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1. Detection, Analysis, and Removal of Glitches From InSight's Seismic Data From Mars

Author

John‐Robert Scholz, Rudolf Widmer‐Schnidrig, Paul Davis, Philippe Lognonné, Baptiste Pinot, Raphaël F. Garcia, Kenneth Hurst, Laurent Pou, Francis Nimmo, Salma Barkaoui, Sébastien de Raucourt, Brigitte Knapmeyer‐Endrun, Martin Knapmeyer, Guénolé Orhand‐Mainsant, Nicolas Compaire, Arthur Cuvier, Éric Beucler, Mickaël Bonnin, Rakshit Joshi, Grégory Sainton, Eléonore Stutzmann, Martin Schimmel, Anna Horleston, Maren Böse, Savas Ceylan, John Clinton, Martin van Driel, Taichi Kawamura, Amir Khan, Simon C. Stähler, Domenico Giardini, Constantinos Charalambous, Alexander E. Stott, William T. Pike, Ulrich R. Christensen, and W. Bruce Banerdt

Subjects
InSight, seismometer, Mars, data processing, glitches, removal, Astronomy, QB1-991, Geology, QE1-996.5
Abstract

Abstract The instrument package SEIS (Seismic Experiment for Internal Structure) with the three very broadband and three short‐period seismic sensors is installed on the surface on Mars as part of NASA's InSight Discovery mission. When compared to terrestrial installations, SEIS is deployed in a very harsh wind and temperature environment that leads to inevitable degradation of the quality of the recorded data. One ubiquitous artifact in the raw data is an abundance of transient one‐sided pulses often accompanied by high‐frequency spikes. These pulses, which we term “glitches”, can be modeled as the response of the instrument to a step in acceleration, while the spikes can be modeled as the response to a simultaneous step in displacement. We attribute the glitches primarily to SEIS‐internal stress relaxations caused by the large temperature variations to which the instrument is exposed during a Martian day. Only a small fraction of glitches correspond to a motion of the SEIS package as a whole caused by minuscule tilts of either the instrument or the ground. In this study, we focus on the analysis of the glitch+spike phenomenon and present how these signals can be automatically detected and removed from SEIS's raw data. As glitches affect many standard seismological analysis methods such as receiver functions, spectral decomposition and source inversions, we anticipate that studies of the Martian seismicity as well as studies of Mars' internal structure should benefit from deglitched seismic data.

Published
2020
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2. 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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6. Resonances and Lander Modes Observed by InSight on Mars (1–9 Hz)

Author

Naomi Murdoch, Philippe Lognonné, Constantinos Charalambous, Nikolaj Dahmen, A. Stott, John-Robert Scholz, Martin Schimmel, Simon Stähler, Savas Ceylan, John Clinton, Géraldine Zenhäusern, Martin van Driel, Cedric Schmelzbach, Domenico Giardini, Sharon Kedar, William T. Pike, Eléonore Stutzmann, Robert Myhill, Mark P. Panning, William B. Banerdt, K. J. Hurst, National Aeronautics and Space Administration (US), Centre National D'Etudes Spatiales (France), State Secretariat for Education, Research and Innovation (Switzerland), Centre National de la Recherche Scientifique (France), Schimmel, Martin [0000-0003-2601-4462], and Schimmel, Martin

Subjects
Engineering, business.industry, Flight operations, Library science, marsquakes, Mars Exploration Program, Planetary Data System, nSight seismic data, Geophysics, Geochemistry and Petrology, Center (algebra and category theory), Planet Mars, business
Abstract

NASA's InSight lander successfully touched down on Mars in November 2018, and, for the first time, a seismometer was deployed on the surface of the planet. The seismic recordings reveal diurnal and seasonal changes of the broadband noise level that are consistent with variations of the local atmospheric conditions. The seismic data include a variety of spectral peaks, which are interpreted as wind‐excited, mechanical resonances of the lander, resonances of the subsurface, or artifacts produced in the measurement system. Understanding the origin of these signals is critical for the detection and characterization of marsquakes as well as for studies investigating the ambient noise. We identify the major spectral peaks up to 9 Hz, corresponding to the frequency range the most relevant to observed marsquakes. We track the variations in frequency, amplitude, and polarization of these peaks over the duration of the mission so far. The majority of these peaks can readily be classified as measurement artifacts or lander resonances (lander modes), of which the latter have a temperature‐dependent peak frequency and a wind‐sensitive amplitude. Of particular interest is a prominent resonance at 2.4 Hz, which is used to discriminate between seismic events and local noise and is possibly produced by a subsurface structure. In contrast to the lander modes, the 2.4 Hz resonance has distinctly different features: (1) a broad and stable spectral shape, slightly shifted on each component; (2) predominantly vertical energy; (3) temperature‐independent peak frequency; (4) comparatively weak amplification by local winds, though there is a slow change in the diurnal and seasonal amplitude; and (5) excitation during all seismic events that excite this frequency band. Based on these observations, we suggest that the 2.4 Hz resonance is the only mode below 9 Hz that could be related to a local ground structure., Bulletin of the Seismological Society of America, 111 (6), ISSN:0037-1106, ISSN:1943-3573

Published
2021

7. 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

8. The marsquake catalogue from InSight, sols 0-1011

Author

Savas Ceylan, John F. Clinton, Domenico Giardini, Simon C. Stähler, Anna Horleston, Taichi Kawamura, Maren Böse, Constantinos Charalambous, Nikolaj L. Dahmen, Martin van Driel, Cecilia Durán, Fabian Euchner, Amir Khan, Doyeon Kim, Matthieu Plasman, John-Robert Scholz, Géraldine Zenhäusern, Eric Beucler, Raphaël F. Garcia, Sharon Kedar, Martin Knapmeyer, Philippe Lognonné, Mark P. Panning, Clément Perrin, William T. Pike, Alexander E. Stott, and William B. Banerdt

Subjects
Mars InSight Seismische Aktivität, Geophysics, Physics and Astronomy (miscellaneous), Space and Planetary Science, Astronomy and Astrophysics
Abstract

The InSight mission (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) has been collecting high-quality seismic data from Mars since February 2019, shortly after its landing. The Marsquake Service (MQS) is the team responsible for the prompt review of all seismic data recorded by the InSight's seismometer (SEIS), marsquake event detection, and curating seismicity catalogues. Until sol 1011 (end of September 2021), MQS have identified 951 marsquakes that we interpret to occur at regional and teleseismic distances, and 1062 very short duration events that are most likely generated by local thermal stresses nearby the SEIS package. Here, we summarize the seismic data collected until sol 1011, version 9 of the InSight seismicity catalogue. We focus on the significant seismicity that occurred after sol 478, the end date of version 3, the last catalogue described in a dedicated paper. In this new period, almost a full Martian year of new data has been collected, allowing us to observe seasonal variations in seismicity that are largely driven by strong changes in atmospheric noise that couples into the seismic signal. Further, the largest, closest and most distant events have been identified, and the number of fully located events has increased from 3 to 7. In addition to the new seismicity, we document improvements in the catalogue that include the adoption of InSight-calibrated Martian models and magnitude scales, the inclusion of additional seismic body-wave phases, and first focal mechanism solutions for three of the regional marsquakes at distances ∼30°.

Published
2022

9. Seismic High-Resolution Acquisition Electronics for the NASA InSight Mission on Mars

Author

William T. Pike, W. Bruce Banerdt, John Clinton, M. Bierwirth, Thomas Haag, Philippe Lognonné, Fabian Euchner, David Sollberger, Michel Eberhardt, Domenico Giardini, Cedric Schmelzbach, Davor Mance, Savas Ceylan, Tobias Nicollier, Simon Stähler, Peter Zweifel, Jan ten Pierick, and Martin van Driel

Subjects
Engineering, Geophysics, Geochemistry and Petrology, business.industry, High resolution, Electronics, Mars Exploration Program, Aerospace engineering, business
Abstract

The Seismic Experiment for Interior Structures (SEIS) was deployed on Mars in November 2018 and began science operations in March 2019. SEIS is the primary instrument of the Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) mission, which was launched by the National Aeronautics and Space Administration (NASA). The acquisition and control (AC) electronics is a key element of SEIS. The AC acquires the seismic signals of the two sets of seismic sensors with high resolution, stores the data in its local nonvolatile memory for later transmission by the lander, and controls the numerous functions of SEIS. In this article, we present an overview of the AC with its connections to the sensors and to the lander, as well as its functionality. We describe the elements of the acquisition chains and filters, and discuss the performance of the seismic and temperature channels. Furthermore, we outline the safety functions and health monitoring, which are of paramount importance for reliable operation on Mars. In addition, we analyze an artefact affecting the seismic data referred to as the “tick-noise” and provide a method to remove this artefact by post-processing the data.

Published
2021

10. The site tilt and lander transfer function from the short period seismometer on InSight on Mars

Author

Alexander E. Stott, Nicholas A Teanby, William T. Pike, Philippe Lognonné, K. J. Hurst, Raphaël F. Garcia, Grace Lim, Naomi Murdoch, David Mimoun, Ashitey Trebi-Ollennu, William B. Banerdt, Anna Horleston, Sharon Kedar, Robert Myhill, J. B. McClean, M. Bierwirth, Constantinos Charalambous, Tristram Warren, and Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)

Subjects
Seismometer, Geophysics, Tilt (optics), Geochemistry and Petrology, Period (geology), Mars Exploration Program, Geodesy, Transfer function, Geology, Mars Seismology, Planétologie
Abstract

The National Aeronautics and Space Administration InSight mission has deployed the seismic experiment, SEIS, on the surface of Mars, and has recorded a variety of signals including marsquakes and dust devils. This work presents results on the tilt and local noise sources, which provide context to aid interpretation of the observed signals and allow an examination of the near-surface properties. Our analysis uses data recorded by the short-period sensors on the deck, throughout deployment and in the final configuration. We use thermal decorrelation to provide an estimate of the sol-to-sol tilt. This tilt is examined across deployment and over a Martian year. After each modification to the site, the tilt is seen to stabilize over 3–20 sols depending on the action, and the total change in tilt is

Published
2021

11. Vortex‐Dominated Aeolian Activity at InSight's Landing Site, Part 1: Multi‐Instrument Observations, Analysis, and Implications

Author

Alexander E. Stott, L. M. Sotomayor, Constantinos Charalambous, John A. Grant, Sebastien Rodriguez, Nicholas H. Warner, Veronique Ansan, Don Banfield, William T. Pike, Naomi Murdoch, Aymeric Spiga, Maria E. Banks, Daniel Viúdez-Moreiras, William B. Banerdt, P. H. Lognonné, Ernst Hauber, Jorge Pla-Garcia, Matthew P. Golombek, Clément Perrin, Ralph D. Lorenz, Justin N. Maki, T. Warren, Anna Mittelholz, Claire E. Newman, Antoine Lucas, Matthew E. Baker, Catherine L. Johnson, J. B. Garvin, Ingrid Daubar, Mark T. Lemmon, Sara Navarro, Catherine M. Weitz, J. B. McClean, 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), Department of Electrical and Electronic Engineering [London] (DEEE), Imperial College London, MIT Haystack Observatory, Massachusetts Institute of Technology (MIT), Johns Hopkins University (JHU), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Space Science Institute [Boulder] (SSI), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Institut de Physique du Globe de Paris (IPG Paris), 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), Institut Pierre-Simon-Laplace (IPSL (FR_636)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), NASA Goddard Space Flight Center (GSFC), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Planetary Science Institute [Tucson] (PSI), Smithsonian Institution, State University of New York at Geneseo (SUNY Geneseo), State University of New York (SUNY), Brown University, German Aerospace Center (DLR), University of British Columbia (UBC), 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), University of Oxford, Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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), Cornell University [New York], Aeolis Research, ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019), Rodriguez, Sébastien, and MArs Geophysical InSight - - MAGIS2019 - ANR-19-CE31-0008 - AAPG2019 - VALID

