  We study how anisotropy of turbulent convection affects diffusion of
large-scale magnetic fields and the dynamo process on the Sun. The effect of
anisotropy is calculated in a mean-field magneto-hydrodynamics framework using
the minimal $\tau$-approximation. We examine two types of mean-field dynamo
models: the well-known benchmark flux-transport model, and a distributed-dynamo
model with the subsurface rotational shear layer. For both models we
investigate effects of the double-cell meridional circulation, recently
suggested by helioseismology. We introduce a parameter of anisotropy as a ratio
of the radial and horizontal intensity of turbulent mixing, to characterize the
anisotropy effects. It is found that the anisotropy of turbulent convection
affects the distribution of magnetic fields inside the convection zone. The
concentration of the magnetic flux near the bottom and top boundaries of the
convection zone is greater when the anisotropy is stronger. It is shown that
the critical dynamo number and the dynamo period approach to constant values
for the large anisotropy parameter. The anisotropy reduces the overlap of the
toroidal fields of subsequent cycles in the time-latitude ``butterfly' diagram.
If we assume that sunspots are formed in the vicinity of the subsurface shear
layer, then the distributed dynamo model with anisotropic diffusivity satisfies
the observational constraints from heloseismology results and is consistent
with the value of effective turbulent diffusion, estimated from the dynamics of
surface magnetic fields.
