2D Studies of Various Approximations Used for Modeling Convection in Giant Planets

Evonuk, M.; Glatzmaier, Gary A.

doi:10.1080/03091920410001696126

Cited by 26 publications

(24 citation statements)

References 23 publications

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“…Although density increases by several orders of magnitude with depth below Jupiter's troposphere, our model neglects fluid compression (Boussinesq approximation). This is clearly a drastic simplification since fluid compressibility effects are certainly important to the dynamics of convection in the Gas Giants (Evonuk and Glatzmaier, 2004;Glatzmaier, 2005a). While the Boussinesq model is inadequate to describe convection within the Gas Giants, it can provide insight into the large-scale dynamics (Yano et al, 2003(Yano et al, , 2005.…”

Section: Parametermentioning

confidence: 98%

Turbulent convection in rapidly rotating spherical shells: A model for equatorial and high latitude jets on Jupiter and Saturn

Heimpel

Aurnou

2007

Icarus

101

114

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Section: Parametermentioning

confidence: 98%

Turbulent convection in rapidly rotating spherical shells: A model for equatorial and high latitude jets on Jupiter and Saturn

Heimpel

Aurnou

2007

Icarus

101

114

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“…The working fluid in our model is Boussinesq, which means that it is incompressible except for the buoyancy effects of temperature perturbations (Tritton 1987). While the fluid in the interiors of the gas giants is compressible (Evonuk & Glatzmaier 2004; Guillot et al 2004), the Boussinesq approximation allows us to model turbulent convective flow (rms Reynolds number Re ∼ 2 × 10 4 ) under quasi‐geostrophic conditions (rms Rossby number Ro ∼ 0.01). These high Re , low Ro conditions are likely characteristic of the adiabatically mixed molecular envelopes of the giant planets (Ingersoll & Pollard 1982; Liao et al 2005).…”

Section: Numerical Modelmentioning

confidence: 99%

“…The working fluid in our model is Boussinesq, which means that it is incompressible except for the buoyancy effects of temperature perturbations (Tritton 1987). While the fluid in the interiors of the gas giants is compressible (Evonuk & Glatzmaier 2004;Guillot (Ingersoll & Pollard 1982;Liao et al 2005). Thus, with Boussinesq fluid, we can simulate the first-order convective mixing processes that occur in the planetary interiors and, thereby, approximate their large-scale dynamics.…”

Section: N U M E R I C a L M O D E Lmentioning

confidence: 99%

Convective heat transfer and the pattern of thermal emission on the gas giants

Aurnou¹,

Heimpel

Allen

et al. 2008

Geophysical Journal International

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S U M M A R YJupiter and Saturn emit nearly twice the thermal energy they receive from the Sun. Although insolation decreases toward the poles, the large-scale outward heat flux is nearly uniform, with smaller-scale latitudinal undulations that correlate with the zonal jet streams. Here we present numerical models of rapidly rotating, turbulent 3-D convection in geometrically thin, uniformly forced layers of Boussinesq fluid that approximate the deep convection zones of Jupiter and Saturn. In previous studies we have demonstrated that such models generate zonal flows comparable to those observed on the gas giants. By analysing the simulated patterns of convective heat transfer, we show here that deep convection in the gas giants can explain the anomalously uniform large-scale thermal emissions as well as the jet-scale variations. In particular, we find that convective heat transfer by quasi-geostrophic thermal plumes in relatively thin spherical shell geometry generates an outward heat flow pattern with a broad equatorial minimum and peaks at the poles. The results suggest an alternative to the hypothesis that insolation controls the large-scale patterns of heat flux and zonal flow on the gas giants. Instead, we propose that the large-scale thermal and zonal flow fields originate deep within the planets' molecular envelopes.

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“…The attenuation of zonal flows with depth can result from the effects of increasing density within the planet (Evonuk and Glatzmaier, 2004). In addition, electromagnetic induction effects can become important in regions where the electrical conductivity is nonzero (Kirk and Stevenson, 1987).…”

Section: Introductionmentioning

confidence: 99%

The effects of vigorous mixing in a convective model of zonal flow on the ice giants

Aurnou

Heimpel

Wicht

2007

Icarus

125

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2D Studies of Various Approximations Used for Modeling Convection in Giant Planets

Cited by 26 publications

References 23 publications

Turbulent convection in rapidly rotating spherical shells: A model for equatorial and high latitude jets on Jupiter and Saturn

Turbulent convection in rapidly rotating spherical shells: A model for equatorial and high latitude jets on Jupiter and Saturn

Convective heat transfer and the pattern of thermal emission on the gas giants

The effects of vigorous mixing in a convective model of zonal flow on the ice giants

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