Subjects
Convection, 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, 01 natural sciences, Wind speed, Physics::Geophysics, aeolian changes at the InSight landing site on Mars, convective vortices as a primary driver of particle motion, dust lifting and saltation, multi-instrument measurements constrain the timing and atmospheric conditions of aeolian changes, passing vortices lifting dust are correlated with magnetic signatures, surface creep, surface tracks, particle transport, Geochemistry and Petrology, Planet, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), wind, 14. Life underwater, 010303 astronomy & astrophysics, Physics::Atmospheric and Oceanic Physics, InSight, 0105 earth and related environmental sciences, Mars landing, Mars Exploration Program, Geophysics, Vortex, Planetengeologie, [PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], 13. Climate action, Space and Planetary Science, Aeolian processes, Astrophysics::Earth and Planetary Astrophysics, Geology, camera
Abstract

International audience; We report the aeolian changes observed in situ by NASA's InSight lander during the first 400 sols of operations: Granule creep, saltation, dust removal, and the formation of dark surface tracks. Aeolian changes are infrequent and sporadic. However, on sols, when they do occur, they consistently appear between noon to 3 p.m., and are associated with the passage of convective vortices during periods of high vortex activity. Aeolian changes are more frequent at elevated locations, such as the top surfaces of rocks and lander footpads. InSight observed these changes using, for the first time, simultaneous insitu and orbital imaging and high-frequency meteorological, seismological, and magnetic measurements. Seismometer measurements of ground acceleration constrain the timing and trajectory of convective vortex encounters, linking surface changes to source vortices. Magnetometer measurements show perturbations in magnetic field strength during the passage of convective vortices consistent with chargedparticle motion. Detachment of sand-scale particles occurs when high background winds and vortexinduced turbulence provide a peak surface friction wind speed above the classic saltation fluid threshold. However, detachment of dust-and granule-scale particles also occurred when the surface friction wind speed remained below this threshold. This may be explained by local enhancement of the surface roughness and other effects described here and further studied in Part 2 (Baker et al., 2021). The lack of saltation and bright dust-coated surfaces at the InSight landing site implies surface stability and the onset of particle motion may be suppressed by dust "cushioning." This differentiates the InSight landing site from other areas on Mars that exhibit more aeolian activity. Plain Language Summary Aeolian activity, the movement of dust and sand by the wind, is common on Earth and has been observed on other planets, including Mars. A new Mars lander, InSight, has for the first time monitored aeolian changes by combining imaging with weather, seismic and CHARALAMBOUS ET AL.

Published
2021

12. First Focal Mechanisms of Marsquakes

Author

Domenico Giardini, John-Robert Scholz, Martin van Driel, Philippe Lognonné, Cedric Schmelzbach, Maren Böse, John Clinton, Guenole Mainsant, A. Jacob, Savas Ceylan, Brigitte Knapmeyer-Endrun, William T. Pike, Nienke Brinkman, Eric Beucler, Amir Khan, William B. Banerdt, Taichi Kawamura, Nobuaki Fuji, Constantinos Charalambous, Fabian Euchner, Johan O. A. Robertsson, Mark P. Panning, Clément Perrin, Simon Stähler, Anna Horleston, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), 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 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), Universität zu Köln, Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Max Planck Institute for Solar System Research (MPS), and Max-Planck-Gesellschaft

Subjects
010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Mars Exploration Program, Geophysics, 010502 geochemistry & geophysics, Source inversion, 01 natural sciences, Tectonics, 13. Climate action, Space and Planetary Science, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Geology, 0105 earth and related environmental sciences
Abstract

International audience; Since February 2019, NASA's InSight lander is recording seismic signals on the planet Mars, which, for the first time, allows to observe ongoing tectonic processes with geophysical methods. A number of Marsquakes have been located in the Cerberus Fossae graben system in Elysium Planitia and further west, in the Orcus Patera depression. We present a first study of the focal mechanisms of three well-recorded events (S0173a, S0183a, S0235b) to determine the processes dominating in the source region. We infer for all three events a predominantly extensional setting. Our method is adapted to the case of a single, multicomponent receiver and based on fitting waveforms of P and S waves against synthetic seismograms computed for the initial crustal velocity model derived by the InSight team. We explore the uncertainty due to the single-station limitation and find that even data recorded by one station constrains the mechanisms (reasonably) well. For the events in the Cerberus Fossae region (S0173a, S0235b) normal faulting with a relatively steep dipping fault plane is inferred, suggesting an extensional regime mainly oriented E-W to NE-SW. The fault regime in the Orcus Patera region is not determined uniquely because only the P wave can be used for the source inversion. However, we find that the P and weak S waves of the S0183a event show similar polarities to the event S0173, which indicates similar fault regimes.

Published
2021

13. Autocorrelation of the Ground Vibrations Recorded by the SEIS‐InSight Seismometer on Mars

Author

Nicholas Schmerr, Nicolas Compaire, Vedran Lekic, Raphaël F. Garcia, Martin Schimmel, Eléonore Stutzmann, Baptiste Pinot, Guenolé Orhand-Mainsant, William T. Pike, Laurent Gizon, Do-Yeon Kim, Marie Calvet, Benoit Tauzin, William B. Banerdt, Philippe Lognonné, Ludovic Margerin, Brigitte Knapmeyer-Endrun, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), 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), 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 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), 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), ANR-14-CE36-0012,SEISMARS,Seismology on Mars(2014), ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019), Agence Nationale de la Recherche (France), Université de Toulouse, Schimmel, Martin, and Schimmel, Martin [0000-0003-2601-4462]

Subjects
Seismometer, Engineering, 010504 meteorology & atmospheric sciences, Autocorrelation functions, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Mars seismic interferometry, Flight operations, Seismic interferometry, 01 natural sciences, SEIS seismometer, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Autre, Aeronautics, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Ground vibrations, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, NASA InSight mission, MIDI, business.industry, Autocorrelation, Mars Exploration Program, computer.file_format, autocorrelation functions, seismic interferometry, Geophysics, 13. Climate action, Space and Planetary Science, business, computer
Abstract

Since early February 2019, the SEIS (Seismic Experiment for Interior Structure) seismometer deployed at the surface of Mars in the framework of the InSight mission has been continuously recording the ground motion at Elysium Planitia. In this study, we take advantage of this exceptional data set to put constraints on the crustal properties of Mars using seismic interferometry (SI). To carry out this task, we first examine the continuous records from the very broadband seismometer. Several deterministic sources of environmental noise are identified and specific preprocessing strategies are presented to mitigate their influence. Applying the principles of SI to the single-station configuration of InSight, we compute, for each Sol and each hour of the martian day, the diagonal elements of the time-domain correlation tensor of random ambient vibrations recorded by SEIS. A similar computation is performed on the diffuse waveforms generated by more than a hundred Marsquakes. A careful signal-to-noise ratio analysis and an inter-comparison between the two datasets suggest that the results from SI are most reliable in a narrow frequency band around 2.4 Hz, where an amplification of both ambient vibrations and seismic events is observed. The average autocorrelation functions (ACFs) contain well identifiable seismic arrivals, that are very consistent between the two datasets. Interpreting the vertical and horizontal ACFs as, respectively, the P- and S- seismic reflectivity below InSight, we propose a simple stratified velocity model of the crust, which is mostly compatible with previous results from receiver function analysis. Our results are discussed and compared to recent works from the literature., This study is InSight contribution number 164. The authors acknowledge both "Universite Federale de Toulouse Midi Pyrenees" and the "Region Occitanie" for funding the PhD grant of Nicolas Compaire. The French authors acknowledge the French Space Agency CNES and ANR (ANR-14-CE36-0012-02 and ANR-19-CE31-0008-08) for funding the InSight Science analysis. 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.

Published
2021

15. Atmospherically driven ground motion at InSight: a machine learning perspective

Author

William T. Pike, Don Banfield, Naomi Murdoch, Sara Navarro, David Mimoun, Philippe Lognonné, Anna Horleston, Aymeric Spiga, Baptiste Pinot, Constantinos Charalambous, Raphaël F. Garcia, Luis Mora-Sotomayor, and Alexander E. Stott

Subjects
Ground motion, Computer science, Human–computer interaction, Perspective (graphical)
Abstract

The NASA InSight lander is a geophysical and meteorological observatory operating on Mars for over a Martian year/two Earth years. Continuous records of seismic, pressure, wind and temperature data over this period have led to significant breakthroughs in determining the planet's structure and climate. With such a wealth of data now received, machine learning offers a nascent tool to extract further information. The seismic data is extremely correlated to the atmospheric conditions. Discerning the coupling between the atmosphere and ground motion is of significant interest and this work aims to predict the ground motion generated by wind and pressure forcing using machine learning techniques. From this prediction we can untangle the various contributions to ground motion, determine atmospheric/ground properties, analyse/discriminate marsquakes and potentially decorrelate waveforms to remove the atmospheric contribution. While a physical model for this atmospheric forcing is desirable, machine learning approaches the problem from an alternative view point where mathematical and algorithmic tools add the necessary complexity for fitting the data. In this way, we may be able to capture detailed variation and inform further modelling efforts.We will detail the initial application of machine learning for predicting the ground motion from the atmospheric data inputs of wind speed, wind direction, pressure and temperature. First though, we will describe the issues that need to be tackled to obtain a good prediction using the InSight data. To illustrate some of some of these problems, consider that glitches are known to occur in the seismic data. They offer a way to detect overfitting as they should not in general be predicted from atmospheric forcing. However, a subset of the glitches are correlated to temperature on top of the fact they are only visible during quiet enough periods, as are marsquakes. Therefore, they are not a normally distributed source of noise or uncorrelated from the input atmospheric data, breaking typical assumptions used for regression. A similar issue is presented by the changing weather conditions throughout a Martian sol, where the time series distribution varies. As a result, prior information on the instrumentation and data qualities is essential for applying the machine learning methods and interpretation of the results.We demonstrate the specifics of the InSight data with respect to 1) how a curve fitting problem can be constructed, 2) the necessary degrees of freedom of the problem, 3) consideration of non-stationary/heteroscedastic errors and 4) the optimisation and machine learning method applied. Current results will be presented from the implementation of random forests and gaussian processes. These results demonstrate a good performance so far for capturing the global variation and we will offer perspectives on how these results can be used and improved.

