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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.  
DOI: 10.1126/science.1235954
Using the multiscale flow emulation model EULAG (also here)

LEFT
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

CENTER  
radial magnetic field at the same depth

gray to yellow, outward-directed magnetic field;
gray to green, inward-directed

RIGHT  
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.

(via Modeling the Solar Dynamo)

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