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Context. Ice lines are suggested to play a significant role in grain growthand planetesimal formation in protoplanetary disks. Evaporation fronts directlyinfluence the gas and ice abundances of volatile species in the disk andtherefore the coagulation physics and efficiency and the chemical compositionof the resulting planetesimals.  Aims. In this work we investigate the influence of the existence of the COice line on the particle growth and on the distribution of CO in the disk.  Methods. We include the possibility of tracking the CO content and/or othervolatiles in particles and in the gas in our existing dust coagulation and diskevolution model and developed a method for evaporation and condensation of COusing the Hertz-Knudsen equation. Our model does not include fragmentation,yet, which will be part of further investigations.  Results. We find no enhanced grain growth just outside the ice line where theparticle size is limited by radial drift. Instead we find a depletion of solidmaterial inside the ice line which is solely due to evaporation of the CO. Sucha depression inside the ice line may be observable and may help to quantify theprocesses described in this work. Furthermore, we find that the viscosity anddiffusivity of the gas heavily influence the re-distribution of vaporized CO atthe ice line and can lead to an increase in the CO abundance by up to a factorsof a few in the region just inside the ice line. Depending on the strength ofthe gaseous transport mechanisms the position of the ice line in our model canchange by up to 10 AU and consequently, the temperature at that location canrange from 21 K to 23 K.

Redistribution of CO at the Location of the CO Ice Line in evolving Gas and Dust Disks