Published
2021

16. Super High Frequency Events: A New Class of Events Recorded by the InSight Seismometers on Mars

Author

Constantinos Charalambous, Nikolaj Dahmen, Renee Weber, John Clinton, Simon Stähler, Anna Horleston, William B. Banerdt, William T. Pike, Philippe Lognonné, Amir Khan, Taichi Kawamura, Savas Ceylan, Fabian Euchner, Domenico Giardini, Martin van Driel, Maren Böse, John-Robert Scholz, and Guenolé Orhand-Mainsant

Subjects
Seismometer, Super high frequency, Geophysics, Space and Planetary Science, Geochemistry and Petrology, Template matching, Earth and Planetary Sciences (miscellaneous), Mars Exploration Program, Geology, Seismology
Published
2021

17. High‐Frequency Seismic Events on Mars Observed by InSight

Author

Philippe Lognonné, William T. Pike, John Clinton, Amir Khan, Ludovic Margerin, Domenico Giardini, Constantinos Charalambous, Simon Stähler, Anna Horleston, Nicholas Schmerr, Maren Böse, Guenolé Orhand-Mainsant, William B. Banerdt, Martin Knapmeyer, Fabian Euchner, Taichi Kawamura, John‐R. Scholz, Martin van Driel, Savas Ceylan, 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), ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019), 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), 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), 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), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), School of Earth Sciences [Bristol], University of Bristol [Bristol], 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, Department of Electrical and Electronic Engineering [London] (DEEE), Imperial College London, Institute for Theoretical Physics [ETH Zürich] (ITP), Department of Physics [ETH Zürich] (D-PHYS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), University of Maryland [College Park], University of Maryland System, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), and ANR-14-CE36-0012,SEISMARS,Seismology on Mars(2014)

Subjects
Seismometer, Martian, 010504 meteorology & atmospheric sciences, Scattering, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Attenuation, Crust, Mars Exploration Program, Mars InSight Marsbeben, 01 natural sciences, Coda, Geophysics, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, 13. Climate action, Space and Planetary Science, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Layering, Seismology, Geology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

International audience; The seismometer deployed on the surface of Mars as part of the InSight mission (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) has recorded several hundreds of marsquakes in the first 478 sols after landing. The majority of these are classified as high-frequency (HF) events in the frequency range from approximately 1 to 10 Hz on Mars' surface. All the HF events excite a resonance around 2.4 Hz and show two distinct but broad arrivals of seismic energy that are separated by up to 450 s. Based on the frequency content and vertical-to-horizontal energy ratio, the HF event family has been subdivided into three event types, two of which we show to be identical and only appear separated due to the signal-to-noise ratio. We show here that the envelope shape of the HF events is explained by guided Pg and Sg phases in the Martian crust using simple layered models with scattering. Furthermore, the relative travel times between these two arrivals can be related to the epicentral distance, which shows distinct clustering. The rate at which HF events are observed varies by an order of magnitude over the course of one year and cannot be explained by changes of the background noise only. The HF content and the absence of additional seismic phases constrain crustal attenuation and layering, and the coda shape constrains the diffusivity in the uppermost shallow layers of Mars.

Published
2021

18. A Comodulation Analysis of Atmospheric Energy Injection into the Ground Motion at InSight, Mars

Author

M. van Driel, John Clinton, Constantinos Charalambous, L. M. Sotomayor, Domenico Giardini, Naomi Murdoch, Simon Stähler, Anna Horleston, T. Warren, William B. Banerdt, William T. Pike, John-Robert Scholz, Aymeric Spiga, Guenolé Orhand-Mainsant, Savas Ceylan, Don Banfield, Amir Khan, Maren Böse, Alexander E. Stott, Raphaël F. Garcia, J. B. McClean, Taichi Kawamura, P. H. Lognonné, Sara Navarro, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Murdoch, N. [0000-0002-9701-4075], Lognonne, P. [0000-0002-1014-920X], Charalambous, C. [0000-0002-9139-3895], Stott, A. E. [0000-0001-6121-705X], Spiga, A. [0000-0002-6776-6268], Stähler, S. [0000-0002-0783-2489], Scholz, J. R. [0000-0003-1404-2335], Ceylan, S. [0000-0002-6552-6850], Khan, A. [0000-0003-4462-3173], Van Driel, M. [0000-0002-8938-4615], Horleston, A. [0000-0002-6748-6522], Giardini, D. [0000-0002-5573-7638], and Banerdt, W. B. [0000-0003-3125-1542]

Subjects
Ground motion, 010504 meteorology & atmospheric sciences, ground motion, marsquakes, Method of moments (statistics), 01 natural sciences, Mars Atmosphere, Atmosphere, atmosphere‐induced noise, comodulation, method of moments, noise discrimination, Autre, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), 0105 earth and related environmental sciences, Martian, Mars Exploration Program, Geophysics, Space and Planetary Science, Environmental science, Atmospheric electricity, Mars seismology, Noise (radio)
Abstract

Seismic observations involve signals that can be easily masked by noise injection. For the NASA Mars lander InSight, the atmosphere is a significant noise contributor, impeding the identification of seismic events for two thirds of a Martian day. While the noise is below that seen at even the quietest sites on Earth, the amplitude of seismic signals on Mars is also considerably lower, requiring an understanding and quantification of environmental injection at unprecedented levels. Mars' ground and atmosphere are a continuously‐coupled seismic system, and although atmospheric functions are of distinct origins, the superposition of these noise contributions is poorly understood, making separation a challenging task. We present a novel method for partitioning the observed signal into seismic and environmental contributions. Atmospheric pressure and wind fluctuations are shown to exhibit temporal cross‐frequency coupling across multiple bands, injecting noise that is neither random nor coherent. We investigate this through comodulation, quantifying the synchrony of the seismic motion, wind and pressure signals. By working in the time‐frequency domain, we discriminate between the different origins of underlying processes and determine the site's environmental sensitivity. Our method aims to create a virtual vault at InSight's landing site on Mars, shielding the seismometers with effective post‐processing in lieu of a physical vault. This allows us to describe the environmental and seismic signals over a sequence of sols, to quantify the wind and pressure injection and estimate the seismic content of possible marsquakes with a signal‐to‐noise ratio that can be quantified in terms of environmental independence. Finally, we exploit the relationship between the comodulated signals to identify their sources., Journal of Geophysical Research: Planets, 126 (4), ISSN:0148-0227, ISSN:2169-9097

Published
2021
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19. Resonances of the InSight Seismometer on Mars

Author

K. Hurst, Taichi Kawamura, Savas Ceylan, William B. Banerdt, M. Bierwirth, Sharon Kedar, T. Nebut, Cedric Schmelzbach, Oliver Robert, Maren Böse, William T. Pike, Domenico Giardini, Simon Stähler, Constantino Charalambous, Alexander E. Stott, John-Robert Scholz, Anna Horleston, Jennifer Stevanović, Amir Khan, Tristram Warren, Joan Ervin, Brigitte Knapmeyer-Endrun, S. B. Calcutt, Guenolé Orhand-Mainsant, Lucile Fayon, Martin van Driel, Philippe Lognonné, John Clinton, T. Gabsi, S. Tillier, and Sebastien de Raucourt

Subjects
Seismometer, Geophysics, Geochemistry and Petrology, Mars Exploration Program, Geology, Astrobiology
Abstract

The Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) seismometer was deployed to the surface of Mars in December 2018–February 2019. The specific deployment conditions, which are very different from those of a standard broadband instrument on the Earth, result in resonances caused by different parts of the sensor assembly (SA) that are recorded by the seismometer. Here, we present and characterize the resonances known to be present in the SA and their causes to aid interpretation of the seismic signals observed on Mars. Briefly, there are resonances in the SA at about 2.9, 5.3, 9.5, 12, 14, 23–28, and 51 Hz. We discuss various methods and tests that were used to characterize these resonances, and provide evidence for some of them in data collected on Mars. In addition to their relevance for the high frequency analysis of seismic data from InSight, specifically for phase measurements near the resonant frequencies, the tests and observations described here are also of potential use in the further development of planetary seismometers, for example, for Mars, the Moon, or Europa.

Published
2021

20. Companion guide to the Marsquake catalog from InSight, sols 0–478: Data content and non-seismic events

Author

Clément Perrin, Nikolaj Dahmen, Suzanne E. Smrekar, Raphaël F. Garcia, Martin Schimmel, Simon Stähler, Maren Böse, William B. Banerdt, Anna Horleston, Alexander E. Stott, Sharon Kedar, Eléonore Stutzmann, Ralph D. Lorenz, Jan ten Pierick, K. Hurst, Don Banfield, John Clinton, Taichi Kawamura, Constantinos Charalambous, Fabian Euchner, Aymeric Spiga, Eric Beucler, Amir Khan, William T. Pike, Vincent Conejero, Philippe Lognonné, Savas Ceylan, Martin van Driel, Domenico Giardini, Mark P. Panning, Constanza Pardo, Guenolé Orhand-Mainsant, John-Robert Scholz, Swiss National Science Foundation, Agence Nationale de la Recherche (France), Swiss National Supercomputing Centre, UK Space Agency, Centre National D'Etudes Spatiales (France), ETH Zurich, State Secretariat for Education, Research and Innovation (Switzerland), Schimmel, Martin, Département Electronique, Optronique et Signal (DEOS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), and Schimmel, Martin [0000-0003-2601-4462]

Subjects
[SPI.OTHER]Engineering Sciences [physics]/Other, Seismometer, 010504 meteorology & atmospheric sciences, Physics and Astronomy (miscellaneous), Mars, Data inventory, 010502 geochemistry & geophysics, 01 natural sciences, Autre, Broadband, Data content, InSight mission, Non-seismic signals, Marsquakes, 0105 earth and related environmental sciences, Scientific instrument, Martian, Payload, Astronomy and Astrophysics, Mars Exploration Program, Geophysics, 13. Climate action, Space and Planetary Science, Noise (video), Mars seismology, Geology, Seismology
Abstract

The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission landed on the surface of Mars on November 26, 2018. One of the scientific instruments in the payload that is essential to the mission is the SEIS package (Seismic Experiment for Interior Structure) which includes a very broadband and a short period seismometer. More than one year since the landing, SEIS continues to be fully operational and has been collecting an exceptional data set which contains not only the signals of seismic origins, but also noise and artifacts induced by the martian environment, the hardware on the ground that includes the seismic sensors, and the programmed operational activities of the lander. Many of these non-seismic signals will be unfamiliar to the scientific community. In addition, many of these signals have signatures that may resemble seismic events either or both in time and frequency domains. Here, we report our observations of common non-seismic signals as seen during the first 478 sols of the SEIS data, i.e. from landing until the end of March 2020. This manuscript is intended to provide a guide to scientists who use the data recorded on SEIS, detailing the general attributes of the most commonly observed non-seismic features. It will help to clarify the characteristics of the seismic dataset for future research, and to avoid misinterpretations when searching for marsquakes., 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. We also acknowledge the funding by (1) Swiss National Science Foundation and French Agence Nationale de la Recherche (SNF-ANR project “Seismology on Mars”, ANR-14-CE36-0012-02 and MAGIS, ANR-19-CE31-0008-08), (2) Swiss State Secretariat for Education, Research and Innovation (SEFRI project “MarsQuake Service-Preparatory Phase”), (3) ETH Research grant ETH-06 17-02 and, for French co-authors, (4) the French Space agency CNES. Additional support came from the Swiss National Supercomputing Centre (CSCS) under project ID s922. AH is funded by UKSA through grant #ST/R002096/1. Visualizations were created using Matplotlib (Hunter, 2007). The data was processed with NumPy (Oliphant, 2006), Scipy (Jones et al., 2001), ObsPy (Krischer et al., 2015) and custom software developed by gempa GmbH. This paper is InSight Contribution Number 150.

Published
2021

21. Autocorrelation of the ground vibration recorded by the SEIS-InSight seismometer on Mars for imaging and monitoring applications

Author

Martin Schimmel, Benoit Tauzin, Philippe Lognonné, Bruce Banerdt, Eléonore Stutzmann, Guenolé Orhand-Mainsant, Nicholas Schmerr, Vedran Lekic, William T. Pike, Ludovic Margerin, Laurent Gizon, Baptiste Pinot, Marie Calvet, Raphaël F. Garcia, Nicolas Compaire, Brigitte Knapmeyer-Endrun, and Do-Yeon Kim

Subjects
Vibration, Seismometer, Autocorrelation, Mars, Mars Exploration Program, SEIS-InSight seismometer, Seismology, Geology
Abstract

vEGU21: Gather Online | 19–30 April 2021, Since early February 2019, the SEIS seismometer deployed at the surface of Mars in the framework of the NASA-InSight mission has been continuously recording the ground motion at Elysium Planitia. In this work, we take advantage of this exceptional dataset to put constraints on the crustal properties of Mars using seismic interferometry (SI). This method use the seismic waves, either from background vibrations of the planet or from quakes, that are scattered in the medium in order to recover the ground response between two seismic sensors. Applying the principles of SI to the single-station configuration of SEIS, we compute, for each Sol (martian day) and each local hour, all the components of the time-domain autocorrelation tensor of random ambient vibrations in various frequency bands. A similar computation is performed on the diffuse waveforms generated by more than a hundred Marsquakes. For imaging application a careful signal-to-noise ratio analysis and an inter-comparison between the two datasets are applied. These analyses suggest that the reconstructed ground responses are most reliable in a relatively narrow frequency band around 2.4Hz, where an amplification of both ambient vibrations and seismic events is observed. The average Auto-Correlation Functions (ACFs) from both ambient vibrations and seismic events contain well identifiable seismic arrivals, that are very consistent between the two datasets. We interpret the vertical and horizontal ACFs as the ground reflection response below InSight for the compressional waves and the shear waves respectively. We propose a simple stratified velocity model of the crust, which is most compatible with the arrival times of the detected phases, as well as with previous seismological studies of the SEIS record. The hourly computation of the ACFs over one martian year also allows us to study the diurnal and seasonal variations of the reconstructed ground response with a technique call Passive Image Interferometry (PII). In this study we present measurements of the relative stretching coefficient between consecutive ACF waveforms and discuss the potential origins of the observed temporal variations.

