Clusters of heavy particles in two-dimensional Keplerian turbulence

TL;DR

This study uses two-dimensional simulations to analyze how particles cluster in Keplerian turbulence, revealing conditions that promote planetesimal formation through particle concentration and multifractal distributions.

Contribution

It provides new insights into particle clustering mechanisms in Keplerian turbulence, highlighting the roles of rotation, shear, and particle size in planetesimal formation.

Findings

Faster Keplerian rotation enhances particle clustering.

Particles tend to concentrate in anticyclones at intermediate sizes.

Particle distributions are multifractal, aiding gravitational collapse.

Abstract

Protoplanetary disks are gaseous systems in Keplerian rotation around young stars, known to be turbulent. They include a small fraction of dust from which planets form. In the incremental scenario for planet growth, the formation of kilometer-size objects (planetesimals) from pebbles is a major open question. Clustering of particles is necessary for solids to undergo a local gravitational collapse. To address this question, the dynamic of inertial particles in turbulent flows with Keplerian rotation and shear is studied. Two-dimensional direct numerical simulations are performed to explore systematically two physical parameters: the rotation rate, which depends on the distance to the star, and the particle response time, which relates to their size. Shear is found to drastically affect the characteristics of the turbulent flow destroying cyclones and favoring the survival of anticyclones. Faster Keplerian rotation enhances clustering of particles. For intermediate sizes, particles concentrate in anticyclones. These clusters form in a hierarchical manner and merge together with time. For other parameter values, solids concentrate on fractal sets that get more singular with rotation. The mass distribution of particles is then found to be multifractal with small dimensions at large orders, intriguing for triggering their gravitational collapse. Such results are promising for a precise description and better understanding of planetesimal formation.