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16 results on '"Balthasar Kenda"'

1. Transient convection experiments in internally-heated systems

Author: Angela Limare, Vasile Surducan, Balthasar Kenda, Emanoil Surducan, Edouard Kaminski, and Camelia Neamtu
Subjects: Convection, Materials science, Science, Clinical Biochemistry, Prandtl number, 010501 environmental sciences, Viscous liquid, 01 natural sciences, Scaling law, Physics::Fluid Dynamics, 03 medical and health sciences, symbols.namesake, Laser induced fluorescence, Thermal, Scaling for the transient regime of internally-heated convection systems, 030304 developmental biology, 0105 earth and related environmental sciences, Thermochromic liquid crystals, 0303 health sciences, Runge-Kutta integration, Time evolution, Rayleigh number, Mechanics, Method Article, 3D temperature field, Medical Laboratory Technology, Volume (thermodynamics), symbols, Internal heating
Abstract: Radioactive decay of unstable isotopes is one of the main heat sources in the early stages of planetary formation as well as in the mantle of terrestrial planets. Laboratory studies characterized by Rayleigh and Prandtl numbers in the range relevant for planetary bodies had remained beyond the ability of the experimental approach until the development of a new technique based on microwave heating. Using this technique, we performed a series of experiments focused on the thermal evolution of an internally heated viscous fluid cooled from above. We established a steady-state scaling law relying the internal temperature variation to the Rayleigh number and we showed that this scaling law remains valid during the transitory regime provided both internal heating and secular evolution of the temperature are taken into account. The result is a parameterized model describing the average internal temperature of the fluid as a function of time in terms of experimental conditions and fluid properties.•We generated a uniform and stable volume heat source in a large volume tank, based on absorption of microwaves guided through an innovative design of microwave circuits.•Automatic laser scanning of the tank coupled with image acquisition and processing enables us the measurement of the 3D temperature field in the convective fluid from which we extracted the volume average temperature and surface heat flux evolution in time.•We validated a transient scaling law for the time evolution of the volume average temperature in an internally-heated convective system., Graphical abstract Image, graphical abstract
Published: 2021

2. Early accretion of planetesimals unraveled by the thermal evolution of the parent bodies of magmatic iron meteorites

Author: Balthasar Kenda, Marc Chaussidon, Edouard Kaminski, Angela Limare, Institut de Physique du Globe de Paris (IPGP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), and Tellus/PNP program of INSU-CNRS IdEx project Universite de Paris ANR-18-IDEX-0001 ANR-11-IS04-0004
Subjects: Convection, Planetesimal, 010504 meteorology & atmospheric sciences, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Astrophysics, 010502 geochemistry & geophysics, Protoplanetary disk, 01 natural sciences, Parent body, analog experiments, accretion, Geochemistry and Petrology, Chondrite, Gravitational collapse, Earth and Planetary Sciences (miscellaneous), planetesimals, ComputingMilieux_MISCELLANEOUS, convection, 0105 earth and related environmental sciences, Accretion (astrophysics), Geophysics, Meteorite, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Geology, magmatic iron meteorites
Abstract: The timing of formation of 100-300 km size planetesimals in the protoplanetary disk remains largely unconstrained. Recent models show that gravitational collapse of boulders in overdense regions of a dusty accretion disk can overcome the meter-sized barrier and lead to rapid formation of planetesimals with size of several km that further grow by pebble accretion. Hf/W ages indicate that the first large planetesimals to form could be the parent bodies of magmatic iron meteorites. These ages have been so far used to constrain timing of accretion considering (i) instantaneous accretion, and (ii) purely conductive heat transfer in the planetesimal. To relax these hypotheses we model the thermal evolution of a planetesimal in course of accretion and we take into account the possibility of convection onset. Our model is further based on considering the possibility of a common thermal evolution for all the parent bodies of iron meteorites. Within that framework we show that the planetesimals could have grown following a universal accretion law starting at the very beginning of the history of the disk by a nearly instantaneous formation of 60 ± 30 km size nuclei, followed by a growth via pebble accretion at a much slower pace to reach final sizes of 150–300 km in about 3 Myr. In this universal scenario, complete melting and total differentiation are not bound to happen in the parent body due to the continuous accretion of cold pebbles. The model, though calibrated here on iron meteorites, is general and can in principle be applied to other types of planetesimals such as for instance the parent bodies of CV chondrites.
Published: 2020
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3. Polarized ambient noise on Mars

Author: A. Jacob, Simon Stähler, Balthasar Kenda, Anna Horleston, John Clinton, Raphaël F. Garcia, Constantinos Charalambous, Philippe Lognonné, Martin Schimmel, Taichi Kawamura, Ludovic Margerin, K. Hurst, Lucie fayon, Eléonore Stutzmann, Aymeric Spiga, T. Pike, William B. Banerdt, Naomi Murdoch, Mélanie Drilleau, Marie Calvet, John-Robert Scholz, Savas Ceylan, Domenico Giardini, Mark P. Panning, and Martin van Driel
Subjects: Seismometer, 010504 meteorology & atmospheric sciences, Ambient noise level, Mars Exploration Program, Seismic noise, 01 natural sciences, Seismology, Geology, Noise (radio), 0105 earth and related environmental sciences
Abstract: Seismic noise recorded at the surface of Mars has been monitored since February 2019, using the seismometers of the InSight lander. The noise on Mars is 500 times lower than on Earth at ni...
Published: 2020
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4. Subsurface Structure at the InSight Landing Site From Compliance Measurements by Seismic and Meteorological Experiments