Published
2021

22. Detection, Analysis, and Removal of Glitches From InSight's Seismic Data From Mars

Author

L. Pou, Martin Knapmeyer, S. Barkaoui, Taichi Kawamura, Eric Beucler, Amir Khan, Baptiste Pinot, Bruce Banerdt, Rakshit Joshi, Brigitte Knapmeyer-Endrun, John Clinton, Raphaël F. Garcia, Mickael Bonnin, Arthur Cuvier, Grégory Sainton, Constantinos Charalambous, Savas Ceylan, Sebastien de Raucourt, Eléonore Stutzmann, Simon Stähler, John-Robert Scholz, Paul M. Davis, Anna Horleston, Guenolé Orhand-Mainsant, Nicolas Compaire, Francis Nimmo, Ulrich R. Christensen, Martin van Driel, Domenico Giardini, William T. Pike, Martin Schimmel, Maren Böse, Alexander E. Stott, K. Hurst, Rudolf Widmer-Schnidrig, Philippe Lognonné, Agence Nationale de la Recherche (France), Swiss Space Office, Schimmel, Martin [0000-0003-2601-4462], Schimmel, Martin, Widmer‐Schnidrig, Rudolf, 2 Black Forest Observatory, Institute of Geodesy Stuttgart University Stuttgart Germany, Davis, Paul, 3 Department of Earth, Planetary, and Space Sciences University of California Los Angeles Los Angeles CA USA, Lognonné, Philippe, 4 Université de Paris, Institut de physique du globe de Paris, CNRS Paris France, Pinot, Baptiste, 5 Institut Supérieur de l'Aéronautique et de l'Espace SUPAERO Toulouse France, Garcia, Raphaël F., Hurst, Kenneth, 6 Jet Propulsion Laboratory California Institute of Technology Pasadena USA, Pou, Laurent, 7 Department of Earth and Planetary Sciences University of California Santa Cruz Santa Cruz CA USA, Nimmo, Francis, Barkaoui, Salma, de Raucourt, Sébastien, Knapmeyer‐Endrun, Brigitte, 8 Bensberg Observatory University of Cologne Bergisch Gladbach Germany, Knapmeyer, Martin, 9 DLR Institute of Planetary Research Berlin Germany, Orhand‐Mainsant, Guénolé, Compaire, Nicolas, Cuvier, Arthur, 10 Laboratoire de Planétologie et Géodynamique, Université de Nantes, Université d'Angers Nantes France, Beucler, Éric, Bonnin, Mickaël, Joshi, Rakshit, 1 Max Planck Institute for Solar System Research Göttingen Germany, Sainton, Grégory, Stutzmann, Eléonore, 11 Institute of Earth Sciences Jaume Almera ‐ CSIC Barcelona Spain, Horleston, Anna, 12 School of Earth Sciences University of Bristol Bristol UK, Böse, Maren, 13 Swiss Seismological Service (SED) ETH Zurich Zurich, Switzerland, Ceylan, Savas, 14 Institute of Geophysics ETH Zürich Zurich Switzerland, Clinton, John, van Driel, Martin, Kawamura, Taichi, Khan, Amir, Stähler, Simon C., Giardini, Domenico, Charalambous, Constantinos, 16 Department of Electrical and Electronic Engineering Imperial College London London UK, Stott, Alexander E., Pike, William T., Christensen, Ulrich R., Banerdt, W. Bruce, and Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)

Subjects
Seismometer, 010504 meteorology & atmospheric sciences, lcsh:Astronomy, glitches, seismometer, Mars, Environmental Science (miscellaneous), 010502 geochemistry & geophysics, 01 natural sciences, Glitches, lcsh:QB1-991, Autre, Broadband, 0105 earth and related environmental sciences, InSight, Data processing, removal, lcsh:QE1-996.5, Mars Exploration Program, lcsh:Geology, General Earth and Planetary Sciences, InSight Mars Seismogramme Datenbearbeitung, Mars seismology, Removal, Geology, Seismology, data processing
Abstract

The instrument package SEIS (Seismic Experiment for Internal Structure) with the three very broadband and three short‐period seismic sensors is installed on the surface on Mars as part of NASA's InSight Discovery mission. When compared to terrestrial installations, SEIS is deployed in a very harsh wind and temperature environment that leads to inevitable degradation of the quality of the recorded data. One ubiquitous artifact in the raw data is an abundance of transient one‐sided pulses often accompanied by high‐frequency spikes. These pulses, which we term “glitches”, can be modeled as the response of the instrument to a step in acceleration, while the spikes can be modeled as the response to a simultaneous step in displacement. We attribute the glitches primarily to SEIS‐internal stress relaxations caused by the large temperature variations to which the instrument is exposed during a Martian day. Only a small fraction of glitches correspond to a motion of the SEIS package as a whole caused by minuscule tilts of either the instrument or the ground. In this study, we focus on the analysis of the glitch+spike phenomenon and present how these signals can be automatically detected and removed from SEIS's raw data. As glitches affect many standard seismological analysis methods such as receiver functions, spectral decomposition and source inversions, we anticipate that studies of the Martian seismicity as well as studies of Mars' internal structure should benefit from deglitched seismic data., Plain Language Summary: The instrument package SEIS (Seismic Experiment for Internal Structure) with two fully equipped seismometers is installed on the surface of Mars as part of NASA's InSight Discovery mission. When compared to terrestrial installations, SEIS is more exposed to wind and daily temperature changes that leads to inevitable degradation of the quality of the recorded data. One consequence is the occurrence of a specific type of transient noise that we term “glitch”. Glitches show up in the recorded data as one‐sided pulses and have strong implications for the typical seismic data analysis. Glitches can be understood as step‐like changes in the acceleration sensed by the seismometers. We attribute them primarily to SEIS‐internal stress relaxations caused by the large temperature variations to which the instrument is exposed during a Martian day. Only a small fraction of glitches correspond to a motion of the whole SEIS instrument. In this study, we focus on the detection and removal of glitches and anticipate that studies of the Martian seismicity as well as studies of Mars's internal structure should benefit from deglitched seismic data., Key Points: Glitches due to steps in acceleration significantly complicate seismic records on Mars. Glitches are mostly due to relaxations of thermal stresses and instrument tilt. We provide a toolbox to automatically detect and remove glitches., Centre National d'Etudes Spatiales (CNES), InSight PSP Program, Agence Nationale de la Recherche http://dx.doi.org/10.13039/501100001665, ANR‐19‐CE31‐0008‐08

Published
2020

23. The Marsquake Catalogue from InSight, Sols 0-478

Author

John Clinton, Savas Ceylan, Martin van Driel, Domenico Giardini, Simon C. Stähler, Maren Böse, Constantinos Charalambous, Nikolaj L. Dahmen, Anna Horleston, Taichi Kawamura, Amir Khan, Guenole Orhand-Mainsant, John-Robert Scholz, Fabian Euchner, William B. Banerdt, Philippe Lognonne, Don Banfield, Eric Beucler, Sharon Kedar, Mark Panning, Clement Perrin, William T. Pike, Suzanne E. Smrekar, Aymeric Spiga, and Alexander E. Stott

Abstract

The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission began collecting high quality seismic data on Mars from February 2019. This manuscript documents the seismicity observed by SEIS, InSight’s seismometer, since this time until the end of March, 2020. Within the InSight project, the Marsquake Service (MQS) is responsible for prompt review of all seismic data collected by InSight, detection of events that are likely to be of seismic origin, and curation and release of seismic catalogues. In the first year of data collection, MQS have identified 465 seismic events that we interpret to be from regional and teleseismic marsquakes. Seismic events are grouped into 2 different event families: the low frequency family are dominated by energy at long period below 1 second, and the high frequency family primarily include energy at and above 2.4~Hz. Event magnitudes, from Mars-specific scales, range from 1.3 to 3.7. A third class of events with very short duration but high frequency bursts have been observed 712 times. These are likely associated with a local source driven by thermal stresses. This paper describes the data collected so far in the mission and the procedures under which MQS operates; summarises the content of the current MQS seismic catalogue; and presents the key features of the events we have observed so far, using the largest events as examples.

Published
2020

24. Assessment of InSight Landing Site Predictions

Author

Sylvain Piqueux, William T. Pike, Constantinos Charalambous, Nathan R. Williams, Nicholas H. Warner, Matthew P. Golombek, Ingrid Daubar, and David M. Kass

Subjects
Surface Materials and Properties, 010504 meteorology & atmospheric sciences, landing sites, Amazonian, Mars, surfaces, Surface pressure, 01 natural sciences, Remote Sensing, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Geomorphology, Planetary Sciences: Solid Surface Planets, Research Articles, InSight, 0105 earth and related environmental sciences, Radiometer, geomorphology, Mars Exploration Program, Albedo, InSight at Mars, Atmospheric temperature, Physical Properties of Materials, Regolith, Geophysics, Space and Planetary Science, Hesperian, Geology, Research Article
Abstract

Comprehensive analysis of remote sensing data used to select the Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) landing site correctly predicted the atmospheric temperature and pressure profile during entry and descent, the safe landing surface, and the geologic setting of the site. The smooth plains upon which the InSight landing site is located were accurately predicted to be generally similar to the Mars Exploration Rover Spirit landing site with relatively low rock abundance, low slopes, and a moderately dusty surface with a 3–10 m impact fragmented regolith over Hesperian to Early Amazonian basaltic lava flows. The deceleration profile and surface pressure encountered by the spacecraft during entry, descent, and landing compared well (within 1σ) of the envelope of modeled temperature profiles and the expected surface pressure. Orbital estimates of thermal inertia are similar to surface radiometer measurements, and materials at the surface are dominated by poorly consolidated sand as expected. Thin coatings of bright atmospheric dust on the surface were as indicated by orbital albedo and dust cover index measurements. Orbital estimates of rock abundance from shadow measurements in high‐resolution images and thermal differencing indicated very low rock abundance and surface counts show 1–4% area covered by rocks. Slopes at 100 to 5 m length scale measured from orbital topographic and radar data correctly indicated a surface comparably smooth and flat as the two smoothest landing sites (Opportunity and Phoenix). Thermal inertia and radar data indicated the surface would be load bearing as found., Key Points The atmosphere, safe surface, and geologic setting of the landing site were correctly predicted by remote sensing data before landingThe modeled atmospheric temperature profiles and surface pressure were within 1 sigma of the measured deceleration profile and surface pressureInSight’s surface is similar to Spirit’s with low rock abundance, low slopes, moderate dust, and is composed of impact regolith over basalt

