Scaling of time‐dependent stagnant lid convection: Application to small‐scale convection on Earth and other terrestrial planets

By V. Solomatov, Louis Moresi. 2000

328 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/abbe4359f2a265dff2bffccdb1c50091e52a5443

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In Geophysics

Citations in the corpus

The effect of rheological parameters on plate behaviour in a self-consistent model of mantle convection (2004, background): “…configurations, among them extremely strong temperature dependence of the viscosity (Torrance and Turcotte, 1971; Christensen, 1984b; Ogawa et al., 1991; Hansen and Yuen, 1993; Tackley, 1993, 1996; Moresi and Solomatov, 1995; Solomatov and Moresi, 1996, 2000; Trompert and Hansen, 1998a).”
Energetics of mantle convection and the fate of fossil heat (2003, unknown): “…zero exponent results from the assumption of a constant plate thickness over a wide range of mantle temperature, which does not seem realistic because the maximum thickness of plate is most likely limited by its own convective instability [Parsons and McKenzie, 1978; Solomatov and Moresi, 2000].”
LINKS BETWEEN LONG‐LIVED HOT SPOTS, MANTLE PLUMES, D″, AND PLATE TECTONICS (2004, background): “…1976; Weinstein and Christiansen, 1991; Stengel et al., 1982; Richter et al., 1983; Christensen, 1984a; Ogawa et al., 1991; Davaille and Jaupart, 1993; Giannandrea and Christensen, 1993; Solomatov, 1995; Moresi and Solomatov, 1995, 1998; Solomatov and Moresi, 1996, 2000; Trompert and Hansen, 1998].”
Conditions for the onset of plate tectonics on terrestrial planets and moons (2007, background): “Solomatov and Moresi (2000) show that velocity and thermal boundary layer thickness scale as v=A(κ/dmantle) (Ra/θ) β, and δ=(dmantle/B)(θ α/Raλ) respectively.”
Interior composition, structure and dynamics of the Galilean satellites (2004, background): “Convection is also more difficult to achieve if the ice rheology is nonNewtonian (Solomatov and Moresi 2000).”
Thermal and crustal evolution of Mars (2002, methodology): “Furthermore, a wet olivine rheology provides the best fit for the temperature and heat flux for smallscale (time-dependent stagnant lid) convection beneath the Earth’s oceanic lithosphere [Solomatov and Moresi, 2000].”
Sulfur's impact on core evolution and magnetic field generation on Ganymede (2005, methodology): “22n)q 2 nþ1 ð Þ nþ2 ð Þ Rai n nþ2 [Solomatov and Moresi, 2000], where n is the exponent of the deviatoric stress in the flow law (e.”
Internal and tectonic evolution of Mercury (2003, background): “22n)hð 2ðnþ1Þ=ðnþ2ÞÞRaðn=ðnþ2ÞÞ [18], where n is the exponent of the deviatoric stress in the flow law (e.”
The influence of potassium on core and geodynamo evolution (2003, background): “First, there is now a much better understanding of how to parametrize ( Solomatov & Moresi 2000 ) or numerically model (Tackley 2000; Montague & Kellogg 2000) planetary heat transfer when plate tectonics, compositional contrasts, or”