Computer Science
Scientific paper
Aug 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984em%26p...31...49b&link_type=abstract
Earth, Moon, and Planets (ISSN 0167-9295), vol. 31, Aug. 1984, p. 49-61.
Computer Science
6
Geomorphology, Mars Surface, Planetary Geology, Ridges, Erosion, Geodynamics, Lithosphere, Lunar Surface, Mars Volcanoes
Scientific paper
The morphology of Martian ridges between 30 deg N and 30 deg S is characterized and illustrated with drawings and Viking Orbiter photographs, and its implications for the ridge formation mechanism are analyzed. Consideration is given to the volcanic formation of similar ridges in lunar maria, the spatial relationship between the Martian ridge fields and the presence of a hydrolithosphere, structural considerations, geodynamic processes, and erosion. The ridges are shown to extend to several hundred km in length, forming parallel groups up to thousands of km long, and to comprise elongated arcuated bulges usually 50-100 m high (maxima 300-400 m) and up to 10 km wide and continuous or stepped sometimes narrow or crested superimposed ridges. While some of the low-latitude Martian ridges are seen as resulting from extrusion of hydrolithospheric material, most are attributed to the compression of a thin crust lying unconformably over a substratum of water-saturated porous sediments, a process having similar dynamics but a different origin than that active on the moon.
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