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We review recent advances in modeling global-scale convection and dynamoprocesses with the Anelastic Spherical Harmonic (ASH) code. In particular, wehave recently achieved the first global-scale solar convection simulations thatexhibit turbulent pumping of magnetic flux into a simulated tachocline and thesubsequent organization and amplification of toroidal field structures byrotational shear. The presence of a tachocline not only promotes the generationof mean toroidal flux, but it also enhances and stabilizes the mean poloidalfield throughout the convection zone, promoting dipolar structure with lessfrequent polarity reversals. The magnetic field generated by a convectivedynamo with a tachocline and overshoot region is also more helical overall,with a sign reversal in the northern and southern hemispheres. Toroidaltachocline fields exhibit little indication of magnetic buoyancy instabilitiesbut may be undergoing magneto-shear instabilities.

Three-Dimensional Simulations of Solar and Stellar Dynamos: The Influence of a Tachocline