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All four giant planets in the Solar System feature zonal flows on the orderof 100 m/s in the cloud deck, and large-scale intrinsic magnetic fields on theorder of 1 Gauss near the surface. The vertical structure of the zonal flowsremains obscure. The end-member scenarios are shallow flows confined in theradiative atmosphere and deep flows throughout the entire planet. Theelectrical conductivity increases rapidly yet smoothly as a function of depthinside Jupiter and Saturn. Deep zonal flows will inevitably interact with themagnetic field, at depth with even modest electrical conductivity. Here weinvestigate the interaction between zonal flows and magnetic fields in thesemi-conducting region of giant planets. Employing mean-field electrodynamics,we show that the interaction will generate detectable poloidal magnetic fieldperturbations spatially correlated with the deep zonal flows. Assuming the peakamplitude of the dynamo alpha-effect to be 0.1 mm/s, deep zonal flows on theorder of 0.1 - 1 m/s in the semi-conducting region of Jupiter and Saturn wouldgenerate poloidal magnetic perturbations on the order of 0.01% - 1% of thebackground dipole field. These poloidal perturbations should be detectable withthe in-situ magnetic field measurements from the Juno mission and the CassiniGrand Finale. This implies that magnetic field measurements can be employed toconstrain the properties of deep zonal flows in the semi-conducting region ofgiant planets.

Zonal Flow Magnetic Field Interaction in the Semi-Conducting Region of Giant Planets