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The evolution of the interior of stagnant-lid bodies is comparatively easierto model and predict with respect to the Earth's due to the absence of thelarge uncertainties associated with the physics of plate tectonics, its onsettime and efficiency over the planet's history. Yet, the observational recordfor these bodies is both scarcer and sparser with respect to the Earth's. It isrestricted to a limited number of samples and a variety of remote-sensingmeasurements of billions-of-years-old surfaces whose actual age is difficult todetermine precisely. Combining these observations into a coherent picture ofthe thermal and convective evolution of the planetary interior represents thusa major challenge. In this chapter, we review key processes and (mostlygeophysical) observational constraints that can be used to infer the globalcharacteristics of mantle convection and thermal evolution of the interior ofMercury, the Moon and Mars, the three major terrestrial bodies where a stagnantlid has likely been present throughout most of their history.

Mercury, Moon, Mars: Surface expressions of mantle convection and interior evolution of stagnant-lid bodies