  Our global 3D simulations of convection and dynamo action in a Sun-like star
reveal that persistent wreaths of strong magnetism can be built within the bulk
of the convention zone. Here we examine the characteristics of buoyant magnetic
structures that are self-consistently created by dynamo action and turbulent
convective motions in a simulation with solar stratification but rotating at
three times the current solar rate. These buoyant loops originate within
sections of the magnetic wreaths in which turbulent flows amplify the fields to
much larger values than is possible through laminar processes. These amplified
portions can rise through the convective layer by a combination of magnetic
buoyancy and advection by convective giant cells, forming buoyant loops. We
measure statistical trends in the polarity, twist, and tilt of these loops.
Loops are shown to preferentially arise in longitudinal patches somewhat
reminiscent of active longitudes in the Sun, although broader in extent. We
show that the strength of the axisymmetric toroidal field is not a good
predictor of the production rate for buoyant loops or the amount of magnetic
flux in the loops that are produced.