Author: Naomi Murdoch, David Mimoun, Mélanie Drilleau, Balthasar Kenda, Aymeric Spiga, Veronique Ansan, Philippe Lognonné, Nicolas Compaire, Raphaël F. Garcia, Ulrich R. Christensen, Antoine Mocquet, R. Widmer-Schnidrig, Daniele Antonangeli, Christos Vrettos, Don Banfield, Sebastien Rodriguez, Pierre Delage, Tilman Spohn, William B. Banerdt, Taichi Kawamura, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), ANR-14-CE36-0012,SEISMARS,Seismology on Mars(2014), ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019), ANR-10-LABX-0023,UnivEarthS,Earth - Planets - Universe: observation, modeling, transfer(2010), ANR-11-IDEX-0005,USPC,Université Sorbonne Paris Cité(2011), Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), Institut de Physique du Globe de Paris (IPG Paris), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), 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-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), University of Stuttgart, École des Ponts ParisTech (ENPC), Technical University of Kaiserslautern (TU Kaiserslautern), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Cornell University [New York], Muséum national d'Histoire naturelle (MNHN), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, German Aerospace Center (DLR), Laboratoire Navier (NAVIER UMR 8205), École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Université Gustave Eiffel, Université d'Angers (UA)-Université de Nantes - Faculté des Sciences et des Techniques, and Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)
Subjects: 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Compaction, Young's modulus, regolith, subsurface, 01 natural sciences, Regolith, compliance, symbols.namesake, [SPI]Engineering Sciences [physics], inversion, [PHYS.MECA.STRU]Physics [physics]/Mechanics [physics]/Structural mechanics [physics.class-ph], Autre, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Surface response, Traitement du signal et de l'image, Young modulus, Subsurface, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, InSight, [SPI.GCIV.GEOTECH]Engineering Sciences [physics]/Civil Engineering/Géotechnique, Inversion, Markov chain Monte Carlo, Inversion (meteorology), [SPI.GCIV]Engineering Sciences [physics]/Civil Engineering, Geophysics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], symbols, Mars seismology, Geology, Seismology, Compliance
Abstract: International audience; Key Points: 28 • Ground compliance measurements by InSight depend on the elastic properties in 29 the near surface of Mars 30 • Observed compliance from convective vortex encounters and other pressure fluc-31 tuations opens the way to the exploration of the near surface 32 • Markov chain Monte Carlo inversion for the Young modulus profile suggests strat-33 ification within and below the regolith 34 Corresponding author: Balthasar Kenda, kenda@ipgp.fr-1-Abstract 35 Measurements of ground compliance at the InSight landing site-describing the surface 36 response to pressure loading-are obtained from seismic and meteorological data. Com-37 pliance observations show an increase with frequency indicating the presence of a stiffer 38 rock layer beneath the exposed regolith. We performed a Markov chain Monte Carlo in-39 version to investigate the vertical profile of the elastic parameters down to 20 m below 40 InSight. Compliance was inverted both freely and assuming prior knowledge of compaction 41 in the regolith, and the limitations and strengths of the methods were assessed on the 42 basis of theoretical considerations and synthetic tests. The inverted Young modulus ex-43 hibits an increase by a factor of 10-100 over the first 10-15 meters, compatible with a struc-44 tural discontinuity between 0.7 and 7 m. The proposed scheme can be used for joint in-45 version of other seismic, geological or mechanical constraints to refine the resulting ver-46 tical section. 47 Plain Language Summary 48 Pressure fluctuations of the Mars' atmosphere induce tiny deformations of the ground 49 that can be measured by the very sensitive seismometer of the InSight mission. The amount 50 of deformation depends on the elastic properties of the sandy regolith (the surface layer 51 exposed and highly fractured by impacts) and of the underlying rocks, and can thus be 52 used to explore beneath the surface. In this work, we review the theory describing the 53 ground motion caused by moving pressure perturbations, and we analyze the effect of 54 various parameters (wind speed, layering in the subsurface). We then develop a method 55 to retrieve a vertical profile of the elastic parameters beneath the lander from the mea-56 surements. After testing the method on ideal cases, we apply it to data from Mars: the 57 results show that the regolith becomes stiffer with depth, and that a layer of harder rock 58 may be present below, with the interface possibly located between 0.7 and 7 depth. De-59 termining the structure of the near surface provides constraints on the geologic history 60 of the landing site and contributes to the explanation of measured seismic signals.
Published: 2020
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5. Seismic investigations of the Martian near-surface at the InSight landing site

Author: W. Tom Pike, Naomi Murdoch, Domenico Giardini, Matthias Grott, Philippe Lognonné, Simon Stähler, Johan O. A. Robertsson, David Sollberger, Tilman Spohn, Mellanie Drilleau, Nienke Brinkman, Cedric Schmelzbach, Balthasar Kenda, Fredrik Andersson, Troy L. Hudson, Raphaël F. Garcia, K. Hurst, Jan ten Pierick, Martin van Driel, and Sharon Kedar
Subjects: Martian, Seismometer, Planetenphysik, Planet, Institut für Planetenforschung, Martian surface, Thermal, Mars Exploration Program, Geophysics, Induced seismicity, Regolith, InSight Mars HP3 SEIS, Geology
Abstract: The InSight ultra-sensitive broadband seismometer package (SEIS) was installed on the Martian surface with the goal to study the seismicity on Mars and the deep interior of the Planet. A second surface-based instrument, the heat flow and physical properties package HP3, was placed on the Martian ground about 1.1 m away from SEIS. HP3 includes a self-hammering probe called the ‘mole’ to measure the heat coming from Mars' interior at shallow depth to reveal the planet's thermal history. While SEIS was designed to study the deep structure of Mars, seismic signals such as the hammering ‘noise’ as well as ambient and other instrument-generated vibrations allow us to investigate the shallow subsurface. The resultant near-surface elastic property models provide additional information to interpret the SEIS data and allow extracting unique geotechnical information on the Martian regolith.The seismic signals recorded during HP3 mole operations provide information about the mole attitude and health as well as shed light on the near-surface, despite the fact that the HP3 mole continues to have difficulty penetrating below 40 cm (one mole length). The seismic investigation of the HP3 hammering signals, however, was not originally planned during mission design and hence faced several technical challenges. For example, the anti-aliasing filters of the seismic-data acquisition chain were adapted when recording the mole hammering to allow recovering information above the nominal Nyquist frequency. In addition, the independently operating SEIS, HP3 and lander clocks had to be correlated more frequently than in normal operation to enable high-precision timing.To date, the analysis of the hammering signals allowed us to constrain the bulk P-wave velocity of the volume between the mole tip and SEIS (top 30 cm) to around 120 m/s. This low velocity value is compatible with laboratory tests performed on Martian regolith analogs with a density of around 1500 kg/m3. Furthermore, the SEIS leveling system resonances, seismic recordings of atmospheric pressure signals, HP3 housekeeping data, and imagery provide additional constraints to establish a first seismic model of the shallow (topmost meters) subsurface at the landing site.
Published: 2020
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6. Pressure effects on SEIS-INSIGHT instrument, improvement of seismic records and characterization of gravity waves from ground displacements

Author: Rudolf Widmer-Schnidrig, Naomi Murdoch, Nicolas Compaire, Philippe Lognonné, Don Banfield, Balthasar Kenda, Williams Bruce Banerdt, Mélanie Drilleau, Guenolé Orhand-Mainsant, Raphaël F. Garcia, Aymeric Spiga, and Taichi Kawamura
Subjects: Gravitational wave, Geology, Seismology, Characterization (materials science)
Abstract: Mars atmospheric pressure variations induce ground displacements through elastic deformations. The various sensors of INSIGHT mission were designed in order to be able to understand and correct these ground deformations induced by atmospheric effects. Particular efforts were done on one side to avoid direct pressure and wind effects on the seismometer, and on the other side to have a high performance pressure sensor operating in the same frequency range than the seismometer.As a consequence of the high performances of both instruments, their very efficient protection systems against direct atmospheric disturbances, and the low Mars background seismic noise, INSIGHT mission is opening a new science domain for which the ground displacements can be used to perform atmospheric science.This study presents an analysis of pressure and seismic signals and their relations. After a short description of the pressure and seismic sensors deployed by INSIGHT, we present an analysis of these signals as a function of local time at INSIGHT location.Then, the background and event like coherent signals between Pressure and seismometer sensors are interpreted in terms of various atmospheric excitations and induced ground deformation processes. Different methods to remove the pressure effects recorded by SEIS sensors are presented, and their efficiency is estimated. Finally, we demonstrate that the pressure and ground deformations measurements can be used to decipher between various atmospheric excitation types (meteorological pressure variations, acoustic and gravity waves) and characterize these. Effects of the local sub-surface structure are also suggested by the data analysis.
Published: 2020
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7. MSS/1: Single-Station and Single-Event Marsquake Inversion

