Abstract
The Martian ridges present a larger diversity of forms and patterns than the lunar ridges. The main explanation is the following: unlike the lunar-ridges, the low latitude ridges on Mars are not related to volcanism, but are in close connection with hydro-lithosphere. Their morphologic similarities with the lunar ridges are probably due to a similar dynamic origin — i.e., compression of a thin crust lying unconformably over the substratum (on Mars, porous sediments saturated with water). It is suggested that in some areas Martian ridges are mainly of extrusive origin (material extruded from the hydro-lithosphere), unlike the lunar ridges.
Résumé
Les rides de Mars présentent une plus grande diversité de formes et de dispositions que les rides de la Lune. Alors que les rides de la Lune sont liées au volcanisme des mers, les rides de Mars sont en étroite relation avec l'existence d'une hydrolithosphère, et là résidue sans doute la cause des différences observées. Les analogies morphologiques avec les rides de la Lune s'expliquent le mieux par une origine dynamique comparable, à savoir la compression d'une croûte suffisamment mince reposant en discordance sur un substratum constitué sur Mars par des sédiments poreux gorgés d'eau. Il est suggéré que dans certaines régions de Mars les rides sont surtout des formes extrusives, constituées par du matérial originaire de l'hydrolithosphére.
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Battistini, R. Morphology and origin of ridges in low-latitude areas of Mars. Earth Moon Planet 31, 49–61 (1984). https://doi.org/10.1007/BF00058111
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DOI: https://doi.org/10.1007/BF00058111