Tectonic evolution of terrestrial planets

Details Tectonic evolution of terrestrial planets Tectonic evolution of terrestrial planets

Jul 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981sci...213...62h&link_type=abstract

Science, vol. 213, July 3, 1981, p. 62-76.

Computer Science

50

Planetary Evolution, Planetary Structure, Planetary Surfaces, Tectonics, Terrestrial Planets, Earth Planetary Structure, Lithosphere, Lunar Craters, Mars Surface, Moon, Venus Surface, Planets, Terrestrial Planets, Evolution, Tectonism, Comparisons, Maps, Lithosphere, Thickness, Mantles, Earth, Moon, Mars, Mercury (Planet), Size, Chemistry, Heating, Source Medium, Rheology, Surface, Diagrams, Photographs, Venus, Terrain, Serenitatis, Mare, Interiors, Volcanism, Data, Scarps, Topography, Tharsis Montes, Valli

Scientific paper

The tectonic style of each terrestrial planet, referring to the thickness and division of its lithosphere, can be inferred from surface features and compared to models of planetary thermal history. Factors governing planetary tectonic evolution are planet diameter, chemistry, and external and internal heat sources, all of which determine how a planet generates and rids itself of heat. The earth is distinguished by its distinct, mobile plates, which are recycled into the mantle and show large-scale lateral movements, whereas the moon, Mars, and Mercury are single spherical shells, showing no evidence of destruction and renewal of the lithospheric plates over the latter 80% of their history. Their smaller volume to surface area results in a more rapid cooling, formation, and thickening of the lithosphere. Vertical tectonics, due to lithospheric loading, is controlled by the local thickness and rheology of the lithosphere. Further studies of Venus, which displays both the craterlike surface features of the one-plate planets, and the rifts and plateaus of earth, may indicate which factors are most important in controlling the tectonic evolution of terrestrial planets.

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