Numerical models of the transition from zonal flow to dynamo action in Jupiter and Saturn

Details Numerical models of the transition from zonal flow to dynamo action in Jupiter and Saturn Numerical models of the transition from zonal flow to dynamo action in Jupiter and Saturn

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.p11b1276h&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #P11B-1276

Physics

0545 Modeling (4255), 5724 Interiors (8147), 5734 Magnetic Fields And Magnetism, 6220 Jupiter, 6275 Saturn

Scientific paper

The surface winds and magnetic fields of Jupiter and Saturn are broadly comparable. Each planet has a strong and prograde equatorial jet and weaker, alternating jets at higher latitudes. Furthermore, both planets exhibit relatively strong, dipolar magnetic fields. Saturn's magnetic field is weaker and more axisymmetric than that of Jupiter. In addition, Saturn's equatorial jet is broader and stronger than that of Jupiter. We have performed a set of numerical simulations of rotating convection and dynamo action in spherical shells. The model fluid is Boussinesq with radially varying electrical conductivity. The electrical conductivity, which is nearly constant in the deeper parts of the shell, exponentially decreases outward, starting at a chosen radius parameter. In some of the simulations a strong, mainly dipolar dynamo develops in the deeper region of high electrical conductivity. In contrast, strong zonal flow with an equatorial jet develops near the low-conductivity, free slip outer surface, and penetrates to a depth associated with the conductivity profile. The strong zonal flow is attenuated by Lorentz forces 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 their low-conductivity molecular envelopes to their liquid metal interiors.

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