A variety of methods are brought to bear on the problem of appreciating
turbulent convection in the solar interior. Seismic analyses of observations taken by
the Helioseismic and Magnetic Imager onboard the Solar Dynamics Observatory reveal
convective velocities that are almost two orders in magnitude smaller than current
theoretical and computational predictions. The associated Reynolds' stresses would be too
small to explain meridional circulation and differential rotation in the convection envelope
and throw into question models of dynamo action in the Sun.
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