  We report the results of a magneto-hydrodynamic (MHD) simulation of a
convective dynamo in a model solar convective envelope driven by the solar
radiative diffusive heat flux. The convective dynamo produces a large-scale
mean magnetic field that exhibits irregular cyclic behavior with oscillation
time scales ranging from about 5 to 15 years and undergoes irregular polarity
reversals. The mean axisymmetric toroidal magnetic field is of opposite signs
in the two hemispheres and is concentrated at the bottom of the convection
zone. The presence of the magnetic fields is found to play an important role in
the self-consistent maintenance of a solar-like differential rotation in the
convective dynamo model. Without the magnetic fields, the convective flows
drive a differential rotation with a faster rotating polar region. In the midst
of magneto-convection, we found emergence of strong super-equipartition flux
bundles at the surface, exhibiting properties that are similar to emerging
solar active regions.
