Different Tectonic Styles in a Self-Consistent Mantle Convection Model

Details Different Tectonic Styles in a Self-Consistent Mantle Convection Model Different Tectonic Styles in a Self-Consistent Mantle Convection Model

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufm.u72b0027s&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #U72B-0027

Mathematics

Logic

3210 Modeling, 3220 Nonlinear Dynamics, 8149 Planetary Tectonics (5475), 8162 Rheology: Mantle

Scientific paper

By using a complex rheology in a three-dimensional numerical convection model, we are able to explain, in a self-consistent manner, some features of the surface behaviour of various terrestrial planets. With a temperature-, stress- and pressure-dependent viscosity, the plate-like behaviour of the Earth appears for small yield stresses, the episodic behaviour of Venus for intermediate values, and the stagnant lid convection of Mars and Mercury is found at high yield stresses. This last regime is, for an asymptotical value of the yield stress, identical to purely thermoviscous convection. In the episodic regime, the subduction is faster than the conductive cooling from above, leading to an intermittent behaviour. But in the Earth-like regime we have smoothly evolving extended plates. Due to the slow subduction, we have slowly moving plates. Furthermore, we find cylindrical upwellings, sheetlike downwellings and trench migration. The transitions to the different regimes as well as some diagnostical values (surface velocity, boundary-plate ratio, toroidal-poloidal ratio) are strongly influenced by the rheological parameters used. For example, we find that for a high amount of internal heating and a strongly depth-dependent thermal expansivity the stagnant lid regime exists over a wide range of yield stresses. In general we find, that the surface velocity, for example, decreases with stronger depth dependance but increases with a higher amount of internal heating or a higher Rayleigh number.

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