Author: Henri Samuel, Taichi Kawamura, Suzanne E. Smrekar, Philippe Lognonné, Brigitte Knapmeyer-Endrun, Balthasar Kenda, Eléonore Stutzmann, Eric Beucler, Martin Schimmel, Amir Khan, Sabrina Menina, Attilio Rivoldini, W. Bruce Banerdt, Martin van Driel, Simon Stähler, Mickael Bonnin, John Clinton, Domenico Giardini, Saikiran Tharimena, Rakshit Joshi, Savas Ceylan, Benoit Tauzin, Mélanie Drilleau, Vedran Lekic, Mark P. Panning, Caroline Beghein, Naomi Murdoch, Antoine Mocquet, Haotian Xu, California Institute of Technology, National Aeronautics and Space Administration (US), National Supercomputing Center of Tianjin, Swiss National Science Foundation, NASA Jet Propulsion Laboratory, Schimmel, Martin [0000-0003-2601-4462], Centre National de la Recherche Scientifique (CNRS), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Schimmel, Martin, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), ANR-14-CE36-0012,SEISMARS,Seismology on Mars(2014), ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019), ANR-10-LABX-0023,UnivEarthS,Earth - Planets - Universe: observation, modeling, transfer(2010), ANR-11-IDEX-0005,USPC,Université Sorbonne Paris Cité(2011), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Department of Geological Sciences [Gainesville] (UF|Geological), University of Florida [Gainesville] (UF), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Swiss Fed Inst Technol, Inst Geophys, Sonneggstr 5, CH-8092 Zurich, Switzerland, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: 010504 meteorology & atmospheric sciences, Panning, InSight, Inversion, Seismology, Model validationone-dimensional modeling, É, 010502 geochemistry & geophysics, 01 natural sciences, Lognonné, M, lcsh:QB1-991, Performance assessment, Autre, et al. (2020). MSS/1: Single-station and single-event marsquake inversion. Earth and Space Science. 7, Seismic velocity, ComputingMilieux_MISCELLANEOUS, P, lcsh:QE1-996.5, Mars Exploration Program, Geodesy, Surface wave, M. P, [SDU.OTHER]Sciences of the Universe [physics]/Other, Geology, Algorithms, Seismometer, W. B, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], lcsh:Astronomy, Seismograph, Mars, Environmental Science (miscellaneous), Induced seismicity, Synthetic data, Knapmeyer-Endrun, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, 0105 earth and related environmental sciences, Drilleau, e2020EA001118, Seismicity, Crust, Inversion (meteorology), Arrival time, Great circle, lcsh:Geology, B, Banerdt, 13. Climate action, [SDU]Sciences of the Universe [physics], General Earth and Planetary Sciences, Beucler, Mantle
Abstract: SEIS, the seismometer of the InSight mission, which landed on Mars on 26 November 2018, is monitoring the seismic activity of the planet. The goal of the Mars Structure Service (MSS) is to provide, as a mission product, the first average 1-D velocity model of Mars from the recorded InSight data. Prior to the mission, methodologies have been developed and tested to allow the location of the seismic events and estimation of the radial structure, using surface waves and body waves arrival times, and receiver functions. The paper describes these validation tests and compares the performance of the different algorithms to constrain the velocity model below the InSight station and estimate the 1-D average model over the great circle path between source and receiver. These tests were performed in the frame of a blind test, during which synthetic data were inverted. In order to propagate the data uncertainties on the output model distribution, Bayesian inversion techniques are mainly used. The limitations and strengths of the methods are assessed. The results show the potential of the MSS approach to retrieve the structure of the crust and underlying mantle. However, at this time, large quakes with clear surface waves have not yet been recorded by SEIS, which makes the estimation of the 1-D average seismic velocity model challenging. Additional locatable events, especially at large epicentral distances, and development of new techniques to fully investigate the data, will ultimately provide more constraints on the crust and mantle of Mars. ©2020 The Authors., Xu and Beghein were funded by NASA InSight PSP Grant 80NSSC18K1679. M. P. P., W. B. B., S. E. S., and S. T. were supported the NASA InSight mission and funds from the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The French authors acknowledge the French Space Agency CNES as well as CNRS and the French team universities for personal and infrastructure supports. The development of the MSS and associated software was provided by ANR (ANR‐14‐CE36‐0012‐02 and ANR‐19‐CE31‐0008‐08) and, for IPGP team, by UnivEarthS Labex program (ANR‐10‐LABX‐0023), IDEX Sorbonne Paris Cit (ANR‐11‐IDEX‐0005‐0). M1a and M2b models computation used HPC resources of CINES under the allocation A0050407341 and A0070407341 attributed by GENCI (Grand Equipement National de Calcul Intensif). M1b model is computed at the Centre de calcul des pays de la Loire (ccipl). This is InSight Contribution Number 141 and IPGP Contribution 4104. M. v. D. and S. C. S. were supported by a grant from the Swiss National Science Foundation (SNF‐ANR Project 157133 Seismology on Mars) and the Swiss National Supercomputing Center (CSCS) under Project ID sm682. A. K. and D. G. would like to acknowledge support from the Swiss National Science Foundation (SNF‐ANR project 172508 Mapping the internal structure of Mars).
Published: 2020
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8. The atmosphere of Mars as observed by InSight

