Ref: POSTER-2021-0018

Seismic Velocities Distribution in a 3D Mantle: Implications for InSight Measurements

Plesa, Ana-Catalina ; Bozdag, Ebru ; Rivoldini, Attilio ; Knapmeyer, Martin ; McLennan, Scott ; Padovan, Sebastiano ; Tosi, Nicola ; Breuer, Doris ; Peter, Daniel ; Staehler, Simon ; Wieczorek, Mark ; van Driel, Martin ; Khan, Amir ; Spohn, Tilman ; Ciardelli, Caio ; King, Scott

Poster presented at AGU Fall Meeting 2020, Virtual on 2020-12-15

Abstract: The InSight mission [1] landed in November 2018 in the Elysium Planitia region [2] bringing the first geophysical observatory to Mars. Since February 2019 the seismometer SEIS [3] has continuously recorded Mars' seismic activity, and a list of the seismic events is available in the InSight Marsquake Service catalog [4]. In this study, we predict present-day seismic velocities in the Martian interior using the 3D thermal evolution models of [5] (Fig. 1a, b). We then use the 3D velocity distributions to interpret seismic observations recorded by InSight. Our analysis is focused on the two high quality events S0173a and S0235b. Both have distinguishable P- and S-wave arrivals and are thought to originate in Cerberus Fossae [6], a potentially active fault system [7]. Our results show that models with a crust containing more than half of the total amount of heat producing elements (HPE) of the bulk of Mars lead to large variations of the seismic velocities in the lithosphere. A seismic velocity pattern similar to the crustal thickness structure is observed at depths larger than 400 km for cases with cold and thick lithospheres. Models, with less than 20% of the total HPE in the crust have thinner lithospheres with shallower but more prominent low velocity zones. The latter, lead to shadow zones that are incompatible with the observed P- and S-wave arrivals of seismic events occurring in Cerberus Fossae, in 20° - 40° epicentral distance (Fig. 1c). We therefore expect that future high-quality seismic events have the potential to further constrain the amount of HPE in the Martian crust. Future work will combine the seismic velocities distribution calculated in this study with modeling of seismic wave propagation [8, 9] (Fig. 1d). This will help to assess the effects of a 3D thermal structure on the waveforms and provide a powerful framework for the interpretation of InSight’s seismic data.

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Royal Observatory of Belgium > Reference Systems & Planetology
Conference Contributions & Seminars > Posters

 Record created 2021-02-01, last modified 2021-02-01