Numerical Experiments of Convective Heat Transfer in a Fluid with Strongly Temperature Dependent Viscosity: Implications for Thermal Planetary Evolution

Details Numerical Experiments of Convective Heat Transfer in a Fluid with Strongly Temperature Dependent Viscosity: Implications for Thermal Planetary Evolution Numerical Experiments of Convective Heat Transfer in a Fluid with Strongly Temperature Dependent Viscosity: Implications for Thermal Planetary Evolution

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996lpi....27..451g&link_type=abstract

Lunar and Planetary Science, volume 27, page 451

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Boundary Layer, Convection, Evolution: Planetary Thermal, Stagnant Lid Regime, Variable Viscosity

Scientific paper

Predictions of planetary thermal evolution depend on understanding the rate of heat transfer in a convecting fluid with a strongly temperature dependent viscosity. At high Rayleigh number, the heat flux for a constant viscosity fluid cooled from above is proportional tom 1/3 DT 4/3 where m is the viscosity and DT is the temperature difference across the thermal boundary layer. This relationship has frequently been applied to planetary thermal evolution by calculating the viscosity at the temperature of the well-mixed interior. However, according to scaling analysis, a conductive lid regime appears above a viscosity variation of 104-105. This regime has been observed both in laboratory experiments and in numerical models. In this regime, laboratory experiments indicate that the appropriate DT is the temperature difference across only the convecting part of the thermal boundary layer with Tm the temperature in the well mixed layer. Numerical studies for a fluid heated from within with large viscosity variations are presented. For a steady state volumetrically heated fluid cooled from above, as in the transient cooling laboratory experiments, the structure consists of a nearly isotherm well-mixed layer, an unstable boundary layer, and a stagnant conductive lid. New estimates of DTv are proposed and implications for planetary evolution are discussed.

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