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One of the main problems in planet formation, hampering the growth of smalldust to planetesimals, is the so-called radial-drift barrier. Pebbles of cm todm sizes are thought to drift radially across protoplanetary discs faster thanthey can grow to larger sizes, and thus to be lost to the star. To overcomethis barrier, drift has to be slowed down or stopped, or growth needs to besped up. In this paper, we investigate the role of porosity on both drift andgrowth. We have developed a model for porosity evolution during grain growthand applied it to numerical simulations of protoplanetary discs. We find thatgrowth is faster for porous grains, enabling them to transition to the Stokesdrag regime, decouple from the gas, and survive the radial-drift barrier.Direct formation of small planetesimals from porous dust is possible over largeareas of the disc.

Evolution of porous dust grains in protoplanetary discs -- I. Growing grains