Modeling Deep Convective Zonal Flows on the Giant Planets

Details Modeling Deep Convective Zonal Flows on the Giant Planets Modeling Deep Convective Zonal Flows on the Giant Planets

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p52a..02a&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #P52A-02

Physics

1507 Core Processes (1213, 8115), 3314 Convective Processes, 3367 Theoretical Modeling, 5704 Atmospheres (0343, 1060), 5724 Interiors (8147)

Scientific paper

The large-scale zonal winds observed on the Giant Planets most likely describe two distinct fluid dynamical regimes. On Jupiter and Saturn, strong prograde equatorial jets are flanked at higher latitudes by alternating, smaller-scale bands. In contrast, the surface zonal winds of Uranus and Neptune are dominated by retrograde flow in the equatorial region, flanked by one large prograde jet in each hemisphere. Here we will show that numerical simulations of Boussinesq rotating convection in a spherical shell can generate zonal flows like those observed on all four Giants Planets. In simulations where the Coriolis forces dominate the buoyancy forces, cylindrical Reynolds stresses drive prograde equatorial jets, similar to those observed on Jupiter and Saturn. In addition, small wavelength Rhines-scale jets form at middle and higher latitudes. However, in cases where the buoyancy forces are comparable to or exceed the Coriolis forces, the cylindrical symmetry of the flow weakens and isotropic turbulence homogenizes the fluid layer's angular momentum. This leads to the reversal of the equatorial jet direction, while the high latitude zonal flow in each hemisphere takes the form of a single, strong prograde jet. Thus, rotationally-dominated models produce surface zonal flows similar to those observed on Jupiter and Saturn, whereas buoyancy-dominated models produce zonal flows similar to those observed of Uranus and Neptune.

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