2011ApJS..196...25S

We study the influence of transport processes on the chemical evolution of DM Tau-like protoplanetary disks. Turbulent transport of gases and ices is implicitly modeled in full two dimensions (2D), using the mixing-length approximation, along with the time-dependent chemistry. We find that turbulent transport enhances abundances and column densities of many gas-phase species and ices, particularly, complex ones. The influence of turbulent mixing on disk chemistry is more pronounced in the inner, planet-forming disk region where gradients of temperature and high-energy radiation intensities are steeper than in the outer region. The molecules that are unresponsive to transport include, e.g., C₂H, C⁺, CH₄, CN, CO, HCN, HNC, H₂CO, OH, as well as water and ammonia ice. Their column densities computed with the laminar and 2D mixing model differ by a factor of ≲ 2-5. Molecules whose vertical column densities in the laminar and dynamical models differ by up to two orders of magnitude include, e.g., C₂H₂, some carbon chains, CS, H₂CS, H₂O, HCO⁺, HCOOH, HNCO, N₂H⁺, NH₃, CO ice, H₂ CO ice, CH₃ OH ice, and electrons. Molecules whose column densities are altered by diffusion by more than two orders of magnitude include, e.g., C₂S, C₃S, C₆H₆, CO₂, O₂, SiO, SO, SO₂, long carbon chain ices, CH₃ CHO ice, HCOOH ice, O₂ice, and OCN ice. We indicate several observable or potentially detectable tracers of transport processes in protoplanetary disks and the solar nebula, such as heavy hydrocarbon ices, complex organics, CO₂, O₂, SO, SO₂, C₂S, C₃ S compared to CO and water ice.