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The snowlines of various volatile species in protoplanetary disks areassociated with abrupt changes in gas composition and dust physical properties.Volatiles may affect dust growth, as they cover grains with icy mantles thatcan change the fragmentation velocity of the grains. In turn, dust coagulation,fragmentation, and drift through the gas disk can contribute to theredistribution of volatiles between the ice and gas phases. Here we present thehydrodynamic model FEOSAD for protoplanetary disks with two dust populationsand volatile dynamics. We compute the spatial distributions of major volatilemolecules (H$_2$O, CO$_2$, CH$_4$, and CO) in the gas, on small and grown dust,and analyze the composition of icy mantles over the initial 0.5 Myr of diskevolution. We show that most of ice arrives to the grown dust throughcoagulation with small grains. Spiral structures and dust rings forming in thedisk, as well as photodissociation in the outer regions, lead to the formationof complex snowline shapes and multiple snowlines for each volatile species.During the considered disk evolution, the snowlines shift closer to the star,with their final position being a factor $4-5$ smaller than that at the diskformation epoch. We demonstrate that volatiles tend to collect in the vicinityof their snowlines, both in the ice and gas phases, leading to the formation ofthick icy mantles potentially important for dust dynamics. The dust size isaffected by a lower fragmentation velocity of bare grains in the model with ahigher turbulent viscosity.

Gravitoviscous protoplanetary disks with a dust component. V. The dynamic model for freeze-out and sublimation of volatiles