Published
2020

25. Detection, analysis and removal of glitches from InSight's 1 seismic data from Mars

Author

John-Robert Scholz, Rudolf Widmer-Schnidrig, Paul Davis, Philippe Lognonné, Baptiste Pinot, Raphaël F Garcia, Francis Nimmo, Kenneth Hurst, Salma Barkaoui, Sébastien De Raucourt, Laurent Pou, Guénolé Mainsant, Nicolas Compaire, Arthur Cuvier, Eric Beucler, Mickaël Bonnin, Rakshit Joshi, Eléonore Stutzmann, Martin Schimmel, Anna Horleston, Maren Böse, Savas Ceylan, John Clinton, Martin Van Driel, Taichi Kawamura, Amir Khan, Simon C Stähler, Domenico Giardini, Constantinos Charalambous, Alexander E Stott, William T Pike, Ulrich R Christensen, and W Bruce Banerdt

Published
2020

26. A reconstruction algorithm for temporally aliased seismic signals recorded by the InSight Mars lander

Author

Nienke Brinkman, Martin van Driel, Sharon Kedar, Raphaël F. Garcia, Johan O. A. Robertsson, Fredrik Andersson, Cedric Schmelzbach, John Clinton, Philippe Lognonné, Simon Stähler, Thomas Haag, Tilman Spohn, David Sollberger, William B. Banerdt, Matthias Grott, William T. Pike, Troy L. Hudson, Domenico Giardini, Peter Zweifel, Jan ten Pierick, and Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)

Subjects
Informatics, Astronomy, aliasing, Time Series Experiments, Signal, Planetary Sciences: Solar System Objects, Sampling (signal processing), Aliasing, Stochastic Phenomena, Traitement du signal et de l'image, signal reconstruction, Instruments and Techniques, QE1-996.5, Exploration Geophysics, Nonlinear Geophysics, Mars landing, Geology, Reconstruction algorithm, Mars Exploration Program, Oceanography: General, Probability Distributions, Heavy and Fat‐tailed, Planetary Sciences: Comets and Small Bodies, Mathematical Geophysics, Research Article, Seismometer, Persistence, Memory, Correlations, Clustering, Acoustics, Mars, QB1-991, Temporal Analysis and Representation, seismic exploration, Environmental Science (miscellaneous), Extreme Events, Time Series Analysis, signal processing, Planetary Sciences: Solid Surface Planets, Planetary Sciences: Fluid Planets, Mars seismic data analysis, Stochastic Processes, Computational Methods: Seismic, Interiors, InSight at Mars, Tectonophysics, General Earth and Planetary Sciences, Space Plasma Physics, Nyquist frequency, Hydrology, Scaling: Spatial and Temporal, InSight Mars Geophysics Regolith HP3 SEIS, Natural Hazards, Planetary Interiors
Abstract

In December 2018, the NASA InSight lander successfully placed a seismometer on the surface of Mars. Alongside, a hammering device was deployed at the landing site that penetrated into the ground to attempt the first measurements of the planetary heat flow of Mars. The hammering of the heat probe generated repeated seismic signals that were registered by the seismometer and can potentially be used to image the shallow subsurface just below the lander. However, the broad frequency content of the seismic signals generated by the hammering extends beyond the Nyquist frequency governed by the seismometer's sampling rate of 100 samples per second. Here, we propose an algorithm to reconstruct the seismic signals beyond the classical sampling limits. We exploit the structure in the data due to thousands of repeated, only gradually varying hammering signals as the heat probe slowly penetrates into the ground. In addition, we make use of the fact that repeated hammering signals are sub-sampled differently due to the unsynchronized timing between the hammer strikes and the seismometer recordings. This allows us to reconstruct signals beyond the classical Nyquist frequency limit by enforcing a sparsity constraint on the signal in a modified Radon transform domain. In addition, the proposed method reduces uncorrelated noise in the recorded data. Using both synthetic data and actual data recorded on Mars, we show how the proposed algorithm can be used to reconstruct the high-frequency hammering signal at very high resolution., Earth and Space Science, 8 (8), ISSN:2333-5084

Published
2020

27. An international comparison of the second derivative of COVID-19 deaths after implementation of social distancing measures

Author

Vikas Saini and William T. Pike

Subjects
medicine.medical_specialty, Geography, Coronavirus disease 2019 (COVID-19), Social distance, Public health, Mortality rate, medicine, China, Demography
Abstract

This work compares deaths for confirmed COVID-19 cases in China to eight other countries, Italy, Spain, France, USA, UK, Germany, Netherlands and South Korea. After implementing varying intensities and timing of social distancing measures, several appear to be converging onto the decline in the daily growth rate of deaths, or relative second derivative of total deaths, seen in China after the implementation an aggressive social distancing policy. By calculating future trajectories in these countries based on the observed Chinese fatality statistics, an estimate of the total deaths and maximum daily death rates over a defined period of time is made. Our lower bound estimate for the United Kingdom based on the real data approximates the lower bound estimate of the recent modelling study of Ferguson et al. [1]. These results suggest there may be a threshold of effective public health intervention. Our method of viewing the data may be helpful in monitoring the course of the epidemic, judging the effectiveness of implementation, and monitoring the relaxation of social distancing.

Published
2020

28. Results From the Insight Mission After a Year and a Half on Mars

Author

Philippe Lognonné, Don Banfield, Christopher T. Russell, Véronique Dehant, Tilman Spohn, Catherine Johnson, William T. Pike, Aymeric Spiga, Suzanne E. Smrekar, Domenico Giardini, William B. Banerdt, William M. Folkner, and Matthew P. Golombek

Subjects
Mars Exploration Program, Geology, Astrobiology
Abstract

The InSight mission landed on Mars in November of 2018 and completed installation of a seismometer (SEIS) on the surface about two months later. In addition to SEIS, InSight carries a diverse geophysical observatory including a heat flow and sub-surface physical properties experiment (HP3), a geodesy (planetary rotation dynamics) experiment (RISE), and a suite of environmental sensors measuring the magnetic field and atmospheric temperature, pressure and wind (APSS). For more than a year, SEIS has been providing near-continuous seismic monitoring of Mars, with background noise levels orders of magnitude lower than that achievable on the Earth. Since installation was completed, the SEIS team has identified more than 400 events that we have not attributed to the local environment or spacecraft activity, and dozens that appear to be marsquakes of tectonic origin. We present an overview of observations by the SEIS instrument as well as a summary of other geophysical observations made by InSight during the past year and a half.

Published
2020

29. On-deck seismology: Lessons from InSight for future planetary seismology

Author

Alexander E. Stott, Simon Stähler, Philippe Lognonné, Constantinos Charalambous, Sharon Kedar, Angela G. Marusiak, William T. Pike, Ralph D. Lorenz, Mark P. Panning, J. B. McClean, Don Banfield, William B. Banerdt, Naomi Murdoch, Ceri Nunn, Tristram Warren, and Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)

Subjects
Seismometer, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Mars, Induced seismicity, Exploration of Mars, 01 natural sciences, Wind speed, Physics - Geophysics, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysique, Seismology, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Mars Exploration Program, Geophysics (physics.geo-ph), Geophysics, Planetary science, 13. Climate action, Space and Planetary Science, QUIET, Astrophysics - Instrumentation and Methods for Astrophysics, Noise (radio), Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract

Before deploying to the surface of Mars, the short-period (SP) seismometer of the InSight mission operated on deck for a total of 48 hours. This dataset can be used to understand how deck-mounted seismometers can be used in future landed missions to Mars, Europa, and other planetary bodies. While operating on deck, the SP seismometer showed signals comparable to the Viking-2 seismometer near 3 Hz where the sensitivity of the Viking instrument peaked. Wind sensitivity showed similar patterns to the Viking instrument, although amplitudes on InSight were ~80% larger for a given wind velocity. However, during the low wind evening hours the instrument noise levels at frequencies between 0.1 and 1 Hz were comparable to quiet stations on Earth, although deployment to the surface below the Wind and Thermal Shield lowered installation noise by roughly 40 dB in acceleration power. With the observed noise levels and estimated seismicity rates for Mars, detection probability for quakes for a deck-mounted instrument are low enough that up to years of on-deck recordings may be necessary to observe an event. Because the noise is dominated by wind acting on the lander, though, deck-mounted seismometers may be more practical for deployment on airless bodies, and it is important to evaluate the seismicity of the target body and the specific design of the lander. Detection probabilities for operation on Europa reach over 99% for some proposed seismicity models for a similar duration of operation if noise levels are comparable to low-wind time periods on Mars., 20 pages, 7 figures, accepted to Journal of Geophysical Research: Planets

Published
2020

30. Geology of the InSight landing site on Mars

Author

Jeffery L. Hall, R. Hausmann, Claire E. Newman, Sharon A. Wilson, Nathan R. Williams, L. Berger, H. Abarca, Matthew P. Golombek, Constantinos Charalambous, Justin N. Maki, Paul M. Andres, Matthias Grott, Maria E. Banks, Sylvain Piqueux, A. DeMott, Philippe Lognonné, M. Kopp, François Forget, T. J. Parker, Ehouarn Millour, Niclas S. Mueller, M. M. Baker, Fred Calef, James B. Garvin, Aymeric Spiga, E. Hauber, Eloise Marteau, Veronique Ansan, William T. Pike, Christos Vrettos, John A. Grant, Clément Perrin, Sebastien Rodriguez, Naomi Murdoch, Nicholas H. Warner, N. Ruoff, William B. Banerdt, A. Trussell, Don Banfield, H. Lethcoe-Wilson, Suzanne E. Smrekar, Ingrid Daubar, Tilman Spohn, Robert G. Deen, S. Le Maistre, William M. Folkner, Catherine M. Weitz, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), UCL - SST/ELI/ELIC - Earth & Climate, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), State University of New York at Geneseo (SUNY Geneseo), State University of New York (SUNY), Smithsonian Institution, DLR Institute of Planetary Research, German Aerospace Center (DLR), 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), Planetary Science Institute [Tucson] (PSI), Department of Mechanical Engineering [Imperial College London], Imperial College London, Technical University of Kaiserslautern (TU Kaiserslautern), Royal Observatory of Belgium [Brussels] (ROB), 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 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), Johns Hopkins University (JHU), NASA Goddard Space Flight Center (GSFC), Cornell University [New York], and Aeolis Research

Subjects
geology, landing site, 010504 meteorology & atmospheric sciences, Science, General Physics and Astronomy, Mars, Genetics and Molecular Biology, Mass wasting, 01 natural sciences, Article, General Biochemistry, Genetics and Molecular Biology, Elysium, Planetenphysik, Impact crater, 0103 physical sciences, Planetary science, Traitement du signal et de l'image, Petrology, lcsh:Science, 010303 astronomy & astrophysics, Duricrust, InSight, 0105 earth and related environmental sciences, Multidisciplinary, Geomorphology, Geology, Mars Exploration Program, General Chemistry, 15. Life on land, Regolith, Planetengeologie, General Biochemistry, Aeolian processes, lcsh:Q, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) spacecraft landed successfully on Mars and imaged the surface to characterize the surficial geology. Here we report on the geology and subsurface structure of the landing site to aid in situ geophysical investigations. InSight landed in a degraded impact crater in Elysium Planitia on a smooth sandy, granule- and pebble-rich surface with few rocks. Superposed impact craters are common and eolian bedforms are sparse. During landing, pulsed retrorockets modified the surface to reveal a near surface stratigraphy of surficial dust, over thin unconsolidated sand, underlain by a variable thickness duricrust, with poorly sorted, unconsolidated sand with rocks beneath. Impact, eolian, and mass wasting processes have dominantly modified the surface. Surface observations are consistent with expectations made from remote sensing data prior to landing indicating a surface composed of an impact-fragmented regolith overlying basaltic lava flows., The InSight spacecraft landed on Mars on November 2018. Here, the authors characterize the surficial geology of the landing site and compare with observations and models derived from remote sensing data prior to landing and from ongoing in situ geophysical investigations of the subsurface.