Author: Justin N. Maki, A. Jacob, Stephen R. Lewis, Nicholas A Teanby, Mercedes Marin-Jimenez, Anna Mittelholz, Constantinos Charalambous, Sara Navarro, M. M. Baker, Mark T. Lemmon, Tristram Warren, Javier Gómez-Elvira, Alexander E. Stott, Matthew P. Golombek, Antoine Lucas, Jorge Pla-Garcia, J. Torres, Eric Beucler, Balthasar Kenda, Aymeric Spiga, Rudolf Widmer-Schnidrig, Philippe Lognonné, Veronique Ansan, V. Peinado, Özgür Karatekin, William T. Pike, Nils Mueller, Savas Ceylan, K. Hurst, Daniel Viúdez-Moreiras, Christopher T. Russell, Antonio Molina, Sebastien Rodriguez, Clément Perrin, Naomi Murdoch, David Mimoun, Claire E. Newman, Ralph D. Lorenz, L. Martire, Luis Mora-Sotomayor, Simon Stähler, Tilman Spohn, Lucie Rolland, Stephen Sackett, Ingrid Daubar, Raphaël F. Garcia, W. Bruce Banerdt, Catherine L. Johnson, Domenico Giardini, Brian Carcich, Don Banfield, Suzanne E. Smrekar, John Clinton, François Forget, Ehouarn Millour, Taichi Kawamura, J. A. Rodríguez-Manfredi, Bart Van Hove, A. Lepinette, Anni Määttänen, J. B. McClean, Cornell Center for Astrophysics and Planetary Science (CCAPS), Cornell University, 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), Aeolis Research, Space Science Institute [Boulder] (SSI), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Royal Observatory of Belgium [Brussels], School of Earth Sciences [Bristol], University of Bristol [Bristol], Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Department of Electrical and Electronic Engineering [London] (DEEE), Imperial College London, Department of Earth, Ocean and Atmospheric Sciences [Vancouver] (EOAS), University of British Columbia (UBC), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Sorbonne Université (SU), School of Physical Sciences [Milton Keynes], The Open University [Milton Keynes] (OU), Swiss Seismological Service [ETH Zurich] (SED), Institute of Geophysics [ETH Zürich], Department of Earth Sciences [ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Department of Earth Sciences [ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Department of Physics [Oxford], University of Oxford [Oxford], Department of Earth, Environmental and Planetary Sciences [Providence], Brown University, Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Université Côte d'Azur (UCA), Universität Stuttgart [Stuttgart], Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Morton K. Blaustein Department of Earth and Planetary Sciences [Baltimore], Johns Hopkins University (JHU), Center for Earth and Planetary Studies [Washington] (CEPS), Smithsonian National Air and Space Museum, Smithsonian Institution-Smithsonian Institution, Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), University of California-University of California, Département Electronique, Optronique et Signal (DEOS), Cornell University [New York], 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), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Royal Observatory of Belgium [Brussels] (ROB), NASA-California Institute of Technology (CALTECH), Department of Earth, Ocean and Atmospheric Sciences [Vancouver] (UBC EOAS), 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), Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)-Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), 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), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), University of Oxford, University of California (UC)-University of California (UC), ANR-14-CE36-0012,SEISMARS,Seismology on Mars(2014), ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Määttänen, A. [0000-0002-7326-8492], Martire, L. [0000-0002-9402-6150], Rodríguez Manfredi, J. A. [0000-0003-0461-9815], Lognonné, P. [0000-0002-1014-920X], Rodríguez, S. [0000-0003-1219-0641], Spiga, A. [0000-0002-6776-6268], Perrin, C. [0000-0002-7200-5682], Molina, A. [0000-0002-5038-2022], García, R. [0000-0003-1460-6663], Murdoch, N. [0000-0002-9701-4075], Lorenz, R. [0000-0001-8528-4644], Mittelholz, A. [0000-0002-5603-7334], Kawamura, T. [0000-0001-5246-5561], Widmer Schnidrig, R. [0000-0001-9698-2739], McClean, J. [0000-0002-7863-0120], Mueller, N. [0000-0001-9229-8921], Lewis, S. [0000-0001-7237-6494], Teanby, N. [0000-0003-3108-5775], Warren, T. [0000-0003-3877-0046], Milliour, E. [0000-0003-4808-9203], Lemmon, M. [0000-0002-4504-5136], Clinton, J. [0000-0001-8626-2703], Ceylan, S. [0000-0002-6552-6850], Banfield, D. [0000-0003-2664-0164], Agence Nationale de la Recherche (ANR), and Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)
Subjects: Martian, 010504 meteorology & atmospheric sciences, Atmosphere, Mars, Mars Exploration Program, Atmosphere of Mars, 010502 geochemistry & geophysics, Mars Atmosphere, 01 natural sciences, Wind speed, Astrobiology, Autre, 13. Climate action, Dust storm, [SDU]Sciences of the Universe [physics], General Earth and Planetary Sciences, Environmental science, Aeolian processes, [SDU.OTHER]Sciences of the Universe [physics]/Other, Meteorologie, InSight mission, Dust devil, 0105 earth and related environmental sciences, InSight
Abstract: Banfield, D. et al., The atmosphere of Mars is thin, although rich in dust aerosols, and covers a dry surface. As such, Mars provides an opportunity to expand our knowledge of atmospheres beyond that attainable from the atmosphere of the Earth. The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) lander is measuring Mars’s atmosphere with unprecedented continuity, accuracy and sampling frequency. Here we show that InSight unveils new atmospheric phenomena at Mars, especially in the higher-frequency range, and extends our understanding of Mars’s meteorology at all scales. InSight is uniquely sensitive to large-scale and regional weather and obtained detailed in situ coverage of a regional dust storm on Mars. Images have enabled high-altitude wind speeds to be measured and revealed airglow—faint emissions produced by photochemical reactions—in the middle atmosphere. InSight observations show a paradox of aeolian science on Mars: despite having the largest recorded Martian vortex activity and dust-devil tracks close to the lander, no visible dust devils have been seen. Meteorological measurements have produced a catalogue of atmospheric gravity waves, which included bores (soliton-like waves). From these measurements, we have discovered Martian infrasound and unexpected similarities between atmospheric turbulence on Earth and Mars. We suggest that the observations of Mars’s atmosphere by InSight will be key for prediction capabilities and future exploration., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737); Centro de Desarrollo Tecnológico e Industrial (CDTI), Ministerio de Economía y Competitividad and the Instituto Nacional de Técnica Aeroespacial (INTA).
Published: 2020
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9. Preparing for InSight: Evaluation of the Blind Test for Martian Seismicity

