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Crustal Structure Constraints from the Detection of the SsPp Phase on Mars
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  • Jiaqi Li,
  • Caroline Beghein,
  • Paul Davis,
  • Mark A Wieczorek,
  • Scott M Mclennan,
  • Doyeon Kim,
  • Ved Lekić,
  • Matthew Golombek,
  • Eleonore Stutzmann,
  • Philippe Lognonné,
  • William Bruce Banerdt,
  • Martin Schimmel
Jiaqi Li
University of California, Los Angeles

Corresponding Author:[email protected]

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Caroline Beghein
University of California, Los Angeles
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Paul Davis
University of California, Los Angeles
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Mark A Wieczorek
Université
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Scott M Mclennan
State University of New York at Stony Brook
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Doyeon Kim
ETH Zürich
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Ved Lekić
University of Maryland
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Matthew Golombek
California Institute of Technology
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Eleonore Stutzmann
Université de Paris
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Philippe Lognonné
Université de Paris
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William Bruce Banerdt
California Institute of Technology
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Martin Schimmel
Geosciences Barcelona (GEO3BCN - CSIC)
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Abstract

The shallowest intracrustal layer (extending to 8 ± 2 km depth) beneath the Mars InSight Lander site exhibits low seismic wave velocity, which are likely related to a combination of high porosity and other lithological factors. The SsPp phase, an SV-to P-wave reflection on the receiver side, is naturally suited for constraining the seismic structure of this top crustal layer since its prominent signal makes it observable with a single station without the need for stacking. We have analyzed eight broadband and low-frequency seismic events recorded on Mars and made the first coherent detection of the SsPp phase on the red planet. The timing and amplitude of SsPp confirm the existence of the ~8 km interface in the crust and the large wave speed (or impedance) contrast across it. With our new constraints from the SsPp phase, we determined that the P-wave speed in the top crustal layer is between 2.5 km/s and 3.3 km/s, which is a more precise and robust estimate than the previous range of 2.0-3.5 km/s obtained by receiver function analysis. The porosity in Layer 1 is estimated to be as much as 21-31% (assuming an aspect ratio of 0.1 for the pore space), but could be lower if some pores are filled by low-density cements or other secondary 1 mineral phases. These porosities and P-wave speeds are compatible with our current understanding of the upper crustal stratigraphy beneath the InSight Lander site.