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Dust is a major component of protoplanetary and debris disks as it is themain observable signature of planetary formation. However, since dust dynamicsis size-dependent (because of gas-drag or radiation pressure) any attempt tounderstand the full dynamical evolution of circumstellar dusty-disks thatneglect the coupling of collisional evolution with dynamical evolution isthwarted because of the feedback between these two processes. Here, a newhybrid lagrangian/eulerian code is presented that overcomes some of thesedifficulties. The particles representing "dust-clouds" are tracked individuallyin a lagrangian way. This system is then mapped on an eulerian spatial grid,inside the cells of which the local collisional evolutions are computed.Finally, the system is remapped back in a collection of discrete lagrangianparticles keeping constant their number. An application example on dust growthin a turbulent protoplanetary disk at 1 AU is presented. First the growth ofdust is considered in the absence of a dead-zone and the vertical distributionof dust is self-consistently computed. It is found that the mass is rapidlydominated by particles about a fraction of millimeter in size. Then the samecase with an embedded dead-zone is investigated and It is found thatcoagulation is much more efficient and produces, in a short time scale,1cm-10cm dust pebbles that dominate the mass. These pebbles may then beaccumulated into embryos sized objects inside large-scale turbulent structuresas shown recently (see e.g. Johansen et al., 2007).

A method for coupling dynamical and collisional evolution of dust in circumstellar disks: the effect of a dead zone