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We propose a pebble-driven planet formation scenario to form giant planetswith high multiplicity and large orbital distances in the early gas disk phase.We perform N-body simulations to investigate the growth and migration oflow-mass protoplanets in the disk with inner viscously heated and outer stellarirradiated regions. The key feature of this model is that the giant planetcores grow rapidly by a combination of pebble accretion and planet-planetcollisions. This consequently speeds up their gas accretion. Because ofefficient growth, the planet transitions from rapid type I migration to slowtype II migration early, reducing the inward migration substantially. Multiplegiant planets can sequentially form in this way with increasing semimajor axes.Both mass growth and orbital retention are more pronounced when a large numberof protoplanets are taken into account compared to the case of single planetgrowth. Eventually, a few numbers of giant planets form with orbital distancesof a few to a few tens of AUs within $1.5{-}3$ Myr after the birth of theprotoplanets. The resulting simulated planet populations could be linked to thesubstructures exhibited in disk observations as well as large orbital distanceexoplanets observed in radial velocity and microlensing surveys.

Promoted Mass Growth of Multiple, Distant Giant Planets through Pebble Accretion and Planet-Planet Collision