Geoid, topography, and convection-driven crustal deformation on Venus

Details Geoid, topography, and convection-driven crustal deformation on Venus Geoid, topography, and convection-driven crustal deformation on Venus

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992lpico.789..110s&link_type=abstract

In Lunar and Planetary Inst., Papers Presented to the International Colloquium on Venus p 110-112 (SEE N93-14288 04-91)

Computer Science

Crustal Fractures, Deformation, Geoids, Gravitational Fields, Lithosphere, Plates (Tectonics), Topography, Venus Surface, Gravitation, Magellan Spacecraft (Nasa), Planetary Geology, Satellite Altimetry, Tectonics, Venus (Planet)

Scientific paper

High-resolution Magellan images and altimetry of Venus reveal a wide range of styles and scales of surface deformation that cannot readily be explained within the classical terrestrial plate tectonic paradigm. The high correlation of long-wavelength topography and gravity and the large apparent depths of compensation suggest that Venus lacks an upper-mantle low-viscosity zone. A key difference between Earth and Venus may be the degree of coupling between the convecting mantle and the overlying lithosphere. Mantle flow should then have recognizable signatures in the relationships between surface topography, crustal deformation, and the observed gravity field.

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