  Our Sun exhibits strong convective dynamo action which results in magnetic
flux bundles emerging through the stellar surface as magnetic spots.
Global-scale dynamo action is believed to generate large-scale magnetic
structures in the deep solar interior through the interplay of convection,
rotation, and shear. Portions of these large-scale magnetic structures are then
believed to rise through the convective layer, forming magnetic loops which
then pierce the photosphere as sunspot pairs. Previous global simulations of 3D
MHD convection in rotating spherical shells have demonstrated mechanisms
whereby large-scale magnetic wreaths can be generated in the bulk of the
convection zone. Our recent simulations have achieved sufficiently high levels
of turbulence to permit portions of these wreaths to become magnetically
buoyant and rise through the simulated convective layer through a combination
of magnetic buoyancy and advection by convective giant cells. These buoyant
magnetic loops are created in the bulk of the convective layer as strong
Lorentz force feedback in the cores of the magnetic wreaths dampen small-scale
convective motions, permitting the amplification of local magnetic energies to
over 100 times the local kinetic energy. While the magnetic wreaths are largely
generated the shearing of axisymmetric poloidal magnetic fields by axisymmetric
rotational shear (the $\Omega$-effect), the loops are amplified to their peak
field strengths before beginning to rise by non-axisymmetric processes. This
further extends and enhances a new paradigm for the generation of emergent
magnetic flux bundles, which we term turbulence-enabled magnetic buoyancy.
