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Space Science Reviews, Pre-Landing Insight Issue, January 25, 2018

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Space Scien ce Reviews Geology and Physical Properties Investigations by the InSight Lander --Manuscript Draft-- Manuscript Number: SPAC-D-18-00006R1 Full Title: Geology and Physical Properties Investigations by the InSight Lander Article Type: Vol xxx: InSight 2 Keywords: InSight Mars Geology Physical Properties Surface materials Corresponding Author: Matthew Golombek, Ph.D. Jet Propulsion Laboratory Pasadena, CA UNITED STATES Corresponding Author Secondary Information: Corresponding Author's Institution: Jet Propulsion Laboratory Corresponding Author's Secondary Institution: First Author: Matthew Golombek, Ph.D. First Author Secondary Information: Order of Authors: Matthew Golombek, Ph.D. Matthias Grott Gunter Kargl Jose Andrade Jason Marshall Nicholas Warner Nicholas Teanby Veronique Ansan Ernst Hauber J. Voigt Roy Lichtenheldt Brigitte Knapmeyer-Endrun Ingrid Daubar Devin Kipp Nils Muller Philippe Lognonné Cedric Schmelzbach Don Banfield Ashitey Trebi-Ollennu Justin Maki Sharon Kedar Powered by Editorial Manager® and ProduXion Manager® from Aries Systems Corporation David Mimoun Naomi Murdoch Sylvain Piqueux Pierre Delage William T. Pike Constantinos Charalambous Ralph Lorenz Lucile Fayon Antoine Lucas Sebastien Rodriguez Paul Morgan Aymeric Spiga Mark Panning Tilman Spohn Suzanne Smrekar Tamara Gudkova Raphael Garcia Domenico Giardini U. Christensen T. Nicollier D. Sollberger Johan Robertsson Khaled Ali Balthasar Kenda W. B. Banerdt Order of Authors Secondary Information: Funding Information: Agence Nationale de la Recherche (FR) Philippe Lognonné Institut Universitaire de France Aymeric Spiga Landmark University Grant Program Cedric Schmelzbach National Aeronautics and Space Dr. Matthew Golombek Administration CNES Philippe Lognonné UnivEarthS Labex program Philippe Lognonné UK Space Agency Nicholas Teanby ETH Research Grant Cedric Schmelzbach Abstract: Although not the prime focus of the InSight mission, the near-surface geology and physical properties investigations provide critical information for both placing the instruments (seismometer and heat flow probe with mole) on the surface and for understanding the nature of the shallow subsurface and its effect on recorded seismic waves. Two color cameras on the lander will obtain multiple stereo images of the surface and its interaction with the spacecraft. Images will be used to identify the geologic materials and features present, quantify their areal coverage, help determine the basic geologic evolution of the area, and provide ground truth for orbital remote Powered by Editorial Manager® and ProduXion Manager® from Aries Systems Corporation sensing data. A radiometer will measure the hourly temperature of the surface in two spots, which will determine the thermal inertia of the surface materials present and their particle size and/or cohesion. Continuous measurements of wind speed and direction offer a unique opportunity to correlate dust devils and high winds with eolian changes imaged at the surface and to determine the threshold friction wind stress for grain motion on Mars. During the first two weeks after landing, these investigations will support the selection of instrument placement locations that are relatively smooth, flat, free of small rocks and load bearing. Soil mechanics parameters and elastic properties of near surface materials will be determined from mole penetration and thermal conductivity measurements from the surface to 3-5 m depth, the measurement of seismic waves during mole hammering, passive monitoring of seismic waves, and experiments with the arm and scoop of the lander (indentations, scraping and trenching). These investigations will determine and test the presence and mechanical properties of the expected 3-17 m thick fragmented regolith (and underlying fractured material) built up by impact and eolian processes on top of Hesperian lava flows and determine its seismic properties for the seismic investigation of Mars' interior. Powered by Editorial Manager® and ProduXion Manager® from Aries Systems Corporation Manuscript Click here to download Manuscript InSight Geology Phys Prop Invest v.6.docx Click here to view linked References Geology and Physical Properties Investigations by the InSight Lander M. Golombek1, M. Grott2, G. Kargl3, J. Andrade4, J. Marshall4, N. Warner5, N. A. Teanby6, V. Ansan7, E. Hauber2, J. Voigt2, R. Lichtenheldt8, B. Knapmeyer-Endrun9, I. J. Daubar1, D. Kipp1, N. Muller1, P. Lognonné10, C. Schmelzbach11, D. Banfield12, A. Trebi-Ollennu1, J. Maki1, S. Kedar1, D. Mimoun13, N. Murdoch13, S. Piqueux1, P. Delage14, W. T. Pike15, C. Charalambous15, R. Lorenz16, L. Fayon10, A. Lucas10, S. Rodriguez10, P. Morgan17, A. Spiga18,19, M. Panning1, T. Spohn2, S. Smrekar1, T. Gudkova20, R. Garcia13, D. Giardini11, U. Christensen9, T. Nicollier11, D. Sollberger11, J. Robertsson11, K. Ali1, B. Kenda10, W. B. Banerdt1 1Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 2DLR, Institute of Planetary Research, Berlin 3Space Research Institute, Austrian Academy of Sciences 4Mechanical and Civil Engineering, California Institute of Technology, Pasadena, CA 5SUNY Geneseo 6School of Earth Sciences, University of Bristol, Wills Memorial Building, Queens Road, Bristol, BS8 1RJ, UK 7Laboratoire de Planétologie et Géodynamique, CNRS URM6112, Université de Nantes, Nantes, France 8DLR, Institute of System Dynamics and Control, Oberpfaffenhofen 9Max Planck Institute for Solar System Research, Göttingen, Germany 10Institut de Physique du Globe de Paris 11ETH Swiss Federal Institute of Technology, Zurich, Switzerland 12420 Space Sciences, Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY, 14853 13Institut Supérieur de l’Aéronautique et de l’Espace (ISAE-SUPAERO), Université de Toulouse, 31400 Toulouse, France 14École des Ponts Paris Tech 15Imperial College, London 16Johns Hopkins University Applied Physics Lab 17Colorado School of Mines 18Laboratoire de Météorologie Dynamique (LMD/IPSL), Sorbonne Université, Centre National de la Recherche Scientifique, École Normale Supérieure, École Polytechnique, Paris, France 19Institut Universitaire de France, Paris, France 20Schmidt Institute of Physics of the Earth v. 6, Revised May 9, 2018 First Submitted to Space Science Reviews, Pre-landing InSight Issue, January 25, 2018 1 Abstract Although not the prime focus of the InSight mission, the near-surface geology and physical properties investigations provide critical information for both placing the instruments (seismometer and heat flow probe with mole) on the surface and for understanding the nature of the shallow subsurface and its effect on recorded seismic waves. Two color cameras on the lander will obtain multiple stereo images of the surface and its interaction with the spacecraft. Images will be used to identify the geologic materials and features present, quantify their areal coverage, help determine the basic geologic evolution of the area, and provide ground truth for orbital remote sensing data. A radiometer will measure the hourly temperature of the surface in two spots, which will determine the thermal inertia of the surface materials present and their particle size and/or cohesion. Continuous measurements of wind speed and direction offer a unique opportunity to correlate dust devils and high winds with eolian changes imaged at the surface and to determine the threshold friction wind stress for grain motion on Mars. During the first two weeks after landing, these investigations will support the selection of instrument placement locations that are relatively smooth, flat, free of small rocks and load bearing. Soil mechanics parameters and elastic properties of near surface materials will be determined from mole penetration and thermal conductivity measurements from the surface to 3-5 m depth, the measurement of seismic waves during mole hammering, passive monitoring of seismic waves, and experiments with the arm and scoop of the lander (indentations, scraping and trenching). These investigations will determine and test the presence and mechanical properties of the expected 3-17 m thick fragmented regolith (and underlying fractured material) built up by impact and eolian processes on top of Hesperian lava flows and determine its seismic properties for the seismic investigation of Mars’ interior. 2 1. Introduction The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission is a Discovery Program lander to investigate the internal structure of Mars and the differentiation of the terrestrial planets (Banerdt et al. 2018). The spacecraft carries a seismometer (SEIS, Lognonné et al. 2018) with a Wind and Thermal Shield (WTS), heat flow probe (Heat Flow and Physical Properties Package, HP3, Spohn et al. 2018) and a precision tracking system (Rotation and Interior Structure Experiment, RISE, Folkner et al. 2018) to measure the size and state of the core, mantle and crust. The lander is designed to operate on the surface for one Mars year after landing (November 2018), listening for marsquakes and impacts, measuring heat flow (including the sub-surface and surface temperature), and tracking the precession and nutation of the spin axis. The spacecraft is based on the Phoenix (PHX) lander and consists of a cruise stage, aeroshell, and backshell. It will land on smooth plains below -2.5 km elevation (for entry, descent and landing) and between 3°-5°N latitude (for solar power and thermal management) in western Elysium Planitia, which also satisfies
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  • Mars Global Simulant MGS-1: a Rocknest-Based Open Standard For

