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The journey from dust particle to planetesimal involves physical processesacting on scales ranging from micrometers (the sticking and restructuring ofaggregates) to hundreds of astronomical units (the size of the turbulentprotoplanetary nebula). Considering these processes simultaneously is essentialwhen studying planetesimal formation. We develop a novel, global,semi-analytical model for the evolution of the mass-dominating dust particlesin a turbulent protoplanetary disk that takes into account the evolution of thedust surface density while preserving the essential characteristics of theporous coagulation process. This panoptic model is used to study the growthfrom submicron to planetesimal sizes in disks around Sun-like stars. For highlyporous ices, unaffected by collisional fragmentation and erosion, rapid growthto planetesimal sizes is possible in a zone stretching out to${\sim}10\mathrm{~AU}$ for massive disks. When porous coagulation is limited byerosive collisions, the formation of planetesimals through direct coagulationis not possible, but the creation of a large population of aggregates withStokes numbers close to unity might trigger the streaming instability (SI).However, we find that reaching conditions necessary for SI is difficult andlimited to dust-rich disks, (very) cold disks, or disks with weak turbulence.Behind the snow-line, porosity-driven aggregation of icy grains results inrapid (${\sim}10^{4}\mathrm{~yr}$) formation of planetesimals. If erosivecollisions prevent this, SI might be triggered for specific disk conditions.The numerical approach introduced in this work is ideally suited for studyingplanetesimal formation and pebble delivery simultaneously and will help build acoherent picture of the start of the planet formation process.

A panoptic model for planetesimal formation and pebble delivery