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Dynamos of giant planets

Published online by Cambridge University Press:  01 August 2006

F. H. Busse  and
R. Simitev
F. H. Busse
Affiliation:
Institute of Physics, University of Bayreuth, D95440 Bayreuth, Germany email: busse@uni-bayreuth.de
R. Simitev
Affiliation:
Department of Mathematics, University of Glasgow, UK email: rs@maths.gl.ac.uk
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Abstract

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Possibilities and difficulties of applying the theory of magnetic field generation by convection flows in rotating spherical fluid shells to the Giant Planets are outlined. Recent progress in the understanding of the distribution of electrical conductivity in the Giant Planets suggests that the dynamo process occurs predominantly in regions of semiconductivity. In contrast to the geodynamo the magnetic field generation in the Giant Planets is thus characterized by strong radial conductivity variations. The importance of the constraint on the Ohmic dissipation provided by the planetary luminosity is emphasized. Planetary dynamos are likely to be of an oscillatory type, although these oscillations may not be evident from the exterior of the planets.

Keywords

Planetsmagnetic fieldsMHD
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S239: Convection in Astrophysics , August 2006 , pp. 467 - 474
Copyright
Copyright © International Astronomical Union 2007

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