Simulation of the Effect of Topography and Crustal Thickness on the Martian Seismograms by the Coupled Method.

Details Simulation of the Effect of Topography and Crustal Thickness on the Martian Seismograms by the Coupled Method. Simulation of the Effect of Topography and Crustal Thickness on the Martian Seismograms by the Coupled Method.

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufm.p62a0367l&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #P62A-0367

Physics

3230 Numerical Solutions, 5430 Interiors (8147), 7200 Seismology

Scientific paper

Whereas the past 4 decades of Mars exploration have provided much information about the Martian surface, its interior structure remains relatively unknown. Most of our knowledge of the interior come from gravity data, which is intrinsically non-unique and thus requires many model assumptions, such as mean depths. As demonstrated for the Earth and the Moon, seismology seems the most effective tool to investigate the details of the Martian interior.
Although the subsurface structure is poorly constrained, it is clear that there are tremendous lateral variations in the crustal thickness, such as the North-South dichotomy and the Tharsis province, which may have significant consequences for the interpretation of seismic data. Recent progress in numerical methods allow us to compute seismograms in models with such variations of shallow structure.
To tackle this problem we compute synthetic seismograms using a recently developed numerical method, the coupled modal solution (MS)--spectral elements method (SEM), which is particularly well--suited to our problem. The Mars model is divided into two domains. To reduce the numerical cost of discretizing the entire model, the displacement field is computed only in the outer shell by SEM. The inner part is discretized as a development into a modal solution of the traction at the interface between the two domains. SEM combines the geometrical flexibility of finite elements and the superior accuracy of high--degree polynomial methods. In this way, a complicated geometry at the free--surface or strong lateral variations of the velocity model can be accommodated.
In this study, we compute seismograms in the spherical reference Mars model of Sohl and Spohn (1997) and compare them with those for models which include crustal thickness and topography variations to spherical degree 50. The goal is to assess the effects of shallow structure on future Martian seismic records. The idea is to improve the extraction of data in order to obtain the best possible 1-D model. Finally, some differences between Martian and terrestrial seismicity will be shown.

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