Brigitte Knapmeyer‐Endrun

Deutsches Zentrum für Luft- und Raumfahrt e. V. (DLR)

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Philippe Lognonné

Université Paris Cité

W. B. Banerdt

Jet Propulsion Laboratory

Domenico Giardini

ETH Zurich

R. García

Institut Superieur de l'Aeronautique et de l'Espace (ISAE-SUPAERO)

M. P. Panning

Jet Propulsion Laboratory

Simon C. Stähler

ETH Zurich

John Clinton

ETH Zurich

W. T. Pike

Imperial College London

Taïchi Kawamura

Institut de physique du globe de Paris

Martin van Driel

Czech Academy of Sciences, Institute of Geophysics

Cooperative Institutions

Centre National de la Recherche Scientifique

101

Jet Propulsion Laboratory

California Institute of Technology

ETH Zurich

Centre National d'Études Spatiales

Institut de physique du globe de Paris

Université Paris Cité

Planetary Science Institute

Ruhr University Bochum

Institut de Recherche pour le Développement

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Microseismicity On Crete

EGS General Assembly Conference Abstracts (2002)

Thomas Meier M. Rische Olaf Knabenbauer Stefan Baisch Lars Ceranna

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Improving Constraints on Planetary Interiors With PPs Receiver Functions

Journal of Geophysical Research Planets (2021)

Doyeon Kim V. Lekić J. C. E. Irving N. C. Schmerr Brigitte Knapmeyer‐Endrun

Seismological constraints obtained from receiver function (RF) analysis provide important information about the crust and mantle structure. Here, we explore the utility of the free-surface multiple of the P-wave (PP) and the corresponding conversions in RF analysis. Using earthquake records, we demonstrate the efficacy of PPs-RFs before illustrating how they become especially useful when limited data is available in typical planetary missions. Using a transdimensional hierarchical Bayesian deconvolution approach, we compute robust P-to-S (Ps)- and PPs-RFs with

Receiver function

10.1029/2021je006983

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Citations (49)

InSight seismic data from Mars: Effect and treatment of transient data disturbances

AGU Fall Meeting Abstracts (2020)

John‐Robert Scholz Rudolf Widmer‐Schnidrig Paul D. Davis Philippe Lognonné Baptiste Pinot

Transient (computer programming)

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

Nienke Brinkman Cédric Schmelzbach David Sollberger Martin van Driel Jan ten Pierick

In November 2018, the InSight lander successfully touched down in the Elysium Planitia plain on Mars. Since then, two scientific instruments were deployed directly onto the surface of Mars: (1) SEIS, a package consisting of two three component seismic sensors and (2) HP3, the heat flow and physical properties package. HP3 includes a self-hammering penetrator (mole) that hammers itself into the subsurface of Mars to a maximum depth of five meters. The mole hammering generates seismic signals that are recorded by SEIS and can be used to image the shallow subsurface just below the landing site. Even though not included in the level-one mission's objectives, this opportunistic seismic experiment is, to the best of our knowledge, the first active seismic experiment ever conducted on a different planet. Here, we discuss the most important aspects of the implementations of this opportunistic experiment. Presentation Date: Monday, September 16, 2019 Session Start Time: 1:50 PM Presentation Start Time: 3:30 PM Location: 301B Presentation Type: Oral

Mars landing

10.1190/segam2019-3215661.1

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Constraints for the Martian Crustal Structure From Rayleigh Waves Ellipticity of Large Seismic Events

Geophysical Research Letters (2023)

Sebastián Carrasco Brigitte Knapmeyer‐Endrun Ludovic Margerin Zongbo Xu Rakshit Joshi

Abstract For the first time, we measured the ellipticity of direct Rayleigh waves at intermediate periods (15–35 s) on Mars using the recordings of three large seismic Martian events, including S1222a, the largest event recorded by the InSight mission. These measurements, together with P‐to‐s receiver functions and P‐wave reflection times, were utilized for performing a joint inversion of the local crustal structure at the InSight landing site. Our inversion results are compatible with previously reported intra‐crustal discontinuities around 10 and 20 km depths, whereas the preferred models show a strong discontinuity at ∼37 km, which is interpreted as the crust‐mantle interface. Additionally, we support the presence of a shallow low‐velocity layer of 2–3 km thickness. Compared to nearby regions, lower seismic wave velocities are derived for the crust, suggesting a higher porosity or alteration of the whole local crust.

