Dynamos of giant planets

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 dyna...

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Published inProceedings of the International Astronomical Union Vol. 2; no. S239; pp. 467 - 474
Main Authors Busse, F. H., Simitev, R.
Format Journal Article
LanguageEnglish
Published Cambridge, UK Cambridge University Press 01.08.2006
Subjects
Astronomy
Astrophysics
Contributed Papers
Fluid dynamics
Magnetic fields
Planets
MHD
Planets
magnetic fields
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Summary: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.
Bibliography:ObjectType-Article-2
SourceType-Scholarly Journals-1
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ISSN:1743-9213
1743-9221
DOI:10.1017/S1743921307000920