Mercury, Moon, Mars: Surface expressions of mantle convection and interior evolution of stagnant-lid bodies
arXiv:1912.05207
Abstract
The evolution of the interior of stagnant-lid bodies is comparatively easier to model and predict with respect to the Earth's due to the absence of the large uncertainties associated with the physics of plate tectonics, its onset time and efficiency over the planet's history. Yet, the observational record for these bodies is both scarcer and sparser with respect to the Earth's. It is restricted to a limited number of samples and a variety of remote-sensing measurements of billions-of-years-old surfaces whose actual age is difficult to determine precisely. Combining these observations into a coherent picture of the thermal and convective evolution of the planetary interior represents thus a major challenge. In this chapter, we review key processes and (mostly geophysical) observational constraints that can be used to infer the global characteristics of mantle convection and thermal evolution of the interior of Mercury, the Moon and Mars, the three major terrestrial bodies where a stagnant lid has likely been present throughout most of their history.
arXiv comment45 pages, 6 figures, Accepted chapter to appear in "Mantle Convection and Surface Expressions", H. Marquardt, M. Ballmer, S. Cottar, K. Jasper (eds.), AGU Monograph Series
References in corpus (6)
- The timeline of the Lunar bombardment - revisited
- The Chemical Composition of Mercury
- Coupling SPH and thermochemical models of planets: Methodology and example of a Mars-sized body
- Rayleigh-Bénard convection in a creeping solid with melting and freezing at either or both its horizontal boundaries
- Dynamical effects of multiple impacts: Large impacts on a Mars-like planet
- "Isocrater" impacts: Conditions and mantle dynamical responses for different impactor types