  We carry out a magneto-hydrodynamic (MHD) simulation of convective dynamo in
the rotating solar convective envelope driven by the solar radiative diffusive
heat flux. The simulation is similar to that reported in Fan & Fang (2014) but
with further reduced viscosity and magnetic diffusion. The resulting convective
dynamo produces a large scale mean field that exhibits similar irregular cyclic
behavior and polarity reversals, and self-consistently maintains a solar-like
differential rotation. The main driver for the solar-like differential rotation
(with faster rotating equator) is a net outward transport of angular momentum
away from the rotation axis by the Reynolds stress, and we found that this
transport is enhanced with reduced viscosity and magnetic diffusion.