Published
2020

31. Is there a Seasonality of the Martian Seismic Event Rate?

Author

Savas Ceylan, Constantinos Charalambous, Renee Weber, Simon Stähler, Anna Horleston, Martin van Driel, Domenico Giardini, Philippe Lognonné, Raphaël F. Garcia, Maren Böse, John Clinton, W. Bruce Banerdt, John-Robert Scholz, Martin Knapmeyer, Mark P. Panning, Amir Khan, Taichi Kawamura, and William T. Pike

Subjects
Martian, Climatology, Event (relativity), InSight Mars Seismizität, medicine, Seasonality, medicine.disease, Geology
Abstract

We analyze the sequence of seismic events of different types as recorded by the SEIS instrument of the InSight mission. After several weeks without any detection, event counts started to increase at the end of May 2019. The majority of recorded events belongs to the class of 2.4 Hz events, which prominently excite a continuously observed natural resonance frequency.After a sudden onset of seismic detections by the end of May 2019 (about sol 180, LS≈32°), especially the combined event rate of the High Frequency, Very High Frequency, and 2.4 Hz family of events increased from 3.6 events/sol in June 2019 to more than 9 events/sol until late August 2019, i.e. increased by a factor of about 3.Estimating event rates as if events are the result of a constant-rate Poisson process leads to contradictions with the statistical properties of those, either in the cumulative event count or in the lag time distribution. These contradictions can be overcome by assuming a step-wise increase of the event rate.Any deviation from a purely random occurrence of quakes, in both time and space, requires a mechanism to suppress or support the source process. The seismic activity of the Moon is mainly controlled by tidal deformation, at least in terms of source time. What controls the event rate of Martian high frequency events is currently elusive.

Published
2020

32. 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

33. The atmosphere of Mars as observed by InSight

Author

Justin N. Maki, A. Jacob, Stephen R. Lewis, Nicholas A Teanby, Mercedes Marin-Jimenez, Anna Mittelholz, Constantinos Charalambous, Sara Navarro, M. M. Baker, Mark T. Lemmon, Tristram Warren, Javier Gómez-Elvira, Alexander E. Stott, Matthew P. Golombek, Antoine Lucas, Jorge Pla-Garcia, J. Torres, Eric Beucler, Balthasar Kenda, Aymeric Spiga, Rudolf Widmer-Schnidrig, Philippe Lognonné, Veronique Ansan, V. Peinado, Özgür Karatekin, William T. Pike, Nils Mueller, Savas Ceylan, K. Hurst, Daniel Viúdez-Moreiras, Christopher T. Russell, Antonio Molina, Sebastien Rodriguez, Clément Perrin, Naomi Murdoch, David Mimoun, Claire E. Newman, Ralph D. Lorenz, L. Martire, Luis Mora-Sotomayor, Simon Stähler, Tilman Spohn, Lucie Rolland, Stephen Sackett, Ingrid Daubar, Raphaël F. Garcia, W. Bruce Banerdt, Catherine L. Johnson, Domenico Giardini, Brian Carcich, Don Banfield, Suzanne E. Smrekar, John Clinton, François Forget, Ehouarn Millour, Taichi Kawamura, J. A. Rodríguez-Manfredi, Bart Van Hove, A. Lepinette, Anni Määttänen, J. B. McClean, Cornell Center for Astrophysics and Planetary Science (CCAPS), Cornell University, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Aeolis Research, Space Science Institute [Boulder] (SSI), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Royal Observatory of Belgium [Brussels], School of Earth Sciences [Bristol], University of Bristol [Bristol], Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Department of Electrical and Electronic Engineering [London] (DEEE), Imperial College London, Department of Earth, Ocean and Atmospheric Sciences [Vancouver] (EOAS), University of British Columbia (UBC), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Sorbonne Université (SU), School of Physical Sciences [Milton Keynes], The Open University [Milton Keynes] (OU), Swiss Seismological Service [ETH Zurich] (SED), Institute of Geophysics [ETH Zürich], Department of Earth Sciences [ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Department of Earth Sciences [ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Department of Physics [Oxford], University of Oxford [Oxford], Department of Earth, Environmental and Planetary Sciences [Providence], Brown University, Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Université Côte d'Azur (UCA), Universität Stuttgart [Stuttgart], Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Morton K. Blaustein Department of Earth and Planetary Sciences [Baltimore], Johns Hopkins University (JHU), Center for Earth and Planetary Studies [Washington] (CEPS), Smithsonian National Air and Space Museum, Smithsonian Institution-Smithsonian Institution, Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), University of California-University of California, Département Electronique, Optronique et Signal (DEOS), Cornell University [New York], École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Royal Observatory of Belgium [Brussels] (ROB), NASA-California Institute of Technology (CALTECH), Department of Earth, Ocean and Atmospheric Sciences [Vancouver] (UBC EOAS), PLANETO - LATMOS, Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)-Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), University of Oxford, University of California (UC)-University of California (UC), ANR-14-CE36-0012,SEISMARS,Seismology on Mars(2014), ANR-19-CE31-0008,MAGIS,MArs Geophysical InSight(2019), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Määttänen, A. [0000-0002-7326-8492], Martire, L. [0000-0002-9402-6150], Rodríguez Manfredi, J. A. [0000-0003-0461-9815], Lognonné, P. [0000-0002-1014-920X], Rodríguez, S. [0000-0003-1219-0641], Spiga, A. [0000-0002-6776-6268], Perrin, C. [0000-0002-7200-5682], Molina, A. [0000-0002-5038-2022], García, R. [0000-0003-1460-6663], Murdoch, N. [0000-0002-9701-4075], Lorenz, R. [0000-0001-8528-4644], Mittelholz, A. [0000-0002-5603-7334], Kawamura, T. [0000-0001-5246-5561], Widmer Schnidrig, R. [0000-0001-9698-2739], McClean, J. [0000-0002-7863-0120], Mueller, N. [0000-0001-9229-8921], Lewis, S. [0000-0001-7237-6494], Teanby, N. [0000-0003-3108-5775], Warren, T. [0000-0003-3877-0046], Milliour, E. [0000-0003-4808-9203], Lemmon, M. [0000-0002-4504-5136], Clinton, J. [0000-0001-8626-2703], Ceylan, S. [0000-0002-6552-6850], Banfield, D. [0000-0003-2664-0164], Agence Nationale de la Recherche (ANR), and Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)

Subjects
Martian, 010504 meteorology & atmospheric sciences, Atmosphere, Mars, Mars Exploration Program, Atmosphere of Mars, 010502 geochemistry & geophysics, Mars Atmosphere, 01 natural sciences, Wind speed, Astrobiology, Autre, 13. Climate action, Dust storm, [SDU]Sciences of the Universe [physics], General Earth and Planetary Sciences, Environmental science, Aeolian processes, [SDU.OTHER]Sciences of the Universe [physics]/Other, Meteorologie, InSight mission, Dust devil, 0105 earth and related environmental sciences, InSight
Abstract

Banfield, D. et al., The atmosphere of Mars is thin, although rich in dust aerosols, and covers a dry surface. As such, Mars provides an opportunity to expand our knowledge of atmospheres beyond that attainable from the atmosphere of the Earth. The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) lander is measuring Mars’s atmosphere with unprecedented continuity, accuracy and sampling frequency. Here we show that InSight unveils new atmospheric phenomena at Mars, especially in the higher-frequency range, and extends our understanding of Mars’s meteorology at all scales. InSight is uniquely sensitive to large-scale and regional weather and obtained detailed in situ coverage of a regional dust storm on Mars. Images have enabled high-altitude wind speeds to be measured and revealed airglow—faint emissions produced by photochemical reactions—in the middle atmosphere. InSight observations show a paradox of aeolian science on Mars: despite having the largest recorded Martian vortex activity and dust-devil tracks close to the lander, no visible dust devils have been seen. Meteorological measurements have produced a catalogue of atmospheric gravity waves, which included bores (soliton-like waves). From these measurements, we have discovered Martian infrasound and unexpected similarities between atmospheric turbulence on Earth and Mars. We suggest that the observations of Mars’s atmosphere by InSight will be key for prediction capabilities and future exploration., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737); Centro de Desarrollo Tecnológico e Industrial (CDTI), Ministerio de Economía y Competitividad and the Instituto Nacional de Técnica Aeroespacial (INTA).

Published
2020

34. Full-Band Signal Extraction From Sensors in Extreme Environments: The NASA InSight Microseismometer

Author

Alexander E. Stott, Constantinos Charalambous, William T. Pike, Tristram Warren, and Science & Technology Facilities Council

Subjects
Technology, Computer science, instrument response correction, 0205 Optical Physics, 02 engineering and technology, 01 natural sciences, Physics, Applied, NOISE, Analytical Chemistry, Engineering, 0103 physical sciences, Electrical and Electronic Engineering, MEMS seismometer, temperature dependence, Instruments & Instrumentation, 010303 astronomy & astrophysics, Instrumentation, Decorrelation, Remote sensing, Sensor fusion, Signal processing, Science & Technology, Physics, Attenuation, Bandwidth (signal processing), Engineering, Electrical & Electronic, Kalman filter, Mars Exploration Program, 021001 nanoscience & nanotechnology, 0906 Electrical and Electronic Engineering, Physical Sciences, space applications, SEISMOMETER, 0210 nano-technology, 0913 Mechanical Engineering
Abstract

Physically meaningful signal extraction from sensors deployed in extreme environments requires a combination of attenuation of confounding inputs and the removal of their residual using decorrelation techniques. In space applications where the resources for physical attenuation are limited, there is a necessity to apply the most effective post-processing analysis available. This paper describes the extraction of the seismic signal from an MEMS microseismometer to be deployed on the surface of Mars. The signal processing, which covers the full bandwidth $1 \times 10^{-5}$ Hz to 40 Hz, uses a novel application of sensor fusion through an indirect Kalman Filter in combination with a thermal model of the microseismometer to remove the aseismic contribution of temperature over the frequency range. Owing to the full-band decorrelation, the analysis (based on pre-landing testing in analogous scenarios) produces both a characterization of the microseismomter and a signal processing approach for information retrieval on Mars, along with other planetary and terrestrial planetary deployments.

Published
2018

35. Passive Method for Reducing Temperature Sensitivity of a Microelectromechanical Seismic Accelerometer for Marsquake Monitoring Below 1 Nano- g

Author

Alexander E. Stott, William T. Pike, Constantinos Charalambous, and Huafeng Liu

Subjects
Materials science, Gravimeter, Acoustics, General Physics and Astronomy, 02 engineering and technology, 021001 nanoscience & nanotechnology, Accelerometer, 01 natural sciences, Displacement (vector), Thermal expansion, Acceleration, Thermoelastic damping, 0103 physical sciences, Sensitivity (control systems), 010306 general physics, 0210 nano-technology, Reduction (mathematics)
Abstract

The passive technology described in this paper is important for reducing the thermoelastic response of silicon-based high-precision accelerometers and gravimeters. This study uses the angular strain induced by mismatched coefficients of thermal expansion to passively compensate for the sag displacement in Si-based spring-mass systems in environments with fluctuating temperature. The hundredfold reduction in temperature sensitivity allows a top acceleration sensitivity of less than 10${}^{\ensuremath{-}9}$ $g$. Such a temperature-compensated seismic accelerometer has already been used as a science payload of the InSight Mars lander, which touched down in November 2018, for marsquake monitoring.

