Chemical evolution of turbulent protoplanetary disks and the Solar
  nebula
  This is the second paper in a series where we study the influence of
transport processes on the chemical evolution of protoplanetary disks. Our
analysis is based on a flared alpha-model of the DM Tau system, coupled to a
large gas-grain chemical network. To account for production of complex
molecules, the chemical network is supplied with an extended set of surface
reactions and photo-processes in ice mantles. Our disk model covers a wide
range of radii, 10-800 AU (from a Jovian planet-forming zone to the outer disk
edge). Turbulent transport of gases and ices is implicitly modeled in full 2D
along with the time-dependent chemistry. Two regimes are considered, with high
and low efficiency of turbulent mixing. The results of the chemical model with
suppressed turbulent diffusion are close to those from the laminar model, but
not completely. A simple analysis for the laminar chemical model to highlight
potential sensitivity of a molecule to transport processes is performed. It is
shown that the higher the ratio of the characteristic chemical timescale to the
turbulent transport timescale for a given molecule, the higher the probability
that its column density will be affected by diffusion. We find that turbulent
transport enhances abundances and column densities of many gas-phase species
and ices, particularly, complex ones. For such species a chemical steady-state
is not reached due to long timescales associated with evaporation and surface
photoprocessing and recombination. In contrast, simple radicals and molecular
ions, which chemical evolution is fast and proceeds solely in the gas phase,
are not much affected by dynamics. All molecules are divided into three groups
according to the sensitivity of their column densities to the turbulent
diffusion. [Abridged]
