Mean field from differential rotation

Dynamo runs


  • The following runs show By. The front side is the xz plane, on the left we have the yz plane at what corresponds to the bottom of the convection zone, and above we have the xy plane at what corresponds to mid-latitudes. Note that the latter two surfaces are perfectly conducting.

    negative helicity, 128x512x128 AVI (13M), mpeg (6.1M)

    no helicity, 128x512x128, Part I AVI (24M), mpeg (11M)

    no helicity, 128x512x128, Part II AVI (21M), mpeg (9.7M)


  • Here we show Bx, but now all planes are swapped, so the side on the left is the yz plane on the outer surface, the upper plane corresponds to the equator, and the front plane corresponds still to the xz plane on a periodic boundary.

    positive helicity, 128x512x128, bx, outer surface AVI (1.5M), mpeg (1.0M)

    same as above, but 1 frame per second AVI (1.5M), mpeg (1.0M)

    negative helicity, 128x512x128, bx, outer surface AVI (6.9M), mpeg (4.4M)


    Low resolution runs

    no helicity, 64x256x64, by, on perf. cond. surface AVI (31M), mpeg (15M)


  • Brandenburg, A.: 2005, ``The case for a distributed solar dynamo shaped by near-surface shear,'' Astrophys. J. (http://www.nordita.dk/~brandenb/tmp/surfdiffrot)
    $Date: 2005/04/10 03:02:25 $, $Author: brandenb $, $Revision: 1.7 $