Crustal Structure Constraints From the Detection of the SsPp Phase on Mars

The shallowest intracrustal layer (extending to 8 +/- 2 km depth) beneath the Mars InSight Lander site exhibits low seismic wave velocity, which is 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 six 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 similar to 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 average P-wave speed in the top crustal layer is between 2.5 and 3.2 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 low velocity of Layer 1 likely results from the presence of relatively low-density lithified sedimentary rocks and/or aqueously altered igneous rocks that also have a significant amount of porosity, possibly as much as 22%-30% by volume (assuming an aspect ratio of 0.1 for the pore space). These porosities and average P-wave speeds are compatible with our current understanding of the upper crustal stratigraphy beneath the InSight Lander site.

Automated summary

The shallowest layer beneath the Mars InSight Lander site has low seismic wave velocity due to high porosity and other lithological factors. The SsPp phase was detected on Mars for the first time, confirming the existence of an 8 km interface and a large wave speed contrast across it. The average P-wave speed in the top crustal layer was found to be between 2.5 and 3.2 km/s, providing a more precise estimate than previous studies.