, K. A., Glavin, D. P., Harrington, A. D., Hays, L. E., Hutzler, A., Wadhwa, M., Czaja, A. D., Zorzano, M.‐P., Kminek, G., Meyer, M. A., Beaty, D. W., Sefton‐Nash, E., Carrier, B. L., Thiessen, F., Haltigin, T., Bouvier, A., Dauphas, N., French, K. L., Hallis, L. J., Harris, R. L., Hauber, E., Rodriguez, L. E., Schwenzer, S., Steele, A., Tait, K. T., Thorpe, M. T., Usui, T., Vanhomwegen, J., Velbel, M. A., Edwin, S., Farley, K. A., Glavin, D. P., Harrington, A. D., Hays, L. E., Hutzler, A., and Wadhwa, M.

Abstract

The Mars 2020/Mars Sample Return (MSR) Sample Depot Science Community Workshop was held on September 28 and 30, 2022, to assess the Scientifically‐Return Worthy (SRW) value of the full collection of samples acquired by the rover Perseverance at Jezero Crater, and of a proposed subset of samples to be left as a First Depot at a location within Jezero Crater called Three Forks. The primary outcome of the workshop was that the community is in consensus on the following statement: The proposed set of ten sample tubes that includes seven rock samples, one regolith sample, one atmospheric sample, and one witness tube constitutes a SRW collection that: (1) represents the diversity of the explored region around the landing site, (2) covers partially or fully, in a balanced way, all of the International MSR Objectives and Samples Team scientific objectives that are applicable to Jezero Crater, and (3) the analyses of samples in this First Depot on Earth would be of fundamental importance, providing a substantial improvement in our understanding of Mars. At the conclusion of the meeting, there was overall community support for forming the First Depot as described at the workshop and placing it at the Three Forks site. The community also recognized that the diversity of the Rover Cache (the sample collection that remains on the rover after placing the First Depot) will significantly improve with the samples that are planned to be obtained in the future by the Perseverance rover and that the Rover Cache is the primary target for MSR to return to Earth.

98. The potential science and engineering value of samples delivered to Earth by Mars sample return

Author

Beaty, D. W., Grady, Monica, McSween, H. Y., Sefton-Nash, E., Carrier, B. L., Altieri, F., Amelin, Y., Ammannito, E., Anand, M., Benning, L. G., Bishop, J. L., Borg, L. E., Boucher, D., Brucato, J. R., Busemann, H., Campbell, K. A., Czaja, A. D., Debaille, V., Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, A. D., M. Hausrath, E., Herd, C. D. K., Horgan, B., Humanyun, M., Kleine, T., Kleinhenz, J., Mackelprang, R., Mangold, N., Mayhew, L. E., McCoy, J. T., McCubbin, F. M., McLennan, S. M., Moser, D. E., Moynier, F., Mustard, J. F., Niles, P. B., Ori, G. G., Raulin, F., Rettberg, P., Rucker, M. A., Schmitz, N., Schwenzer, S. P., Sephton, M. A., Shaheen, R., Sharp, Z. D., Schuster, D. L., Siljestrom, S., Smith, C. L., Spry, J. A., Steele, A., Swindle, T. D., ten Kate, I. L., Tosca, N. J., Usui, T., Van Kranendonk, M. J., Wadhwa, M., Weiss, B. P., Werner, S. C., Westall, F., Wheeler, R. M., Zipfel, J., Zorzano, M. P., Beaty, D. W., Grady, Monica, McSween, H. Y., Sefton-Nash, E., Carrier, B. L., Altieri, F., Amelin, Y., Ammannito, E., Anand, M., Benning, L. G., Bishop, J. L., Borg, L. E., Boucher, D., Brucato, J. R., Busemann, H., Campbell, K. A., Czaja, A. D., Debaille, V., Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, A. D., M. Hausrath, E., Herd, C. D. K., Horgan, B., Humanyun, M., Kleine, T., Kleinhenz, J., Mackelprang, R., Mangold, N., Mayhew, L. E., McCoy, J. T., McCubbin, F. M., McLennan, S. M., Moser, D. E., Moynier, F., Mustard, J. F., Niles, P. B., Ori, G. G., Raulin, F., Rettberg, P., Rucker, M. A., Schmitz, N., Schwenzer, S. P., Sephton, M. A., Shaheen, R., Sharp, Z. D., Schuster, D. L., Siljestrom, S., Smith, C. L., Spry, J. A., Steele, A., Swindle, T. D., ten Kate, I. L., Tosca, N. J., Usui, T., Van Kranendonk, M. J., Wadhwa, M., Weiss, B. P., Werner, S. C., Westall, F., Wheeler, R. M., Zipfel, J., and Zorzano, M. P.

99. Fluids during diagenesis and sulfate vein formation in sediments at Gale crater, Mars

Author

Schwenzer, S. P., Bridges, J. C., Wiens, R. C., Conrad, P. G., Kelley, S. P., Leveille, R., Mangold, N., Martin-Torres, J., McAdam, A., Newsom, H., Zorzano, M. P., Rapin, W., Spray, J., Treiman, A. H., Westall, F., Fairen, A. G., Meslin, P.-Y., Schwenzer, S. P., Bridges, J. C., Wiens, R. C., Conrad, P. G., Kelley, S. P., Leveille, R., Mangold, N., Martin-Torres, J., McAdam, A., Newsom, H., Zorzano, M. P., Rapin, W., Spray, J., Treiman, A. H., Westall, F., Fairen, A. G., and Meslin, P.-Y.

Abstract

We model the fluids involved in the alteration processes recorded in the Sheepbed Member mudstones of Yellowknife Bay (YKB), Gale crater, Mars, as revealed by the Mars Science Laboratory Curiosity rover investigations. We compare the Gale crater waters with fluids modeled for shergottites, nakhlites, and the ancient meteorite ALH 84001, as well as rocks analyzed by the Mars Exploration rovers, and with terrestrial ground and surface waters. The aqueous solution present during sediment alteration associated with phyllosilicate formation at Gale was high in Na, K, and Si; had low Mg, Fe, and Al concentrations—relative to terrestrial groundwaters such as the Deccan Traps and other modeled Mars fluids; and had near neutral to alkaline pH. Ca and S species were present in the 10−3 to 10−2 concentration range. A fluid local to Gale crater strata produced the alteration products observed by Curiosity and subsequent evaporation of this groundwater-type fluid formed impure sulfate- and silica-rich deposits—veins or horizons. In a second, separate stage of alteration, partial dissolution of this sulfate-rich layer in Yellowknife Bay, or beyond, led to the pure sulfate veins observed in YKB. This scenario is analogous to similar processes identified at a terrestrial site in Triassic sediments with gypsum veins of the Mercia Mudstone Group in Watchet Bay, UK.

100. Fluids, evaporation and precipitates at Gale Crater

Author

Schwenzer, S. P., Bridges, J. C., Leveille, R., Wiens, R. C., Mangold, N., McAdam, A., Conrad, P., Kelley, S. P., Westall, F., Martín-Torres, F., Zorzano, M.-P., Schwenzer, S. P., Bridges, J. C., Leveille, R., Wiens, R. C., Mangold, N., McAdam, A., Conrad, P., Kelley, S. P., Westall, F., Martín-Torres, F., and Zorzano, M.-P.

Abstract

The Mars Science Laboratory (MSL) mission landed in Gale Crater, Mars, on 6th August 2012, and has explored the Yellowknife Bay area. The detailed mineralogical and sedimentological studies provide a unique opportunity to characterise the secondary fluids associated with this habitable environment.

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