Laboratory simulation of Jupiter's Great Red Spot

@article{Sommeria1988LaboratorySO,
  title={Laboratory simulation of Jupiter's Great Red Spot},
  author={J. Sommeria and S. Meyers and H. Swinney},
  journal={Nature},
  year={1988},
  volume={331},
  pages={689-693}
}
Isolated large stable vortices have long been observed in the jovian atmosphere and more recently on Saturn. The existence of such stable vortices in strongly turbulent planetary atmospheres is a challenging problem in fluid mechanics. In a numerical simulation Marcus1 found that a single stable vortex developed for a wide variety of conditions in a turbulent shear flow in a rotating annulus. To test this we conducted an experiment on a rotating annulus filled with fluid pumped in the radial… Expand
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1
2
3
4
5
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References

SHOWING 1-10 OF 17 REFERENCES
Numerical simulation of Jupiter's Great Red Spot
Jupiter's Great Red Spot is viewed as a vortex that arises naturally from the equations of motion of the jovian atmosphere. Here I solve numerically the equations governing fluid motion in a model ofExpand
Rossby autosoliton and stationary model of the jovian Great Red Spot
A theory proposed about 10 years ago claimed that the jovian Great Red Spot (GRS) was a solitary wave vortex (Rossby soliton) kept stationary by counter–streaming zonal winds. We have attempted toExpand
Numerical Model of Long-Lived Jovian Vortices
A nonlinear numerical model of long-lived Jovian vortices has been constructed. We assume that the measured zonal velocity profile ubar(y) extends into the adiabatic interior, but that the eddies andExpand
Quasi-geostrophic turbulence in a rotating homogeneous fluid
Abstract Quasi-two-dimensional turbulence is generated in a rotating cylinder by an homogeneous distribution of bottom sources and sinks which oscillate in time. Typical Reynolds numbers reach 2000Expand
An isolated baroclinic eddy as a laboratory analogue of the Great Red Spot on Jupiter
We have recently presented evidence1 supporting the hypothesis2 that the long-lived large oval atmospheric eddies on Jupiter and Saturn, including Jupiter's anticyclonic Great Red Spot (GRS) andExpand
A shear-flow instability in a circular geometry
A circular shear zone is created in a thin layer of fluid. The Kelvin-Helmholtz instability induces regular, steady patterns of m vortices. The experimental conditions are such that neither theExpand
Oscillations and velocity structure of a long‐lived cyclonic spot
Dark brown cyclonic spots ('barges') at 14°N were studied by using Voyager 1 and 2 images of Jupiter. Movie sequences were made to study the spots' behavior over intervals of 50 days and longer.Expand
Global dynamics and thermal structure of Jupiter's atmosphere
Abstract Jupiter has an intrinsic luminosity, and most, if not all of its interior is believed to be fluid and of low viscosity. These imply a regime of thermally driven turbulent convection. TheExpand
Detached shear layers in a rotating fluid
The occurrence of detached shear layers should, according to straightforward theoretical arguments, often characterize hydrodynamical motions in a rapidly rotating fluid. Such layers have beenExpand
Jovian and comparative atmospheric modeling
Publisher Summary This chapter presents the development of a Jovian meteorology and assesses its impact on the evolution of comparative meteorology. The Jovian vortex theories conflict with theExpand
...
1
2
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