    Mars Global Simulant MGS-1: a Rocknest-Based Open Standard For

    1 Mars Global Simulant MGS-1: A Rocknest-based open standard for 2 basaltic martian regolith simulants 3 Kevin M. Cannon1,*, Daniel T .Britt1, Trent M. Smith2, Ralph F. Fritsche2, and Daniel 4 Batcheldor3 5 1University of Central Florida, Department of Physics, Orlando, Florida 32816 6 2NASA Kennedy Space Center, Titusville, FL 32899 7 3Florida Institute of Technology, Melbourne, FL 32901 8 *Corresponding author: [email protected] 9 4111 Libra Drive 10 Physical Sciences Building 430 11 Orlando, FL 32816 12 13 14 15 16 17 18 19 20 21 22 23 24 Abstract 25 The composition and physical properties of martian regolith are dramatically 26 better understood compared to just a decade ago, particularly through the use of X-ray 27 diffraction by the Curiosity rover. Because there are no samples of this material on Earth, 28 researchers and engineers rely on terrestrial simulants to test future hardware and address 29 fundamental science and engineering questions. Even with eventual sample return, the 30 amount of material brought back would not be enough for bulk studies. However, many 31 of the existing regolith simulants were designed 10 or 20 years ago based on a more 32 rudimentary understanding of martian surface materials. Here, we describe the Mars 33 Global Simulant (MGS-1), a new open standard designed as a high fidelity mineralogical 34 analog to global basaltic regolith on Mars, as represented by the Rocknest windblown 35 deposit at Gale crater. We developed prototype simulants using the MGS-1 standard and 36 characterized them with imaging techniques, bulk chemistry, spectroscopy, and 37 thermogravimetric analysis.