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Dust growth and its associated dynamics play key roles in the first phase ofplanet formation in young stellar objects (YSOs). Observations have detectedsigns of dust growth in very young protoplanetary disks. Furthermore, signs ofplanet formation, gaps in the disk at a distance of several 10 astronomicalunits (AU) from the central protostar are also reported. From a theoreticalpoint of view, however, it is not clear how planet form at the outer region ofa disk despite the difficulty due to rapid inward drift of dust so calledradial drift barrier. Here, on the basis of three-dimensionalmagneto-hydrodynamical simulations of disk evolution with the dust growth, wepropose a mechanism named "ash-fall" phenomenon induced by powerful molecularoutflow driven by magnetic field which may circumvent the radial drift barrier.We found that the large dust which grows to a size of $\sim \cm$ in the innerregion of a disk is entrained by an outflow from the disk. Then large dustdecoupled from gas is ejected from the outflow due to centrifugal force,enriching the grown dust in the envelope and is eventually fall onto the outeredge of the disk. The overall process is similar to behaviour of ash-fall fromvolcanic eruptions. In the ash-fall phenomenon, the Stokes number of dustincreases by reaccreting to the less dense disk outer edge. This may make thedust grains overcome the radial drift barrier. Consequently, the ash-fallphenomenon can provide a crucial assist for making the formation of theplanetesimals in outer region of the disk possible, and hence the formation ofwide-orbit planets and the formation of the gaps.

"Ash-fall" induced by molecular outflow in protostar evolution