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Dust growth is often neglected when building models of protoplanetary disksdue to its complexity and computational expense. However, it does play a majorrole in shaping the evolution of protoplanetary dust and planet formation. Inthis paper, we present a numerical model coupling 2-D hydrodynamic evolution ofa protoplanetary disk, including a Jupiter-mass planet, and dust coagulation.This is obtained by including multiple dust fluids in a single grid-basedhydrodynamic simulation and solving the Smoluchowski equation for dustcoagulation on top of solving for the hydrodynamic evolution. We find thatfragmentation of dust aggregates trapped in a pressure bump outside of theplanetary gap leads to an enhancement in density of small grains. We comparethe results obtained from the full coagulation treatment to the commonly used,fixed dust size approach and to previously applied, less computationallyintensive methods for including dust coagulation. We find that the fullcoagulation results cannot be reproduced using the fixed-size treatment, butsome can be mimicked using a relatively simple method for estimating thecharacteristic dust size in every grid cell.

Including Dust Coagulation in Hydrodynamic Models of Protoplanetary Disks: Dust Evolution in the Vicinity of a Jupiter-mass Planet