Author: Franziska Mehrkens, Lucie Rolland, Claudia Haindl, Christoph Schröer, Andre Lamert, Ingrid Daubar, Jiaxuan Li, Katharina Grunert, David Ambrois, Marc S. Boxberg, Thomas Möller, Paul Neumann, Harriet Godwin, Mélanie Drilleau, Raphaël F. Garcia, Sarah Mader, Martin van Driel, Mark P. Panning, Sharon Kedar, Titus Casademont, Matthew P. Golombek, Domenico Giardini, Amir Allam, Bruce Banerdt, Jérôme Chèze, Diego Mercerat, Simon Stähler, Dirk Becker, Lorenz Marten, Hector Alemany, John Clinton, Philippe Lognonné, Eléonore Stutzmann, Savas Ceylan, Balthasar Kenda, Isabell Hochfeld, Kasra Hosseini, Hao Hu, Fabrice Peix, David Essing, Fabian Dethof, T. Garth, Benjamin Fernando, Aymeric Spiga, Robert Neurath, Fabian Euchner, Shane Zhang, Tabea Kilchling, Julien Balestra, Nienke Brinkman, Marcel Paffrath, Brigitte Knapmeyer-Endrun, Martin Schimmel, Maren Böse, Yingcai Zheng, Manuel Ditz, Cedric Twardzik, Alexandre Szenicer, Céline Hadziioannou, Naomi Murdoch, Renee Weber, Anne Deschamps, David Mimoun, René Steinmann, Noah Trumpik, Philipp Werdenbach‐Jarklowski, Maria Tsekhmistrenko, Amir Khan, Conny Hammer, Ludovic Perrin, Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Centre d'Etudes et d'Expertise sur les Risques, l'Environnement, la Mobilité et l'Aménagement - Equipe-projet MOUVGS (Cerema Equipe-projet MOUVGS), Centre d'Etudes et d'Expertise sur les Risques, l'Environnement, la Mobilité et l'Aménagement (Cerema), INSIGHT, Swiss National Science Foundation, Centre National D'Etudes Spatiales (France), Swiss National Supercomputing Centre, Schimmel, Martin, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Centre National d'Études Spatiales [Toulouse] (CNES), 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), 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), Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), and Schimmel, Martin [0000-0003-2601-4462]
Subjects: Seismometer, Outreach, 010504 meteorology & atmospheric sciences, Computer science, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Location, Polarization analysis, Mars, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Mission, Induced seismicity, 010502 geochemistry & geophysics, 01 natural sciences, 7. Clean energy, Synthetic data, Autre, Models, Single-station, Blind test, Seismology, 0105 earth and related environmental sciences, Quake (natural phenomenon), Martian, Fault zone, Inversion, Single station, Mars Exploration Program, Data science, Geophysics, 13. Climate action, [SDU]Sciences of the Universe [physics], Seismograms, Insight, Noise
Abstract: In December 2018, the National Aeronautics and Space Administration (NASA) Interior exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) mission deployed a seismometer on the surface of Mars. In preparation for the data analysis, in July 2017, the marsquake service initiated a blind test in which participants were asked to detect and characterize seismicity embedded in a one Earth year long synthetic data set of continuous waveforms. Synthetic data were computed for a single station, mimicking the streams that will be available from InSight as well as the expected tectonic and impact seismicity, and noise conditions on Mars (Clinton et al., 2017). In total, 84 teams from 20 countries registered for the blind test and 11 of them submitted their results in early 2018. The collection of documentations, methods, ideas, and codes submitted by the participants exceeds 100 pages. The teams proposed well established as well as novel methods to tackle the challenging target of building a global seismicity catalog using a single station. This article summarizes the performance of the teams and highlights the most successful contributions., This work was jointly funded by Swiss National Science Foundation and French Agence Nationale de la Recherche (SNF-ANR project 157133 "Seismology on Mars"); Swiss State Secretariat for Education, Research and Innovation (project "MarsQuake Service-Preparatory Phase"); and ETH Zurich (project "Preparatory phase for Mars InSight Ground Segment Support"). Additional support came from the Swiss National Supercomputing Centre (CSCS) under Project ID s682. Some of the research described in this article was supported by the Interior exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) project, Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). The Houston team was partially funded by EAR-1621878. A. Spiga and L. Rolland acknowledge funding by Centre National d'Etudes Spatiales (CNES). This article constitutes InSight Contribution Number 93.
Published: 2019
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10. Impact-Seismic Investigations of the InSight Mission

Author: Foivos Karakostas, James Wookey, Jennifer Stevanović, Matthew P. Golombek, Philippe Lognonné, Veronique Ansan, W. Bruce Banerdt, Stéphane May, Antoine Lucas, Maria E. Banks, Mark P. Panning, Nicholas Schmerr, Jeremie Vaubaillon, Sharon Kedar, Sebastien Rodriguez, Mélanie Drilleau, Nicholas A Teanby, Eleanor K. Sansom, Justin N. Maki, James E. Richardson, Taichi Kawamura, C. Yana, John Clinton, Maren Böse, Mark T. Lemmon, Ingrid Daubar, Gareth S. Collins, Raphaël F. Garcia, Balthasar Kenda, Hiroo Kanamori, Nobuaki Fuji, Katarina Miljković, Simon Stähler, Suzanne E. Smrekar, Don Banfield, Tamara Gudkova, Martin van Driel, Institut de Physique du Globe de Paris (IPGP), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), and Science and Technology Facilities Council (STFC)
Subjects: Seismometer, 010504 meteorology & atmospheric sciences, Mars, Astronomy & Astrophysics, 01 natural sciences, Autre, Impact crater, 0103 physical sciences, 010303 astronomy & astrophysics, Seismology, 0105 earth and related environmental sciences, InSight, Physical model, Astronomy and Astrophysics, Acoustic wave, Mars Exploration Program, Atmosphere of Mars, 0201 Astronomical And Space Sciences, Planetary science, Amplitude, 13. Climate action, Space and Planetary Science, Impact cratering, [SDU.OTHER]Sciences of the Universe [physics]/Other, Geology
Abstract: Impact investigations will be an important aspect of the InSight mission. One of the scientific goals of the mission is a measurement of the current impact rate at Mars. Impacts will additionally inform the major goal of investigating the interior structure of Mars. In this paper, we review the current state of knowledge about seismic signals from impacts on the Earth, Moon, and laboratory experiments. We describe the generalized physical models that can be used to explain these signals. A discussion of the appropriate source time function for impacts is presented, along with spectral characteristics including the cutoff frequency and its dependence on impact momentum. Estimates of the seismic efficiency (ratio between seismic and impact energies) vary widely. Our preferred value for the seismic efficiency at Mars is $5 \times 10^{- 4}$ , which we recommend using until we can measure it during the InSight mission, when seismic moments are not used directly. Effects of the material properties at the impact point and at the seismometer location are considered. We also discuss the processes by which airbursts and acoustic waves emanate from bolides, and the feasibility of detecting such signals. We then consider the case of impacts on Mars. A review is given of the current knowledge of present-day cratering on Mars: the current impact rate, characteristics of those impactors such as velocity and directions, and the morphologies of the craters those impactors create. Several methods of scaling crater size to impact energy are presented. The Martian atmosphere, although thin, will cause fragmentation of impactors, with implications for the resulting seismic signals. We also benchmark several different seismic modeling codes to be used in analysis of impact detections, and those codes are used to explore the seismic amplitude of impact-induced signals as a function of distance from the impact site. We predict a measurement of the current impact flux will be possible within the timeframe of the prime mission (one Mars year) with the detection of ∼ a few to several tens of impacts. However, the error bars on these predictions are large. Specific to the InSight mission, we list discriminators of seismic signals from impacts that will be used to distinguish them from marsquakes. We describe the role of the InSight Impacts Science Theme Group during mission operations, including a plan for possible night-time meteor imaging. The impacts detected by these methods during the InSight mission will be used to improve interior structure models, measure the seismic efficiency, and calculate the size frequency distribution of current impacts.
Published: 2018
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11. Influence of body waves, instrumentation resonances, and prior assumptions on Rayleigh wave ellipticity inversion for shallow structure at the InSight landing site

