Dynamos of giant planets

Busse, F.H. and Simitev, R. (2006) Dynamos of giant planets. Proceedings of the International Astronomical Union, 2(S239), pp. 467-474. (doi:10.1017/S1743921307000920)

[img] Text
arxiv.html

3kB

Publisher's URL: http://dx.doi.org/10.1017/S1743921307000920

Abstract

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.

Item Type:Articles
Status:Published
Refereed:Yes
Glasgow Author(s) Enlighten ID:Simitev, Dr Radostin
Authors: Busse, F.H., and Simitev, R.
Subjects:Q Science > QB Astronomy
Q Science > QC Physics
College/School:College of Science and Engineering > School of Mathematics and Statistics > Mathematics
Journal Name:Proceedings of the International Astronomical Union
ISSN:1743-9213
ISSN (Online):1743-9221
Published Online:21 May 2007

University Staff: Request a correction | Enlighten Editors: Update this record