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Seismic Noise Autocorrelations on Mars
  • +14
  • Martin Schimmel,
  • Eleonore Stutzmann,
  • Philippe H. Lognonne,
  • Nicolas Compaire,
  • Paul McEwan Davis,
  • Mélanie Drilleau,
  • Raphael F. Garcia,
  • Doyeon Kim,
  • Brigitte Knapmeyer-Endrun,
  • Vedran Lekic,
  • Ludovic Margerin,
  • Mark Paul Panning,
  • Nicholas Charles Schmerr,
  • John-Robert Scholz,
  • Aymeric Spiga,
  • Benoit Tauzin,
  • William Bruce Banerdt
Martin Schimmel
Geosciences Barcelona

Corresponding Author:[email protected]

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Eleonore Stutzmann
Institut De Physique Du Globe De Paris
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Philippe H. Lognonne
Institut De Physique Du Globe De Paris
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Nicolas Compaire
Institut Supérieur de l'Aéronautique et de l'Espace, ISAE-SUPAERO
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Paul McEwan Davis
University of California Los Angeles
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Mélanie Drilleau
Institut de Physique du Globe de Paris
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Raphael F. Garcia
Institut Supérieur de l'Aéronautique et de l'Espace, ISAE-SUPAERO
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Doyeon Kim
University of Maryland, College Park
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Brigitte Knapmeyer-Endrun
Bensberg Observatory, University of Cologne
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Vedran Lekic
University of Maryland, College Park
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Ludovic Margerin
Paul Sabatier University - Toulouse III
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Mark Paul Panning
Jet Propulsion Laboratory, California Institute of Technology
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Nicholas Charles Schmerr
University of Maryland, College Park
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John-Robert Scholz
Max-Planck-Institut für Sonnensystemforschung
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Aymeric Spiga
Sorbonne Université (Faculté des Sciences)
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Benoit Tauzin
Universite de Lyon
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William Bruce Banerdt
Jet Propulsion Lab (NASA)
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Abstract

Mars is the first extraterrestrial planet with seismometers (SEIS) deployed directly on its surface in the framework of the InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) mission. The lack of strong Marsquakes, however, strengthens the need of seismic noise studies to additionally constrain the Martian structure. Seismic noise autocorrelations of single-station recordings permit the determination of the zero-offset reflection response underneath SEIS. We present a new autocorrelation study which employs state-of-the-art approaches to determine a robust reflection response by avoiding bias from aseismic signals which are recorded together with seismic waves due to unfavorable deployment and environmental conditions. Data selection and segmentation is performed in a data-adaptive manner which takes the data root-mean-square amplitude variability into account. We further use the amplitude-unbiased phase cross-correlation and work in the 1.2-8.9 Hz frequency band. The main target are crustal scale reflections, their robustness and convergence. The strongest signal appears at 10.6 s, and, if interpreted as P-wave reflection, would correspond to a discontinuity at about 24 km depth. This signal is a likely candidate for a reflection from the base of the Martian crust due to its strength, polarity, and stability. Additionally we identify, among the stable signals, a signal at about 6.85 s that can be interpreted as a P-wave reflection from the mid-crust at about 9.5 km depth.