Modelling dust coagulation, dynamical drag and turbulent mixing during star and disc formation

Abstract

Planet formation in the discs around young stars involves the coagulation of sub-micron sized dust grains into much larger grains that may be mixed by turbulence and migrate through the disc. In this paper, we describe how we have combined a method for modelling the coagulation of a population of dust grains with the MULTIGRAIN algorithm for modelling the dynamical evolution of a population of dust grains that are subject to strong gas drag. We solve the dynamical evolution of the dust grains due to gas drag using a recently-developed implicit integration method, and we introduce a new implicit method to model the diffusion of the dust due to unresolved hydrodynamic turbulence. The resulting smoothed particle hydrodynamics (SPH) code allows us, for the first time, to model the growth, mixing and migration of dust grain populations during the early stages of star formation and the formation, growth and evolution of a young protoplanetary disc using three-dimensional hydrodynamical simulations. In doing so, we find that including turbulent dust diffusion within the disc provides a substantial enhancement of the rate of dust grain growth due to the fact that the turbulent diffusion provides a source of small and intermediate dust grains to the regions in which the largest dust grains are growing.

Submitted to MNRAS, includes changes following referee's first report. 29 pages, 18 figures

References in corpus (54)

• Streaming Instabilities in Protoplanetary Disks
• Modelling Accretion in Protobinary Systems
• SPLASH: An interactive visualisation tool for Smoothed Particle Hydrodynamics simulations
• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• The effect of gas drag on the growth of protoplanets -- Analytical expressions for the accretion of small bodies in laminar disks
• Closed-form expressions for particle relative velocities induced by turbulence
• Rapid Coagulation of Porous Dust Aggregates Outside the Snow Line: A Pathway to Successful Icy Planetesimal Formation
• An energy-conserving formalism for adaptive gravitational force softening in SPH and N-body codes
• Dust Evolution and the Formation of Planetesimals
• Dust coagulation and fragmentation in molecular clouds. I. How collisions between dust aggregates alter the dust size distribution
• The impact of magnetic fields on single and binary star formation
• Magnetic fields in protoplanetary disks
• Collapse of a Molecular Cloud Core to Stellar Densities: The First Three-Dimensional Calculations
• The thermodynamics of collapsing molecular cloud cores using smoothed particle hydrodynamics with radiative transfer
• Magnetorotational Instability Driven Accretion in Protoplanetary Disks
• On the water delivery to terrestrial embryos by ice pebble accretion
• Observations of edge-on protoplanetary disks with ALMA I. Results from continuum data
• Circumbinary, not transitional: On the spiral arms, cavity, shadows, fast radial flows, streamers and horseshoe in the HD142527 disc
• Smoothed Particle Magnetohydrodynamics II. Variational principles and variable smoothing length terms
• Dust Dynamics in Compressible MHD Turbulence
• Formation Process of the Circumstellar Disk: Long-term Simulations in the Main Accretion Phase of Star Formation
• Thresholds for Particle Clumping by the Streaming Instability
• Shattering and coagulation of dust grains in interstellar turbulence
• Smoothed Particle Magnetohydrodynamics III. Multidimensional tests and the div B = 0 constraint
• Global MHD simulations of stratified and turbulent protoplanetary discs. II. Dust settling
• The Origin and Formation of the Circumstellar Disk
• A faster algorithm for smoothed particle hydrodynamics with radiative transfer in the flux-limited diffusion approximation
• On linear dust-gas streaming instabilities in protoplanetary discs
• The statistical properties of stars and their dependence on metallicity
• The statistical properties of stars and their dependence on metallicity: the effects of opacity
• Collapse of a molecular cloud core to stellar densities: the formation and evolution of pre-stellar discs
• Smoothed particle hydrodynamics with radiative transfer in the flux-limited diffusion approximation
• A panoptic model for planetesimal formation and pebble delivery
• Vertical Shearing Instabilities in Radially Shearing Disks: The Dustiest Layers of the Protoplanetary Nebula
• A fast and explicit algorithm for simulating the dynamics of small dust grains with smoothed particle hydrodynamics
• Dust and gas mixtures with multiple grain species - a one-fluid approach
• Prograde rotation of protoplanets by accretion of pebbles in a gaseous environment
• Resolution requirements for simulating gravitational fragmentation using SPH
• "Ash-fall" induced by molecular outflow in protostar evolution
• Dust coagulation feedback on magnetohydrodynamic resistivities in protostellar collapse
• Protostellar collapse simulations in spherical geometry with dust coagulation and fragmentation
• MULTIGRAIN: A smoothed particle hydrodynamics algorithm for multiple small dust grains and gas
• Metallicity and the Universality of the IMF
• Three-Dimensional Simulations of Kelvin-Helmholtz Instability in Settled Dust Layers in Protoplanetary Disks
• Enforcing dust mass conservation in 3D simulations of tightly-coupled grains with the Phantom SPH code
• Millimeter-sized grains in the protostellar envelopes: where do they come from?
• Combining radiative transfer and diffuse interstellar medium physics to model star formation
• Polydisperse Streaming Instability III. Dust evolution encourages fast instability
• Grain growth for astrophysics with Discontinuous Galerkin schemes
• Dust coagulation in star formation with different metallicities
• Polydisperse Streaming Instability II. Methods for solving the linear stability problem
• Impact of dust size distribution including large dust grains on magnetic resistivity: an analytical approach
• Presolar grain dynamics: creating nucleosynthetic variations through a combination of drag and viscous evolution
• Dust evolution during the protostellar collapse: influence on the coupling between the neutral gas and the magnetic field