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

TL;DR

This paper introduces the FEOSAD hydrodynamic model to study volatile distribution and snowline dynamics in protoplanetary disks, revealing complex snowline structures and volatile accumulation patterns during disk evolution.

Contribution

The study presents a new dynamic model for volatile behavior in protoplanetary disks, incorporating dust populations and snowline evolution, with detailed analysis of volatile distribution and snowline shifts.

Findings

Most ice reaches grown dust via coagulation with small grains

Complex snowline shapes form due to spiral structures and photodissociation

Snowlines shift closer to the star over time, becoming 4-5 times smaller

Abstract

The snowlines of various volatile species in protoplanetary disks are associated with abrupt changes in gas composition and dust physical properties. Volatiles may affect dust growth, as they cover grains with icy mantles that can change the fragmentation velocity of the grains. In turn, dust coagulation, fragmentation, and drift through the gas disk can contribute to the redistribution of volatiles between the ice and gas phases. Here we present the hydrodynamic model FEOSAD for protoplanetary disks with two dust populations and volatile dynamics. We compute the spatial distributions of major volatile molecules (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 disk evolution. We show that most of ice arrives to the grown dust through coagulation with small grains. Spiral structures and dust rings forming in the disk, as well as photodissociation in the outer regions, lead to the formation of 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 disk formation epoch. We demonstrate that volatiles tend to collect in the vicinity of their snowlines, both in the ice and gas phases, leading to the formation of thick icy mantles potentially important for dust dynamics. The dust size is affected by a lower fragmentation velocity of bare grains in the model with a higher turbulent viscosity.