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Gas-giant planets, such as Jupiter, Saturn and massive exoplanets, wereformed via the gas accretion onto the solid cores each with a mass of roughlyten Earth masses. However, rapid radial migration due to disk-planetinteraction prevents the formation of such massive cores via planetesimalaccretion. Comparably rapid core growth via pebble accretion requires verymassive protoplanetary disks because most pebbles fall into the central star.Although planetesimal formation, planetary migration, and gas-giant coreformation have been studied with much effort, the full evolution path from dustto planets are still uncertain. Here we report the result of full simulationsfor collisional evolution from dust to planets in a whole disk. Dust growthwith realistic porosity allows the formation of icy planetesimals in the innerdisk (> 10 au), while pebbles formed in the outer disk drift to the inner diskand there grow to planetesimals. The growth of those pebbles to planetesimalssuppresses their radial drift and supplies small planetesimals sustainably inthe vicinity of cores. This enables rapid formation of sufficiently massiveplanetary cores within 0.2-0.4 million years, prior to the planetary migration.Our models shows first gas giants form at 2-7 au in rather commonprotoplanetary disks, in agreement with the exoplanet and solar systems.

Rapid formation of Gas Giant Planets via Collisional Coagulation from Dust Grains to Planetary Cores