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1. Constraints on Lateral Variations of Martian Crustal Thickness From Seismological and Gravity Field Measurements

Author: Mélanie Drilleau, Henri Samuel, Raphaël F. Garcia, Attilio Rivoldini, Clément Perrin, Mark Wieczorek, Philippe Lognonné, and William B. Banerdt
Subjects: Geophysics. Cosmic physics, QC801-809
Abstract: Abstract Using body wave arrival times from 31 seismic events recorded on Mars by the InSight mission, combined with topography and gravity field modeling, we constrained lateral variations of crustal thickness through a Bayesian inversion approach. The parameterization of the seismic structure relies on quantities that influence the thermochemical evolution of Mars, enabling the seismic velocities and densities in the different planetary envelopes to be consistently linked through common physical assumptions. Compared to a 1D structure, models with lateral variations of crustal thickness show two possible interpretations of the thermal evolution of Mars, with either a hot or cold scenario at the present‐day. We found the hot scenario to be more compatible with InSight's radiotracking data and the tidal Love number. We relocated the marsquakes and derived maps of seismicity recorded by InSight, which is mostly located along or North of the boundary between the Northern lowlands and the Southern highlands.
Published: 2024
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2. Structure of the Martian Crust Below InSight From Surface Waves and Body Waves Generated by Nearby Meteoroid Impacts

Author: Mélanie Drilleau, Éric Beucler, Jing Shi, Brigitte Knapmeyer‐Endrun, Raphaël F. Garcia, Véronique Ansan, Doyeon Kim, Philippe Lognonné, and William B. Banerdt
Subjects: surface waves, body waves, InSight mission, crustal structure, meteoroid impacts, Mars, Geophysics. Cosmic physics, QC801-809
Abstract: Abstract We measure group velocity dispersion of surface waves generated by two meteoroid impacts on Mars close to the lander of the InSight mission. This allows us to probe the crustal structure in the first few kilometers beneath the InSight lander. In combination with body wave arrival times from five impact events, we obtain direct seismic constraints on the seismic velocity of the crust in the vicinity of the InSight landing site. We confirm the existence of a uppermost low‐velocity layer with a mean thickness of ∼1.2 km, interpreted as layered volcanic materials, possibly interstratified with sedimentary and altered materials. Our joint inversion of surface and body waves shows a four‐layer model for the Martian crust, compatible with high‐ and low‐frequency P‐to‐S receiver functions estimated in previous studies.
Published: 2023
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3. MSS/1: Single‐Station and Single‐Event Marsquake Inversion

Author: Mélanie Drilleau, Éric Beucler, Philippe Lognonné, Mark P. Panning, Brigitte Knapmeyer‐Endrun, W. Bruce Banerdt, Caroline Beghein, Savas Ceylan, Martin vanDriel, Rakshit Joshi, Taichi Kawamura, Amir Khan, Sabrina Menina, Attilio Rivoldini, Henri Samuel, Simon Stähler, Haotian Xu, Mickaël Bonnin, John Clinton, Domenico Giardini, Balthasar Kenda, Vedran Lekic, Antoine Mocquet, Naomi Murdoch, Martin Schimmel, Suzanne E. Smrekar, Éléonore Stutzmann, Benoit Tauzin, and Saikiran Tharimena
Subjects: InSight, inversion, seismology, Astronomy, QB1-991, Geology, QE1-996.5
Abstract: 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.
Published: 2020
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4. Seismic detection of a deep mantle discontinuity within Mars by InSight

Author: Quancheng Huang, Nicholas C. Schmerr, Scott D. King, Doyeon Kim, Attilio Rivoldini, Ana-Catalina Plesa, Henri Samuel, Ross R. Maguire, Foivos Karakostas, Vedran Lekić, Constantinos Charalambous, Max Collinet, Robert Myhill, Daniele Antonangeli, Mélanie Drilleau, Misha Bystricky, Caroline Bollinger, Chloé Michaut, Tamara Gudkova, Jessica C. E. Irving, Anna Horleston, Benjamin Fernando, Kuangdai Leng, Tarje Nissen-Meyer, Frederic Bejina, Ebru Bozdağ, Caroline Beghein, Lauren Waszek, Nicki C. Siersch, John-Robert Scholz, Paul M. Davis, Philippe Lognonné, Baptiste Pinot, Rudolf Widmer-Schnidrig, Mark P. Panning, Suzanne E. Smrekar, Tilman Spohn, William T. Pike, Domenico Giardini, and W. Bruce Banerdt
Published: 2022
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5. Systematic catalog of Martian convective vortices observed by InSight

Author: Keisuke Onodera, Kiwamu Nishida, Taichi Kawamura, Naomi Murdoch, Mélanie Drilleau, Ryoji Otsuka, Ralph D. Lorenz, Anna Catherine Horleston, Rudolf Widmer-Schnidrig, Martin Schimmel, Sebastien Rodriguez, Sebastián Carrasco, Satoshi Tanaka, Clement Perrin, Philippe Lognonné, Aymeric Spiga, Donald Banfield, Mark Paul Panning, and William Bruce Banerdt
Abstract: Convective vortices (whirlwinds) and dust devils (dust-loaded vortices) are one of the most common phenomena on Mars, observable on a daily basis. They reflect the local thermodynamical structure of the atmosphere and are the driving force of the dust cycle. Additionally, they cause an elastic ground deformation, which is useful for retrieving the subsurface rigidity. Therefore, investigating Martian convective vortices with the right instrumentation can lead to a better understanding of the Martian atmospheric structures as well as the subsurface physical properties. In this study, we quantitatively characterized the convective vortices detected by NASA’s InSight mission (~13,000 events) using both meteorological (e.g., pressure, wind speed, temperature) and seismic data. The evaluated parameters, such as the signal-to-noise ratio, event duration, asymmetricity of pressure drop profiles, and cross-correlation coefficient between seismic and pressure signals, are compiled as a catalog. To demonstrate how our catalog can contribute to scientific investigations, we show two analysis results about (i) asymmetrical features seen in the vortex-related pressure drops and (ii) atmospheric-ground interaction to retrieve the subsurface physical properties.
Published: 2023

6. An autonomous lunar geophysical experiment package (ALGEP) for future space missions

Author: Taichi Kawamura, Matthias Grott, Raphael Garcia, Mark Wieczorek, Sébastien de Raucourt, Philippe Lognonné, Felix Bernauer, Doris Breuer, John Clinton, Pierre Delage, Mélanie Drilleau, Luigi Ferraioli, Nobuaki Fuji, Anna Horleston, Günther Kletetschka, Martin Knapmeyer, Brigitte Knapmeyer-Endrun, Sebastiano Padovan, Ana-Catalina Plesa, Attilio Rivoldini, Johan Robertsson, Sebastien Rodriguez, Simon C. Stähler, Eleonore Stutzmann, Nicholas A. Teanby, Nicola Tosi, Christos Vrettos, Bruce Banerdt, Wenzhe Fa, Qian Huang, Jessica Irving, Yoshiaki Ishihara, Katarina Miljković, Anna Mittelholz, Seiichi Nagihara, Clive Neal, Shaobo Qu, Nicholas Schmerr, and Takeshi Tsuji
Subjects: Space and Planetary Science, Astronomy and Astrophysics
Abstract: Geophysical observations will provide key information about the inner structure of the planets and satellites and understanding the internal structure is a strong constraint on the bulk composition and thermal evolution of these bodies. Thus, geophysical observations are a key to uncovering the origin and evolution of the Moon. In this article, we propose the development of an autonomous lunar geophysical experiment package, composed of a suite of instruments and a central station with standardized interface, which can be installed on various future lunar missions. By fixing the interface between instruments and the central station, it would be possible to easily configure an appropriate experiment package for different missions. We describe here a series of geophysical instruments that may be included as part of the geophysical package: a seismometer, a magnetometer, a heat flow probe, and a laser reflector. These instruments will provide mechanical, thermal, and geodetic parameters of the Moon that are strongly related to the internal structure. We discuss the functionality required for future geophysical observations of the Moon, including the development of the central station that will be used commonly by different payloads.
Published: 2022

7. First observations of core-transiting seismic phases on Mars

Author: Jessica C. E. Irving, Vedran Lekić, Cecilia Durán, Mélanie Drilleau, Doyeon Kim, Attilio Rivoldini, Amir Khan, Henri Samuel, Daniele Antonangeli, William Bruce Banerdt, Caroline Beghein, Ebru Bozdağ, Savas Ceylan, Constantinos Charalambous, John Clinton, Paul Davis, Raphaël Garcia, null Domenico Giardini, Anna Catherine Horleston, Quancheng Huang, Kenneth J. Hurst, Taichi Kawamura, Scott D. King, Martin Knapmeyer, Jiaqi Li, Philippe Lognonné, Ross Maguire, Mark P. Panning, Ana-Catalina Plesa, Martin Schimmel, Nicholas C. Schmerr, Simon C. Stähler, Eleonore Stutzmann, Zongbo Xu, University of Bristol, School of Earth Sciences, Department of Geology, University of Maryland, Institute of Geophysics [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), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Royal Observatory of Belgium [Brussels] (ROB), 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), 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), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Earth, Planetary, and Space Sciences, University of California Los Angeles, Department of Applied Mathematics and Statistics & Department of Geophysics, Colorado School of Mines, Department of Electrical and Electronic Engineering, Imperial College London, South Kensington Campus, London, United Kingdom, Swiss Seismological Service [ETH Zurich] (SED), 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), School of Earth Sciences [Bristol], University of Bristol [Bristol], Department of Applied Mathematics and Statistics & Department of Geophysics, Colorado School of Mines, Golden, CO, USA, Department of Geosciences, Virginia Tech, Blacksburg, VA, DLR-Berlin, Institute of Planetary Research, Germany, Department of Geology, University of Illinois Urbana-Champaign, Urbana, IL, USA, Geosciences Barcelona - CSIC, Barcelona, Spain, Department of Geology, University of Maryland, College Park, USA, S-CAPAD/DANTE, MAGIS, ANR-19-CE31-0008-08, and ANR-18-IDEX-0001
Subjects: Core evolution, Mars, Planetary structure, Multidisciplinary, marsquake, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [PHYS.PHYS.PHYS-GEO-PH]Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph], planetary structure, Impact, [SDU]Sciences of the Universe [physics], Mars InSight Seismology SKS Core, core evolution, Core, Seismology
Abstract: We present the first observations of seismic waves propagating through the core of Mars. These observations, made using seismic data collected by the InSight geophysical mission, have allowed us to construct the first seismically constrained models for the elastic properties of Mars' core. We observe core-transiting seismic phase SKS from two farside seismic events detected on Mars and measure the travel times of SKS relative to mantle traversing body waves. SKS travels through the core as a compressional wave, providing information about bulk modulus and density. We perform probabilistic inversions using the core-sensitive relative travel times together with gross geophysical data and travel times from other, more proximal, seismic events to seek the equation of state parameters that best describe the liquid iron-alloy core. Our inversions provide constraints on the velocities in Mars' core and are used to develop the first seismically based estimates of its composition. We show that models informed by our SKS data favor a somewhat smaller (median core radius = 1,780 to 1,810 km) and denser (core density = 6.2 to 6.3 g/cm3) core compared to previous estimates, with a P-wave velocity of 4.9 to 5.0 km/s at the core-mantle boundary, with the composition and structure of the mantle as a dominant source of uncertainty. We infer from our models that Mars' core contains a median of 20 to 22 wt% light alloying elements when we consider sulfur, oxygen, carbon, and hydrogen. These data can be used to inform models of planetary accretion, composition, and evolution., Proceedings of the National Academy of Sciences of the United States of America, 120 (18), ISSN:0027-8424, ISSN:1091-6490
Published: 2023
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8. Energy Envelope and Attenuation Characteristics of High-Frequency (HF) and Very-High-Frequency (VF) Martian Events

Author: Simon Stähler, Raphaël F. Garcia, Jules Marti, Sabrina Menina, Nicholas Schmerr, William B. Banerdt, Nicolas Compaire, Grégory Sainton, Mélanie Drilleau, Martin van Driel, Sebastián Carrasco, Domenico Giardini, Ludovic Margerin, Marie Calvet, Philippe Lognonné, Matthieu Plasman, Taichi Kawamura, Brigitte Knapmeyer-Endrun, Foivos Karakostas, 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 de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), University of Maryland [College Park], University of Maryland System, Istituto Nazionale di Geofisica e Vulcanologia - Sezione di Bologna (INGV), Istituto Nazionale di Geofisica e Vulcanologia, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Universität zu Köln, Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, 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), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-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), Universität zu Köln = University of Cologne, NASA-California Institute of Technology (CALTECH), and ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019)
Subjects: Martian, Physics, 010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Attenuation, Very high frequency, 010502 geochemistry & geophysics, 01 natural sciences, Computational physics, Geophysics, 13. Climate action, Geochemistry and Petrology, Mars seismology, Energy (signal processing), 0105 earth and related environmental sciences, Envelope (waves)
Abstract: Since its deployment at the surface of Mars, the Seismic Experiment for Interior Structure (SEIS) instrument of the InSight mission has detected hundreds of small-magnitude seismic events. In this work, we highlight some features of two specific families: high-frequency (HF) and very-high-frequency (VF) events. We characterize the shape of the energy envelopes of HF and VF events with two parameters: (1) the delay time td between the onset and the peak of the dominant arrival; and (2) the quality factor Qc, which quantifies the energy decay rate in the coda. We observe that the envelope of HF and VF events is frequency independent. As a consequence, a single delay time suffices to characterize envelope broadening in the 2.5–7.5 Hz band. The typical coda decay time is also frequency independent, as attested by the close to linear increase of Qc with frequency. Finally, we use elastic radiative transfer theory to perform a series of inversion of seismogram envelopes for the attenuation properties of the Martian lithosphere. The good fit between synthetic and observed envelopes confirms that multiple scattering of elastic waves released by internal sources is a plausible explanation of the events characteristics. We quantify scattering and attenuation properties of Mars and highlight the differences and similarities with the Earth and the Moon. The albedo, that is, the contribution of scattering to the total attenuation, derived from VF events is very high, which we interpret as a signature of a mostly dry medium. Our results also suggest a stratification of the scattering and attenuation properties.
Published: 2021

9. Proceedings of the National Academy of Sciences of the United States of America

Author: Quancheng Huang, Nicholas C. Schmerr, Scott D. King, Doyeon Kim, Attilio Rivoldini, Ana-Catalina Plesa, Henri Samuel, Ross R. Maguire, Foivos Karakostas, Vedran Lekić, Constantinos Charalambous, Max Collinet, Robert Myhill, Daniele Antonangeli, Mélanie Drilleau, Misha Bystricky, Caroline Bollinger, Chloé Michaut, Tamara Gudkova, Jessica C. E. Irving, Anna Horleston, Benjamin Fernando, Kuangdai Leng, Tarje Nissen-Meyer, Frederic Bejina, Ebru Bozdağ, Caroline Beghein, Lauren Waszek, Nicki C. Siersch, John-Robert Scholz, Paul M. Davis, Philippe Lognonné, Baptiste Pinot, Rudolf Widmer-Schnidrig, Mark P. Panning, Suzanne E. Smrekar, Tilman Spohn, William T. Pike, Domenico Giardini, W. Bruce Banerdt, University of Maryland [College Park], University of Maryland System, Graphics and Vision Research Laboratory (Graphics Lab), University of Otago [Dunedin, Nouvelle-Zélande], Royal Observatory of Belgium [Brussels] (ROB), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Department of Geology [College Park], University of Maryland System-University of Maryland System, Michigan State University [East Lansing], Michigan State University System, Istituto Nazionale di Geofisica e Vulcanologia - Sezione di Bologna (INGV), Istituto Nazionale di Geofisica e Vulcanologia, Department of Electrical and Electronic Engineering [London] (DEEE), Imperial College London, 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), Institut de Physique du Globe de Paris (IPGP), 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 en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-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), Bavarian Research Institute of Experimental Geochemistry and Geophysics (Bayerisches Geoinstitut), Universität Bayreuth, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-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.), Institut de Physique du Globe de Paris (IPG Paris), ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019), 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 de Physique du Globe de Paris (IPGP (UMR_7154)), and 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)
Subjects: thermal evolution of Mars, Minerals, Multidisciplinary, Extraterrestrial Environment, Earth, Planet, Mantle transition zone, Iron, interior of Mars, mantle transition zone, Mars, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], Seismic discontinuity, InSight
Abstract: Constraining the thermal and compositional state of the mantle is crucial for deciphering the formation and evolution of Mars. Mineral physics predicts that Mars' deep mantle is demarcated by a seismic discontinuity arising from the pressure-induced phase transformation of the mineral olivine to its higher-pressure polymorphs, making the depth of this boundary sensitive to both mantle temperature and composition. Here, we report on the seismic detection of a midmantle discontinuity using the data collected by NASA's InSight Mission to Mars that matches the expected depth and sharpness of the postolivine transition. In five teleseismic events, we observed triplicated P and S waves and constrained the depth of this discontinuity to be 1,006 [Formula: see text] 40 km by modeling the triplicated waveforms. From this depth range, we infer a mantle potential temperature of 1,605 [Formula: see text] 100 K, a result consistent with a crust that is 10 to 15 times more enriched in heat-producing elements than the underlying mantle. Our waveform fits to the data indicate a broad gradient across the boundary, implying that the Martian mantle is more enriched in iron compared to Earth. Through modeling of thermochemical evolution of Mars, we observe that only two out of the five proposed composition models are compatible with the observed boundary depth. Our geodynamic simulations suggest that the Martian mantle was relatively cold 4.5 Gyr ago (1,720 to 1,860 K) and are consistent with a present-day surface heat flow of 21 to 24 mW/m2., Proceedings of the National Academy of Sciences of the United States of America, 119 (42), ISSN:0027-8424, ISSN:1091-6490
Published: 2022

