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Geophys. J. Int. (2008) 172, 945956 doi: 10.1111/j.1365-246X.2007.03693.x GJIGeomagnetism,rockmagnetismandpalaeomagnetism

Summary: Geophys. J. Int. (2008) 172, 945­956 doi: 10.1111/j.1365-246X.2007.03693.x
The magnetic structure of convection-driven numerical dynamos
Julien Aubert,1
Jonathan Aurnou2
and Johannes Wicht3
1Dynamique des Fluides G´eologiques, Institut de Physique du Globe de Paris, 4 place Jussieu, 75252 Paris cedex 5, France. E-mail: aubert@ipgp.jussieu.fr
2Department of Earth and Space Sciences, University of California, Los Angeles, USA
3Max-Planck Institute for Solar System Research, Katlenburg-Lindau, Germany
Accepted 2007 November 21. Received 2007 November 15; in original form 2007 April 24
The generation of a magnetic field in numerical simulations of the geodynamo is an intrinsically
3-D and time-dependent phenomenon. The concept of magnetic field lines and the frozen-flux
approximation can provide insight into such systems, but a suitable visualization method is re-
quired. This paper presents results obtained using the Dynamical Magnetic Field line Imaging
(DMFI) technique, which is a representation of magnetic field lines accounting for their local
magnetic energy, together with an algorithm for the time evolution of their anchor points. The
DMFI illustrations are consistent with previously published dynamo mechanisms, and allow
further investigation of spatially and temporally complex systems. We highlight three types
of magnetic structures: (i) magnetic cyclones and (ii) magnetic anticyclones are expelled by,


Source: Aubert, Julien - Institut de Physique du Globe de Paris
Aurnou, Jonathan - Department of Earth and Space Sciences, University of California at Los Angeles


Collections: Geosciences