Numerical models of zonal flow and dynamo action in Jupiter and Saturn (Invited)

Details Numerical models of zonal flow and dynamo action in Jupiter and Saturn (Invited) Numerical models of zonal flow and dynamo action in Jupiter and Saturn (Invited)

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p44a..09h&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #P44A-09

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[0545] Computational Geophysics / Modeling, [1510] Geomagnetism And Paleomagnetism / Dynamo: Theories And Simulations, [5704] Planetary Sciences: Fluid Planets / Atmospheres, [5724] Planetary Sciences: Fluid Planets / Interiors

Scientific paper

The surface winds of Jupiter and Saturn exhibit a similar latitudinal structure. Each planet has a strong, prograde equatorial jet and weaker, alternating higher latitude jets. Saturn's equatorial jet is broader and stronger than that of Jupiter. In addition, both planets exhibit dipolar magnetic fields. Jupiter's magnetic field is strong and slightly tilted while that of Saturn is weaker and highly axisymmetric. We have performed a set of numerical simulations of rotating convection and dynamo action in thick 3D spherical shells. The model fluid electrical conductivity, which is high and nearly constant at great depth, exponentially decreases toward the outer boundary. A strong dynamo develops in the deeper region of high electrical conductivity. Near the low-conductivity, free slip outer surface a strong equatorial zonal jet develops and penetrates to a depth associated with the conductivity profile. Strong zonal flow is attenuated at depth and does not persist in the dynamo region. The relationship between the structure of equatorial jets and the magnetic fields generated in our models imply that major differences between the surface zonal flow and magnetic fields of Jupiter and Saturn arise from the different depths of transition from the low-conductivity molecular envelopes to their liquid metal interior dynamos.

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