Toward a Population Synthesis of Disks and Planets I. Evolution of Dust with Entrainment in Winds and Radiation Pressure

Abstract

Millimeter astronomy provides valuable information on the birthplaces of planetary systems. In order to compare theoretical models with observations, the dust component has to be carefully calculated. Here, we aim to study the effects of dust entrainment in photoevaporative winds and the ejection and drag of dust due to effects caused by radiation from the central star. We improved and extended the existing implementation of a two-population dust and pebble description in the global Bern/Heidelberg planet formation and evolution model. Modern prescriptions for photoevaporative winds were used and we account for settling and advection of dust when calculating entrainment rates. In order to prepare for future population studies with varying conditions, we explore a wide range of disk-, photoevaporation-, and dust-parameters. We find that if dust can grow to pebble sizes, that is, if they are resistant to fragmentation or turbulence is weak, drift dominates and the entrained mass is small but larger than under the assumption of no vertical advection of grains with the gas flow. For the case of fragile dust shattering at velocities of 1 m/s - as indicated in laboratory experiments -, an order of magnitude more dust is entrained which becomes the main dust removal process. Radiation pressure effects disperse massive, dusty disks on timescales of a few 100 Myr. These results highlight the importance of dust entrainment in winds as a solid mass removal process. Furthermore, this model extension lies the basis for future statistical studies of planet formation in their birth environment.

arXiv commentAccepted for publication in A&A

References in corpus (68)

• Disk Frequencies and Lifetimes in Young Clusters
• Spectral Energy Distributions of T Tauri Stars With Passive Circumstellar Disks
• New evolutionary models for pre-main sequence and main sequence low-mass stars down to the hydrogen-burning limit
• Rapid planetesimal formation in turbulent circumstellar discs
• Using FU Orionis Outbursts to Constrain Self-Regulated Protostellar Disk Models
• A simple model for the evolution of the dust population in protoplanetary disks
• Gas- and dust evolution in protoplanetary disks
• 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
• ALMA Survey of Lupus Protoplanetary Disks I: Dust and Gas Masses
• Wind-driven Accretion in Protoplanetary Disks. I: Suppression of the Magnetorotational Instability and Launching of the Magnetocentrifugal Wind
• X-Shooter spectroscopy of young stellar objects in Lupus: Accretion properties of class II and transitional objects
• Closed-form expressions for particle relative velocities induced by turbulence
• The Birth Environment of the Solar System
• A Steeper than Linear Disk Mass-Stellar Mass Scaling Relation
• X-Shooter spectroscopy of young stellar objects: IV -- Accretion in low-mass stars and sub-stellar objects in Lupus
• The Disk Substructures at High Angular Resolution Project (DSHARP) VI: Dust trapping in thin-ringed protoplanetary disks
• ALMA Survey of Lupus Protoplanetary Disks II: Gas Disk Radii
• The XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST)
• An ALMA Survey of Protoplanetary Disks in the $\sigma$ Orionis Cluster
• The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. A Statistical Characterization of Class 0 and I Protostellar Disks
• Evolution of protoplanetary disks: Constraints from DM Tauri and GM Aurigae
• On the theory of disc photoevaporation
• Dust Evolution and the Formation of Planetesimals
• ALMA Observations of Circumstellar Disks in the Upper Scorpius OB Association
• Statistical properties of exoplanets II. Metallicity, orbital parameters, and space velocities
• A Three-Dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk using DCO${}^{+}$
• Protoplanetary disc evolution and dispersal: the implications of X-ray photoevaportion
• Dust size distributions in coagulation/fragmentation equilibrium: Numerical solutions and analytical fits
• Magneto-thermal Disk Wind from Protoplanetary Disks
• The New Generation Planetary Population Synthesis (NGPPS). I. Bern global model of planet formation and evolution, model tests, and emerging planetary systems
• Contacts of Water Ice in Protoplanetary Disks - Laboratory Experiments
• The Coupled Physical Structure of Gas and Dust in the IM Lup Protoplanetary Disk
• X-ray irradiated protoplanetary disk atmospheres II: Predictions from models in hydrostatic equilibrium
• X-Shooter study of accretion in Chamaeleon I: II. A steeper increase of accretion with stellar mass for very low mass stars?
• Convective Overstability in radially stratified accretion disks under thermal relaxation
• The dispersal of protoplanetary discs I: A new generation of X-ray photoevaporation models
• Viscous diffusion and photoevaporation of stellar disks
• External photoevaporation of protoplanetary discs in sparse stellar groups: the impact of dust growth
• X-Shooter study of accretion in Chamaeleon I
• Global MHD simulations of stratified and turbulent protoplanetary discs. II. Dust settling
• Circumstellar Disk Lifetimes In Numerous Galactic Young Stellar Clusters
• The FRIED grid of mass loss rates for externally irradiated protoplanetary discs
• Turbulence sets the length scale for planetesimal formation: Local 2D simulations of streaming instability and planetesimal formation
• The efficiency of dust trapping in ringed proto-planetary discs
• The evolution of dust in discs influenced by external photoevaporation
• Sticking Properties of Silicates in Planetesimal Formation Revisited
• Planetesimal Population Synthesis: Pebble Flux Regulated Planetesimal Formation
• Vertical structure of debris discs
• The dispersal of protoplanetary discs. II: Photoevaporation models with observationally derived irradiating spectra
• Requirements for gravitational collapse in planetesimal formation --- the impact of scales set by Kelvin-Helmholtz and nonlinear streaming instability
• The first multi-dimensional view of mass loss from externally FUV irradiated protoplanetary discs
• Dust growth in protoplanetary disks - a comprehensive experimental/theoretical approach
• Growing and Trapping Pebbles with Fragile Collisions of Particles in Protoplanetary Disks
• Dust Distribution in Gas Disks. A Model for the Ring Around HR 4796A
• The imprint of photoevaporation on edge-on discs
• The impact of pebble flux regulated planetesimal formation on giant planet formation
• Surface Outflow in Optically Thick Dust Disks by the Radiation Pressure
• Radiation pressure clear-out of dusty photoevaporating discs
• Large gaps and high accretion rates in photoevaporative transition disks with a dead zone
• Modeling the delivery of dust from discs to ionized winds
• Influence of grain growth on the thermal structure of protoplanetary discs
• Dust entrainment in photoevaporative winds: The impact of X-rays
• Gas accretion damped by dust back-reaction at the snow line
• Dust delivery and entrainment in photoevaporative winds
• Linking planetesimal and dust content in protoplanetary disks via a local toy model
• On the maximum grain size entrained by photoevaporative winds
• Dust entrainment in photoevaporative winds: Synthetic observations of transition disks

Cited by in corpus (5)

• Planet formation via pebble accretion in externally photoevaporating discs
• Towards a population synthesis of discs and planets. II. Confronting disc models and observations at the population level
• Vertical shear instability in two-moment radiation-hydrodynamical simulations of irradiated protoplanetary disks I. Angular momentum transport and turbulent heating
• TriPoD: Tri-Population size distributions for Dust evolution. Coagulation in vertically integrated hydrodynamic simulations of protoplanetary disks
• Effects of Stellar X-ray Photoevaporation on Planetesimal Formation via the Streaming Instability