10. Martian free oscillations: Search in SEIS data and implications

Author: Philippe Lognonné, Martin Schimmel, Eleonore Stutzmann, Mélanie Drilleau, Henri Samuel, Mark Panning, and W.Bruce Banerdt
Abstract: Introduction: For a single seismometer, the most effective techniques for studying deep structure use norma mode frequencies, which do not require knowledge of the source location. Past modeling (Lognonné et al., 1996, Lognonné, 2005) suggest that Normal mode spectral peaks from 5–20 mHz (sensitive to mantle structure) are expected to have amplitude larger than the SEIS requirement (10-9 m/s2/Hz1/2) for moment larger than 2 1017 Nm (equivalent magnitude ∼5.5).Even for the event 1222 from May, 4, 2022, with an estimated magnitude of 5, the amplitude of normal modes is therefore low and their identification will be challenging in the data recorded by the SEIS VBB (Lognonné et al., 2019).Signal preprocessing: A very careful cleaning of the SEIS data is therefore requested, especially in order to remove most of the thermal glitches. If not made, the spectra are dominated by these glitches. This pre-cleaning allow to converge to a corrected signal, which is robust with respect to deglitching parameters (Figure 1).Figure 1: (left) raw VBBZ data and (right) deglitched VBB data. Spectra from the night following the 1222 event.The further detection of modes relies on the identification of spectral peaks in the Fourier amplitude or power spectra. However, close to the background noise level these spectral peaks can be either due to small harmonic signals contaminated by noise or due to the fortuitous constructive interference of noise. Besides, harmonic signals may be perceptive only during a limited portion of the analyzed time series which together with other larger amplitude signals further complicate the detection. For these reasons, we employ phase autocorrelation spectra (Schimmel et al., 2018) and conduct also a Phasor-Walkout analysis (e.g., Zürn and Rydelek, 1994, Schimmel et al., 2002) to search for and evidence normal modes. In the following, we briefly summarize these strategies.Phase autocorrelation spectra. The identification of modes and determination of their frequency are usually based on the computation of the power or energy spectral density (PSD or ESD) which can be obtained through the Fourier Transform of differently defined autocorrelations. ESD can be computed for transient waveforms and equals the squared amplitude spectrum of the seismic recording while PSD is employed when the time series cannot be directly Fourier transformed due to infinite signal energy. Although the underlying autocorrelations are differently defined, they measure the self-similarity of the time series to reveal the spectral contents. In Schimmel et al. (2018), the conventional autocorrelations have been replaced by the phase cross-correlation (PCC; Schimmel ,1999) to show that phase autocorrelations provide an approach which can further aid the detection of modes. PCC is amplitude unbiased as it is based on envelope normalized analytic signals. Inherent to this, PCC is much less affected by outlying signals and supplies robust and independent spectra.Phasor-Walkout. The Phasor-Walkout approach (see Zürn and Rydelek, 1994 for a review and further references) is a graphical representation of the Fourier Transform at a given test-frequency. It pictures the construction of the amplitude spectrum as a vector summation in the complex number space. In this summation, each vector corresponds to a time sample where the sample amplitude and time provide the length of the vector and its angle or phase. The sum of all vectors equals the Fourier amplitude of the spectrum at that frequency. The “walk” of the vectors in the complex number space is called Phasor-Walkout and permits to assess how the spectral amplitude has been build up. If the vectors point into similar directions then the summation becomes constructive while random directions produce a destructive summation which depends on the individual vector amplitudes. For harmonic signals where the test-frequency matches the frequency of the oscillation the walk is straight while for pure random noise the Phasor-Walkout produces a random walk around its start point. Thus the qualitative inspection of Phasor-Walkout patterns may reveal the origin of spectral peaks.Fig. 2 shows an example of phasor-walkouts at four different test frequencies. Amplitude scaleis arbitrary and each color marks a two hours segment of the data. The walk starts at (0,0) which corresponds to the MQS event origin time. The top right panel shows a random walk while the other three panels contain linear walkouts of more than 6 hours.Figure 2: walkout for 4 test frequencies.Further work is required to present clean walkouts validating normal modes in the signal of the largest marsquake recorded by SEIS. When achieved, these frequencies might be inverted and will provide new constraints on the interior structure of the planet (Panning et al., 2017)References:Lognonné, P., J. Gagnepain-Beyneix, W.B. Banerdt, S.Cacho, J.F. Karczewski, M. Morand, An Ultra-Broad Band Seismometer on InterMarsnet, Planetary Space Sciences, 44, 1237-1249, doi:10.1016/S0032-0633(96)00083-9, 1996.Lognonné, P., Planetary seismology, Annual Review in Earth Planet. Sci., 33 :19.1-19.34, doi :10.1146/annurev.earth.33.092203.122605, 2005.Lognonné, P., Banerdt, W.B., Giardini, D. et al., SEIS: Insight’s Seismic Experiment for Internal Structure of Mars, Space Sci Rev, 215, 12, doi : 1007/s11214-018-0574-6 , 2019.Nishikawa, Y., Lognonné, P., Kawamura, T., Spiga, A., Stutzmann, E., Schimmel, M., Bertrand, T., Forget, F., K. Kurita, K., Mars’ Background Free Oscillations, Space Science Reviews 215:13, doi: 10.1007/s11214-019-0579-9, 2019.Panning, M.P., P.Lognonné, W. B. Banerdt et al., Planned products of the Mars Structure Service for the InSight mission, Mars, Space Science review, 211, 611–650, doi: 10.1007/s11214-016-0317-5, 2017.Schimmel M., Phase cross-correlations: design, comparisons and applications, Bull. Seismol. Soc. Am., 89, 1366-1378, 1999.Schimmel M., J. Waterhouse, M.D. Marques, D. Weinert, Circadian and ultradian rhythmicities in very premature neonates maintained in incubators , Biol. Rhythm Res., 33, 83-111, doi:10.1076/brhm.33.1.83.1321 , 2002.Schimmel, M., Stutzmann, E., Ventosa, S., Low-frequency ambient noise autocorrelations: Waveforms and normal modes, Seismological Research Letters, 89 (4), 1488-1496, doi: 10.1785/0220180027, 2018.Zürn, W.; Rydelek, P., Revisiting the phasor-walkout method for detailed investigation of harmonic signals in time series, Surv. in geophys. 15, 409-431, 1994.
Published: 2022

11. Farside Seismic Suite (FSS): First-ever seismology on the farside of the Moon and a model for long-lived lunar science

Author: Mark Panning, Sharon Kedar, Neil Bowles, Simon Calcutt, Mélanie Drilleau, Raphael Garcia, Taichi Kawamura, Philippe Lognonné, David Mimoun, Ceri Nunn, W. Tom Pike, Dilan Portela-Moreira, Sébastien de Raucourt, Renee Weber, and Arnaud Wilhelm
Abstract: The Farside Seismic Suite (FSS), recently selected for flight as part of the NASA PRISM (Payloads and Research Investigations on the Surface of the Moon) program and planned for flight in 2024 or 2025, would deliver two seismometers (both flight-proven through the InSight mission to Mars [Banerdt et al., 2020]) to Schrödinger Basin. The vertical Very BroadBand (VBB) seismometer is the most sensitive flight-ready seismometer ever built [Lognonné et al., 2019], while the Short Period (SP) sensor is the most sensitive and mature compact triaxial sensor available for space application [Lognonné et al., 2019]. Packaged as a self-sufficient payload, with independent power, communications and thermal control allowing survival and operation over the long lunar night, the FSS will outlive the commercial delivery lander, and provide a long-lived seismic experiment capable of answering key scientific questions (figure 1). FSS will address three science objectives with this project:Investigate deep lunar structure and the difference between near and farside activity. Understanding the absence of farside seismicity recorded on Apollo seismometers [e.g. Nakamura et al., 1981] is fundamental to our understanding of the lunar deep interior. Does it reflect a nearside-farside difference in activity rate, or does seismic attenuation from partial melting in the mantle prevent observation of distant events [e.g. Weber et al., 2011]? Direct recording of farside activity, as well as possible recording of known repeating nearside moonquakes or events determined from impact flash observations will illuminate these questions. Understand how the lunar crust is affected by the development of an impact melt basin. Dynamic models of impact processes [e.g. Kring et al., 2016] predict deep structure beneath a well-preserved peak ring impact basin like Schrödinger Basin that can only be revealed through geophysical techniques based on receiver functions [e.g. Vinnik et al., 2011; Knapmeyer-Endrun et al., 2021] and autocorrelation of ambient noise and/or event codas [e.g. Larose et al., 2005; Compaire et al., 2020; Schimmel et al., 2021]. Evaluate the current micrometeorite impact rate and local tectonic activity. Directly constraining micrometeorite impact rates has important implications for future lunar occupation. The lunar background seismic noise is modeled to be driven by micrometeorite impacts [Lognonné et al., 2009]. FSS will record at least 4 months of lunar background hum created by micrometeorite impacts. In order to meet these science objectives, a series of planned measurements were defined and, based on observed Apollo-era seismicity, instrument sensitivity requirements were define. For example, in order to make an estimate of farside seismicity to address objective 1, we require recording at least 50 seismic events, and we assessed that a VBB sensitivity of 2 x 10-10 m/s2/rtHz across the frequency band of 0.1-1Hz would be sufficient to make the measurement during the mission. This is a target, but we assess that we have ample scientific margin if the instrument is unable to reach this noise floor due to either instrument self-noise or other environmental sources of noise (figure 2). To better assess this margin, we are working to quantify the noise sources from the FSS and lander system and the lunar environment (figures 3 and 4). In current modeling, the most important noise sources for the single-component vertical VBB appear to be the instrument self-noise, the noise induced by magnetic field variations as the Moon crosses over the bowshocks surrounding the Earth’s magnetotail, and thermal tilt noise from the regolith which can couple into the VBB signal if the lander is tilted relative to the Moon’s gravitational vector. At typical levels, this noise is close to the proposed instrument requirements (figure 3), while in the stacked worst case (maximum allowed lander tilt and during a bowshock crossing), the noise may exceed the requirement by a factor of 2-3, which still should leave margin for achieving science objectives. FSS is designed to answer several key lunar science questions from a single station on the farside of the Moon. The FSS will also allow for key technical advancement and risk reduction for future missions, such as the Lunar Geophysical Network, a candidate New Frontiers 5 mission [Neal et al., 2020]. Because deployment increases cost and complexity, assessing the need for deployment and characterizing the lander seismic noise environment will be key. In addition, measuring the lunar seismic noise floor beyond what was possible with the Apollo data will permit better requirements definition for future lunar seismic missions and future astrophysics observatories sensitive to lunar ground stability.Figure 1: FSS will return data with unprecedented sensitivity from Schrödinger Crater over multiple lunar diurnal cycles after outliving the delivery lander. Figure adapted from Wieczorek (2009) and Kring et al. (2016).Figure 2: Expected number of events recorded through the mission at various VBB sensitivity levels based on Apollo observation rates, with 95% confidence bounds based on Poisson statistics. Requirements are easily met if VBB performance is within a factor of 5 of the requirement.Figure 3: Expected summed noise sources for a “typical” environment with magnetic noise away from the bowshock crossing and a lander tilt of 5 degrees (half the allowed maximum tilt).Figure 4: Expected worst case instrument noise with magnetic noise at the bowshock crossing and lander tilt at the maximum allowed (10 degrees).
Published: 2022

12. Testing the Presence Deep Martian Mantle Layering in the light of InSight Seismic Data

Author: Henri Samuel, Mélanie Drilleau, Raphael Garcia, Quancheng Huang, Attilio Rivoldini, Philippe Lognonné, and Bruce Banerdt
Abstract: Introduction: The identification of deep reflected phases in the InSight mission seismic recording as core reflected phases have led to the first seismic detection of the Martian core [1]. These results indicated that the core size of Mars spans the higher end of InSight pre-mission estimates, implying a large fraction of Sulfur in the core together with smaller fractions of O, C, and H. The presence of well-separated silicate and metallic envelopes indicates that Mars experienced an early global magma ocean stage whose crystallisation likely led to the formation of a compositionally distinct layer at the bottom of the mantle [2]. Such a layer is expected to be heavily enriched in heat-producing elements and in iron, leading to long-term stability with little mixing between the layer and the overlying mantle. The presence of this enriched basal layer often yields the development of a molten silicate layer above the core that could act as a deep seismic reflector [3]. Objectives and approach: To test the compatibility of Martian mantle layering with seismic data, we conducted Monte Carlo Markov chain inversions in which the long-term thermo-chemical history of Mars’ main envelopes is embedded into the forward problem (Fig. 1). Contrary to more classical approaches that directly invert for seismic velocities and density along a radial planetary profile, we explore a different and smaller model space that consists in parameters that govern the thermo-chemical evolution of Mars: the planetary initial thermal state, the core size, the mantle rheology, or the crustal enrichment in heat-producing element with respect to the mantle. For each model we evolve the system for 4.5 Gyr. Figure 1: Schematic representation of a classical [5] (left) and a geodynamic parameterization [4] (used here) to infer Mars’ seismic structure via Monte Carlo Markov chain inversion of seismic data. This results in thermal structures at present-day that are converted into seismic structures [4]. This approach allows for a more coherent and more constrained profile than in classical inversions (Fig. 1), due to the more informative prior considered, and allows reconstructing the long-term history of the planet. Our inversion approach also considers an enriched silicate layer above the core-mantle boundary and we therefore invert for the layer thickness and for its thermal conductivity. We used the most recent travel time dataset that contains considerably more shallow and deep phases compared to previous studies. Altogether, this allows us to test the hypothesis of the presence of a molten layer at the top of Mars' core, along with the associated consequences on the interpretation of seismic, geodetic, and geochemical data. Results: Our inversion results indicate that the presence of a basal mantle layer is at least as compatible with seismic data than a homogeneous Martian structure (Fig. 2). Figure 2: Data fit for the inversion output considering a basal mantle layer (left) or a homogeneous mantle (right). Warm and cold colors indicate respectively high and small probability densities. Figure 3: Inversion results without (top) and with (bottom) a mantle stratification. Prior (grey) and posterior (blue) distribution for several inverted parameters. The plain and dashed red lines indicate the posterior mean value and 1-sigma range. Fig. 3 shows that the basal mantle layer yields a thinner, crust less enriched in heat-producing element than in the case of a homogeneous mantle. It also shows that a basal mantle layer is also compatible with geodetic constraints on k2 values: 0.174±0.008 [7], in good agreement with theoretical predictions [3]. Conclusions: Our new inversion results indicate that the presence of a basal mantle layer is compatible with seismic data. The basal mantle layer stores a significant fraction of heat-producing elements and depletes the rest of the mantle. This reduces shallow mantle heating and melting leading to thinner crusts that are more compatible with receiver functions and gravity data constraints [8]. Finally, the presence of the enriched basal mantle layer is also compatible with the Love number values for Mars [7]. We will present more advanced inversion results using an augmented database that will contain additional phases, including phases that are most sensitive to the deep mantle structure (e.g., Pdiff). References: [1] Stähler, S., et al., Science 373, 443–448 (2021) [2] Elkins-Tanton, L. et al., JGR., doi:10.1029/2005JE002480 (2003) [3] Samuel, H. et al., JGR, doi:10.1029/2020JE006613 (2021). [4] Drilleau, M. et al., G. J. Int., 226, 1615-1644 (2021) [5] Drilleau M., et al., G. J. Int., 195, 1165-1183 (2013) [6] Khan, A., et al., Science, 373, 434-438 (2021) [7] Konopliv, A. et al., JGR, 47, doi: 10.1029/2020GL090568 (2020) [8] Knapmeyer-Endrun, B. et al., Science, 373 (2021)
Published: 2022

