Can dust coagulation trigger streaming instability?

TL;DR

This study explores whether dust coagulation can produce large enough grains to trigger streaming instability, facilitating planetesimal formation, especially outside the snow line, depending on local disk conditions.

Contribution

The paper introduces a semi-analytical model integrating dust coagulation with streaming instability, highlighting conditions for planetesimal formation in protoplanetary disks.

Findings

Planetesimal formation is more likely outside the snow line with icy aggregates.

High dust abundance and super-solar metallicity enhance planetesimal formation.

The process typically takes about 100 orbital periods for grain growth and 1000 for planetesimal formation.

Abstract

Streaming instability can be a very efficient way of overcoming growth and drift barriers to planetesimal formation. However, it was shown that strong clumping, which leads to planetesimal formation, requires a considerable number of large grains. State-of-the-art streaming instability models do not take into account realistic size distributions resulting from the collisional evolution of dust. We investigate whether a sufficient quantity of large aggregates can be produced by sticking and what the interplay of dust coagulation and planetesimal formation is. We develop a semi-analytical prescription of planetesimal formation by streaming instability and implement it in our dust coagulation code based on the Monte Carlo algorithm with the representative particles approach. We find that planetesimal formation by streaming instability may preferentially work outside the snow line, where sticky icy aggregates are present. The efficiency of the process depends strongly on local dust abundance and radial pressure gradient, and requires a super-solar metallicity. If planetesimal formation is possible, the dust coagulation and settling typically need ~100 orbits to produce sufficiently large and settled grains and planetesimal formation lasts another ~1000 orbits. We present a simple analytical model that computes the amount of dust that can be turned into planetesimals given the parameters of the disk model.