Effects of compressibility on driving zonal flow in gas giants

  title={Effects of compressibility on driving zonal flow in gas giants},
  author={Thomas Gastine and Johannes Wicht},
Mechanisms for Limiting the Depth of Zonal Winds in the Gas Giant Planets
Gravity signatures observed by the Juno and Cassini missions that are associated with the strong zonal winds in Jupiter’s and Saturn’s outer envelopes suggest that these flows extend for several
Generation of shear flows and vortices in rotating anelastic convection
We consider the effect of stratification on systematic, large-scale flows generated in anelastic convection. We present results from three-dimensional numerical simulations of convection in a
Effect of shear and magnetic field on the heat-transfer efficiency of convection in rotating spherical shells
We study rotating thermal convection in spherical shells. We base our analysis on a set of about 450 direct numerical simulations of the (magneto)hydrodynamic equations under the Boussinesq
Penetrative Convection in Partly Stratified Rapidly Rotating Spherical Shells
Celestial objects host interfaces between convective and stable stratified interior regions. The interaction between both, e.g., the transfer of heat, mass, or angular momentum depends on whether and
Onset of rotating and non-rotating convection in compressible and anelastic ideal gases
A linear stability analysis for compressible convection in a plane layer geometry both with and without the influence of rotation is presented. For the rotating cases we employ the tilted -plane


The effects of vigorous mixing in a convective model of zonal flow on the ice giants
Zonal flow driven by strongly supercritical convection in rotating spherical shells
  • U. Christensen
  • Physics, Environmental Science
    Journal of Fluid Mechanics
  • 2002
Thermal convection in a rotating spherical shell with free-slip boundaries can excite a dominant mean zonal flow in the form of differentially rotating cylinders concentric to the principal rotation
Compressible Convection in a Rotating Spherical Shell
Giant cell stellar convection is modeled by solving the fluid equations for a compressible, rotating, spherical, fluid shell. A large part of the motivation is to understand the maintenance of the
Scaling properties of convection-driven dynamos in rotating spherical shells and application to planetary magnetic fields
SUMMARY We study numerically an extensive set of dynamo models in rotating spherical shells, varying all relevant control parameters by at least two orders of magnitude. Convection is driven by a
Convection driven zonal flows and vortices in the major planets.
The dynamical properties of convection in rotating cylindrical annuli and spherical shells are reviewed and the generation of zonal mean flows is discussed in some detail and examples of recent numerical computations are presented.
Scaling laws for convection and jet speeds in the giant planets
Linear theory of compressible convection in rapidly rotating spherical shells, using the anelastic approximation
The onset of compressible convection in rapidly rotating spherical shells is studied in the anelastic approximation. An asymptotic theory valid at low Ekman number is developed and compared with
Anelastic Magnetohydrodynamic Equations for Modeling Solar and Stellar Convection Zones
The anelastic approximation has strong advantages for numerical simulations of stellar and solar convection zones. The chief and generally known one is that it suppresses acoustic modes, permitting
Differential rotation in giant planets maintained by density-stratified turbulent convection
The zonal winds on the surfaces of giant planets vary with latitude. Jupiter and Saturn, for example, have several bands of alternating eastward (prograde) and westward (retrograde) jets relative to