Planetesimal formation during protoplanetary disk buildup (<i>Corrigendum</i>)

Models of dust coagulation and subsequent planetesimal formation are usually computed on the backdrop an already fully formed protoplanetary disk model. At same time, observational studies suggest that should start early, possibly even before is formed. In this paper, we investigate under which conditions planetesimals form during buildup stage, in gas fall onto from its parent molecular cloud. We couple our earlier model at water snow line to a simple evolution. find most only after stage when becomes less massive hot. However, there parameters for buildup. This occurs viscosity driving evolution intermediate ($\alpha_v \sim 10^{-3}-10^{-2}$) while turbulent mixing reduced compared ($\alpha_t \le 0.03 \cdot \alpha_v$), with assumption vapor vertically well-mixed gas. Such $\alpha_t \ll \alpha_v$ scenario could be expected layered accretion, where flow mostly driven by active surface layers, midplane resides, quiescent.