Enforcing dust mass conservation in 3D simulations of tightly-coupled grains with the Phantom SPH code

Abstract

We describe a new implementation of the one-fluid method in the SPH code Phantom to simulate the dynamics of dust grains in gas protoplanetary discs. We revise and extend previously developed algorithms by computing the evolution of a new fluid quantity that produces a more accurate and numerically controlled evolution of the dust dynamics. Moreover, by limiting the stopping time of uncoupled grains that violate the assumptions of the terminal velocity approximation, we avoid fatal numerical errors in mass conservation. We test and validate our new algorithm by running 3D SPH simulations of a large range of disc models with tightly- and marginally-coupled grains.

arXiv comment6 pages, 3 figures

References in corpus (16)

• Streaming Instabilities in Protoplanetary Disks
• SPLASH: An interactive visualisation tool for Smoothed Particle Hydrodynamics simulations
• Dust Evolution and the Formation of Planetesimals
• Dusty gas with SPH - I. Algorithm and test suite
• Dusty gas with one fluid
• The complex morphology of the young disk MWC 758: Spirals and dust clumps around a large cavity
• 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
• Individual and collective behavior of dust particles in a protoplanetary nebula
• Grand challenges in protoplanetary disc modelling
• Dusty gas with one fluid in smoothed particle hydrodynamics
• Two fluid dust and gas mixtures in SPH: A semi-implicit approach
• MULTIGRAIN: A smoothed particle hydrodynamics algorithm for multiple small dust grains and gas
• Smoothed particle hydrodynamics simulations of gas and dust mixtures
• Two-fluid dust and gas mixtures in smoothed particle hydrodynamics II: an improved semi-implicit approach
• Resolved observations of transition disks

Cited by in corpus (29)

• Phantom: A smoothed particle hydrodynamics and magnetohydrodynamics code for astrophysics
• Kinematic detection of a planet carving a gap in a protoplanetary disc
• Flybys in protoplanetary discs: I. Gas and dust dynamics
• Flybys in protoplanetary discs: II. Observational signatures
• Spiral Arms and a Massive Dust Disk with non-Keplerian Kinematics: Possible Evidence for Gravitational Instability in the Disk of Elias 2-27
• The Ring Structure in the MWC 480 Disk Revealed by ALMA
• Gas and multi-species dust dynamics in viscous protoplanetary discs: the importance of the dust back-reaction
• A dust and gas cavity in the disc around CQ Tau revealed by ALMA
• Predicting the kinematic evidence of gravitational instability
• Long lived dust rings around HD169142
• Planet migration, resonant locking and accretion streams in PDS70: Comparing models and data
• HD 143006: circumbinary planet or misaligned disc?
• Circumbinary and circumstellar discs around the eccentric binary IRAS 04158+2805 -- a testbed for binary-disc interaction
• Spirals, shadows & precession in HD 100453 -- I. The orbit of the binary
• Dust growth, fragmentation and self-induced dust traps in PHANTOM
• Is the gap in the DS Tau disc hiding a planet?
• Multi-wavelength observations of protoplanetary discs as a proxy for the gas disc mass
• Kinematic evidence for an embedded planet in the IM Lupi disc
• A solution to the overdamping problem when simulating dust-gas mixtures with smoothed particle hydrodynamics
• Compaction during fragmentation and bouncing produces realistic dust grain porosities in protoplanetary discs
• Dynamical dust traps in misaligned circumbinary discs: analytical theory and numerical simulations
• Presolar grain dynamics: creating nucleosynthetic variations through a combination of drag and viscous evolution
• A giant planet shaping the disk around the very low-mass star CIDA 1
• Dust dynamics in current sheets within protoplanetary disks. I. Isothermal models including ambipolar diffusion and Ohmic resistivity
• A smoothed particle hydrodynamics algorithm for multigrain dust with separate sets of particles
• Single Fluid vs. Multifluid: Comparison between single fluid and multifluid dust models for disc planet interactions
• Constraining protoplanetary disc mass using the GI wiggle
• Modelling dust coagulation, dynamical drag and turbulent mixing during star and disc formation
• MULTIGRAIN: Simulating mixtures of multiple dust grains and gas with SPH