  The current dynamo paradigm for the Sun and sun-like stars places the
generation site for strong toroidal magnetic structures deep in the solar
interior. Sunspots and star-spots on sun-like stars are believed to arise when
sections of these magnetic structures become buoyantly unstable and rise from
the deep interior to the photosphere. Here we present the first 3-D global
magnetohydrodynamic (MHD) simulation in which turbulent convection,
stratification, and rotation combine to yield a dynamo that self-consistently
generates buoyant magnetic loops. We simulate stellar convection and dynamo
action in a spherical shell with solar stratification, but rotating three times
faster than the current solar rate. Strong wreaths of toroidal magnetic field
are realized by dynamo action in the convection zone. By turning to a dynamic
Smagorinsky model for subgrid-scale turbulence, we here attain considerably
reduced diffusion in our simulation. This permits the regions of strongest
magnetic field in these wreaths to rise toward the top of the convection zone
via a combination of magnetic buoyancy instabilities and advection by
convective giant cells. Such a global simulation yielding buoyant loops
represents a significant step forward in combining numerical models of dynamo
action and flux emergence.