13. Bayesian inversion of the Martian structure using geodynamic constraints

Author: Henri Samuel, Mark P. Panning, Mélanie Drilleau, Philippe Lognonné, Attilio Rivoldini, 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), and 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)
Subjects: Seismometer, Martian, 010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Inversion (meteorology), Crust, Context (language use), Mars Exploration Program, Geophysics, 01 natural sciences, Mantle (geology), Physics::Geophysics, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, 13. Climate action, Geochemistry and Petrology, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Parametrization, Geology, 0105 earth and related environmental sciences
Abstract: SUMMARY The ongoing InSight mission has recently deployed very broad band seismometers to record the Martian seismic activity. These recordings constitute the first seismic data set collected at the surface of Mars. This unique but sparse record compels for the development of new techniques tailored to make the best use of the specific context of single station-multiple events with several possible ranges of uncertainties on the event location. To this end, we conducted sets of Markov chain Monte Carlo inversions for the 1-D seismic structure of Mars. We compared two inversion techniques that differ from the nature of the parametrization on which they rely. A first classical approach based on a parametrization of the 1-D seismic profile using Bézier curves. A second, less conventional approach that relies on a parametrization in terms of quantities that influence the thermochemical evolution of the planet (mantle rheology, initial thermal state and composition), which accounts for 4.5 Gyr of planetary evolution. We considered several combinations of true model parameters to retrieve, and explored the influence of the type of seismic data (body waves with or without surface waves), the number of events and their associated epicentral distances and uncertainties, and the presence of potential constraints on Moho depth inferred from independent measurements/considerations (receiver functions and gravity data). We show that due to its inherent tighter constraints the coupled approach allows a considerably better retrieval of Moho depth and the seismic structure underneath it than the classical inversion, under the condition that the physical assumptions made in the coupled approach are valid for Mars. In addition, our tests indicate that in order to constrain the seismic structure of Mars with InSight data, the following independent conditions must be met: (1) The presence of surface waves triggered by an internal source to constrain the epicentral distance. (2) The presence of just a few well-localized impact sources, with at least one located at close epicentral distance (
Published: 2021

14. Seismic detection of the martian core

Author: Henri Samuel, Cedric Schmelzbach, Raphaël F. Garcia, Philippe Lognonné, Eléonore Stutzmann, Clément Perrin, Suzanne E. Smrekar, Paul M. Davis, Vedran Lekic, A. Cecilia Duran, Constantinos Charalambous, Taichi Kawamura, Simon Stähler, David Sollberger, Mélanie Drilleau, Anna Horleston, Ana-Catalina Plesa, Martin Schimmel, Ross Maguire, Martin Knapmeyer, Nicholas Schmerr, Mark P. Panning, Savas Ceylan, Do-Yeon Kim, Angela G. Marusiak, W. Bruce Banerdt, Matthieu Plasman, Eric Beucler, John Clinton, Géraldine Zenhäusern, Zongbo Xu, Amir Khan, Nikolaj Dahmen, Attilio Rivoldini, Martin van Driel, Tamara Gudkova, Domenico Giardini, Jessica C. E. Irving, Quancheng Huang, W. Thomas Pike, Daniele Antonangeli, Centre National de la Recherche Scientifique - CNRS (FRANCE), Consejo Superior de Investigaciones Científicas - CSIC (SPAIN), Institut de Physique du Globe de Paris - IPGP (FRANCE), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Institut de Recherche pour le Développement - IRD (FRANCE), Sorbonne Université (FRANCE), Université de Nantes (FRANCE), University of Bristol (UNITED KINGDOM), University of Maryland (USA), California Institute of Technology - Caltech (USA), DLR Institute of Planetary Research (GERMANY), Imperial College London (UNITED KINGDOM), Museum National d'Histoire Naturelle - MNHN (FRANCE), Royal Observatory of Belgium (BELGIUM), Russian academy of sciences (RUSSIA), Eidgenössische Technische Hochschule Zürich - ETHZ (SWITZERLAND), Université d'Angers (FRANCE), University of California-Los Angeles - UCLA (USA), Universität Zürich - UZH (SWITZERLAND), Centre National de la Recherche Scientifique (CNRS), 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 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-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019), NASA Jet Propulsion Laboratory, European Commission, Agence Nationale de la Recherche (France), Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia, Innovación y Universidades (España), UK Space Agency, and 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)
Subjects: Martian, Multidisciplinary, 010504 meteorology & atmospheric sciences, Martian Core, Mars, Mars Exploration Program, Radius, Geophysics, 010502 geochemistry & geophysics, 01 natural sciences, Mantle (geology), Seismic wave, Planétologie, Core (optical fiber), [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, 13. Climate action, Planet, Transition zone, Seismic data, Mars seismology, Geology, 0105 earth and related environmental sciences, InSight
Abstract: Clues to a planet’s geologic history are contained in its interior structure, particularly its core. We detected reflections of seismic waves from the core-mantle boundary of Mars using InSight seismic data and inverted these together with geodetic data to constrain the radius of the liquid metal core to 1830 ± 40 kilometers. The large core implies a martian mantle mineralogically similar to the terrestrial upper mantle and transition zone but differing from Earth by not having a bridgmanite-dominated lower mantle. We inferred a mean core density of 5.7 to 6.3 grams per cubic centimeter, which requires a substantial complement of light elements dissolved in the iron-nickel core. The seismic core shadow as seen from InSight’s location covers half the surface of Mars, including the majority of potentially active regions—e.g., Tharsis—possibly limiting the number of detectable marsquakes., Science, 373 (6553), ISSN:0036-8075, ISSN:1095-9203
Published: 2021

15. Seismic Noise Autocorrelations on Mars

Author: Raphaël F. Garcia, Nicholas Schmerr, Martin Schimmel, Philippe Lognonné, Mark P. Panning, Brigitte Knapmeyer-Endrun, Mélanie Drilleau, Benoit Tauzin, John Robert Scholz, Aymeric Spiga, Paul M. Davis, Vedran Lekic, Nicolas Compaire, Bruce Banerdt, Ludovic Margerin, Eléonore Stutzmann, Do-Yeon Kim, 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), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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), ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019), 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 national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Centre National de la Recherche Scientifique (France), Schimmel, Martin, and Schimmel, Martin [0000-0003-2601-4462]
Subjects: Seismometer, 010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Astronomy, Greens-Function, QB1-991, Extraction, Environmental Science (miscellaneous), Seismic noise, 010502 geochemistry & geophysics, 01 natural sciences, Basin, Receiver Functions, Planet, 0105 earth and related environmental sciences, QE1-996.5, Geology, Zone, Mars Exploration Program, Rayleigh-Wave Ellipticity, Crust, 13. Climate action, Extraterrestrial life, General Earth and Planetary Sciences, Seismology
Abstract: Mars is the first extraterrestrial planet with seismometers (Seismic Experiment for Interior Structure, SEIS) deployed directly on its surface in the framework of the Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) mission. The lack of strong Marsquakes, however, strengthens the need of seismic noise studies to additionally constrain the Martian structure. Seismic noise autocorrelations of single-station recordings permit the determination of the zero-offset reflection response underneath SEIS. We present a new autocorrelation study which employs state-of-the-art approaches to determine a robust reflection response by avoiding bias from aseismic signals which are recorded together with seismic waves due to unfavorable deployment and environmental conditions. Data selection and segmentation is performed in a data-adaptive manner which takes the data root-mean-square amplitude variability into account. We further use the amplitude-unbiased phase cross-correlation and work in the 1.2-8.9 Hz frequency band. The main target are crustal scale reflections, their robustness and convergence. The strongest signal appears at 10.6 s, and, if interpreted as a P-wave reflection, would correspond to a discontinuity at about 21 km depth. This signal is a likely candidate for a reflection from the base of the Martian crust due to its strength, polarity, and stability. Additionally we identify, among the stable signals, a signal at about 6.15 s that can be interpreted as the P-wave reflection from the mid-crust at about 9.5 km depth., This is the InSight contribution number 144 and IPGP contribution number 4215. French authors are supported by ANR MAGIS (ANR-19-CE31-0008-08) and by CNES SEIS/InSight Phase E2. MS thanks SANIMS (RTI2018-095594-B-I00), Generalitat de Catalunya (2017SGR1022), and invitations for research stays at IPGP.
Published: 2021

16. Low-velocity impacts into granular material: application to small-body landing

Author: Yves Gourinat, Gautier Nguyen, Naomi Murdoch, Mélanie Drilleau, Florian Thuillet, Arnaud Wilhelm, Cecily Sunday, Département Electronique, Optronique et Signal (DEOS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Clément Ader (ICA), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-IMT École nationale supérieure des Mines d'Albi-Carmaux (IMT Mines Albi), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-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)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-IMT École nationale supérieure des Mines d'Albi-Carmaux (IMT Mines Albi), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Centre National de la Recherche Scientifique - CNRS (FRANCE), Ecole nationale supérieure des Mines d'Albi-Carmaux - IMT Mines Albi (FRANCE), Institut National des Sciences Appliquées de Toulouse - INSA (FRANCE), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Observatoire de la Côte d'Azur (FRANCE), Université Toulouse III - Paul Sabatier - UT3 (FRANCE), and Université Côte d'Azur (FRANCE)
Subjects: Physics, Gravity (chemistry), Spacecraft, Projectile, business.industry, Minor planets, Astronomy and Astrophysics, Penetration (firestop), Mechanics, Granular material, 01 natural sciences, Regolith, Asteroids: general – Comets: general – Planets and satellites: surfaces, Space and Planetary Science, Drag, general – Comets: general – Planets and satellites: surfaces [Asteroids], 0103 physical sciences, Resistance force, Traitement du signal et de l'image, 010306 general physics, business, 010303 astronomy & astrophysics, [SPI.SIGNAL]Engineering Sciences [physics]/Signal and Image processing
Abstract: With the flourishing number of small body missions that involve surface interactions, understanding the mechanics of spacecraft – surface interactions is crucial for improving our knowledge about the landing phases of space missions, for preparing spacecraft operations, and for interpreting the results of measurements made during the surface interactions. Given their regolith-covered surfaces, the process of landing on a small body can be considered as an impact at low-velocity on to a granular material in reduced-gravity. In order to study the influence of the surface material, projectile shape, and gravity on the collision dynamics, we used two experimental configurations (one for terrestrial gravity experiments and one for reduced-gravity experiments) to perform low-velocity collisions into different types of granular materials: quartz sand, and two different sizes of glass beads (1.5 and 5 mm diameter). Both a spherical and a cubic projectile (with varying impact orientation) were used. The experimental data support a drag model for the impact dynamics composed of both a hydrodynamic drag force and quasi-static resistance force. The hydrodynamic and quasi-static contributions are related to the material frictional properties, the projectile geometry, and the gravity. The transition from a quasi-static to a hydrodynamical regime is shown to occur at lower impact velocities in reduced-gravity trials than in terrestrial gravity trials, indicating that regolith has a more fluid-like behaviour in low-gravity. The reduced quasi-static regime of a granular material under low-gravity conditions leads to a reduction in the strength, resulting in a decreased resistance to penetration and larger penetration depths.
Published: 2021

17. The Polarization of Ambient Noise on Mars

Author: Taichi Kawamura, Marie Calvet, Bruce Banerdt, Martin van Driel, Naomie Murdoch, Eléonore Stutzmann, Savas Ceylan, Martin Schimmel, Simon Stähler, Anna Horleston, B. Kenda, Lucile Fayon, Raphaël F. Garcia, A. Jacob, John Clinton, Philippe Lognonné, Constantinos Charalambous, Mélanie Drilleau, M. P. Panning, and Ludovic Margerin
Subjects: Background noise, Physics, Optics, business.industry, Ambient noise level, Degree of polarization, Elliptical polarization, Seismic noise, business, Polarization (waves), Horizontal plane, Noise (radio)
Abstract: Seismic noise recorded at the surface of Mars has been monitored since February 2019, using the InSight seismometers.This noise can reach -200 dB and is 500 times lower than on Earth at night and it increases of 30 dB during the day. We analyze its polarization as a function of time and frequency in the band 0.03-1Hz. We use the degree of polarization to extract signals with stable polarization independent of their amplitude and type of polarization. We detect polarized signals at all frequencies and all times. Glitches correspond to linear polarized signals which are more abundant during the night. For signals with elliptical polarization, the ellipse is in the horizontal plane below 0.3 Hz (LF). Above 0.3 Hz (HF) and except in the evening, the ellipse is in the vertical plane and the major axis is tilted. While polarization azimuths are different in the two frequency bands, they both vary as a function of local hour and season. They are also correlated with wind direction, particularly during the daytime.We investigate possible aseismic and seismic origins of the polarized signals. Lander or tether noise can be discarded. Pressure fluctuations transported by wind may explain part of the HF polarization but not the tilt of the ellipse. This tilt can be obtained if the source is an acoustic emission coming from high altitude at critical angle. Finally, in the evening when the wind is low, the polarized signals may correspond to the seismic wavefield of the Mars background noise.
Published: 2021

18. Estimation of the marsquakes’ location and the interior structure of Mars using InSight data

Author: Mélanie Drilleau, Paul M. Davis, John Clinton, Taichi Kawamura, Mark P. Panning, Amir Khan, Attilio Rivoldini, Nicholas Schmerr, Raphaël F. Garcia, Quancheng Huang, Henri Samuel, John-Robert Scholz, Simon Stähler, Clément Perrin, Do-Yeon Kim, Mark A. Wieczorek, Domenico Giardini, Vedran Lekic, Philippe Lognonné, and Savas Ceylan
Subjects: Estimation, Structure (category theory), Geophysics, Mars Exploration Program, Geology
Abstract: The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) lander successfully delivered a geophysical instrument package to the Martian surface on November 26, 2018, including a broadband seismometer called SEIS (Seismic Experiment for Interior Structure). After two years of recording, seismic body waves phases of a small number of high-quality marsquakes have been clearly identified. In this work, we will present how we estimate the body waves arrival times, and how we handle them to constrain the locations of the marsquakes and the interior structure. The inverse problem relies on a Bayesian approach, to investigate a large range of possible locations and interior models. Due to the small number of data, the advantage of using such a method is to provide a quantitative measure of the uncertainties and the non-uniqueness. In order to take into account the strong variations of the crustal thickness due to the crustal dichotomy, and thus consider the seismic lateral variations, which could cause significant misinterpretations, arrival times corrections are added using crustal thickness maps obtained from gravity and topography data.
Published: 2021

19. Energetic characteristics of High Frequency (HF) and Very High Frequency (VF) Martian events

Author: Ludovic Margerin, Martin van Driel, Taichi Kawamura, Sabrina Menina, Mélanie Drilleau, Foivos Karakostas, Jules Marti, Marie Calvet, Nicholas Schmerr, and Philippe Lognonné
Subjects: Martian, Materials science, Very high frequency, Geophysics
Abstract: The InSight seismometer SEIS recorded tens of high-frequency (1.5-5Hz; HF) and Very-high frequency (1.5-15Hz, VF) Martian events. They are characterized by two temporally separated arrivals with a gradual beginning, a broad maximum and a very long decay. This observation is consistent with a long-range propagation of seismic P and S waves in a heterogeneous crust (Van Driel et al., accepted). To examine this hypothesis, first, we employ basic multiple-scattering concepts on the two groups of events. Then, we propose a full envelope modeling based on elastic radiative transport in a half-space. The model parametrization and the radiative transfer equations are presented in (Lognonné, P., et al. (2020) and Margerin, L., (2017)). We find that both HF and VF signals are depolarized and verify Gaussian statistics, at the exception of the ballistic primary and secondary arrivals. These properties agree with a multiple-scattering origin. For VF events, the energy partitioning ratio V2/H2 between horizontal and vertical components is frequency dependent. We observe that V2/H2 is maximum at the so-called ‘2.4Hz resonance’ (~2) and decreases rapidly at frequencies higher than 5Hz (~0.1) then i remains relatively low up to frequencies of 15Hz at least. HF events do not exhibit a decrease of V2/H2 at high frequencies however further analysis reveals a strong correlation between energy partitioning and signal-to-noise (S/N) ratio for HF events. This observation suggests that a part of the difference between the HF and VF events can to some extent be explained by noise contamination. The generally low V2/H2 ratio of VF events is reminiscent of the response of unconsolidated layers, as observed at Pinyon Flats Observatory on Earth (Margerin, L., et al. (2009)). Unlike earthquakes and moonquakes observed in the same frequency band, the delay time measured from onset to peak of the secondary arrival of HF and VF events is frequency-independent. This suggests that the spectrum of heterogeneity of the Martian crust is smooth. We observe that, for HF and VF events, the delay time is weakly dependent on hypocentral distance. This observation cannot be reconciled with the predictions of multiple-scattering theories in a statistically homogeneous medium however it suggests a stratification of heterogeneity in the Martian lithosphere. The coda quality factor Qc of VF events is high and shows a linear increase with frequency. Qc of HF events is higher but it may be overestimated due to the noise contamination. The linear frequency dependence of Qc is strongly reminiscent of the leakage effect in a crustal scattering waveguide and suggests that part of the observed coda attenuation may be of structural origin. The full envelope modeling of the S0334a VF event results shows that the estimated value of the diffusivity (≃ 619 km2/s) is almost 6 times greater than for the S0128a VF event (≃ 90 km2/s). This observation again suggests a stratification of heterogeneity. In future works, we will perform the full envelope modeling of all the VF selected events at different frequencies to constrain a 1D attenuation and diffusion model of the Martian crust.
Published: 2021

