Other
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmdi51a..02o&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #DI51A-02
Other
5734 Magnetic Fields And Magnetism, 1015 Composition Of The Core, 1507 Core Processes (1213, 8115), 1510 Dynamo: Theories And Simulations, 1521 Paleointensity
Scientific paper
Planets and satellites in the solar system with active dynamos exhibit diverse magnetic field morphologies and dipole moments that span nearly eight orders of magnitude. In spite of major differences in planetary structure, composition, and history, most of the active dynamos are thought to involve thermal and/or compositional convection in electrically-conducting fluids in the planet interiors. Numerical dynamos can now model planetary magnetism in terms of the fundamental core processes, however, these models are far removed in parameter space from most planets. In terms of the dimensionless parameters that control convective dynamos, the Rayleigh number is too small, and the Ekman and magnetic Prandtl numbers are too large in the models. Scaling laws offer a means to extrapolate numerical results to planetary conditions and there are now scaling laws for the time-averaged magnetic dipole moment, magnetic energy, dissipation, and fluid velocity derived from convection-driven numerical dynamo models spanning the accessible parameter space and a variety of boundary conditions. Several planetary dynamos are broadly consistent with these scalings, provided that turbulent (ie, magnetic Prandtl number~eq1) conditions apply. Because most dynamo models were formulated for the Earth, there is urgent need for additional modeling to understand the role of differences in fluid shell depth, smaller Ekman and magnetic Prandtl numbers, alternative forms of boundary heterogeneity, fluid compressibility, turbulence parameterizations, variable rotation, precession, and other less- studied effects.
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