Dust growth, fragmentation and self-induced dust traps in PHANTOM
arXiv:2108.00878 · doi:10.1093/mnras/stab2263
Abstract
We present the implementation of a dust growth and fragmentation module in the public Smoothed Particle Hydrodynamics (SPH) code PHANTOM. This module is made available for public use with this paper. The coagulation model considers locally monodisperse dust size distributions around single values that are carried by the SPH particles. Along with the presentation of the model, implementation and tests, we showcase growth and fragmentation in a few typical circumstellar disc simulations and revisit previous results. The module is also interfaced with the radiative transfer code MCFOST, which facilitates the comparison between simulations and ALMA observations by generating synthetic maps. Circumstellar disc simulations with growth and fragmentation reproduce the `self-induced dust trap' mechanism first proposed by Gonzalez et al., which supports its existence. Synthetic images of discs featuring this mechanism suggest it would be detectable by ALMA as a bright axisymmetric ring at several tens of au from the star. With this paper, our aim is to provide a public tool to be able to study and explore dust growth in a variety of applications related to planet formation.
22 pages, 27 figures, accepted for publication in MNRAS
References in corpus (35)
- SPLASH: An interactive visualisation tool for Smoothed Particle Hydrodynamics simulations
- Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
- Gas- and dust evolution in protoplanetary disks
- Ring shaped dust accumulation in transition disks
- Monte Carlo radiative transfer in protoplanetary disks
- Dust filtration at gap edges: Implications for the spectral energy distributions of discs with embedded planets
- Planetesimal formation starts at the snow line
- Close-in planetesimal formation by pile-up of drifting pebbles
- Dust settling in local simulations of turbulent protoplanetary disks
- Initial mass function of planetesimals formed by the streaming instability
- Dust retention in protoplanetary disks
- Nine localised deviations from Keplerian rotation in the DSHARP circumstellar disks: Kinematic evidence for protoplanets carving the gaps
- On the origin of horseshoes in transitional discs
- A representative particle approach to coagulation and fragmentation of dust aggregates and fluid droplets
- Dust unveils the formation of a mini-Neptune planet in a protoplanetary ring
- Including Dust Coagulation in Hydrodynamic Models of Protoplanetary Disks: Dust Evolution in the Vicinity of a Jupiter-mass Planet
- An opening criterion for dust gaps in protoplanetary discs
- Flybys in protoplanetary discs: II. Observational signatures
- Monte Carlo simulation of particle interactions at high dynamic range: Advancing beyond the Googol
- Dust and gas mixtures with multiple grain species - a one-fluid approach
- Signatures of an eccentric disc cavity: Dust and gas in IRS 48
- Effect of dust radial drift on viscous evolution of gaseous disk
- Modeling dust growth in protoplanetary disks: The breakthrough case
- Linear growth of streaming instability in pressure bumps
- SPH simulations of grain growth in protoplanetary disks
- Long lived dust rings around HD169142
- Grain growth for astrophysics with Discontinuous Galerkin schemes
- Flyby-induced misalignments in planet-hosting discs
- Self-Induced Dust Traps Around Snow Lines in Protoplanetary Discs
- Effects of Ringed Structures and Dust Size Growth on Millimeter Observations of Protoplanetary Disks
- Tracking Dust Grains During Transport and Growth in Protoplanetary Disks
- Is the gap in the DS Tau disc hiding a planet?
- A solution to the overdamping problem when simulating dust-gas mixtures with smoothed particle hydrodynamics
- Ring Morphology with Dust Coagulation in Protoplanetary Disks
- Size and density sorting of dust grains in SPH simulations of protoplanetary disc II: Fragmentation
Cited by in corpus (5)
- A highly settled disk around Oph 163131
- If you like C/O variations, you should have put a ring on it
- Exciting spiral arms in protoplanetary discs from flybys
- Impact of turbulence intensity and fragmentation velocity on dust particle size evolution and non-ideal magnetohydrodynamics effects
- Single Fluid vs. Multifluid: Comparison between single fluid and multifluid dust models for disc planet interactions