Magnetic fieldlines in a global convection simulation

Snapshot of a magnetohydrodynamical simulation of the solar convection zone taken at a maximum of the cycle's strength. Magnetic field lines traced here originate at the bottom of the domain (red sphere) and extend all the way to the top (yellow sphere) as they permeate through the interface that separates the radiative and the convection zone. Note how the alignment of the magnetic field switches from the azimuthal to the radial direction as one travels from the bottom to the top of the domain. The former is caused by the longitudinal stretching produced by differential rotation at and below the base of the convection zone, while the latter results from the concentration of the magnetic field in convective downdrafts in the bulk of the convection zone. Here the simulation domain has been artificially inflated radially to facilitate the viewing of the magnetic fieldlines. .

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Ghizaru, M., Charbonneau, P., et Smolarkiewicz, P.K., Magnetic cycles in a large eddy simulation of solar convection, The Astrophysical Journal Letters, 715, L133-L137; on ADS
Racine, E., Charbonneau, P., Ghizaru, M., Bouchat, A., et Smolarkiewicz, P.K., On the mode of dynamo action in a global large-eddy simulation of solar convection, The Astrophysical Journal, 735, id46; on ADS