Other
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmgp22b..01j&link_type=abstract
American Geophysical Union, Fall Meeting 2001, abstract #GP22B-01
Other
1507 Core Processes (8115), 1510 Dynamo Theories, 1535 Reversals (Process, Timescale, Magnetostratigraphy), 7536 Solar Activity Cycle (2162), 7544 Stellar Interiors And Dynamo Theory
Scientific paper
There has been significant progress in the development of numerical geodynamo models over the last eight years. Advances in computer technology have made it possible to perform three-dimensional simulations, with thermal or compositional convection as the driving mechanism. These numerical simulations give reasonable results for the morphology and strength of the field at the core-mantle boundary, and the models are also capable of giving reversals and excursions which can be compared with paleomagnetic observations. Some useful constraints are obtained by considering the entropy balance and the ohmic dissipation. However, recent studies of plane layer dynamos suggest that the current generation of dynamo models have not yet reached the correct dynamical regime. A rather severe test of how well we understand the geodynamo comes when we try to apply the theory to the magnetic fields of stars and other planets. It becomes clear that not all dynamos are in the same dynamical regime. Some, like the Earth, are in magnetostrophic balance; others like the Sun, are not. Some are in a strong field regime with Elsasser number of order one, others (including some planetary dynamos) are not. Even within late type stars, the rotation rate strongly affects the dynamical regime that the dynamo operates in. The prospects for classifying the various type of convection driven dynamo, by elucidating the possible dynamical regimes, will be reviewed.
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