20. Measuring Fundamental and Higher Mode Surface Wave Dispersion on Mars From Seismic Waveforms

Author: Mélanie Drilleau, B. Kenda, Naomi Murdoch, M. van Driel, Fabian Euchner, Maren Böse, P. H. Lognonné, Nienke Brinkman, Caroline Beghein, Domenico Giardini, John Clinton, Haotian Xu, Taichi Kawamura, Mark P. Panning, Savas Ceylan, Simon Stähler, Anna Horleston, 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 de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)
Subjects: 010504 meteorology & atmospheric sciences, lcsh:Astronomy, Monte Carlo method, Mars, Seismic Waveforms, Environmental Science (miscellaneous), Overfitting, 010502 geochemistry & geophysics, 01 natural sciences, Synthetic data, lcsh:QB1-991, Traitement du signal et de l'image, Dispersion (water waves), Seismogram, 0105 earth and related environmental sciences, lcsh:QE1-996.5, Mars Exploration Program, lcsh:Geology, Noise, 13. Climate action, General Earth and Planetary Sciences, Algorithm, [SPI.SIGNAL]Engineering Sciences [physics]/Signal and Image processing, Geology, Test data
Abstract: International audience; One of the goals of the Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) mission is to constrain the interior structure of Mars. We present a hierarchical transdimensional Bayesian approach to extract phase velocity dispersion and interior shear‐wave velocity (VS) models from a single seismogram. This method was adapted to Mars from a technique recently developed for Earth (Xu & Beghein, 2019, https://doi.org/10.1093/gji/ggz133). Monte Carlo Markov Chains seek an ensemble of one dimensional (1‐D) VS models between a source and a receiver that can explain the observed waveform. The models obtained are used to calculate the phase velocities of fundamental and higher modes at selected periods, and a subsequent analysis is performed to assess which modes were reliably measured. An advantage of our approach is that it can also fit unknown data noise, which reduces the risk of overfitting the data. In addition, uncertainties in the source parameters can be propagated, yielding more accurate model parameter uncertainties. In this study, we first present our technique and discuss the challenges stemming from using a single station to characterize both structure and the source and from the absence of a Mars reference model. We then demonstrate the method feasibility using the Mars Structure Service blind test data and our own synthetic data, which included realistic noise levels based on the noise recorded by InSight.
Published: 2021

21. The Polarization of Ambient Noise on Mars

Author: Eléonore Stutzmann, Naomi Murdoch, M. Calvet, Mark P. Panning, Martin Schimmel, Ludovic Margerin, Philippe Lognonné, K. Hurst, Simon Stähler, Anna Horleston, M. van Driel, B. Kenda, Mélanie Drilleau, Raphaël F. Garcia, John-Robert Scholz, Bruce Banerdt, Savas Ceylan, Constantinos Charalambous, John Clinton, Taichi Kawamura, Lucile Fayon, A. Jacob, Aymeric Spiga, T. Pike, Domenico Giardini, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Agence Nationale de la Recherche (France), UK Space Agency, Ministerio de Ciencia, Innovación y Universidades (España), Schimmel, Martin, 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), 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), and Schimmel, Martin [0000-0003-2601-4462]
Subjects: Polarization azimuth, Seismic noise on Mars, 010504 meteorology & atmospheric sciences, Seismic noise, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Ambient noise level, Mars, 010502 geochemistry & geophysics, 01 natural sciences, Physics::Geophysics, Optics, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Geochemistry and Petrology, Polarization, Earth and Planetary Sciences (miscellaneous), Traitement du signal et de l'image, 0105 earth and related environmental sciences, seismic noise, polarization, InSight mission, business.industry, inSight mission, Mars Exploration Program, Polarization (waves), Geophysics, 13. Climate action, Space and Planetary Science, business, Mars seismology, Geology
Abstract: Seismic noise recorded at the surface of Mars has been monitored since February 2019, using the InSight seismometers. This noise can reach -200 dB. It is 500 times lower than on Earth at night and it increases of 30 dB during the day. We analyze its polarization as a function of time and frequency in the band 0.03-1 Hz. We use the degree of polarization to extract signals with stable polarization independent of their amplitude and type of polarization. We detect polarized signals at all frequencies and all times. Glitches correspond to linear polarized signals which are more abundant during the night. For signals with elliptical polarization, the ellipse is in the horizontal plane below 0.3 Hz. In the 0.3-1Hz high frequency band (HF) and except in the evening, the ellipse is in the vertical plane and the major axis is tilted. While polarization azimuths are different in the two frequency bands, they both vary as a function of local hour and season. They are also correlated with wind direction, particularly during the daytime. We investigate possible aseismic and seismic origins of the polarized signals. Lander or tether noise can be discarded. Pressure fluctuations transported by wind may explain part of the HF polarization but not the tilt of the ellipse. This tilt can be obtained if the source is an acoustic emission coming from high altitude at critical angle. Finally, in the evening when the wind is low, the measured polarized signals may correspond to the seismic wavefield of the Mars background noise. Plain Language Summary Seismic noise at the surface of Mars was unknown until the first measurements by the seismometers from the InSight mission in January 2019. On Earth, the microseismic noise (0.05-1 Hz) is composed dominantly of surface waves generated by the numerous sources related to ocean wave activities. On Mars, because there is no ocean, seismic noise is down to 500 times lower than on Earth reaching -200 dB in acceleration at night. In order to determine the nature of the Mars noise, we analyze its polarization with a statistical method and show that it is different to that on Earth. In the low frequency band 0.03-0.3 Hz, we detect signals with elliptical polarization in the horizontal plane. In the high frequency band 0.3-1Hz (HF), signals have elliptical polarization in the vertical plane. The polarization ellipse azimuth gives the direction toward the source. On Mars, these azimuths are varying as a function of local hour and season and they are correlated with wind direction during the daytime. The HF polarized signals may be explained by local effects of pressure fluctuations and/or by acoustic emission coming from high altitudes in particular conditions. It is only in the evening when the wind is low, that the measured polarized signals may correspond to propagating seismic waves that would be the Mars seismic background noise., This is the InSight contribution number 143 and IPGP contribution number 4183. We acknowledge NASA, CNES, their partner agencies and institutions (UKSA, SSO, DLR, JPL, IPGP-CNRS, ETHZ, IC, MPS-MPG) and the flight operations team at JPL, SISMOC, MSDS, IRIS-DMC, and PDS for providing SEED SEIS data. French authors are supported by ANR MAGIS (ANR-19-CE31-0008-08) and by CNES for SEIS science support. A. Horleston is supported by the UK Space Agency through grant #ST/R002096/1. M. Schimmel is supported by the SANIMS project (RTI2018-095594-B-I00, MICINN, Spain).
Published: 2021

22. 3-D crustal VS model of western France and the surrounding regions using Monte-Carlo inversion of seismic noise cross-correlation dispersion diagrams

Author: G Aertgeerts, Ianis Gaudot, M. Haugmard, Mélanie Drilleau, A. Mocquet, E. Beucler, D. Leparoux, M Bonnin, Bureau de Recherches Géologiques et Minières (BRGM) (BRGM), 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 Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Laboratoire Géophysique et évaluation non destructive (GERS-GeoEND ), and Université Gustave Eiffel
Subjects: 010504 meteorology & atmospheric sciences, Cross-correlation, Inversion (geology), Monte Carlo method, Inverse theory, Seismic interferometry, Seismic noise, 010502 geochemistry & geophysics, 01 natural sciences, Geophysics, Geochemistry and Petrology, [SDU]Sciences of the Universe [physics], Dispersion (water waves), Seismology, Geology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: Summary Due to a too sparse permanent seismic coverage during the last decades, the crustal structure of western France and the surrounding regions is poorly known. In this study, we present a 3-D seismic tomographic model of this area obtained from the analysis of 2-year continuous data recorded from 55 broad-band seismometers. An unconventional approach is used to convert Rayleigh wave dispersion diagrams obtained from ambient noise cross-correlations into posterior distributions of 1-D VS models integrated along each station pair. It allows to avoid the group velocity map construction step (which means dispersion curve extraction) while providing meaningful VS posterior uncertainties. VS models are described by a self-adapting and parsimonious parameterization using cubic Bézier splines. 1268 separately inverted 1-D VS profiles are combined together using a regionalization scheme, to build the 3-D VS model with a lateral resolution of 75 km over western France. The shallower part of the model (horizontal cross-section at 4 km depth) correlates well with the known main geological features. The crystalline Variscan basement is clearly associated with positive VS perturbations while negative heterogeneities match the Mesocenozoic sedimentary basins. At greater depths, the Bay of Biscay exhibits positive VS perturbations,which eastern and southern boundaries can be interpreted as the ocean-continent transition. The overall crustal structure below the Armorican Massif appears to be heterogenous at the subregional scale, and tends to support that both the South-Armorican Shear Zone and the Paris Basin Magnetic Anomaly are major crustal discontinuities that separate distinct domains.
Published: 2020

23. Experimental and theoretical investigations of low-velocity collisions into granular material

Author: Mélanie Drilleau, Cecily Sunday, Florian Thuillet, Yves Gourinat, Gautier Nguyen, and Naomi Murdoch
Subjects: Materials science, Mechanics, Granular material
Abstract: In order to study the mechanical properties of a small body surface, accelerometers can be used to record the acceleration profile during landing and rebounding of a surface package. However, given the low gravity environment, the behaviour of the grains can be different to under terrestrial gravity [e.g., 1]. Here we present data from experiments of low-velocity impacts of projectiles of various shapes into different types of granular material in both normal and reduced gravity. Then, to further investigate the dynamics, we employ a collisional model in order to fit the experimental data using an empirical force law involving both a hydrodynamic drag force term and a static resistance force term. The contributions of these two force terms are discussed and compared for the different configurations. Framework In terms of collision frequency with the Earth, the most threatening NEOs are the smaller ones (< 1 km diameter). They are also the less well known, because ground observations cannot provide adequate information at these sizes. The JAXA Hayabusa 1 and 2 missions [2, 3], and the NASA OSIRIS-REX [4] missions, have highlighted the complex histories experienced by small bodies. The unintuitive nature of the asteroid response to the Small Carry-on Impactor experiment of the Hayabusa 2 mission [5] also demonstrated the importance of interacting directly with the surface in order to constrain the mechanical properties. The upcoming ESA Hera mission (launch planned for late 2024; [6]) to the binary asteroid Didymos is going to be a great opportunity to study an even smaller asteroid of 150 m diameter. This work is carried in the framework of the NEO-MAPP project (Near Earth Object Modelling and Payloads for Protection), which aims to provide significant advances in our understanding of the response of NEOs to external forces. In the context of the Hera mission, one goal of the NEO-MAPP project [6] is to better understand the physics of low-velocity collisions, and the mechanical properties of the regolith that composes the surface of asteroids. These points are crucial for understanding the evolution of small body surfaces, the main processes that have shaped the surfaces, and for the design and operations of space missions. Our objective is to use experimental data to obtained in both static and low-gravity trials, to develop a theoretical framework to describe low velocity collisions into granular material under varying gravity conditions. Experiments Following the previous work of [1], low-velocity impact experiments were performed using two different projectile shapes (spherical and cubic) and four different granular surface materials (quartz sand of 1.5 mm, 5 mm, and 10 mm glass beads). The projectiles, shown in Figure 1, weigh approximately 1 kg and are made of aluminium. The cubic projectile can be oriented to fall on a face, an edge or a corner. The experiments were performed under both Earth and reduced-gravity conditions (~0.02 – 0.1g effective gravitational acceleration), using a static laboratory set-up and an Atwood-type drop tower [7], respectively. During all trials, in-situ accelerometers were mounted inside the projectiles to measure the in-situ acceleration profile during the impact. Results From the recorded data, we extracted three key parameters: the maximum acceleration, the final penetration depth, and the collision duration. Figure 2 shows the measurements for the experiments performed using the spherical projectile at several drop heights, giving a range of collision velocities. Similarly to [1], the data present a quadratic trend for the maximal acceleration. The post-collision penetration depth was found to be linearly-dependent on the collision velocity, and the collision duration was found to be independent of the collision velocity, at least for collision velocity larger than 0.4 m s-1. We employ a collisional model [8] to fit the data, using an empirical force law involving both a hydrodynamic drag force term (h(z)) and a static resistance force term (f(z)). To fit the data, one must assume specific forms for h(z) and f(z), typically that they are constants [9]. However, the scatter of the data makes this assumption difficult to consider. Instead, we reformulate the force-law model into a linear differential equation in kinetic energy [10]. This solution provides a natural way to experimentally measure f(z) and h(z), with no assumptions about the functional form of these terms. The contributions of these two terms are discussed and compared considering the different projectiles, surface materials and gravity conditions. The behaviour of the granular medium in interaction with the probe, in a very low gravity environment, is an important opportunity for mathematical models combining the dynamics of shocks, frictions and deformations. These models can find applications in various fields of engineering. [1] Murdoch, N., et al. “An experimental study of low-velocity impacts into granular material in reduced gravity.” Monthly Notices of the Royal Astronomical Society, 468 (2), p. 1259-1272 (2017). [2] Fujiwara, Akira, et al. "The rubble-pile asteroid Itokawa as observed by Hayabusa." Science 312.5778 (2006): 1330-1334. [3] Watanabe, Sei-ichiro, et al. "Hayabusa2 mission overview." Space Science Reviews 208.1-4 (2017): 3-16. [4] Lauretta, D. S., et al. "OSIRIS-REx: sample return from asteroid (101955) Bennu." Space Science Reviews 212.1-2 (2017): 925-984. [5] Saiki, T., Imamura, H., et al. “The Small Carry-on Impactor (SCI) and the Hayabusa2 Impact Experiment”. Space Science Reviews, 208, p. 1-22 (2016). [6] Michel, P., Falke, A., Ulamec, S., and the NEO-MAPP Team. “The European Commission funded NEO-MAPP project in support of the ESA Hera mission: Near-Earth Object Modelling And Payload for Protection”, EPSC abstract, Vol. EPSC2020-103 (2020). [7] Sunday, C., et al. "A novel facility for reduced-gravity testing: A setup for studying low-velocity collisions into granular surfaces." Review of Scientific Instruments 87 (8), p. 084504 (2016). [8] Katsuragi, H. “Physics of Soft Impact and Cratering”, Lecture Notes in Physics, Springer Japan (2016). [9] Goldman, D. I. and Umbanhowar, P. “Scaling and dynamics of sphere and disk impact into granular media”. Phys. Rev. E, 77 (2), p. 021308 (2008). [10] Bester, C. S., and Behringer, R. P. “Collisional Model of Energy Dissipation in Three-Dimensional Granular Impact.” Physical Review E, 95 (3), p. 032906 (2017).
Published: 2020

