THE SUN'S DEEP-SEATED CONVECTIVE FLOWS MUST ULTIMATELY SUSTAIN BOTH THE EFFICIENT EMF FROM WHICH SOLAR MAGNETISM DERIVES AND THE DIFFERENTIAL ROTATION AND MERIDIONAL CIRCULATION THOUGHT TO IMBUE THAT MAGNETISM WITH ITS REMARKABLE SPATIOTEMPORAL ORDERING. EXPLORATION OF THE DYNAMO PROCESS ULTIMATELY REQUIRES KNOWLEDGE OF HOW THESE DEEP CONVECTIVE FLOWS ARE STRUCTURED AND YET PRESENT HELIOSEISMIC TECHNIQUES HAVE ONLY RECENTLY BEEN ABLE TO IMAGE FLOWS IN THE LOWER PORTION OF THE CONVECTION ZONE.

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