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Jupiter's and Saturn's convectively driven banded jets in the laboratory
Author(s) -
Read P. L.,
Yamazaki Y. H.,
Lewis S. R.,
Williams P. D.,
MikiYamazaki K.,
Sommeria J.,
Didelle H.,
Fincham A.
Publication year - 2004
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1029/2004gl020106
Subject(s) - saturn , enstrophy , jupiter (rocket family) , geology , physics , turbulence , kinetic energy , geophysics , convection , jet (fluid) , rossby wave , anisotropy , atmospheric sciences , vortex , astrophysics , meteorology , astronomy , planet , mechanics , vorticity , classical mechanics , space shuttle , quantum mechanics
The banded patterns of cloud and wind are among the most striking features of the atmospheres of Jupiter and Saturn, but their dynamical origin remains poorly understood. Most approaches towards understanding zonation so far (also in the terrestrial oceans) have used highly idealized models to show that it might originate from dynamical anisotropy in a shallow turbulent fluid layer due to the planetary β‐effect. Here we report the results of laboratory experiments, conducted on a 14‐m diameter turntable, which quantitatively confirm that multiple zonal jets may indeed be generated and maintained by this mechanism in the presence of deep convection and a topographic β‐effect. At the very small values of Ekman number (≤2 × 10 −5 ) and large local Reynolds numbers (≥2000, based on jet scales) achieved, the kinetic energy spectra suggest the presence of both energy‐cascading and enstrophy‐cascading inertial ranges in addition to the zonation near twice the Rhines wave number.