24. Low velocity impact simulations with pkdgrav and Chrono

Author: Mélanie Drilleau, Naomi Murdoch, Cecily Sunday, Adam Yp-Tcha, Florian Thuillet, and Patrick Michel
Abstract: This work presents the results from a set of low-velocity impact simulations that were performed using the soft-sphere Discrete Element Method and two different codes: pkdgrav and Chrono. In these tests, a spherical projectile is dropped onto a bed of glass beads, where the size of the container, the size of the beads, the impact velocity of the projectile, and the gravity-level are varied. First, the simulation results are compared against experimental data and theoretical collision behaviors. Then, the results from pkdgrav and Chrono are examined in more detail and are compared in terms of output and performance differences. Introduction The robotic exploration of small-body surfaces often involves the direct interaction between a slow-moving mechanism and a bed of loose regolith. Take, for instance, the two most recent missions to near-Earth asteroids. In 2018 and 2019, the Hayabusa2 spacecraft deployed several landers to the surface of the asteroid Ryugu [9]. In October of this year, the OSIRIS-REx mission will collect a sample from the surface of the asteroid Bennu using a ‘touch-and-go’ mechanism [2]. One way to develop our understanding of lander-surface interactions is to study low-velocity collisions dynamics for penetrators of diverse shapes and sizes. The motion of spherical, cylindrical, and conical penetrators through different granular media has been extensively studied for the terrestrial gravity environment [1] but much less so for low-gravity levels. [3] and [4] conducted low-velocity impact experiments under both Earth and reduced-gravity conditions using two different projectile shapes (spherical and cubic) and four different granular surface materials (quartz sand and 1.5 mm, 5 mm, and 10 mm glass beads). The Earth-gravity tests were completed using a static laboratory set-up, while the reduced-gravity tests were performed using an Atwood-type drop-tower [7]. In both configurations, in-situ accelerometers were used to monitor the projectile’s motion. [4] discuss the dependency of certain collision parameters, like collision duration and collision depth, on gravity-level. However, the work examines a limited range of collision cases. Due to internal friction and sizing constraints, the ISAE-Supaéro drop-tower can only reach gravity levels spanning from 0.2 to 1.5 m/s^2. The easiest way to compliment the experimental study is through numerical modeling. This work replicates and expands upon a sub-set of the impact experiments performed by [3] and [4]. Simulations The numerical simulations presented in this study are conducted using two different codes. The first code, pkdgrav, is frequently used for small-body related studies [5]. The second code, Chrono, is presented as an open-source alternative to pkdgrav [7, 8]. One objective of this work is to validate the Chrono code by comparing the simulation results against observations from pkdgrav, collision theory, and laboratory experiments. A second objective is to compare Chrono and pkdgrav in terms of input parameters, results, and overall computational performance. At this time, simulations are restricted to the “static” (1g) set-up with the spherical projectile and the glass-bead surface material. In the static experiments, a 1 kg, 10 cm diameter sphere is dropped into an aluminum bucket with a base diameter of 31.5 cm and a rim diameter of 35 cm (Fig. 1). The fill height of the bucket ranges from 1 to 17 cm, and the impact velocity of the projectile varies from approximately 0 to 1.2 m/s. For simplicity, the simulations assume that the bucket has a constant diameter and that the container is filled with either 5 mm or 10 mm diameter glass beads (Fig 2). In order to investigate the influence of the container size on the collision behavior of the projectile, the diameter and fill height of the bucket are varied from 31.5 and 40 cm and from 2 to 18 cm respectively. Though experimental data for this set-up only exists for the 1g case (g = 9.81 m/s2), simulations are conducted for gravity levels ranging from 0.2 to 9.81 m/s2. Results The simulations are in general agreement with trends observed in the 1g impact experiments from [4]. The results are discussed within the context of existing collision models and theories and are used to identify the optimal material properties for the simulated glass beads. The coefficients of friction differ between pkdgrav and Chrono. This is to be expected, since the two codes implement different friction models. Similarly, the computation times vary due to differences in the codes’ architectures and parallelization methods. Both the experiments and simulations show that the container fill height does not influence collision behavior as long as the particle bed is at least 8 cm deep, at least for the test cases where g = 9.81 m/s^2. Chrono is used to determine if the same conclusion applies for test cases where g = 0.2 m/s^2, or the lowest gravity-level obtained by the drop-tower set-up. Acknowledgements We would like to thank ISAE-Supaéro and the Centre National d’Études Spatiales (CNES) for financially supporting this research effort. References [1] Clark, Abram H., and Robert P. Behringer. "Granular impact model as an energy-depth relation." EPL (Europhysics Letters) 101.6 (2013): 64001. [2] Lauretta, D. S., et al. "OSIRIS-REx: sample return from asteroid (101955) Bennu." Space Science Reviews 212.1-2 (2017): 925-984. [3] Murdoch, N., et al. “An experimental study of low-velocity impacts into granular material in reduced gravity.” Monthly Notices of the Royal Astronomical Society, 468(2) (2017) 1259-1272. [4] Murdoch, N., et al. “Low-velocity and shallow impacts into granular material: application to small-body landing.” (2020) [in preparation]. [5] Schwartz, S. R., et al. “An implementation of the soft-sphere discrete element method in a high-performance parallel gravity tree-code.” Granular Matter, 14(3) (2012): 363-380. [6] Sunday, Cecily, et al. "A novel facility for reduced-gravity testing: A setup for studying low-velocity collisions into granular surfaces." Review of Scientific Instruments 87.8 (2016): 084504. [7] Sunday, C., et al. “Validation of Chrono for granular DEM simulations in reduced-gravity environments.” (2020) [submitted]. [8] Tasora, Alessandro, et al. “Chrono: An open source multi-physics dynamics engine.” International Conference on High Performance Computing in Science and Engineering, Springer, Cham , 2015. [9] Watanabe, Sei-ichiro, et al. "Hayabusa2 mission overview." Space Science Reviews 208.1-4 (2017): 3-16.
Published: 2020

25. Lunar Seismology: A Data and Instrumentation Review

Author: Mélanie Drilleau, Ceri Nunn, Raphaël F. Garcia, Ludovic Margerin, Renee Weber, Yosio Nakamura, Taichi Kawamura, Daoyuan Sun, Peimin Zhu, Amir Khan, Philippe Lognonné, Mark A. Wieczorek, Angela G. Marusiak, Attilio Rivoldini, 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 de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), US Geol Survey, Flagstaff, AZ 86001 USA, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Swiss Fed Inst Technol, Inst Geophys, Sonneggstr 5, CH-8092 Zurich, Switzerland, Royal Observatory of Belgium [Brussels] (ROB), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-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)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)
Subjects: Lunar seismology, 010504 meteorology & atmospheric sciences, Deep moonquakes, Apollo, 01 natural sciences, Coda, Lunar geophysical network, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Passive seismic, 0103 physical sciences, Traitement du signal et de l'image, 010303 astronomy & astrophysics, Seismology, 0105 earth and related environmental sciences, Moon seismology, biology, Meteoroid, Gravimeter, Astronomy and Astrophysics, Mars Exploration Program, Meteoroids, biology.organism_classification, Apollo missions, Shallow moonquakes, Decay time, Planetary science, 13. Climate action, Space and Planetary Science, Geology
Abstract: Several seismic experiments were deployed on the Moon by the astronauts during the Apollo missions. The experiments began in 1969 with Apollo 11, and continued with Apollo 12, 14, 15, 16 and 17. Instruments at Apollo 12, 14, 15, 16 and 17 remained operational until the final transmission in 1977. These remarkable experiments provide a valuable resource. Now is a good time to review this resource, since the InSight mission is returning seismic data from Mars, and seismic missions to the Moon and Europa are in development from different space agencies. We present an overview of the seismic data available from four sets of experiments on the Moon: the Passive Seismic Experiments, the Active Seismic Experiments, the Lunar Seismic Profiling Experiment and the Lunar Surface Gravimeter. For each of these, we outline the instrumentation and the data availability. We show examples of the different types of moonquakes, which are: artificial impacts, meteoroid strikes, shallow quakes (less than 200 km depth) and deep quakes (around 900 km depth). Deep quakes often occur in tight spatial clusters, and their seismic signals can therefore be stacked to improve the signal-to-noise ratio. We provide stacked deep moonquake signals from three independent sources in miniSEED format. We provide an arrival-time catalog compiled from six independent sources, as well as estimates of event time and location where available. We show statistics on the consistency between arrival-time picks from different operators. Moonquakes have a characteristic shape, where the energy rises slowly to a maximum, followed by an even longer decay time. We include a table of the times of arrival of the maximum energy 𝑡�max and the coda quality factor 𝑄�𝑐� . Finally, we outline minimum requirements for future lunar missions to the Moon. These requirements are particularly relevant to future missions which intend to share data with other agencies, and set out a path for an International Lunar Network, which can provide simultaneous multi-station observations on the Moon. ISSN:1572-9672 ISSN:0038-6308
Published: 2020

26. Lunar Seismology: a data and instrumentation review - Electronic Supplement

Author: Nunn, Ceri, Raphael F. Garcia, Yosio Nakamura, Angela G. Marusiak, Taichi Kawamura, Daoyuan Sun, Ludovic Margerin, Renee Weber, Mélanie Drilleau, Mark A. Wieczorek, Amir Khan, Attilio Rivoldini, Philippe Lognonné, and Peimin Zhu
Abstract: To get started, read DataPaper_ElectronicSup1.docx. This repository is a collection of resources for lunar seismology, including: S1: Location Parameters S2 - Deep Moonquake Stacks S3 - Lunar Catalog from Various Sources S4 - Extensive Lunar Catalog from Nakamura et al. 1981 and updates S5 - Attenuation Parameters from Gillet et al. (2017) S6 - Low-Level Requirements for Future Seismic Missions to the Moon S7 - Jupyter Notebook to plot the transfer functions S8 - Block Diagrams S9 - Artificial Impacts S10 - Current Data Availability S11 - Response Files, Replaced ImpactParameters.xlsx with ImpactParameters.csv which is easier to import and use. Also corrected an error in the date of the Apollo 15 Lunar Module (A15/LM) impact.
Published: 2020
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27. 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

28. 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

29. Investigation of Mars Seismic Attenuation Using InSight SEIS Data

Author: Martin van Driel, Bruce Banerdt, Mélanie Drilleau, Taichi Kawamura, S. C. Staehler, Philippe Lognonné, Ludovic Margerin, Sabrina Menina, and Nicholas Schmerr
Subjects: Attenuation, Mars Exploration Program, Geology, Seismology
Abstract: NASA InSight (the Interior Exploration using Geodesy and Heat Transport) has placed the first broadband seismometer (SEIS) on the Martian surface and now continuously monitoring Martian seismic activity. Since the first detection of a marsquake in March 2019, SEIS detected more than 200 marsquakes and Mars has been revealed to be a seismically active planet. The dataset can now be used to perform the seismic investigation of the Mars interior and interpret this in a comparative manner by referring to the examples from the Earth and the Moon.In this study, we investigate the seismic attenuation on Mars and compare this with the Earth and the Moon. Attenuation can be described as a combination of inelastic absorption and elastic diffusion of energy. Such properties will give important constraints on the composition of the Mars interior and also its thermal state. Another interesting aspect will be to discuss the water content with respect to the attenuation. Given the large variety of water content for the Earth, the Moon and Mars, the attenuation feature will be likely to differ significantly between these planets and satellite. Here we use the seismic dataset obtained by InSight SEIS and construct a 1D structure of seismic attenuation on Mars. Then we refer to the values obtained for the Earth and the Moon to discuss the possible implication on their differences and similarities. The presentation aims to summarize the results from different approaches taken by the authors. The approach includes; 1) spectral analyses of seismic signals and spectral decay fitting, 2) seismic coda analyses with coda rise time and decay, 3) numerical coda simulation with diffusion theory on seismic energy. With these approaches we will be constraining seismic quality factor Q and diffusivity D for different depth range. Different approaches have sensitivities to different depth and prarameters and we aim to provide our view on the martian attenuation and diffusion to date by summarizing the obtained results.
Published: 2020

30. 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

31. Initial results from the InSight mission on Mars

Author: Sharon Kedar, Don Banfield, Scott M. McLennan, Nicholas Schmerr, Justin N. Maki, Gareth S. Collins, John Clinton, Anna Mittelholz, Paul Morgan, Mélanie Drilleau, Sabine Stanley, Chloé Michaut, Nicholas A Teanby, Daniele Antonangeli, Jeroen Tromp, W. Bruce Banerdt, James B. Garvin, Mark A. Wieczorek, Jerzy Grygorczuk, Suzanne E. Smrekar, Catherine L. Johnson, Aymeric Spiga, Peter Chi, Brigitte Knapmeyer-Endrun, Raphaël F. Garcia, Claire E. Newman, Seiichi Nagihara, Matthias Grott, W. Thomas Pike, Philippe Lognonné, Véronique Dehant, Ana-Catalina Plesa, Matthew Fillingim, Domenico Giardini, Taichi Kawamura, Mark T. Lemmon, Antoine Mocquet, Naomi Murdoch, Ebru Bozdag, David Mimoun, Ludovic Margerin, Matthew P. Golombek, Jessica C. E. Irving, Troy L. Hudson, Sami W. Asmar, Günter Kargl, Martin Knapmeyer, Mark P. Panning, Francis Nimmo, Scott D. King, John A. Grant, Sebastien Rodriguez, Martin van Driel, Nicholas H. Warner, Nils Mueller, José Antonio Rodríguez-Manfredi, Christopher T. Russell, Caroline Beghein, Clément Perrin, Ulrich R. Christensen, William M. Folkner, Renee Weber, Neil Bowles, Ingrid Daubar, Simon Stähler, Tilman Spohn, Eléanore Stutzmann, Ralph D. Lorenz, Matthew A. Siegler, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Cornell Center for Astrophysics and Planetary Science (CCAPS), Cornell University, 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, Ocean and Atmospheric Sciences [Vancouver] (EOAS), University of British Columbia (UBC), Département de géophysique spatiale et planétaire (DGSP (UMR_7096)), Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-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)-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), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), 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 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), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford [Oxford], Department of Geosciences [Princeton], Princeton University, Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Swiss Seismological Service [ETH Zurich] (SED), 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), Department of Earth Science and Engineering [Imperial College London], Imperial College London, Department of Earth, Environmental and Planetary Sciences [Providence], Brown University, Royal Observatory of Belgium [Brussels], Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Département Electronique, Optronique et Signal (DEOS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Institute of Remote Sensing and Geographic Information System (IRSGIS), School of Earth and Space Sciences [Beijing], Peking University [Beijing]-Peking University [Beijing], Austrian Academy of Sciences (OeAW), Graphics and Vision Research Laboratory (Graphics Lab), University of Otago [Dunedin, Nouvelle-Zélande], Deutsches Zentrum für Luft- und Raumfahrt (DLR), Space Science Institute [Boulder] (SSI), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Department of Geosciences, Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), AstraZeneca, Aeolis Research, Department of Earth and Planetary Sciences [Santa Cruz], University of California [Santa Cruz] (UCSC), Department of Geological Sciences, University of Florida [Gainesville], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), The Open University [Milton Keynes] (OU), Morton K. Blaustein Department of Earth and Planetary Sciences [Baltimore], Johns Hopkins University (JHU), School of Earth Sciences [Bristol], University of Bristol [Bristol], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), University of Southern California (USC), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), Cornell University [New York], 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, Ocean and Atmospheric Sciences [Vancouver] (UBC EOAS), 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), 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), 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), Royal Observatory of Belgium [Brussels] (ROB), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), 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), Southwest Research Institute [Boulder] (SwRI), 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), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University of California, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), NASA-California Institute of Technology (CALTECH), Institut de recherche pour le développement [IRD] : UR206-Muséum national d'Histoire naturelle (MNHN)-Sorbonne Université (SU)-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), 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), Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Centre National de la Recherche Scientifique (CNRS), University of Oxford, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UC Santa Cruz), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), 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), University of California (UC), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Tromp, J. [0000-0002-2742-8299], Rodríguez, S. [0000-0003-1219-0641], Lognonné, P. [0000-0002-1014-920X], Perrin, C. [0000-0002-7200-5682], Murdoch, N. [0000-0002-9701-4075], Knapmeyer, M. [0000-0003-0319-2514], Rodríguez Manfredi, J. A. [0000-0003-0461-9815], Spiga, A. [0000-0002-6776-6268], Panning, M. P. [0000-0002-2041-3190], García, R. [0000-0003-1460-6663], Johnson, C. [0000-0001-6084-0149], Stutzmann, E. [0000-0002-4348-7475], Knapmeyer-Endrun, B. [0000-0003-3309-6785], Schmerr, N. [0000-0002-3256-1262], Irving, J. C. E. [0000-0002-0866-8246], Morgan, P. [0000-0001-8714-4178], Mueller, N. [0000-0001-9229-8921], Pike, W. [0000-0002-7660-6231], Kawamura, T. [0000-0001-5246-5561], Clinton, J. [0000-0001-8626-2703], Agence Nationale de la Recherche (ANR), Swiss National Science Foundation (SNSF), Agence Nationale de la Recherche (ANR), ANR-10LABX-0023 ANR-11-IDEX-0005-0, Swiss National Science Foundation (SNSF- ANR project), 157133, ETH Research grant, ETH-06 17-02, Lunar and Planetary Institute, 2250, UCL - SST/ELI/ELIC - Earth & Climate, Science and Technology Facilities Council (STFC), and Science & Technology Facilities Council
Subjects: Seismometer, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, 010502 geochemistry & geophysics, 01 natural sciences, Atmosphere, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Impact crater, Autre, Planet, Inner planets, InSight Mars Geophysik, Meteorology & Atmospheric Sciences, Seismology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Atmospheric dynamics, Geomorphology, Moment magnitude scale, Mars InSight, Geomagnetism, Mars Exploration Program, Geophysics, [SDU]Sciences of the Universe [physics], 13. Climate action, Intraplate earthquake, General Earth and Planetary Sciences, Timekeeping on Mars, [SDU.OTHER]Sciences of the Universe [physics]/Other, InSight mission, Geology
Abstract: Banerdt, William B. et al., NASA’s InSight (Interior exploration using Seismic Investigations, Geodesy and Heat Transport) mission landed in Elysium Planitia on Mars on 26 November 2018. It aims to determine the interior structure, composition and thermal state of Mars, as well as constrain present-day seismicity and impact cratering rates. Such information is key to understanding the differentiation and subsequent thermal evolution of Mars, and thus the forces that shape the planet’s surface geology and volatile processes. Here we report an overview of the first ten months of geophysical observations by InSight. As of 30 September 2019, 174 seismic events have been recorded by the lander’s seismometer, including over 20 events of moment magnitude M = 3–4. The detections thus far are consistent with tectonic origins, with no impact-induced seismicity yet observed, and indicate a seismically active planet. An assessment of these detections suggests that the frequency of global seismic events below approximately M = 3 is similar to that of terrestrial intraplate seismic activity, but there are fewer larger quakes; no quakes exceeding M = 4 have been observed. The lander’s other instruments—two cameras, atmospheric pressure, temperature and wind sensors, a magnetometer and a radiometer—have yielded much more than the intended supporting data for seismometer noise characterization: magnetic field measurements indicate a local magnetic field that is ten-times stronger than orbital estimates and meteorological measurements reveal a more dynamic atmosphere than expected, hosting baroclinic and gravity waves and convective vortices. With the mission due to last for an entire Martian year or longer, these results will be built on by further measurements by the InSight lander., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)
Published: 2020

