EGU23-12524, updated on 20 Oct 2023
EGU General Assembly 2023
© Author(s) 2023. This work is distributed under
the Creative Commons Attribution 4.0 License.

Crustal structure observed by the InSight mission to Mars

Doyeon Kim1, Simon Stähler1, Christian Boehm1, Ved Lekic2, Domenico Giardini1, Savas Ceylan1, John Clinton3, Paul Davis4, Cecilia Duran1, Amir Khan1, Brigitte Knapmeyer-Endrun5, Ross Maguire6, Mark Panning7, Ana-Catalina Plesa8, Nicholas Schmerr2, Mark Wieczorek9, Géraldine Zenhäusern1, Philippe Lognonné10, and William Banerdt7
Doyeon Kim et al.
  • 1Institute of Geophysics, ETH Zurich, Zurich, Switzerland (
  • 2Department of Geology, University of Maryland, College Park, USA
  • 3Swiss Seismological Service, ETH Zürich, Zürich, Switzerland
  • 4Department of Earth, Planetary and Space Sciences, University of California, Los Angeles, USA
  • 5Bensberg Observatory, University of Cologne, Bergiscch Gladbach, Germany
  • 6Department of Geology, University of Illinois Urbana-Champaign, Champaign, USA
  • 7Jet Propulsion Laboratory, California Institute of Technology, Pasadena, USA
  • 8Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany
  • 9Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Nice, France
  • 10Université Paris Cité, Institut de physique du globe de Paris, CNRS, Paris, France

After more than 4 Earth years of operation on the martian surface monitoring the planet’s ground vibrations, the InSight’s seismometer is now retired. Throughout the mission, analyses of body waves from marsquakes and impacts have led to important discoveries about the martian interior structure of the crust, mantle, and core. Recent detection of surface waves, together with gravimetric modeling enabled the characterization of crustal structure variations away from the InSight landing site and showed that average crustal velocity and density structure is similar between the northern lowlands and the southern highlands. Especially for the observed overtones and multi-orbiting surface waves in S1222a, we find the depth sensitivity expands down to the uppermost mantle close to 90 km. Furthermore, our 3D wavefield simulations show significantly broadened volumetric sensitivity of the higher-orbit surface waves. These new constraints obtained by our surface wave analyses provide an important opportunity not only to refine and verify our previous radially symmetric models of the planet’s interior structure but also to improve understanding of seismo-tectonic environments on Mars. Here, we summarize our recent effort in the analyses of surface waves on Mars and discuss the inferred crustal property and its global implications.

How to cite: Kim, D., Stähler, S., Boehm, C., Lekic, V., Giardini, D., Ceylan, S., Clinton, J., Davis, P., Duran, C., Khan, A., Knapmeyer-Endrun, B., Maguire, R., Panning, M., Plesa, A.-C., Schmerr, N., Wieczorek, M., Zenhäusern, G., Lognonné, P., and Banerdt, W.: Crustal structure observed by the InSight mission to Mars, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-12524,, 2023.