THREE SNAPSHOTS from a SIMULATION of the SOLAR DYNAMO
The Magnetohydrodynamics of Solar Convection
SOURCE Paul Charbonneau, Piotr K. Smolarkiewicz
Modeling the Solar Dynamo
Science 5 April 2013: Vol. 340 no. 6128 pp. 42-43.
Using the multiscale flow emulation model EULAG (also here)
color rendering of the radial component of the convective flow in the subsurface layers of the simulation
orange to light yellow, upflows;
red to dark blue, downflows
radial magnetic field at the same depth
gray to yellow, outward-directed magnetic field;
gray to green, inward-directed
magnitude of the zonal magnetic field component,
deep in the interior of the simulation,
at the base of the convection layer.
The banded torus-like structure at mid-latitudes - and its opposite-polarity counterpart in the other hemisphere - undergo synchronous polarity reversals about every 40 years.