32. 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

33. The seismicity of Mars

Author: Simon Stähler, Anna Horleston, Sharon Kedar, John-Robert Scholz, L. Luno, J. B. McClean, Henri Samuel, Fabian Euchner, S. Barkaoui, Tristram Warren, Mélanie Drilleau, Martin Schimmel, Maren Böse, M. Nonon, M. van Driel, Nicholas A Teanby, Alexander E. Stott, Savas Ceylan, Ludovic Margerin, A. Jacob, Brigitte Knapmeyer-Endrun, William B. Banerdt, Guenole Mainsant, Tamara Gudkova, Antoine Lucas, T. Gabsi, Renee Weber, Taichi Kawamura, Vincent Conejero, Eléonore Stutzmann, Daniele Antonangeli, C. Agard, Constantinos Charalambous, C. Ferrier, P. Combes, K. Hurst, Philippe Lognonné, Don Banfield, Aymeric Spiga, William T. Pike, Constanza Pardo, J. A Rodriguez Manfredi, Martin Knapmeyer, Attilio Rivoldini, Francis Nimmo, U. R. Christensen, Sue Smrekar, Ingrid Daubar, R. Llorca-Cejudo, Mark P. Panning, Scott D. King, Eric Beucler, Foivos Karakostas, Amir Khan, E. Barrett, Mark A. Wieczorek, Raphaël F. Garcia, Clément Perrin, Naomi Murdoch, David Mimoun, C. Yana, John Clinton, Domenico Giardini, Swiss National Supercomputing Centre, Swiss National Science Foundation, Agence Nationale de la Recherche (France), State Secretariat for Education, Research and Innovation (Switzerland), UK Space Agency, California Institute of Technology, German Centre for Air and Space Travel, Schimmel, Martin, Centre National de la Recherche Scientifique (CNRS), 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), Institute of Geophysics [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), Institut de Physique du Globe de Paris, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Mechanical Engineering [Imperial College London], Imperial College London, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, INSTITUT OF GEOPHYSICS ETHZ, Swiss Seismological Service, Department of Earth and Environmental Sciences [München], Ludwig-Maximilians-Universität München (LMU), Department of Geological Sciences [Gainesville] (UF|Geological), University of Florida [Gainesville] (UF), Cornell University [New York], 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), European Academy-EURAC, Institute for Applied Remote Sensing, Kyoto University [Kyoto], Departments of Anesthesiology and Physiology and Biophysics, University of Alabama at Birmingham [ Birmingham] (UAB), 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), unité de recherche de l'institut du thorax UMR1087 UMR6291 (ITX), Université de Nantes - UFR de Médecine et des Techniques Médicales (UFR MEDECINE), Université de Nantes (UN)-Université de Nantes (UN)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), 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), De la Préhistoire à l'Actuel : Culture, Environnement et Anthropologie (PACEA), Université de Bordeaux (UB)-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), Schmidt United Institute of Physics of the Earth [Moscow] (IPE), Russian Academy of Sciences [Moscow] (RAS), NASA, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'Ingénierie des Matériaux (LIM), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), UNS-CNRS-Observatoire de la Côte d'Azur, Department of Earth and Planetary Sciences [Santa Cruz], University of California [Santa Cruz] (UCSC), University of California-University of California, School of Earth Sciences [Bristol], University of Bristol [Bristol], Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-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), 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), California Institute of Technology (CALTECH)-NASA, Department of Geological Sciences, University of Florida [Gainesville], Oncogenesis Stress Signaling (OSS), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-CRLCC Eugène Marquis (CRLCC), Cornell University, Université d'Angers (UA)-Université de Nantes - Faculté des Sciences et des Techniques, 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)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Université de Nantes - UFR de Médecine et des Techniques Médicales (UFR MEDECINE), Université de Nantes (UN)-Université de Nantes (UN), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), Schimmel, Martin [0000-0003-2601-4462], Department of Earth and Environmental Sciences [Munich], 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), Laboratoire de Géophysique Interne et Tectonophysique (LGIT), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Laboratoire Central des Ponts et Chaussées (LCPC)-Institut des Sciences de la Terre (ISTerre), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut national des sciences de l'Univers (INSU - CNRS)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique du Globe de Paris (IPG Paris), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), 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), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Unité de recherche de l'institut du thorax (ITX-lab), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-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)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and ANR-14-CE36-0012,SEISMARS,Seismology on Mars(2014)
Subjects: Seismometer, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, Induced seismicity, InSight Mars Marsbeben Seismizität, 010502 geochemistry & geophysics, seismology, 01 natural sciences, Mantle (geology), Elysium, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Autre, Planet, inner planets, ComputingMilieux_MISCELLANEOUS, Seismology, InSight, 0105 earth and related environmental sciences, Seismicity, Crust, Geology, Mars Exploration Program, [SDU]Sciences of the Universe [physics], 13. Climate action, General Earth and Planetary Sciences
Abstract: The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission landed in Elysium Planitia on Mars on 26 November 2018 and fully deployed its seismometer by the end of February 2019. The mission aims to detect, characterize and locate seismic activity on Mars, and to further constrain the internal structure, composition and dynamics of the planet. Here, we present seismometer data recorded until 30 September 2019, which reveal that Mars is seismically active. We identify 174 marsquakes, comprising two distinct populations: 150 small-magnitude, high-frequency events with waves propagating at crustal depths and 24 low-frequency, subcrustal events of magnitude Mw 3–4 with waves propagating at various depths in the mantle. These marsquakes have spectral characteristics similar to the seismicity observed on the Earth and Moon. We determine that two of the largest detected marsquakes were located near the Cerberus Fossae fracture system. From the recorded seismicity, we constrain attenuation in the crust and mantle, and find indications of a potential low-S-wave-velocity layer in the upper mantle. © 2020, The Author(s), under exclusive licence to Springer Nature Limited., We acknowledge NASA, CNES and its partner agencies and institutions (UKSA, SSO, DLR, JPL, IPGP-CNRS, ETHZ, IC and MPS-MPG) and the flight operations team at JPL, SISMOC, MSDS, IRIS-DMC and PDS for providing SEIS data. The Swiss co-authors were jointly funded by (1) the Swiss National Science Foundation and French Agence Nationale de la Recherche (SNF-ANR project 157133 ‘Seismology on Mars’), (2) the Swiss National Science Foundation (SNF project 172508 ‘Mapping the internal structure of Mars’), (3) the Swiss State Secretariat for Education, Research and Innovation (SEFRI project ‘MarsQuake Service-Preparatory Phase’) and (4) ETH Research grant no. ETH-06 17-02. Additional support came from the Swiss National Supercomputing Centre (CSCS) under project ID s922. The Swiss contribution in the implementation of the SEIS electronics was made possible by funding from the federal Swiss Space Office (SSO) and contractual and technical support from the ESA-PRODEX office. The French Team acknowledge the French Space Agency CNES, which has supported and funded all SEIS-related contracts and CNES employees, as well as CNRS and the French team universities for personal and infrastructure support. Additional support was provided by ANR (ANR-14-CE36-0012-02 and ANR-19-CE31-0008-08) and, for the IPGP team, by the UnivEarthS Labex programme (ANR-10-LABX-0023), IDEX Sorbonne Paris Cité (ANR-11-IDEX-0005-0). SEIS-SP development and delivery were funded by the UK Space Agency. A portion of the work was carried out at the InSight Project at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The MPS SEIS team acknowledges funding for development of the SEIS leveling system by the DLR German Space Agency. We thank gempa GmbH for software development related to the MQS tools. This paper is InSight contribution number 102.
Published: 2020

34. Preparing for InSight: An Invitation to Participate in a Blind Test for Martian Seismicity

Author: Mark P. Panning, M. van Driel, Naomi Murdoch, Philippe Lognonné, David Mimoun, B. Kenda, L. Perrin, Bruce Banerdt, Ingrid Daubar, Matthew P. Golombek, John Clinton, Jeroen Tromp, Mélanie Drilleau, Aymeric Spiga, Savas Ceylan, Maren Böse, Raphaël F. Garcia, Renee Weber, Amir Khan, Domenico Giardini, Centre National d'Études Spatiales - CNES (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), Sorbonne Université (FRANCE), University of Florida (USA), California Institute of Technology - Caltech (USA), Princeton University (USA), and Eidgenössische Technische Hochschule Zürich - ETHZ (SWITZERLAND)
Subjects: Martian, 010504 meteorology & atmospheric sciences, Team plan, Seismicity, Mars, Single station, Mars Exploration Program, Induced seismicity, 01 natural sciences, Test (assessment), InSight seismology geophysics noise Mars, Geophysics, Autre, 13. Climate action, 0103 physical sciences, Insight, Routine analysis, 010303 astronomy & astrophysics, Astrophysique, Geology, Seismology, 0105 earth and related environmental sciences
Abstract: The InSight (Interior exploration using Seismic Investigations, Geodesy and Heat Transport) lander will deploy a seismic monitoring package on Mars in November 2018. In prepara- tion for the data return, we prepared a blind test in which we invite participants to detect and characterize seismicity included in a synthetic dataset of continuous waveforms from a single station that mimics both the streams of data that will be available from InSight, as well as expected tectonic and impact seismicity and noise conditions on Mars. We expect that the test will ultimately improve and extend the current set of methods that the InSight team plan to use in routine analysis of the Martian dataset.
Published: 2017

35. Lunar Seismology: An Update on Interior Structure Models

Author: Renee Weber, Raphaël F. Garcia, Philippe Lognonné, Attilio Rivoldini, Ludovic Margerin, Mélanie Drilleau, Amir Khan, Daoyuan Sun, Ceri Nunn, Taichi Kawamura, Yosio Nakamura, Angela G. Marusiak, Mark A. Wieczorek, Peimin Zhu, Département Electronique, Optronique et Signal (DEOS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), 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), 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), Laboratoire de Géophysique Interne et Tectonophysique (LGIT), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Laboratoire Central des Ponts et Chaussées (LCPC)-Institut des Sciences de la Terre (ISTerre), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut national des sciences de l'Univers (INSU - CNRS)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), 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), 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 de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-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)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), 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), Institut des Sciences de la Terre (ISTerre), Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Royal Observatory of Belgium [Brussels] (ROB), and Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)
Subjects: 010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], KREEP, 01 natural sciences, Physics::Geophysics, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Autre, 0103 physical sciences, Range (statistics), Internal structure, Moon, 010303 astronomy & astrophysics, Seismology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Propagation of uncertainty, Spacecraft, business.industry, Astronomy and Astrophysics, Inversion (meteorology), Data set, Planetary science, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Space Science, business, [SDU.OTHER]Sciences of the Universe [physics]/Other, Geology
Abstract: International audience; An international team of researchers gathered, with the support of the Interna-tional Space Science Institute (ISSI), (1) to review seismological investigations of the lunarinterior from the Apollo-era and up until the present and (2) to re-assess our level of knowl-edge and uncertainty on the interior structure of the Moon. A companion paper (Nunn et al.in Space Sci. Rev., submitted) reviews and discusses the Apollo lunar seismic data with theaim of creating a new reference seismic data set for future use by the community. In thisstudy, we first review information pertinent to the interior of the Moon that has becomeavailable since the Apollo lunar landings, particularly in the past ten years, from orbitingspacecraft, continuing measurements, modeling studies, and laboratory experiments. Fol-lowing this, we discuss and compare a set of recent published models of the lunar interior,including a detailed review of attenuation and scattering properties of the Moon. Commonfeatures and discrepancies between models and moonquake locations provide a first esti-mate of the error bars on the various seismic parameters. Eventually, to assess the influenceof model parameterisation and error propagation on inverted seismic velocity models, aninversion test is presented where three different parameterisations are considered. For thispurpose, we employ the travel time data set gathered in our companion paper (Nunn et al. inSpace Sci. Rev., submitted). The error bars of the inverted seismic velocity models demon-strate that the Apollo lunar seismic data mainly constrain the upper- and mid-mantle struc-ture to a depth of ∼1200 km. While variable, there is some indication for an upper mantlelow-velocity zone (depth range 100–250 km), which is compatible with a temperature gradi-◦ent around 1.7 C/km. This upper mantle thermal gradient could be related to the presenceof the thermally anomalous region known as the Procellarum Kreep Terrane, which containsa large amount of heat producing elements.
Published: 2019