Classification of discontinuities

Rayleigh Wave

Discontinuity (linguistics)

10.1029/2023gl104816

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Stratification of Seismic Anisotropy in the Aegean Lithosphere and Relation to Deformation

AGUFM (2006)

Brigitte Knapmeyer‐Endrun Sergei Lebedev Thomas Meier

Seismic anisotropy

Seismotectonics

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SEIS/INSIGHT: One year prior launch for Seismic Discovery on Mars

EGUGA (2017)

Philippe Lognonné W. B. Banerdt Domenico Giardini W. Tom Pike U. Christensen

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Autocorrelation of the ground vibrations recorded by the SEIS-InSight seismometer on Mars

Nicolas Compaire Ludovic Margerin R. García Baptiste Pinot Marie Calvet

The SEIS seismometer of the InSight mission was deployed on the ground of Elysium Planitia, on 19 December 2018. Interferometry techniques can be used to extract information on the internal structure from the autocorrelation of seismic ambient noise and coda of seismic events. In a single-station configuration, the zero-offset global reflection of the ground vertically below the seismometer can be approximated by the stacked ZZ autocorrelation function (ACF) for P-waves and the stacked EE and NN ACFs for S-waves, assuming a horizontally layered medium and homogeneously distributed and mutually uncorrelated noise sources. We analyze continuous records from the very broadband seismometer (SEIS-VBB), and correct for potential environmental disturbances through systematic preprocessing. For each Sol (martian day), we computed the correlations functions in 24 windows of one martian hour in order to obtain a total correlation tensor for various Mars local times. In addition, a similar algorithm is applied to the Marsquake waveforms in different frequency bands. Both stability analysis and inter-comparison between background noise and seismic event results suggest that the background seismic noise at the landing site is reliably observed only around 2.4 Hz, where an unknown mechanism is amplifying the ground shaking, and only during early night hours, when the noise induced by atmospheric disturbances is minimum. Seismic energy arrivals are consistently observed across the various data-sets. Some of these arrivals present multiples. These observations are discussed in terms of Mars’ crustal structure.

Seismometer

Seismic Noise

Geophone

Seismic interferometry

Ground vibrations

10.1002/essoar.10503694.1

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Resonances of the InSight Seismometer on Mars

Bulletin of the Seismological Society of America (2021)

K. Hurst L. Fayon Brigitte Knapmeyer‐Endrun Cédric Schmelzbach Martin van Driel

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.

Seismometer

10.1785/0120210137

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Citations (21)

High‐Frequency Receiver Functions With Event S1222a Reveal a Discontinuity in the Martian Shallow Crust

Geophysical Research Letters (2023)

Jing Shi Matthieu Plasman Brigitte Knapmeyer‐Endrun Zongbo Xu Taïchi Kawamura

Abstract The shallow crustal structure of Mars records the evolutionary history of the planet, which is crucial for understanding the early Martian geological environment. Until now, seismic constraints on the Martian crust have come primarily from the receiver functions (RFs). However, analysis of the Mars RFs did not focus on the shallow structure (1–5 km) so far due to the limitation of the signal‐to‐noise ratio at high frequencies for most events. Here, we take advantage of the S1222a and six other marsquakes, which exhibit high signal‐to‐noise ratios, to probe the shallow structure of Mars. We observe a converted S‐wave at approximately 1 s after the direct P‐wave in the high‐frequency P‐wave RFs. This suggests a discontinutity at 2‐km depth between highly fractured and more coherent crustal materials.

Discontinuity (linguistics)

10.1029/2022gl101627

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Citations (11)