Physics
Scientific paper
May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmgp33a..04w&link_type=abstract
American Geophysical Union, Spring Meeting 2004, abstract #GP33A-04
Physics
6293 Uranus
Scientific paper
We present numerical simulations of a self-consistent dynamo model in a rotating spherical shell. Besides solutions where a magnetic dipole aligned with the rotation axis dominates, we also find dipoles in the equatorial plane. A region of the parameter space exists where the two geometries compete, the axial dipole being subcritical and the equatorial dipole supercritical. The equatorial magnetic field is incompatible with a convection flow mainly made of vortices aligned with the rotation axis, and disrupts this flow at low magnetic energy. As a result the equatorial dipole dynamo saturates at a much lower magnetic field amplitude than the axial dynamo. This argument should pertain in planetary dynamos that are governed by strong rotational constraints. It provides an explanation for the comparatively low Elsasser number inferred for Uranus and Neptune.
Aubert Julien
Wicht Johannes
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