Author: Martin Knapmeyer, Balthasar Kenda, William B. Banerdt, Philippe Lognonné, Sharon Kedar, Lars Witte, Naomi Murdoch, Matthew P. Golombek, Nicolas Verdier, Brigitte Knapmeyer-Endrun, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Département Electronique, Optronique et Signal (DEOS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Institut de Physique du Globe de Paris (IPGP), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), DLR Institute of Planetary Research, German Aerospace Center (DLR), DLR Institute of Space Systems, Centre National d'Études Spatiales [Toulouse] (CNES), Centre National d'Études Spatiales - CNES (FRANCE), Institut de Physique du Globe de Paris - IPGP (FRANCE), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Max Planck Society (GERMANY), California Institute of Technology - Caltech (USA), DLR Institute of Planetary Research (GERMANY), DLR Institute of Space Systems (GERMANY), Département d'Electronique, Optronique et Signal - DEOS (Toulouse, France), and Jet Propulsion Laboratory - JPL (Pasadena, USA)
Subjects: [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Mars, Seismic noise, 010502 geochemistry & geophysics, 01 natural sciences, 7. Clean energy, Regolith, Spectral line, symbols.namesake, Interior, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, 0103 physical sciences, Rayleigh wave, Rayleigh waves, Automatique / Robotique, 010303 astronomy & astrophysics, Scaling, Seismology, 0105 earth and related environmental sciences, InSight, Levelling, Astronomy and Astrophysics, Mars Exploration Program, Computational physics, Amplitude, Space and Planetary Science, symbols, Rayleigh Waves, Geology
Abstract: International audience; Based on an updated model of the regolith’s elastic properties, we simulate the ambient vibrations background wavefield recorded by InSight’s Seismic Experiment for Interior Structure (SEIS) on Mars to characterise the influence of the regolith and invert SEIS data for shallow subsurface structure. By approximately scaling the synthetics based on seismic signals of a terrestrial dust devil, we find that the high-frequency atmospheric background wavefield should be above the self-noise of SEIS’s SP sensors, even if the signals are not produced within 100–200 m of the station. We compare horizontal-to-vertical spectral ratios and Rayleigh wave ellipticity curves for a surface-wave based simulation on the one hand with synthetics explicitly considering body waves on the other hand and do not find any striking differences. Inverting the data, we find that the results are insensitive to assumptions on density. By contrast, assumptions on the velocity range in the upper-most layer have a strong influence on the results also at larger depth. Wrong assumptions can lead to results far from the true model in this case. Additional information on the general shape of the curve, i.e. single or dual peak, could help to mitigate this effect, even if it cannot directly be included into the inversion. We find that the ellipticity curves can provide stronger constraints on the minimum thickness and velocity of the second layer of the model than on the maximum values. We also consider the effect of instrumentation resonances caused by the lander flexible modes, solar panels, and the SEIS levelling system. Both the levelling system resonances and the lander flexible modes occur at significantly higher frequencies than the expected structural response, i.e. above 35 Hz and 20 Hz, respectively. While the lander and solar panel resonances might be too weak in amplitude to be recorded by SEIS, the levelling system resonances will show up clearly in horizontal spectra, the H/V and ellipticity curves. They are not removed by trying to extract only Rayleigh-wave dominated parts of the data. However, they can be distinguished from any subsurface response by their exceptionally low damping ratios of 1% or less as determined by random decrement analysis. The same applies to lander-generated signals observed in actual data from a Moon analogue experiment, so we expect this analysis will be useful in identifying instrumentation resonances in SEIS data.
Published: 2018
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12. VAMOS: a SmallSat mission concept for remote sensing of Venusian seismic activity from orbit

Author: Brian M. Sutin, Jörn Helbert, James A. Cutts, Barry Nakazono, Mélanie Drilleau, Balthasar Kenda, Philippe Lognonné, M. Grawe, Mayer Rud, Jonathan J. Makela, Mark Wallace, Ashley Karp, Gregory Lantoine, Siddharth Krishnamoorthy, Attila Komjathy, and Alan Didion
Subjects: Solar System, biology, Spacecraft, business.industry, Airglow, Venus, NASA Deep Space Network, biology.organism_classification, Astrobiology, law.invention, Orbiter, Planetary science, law, Ionosphere, business, Geology, Earthquakes Electric propulsion Infrared imaging Interplanetary spacecraft Ionosphere Orbits Remote sensing Spacecraft propulsion Tectonics
Abstract: The apparent youthfulness of Venus’ surface features, given a lack of plate tectonics, is very intriguing; however, longduration seismic observations are essentially impossible given the inhospitable surface of Venus. The Venus Airglow Measurements and Orbiter for Seismicity (VAMOS) mission concept uses the fact that the dense Venusian atmosphere conducts seismic vibrations from the surface to the airglow layer of the ionosphere, as observed on Earth. Similarly, atmospheric gravity waves have been observed by the European Venus Express’s Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) instrument. Such observations would enable VAMOS to determine the crustal structure and ionospheric variability of Venus without approaching the surface or atmosphere. Equipped with an instrument of modest size and mass, the baseline VAMOS spacecraft is designed to fit within an ESPA Grande form factor and travel to Venus predominantly under its own power. Trade studies have been conducted to determine mission architecture robustness to launch and rideshare opportunities. The VAMOS mission concept was studied at JPL as part of the NASA Planetary Science Deep Space SmallSat Studies (PSDS3) program, which has not only produced a viable and exciting mission concept for a Venus SmallSat, but has also examined many issues facing the development of SmallSats for planetary exploration, such as SmallSat solar electric propulsion, autonomy, telecommunications, and resource management that can be applied to various inner solar system mission architectures.
Published: 2018
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13. Remote sensing of venusian seismic activity with a small spacecraft, the VAMOS mission concept

Author: Philippe Lognonné, Mélanie Drilleau, M. Grawe, Brian M. Sutin, Balthasar Kenda, Attila Komjathy, Jonathan J. Makela, Jörn Helbert, Mayer Rud, Gregory Lantoine, Mark Wallace, Ashley C. Karp, Siddharth Krishnamoorthy, Alan Didion, James A. Cutts, and Barry Nakazono
Subjects: 010504 meteorology & atmospheric sciences, Ion thruster, Spacecraft, biology, business.industry, Airglow, Venus, NASA Deep Space Network, biology.organism_classification, 01 natural sciences, law.invention, remote sensing, Orbiter, Planetary science, Planet, law, 0103 physical sciences, tectonics, business, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences, Remote sensing
Abstract: The Venusian atmosphere creates inhospitable temperature and pressure conditions for the surface of Venus, Earth's twin planet, making in-situ measurements of any appreciable length difficult, expensive, and risky to obtain. Yet, because of the apparent youthfulness of Venus' surface features, long-duration seismic observations are in high demand in order to determine and understand the dynamic processes taking place in lieu of plate tectonics. The Venus Airglow Measurements and Orbiter for Seismicity (VAMOS) mission concept would make use of the dense Venusian atmosphere as a medium to conduct seismic vibrations from the surface to the ionosphere. Here, the resulting atmospheric gravity waves and acoustic waves can be observed in the form of perturbations in airglow emissions, the basic principles for which have been demonstrated at Earth following a tsunami and at Venus with the European Venus Express's Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) instrument. In addition, these observations would enable VAMOS to determine the crustal structure and ionospheric variability of Venus without approaching the surface or atmosphere themselves. Equipped with an instrument of modest size and mass, the baseline VAMOS spacecraft is designed to fit within a SmallSat form factor and travel to Venus predominantly under its own power. VAMOS would enter into an orbit uniquely suited for the long-duration, full-disk staring observations required for seismic readings. VAMOS' journey would be enabled by modern solar electric propulsion technology and SmallSat avionics, which allow the spacecraft to reach Venus and autonomously filter observation data on board to detect Venus-quake events. Currently, trade studies are being conducted to determine mission architecture robustness to launch and rideshare opportunities. Key spacecraft challenges for VAMOS, just as with many SmallSat-based mission concepts, include thermal and power management, onboard processing capabilities, telecommunications throughput, and propulsion technology. The VAMOS mission concept is being studied at JPL as part of the NASA Planetary Science Deep Space SmallSat Studies (PSDS3) program, which will not only produce a viable and exciting mission concept for a Venus SmallSat, but will have the opportunity to examine many issues facing the development of SmallSats for planetary exploration. These include SmallSat solar electric propulsion, autonomy, telecommunications, and resource management that can be applied to various inner solar system mission architectures.
Published: 2018
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14. Modeling of Ground Deformation and Shallow Surface Waves Generated by Martian Dust Devils and Perspectives for Near-Surface Structure Inversion