Published
2019

36. Sparse Reconstruction of Aliased Seismic Signals Recorded During the Insight Mars Mission

Author

Raphaël F. Garcia, David Sollberger, Sharon Kedar, Thomas Haag, Troy L. Hudson, Philippe Lognonné, Nienke Brinkman, John Clinton, Martin van Driel, Domenico Giardini, Peter Zweifel, Cedric Schmelzbach, Jan ten Pierick, Fredrik Andersson, Matthias Grott, Simon Stähler, Johan O. A. Robertsson, Tilman Spohn, William B. Banerdt, and William T. Pike

Subjects
Seismometer, 010504 meteorology & atmospheric sciences, Radon transform, Signal reconstruction, Wavelet transform, Iterative reconstruction, Mars Exploration Program, 010502 geochemistry & geophysics, 01 natural sciences, Nyquist–Shannon sampling theorem, Nyquist frequency, Seismology, Geology, 0105 earth and related environmental sciences
Abstract

The NASA InSight lander successfully placed a seismometer on the surface of Mars. Alongside, a hammering device was deployed that penetrated into the ground to attempt the first measurements of the planetary heat flow of Mars. The hammering generated repeated seismic signals that were registered by the seismometer. These signals can potentially be used to image the shallow subsurface just below the lander. However, the frequencies excited by the hammering probe widely exceed the Nyquist frequency dictated by the seis-mometer's sampling rate. Here, we propose an algorithm to reconstruct the seismic signals beyond the classical sampling theorem. We exploit the structure in the data due to thousands of repeated, only gradually varying hammering signals as the heat probe slowly penetrates into the ground. This allows us to reconstruct signals by enforcing a sparsity constraint in a modified Radon transform domain.

Published
2019

37. The first active seismic experiment on Mars to characterize the shallow subsurface structure at the InSight landing site

Author

Matthias Grott, K. Hurst, Johan O. A. Robertsson, Cedric Schmelzbach, Domenico Giardini, P. H. Lognonné, M. van Driel, Brigitte Knapmeyer-Endrun, Nicholas A Teanby, A. KiVely, C. Vretto, Christian Krause, David Sollberger, Sharon Kedar, T. Spohn, Nienke Brinkman, Lucile Fayon, J. ten Pierick, Simon Stähler, Anna Horleston, William B. Banerdt, Troy L. Hudson, William T. Pike, Fredrik Andersson, and Pierre Delage

Subjects
Reflection (physics), Mars Exploration Program, Aliasing (computing), Geology, Seismology
Published
2019

38. 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

40. SIZE-FREQUENCY DISTRIBUTION OF ROCKS AT THE INSIGHT LANDING SITE

Author

Ernst Hauber, A. Trussell, Catherine M. Weitz, Constantinos Charalambous, Nicholas H. Warner, Nathan R. Williams, William T. Pike, and Matthew P. Golombek

Subjects
Distribution (number theory), Size frequency, Mineralogy, Geology
Published
2019

41. MODIFICATION OF HOMESTEAD HOLLOW AT THE INSIGHT LANDING SITE

Author

John A. Grant, Nicholas H. Warner, Maria E. Banks, Catherine M. Weitz, A. DeMott, Matthew P. Golombek, M. Kopp, Fred Calef, H. Lethcoe-Wilson, Ernst Hauber, Constantinos Charalambous, Veronique Ansan, William T. Pike, Sharon A. Wilson, and Nathan R. Williams

Published
2019

42. SEISMIC ACTIVITY LEVEL OF MARS ESTIMATED FROM 140 SOLS OF INSIGHT DATA

Author

Martin van Driel, Sharon Kedar, Philippe Lognonné, Taichi Kawamura, Amir Khan, Domenico Giardini, William T. Pike, Guenole Mainsant, Maren Böse, Savas Ceylan, John-Robert Scholz, William B. Banerdt, Martin Knapmeyer, Mark P. Panning, John Clinton, Simon Stähler, and Anna Horleston

Subjects
Activity level, Geophysics, Mars Exploration Program, Geology
Published
2019

43. A Numerical Model of the SEIS Leveling System Transfer Matrix and Resonances: Application to SEIS Rotational Seismology and Dynamic Ground Interaction

Author

Brigitte Knapmeyer-Endrun, Lucile Fayon, M. Bierwirth, Pierre Delage, Cedric Schmelzbach, Sharon Kedar, Philippe Lognonné, Nicolas Verdier, William T. Pike, William B. Banerdt, S. Tillier, Naomi Murdoch, Raphaël F. Garcia, Foivos Karakostas, Kenneth Hurst, A. Kramer, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), 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), University of Cologne, Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, 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), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Centre National d'Études Spatiales [Toulouse] (CNES), Imperial College London, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), and Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)

Subjects
Seismometer, Peak ground acceleration, 010504 meteorology & atmospheric sciences, Mars, 01 natural sciences, Transfer function, Regolith, symbols.namesake, [INFO.INFO-TS]Computer Science [cs]/Signal and Image Processing, Autre, 0103 physical sciences, medicine, Torque, Traitement du signal et de l'image, Rayleigh scattering, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, InSight, Stiffness, Astronomy and Astrophysics, Space and Planetary Science, Surface wave, symbols, Phase velocity, medicine.symptom, [SDU.OTHER]Sciences of the Universe [physics]/Other, Geology, Seismology
Abstract

International audience; Abstract Both sensors of the SEIS instrument (VBBs and SPs) are mounted on the mechanical leveling system (LVL), which has to ensure a level placement on the Martian ground under currently unknown local conditions, and provide the mechanical coupling of the seismometers to the ground. We developed a simplified analytical model of the LVL structure in order to reproduce its mechanical behavior by predicting its resonances and transfer function. This model is implemented numerically and allows to estimate the effects of the LVL on the data recorded by the VBBs and SPs on Mars. The model is validated through comparison with the horizontal resonances (between 35 and 50 Hz) observed in laboratory measurements. These modes prove to be highly dependent of the ground horizontal stiffness and torque. For this reason, an inversion study is performed and the results are compared with some experimental measurements of the LVL feet’s penetration in a martian regolith analog. This comparison shows that the analytical model can be used to estimate the elastic ground properties of the InSight landing site. Another application consists in modeling the 6 sensors on the LVL at their real positions, also considering their sensitivity axes, to study the performances of the global SEIS instrument in translation and rotation. It is found that the high frequency ground rotation can be measured by SEIS and, when compared to the ground acceleration, can provide ways to estimate the phase velocity of the seismic surface waves at shallow depths. Finally, synthetic data from the active seismic experiment made during the HP3 penetration and SEIS rotation noise are compared and used for an inversion of the Rayleigh phase velocity. This confirms the perspectives for rotational seismology with SEIS which will be developed with the SEIS data acquired during the commissioning phase after landing.

Published
2018

44. Standing on Apollo’s Shoulders: A Microseismometer for the Moon

Author

William T. Pike, Mark P. Panning, I. M. Standley, Ceri Nunn, S. B. Calcutt, and Sharon Kedar

Subjects
Geophysics, biology, Space and Planetary Science, Shoulders, Earth and Planetary Sciences (miscellaneous), Apollo, Astronomy and Astrophysics, Ancient history, biology.organism_classification, Geology
Abstract

Seismometers deployed on the Moon by the Apollo astronauts from 1969 to 1972 detected moonquakes and impacts, and added to our understanding of the lunar interior. Several lunar missions are currently being planned, including the Commercial Lunar Payload Services (CLPS), the Lunar Geophysical Network, and the astronaut program Artemis. We propose a microseismometer for the Moon: the Silicon Seismic Package (SSP). The SSP’s sensors are etched in silicon, and are predicted to have a noise floor below 2 × 10 − 10 ( m s − 2 ) / Hz between 0.3 and 3 Hz (similar to the Apollo instruments between 0.3 and 0.5 Hz, and better than Apollo above 0.5 Hz). The SSP will measure horizontal and vertical motion with the three sensors in a triaxial configuration. The instrument is robust to high shock and vibration and has an operational range from −80°C to +60°C, allowing deployment under harsh conditions. The first-generation version of this sensor, the SEIS-SP, was deployed on Mars in 2018 as part of the InSight mission’s seismic package. We will reconfigure the seismometer for the lower gravity of the Moon. We estimate that a single SSP instrument operating for one year would detect around 74 events above a signal-to-noise ratio of 2.5, as well as an additional 500+ above the noise floor. A mission lasting from lunar dawn until dusk, carried on a CLPS lander, could test the instrument in situ, and provide invaluable information for an extensive future network.

Published
2021

45. The Marsquake catalogue from InSight, sols 0–478

Author

Don Banfield, Alexander E. Stott, Maren Böse, Philippe Lognonné, Guenolé Orhand-Mainsant, William T. Pike, Fabian Euchner, Eric Beucler, Mark P. Panning, Amir Khan, Raphaël F. Garcia, Constantinos Charalambous, Savas Ceylan, John Clinton, Aymeric Spiga, Simon Stähler, Anna Horleston, Sharon Kedar, Taichi Kawamura, Suzanne E. Smrekar, Nikolaj Dahmen, William B. Banerdt, John-Robert Scholz, Clément Perrin, Domenico Giardini, Martin van Driel, Swiss Seismological Service [ETH Zurich] (SED), 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 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), Imperial College London, School of Earth Sciences [Bristol], University of Bristol [Bristol], 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), Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, California Institute of Technology (CALTECH), Cornell Center for Astrophysics and Planetary Science (CCAPS), 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), 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 Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)

Subjects
Seismometer, 010504 meteorology & atmospheric sciences, Physics and Astronomy (miscellaneous), [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Marsquakes, Mars seismicity catalogue, InSight mission, Induced seismicity, 010502 geochemistry & geophysics, 01 natural sciences, Mars Seismology, Autre, Long period, Short duration, 0105 earth and related environmental sciences, Data collection, Event (computing), Astronomy and Astrophysics, Mars Exploration Program, Key features, Geophysics, 13. Climate action, Space and Planetary Science, Geology, Seismology
Abstract

The InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission began collecting high quality seismic data on Mars in February 2019. This manuscript documents the seismicity observed by SEIS, InSight’s seismometer, from this time until the end of March 2020. Within the InSight project, the Marsquake Service (MQS) is responsible for prompt review of all seismic data collected by InSight, detection of events that are likely to be of seismic origin, and curation and release of seismic catalogues. In the first year of data collection, MQS have identified 465 seismic events that we interpret to be from regional and teleseismic marsquakes. Seismic events are grouped into 2 different event families: the low frequency family is dominated by energy at long period below 1 s, and the high frequency family primarily include energy at and above 2.4 Hz. Event magnitudes, from Mars-specific scales, range from 1.3 to 3.7. A third class of events with very short duration but high frequency bursts have been observed 712 times. These are likely associated with a local source driven by thermal stresses. This paper describes the data collected so far in the mission and the procedures under which MQS operates; summarises the content of the current MQS seismic catalogue; and presents the key features of the events we have observed so far, using the largest events as examples. ISSN:0031-9201 ISSN:1872-7395

Published
2021

46. Isolation of seismic signal from InSight/SEIS-SP microseismometer measurements

Author

Naomi Murdoch, Tristram Warren, David Mimoun, Neil Bowles, Jane Hurley, S. B. Calcutt, Nicholas A Teanby, William T. Pike, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), University of Bristol (UNITED KINGDOM), Imperial College London (UNITED KINGDOM), Science and Technology Facilities Council - STFC (UNITED KINGDOM), University of Oxford (UNITED KINGDOM), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Département Electronique, Optronique et Signal (DEOS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), University of Bristol [Bristol], University of Oxford [Oxford], and Imperial College London

Subjects
Seismometer, Decorrelation, 010504 meteorology & atmospheric sciences, Mars, 01 natural sciences, 7. Clean energy, Shield, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, InSight, Martian, [SCCO.NEUR]Cognitive science/Neuroscience, Suite, Neurosciences, Astronomy and Astrophysics, Inversion (meteorology), Mars Exploration Program, Regolith, 13. Climate action, Space and Planetary Science, Noise, Geology
Abstract

International audience; The InSight mission is due to launch in May 2018, carrying a payload of novel instruments designed and tested to probe the interior of Mars whilst deployed directly on the Martian regolith and partially isolated from the Martian environment by the Wind and Thermal Shield. Central to this payload is the seismometry package SEIS consisting of two seismometers, which is supported by a suite of environmental/meteorological sensors (Temperature and Wind Sensor for InSight TWINS; and Auxiliary Payload Sensor Suite APSS). In this work, an optimal estimations inversion scheme which aims to decorrelate the short-period seismometer (SEIS-SP) signal due to seismic activity alone from the environmental signal and random noise is detailed, and tested on both simulated and Viking data. This scheme also applies a module to identify measurements contaminated by Single Event Phenomena (SEP). This scheme will be deployed as the pre-processing pipeline for all SEIS-SP data prior to release to the scientific community for analysis.

