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We discovered a new growth mode of dust grains to km-sized bodies inprotoplanetary disks that evolve by viscous accretion and magnetically drivendisk winds (MDWs). We solved an approximate coagulation equation of dust grainswith time-evolving disks that consist of both gas and solid components by aone-dimensional model. With the grain growth, all solid particles initiallydrift inward toward the central star by the gas drag force. However, the radialprofile of gas pressure, $P$, is modified by the MDW that disperses the gas inan inside-out manner. Consequently, a local concentration of solid particles iscreated by the converging radial flux of drifting dust grains at the locationwith the convex upward profile of $P$. When the dimensionless stopping time,${\rm St}$, there exceeds unity, the solid particles spontaneously reach thegrowth dominated state because of the positive feedback between the suppressedradial drift and the enhanced accumulation of dust particles that drift fromthe outer part. Once the solid particles are in the drift limited state, theabove-mentioned condition of ${\rm St} \gtrsim 1$ for the dust growth isequivalent with \begin{equation}  \Sigma_{\rm d}/\Sigma_{\rm g}\gtrsim \eta, \nonumber \end{equation} where$\Sigma_{\rm d}/\Sigma_{\rm g}$ is the dust-to-gas surface-density ratio and$\eta$ is dimensionless radial pressure-gradient force. As a consequence of thesuccessful growth of dust grains, a ring-like structure containingplanetesimal-sized bodies is formed at the inner part of the protoplanetarydisks. Such a ring-shaped concentration of planetesimals is expected to play avital role in the subsequent planet formation.

New growth mechanism of dust grains in protoplanetary disks with magnetically driven disk winds