36. SEIS: Insight’s Seismic Experiment for Internal Structure of Mars

Author: L. Perrin, C. Bonjour, N. Toulemont, Jean-Luc Berenguer, G. Perez, James Wookey, A. G. Mukherjee, Hallie Gengl, Edward A. Miller, Delphine Faye, Antoine Mocquet, J. Sicre, B. Vella, D. Dilhan, C. Larigauderie, John C. Bousman, M. Nonon, Y. Bennour, Véronique Dehant, Jeffrey W. Umland, T. Nebut, D. Hernandez, M. Eberhardt, Vincent Conejero, Rudolf Widmer-Schnidrig, Philippe Lognonné, G. de los Santos, S. A. D’Agostino, Savas Ceylan, Justin N. Maki, G. Aveni, P. Revuz, S. de Raucourt, C. Aicardi, Clément Perrin, A. K. Delahunty, Constanza Pardo, Domenico Giardini, L. Pou, Robert J. Calvet, D. Savoie, O. Robert, V. Gharakanian, S. Ben Charef, Constantinos Charalambous, Kerry Klein, S. M. Madzunkov, J. M. Desmarres, Sue Smrekar, S. B. Calcutt, F. Grinblat, Nicholas A Teanby, I. M. Standley, Naomi Murdoch, Brigitte Knapmeyer-Endrun, M. Deleuze, C. Doucet, William T. Pike, Tom L. Hoffman, F. Mialhe, Cecily M. Sunday, J. Paredes-Garcia, Matthew P. Golombek, P. Bhandari, Huafeng Liu, B. Pouilloux, E. Blanco, Gabriel Pont, Simon Stähler, M. E. Johnson, Nicolas Verdier, L. Luno, Ned W. Ferraro, R. Perez, Mélanie Drilleau, F. Ijpelaan, B. Lecomte, M. van Driel, A. Sauron, I. Estève, Mark P. Panning, David Mimoun, P. A. Dandonneau, B. Kenda, T. Gabsi, W. Raff, P. Boutte, T. Warren, Joan Ervin, Fabian Euchner, S. Tillier, K. J. Hurst, Stephen Larson, Davor Mance, Mark A. Wieczorek, J. A. Rodriguez-Manfredi, Justin Lin, Jaime Singer, M. Monecke, Robert W. Denise, E.-P. Miettinen, Maren Böse, E. Locatelli, I. Savin de Larclause, J. Gagnepain-Beyneix, L. Khachikyan, Philippe Laudet, T. Carlier, Alexander E. Stott, Neil Bowles, Brian Bone, C. Imbert, Sharon Kedar, A. Rosak, Fred Calef, O. Pot, O. M. Avalos, P. Labrot, Jeroen Tromp, Lucile Fayon, C. Moreau, J. Baroukh, William B. Banerdt, M. Bierwirth, Ranah Irshad, M. André, Christopher T. Russell, S. L. Marshall, M. Parise, J.-R. Meyer, P. Pasquier, N. Faye-Refalo, Ingrid Daubar, M. A. Balzer, R. Gonzalez, M. Hetzel, K. Brethomé, Y. Pahn, Raphaël F. Garcia, J. tenPierick, U. R. Christensen, Farah Alibay, Renee Weber, Robert G. Deen, Eléonore Stutzmann, J. Temple, Don Banfield, A. Bouisset, D. B. Klein, A. Borrien, Ashitey Trebi-Ollennu, R. Llorca-Cejudo, L. J. Facto, J. M. Mouret, Alexis Paillet, Peter Zweifel, P. Bruneau, Catherine L. Johnson, C. Brysbaert, J. E. Feldman, A. Kramer, Luigi Ferraioli, Jane Hurley, Taichi Kawamura, Nicholas Onufer, W. Kühne, Eric Beucler, Amir Khan, M. Sodki, L. Kerjean, A. Sylvestre-Baron, C. Desfoux, C. Yana, John Clinton, J. R. Willis, Juan Villalvazo, Pierre Delage, Mihail P. Petkov, M. C. Wallace, T. Camus, Ioannis G. Mikellides, Institut de Physique du Globe de Paris (IPGP), 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), Institute of Geophysics [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), Department of Mechanical Engineering [Imperial College London], Imperial College London, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Centre National d'Études Spatiales [Toulouse] (CNES), Geological Institute (ETHZ), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Oxford, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), 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), NASA Marshall Space Flight Center (MSFC), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de Mecanique des Fluides et d'Acoustique (LMFA), École Centrale de Lyon (ECL), Université de Lyon-Université de Lyon-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), Advanced Technology and Research, Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Clarendon Laboratory [Oxford], Huazhong University of Science and Technology [Wuhan] (HUST), Kinemetrics, Cornell University [New York], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University of California [Los Angeles] (UCLA), University of California (UC), Institut of GeophysicsETHZ, 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]), Swiss Seismological Service, Royal Observatory of Belgium [Brussels] (ROB), Géotechnique (cermes), Laboratoire Navier (navier umr 8205), Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS), 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), University of British Columbia (UBC), Planetary Science Institute [Tucson] (PSI), Laboratoire national de métrologie et d'essais - Systèmes de Référence Temps-Espace (LNE - SYRTE), Systèmes de Référence Temps Espace (SYRTE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), University of Bristol [Bristol], Department of Geosciences [Princeton], Princeton University, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-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)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Universität Stuttgart [Stuttgart], School of Earth Sciences [Bristol], 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), Max-Planck-Institut für Sonnensystemforschung (MPS), University of Oxford [Oxford], Max Planck Institute for Solar System Research (MPS), 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)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of California, INSTITUT OF GEOPHYSICS ETHZ, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Karlsruhe Institute of Technology and Stuttgart University, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), California Institute of Technology (CALTECH)-NASA, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (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 Nice Sophia Antipolis (... - 2019) (UNS), 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), Département Electronique, Optronique et Signal (DEOS), 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), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), 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), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Cornell University, Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), 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), Royal Observatory of Belgium [Brussels], PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), School of Earth Sciences University of Bristol, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Seismometer, DISSIPATIVE FACTOR, 010504 meteorology & atmospheric sciences, FREE OSCILLATIONS, BULK COMPOSITION, Mars, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Astronomy & Astrophysics, 01 natural sciences, Transfer function, Article, NETWORK SCIENCE, Autre, 0103 physical sciences, 0201 Astronomical and Space Sciences, INTERIOR STRUCTURE, ddc:530, Ground segment, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, InSight, Data processing, Science & Technology, Physics, Bandwidth (signal processing), Mars seismology, Astronomy and Astrophysics, Moment magnitude scale, SINGLE-STATION, THERMAL EVOLUTION, Mars Exploration Program, Geodesy, Space and Planetary Science, Physical Sciences, WAVE PROPAGATION, ELYSIUM PLANITIA, [SDU.OTHER]Sciences of the Universe [physics]/Other, Robotic arm, SEIS, Geology, METEORITE IMPACTS
Abstract: By the end of 2018, 42 years after the landing of the two Viking seismometers on Mars, InSight will deploy onto Mars’ surface the SEIS (Seismic Experiment for Internal Structure) instrument; a six-axes seismometer equipped with both a long-period three-axes Very Broad Band (VBB) instrument and a three-axes short-period (SP) instrument. These six sensors will cover a broad range of the seismic bandwidth, from 0.01 Hz to 50 Hz, with possible extension to longer periods. Data will be transmitted in the form of three continuous VBB components at 2 sample per second (sps), an estimation of the short period energy content from the SP at 1 sps and a continuous compound VBB/SP vertical axis at 10 sps. The continuous streams will be augmented by requested event data with sample rates from 20 to 100 sps. SEIS will improve upon the existing resolution of Viking’s Mars seismic monitoring by a factor of ∼2500 at 1 Hz and ∼200000 at 0.1 Hz. An additional major improvement is that, contrary to Viking, the seismometers will be deployed via a robotic arm directly onto Mars’ surface and will be protected against temperature and wind by highly efficient thermal and wind shielding. Based on existing knowledge of Mars, it is reasonable to infer a moment magnitude detection threshold of Mw∼3 at 40∘ epicentral distance and a potential to detect several tens of quakes and about five impacts per year. In this paper, we first describe the science goals of the experiment and the rationale used to define its requirements. We then provide a detailed description of the hardware, from the sensors to the deployment system and associated performance, including transfer functions of the seismic sensors and temperature sensors. We conclude by describing the experiment ground segment, including data processing services, outreach and education networks and provide a description of the format to be used for future data distribution., Space Science Reviews, 215 (1), ISSN:1572-9672, ISSN:0038-6308
Published: 2019

37. 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

38. Pre-mission InSights on the Interior of Mars

Author: Mélanie Drilleau, O. Verhoeven, Matthew P. Golombek, Philippe Lognonné, Anna Mittelholz, Ana-Catalina Plesa, Antoine Mocquet, Benoit Langlais, Robert Myhill, Tamara Gudkova, T. Pike, Catherine L. Johnson, Henri Samuel, Suzanne E. Smrekar, Renee Weber, W. Bruce Banerdt, Martin van Driel, Domenico Giardini, Amir Khan, Tim Van Hoolst, William M. Folkner, Doris Breuer, Mark P. Panning, Véronique Dehant, Clément Perrin, Raphaël F. Garcia, Matthias Grott, Nobuaki Fuji, Ulrich R. Christensen, Mark A. Wieczorek, Simon Stähler, Tilman Spohn, Attilio Rivoldini, 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 Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), 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), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), 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), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-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), and UCL - SST/ELI/ELIC - Earth & Climate
Subjects: Convection, Solar System, 010504 meteorology & atmospheric sciences, Mars, crust, Volcanism, 01 natural sciences, Mantle (geology), Physics::Geophysics, Planetary internal structure, 0103 physical sciences, Thermal, Traitement du signal et de l'image, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, core, Crust, Astronomy and Astrophysics, Mars Exploration Program, Geophysics, interior structure, Planetary science, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, InSight, Interior, Seismology, Heat flow, Geodesy, Mantle, Core, [SPI.SIGNAL]Engineering Sciences [physics]/Signal and Image processing, Geology, mantle
Abstract: International audience; Abstract The Interior exploration using Seismic Investigations, Geodesy, and Heat Trans-port (InSight) Mission will focus on Mars’ interior structure and evolution. The basic structure of crust, mantle, and core form soon after accretion. Understanding the early differentiation process on Mars and how it relates to bulk composition is key to improving our understanding of this process on rocky bodies in our solar system, as well as in other solar systems. Current knowledge of differentiation derives largely from the layers observed via seismology on the Moon. However, the Moon’s much smaller diameter make it a poor analog with respect to interior pressure and phase changes. In this paper we review the current knowledge of the thickness of the crust, the diameter and state of the core, seismic attenuation, heat flow, and interior composition. InSight will conduct the first seismic and heat flow measurements of Mars, as well as more precise geodesy. These data reduce uncertainty in crustal thickness, core size and state, heat flow, seismic activity and meteorite impact rates by a factor of 3–10× relative to previous estimates. Based on modeling of seismic wave propagation, we can further constrain interior temperature, composition, and the location of phase changes. By combining heat flow and a well constrained value of crustal thickness, we can estimate the distribution of heat producing elements between the crust and mantle. All of these quantities are key inputs to models of interior convection and thermal evolution that predict the processes that control subsurface temperature, rates of volcanism, plume distribution and stability, and convective state. Collectively these factors offer strong controls on the overall evolution of the geology and habitability of Mars.
Published: 2019

39. 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

40. The Marsquake Service: Securing Daily Analysis of SEIS Data and Building the Martian Seismicity Catalogue for InSight

Author: Mélanie Drilleau, Bruce Banerdt, John Clinton, Brigitte Knapmeyer-Endrun, Nicholas A Teanby, Antoine Mocquet, Domenico Giardini, M. van Driel, Sharon Kedar, David Mimoun, Raphaël F. Garcia, Taichi Kawamura, Fabian Euchner, Philippe Lognonné, Clément Perrin, Maren Böse, Matthew P. Golombek, Martin Knapmeyer, Mark P. Panning, Eric Beucler, Amir Khan, Simon Stähler, Savas Ceylan, Ingrid Daubar, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (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), 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), 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), 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, and Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA)
Subjects: Seismometer, 010504 meteorology & atmospheric sciences, Mars, Training healthcare professionals, Induced seismicity, computer.software_genre, 01 natural sciences, Martian seismicity, Autre, Observatory, Qualitative research, 0103 physical sciences, Seismologie, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, InSight, Marsquakes, Martian, Event (computing), Communication, Seismicity, Astronomy and Astrophysics, Mars Exploration Program, Clinical trial, Software framework, 13. Climate action, Space and Planetary Science, Impacts, Randomized Controlled Trial, Recruitment, Scale (map), [SDU.OTHER]Sciences of the Universe [physics]/Other, computer, SEIS, Geology, Seismology
Abstract: International audience; The InSight mission expects to operate a geophysical observatory on Mars for at least two Earth years from late 2018. InSight includes a seismometer package, SEIS. The Marsquake Service (MQS) is created to provide a first manual review of the seismic data returned from Mars. The MQS will detect, locate, quantify and classify seismic events, whether tectonic or impact in origin. A suite of new and adapted methodologies have been developed to allow location and quantification of seismic events at the global scale using a single station, and a software framework has been developed that supports these methods. This paper describes the expected signals that will be recorded by SEIS, the methods used for their identification and interpretation, and reviews the planned MQS operational procedures. For each seismic event, the MQS will locate events using all available body and surface phases, using the best estimates of the Martian structure, which will become more accurate as more Martian marsquakes are identified and located. The MQS will curate the Mars seismicity catalogue, with all events being relocated to use revised suites of structure models as they are introduced.
Published: 2018

41. 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

42. 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

43. On the Detectability and Use of Normal Modes for Determining Interior Structure of Mars

Author: Philippe Lognonné, Domenico Giardini, Simon Stähler, Mélanie Drilleau, Tamara Gudkova, Felix Bissig, V. N. Zharkov, Amir Khan, Ana-Catalina Plesa, Martin van Driel, William B. Banerdt, Mark P. Panning, Swiss Fed Inst Technol, Inst Geophys, Sonneggstr 5, CH-8092 Zurich, Switzerland, Institute of Geophysics [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), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), 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), Schmidt Institute of Physics of the Earth of the Russian Academy of Sciences (IPE RAS), Bolshaya Gruzinskaya Str. 10-1, 123242 Moscow, Russia, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA, and Swiss National Science Foundation (SNSF) 200021_172508 Swiss National Supercomputing Centre (CSCS) s830
Subjects: Mars, Seismology, Normal modes, Interior structure, Inverse problems, 010504 meteorology & atmospheric sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], BULK COMPOSITION, Geometry, WAVE-FORMS, 010502 geochemistry & geophysics, 01 natural sciences, Spectral line, Inverse problems KeyWords Plus:FREE OSCILLATIONS, Normal mode, Interior Structure, LUNAR INTERIOR, Range (statistics), EARTH, MARTIAN SEISMICITY, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, TORSIONAL OSCILLATIONS, Series (mathematics), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Autocorrelation, Astronomy and Astrophysics, SINGLE-STATION, Mars Exploration Program, INSIGHT MISSION, MANTLE MINERALS, Data set, Normal Modes, Space and Planetary Science, Surface wave, [SDU]Sciences of the Universe [physics], Author Keywords:Mars
Abstract: The InSight mission to Mars is well underway and will be the first mission to acquire seismic data from a planet other than Earth. In order to maximise the science return of the InSight data, a multifaceted approach will be needed that seeks to investigate the seismic data from a series of different frequency windows, including body waves, surface waves, and normal modes. Here, we present a methodology based on globally-averaged models that employs the long-period information encoded in the seismic data by looking for fundamental-mode spheroidal oscillations. From a preliminary analysis of the expected signal-to-noise ratio, we find that normal modes should be detectable during nighttime in the frequency range 5–15 mHz. For improved picking of (fundamental) normal modes, we show first that those are equally spaced between 5–15 mHz and then show how this spectral spacing, obtained through autocorrelation of the Fourier-transformed time series can be further employed to select normal mode peaks more consistently. Based on this set of normal-mode spectral frequencies, we proceed to show how this data set can be inverted for globally-averaged models of interior structure (to a depth of $\sim 250~\mbox{km}$ ), while simultaneously using the resultant synthetically-approximated normal mode peaks to verify the initial peak selection. This procedure can be applied iteratively to produce a “cleaned-up” set of spectral peaks that are ultimately inverted for a “final” interior-structure model. To investigate the effect of three-dimensional (3D) structure on normal mode spectra, we constructed a 3D model of Mars that includes variations in surface and Moho topography and lateral variations in mantle structure and employed this model to compute full 3D waveforms. The resultant time series are converted to spectra and the inter-station variation hereof is compared to the variation in spectra computed using different 1D models. The comparison shows that 3D effects are less significant than the variation incurred by the difference in radial models, which suggests that our 1D approach represents an adequate approximation of the global average structure of Mars.
Published: 2018

44. Verifying single-station seismic approaches using Earth-based data: Preparation for data return from the InSight mission to Mars

Author: Mark P. Panning, Mélanie Drilleau, Eric Beucler, Antoine Mocquet, W. Bruce Banerdt, Philippe Lognonné, Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA, 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 (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), 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), NASA-California Institute of Technology (CALTECH), and NASA/JPL as part of the InSight mission Centre National D'etudes Spatiales
Subjects: Martian, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Mars, Earth, Astronomy and Astrophysics, Mars Exploration Program, Geodesy, Mantle (geology), Physics::Geophysics, Azimuth, symbols.namesake, Tectonics, Interior, Geophysics, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, Observatory, Surface wave, Physics::Space Physics, symbols, Astrophysics::Earth and Planetary Astrophysics, Rayleigh wave, Geology, Remote sensing
Abstract: International audience; The planned InSight mission will deliver a single seismic station containing 3-component broadband and short-period sensors to the surface of Mars in 2016. While much of the progress in understanding the Earth and Moon's interior has relied on the use of seismic networks for accurate location of sources, single station approaches can be applied to data returned from Mars in order to locate events and determine interior structure. In preparation for the data return from Insight, we use a terrestrial dataset recorded at the Global Seismic Network station BFO, located at the Black Forest Observatory in Germany, to verify an approach for event location and structure determination based on recordings of multiple orbit surface waves, which will be more favorable to record on Mars than Earth due to smaller planetary radius and potentially lower background noise. With this approach applied to events near the threshold of observability on Earth, we are able to determine epicentral distance within approximately 1 degrees (corresponding to similar to 60 km on Mars), and origin time within similar to 30 s. With back azimuth determined from Rayleigh wave polarization, absolute locations are determined generally within an aperture of 10 degrees, allowing for localization within large tectonic regions on Mars. With these locations, we are able to recover Earth mantle structure within +/- 5% (the InSight mission requirements for martian mantle structure) using ID travel time inversions of P and S travel times for datasets of only 7 events. The location algorithm also allows for the measurement of great-circle averaged group velocity dispersion, which we measure between 40 and 200 s to scale the expected reliable frequency range of the InSight data from Earth to Mars data. Using the terrestrial data, we are able to resolve structure down to similar to 200 km, but synthetic tests demonstrate we should be able to resolve martian structure to similar to 400 km with the same frequency content given the smaller planetary size. (C) 2014 Elsevier Inc. All rights reserved.
Published: 2015

