Max Planck Institute for Multidisciplinary Sciences

Time-Evolution of the Earth's Magnetic Field During a Simulated Reversal

Shown is the radial magnetic field of our Earth-like dynamo (chemical convection at E = 3x10-4, Pm = 3, Ra = 35 times critical). Red colors positive, blue negative values. The animations cover the time interval from Fig. 8 of Kutzner and Christensen (2002) [3], see also Fig. 9 therein. Time t above the animations is given in magnetic diffusion time.

Fig. 1: This animation shows the field as it would appear at the surface of the Earth. Contour step is 0.0055. — Fig. 1: This animation shows the field as it would appear at the surface of the Earth. Contour step is 0.0055.

© C. Kutzner

Fig. 1: This animation shows the field as it would appear at the surface of the Earth. Contour step is 0.0055.

© C. Kutzner

Fig. 1: This animation shows the field as it would appear at the surface of the Earth. Contour step is 0.0055. — Fig. 1: This animation shows the field as it would appear at the surface of the Earth. Contour step is 0.0055.

© C. Kutzner

Fig. 1: This animation shows the field as it would appear at the surface of the Earth. Contour step is 0.0055.

© C. Kutzner

Fig. 2: Field at the core-mantle-boundary (CMB), contour step is 0.29. View onto the north pole of the CMB. Notice the strong flux patches that form above the pole at time t=1.866. They are due to expulsion of toroidal field by an upwelling plume. — Fig. 2: Field at the core-mantle-boundary (CMB), contour step is 0.29. View onto the north pole of the CMB. Notice the strong flux patches that form above the pole at time t=1.866. They are due to expulsion of toroidal field by an upwelling plume.

© C. Kutzner

Fig. 2: Field at the core-mantle-boundary (CMB), contour step is 0.29. View onto the north pole of the CMB. Notice the strong flux patches that form above the pole at time t=1.866. They are due to expulsion of toroidal field by an upwelling plume.

© C. Kutzner

Fig. 2: Field at the core-mantle-boundary (CMB), contour step is 0.29. View onto the north pole of the CMB. Notice the strong flux patches that form above the pole at time t=1.866. They are due to expulsion of toroidal field by an upwelling plume. — Fig. 2: Field at the core-mantle-boundary (CMB), contour step is 0.29. View onto the north pole of the CMB. Notice the strong flux patches that form above the pole at time t=1.866. They are due to expulsion of toroidal field by an upwelling plume.

© C. Kutzner

Fig. 2: Field at the core-mantle-boundary (CMB), contour step is 0.29. View onto the north pole of the CMB. Notice the strong flux patches that form above the pole at time t=1.866. They are due to expulsion of toroidal field by an upwelling plume.

© C. Kutzner

Fig. 3: Field at the CMB, contour step is 0.29. View onto the south pole of the CMB. — Fig. 3: Field at the CMB, contour step is 0.29. View onto the south pole of the CMB.

© C. Kutzner

Fig. 3: Field at the CMB, contour step is 0.29. View onto the south pole of the CMB.

© C. Kutzner

Fig. 3: Field at the CMB, contour step is 0.29. View onto the south pole of the CMB. — Fig. 3: Field at the CMB, contour step is 0.29. View onto the south pole of the CMB.

© C. Kutzner

Fig. 3: Field at the CMB, contour step is 0.29. View onto the south pole of the CMB.

© C. Kutzner

Publications

C. Kutzner, U. R. Christensen

Simulated Geomagnetic Reversals and Preferred Virtual Geomagnetic Pole Paths

Geophys. J. Int. 157 (3): 1105–1118, 2004

C. Kutzner

Untersuchung von Feldumkehrungen an einem numerischen Modell des Geodynamos

Dissertation, Georg-August-Universität Göttingen, 2003

C. Kutzner, U. R. Christensen

From Stable Dipolar Towards Reversing Numerical Dynamos

Phys. Earth Planet. Int. 131 (1): 29–45, 2002

C. Kutzner, U. R. Christensen

Effects of Driving Mechanisms in Geodynamo Models

Geophys. Res. Lett. 27 (1): 29–32, 2000

C. Kutzner

Numerische Simulationen zum Geodynamo: Einfluß verschiedener Antriebsarten auf Strömung und Magnetfeld

Diplomarbeit, Institut für Geophysik, Universität Göttingen, 1999