Other
Scientific paper
Feb 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993georl..20..265k&link_type=abstract
Geophysical Research Letters (ISSN 0094-8276), vol. 20, no. 4, p. 265-268.
Other
3
Flow Geometry, Planetary Geology, Planetary Mantles, Stratification, Tectonics, Venus Surface, Viscosity, Convection, Earth Mantle, Venus, Earth, Mantle, Viscosity, Stratification, Flow, Geometry, Surface, Motion, Convection, Velocity, Models, Lithosphere, Crust, Ishtar Terra, Topography, Timescale
Scientific paper
For a fixed heat flow, the surface flow velocity of a convecting layer is not strongly sensitive to the variation of viscosity as a function of depth. Thus, the inferred absence of a low viscosity asthenosphere on Venus can not account for the limited surface motions there. The surface velocity is dependent on the convective geometry. Cartesian geometry convection can produce large surface velocities if the high viscosity surface layer is broken in places by weak zones. On the other hand, a high viscosity surface layer may inhibit the development of large surface velocities in axisymmetric convection.
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