  This paper presents the results of the analysis of 3D simulations of solar
magneto-convection that include the joint action of the ambipolar diffusion and
the Hall effect. Three simulation-runs are compared: one including both
ambipolar diffusion and Hall effect; one including only ambipolar diffusion;
and one without any of these two effects. The magnetic field is amplified from
initial field to saturation level by the action of turbulent local dynamo. In
each of these cases, we study 2 hours of simulated solar time after the local
dynamo reaches the saturation regime. We analyze the power spectra of
vorticity, of magnetic field fluctuations and of the different components of
the magnetic Poynting flux responsible for the transport of vertical or
horizontal perturbations. Our preliminary results show that the ambipolar
diffusion produces a strong reduction of vorticity in the upper chromospheric
layers and that it dissipates the vortical perturbations converting them into
thermal energy. The Hall effect acts in the opposite way, strongly enhancing
the vorticity. When the Hall effect is included, the magnetic field in the
simulations becomes, on average, more vertical and long-lived flux tube-like
structures are produced. We trace a single magnetic structure to study its
evolution pattern and the magnetic field intensification, and their possible
relation to the Hall effect.
