  We present the first global, three-dimensional simulations of solar/stellar
convection that take into account the influence of magnetic flux emergence by
means of the Babcock-Leighton (BL) mechanism. We have shown that the inclusion
of a BL poloidal source term in a convection simulation can promote cyclic
activity in an otherwise steady dynamo. Some cycle properties are reminiscent
of solar observations, such as the equatorward propagation of toroidal flux
near the base of the convection zone. However, the cycle period in this young
sun (rotating three times faster than the solar rate) is very short ($\sim$ 6
months) and it is unclear whether much longer cycles may be achieved within
this modeling framework, given the high efficiency of field generation and
transport by the convection. Even so, the incorporation of mean-field
parameterizations in 3D convection simulations to account for elusive processes
such as flux emergence may well prove useful in the future modeling of solar
and stellar activity cycles.