45. Planned Products of the Mars Structure Service for the InSight Mission to Mars

Author: Antoine Mocquet, Nicholas A Teanby, O. Verhoeven, John Clinton, Atillio Rivoldini, Martin Knapmeyer, Chao Gao, W. Thomas Pike, Mark P. Panning, James Wookey, Renee Weber, Y. Ruan, Ebru Bozdag, Mélanie Drilleau, Véronique Dehant, Brigitte Knapmeyer-Endrun, Domenico Giardini, Raphaël F. Garcia, Tamara Gudkova, J. F. Blanchette-Guertin, Nicholas Schmerr, W. Bruce Banerdt, Naomi Murdoch, Jeroen Tromp, Ulrich R. Christensen, Matthew P. Golombek, Vedran Lekic, David Mimoun, Stefanie Hempel, Mark A. Wieczorek, Eric Beucler, Amir Khan, Philippe Lognonné, Sharon Kedar, Sue Smrekar, Ana-Catalina Plesa, University of Florida [Gainesville] (UF), 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), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, 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), School of Earth Sciences [Bristol], University of Bristol [Bristol], Department of Geosciences [Princeton], Princeton University, NASA Marshall Space Flight Center (MSFC), Géoazur (GEOAZUR 7329), Université Côte d'Azur (UCA)-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)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Schmidt United Institute of Physics of the Earth [Moscow] (IPE), Russian Academy of Sciences [Moscow] (RAS), Moscow Institute of Physics and Technology [Moscow] (MIPT), Institute of Geophysics [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), Department of Geology [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Royal Observatory of Belgium [Brussels] (ROB), Swiss Seismological Service, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Department of Electronic & Electrical Engineering [London], University College of London [London] (UCL), Deutsches Zentrum für Luft- und Raumfahrt [Bonn] (DLR), 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), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), 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]), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), University of Florida [Gainesville], 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), 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), 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), 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), Royal Observatory of Belgium [Brussels], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), and UK Space Agency
Subjects: Seismometer, RECEIVER-FUNCTION, 010504 meteorology & atmospheric sciences, Mars · Seismology · Interior structure · InSight mission, FREE OSCILLATIONS, Mars, Seismology, Interior structure, InSight mission, Astronomy & Astrophysics, 010502 geochemistry & geophysics, 01 natural sciences, RAYLEIGH-WAVE ELLIPTICITY, CERBERUS FOSSAE, Physics::Geophysics, MONTE-CARLO INVERSION, symbols.namesake, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Autre, APOLLO SEISMIC DATA, Rayleigh wave, 0105 earth and related environmental sciences, Radio Science, Remote sensing, Martian, Science & Technology, UPPER-MANTLE, Astronomy and Astrophysics, Observable, Geophysics, Mars Exploration Program, Planetary Data System, 0201 Astronomical And Space Sciences, SPECTRAL-ELEMENT SIMULATIONS, 13. Climate action, Space and Planetary Science, Surface wave, Physical Sciences, symbols, AMBIENT VIBRATION MEASUREMENTS, Astrophysics::Earth and Planetary Astrophysics, [SDU.OTHER]Sciences of the Universe [physics]/Other, Geology
Abstract: International audience; The InSight lander will deliver geophysical instruments to Mars in 2018, including seismometers installed directly on the surface (Seismic Experiment for Interior Structure, SEIS). Routine operations will be split into two services, the Mars Structure Service(MSS) and Marsquake Service (MQS), which will be responsible, respectively, for defining the structure models and seismicity catalogs from the mission. The MSS will deliver a series of products before the landing, during the operations, and finally to the Planetary Data System (PDS) archive. Prior to the mission, we assembled a suite of a priori models of Mars, based on estimates of bulk composition and thermal profiles. Initial models during the mission will rely on modeling surface waves and impact-generated body waves independent of prior knowledge of structure. Later modeling will include simultaneous inversion of seismic observations for source and structural parameters. We use Bayesian inversion techniques to obtain robust probability distribution functions of interior structure parameters. Shallow structure will be characterized using the hammering of the heatflow probe mole, as well as measurements of surface wave ellipticity. Crustal scale structure will be constrained by measurements of receiver function and broadband Rayleigh wave ellipticity measurements. Core interacting body wave phases should be observable above modeled martian noise levels, allowing us to constrain deep structure. Normal modes of Mars should also be observable and can be used to estimate the globally averaged 1D structure, while combination with results from the InSight radio science mission and orbital observations will allow for constraint of deeper structure.
Published: 2017

46. Reassessment of the rifting process in the Western Corinth Rift from relocated seismicity

Author: Mélanie Drilleau, G. Patau, Anne Deschamps, Seid Bourouis, Petra Adamová, Franchesco Pacchiani, Pascal Bernard, S. Lambotte, Alexandre Nercessian, Hélène Lyon-Caen, Institut de physique du globe de Strasbourg (IPGS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de géologie de l'ENS (LGE), Institut national des sciences de l'Univers (INSU - CNRS)-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), Département de sismologie (DS (UMR_7580)), IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (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]), Centre de Recherche en Astronomie Astrophysique et Géophysique (CRAAG), CRLNET, ANR-10-BLAN-0619,SISCOR,Aléas, dynamique SISmogène, et couplages sismiques/asismiques d'un systeme de faille actives dans la région ouest du Rift de CORinthe, Grèce(2010), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-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), 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]), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire de géologie de l'ENS (LGENS), Institut de Physique du Globe de Paris (IPGP), and 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)
Subjects: [SDU.STU.TE]Sciences of the Universe [physics]/Earth Sciences/Tectonics, geography, geography.geographical_feature_category, Rift, Dynamics and mechanics of faulting, 010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Continental tectonics: extensional, Crust, Active fault, Induced seismicity, Fault (geology), Geneva, Seismicity and tectonics, 010502 geochemistry & geophysics, Blind thrust earthquake, 01 natural sciences, Pore water pressure, Geophysics, Geochemistry and Petrology, Submarine pipeline, Geology, Seismology, Switzerland, 0105 earth and related environmental sciences
Abstract: International audience; The seismic activity in the western part of the Corinth Rift (Greece) over the period 2000– 2007, monitored by a dense network of three-component stations, is analysed in terms of multiplets and high precision relocation using double difference techniques. This detailed analysis provides new insights into the geometry of faults at depth, the nature and the structure of the active zone at 6–8 km depth previously interpreted as a possible detachment, and more generally into the rifting process. The seismicity exhibits a complex structure, strongly varying along the rift axis. The detailed picture of the seismic zone below the rift indicates that its shallower part (at depths of 6–8 km) is 1–1.5 km thick with a complex microstructure, and that its deeper part (at depths of 9–12 km) gently dipping to the north (10–20°) is 0.1–0.3 km thick with a microstructure consistent with the general slope of the structure. Although the nature of this seismic zone remains an open question, the presence of seismicity beneath the main active area, the strong variability of the structure along the rift over short distances and the complex microstructure of the shallower part revealed by the multiplet analysis are arguments against the hypothesis of a mature detachment under the rift: this active zone more likely represents a layer of diffuse deformation. The geometry of the mapped active faults is not well defined at depth, as no seismicity is observed between 0 and 4 km, except for the Aigion Fault rooting in the seismic layer at 6 km depth with a dip of 60°. A distinct cloud of seismicity may be associated with the antithetic Kalithea Fault, on which the 1909 Fokis earthquake (M s = 6.3) may have occurred. The link between the 1995 rupture (M s = 6.2) and the faults known at the surface has been better constrained, as the relocated seismicity favours a rupture on an offshore, blind fault dipping at 30° , rather than on the deeper part of the East Helike Fault. Consequently, the 1995 event is expected to have decreased the Coulomb stress on the East Helike Fault. To explain these seismic observations along with the geodetic observations, a new mechanical model for the rifting process in this region is proposed, involving non-elastic, mostly aseismic uniform NS opening below the rift axis, coupled with the downward and northward growth of a yet immature detachment: the reported GPS rates would mainly result from this deep, silent source, and the seismicity would reveal the detachment position, not yet connected to the ductile lower crust. In such a model, the strong fluctuations of microseismicity would result from small strain instabilities, undetected by continuous GPS and possibly related to pore pressure transients.
Published: 2014

47. Oceanic lithosphere-asthenosphere boundaryfrom surface wave dispersion data

Author: Mélanie Drilleau, Yann Capdeville, Gael Burgos, E. Beucler, Antoine Mocquet, J. P. Montagner, 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), Université de Nantes (UN), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), and Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Geophysics, Physics::Geophysics, Azimuth, Amplitude, 13. Climate action, Space and Planetary Science, Geochemistry and Petrology, Lithosphere, Surface wave, Oceanic crust, [SDU]Sciences of the Universe [physics], Earth and Planetary Sciences (miscellaneous), 14. Life underwater, Shear velocity, Anisotropy, Geology, Lithosphere-Asthenosphere boundary
Abstract: According to different types of observations, the nature of lithosphere-asthenosphere boundary (LAB) is controversial. Using a massive data set of surface wave dispersions in a broad period range (15–300 s), we have developed a three-dimensional upper mantle tomographic model (first-order perturbation theory) at the global scale. This is used to derive maps of the LAB from the resolved elastic parameters. The key effects of shallow layers and anisotropy are taken into account in the inversion process. We investigate LAB distribution primarily below the oceans, according to different kinds of proxies that correspond to the base of the lithosphere from the shear velocity variation at depth, the amplitude radial anisotropy, and the changes in azimuthal anisotropy G orientation. The estimations of the LAB depth based on the shear velocity increase from a thin lithosphere (∼20 km) in the ridges, to a thick old-ocean lithosphere (∼120–130 km). The radial anisotropy proxy shows a very fast increase in the LAB depth from the ridges, from ∼50 km to the older ocean where it reaches a remarkable monotonic subhorizontal profile (∼70–80 km). The LAB depths inferred from the azimuthal anisotropy proxy show deeper values for the increasing oceanic lithosphere (∼130–135 km). The difference between the evolution of the LAB depth with the age of the oceanic lithosphere computed from the shear velocity and azimuthal anisotropy proxies and from the radial anisotropy proxy raises questions about the nature of the LAB in the oceanic regions and of the formation of the oceanic plates
Published: 2013

48. A Bayesian approach to infer radial models of temperature and anisotropy in the transition zone from surface wave dispersion curves

Author: Mélanie Drilleau, Gael Burgos, O. Verhoeven, Pierre Vacher, G. Moebs, J. P. Montagner, Eric Beucler, Antoine Mocquet, 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), Département de Mathématiques et Informatique - Université de Nantes, Université de Nantes (UN), 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), 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), and 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)
Subjects: Equation of state, Phase transition, Seismic anisotropy, 010504 meteorology & atmospheric sciences, Bayesian probability, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Geometry, 010502 geochemistry & geophysics, 01 natural sciences, Physics::Geophysics, Geochemistry and Petrology, Transition zone, Inverse theory, Dispersion (water waves), Anisotropy, 0105 earth and related environmental sciences, Geophysics, Probability distributions, Surface wave, Phase transitions, [SDU]Sciences of the Universe [physics], Surface waves and free oscillations, Geology
Abstract: International audience; Mineralogical transformations and material transfers within the Earth's mantle make the 350-1000 km depth range (referred here as the mantle transition zone) highly heterogeneous and anisotropic. Most of the 3-D global tomographic models are anchored on small perturbations from 1-D models such as PREM, and are secondly interpreted in terms of temperature and composition distributions. However, the degree of heterogeneity in the transition zone can be strong enough so that the concept of a 1-D reference seismic model must be addressed. To avoid the use of any seismic reference model, we present in this paper a Markov chain Monte Carlo algorithm to directly interpret surface wave dispersion curves in terms of temperature and radial anisotropy distributions, here considering a given composition of the mantle. These interpretations are based on laboratory measurements of elastic moduli and Birch-Murnaghan equation of state. An originality of the algorithm is its ability to explore both smoothly varying models and first-order discontinuities, using C1-Bézier curves, which interpolate the randomly chosen values for depth, temperature and radial anisotropy. This parametrization is able to generate a self-adapting parameter space exploration while reducing the computing time. Thanks to a Bayesian exploration, the probability distributions on temperature and anisotropy are governed by uncertainties on the data set. The method is applied to both synthetic data and real dispersion curves. Though surface wave data are weakly sensitive to the sharpness of the of the mid-mantle seismic discontinuities, the interpretation of the temperature distribution is highly related to the chosen composition and to the modelling of mineralogical phase transformations. Surface wave measurements along the Vanuatu-California path suggest a strong anisotropy above 400 km depth, which decreases below, and a monotonous temperature distribution between 350 and 1000 km depth.
Published: 2013

49. Seismic Noise Autocorrelations on Mars

Author: Martin Schimmel, Eleonore Stutzmann, Philippe Lognonné, Nicolas Compaire, Paul Davis, Melanie Drilleau, Raphael Garcia, Doyeon Kim, Brigitte Knapmeyer‐Endrun, Vedran Lekic, Ludovic Margerin, Mark Panning, Nicholas Schmerr, John Robert Scholz, Aymeric Spiga, Benoit Tauzin, and Bruce Banerdt
Subjects: Astronomy, QB1-991, Geology, QE1-996.5
Abstract: Abstract Mars is the first extraterrestrial planet with seismometers (Seismic Experiment for Interior Structure, SEIS) deployed directly on its surface in the framework of the Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) mission. The lack of strong Marsquakes, however, strengthens the need of seismic noise studies to additionally constrain the Martian structure. Seismic noise autocorrelations of single‐station recordings permit the determination of the zero‐offset reflection response underneath SEIS. We present a new autocorrelation study which employs state‐of‐the‐art approaches to determine a robust reflection response by avoiding bias from aseismic signals which are recorded together with seismic waves due to unfavorable deployment and environmental conditions. Data selection and segmentation is performed in a data‐adaptive manner which takes the data root‐mean‐square amplitude variability into account. We further use the amplitude‐unbiased phase cross‐correlation and work in the 1.2–8.9 Hz frequency band. The main target are crustal scale reflections, their robustness and convergence. The strongest signal appears at 10.6 s, and, if interpreted as a P‐wave reflection, would correspond to a discontinuity at about 21 km depth. This signal is a likely candidate for a reflection from the base of the Martian crust due to its strength, polarity, and stability. Additionally we identify, among the stable signals, a signal at about 6.15 s that can be interpreted as the P‐wave reflection from the mid‐crust at about 9.5 km depth.
Published: 2021
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50. The interior of Mars constrained by Love and Rayleigh wave joint inversion scheme.

Author: Beucler, Éric, Mélanie, Drilleau, Khan, Amir, Panning, Mark, Lognonné, Philippe, Mocquet, Antoine, van Driel, Martin, Kenda, Balthasar, Murdoch, Naomi, Bonnin, Mickaël, Clinton, John, Böse, Maren, Ceylan, Savas, Stähler, Simon, Kedar, Sharon, Horleston, Anna, Kawamura, Taichi, and Banerdt, Bruce
Subjects: *RAYLEIGH waves, *SEISMIC waves, *SERVICES for blind people, *MARS (Planet), *STRUCTURAL frames
Abstract: The upper part of the Mars’ interior (comprising crust and upper mantle) can be described byclassical well-known elastic isotropic parameters (V P, V S, and ρ) and further byinferring additional anisotropic parameters carried by seismic waveforms. In theview of providing a mean 1D reference model for at least the ﬁrst 300 km of theMars’ interior, surface waves are well-suited since they are travelling guided bythe planet’s surface. At ﬁrst order, the dispersive property of these waves reﬂectsradial heterogeneities of the sampled medium, integrated along the travel path.In the event of a marsquake, the surface waves are propagating along minor- andmajor arcs then providing informations on diﬀerent media. Although Rayleighwaves are widely used to infer the isotropic seismic structure, Love waves can beused to constrain anisotropy. Since azimuthal dependence of seismic waves cannotbe resolved with a single station as InSight, only the polarization anisotropy canbe retrieve. In the framework of the Mars Structure Service blind test, providinga single event dataset, we present results and show that vertical polarization ofS-waves signiﬁcantly diﬀers from horizontal only within the ﬁrst 20 km depth. Thetransverse anisotropy measured by η seems to be inexistent in the input model. [ABSTRACT FROM AUTHOR]
Published: 2019

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