Published
2018

47. Geology and Physical Properties Investigations by the InSight Lander

Author

Sylvain Piqueux, Pierre Delage, William B. Banerdt, Ingrid Daubar, Nils Müller, Matthias Grott, Antoine Lucas, Tamara Gudkova, U. R. Christensen, Johan O. A. Robertsson, Don Banfield, Brigitte Knapmeyer-Endrun, T. Spohn, Suzanne E. Smrekar, Lucile Fayon, David Sollberger, Ralph D. Lorenz, Domenico Giardini, D. Kipp, G. Kargl, Matthew P. Golombek, Nicholas A Teanby, Sharon Kedar, B. Kenda, Ashitey Trebi-Ollennu, Raphaël F. Garcia, Ernst Hauber, Paul Morgan, Khaled Ali, Roy Lichtenheldt, Aymeric Spiga, Philippe Lognonné, Jason P. Marshall, Naomi Murdoch, David Mimoun, Cedric Schmelzbach, Joana Voigt, Constantinos Charalambous, Justin N. Maki, Veronique Ansan, William T. Pike, T. Nicollier, José E. Andrade, Mark P. Panning, Sebastien Rodriguez, Nicholas H. Warner, Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), 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), Département Electronique, Optronique et Signal (DEOS), 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 Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), German Aerospace Center (DLR), Division of Engineering and Applied Science, California Institute of Technology, California Institute of Technology (CALTECH), School of Earth Sciences [Bristol], University of Bristol [Bristol], Interactions et dynamique des environnements de surface (IDES), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Deutsches Zentrum für Luft- und Raumfahrt (DLR), Jülich Centre for Neutron Science (JCNS - PGI, JARA-FIT), Peter Grünberg Institut, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Cornell University, Departments of Anesthesiology and Physiology and Biophysics, University of Alabama at Birmingham [ Birmingham] (UAB), UNS-CNRS-Observatoire de la Côte d'Azur, 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), Department of Mechanical Engineering [Imperial College London], Imperial College London, University of Arizona, 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), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), University of Florida [Gainesville], Schmidt United Institute of Physics of the Earth [Moscow] (IPE), Russian Academy of Sciences [Moscow] (RAS), Departamento de Ecologia (CEAMISH), Universidad Autonoma del Estado de Morelos (UAEM), 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 National Polythechnique Houphouet Boigny, California Institute of Technology (CALTECH)-NASA, 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, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Wind stress, Mars, 01 natural sciences, Wind speed, Seismic wave, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Planetenphysik, 0103 physical sciences, Traitement du signal et de l'image, [SDU.STU.GM]Sciences of the Universe [physics]/Earth Sciences/Geomorphology, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, 010303 astronomy & astrophysics, Dust devil, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, InSight, Raumfahrt-Systemdynamik, Physical properties, Leitungsbereich PF, Astronomy and Astrophysics, Geology, Geophysics, Mars Exploration Program, Surface materials, InSight Mars Geology Physical properties Surface materials, Regolith, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Planetengeologie, Space and Planetary Science, Hesperian, [SPI.SIGNAL]Engineering Sciences [physics]/Signal and Image processing
Abstract

International audience; Although not the prime focus of the InSight mission, the near-surface geology and physical properties investigations provide critical information for both placing the instruments (seismometer and heat flow probe with mole) on the surface and for understanding the nature of the shallow subsurface and its effect on recorded seismic waves. Two color cameras on the lander will obtain multiple stereo images of the surface and its interaction with the spacecraft. Images will be used to identify the geologic materials and features present, quantify their areal coverage, help determine the basic geologic evolution of the area, and provide ground truth for orbital remote sensing data. A radiometer will measure the hourly temperature of the surface in two spots, which will determine the thermal inertia of the surface materials present and their particle size and/or cohesion. Continuous measurements of wind speed and direction offer a unique opportunity to correlate dust devils and high winds with eolian changes imaged at the surface and to determine the threshold friction wind stress for grain motion on Mars. During the first two weeks after landing, these investigations will support the selection of instrument placement locations that are relatively smooth, flat, free of small rocks and load bearing. Soil mechanics parameters and elastic properties of near surface materials will be determined from mole penetration and thermal conductivity measurements from the surface to 3–5 m depth, the measurement of seismic waves during mole hammering, passive monitoring of seismic waves, and experiments with the arm and scoop of the lander (indentations, scraping and trenching). These investigations will determine and test the presence and mechanical properties of the expected 3–17 m thick fragmented regolith (and underlying fractured material) built up by impact and eolian processes on top of Hesperian lava flows and determine its seismic properties for the seismic investigation of Mars’ interior.

Published
2018

48. A broad-band silicon microseismometer with 0.25 NG/rtHz performance

Author

I. M. Standley, S. B. Calcutt, William T. Pike, and A. G. Mukherjee

Subjects
Seismometer, Microelectromechanical systems, Materials science, Silicon, business.industry, 010401 analytical chemistry, Bandwidth (signal processing), chemistry.chemical_element, Broad band, 02 engineering and technology, 021001 nanoscience & nanotechnology, 01 natural sciences, Noise floor, 0104 chemical sciences, Vibration, Transducer, chemistry, Optoelectronics, 0210 nano-technology, business
Abstract

We report a micromachined silicon seismometer with a sensitivity of 0.25 ng/rtHz from 0.1 to 10 Hz. This represents the highest performance of a MEMS inertial sensor to date, and in particular is at or below the noise floor of the Earth's lowest ambient seismic levels over this bandwidth with a performance comparable to conventional seismometers. The microseismometer is robust to high shock (> 1000 g) and vibration (> 30 g rms), and can operate from +60C to −80 C allowing deployment under harsh conditions.

Published
2018

49. Vital Signs: Seismology of Icy Ocean Worlds

Author

Mark P. Panning, Steven D. Vance, Philippe Lognonné, William T. Pike, Julie C. Castillo, Alyssa Rhoden, Sharon Kedar, Bruce G. Bills, Victor C. Tsai, Simon Stähler, Hsin-Hua Huang, Ralph D. Lorenz, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), 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), Leibniz Inst Balt Sea Res IOW, Rostock, Germany, NASA, Jet Prop Lab, CALTECH, 4800 Oak Grove Dr, Pasadena, CA 91109 USA, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Institute of Earth Sciences, Academia Sinica, Taipei, Taiwan, CALTECH, Seismol Lab, Pasadena, CA 91125 USA, Imperial College London, 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), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA, and partially supported by strategic research and tech-nology funds from the Jet Propulsion Laboratory, Caltech,and by the Icy Worlds node of NASA’s Astrobiology Institute(13-13NAI7_2-0024). The research was carried out at the JetPropulsion Laboratory, California Institute of Technology,under a contract with the National Aeronautics and SpaceAdministration

Subjects
GALILEO PHOTOPOLARIMETER-RADIOMETER, Extraterrestrial Environment, 010504 meteorology & atmospheric sciences, SHELL THICKNESS, Oceans and Seas, Planetary engineering, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, Tidal Waves, 01 natural sciences, Physics::Geophysics, Astrobiology, SUBSURFACE OCEAN, Exobiology, 0103 physical sciences, INTERIOR STRUCTURE, AMMONIUM-SULFATE, Moon, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, SEISMIC DETECTION, GRAVITY-FIELD, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, Habitability, I SHELLS, TIDAL DISSIPATION, Ice, Temperature, THERMAL EVOLUTION, Mars Exploration Program, Agricultural and Biological Sciences (miscellaneous), Tectonics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, business, Energy source, Tidal power, Geology
Abstract

International audience; Ice-covered ocean worlds possess diverse energy sources and associated mechanisms that are capable of driving significant seismic activity, but to date no measurements of their seismic activity have been obtained. Such investigations could reveal the transport properties and radial structures, with possibilities for locating and characterizing trapped liquids that may host life and yielding critical constraints on redox fluxes and thus on habitability. Modeling efforts have examined seismic sources from tectonic fracturing and impacts. Here, we describe other possible seismic sources, their associations with science questions constraining habitability, and the feasibility of implementing such investigations. We argue, by analogy with the Moon, that detectable seismic activity should occur frequently on tidally flexed ocean worlds. Their ices fracture more easily than rocks and dissipate more tidal energy than the

Published
2018

50. A Pre-Landing Assessment of Regolith Properties at the InSight Landing Site

Author

Sylvain Piqueux, Naomi Murdoch, Matthias Grott, Brigitte Knapmeyer-Endrun, Axel Hagermann, Pierre Delage, Matthew A. Siegler, Sharon Kedar, Paul Morgan, Nicholas A Teanby, William T. Pike, Roy Lichtenheldt, Philippe Lognonné, Constantinos Charalambous, Nils Müller, Matthew P. Golombek, Ingrid Daubar, Colorado School of Mines, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), 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 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), Département Electronique, Optronique et Signal (DEOS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Imperial College London, The Open University [Milton Keynes] (OU), University of Bristol [Bristol], and Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE)

Subjects
Asteroiden und Kometen, Seismometer, 010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Mécanique des fluides, Mars, Thermal diffusivity, Regolith, 01 natural sciences, InSight landing site, Seismic wave, Physics::Geophysics, [SPI]Engineering Sciences [physics], Planetenphysik, 0103 physical sciences, Emissivity, Regolith Physical properties, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physical properties, Raumfahrt-Systemdynamik, Spacecraft, business.industry, Mars · Regolith · Physical properties · InSight landing site, Astronomy and Astrophysics, Geophysics, Mars Exploration Program, Planetary science, Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, business, Geology
Abstract

International audience; This article discusses relevant physical properties of the regolith at the Mars InSight landing site as understood prior to landing of the spacecraft. InSight will land in the northern lowland plains of Mars, close to the equator, where the regolith is estimated to be ≥3--5 m thick. These investigations of physical properties have relied on data collected from Mars orbital measurements, previously collected lander and rover data, results of studies of data and samples from Apollo lunar missions, laboratory measurements on regolith simulants, and theoretical studies. The investigations include changes in properties with depth and temperature. Mechanical properties investigated include density, grain-size distribution, cohesion, and angle of internal friction. Thermophysical properties include thermal inertia, surface emissivity and albedo, thermal conductivity and diffusivity, and specific heat. Regolith elastic properties not only include parameters that control seismic wave velocities in the immediate vicinity of the Insight lander but also coupling of the lander and other potential noise sources to the InSight broadband seismometer. The related properties include Poisson’s ratio, P- and S-wave velocities, Young’s modulus, and seismic attenuation. Finally, mass diffusivity was investigated to estimate gas movements in the regolith driven by atmospheric pressure changes. Physical properties presented here are all to some degree speculative. However, they form a basis for interpretation of the early data to be returned from the InSight mission.

Published
2018

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