Revisiting collisional dust growth in Class 0/I protostellar disks: Sweep-up can convert a few $10 M_\oplus$ of dust into kg pebbles in 0.1 Myr

Recent observations suggest that the first stages of planet formation likely take place in Class 0/I phase Young Stellar Object evolution, when star and disk are still embedded an infalling envelope. In this study we perform grain coagulation calculations to investigate very stage formation, collisional growth dust grains, disks. We find slow increase mass by high-velocity collision with much smaller grains ("sweep-up") allows $\sim 50 M_\oplus$ grow well beyond fragmentation barrier into $\sim$kg pebbles end (0.1 Myr). analyze linear saturation sweep-up understand our results quantitatively, test whether outcome is sensitive parameters details model. The pebble population could be important for because they less well-coupled gas (compared main below barrier) therefore more favorable known mechanisms clump (which initiate planetesimal formation). It also contains enough form all cores, based on observational estimates budget. Our findings motivate future studies disks, including subsequent evolution population.