Particle Pile-ups and Planetesimal Formation

Abstract

Solid particles in protoplanetary disks that are sufficiently super-solar in metallicity overcome turbulence generated by vertical shear to gravitationally condense into planetesimals. Super-solar metallicities result if solid particles pile up as they migrate starward as a result of aerodynamic drag. Previous analyses of aerodynamic drift rates that account for mean flow differences between gas and particles yield particle pile-ups. We improve on these studies not only by accounting for the collective inertia of solids relative to that of gas, but also by including the transport of angular momentum by turbulent stresses within the particle layer. These turbulent stresses are derived in a physically self-consistent manner from the structure of marginally Kelvin-Helmholtz turbulent flows. They are not calculated using the usual plate drag formulae, whose use we explain is inappropriate. Accounting for the relative inertia of solids to gas retards, but does not prevent, particle pile-ups, and generates more spatially extended regions of metal enrichment. Turbulent transport hastens pile-ups. We conclude that particle pile-up is a robust outcome in sufficiently passive protoplanetary disks. Connections to observations of circumstellar disks, including the Kuiper Belt, and the architectures of planetary systems are made.

Final revised version, accepted to ApJ. Error corrected in density dependence of Epstein drift rate; correction caused quantitative changes, particularly in high particle density limit. Qualitative conclusion that particle pile-ups can trigger planetesimal formation within protostellar disk lifetime is unaffected

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