Author: Aymeric Spiga, William B. Banerdt, Ralph D. Lorenz, Don Banfield, Sharon Kedar, Matthew P. Golombek, Taichi Kawamura, Philippe Lognonné, Balthasar Kenda, Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, 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)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, CALTECH, Jet Prop Lab, M-S 321-B60,4800 Oak Grove Dr, Pasadena, CA 91109 USA, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Cornell University [New York], Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), and NASA-California Institute of Technology (CALTECH)
Subjects: Seismometer, 010504 meteorology & atmospheric sciences, MOTION, Author Keywords:Dust devils, FREQUENCY, 01 natural sciences, Physics::Geophysics, NOISE, RATIO, Large-eddy simulation, SEISMIC SIGNALS, Ground tilt, 0103 physical sciences, Subsurface, LARGE-EDDY SIMULATIONS, 010303 astronomy & astrophysics, Dust devil, 0105 earth and related environmental sciences, Remote sensing, Martian, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], MARS, Astronomy and Astrophysics, Geophysics, Mars Exploration Program, WIND, Regolith, Vortex, INFRASOUND, 13. Climate action, Space and Planetary Science, Surface wave, [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, Noise (radio), Geology, Insight KeyWords Plus:CONVECTIVE BOUNDARY-LAYER
Abstract: International audience; We investigated the possible seismic signatures of dust devils on Mars, both at long and short period, based on the analysis of Earth data and on forward modeling for Mars. Seismic and meteorological data collected in the Mojave Desert, California, recorded the signals generated by dust devils. In the 10-100 s band, the quasi-static surface deformation triggered by pressure fluctuations resulted in detectable ground-tilt effects: these are in good agreement with our modeling based on Sorrells' theory. In addition, high-frequency records also exhibit a significant excitation in correspondence to dust devil episodes. Besides wind noise, this signal includes shallow surface waves due to the atmosphere-surface coupling and is used for a preliminary inversion of the near-surface S-wave profile down to 50 m depth. In the case of Mars, we modeled the long-period signals generated by the pressure field resulting from turbulence-resolving Large-Eddy Simulations. For typical dust-devil-like vortices with pressure drops of a couple Pascals, the corresponding horizontal acceleration is of a few nm/s(2) for rocky subsurface models and reaches 10-20 nm/s(2) for weak regolith models. In both cases, this signal can be detected by the Very-Broad Band seismometers of the InSight/SEIS experiment up to a distance of a few hundred meters from the vortex, the amplitude of the signal decreasing as the inverse of the distance. Atmospheric vortices are thus expected to be detected at the InSight landing site; the analysis of their seismic and atmospheric signals could lead to additional constraints on the near-surface structure, more precisely on the ground compliance and possibly on the seismic velocities
Published: 2017
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15. Estimations of the Seismic Pressure Noise on Mars Determined from Large Eddy Simulations and Demonstration of Pressure Decorrelation Techniques for the Insight Mission

Author: Taichi Kawamura, Balthasar Kenda, Philippe Lognonné, Aymeric Spiga, William B. Banerdt, Naomi Murdoch, David Mimoun, Centre National de la Recherche Scientifique - CNRS (FRANCE), Institut de Physique du Globe de Paris - IPGP (FRANCE), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), National Aeronautics and Space Administration - NASA (USA), Université de Paris Diderot - Paris 7 (FRANCE), Université Pierre et Marie Curie, Paris 6 - UPMC (FRANCE), Université de La Réunion (FRANCE), California Institute of Technology - Caltech (USA), Ecole Normale Supérieure de Paris - ENS Paris (FRANCE), Ecole Polytechnique (FRANCE), Ecole des Ponts ParisTech (FRANCE), Institut national des sciences de l'Univers - INSU (FRANCE), Département Electronique, Optronique et Signal (DEOS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, 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)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), and École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris)
Subjects: Seismometer, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Mars, Surface pressure, 01 natural sciences, Regolith, Physics::Geophysics, Physics - Geophysics, 0103 physical sciences, Pressure, 010303 astronomy & astrophysics, Decorrelation, Astrophysique, Seismology, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Atmospheric pressure, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Atmosphere, Astronomy and Astrophysics, Mars Exploration Program, Geodesy, Pressure sensor, Geophysics (physics.geo-ph), Physics - Atmospheric and Oceanic Physics, Amplitude, Geophysics, 13. Climate action, Space and Planetary Science, Atmospheric and Oceanic Physics (physics.ao-ph), Geology, Noise (radio), Astrophysics - Earth and Planetary Astrophysics
Abstract: International audience; The atmospheric pressure fluctuations on Mars induce an elastic response in the ground that creates a ground tilt, detectable as a seismic signal on the InSight seismometer SEIS. The seismic pressure noise is modeled using Large Eddy Simulations (LES) of the wind and surface pressure at the InSight landing site and a Green’s function ground deformation approach that is subsequently validated via a detailed comparison with two other methods: a spectral approach, and an approach based on Sorrells’ theory (Sorrells,Geophys. J. Int. 26:71–82, 1971; Sorrells et al., Nat. Phys. Sci. 229:14–16, 1971). The horizontal accelerations as a result of the ground tilt due to the LES turbulence-induced pressure fluctuations are found to be typically ∼ 2–40 nm/s2 in amplitude, whereas the direct horizontal acceleration is two orders of magnitude smaller and is thus negligible in comparison. The vertical accelerations are found to be ∼ 0.1–6 nm/s2 in amplitude. These are expected to be worst-case estimates for the seismic noise as we use a half-space approximation; the presence at some (shallow) depth of a harder layer would significantly reduce quasi-static displacement and tilt effects. We show that under calm conditions, a single-pressure measurement is representative of the large-scale pressure field (to a distance of several kilometers), particularly in the prevailing wind direction. However, during windy conditions, small-scale turbulence results in a reduced correlation between the pressure signals, and the single-pressure measurement becomes less representative of the pressure field. The correlation between the seismic signal and the pressure signal is found to be higher for the windiest period because the seismic pressure noise reflects the atmospheric structure close to the seismometer. In the same way that we reduce the atmospheric seismic signal by making use of a pressure sensor that is part of the InSight Auxiliary Payload Sensor Suite, we also the use the synthetic noise data obtained from the LES pressure field to demonstrate a decorrelation strategy. We show that our decorrelation approach is efficient, resulting in a reduction by a factor of ∼ 5 in the observed horizontal tilt noise (in the wind direction) and the vertical noise. This technique can, therefore, be used to remove the pressure signal from the seismic data obtained on Mars during the InSight mission.
Published: 2017
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16. Atmospheric Science with InSight

