3D simulations of double-diffusive convection in the interior of giant planets

Details 3D simulations of double-diffusive convection in the interior of giant planets 3D simulations of double-diffusive convection in the interior of giant planets

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p21c1686g&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #P21C-1686

Physics

[5724] Planetary Sciences: Fluid Planets / Interiors, [5749] Planetary Sciences: Fluid Planets / Origin And Evolution, [6220] Planetary Sciences: Solar System Objects / Jupiter

Scientific paper

When a thermally convective system is stabilized by strong compositional gradients, convection takes a different form called double-diffusive convection. This is thought to occur in the interior of giant planets as core-erosion proceeds, for example. The transport properties of double-diffusive convection are quite different from those of standard convection, as observed for example in the polar region of the Earth's oceans. However, little to date is known about them in the parameter regime relevant for giant planets. The problem of parameterizing them is crucial, however, to a better understanding of the interior structure of the solar system planets, as well as the evolution (and in particular cooling rate) of extrasolar planets. We present the results of 3D simulations of double-diffusive convection in a parameter regime close to that relevant for the interior of giant planets. We find that two states are possible: a homogeneous state, and a layered state. We provide estimates for the mixing rates of heat and composition in the homogeneous state, as well as criteria for the formation of thermo-compositional layers. Finally, we provide preliminary estimates for the mixing rates in the layered phase of double-diffusive convection, and discuss the implication of our findings for the solar system planets as well as exoplanets.

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