The water-ice line as a birthplace of planets: implications of a species-dependent dust fragmentation threshold

The thermodynamic structure of protoplanetary discs is determined by dust opacities, which depend on the size grains and their chemical composition. In inner regions, grain sizes are regulated level turbulence (e.g. α viscosity) fragmentation velocity that represents maximal can have at a collision before they fragment. Here, we perform self-consistently calculated 2D hydrodynamical simulations consider full distribution with transition in water-ice line. This approach accounts for results previous particle laboratory experiments, silicate particles typically lower than particles. Furthermore, probe effects variations water abundance, dust-to-gas ratio, parameter disc structure. For line, find narrow but striking zone planetary outward migration, including low viscosities. addition, bump radial pressure gradient profile tends to be located slightly inside ice Both these features present all tested parameters. Thus, conclude line function both as migration trap, extend growth times planets migrate edge disc, where planetesimal formation initiated or enhanced.