SHAMPOO: A stochastic model for tracking dust particles under the influence of non-local disk processes

Abstract

The abundances of CHNOS are crucial for the composition of planets. At the onset of planet formation, large amounts of these elements are stored in ices on dust grains in planet-forming disks. The evolution of this ice is affected by dynamical transport, collisional processes, and the formation and sublimation of ice. We aim to constrain the disk regions where these processes are fully coupled, and develop a flexible modelling approach that is able to predict the effects of these processes acting simultaneously on the CHNOS budgets of the dust in these regions. We compared timescales associated with these disk processes to constrain the disk regions where this approach is necessary, and developed the SHAMPOO code, which tracks the CHNOS abundances in the ice mantle of a single monomer dust particle, embedded in a larger aggregate and undergoing these processes simultaneously. The adsorption and photodesorption of monomer ices depend on the depth of the monomer in the aggregate. We investigated the effect of fragmentation velocity and aggregate filling factor on the amount of ice on monomers residing at r = 10 AU. The locations where disk processes are fully coupled depend on both grain size and ice species. Monomers embedded in aggregates with fragmentation velocities of 1 m/s are able to undergo adsorption and photodesorption more often compared to a fragmentation velocity of 5 m/s or 10 m/s. Aggregates with a filling factor of $10^{-3}$ are able to accumulate ice 22 times faster on average than aggregates with a filling factor of 1. As different grain sizes are coupled through collisions and the grain ice consists of multiple ice species, it is difficult to isolate the locations where disk processes are fully coupled, necessitating the development of the SHAMPOO code. The processing of ice may not be spatially limited to dust aggregate surfaces for either fragile or porous aggregates.

arXiv comment30 pages, 24 figures, 4 tables, to appear in Astronomy & Astrophysics

References in corpus (61)

• Habitable Zones Around Main-Sequence Stars: New Estimates
• Rapid planetesimal formation in turbulent circumstellar discs
• Streaming Instabilities in Protoplanetary Disks
• Observations of the Icy Universe
• The UMIST database for astrochemistry 2012
• A simple model for the evolution of the dust population in protoplanetary disks
• Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
• Gas- and dust evolution in protoplanetary disks
• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? II. Introducing the bouncing barrier
• The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? I. Mapping the zoo of laboratory collision experiments
• Our astrochemical heritage
• Closed-form expressions for particle relative velocities induced by turbulence
• Forming the cores of giant planets from the radial pebble flux in protoplanetary discs
• Rapid Coagulation of Porous Dust Aggregates Outside the Snow Line: A Pathway to Successful Icy Planetesimal Formation
• Observations of Protoplanetary Disk Structures
• Radiation thermo-chemical models of protoplanetary disks I. Hydrostatic disk structure and inner rim
• Water, O2 and Ice in Molecular Clouds
• Consistent dust and gas models for protoplanetary disks. I. Disk shape, dust settling, opacities, and PAHs
• Gas and grain chemical composition in cold cores as predicted by the Nautilus 3-phase model
• The ancient heritage of water ice in the solar system
• Fluffy dust forms icy planetesimals by static compression
• The great dichotomy of the Solar System: small terrestrial embryos and massive giant planet cores
• Dust size distributions in coagulation/fragmentation equilibrium: Numerical solutions and analytical fits
• Astrochemistry and compositions of planetary systems
• Material enhancement in protoplanetary nebulae by particle drift through evaporation fronts
• Volatile carbon locking and release in protoplanetary disks. A study of TW Hya and HD 100546
• Ingredients for Solar-like Systems: protostar IRAS 16293-2422 B versus comet 67P/Churyumov-Gerasimenko
• Planet-forming material in a protoplanetary disc: the interplay between chemical evolution and pebble drift
• CO Depletion in Protoplanetary Disks: A Unified Picture Combining Physical Sequestration and Chemical Processing
• The Physics of Protoplanetesimal Dust Agglomerates. III. Compaction in Multiple Collisions
• Transport of CO in Protoplanetary Disks: Consequences of Pebble Formation, Settling, and Radial Drift
• Radiation thermo-chemical models of protoplanetary disks II. Line diagnostics
• C/O and Snowline Locations in Protoplanetary Disks: The Effect of Radial Drift and Viscous Gas Accretion
• Disk evolution, element abundances and cloud properties of young gas giant planets
• C2D Spitzer-IRS spectra of disks around T Tauri stars. IV. Crystalline silicates
• Retention of water in terrestrial magma oceans and carbon-rich early atmospheres
• Erosion and the limits to planetesimal growth
• Consistent dust and gas models for protoplanetary disks III. Models for selected objects from the FP7 DIANA project
• Tracing water vapor and ice during dust growth
• X-ray impact on the protoplanetary disks around T Tauri stars
• A panoptic model for planetesimal formation and pebble delivery
• Consistent dust and gas models for protoplanetary disks: II. Chemical networks and rates
• Residence Times of Particles in Diffusive Protoplanetary Disk Environments I. Vertical Motions
• Nitrogen isotope fractionation in protoplanetary disks
• Monte Carlo simulation of particle interactions at high dynamic range: Advancing beyond the Googol
• Radiation thermo-chemical models of protoplanetary discs. IV Modelling CO ro-vibrational emission from Herbig Ae discs
• Rapid Evolution of Volatile CO from the Protostellar Disk Stage to the Protoplanetary Disk Stage
• The Physics of Protoplanetesimal Dust Agglomerates II. Low Velocity Collision Properties
• Sticking of molecules on non-porous amorphous water ice
• Residence Times of Particles in Diffusive Protoplanetary Disk Environments II. Radial Motions and Applications to Dust Annealing
• A Lagrangian Model for Dust Evolution in Protoplanetary Disks: Formation of Wet and Dry Planetesimals at Different Stellar Masses
• Dust diffusion and settling in the presence of collisions: Trapping (sub)micron grains in the midplane
• Efficiency of radial transport of ices in protoplanetary disks probed with infrared observations: the case of CO${}_2$
• Chemical Feedbacks of Pebble Growth: Impacts on CO depletion and C/O ratios
• Mineralogy, structure and habitability of carbon-enriched rocky exoplanets: A laboratory approach
• On water delivery in the inner solar nebula: Monte Carlo simulations of forsterite hydration
• Consistent dust and gas models for protoplanetary disks IV. A panchromatic view of protoplanetary disks
• The Maximum Mass Solar Nebula and the early formation of planets
• The radial structure of planetary bodies formed by the streaming instability
• Circumplanetary disk ices. I. Ice formation vs. viscous evolution and grain drift