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Thanks to ``dust-to-planet'' simulations (DTPSs), which treat the collisionalevolution directly from dust to giant-planet cores in a protoplanetary disk, weshowed that giant-planet cores are formed in $\lesssim 10\,$au in several$10^5$ years, because porous pebbles grow into planetesimals via collisionsprior to drift in 10 au (Kobayashi & Tanaka 2021, Paper I).However, such porouspebbles are unlikely to reproduce the polarized millimeter wavelength lightobserved from protoplanetary disks. We thus investigate gas-giant coreformation with non-porous pebbles via DTPSs. Even non-porous bodies can growinto planetesimals and massive cores to be gas giants are also formed inseveral $10^5$ years. The rapid core formation is mainly via the accretion ofplanetesimals produced by collisional coagulation of pebbles drifting from theouter disk. The formation mechanism is similar to the case with porous pebbles,while core formation occurs in a wider region (5 - 10 au) than that with porouspebbles.

Rapid Formation of Gas-giant Planets via Collisional Coagulation from  Dust Grains to Planetary Cores. II. Dependence on Pebble Bulk Density and  Disk Temperature