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We calculate the chemical evolution of protoplanetary disks consideringradial viscous accretion, vertical turbulent mixing and vertical disk winds. Westudy the effects on the disk chemical structure when different models for theformation of molecular hydrogen on dust grains are adopted. Our gas-phasechemistry is extracted from the UMIST Database for Astrochemistry (Rate06) towhich we have added detailed gas-grain interactions. We use our chemical modelresults to generate synthetic near- and mid-infrared LTE line emission spectraand compare these with recent Spitzer observations. Our results show that if H2formation on warm grains is taken into consideration, the H2O and OH abundancesin the disk surface increase significantly. We find the radial accretion flowstrongly influences the molecular abundances, with those in the cold midplanelayers particularly affected. On the other hand, we show that diffusiveturbulent mixing affects the disk chemistry in the warm molecular layers,influencing the line emission from the disk and subsequently improvingagreement with observations. We find that NH3, CH3OH, C2H2 andsulphur-containing species are greatly enhanced by the inclusion of turbulentmixing. We demonstrate that disk winds potentially affect the disk chemistryand the resulting molecular line emission in a similar manner to that foundwhen mixing is included.

Chemical evolution of protoplanetary disks - the effects of viscous accretion, turbulent mixing and disk winds