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Observations of protoplanetary disks have revealed them to be complex anddynamic, with vertical and radial transport of gas and dust occurringsimultaneously with chemistry and planet formation. Previous models ofprotoplanetary disks focused primarily on chemical evolution of gas and dust ina static disk, or dynamical evolution of solids in a chemically passive disk.In this paper, we present a new 1D method for modelling pebble growth andchemistry simultaneously. Gas and small dust particles are allowed to diffusevertically, connecting chemistry at all elevations of the disk. Pebbles areassumed to form from the dust present around the midplane, inheriting thecomposition of ices at this location. We present the results of this modelafter 1 Myr of disk evolution around a 1$M_\odot$ star at various locationsboth inside and outside of the CO snowline. We find that for a turbulent disk($\alpha = 10^{-3}$), CO is depleted from the surface layers of the disk byroughly 1-2 orders of magnitude, consistent with observations of protoplanetarydisks. This is achieved by a combination of ice sequestration and decreasing UVopacity, both driven by pebble growth. Further, we find the selective removalof ice species via pebble growth and sequestration can increase gas phase C/Oratios to values of approximately unity. However, our model is unable toproduce C/O values of $\sim$1.5-2.0 inferred from protoplanetary diskobservations, implying selective sequestration of ice is not sufficient toexplain C/O ratios $>1$.

Chemical Feedbacks of Pebble Growth: Impacts on CO depletion and C/O ratios