Polydisperse Formation of Planetesimals: The dust size distribution in clumps

TL;DR

This study investigates how a realistic distribution of dust sizes affects the streaming instability in protoplanetary disks, revealing that polydispersity reduces clump formation efficiency and influences dust size segregation in dense regions.

Contribution

It presents the first detailed analysis of the non-linear phase of polydisperse streaming instability using advanced 2D hydrodynamic simulations with multiple dust species.

Findings

Polydisperse streaming instability is less efficient than monodisperse in forming dense clumps.

Larger dust sizes are more abundant in dense structures due to weaker gas coupling.

Size segregation occurs with the largest particles located outside the densest regions.

Abstract

The streaming instability is an efficient method for overcoming the barriers to planet formation in protoplanetary discs. The streaming instability has been extensively modelled by hydrodynamic simulations of gas and a single dust size. However, more recent studies considering a more realistic case of a particle size distribution show that this will significantly decrease the growth rate of the instability. We follow up on these studies by evaluating the polydisperse streaming instability, looking at the non-linear phase of the instability at the highest density regions, and investigating the dust size distribution in the densest dust structures. We employ 2D hydrodynamic simulations in an unstratified shearing box with multiple dust species representing an underlying continuous dust size spectrum using FARGO3D. To calculate the drag force on the gas due to a continuous dust size distribution, we apply the Gauss-Legendre quadrature method in dust size space. This method converges faster with the number of dust species than the usual uniform sampling method. The polydisperse streaming instability is less efficient than its monodisperse counterpart in generating dense clumps that could collapse into planetesimals. In the densest dust structure, the larger dust sizes are more abundant because they are less coupled to the gas and, therefore, can clump together more than the smaller dust grains. This trend is broken at the largest dust size due to size-dependent spatial segregation of the highest-density regions, where particles with the largest Stokes numbers are located just outside the densest areas of the combined dust species. This is observed as a peak in the size distribution at the densest regions, which could relate to the size distribution that ends up in the planetesimal after collapse and can mimic the size distribution of dust growth.