Effect of nucleation on icy pebble growth in protoplanetary discs

Abstract

Solid particles in protoplanetary discs can grow by direct vapour deposition outside of ice lines. The presence of microscopic silicate particles may nevertheless hinder growth into large pebbles, since the available vapour is deposited predominantly on the small grains that dominate the total surface area. Experiments on heterogeneous ice nucleation, performed to understand ice clouds in the Martian atmosphere, show that the formation of a new ice layer on a silicate surface requires a substantially higher water vapour pressure than the deposition of water vapour on an existing ice surface. In this paper, we investigate how the difference in partial vapour pressure needed for deposition of vapour on water ice versus heterogeneous ice nucleation on silicate grains influences particle growth close to the water ice line. We developed and tested a dynamical 1D deposition and sublimation model, where we include radial drift, sedimentation, and diffusion in a turbulent protoplanetary disc. We find that vapour is deposited predominantly on already ice-covered particles, since the vapour pressure exterior of the ice line is too low for heterogeneous nucleation on bare silicate grains. Icy particles can thus grow to centimetre-sized pebbles in a narrow region around the ice line, whereas silicate particles stay dust-sized and diffuse out over the disc. The inhibition of heterogeneous ice nucleation results in a preferential region for growth into planetesimals close to the ice line where we find large icy pebbles. The suppression of heterogeneous ice nucleation on silicate grains may also be the mechanism behind some of the observed dark rings around ice lines in protoplanetary discs, as the presence of large ice pebbles outside ice lines leads to a decrease in the opacity there.

arXiv commentPublished in A&A

References in corpus (43)

• Rapid planetesimal formation in turbulent circumstellar discs
• Streaming Instabilities in Protoplanetary Disks
• First Results from High Angular Resolution ALMA Observations Toward the HL Tau Region
• The Disk Substructures at High Angular Resolution Project (DSHARP): I. Motivation, Sample, Calibration, and Overview
• Rapid growth of gas-giant cores by pebble accretion
• 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
• The effect of gas drag on the growth of protoplanets -- Analytical expressions for the accretion of small bodies in laminar disks
• Ringed Substructure and a Gap at 1 AU in the Nearest Protoplanetary Disk
• The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? I. Mapping the zoo of laboratory collision experiments
• Dust and Gas in the disc of HL Tauri: Surface density, dust settling, and dust-to-gas ratio
• Zonal Flows and Long-Lived Axisymmetric Pressure Bumps in Magnetorotational Turbulence
• The Mass and Size Distribution of Planetesimals Formed by the Streaming Instability. I. The Role of Self-Gravity
• Evidence of fast pebble growth near condensation fronts in the HL Tau protoplanetary disk
• The stickiness of micrometer-sized water-ice particles
• Sintering-induced Dust Ring Formation in Protoplanetary Disks: Application to the HL Tau Disk
• The structure of protoplanetary discs around evolving young stars
• Planetesimal formation starts at the snow line
• Dust size distributions in coagulation/fragmentation equilibrium: Numerical solutions and analytical fits
• Planetesimal formation near the snowline: in or out?
• Dust grain growth in rho-Ophiuchi protoplanetary disks
• Imaging the water-snow line during a protostellar outburst
• Material enhancement in protoplanetary nebulae by particle drift through evaporation fronts
• Three radial gaps in the disk of TW Hydrae imaged with SPHERE
• Initial mass function of planetesimals formed by the streaming instability
• Contacts of Water Ice in Protoplanetary Disks - Laboratory Experiments
• Towards Planetesimals in the Disk around TW Hya: 3.5 centimeter Dust Emission
• The radial dependence of pebble accretion rates: A source of diversity in planetary systems I. Analytical formulation
• On the Evolution of the Snow Line in Protoplanetary Discs
• Formation of dust-rich planetesimals from sublimated pebbles inside of the snow line
• Evidence for universality in the initial planetesimal mass function
• A representative particle approach to coagulation and fragmentation of dust aggregates and fluid droplets
• On the Commonality of 10-30AU Sized Axisymmetric Dust Structures in Protoplanetary Disks
• A Gap with a Deficit of Large Grains in the protoplanetary disk around TW Hya
• Collisions of CO${}_2$ Ice Grains in Planet Formation
• Monte Carlo simulation of particle interactions at high dynamic range: Advancing beyond the Googol
• Ice Grain Collisions in Comparison: CO${}_2$, H${}_2$O and their Mixtures
• Nebular water depletion as the cause of Jupiter's low oxygen abundance
• Nonsticky Ice at the Origin of the Uniformly Polarized Submillimeter Emission from the HL Tau Disk
• Spatially Extended Brackett Gamma Emission in the Environments of Young Stars
• ALMA observations of Elias 2-24: a protoplanetary disk with multiple gaps in the Ophiuchus Molecular Cloud
• FU Orionis outbursts, preferential recondensation of water ice, and the formation of giant planets

Cited by in corpus (30)

• Observations of Protoplanetary Disk Structures
• Astrochemistry and compositions of planetary systems
• Molecules with ALMA at Planet-forming Scales (MAPS) V: CO gas distributions
• Dust growth and evolution in protoplanetary disks
• Influence of sub- and super-solar metallicities on the compositions of solid planetary building blocks
• On the coexistence of the streaming instability and the vertical shear instability in protoplanetary disks
• The eccentricity distribution of giant planets and their relation to super-Earths in the pebble accretion scenario
• Understanding planet formation using microgravity experiments
• Pebble drift and planetesimal formation in protoplanetary discs with embedded planets
• Gravitoviscous protoplanetary disks with a dust component. III. Evolution of gas, dust, and pebbles
• Depletion of gaseous CO in protoplanetary disks by surface-energy-regulated ice formation
• The water-ice line as a birthplace of planets: Implications of a species-dependent dust fragmentation threshold
• On the stickiness of CO${}_2$ and H${}_2$O ice particles
• Into the thick of it: ALMA 0.45 mm observations of HL Tau at 2 au resolution
• How the origin of stars in the Galaxy impacts the composition of planetary building blocks
• Planetesimal formation around the snow line. II. Dust or pebbles?
• Gravitoviscous protoplanetary disks with a dust component. V. The dynamic model for freeze-out and sublimation of volatiles
• Collision fluctuations of lucky droplets with superdroplets
• Which stars can form planets: Planetesimal formation at low metallicities
• Sublimation of refractory minerals in the gas envelopes of accreting rocky planets
• Drifting inwards in protoplanetary discs I Sticking of chondritic dust at increasing temperatures
• The growth of super-Earths: the importance of a self-consistent treatment of disc structures and pebble accretion
• Fast formation of large ice pebbles after FU Orionis outbursts
• The Curie line in protoplanetary disks and the formation of Mercury-like planets
• Effects from different grades of stickiness between icy and silicate particles on carbon depletion in protoplanetary disks
• A formation pathway for terrestrial planets with moderate water content involving atmospheric-volatile recycling
• Constraining the formation history of the HAT-P-11 system by atmospheric abundances
• The Prospects for Hurricane-like Vortices in Protoplanetary Disks
• Icy Volatile Enhancements in Evolving Protoplanetary Disks
• Considering contact forces during the formation of planetesimals by gravitational collapse: mutual orbits, spin states, and shapes