Integration of Particle-Gas Systems with Stiff Mutual Drag Interaction

TL;DR

This paper presents a novel numerical algorithm for efficiently simulating the stiff mutual drag interactions between gas and particles in protoplanetary disks, enabling more accurate modeling of planetesimal formation processes.

Contribution

The authors develop a cell-by-cell integration method that decomposes the coupled gas-particle system, allowing stable and accurate simulations of stiff drag forces in multi-dimensional settings.

Findings

Algorithm effectively handles stiff drag interactions.

Validated with benchmarks in 1D, 2D, and 3D.

Enables high-fidelity modeling of streaming instability.

Abstract

Numerical simulation of numerous mm/cm-sized particles embedded in a gaseous disk has become an important tool in the study of planet formation and in understanding the dust distribution in observed protoplanetary disks. However, the mutual drag force between the gas and the particles can become so stiff, particularly because of small particles and/or strong local solid concentration, that an explicit integration of this system is computationally formidable. In this work, we consider the integration of the mutual drag force in a system of Eulerian gas and Lagrangian solid particles. Despite the entanglement between the gas and the particles under the particle-mesh construct, we are able to devise a numerical algorithm that effectively decomposes the globally coupled system of equations for the mutual drag force and makes it possible to integrate this system on a cell-by-cell basis, which considerably reduces the computational task required. We use an analytical solution for the temporal evolution of each cell to relieve the time-step constraint posed by the mutual drag force as well as to achieve the highest degree of accuracy. To validate our algorithm, we use an extensive suite of benchmarks with known solutions in one, two, and three dimensions, including the linear growth and the nonlinear saturation of the streaming instability. We demonstrate numerical convergence and satisfactory consistency in all cases. Our algorithm can for example be applied to model the evolution of the streaming instability with mm/cm-sized pebbles at high mass loading, which has important consequences for the formation scenarios of planetesimals.