Seismology in the solar system

Stähler, Simon C.; Knapmeyer, Martin

doi:10.1016/bs.agph.2022.07.002

Cited by 5 publications

(2 citation statements)

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“…While seismic observations have greatly improved our understanding of the interiors of the Earth, the Moon, and Mars, currently, the seismic activity for other planetary bodies such as Mercury, Venus, or icy satellites can only be indirectly estimated with large uncertainties. A comprehensive review of the current state of knowledge of planetary seismology and directions for future seismic investigations of planetary bodies is given in Chapter 2 (Stähler and Knapmeyer, 2022).…”

Section: Seismogenic Layer Thickness and The Present-day Seismicitymentioning

confidence: 99%

“…We highlight how our knowledge of the thermal history and present-day state of the interior has improved with the recent InSight results and discuss what future models need to address in order to further constrain the thermal evolution of Mars. Current geodynamic modeling will also help to identify scientifically interesting landing sites for a future seismic network that may become available after 2030 (Stähler and Knapmeyer, 2022).…”

Section: Introductionmentioning

confidence: 99%

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Interior Dynamics and Thermal Evolution of Mars -- a Geodynamic Perspective

Plesa¹,

Wieczorek²,

Knapmeyer³

et al. 2022

Preprint

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Over the past decades, global geodynamical models have been used to investigate the thermal evolution of terrestrial planets. With the increase of computational power and improvement of numerical techniques, these models have become more complex, and simulations are now able to use a high resolution 3D spherical shell geometry and to account for strongly varying viscosity, as appropriate for mantle materials. In this study we review global 3D geodynamic models that have been used to study the thermal evolution and interior dynamics of Mars. We discuss how these models can be combined with local and global observations to constrain the planet's thermal history. In particular, we use the recent InSight estimates of the crustal thickness, upper mantle structure, and core size to show how these constraints can be combined with 3D geodynamic models to improve our understanding of the interior dynamics, present-day thermal state and temperature variations in the interior of Mars. Our results show that the crustal thickness variations control the surface heat flow and the elastic thickness pattern, as well as the location of melting zones in the present-day martian mantle. The lithospheric temperature and the seismic velocities pattern in the shallow mantle reflect the crustal thickness pattern. The large size of the martian core leads to a smaller scale convection pattern in the mantle than previously suggested. Strong mantle plumes that produce melt up to recent times become focused in Tharsis and Elysium, while weaker plumes are distributed throughout the mantle. The thickness of the seismogenic layer, where seismic events can occur, can be used to discriminate between geodynamic models, if the source depth and location of seismic events is known. Furthermore model predictions of present-day martian seismicity can be compared to the values measured by InSight. Future models need to consider recent estimates from the presentday elastic lithosphere thickness at the north pole of Mars, the effects of lateral variations of seismic velocities on waves propagation through the mantle and lithosphere, and to test the spatial distribution of seismicity by comparing model predictions to observations.

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Section: Seismogenic Layer Thickness and The Present-day Seismicitymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%