Deep Convection in the Interior of Major Planets: A Review

Yano, Jun–Ichi

doi:10.1071/p97079

Cited by 11 publications

(8 citation statements)

References 42 publications

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“…Note also that it is shear which disrupts the temperature perturbation. If there is a large constant zonal flowŪ, then waves with phase velocity ≈Ū can happily grow, but if the large velocityŪ varies with position, it is not possible for a single phase speed c to cancel outŪ everywhere in equation (5). Table II indicates the runs for which bursting was observed with the range of the zonal flow also displayed.…”

Section: The Bursting Phenomenonmentioning

confidence: 99%

On the necessary conditions for bursts of convection within the rapidly rotating cylindrical annulus

2012

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Zonal flows are often found in rotating convective systems. Not only are these jet-flows driven by the convection, they can also have a profound effect on the nature of the convection. In this work the cylindrical annulus geometry is exploited in order to perform nonlinear simulations seeking to produce strong zonal flows and multiple jets. The parameter regime is extended to Prandtl numbers that are not unity. Multiple jets are found to be spaced according to a Rhines scaling based on the zonal flow speed, not the convective velocity speed. Under certain conditions the nonlinear convection appears in quasi-periodic bursts. A mean field stability analysis is performed around a basic state containing both the zonal flow and the mean temperature gradient found from the nonlinear simulations.The convective growth rates are found to fluctuate with both of these mean quantities suggesting that both are necessary in order for the bursting phenomenon to occur. a) R.J.Teed@leeds.ac.uk 1

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Section: The Bursting Phenomenonmentioning

confidence: 99%

On the necessary conditions for bursts of convection within the rapidly rotating cylindrical annulus

2012

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“…For many years, progress in this area involved linear or weakly nonlinear analyses of convection and waves in spherical shells, and debate has long existed over the applicability of these results to the strongly nonlinear regime of Jupiter's interior (e.g. Yano (1998)). We refer the reader to Yano (1994Yano ( , 1998 and Busse (1994Busse ( , 2002 for reviews of this early literature.…”

Section: Deep Modelsmentioning

confidence: 99%

“…Yano (1998)). We refer the reader to Yano (1994Yano ( , 1998 and Busse (1994Busse ( , 2002 for reviews of this early literature. The past few years have seen great advances in testing the deep-convection hypothesis, as computers are now fast enough to integrate the three-dimensional fluid equations at parameter regimes and spatial resolutions of greater relevance for giant planets (though the simulated parameter regimes are still far from the Jovian regime).…”

Section: Deep Modelsmentioning

confidence: 99%

Jovian atmospheric dynamics: an update afterGalileoandCassini

2005

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The Galileo and Cassini spacecrafts have greatly enhanced the observational record of Jupiter's tropospheric dynamics, particularly through returning high spatial resolution, multi-spectral and global imaging data with episodic coverage over periods of months to years. These data, along with those from Earth-based telescopes, have revealed the stability of Jupiter's zonal jets, captured the evolution of vortices and equatorial waves, and mapped the distributions of lightning and moist convection. Because no observations of Jupiter's interior exist, a forward modelling approach has been used to relate observations at cloud level to models of shallow or deep jet structure, shallow or deep jet forcing and energy transfer between turbulence, vortices and jets. A range of observed phenomena can be reproduced in shallow models, though the Galileo probe winds and jet stability arguments hint at the presence of deep jets. Many deep models, however, fail to reproduce Jupiter-like non-zonal features (e.g. vortices). Jupiter's dynamics likely include both deep and shallow processes, requiring an integrated approach to future modelling-an important goal for the post-Galileo and Cassini era.

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“…The main theoretical difficulty that the Busse model has encountered is the explanation of the multiple jet structure of Jupiter's zonal flow [ Yano , 1998]. Three‐dimensional simulations [ Christensen , 2001] at moderately small Ekman number do not reproduce the complex array of prograde and retrograde zonal jets in the jovian atmosphere.…”

Section: Introductionmentioning

confidence: 99%

Multiple jets and zonal flow on Jupiter

Jones

Rotvig

Abdulrahman

2003

Geophysical Research Letters

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[1] We investigate the occurrence of multiple jet zonal flows in the 2D rotating annulus model, extended to include the possibility of boundary friction. We consider Rayleigh numbers up to 10 times critical. Without boundary friction the majority of our solutions are single-jet zonal flows, but when boundary friction is present, persistent multiple jet solutions are found much more easily. Compared to the stress-free case, the number of jets increases, though the strength of the zonal flow decreases. The dependence of these features on Ekman and Rayleigh number is discussed, suggesting that at values well beyond the reach of present 3D simulations, solutions resembling the observed jovian zonal flow may exist. The boundary condition at the metallic/insulating hydrogen interface will be an important part of any explanation of the occurrence of multiple jets on the planet Jupiter.

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Deep Convection in the Interior of Major Planets: A Review

Cited by 11 publications

References 42 publications

On the necessary conditions for bursts of convection within the rapidly rotating cylindrical annulus

On the necessary conditions for bursts of convection within the rapidly rotating cylindrical annulus

Jovian atmospheric dynamics: an update afterGalileoandCassini

Multiple jets and zonal flow on Jupiter

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