Author: Mark T. Lemmon, Sébastien Le Maistre, Matthew P. Golombek, Tanguy Bertrand, Yasuhiro Nishikawa, L. Martire, Antoine Mocquet, Naomi Murdoch, Özgür Karatekin, Rudolf Widmer-Schnidrig, Philippe Lognonné, David Mimoun, Véronique Dehant, Bart Van Hove, Don Banfield, Balthasar Kenda, José Antonio Rodríguez Manfredi, William B. Banerdt, Nicholas A Teanby, Aymeric Spiga, Raphaël F. Garcia, Sebastien Rodriguez, Roland Martin, John Clinton, Ralph D. Lorenz, Quentin Brissaud, François Forget, Suzanne E. Smrekar, Eléonore Stutzmann, Ehouarn Millour, Taichi Kawamura, Eric Beucler, Lucie Rolland, Ingrid Daubar, Tilman Spohn, Nils Mueller, Antoine Lucas, 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), 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), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Cornell University [New York], University of Bristol [Bristol], Institut de Physique du Globe de Paris (IPGP), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universität Stuttgart [Stuttgart], Département Electronique, Optronique et Signal (DEOS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Texas A&M University [College Station], Royal Observatory of Belgium [Brussels] (ROB), California Institute of Technology (CALTECH), German Aerospace Center (DLR), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), 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), NASA Ames Research Center Cooperative for Research in Earth Science in Technology (ARC-CREST), NASA Ames Research Center (ARC), Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Géosciences Environnement Toulouse (GET), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-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), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Cornell University, School of Earth Sciences [Bristol], Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Department of Atmospheric Sciences [College Station], Royal Observatory of Belgium [Brussels], Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Johns Hopkins University (JHU), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Advanced CERamics Deposition (ACERDE), Institut Polytechnique de Grenoble - Grenoble Institute of Technology-ACERDE, Swiss Seismological Service, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), NASA-California Institute of Technology (CALTECH), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), 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)-Observatoire Midi-Pyrénées (OMP), 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), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and UCL - SST/ELI/ELIC - Earth & Climate
Subjects: [SPI.OTHER]Engineering Sciences [physics]/Other, 010504 meteorology & atmospheric sciences, Planetary boundary layer, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Mars, Atmospheric sciences, 01 natural sciences, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Autre, Saltation (geology), 0103 physical sciences, Atmospheric science, [SDU.STU.GM]Sciences of the Universe [physics]/Earth Sciences/Geomorphology, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, 010303 astronomy & astrophysics, Dust devil, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, InSight, Radiometer, Astronomy and Astrophysics, Atmosphere of Mars, Mars Exploration Program, Pressure sensor, Planetary science, 13. Climate action, Space and Planetary Science, Atmosphäre, Geology, Planetary atmospheres
Abstract: International audience; In November 2018, for the first time a dedicated geophysical station, the InSight lander, will be deployed on the surface of Mars. Along with the two main geophysical packages, the Seismic Experiment for Interior Structure (SEIS) and the Heat-Flow and Physical Properties Package (HP3), the InSight lander holds a highly sensitive pressure sensor (PS) and the Temperature and Winds for InSight (TWINS) instrument, both of which (along with the InSight FluxGate (IFG) Magnetometer) form the Auxiliary Sensor Payload Suite (APSS). Associated with the RADiometer (RAD) instrument which will measure the surface brightness temperature, and the Instrument Deployment Camera (IDC) which will be used to quantify atmospheric opacity, this will make InSight capable to act as a meteorological station at the surface of Mars. While probing the internal structure of Mars is the primary scientific goal of the mission, atmospheric science remains a key science objective for InSight. InSight has the potential to provide a more continuous and higher-frequency record of pressure, air temperature and winds at the surface of Mars than previous in situ missions. In the paper, key results from multiscale meteorological modeling, from Global Climate Models to Large-Eddy Simulations, are described as a reference for future studies based on the InSight measurements during operations. We summarize the capabilities of InSight for atmospheric observations, from profiling during Entry, Descent and Landing to surface measurements (pressure, temperature, winds, angular momentum), and the plans for how InSight’s sensors will be used during operations, as well as possible synergies with orbital observations. In a dedicated section, we describe the seismic impact of atmospheric phenomena (from the point of view of both “noise” to be decorrelated from the seismic signal and “signal” to provide information on atmospheric processes). We discuss in this framework Planetary Boundary Layer turbulence, with a focus on convective vortices and dust devils, gravity waves (with idealized modeling), and large-scale circulations. Our paper also presents possible new, exploratory, studies with the InSight instrumentation: surface layer scaling and exploration of the Monin-Obukhov model, aeolian surface changes and saltation / lifing studies, and monitoring of secular pressure changes. The InSight mission will be instrumental in broadening the knowledge of the Martian atmosphere, with a unique set of measurements from the surface of Mars.
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16 results on '"Balthasar Kenda"'

1. Transient convection experiments in internally-heated systems

2. Early accretion of planetesimals unraveled by the thermal evolution of the parent bodies of magmatic iron meteorites

3. Polarized ambient noise on Mars

4. Subsurface Structure at the InSight Landing Site From Compliance Measurements by Seismic and Meteorological Experiments

5. Seismic investigations of the Martian near-surface at the InSight landing site

6. Pressure effects on SEIS-INSIGHT instrument, improvement of seismic records and characterization of gravity waves from ground displacements

7. MSS/1: Single-Station and Single-Event Marsquake Inversion

8. The atmosphere of Mars as observed by InSight

9. Preparing for InSight: Evaluation of the Blind Test for Martian Seismicity

10. Impact-Seismic Investigations of the InSight Mission

11. Influence of body waves, instrumentation resonances, and prior assumptions on Rayleigh wave ellipticity inversion for shallow structure at the InSight landing site

12. VAMOS: a SmallSat mission concept for remote sensing of Venusian seismic activity from orbit

13. Remote sensing of venusian seismic activity with a small spacecraft, the VAMOS mission concept

14. Modeling of Ground Deformation and Shallow Surface Waves Generated by Martian Dust Devils and Perspectives for Near-Surface Structure Inversion

15. Estimations of the Seismic Pressure Noise on Mars Determined from Large Eddy Simulations and Demonstration of Pressure Decorrelation Techniques for the Insight Mission

16. Atmospheric Science with InSight

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