Planetesimal formation around the snow line. II. Dust or pebbles?

Abstract

Around the snow line, icy pebbles and silicate dust may locally pile-up and form icy and rocky planetesimals via streaming instability and/or gravitational instability. We perform 1D diffusion-advection simulations that include the back-reaction to radial drift and diffusion of icy pebbles and silicate dust, ice sublimation, release of silicate dust, and their recycling through recondensation and sticking onto pebbles outside the snow line. We use a realistic description of the scale height of silicate dust obtained from Ida et al. and that of pebbles including the effects of a Kelvin-Helmholtz instability. We study the dependence of solid pile-up on distinct effective viscous parameters for turbulent diffusions in the radial and vertical directions (${\alpha }_{\mathrm{Dr}}$ and ${\alpha }_{\mathrm{Dz}}$) and for the gas accretion to the star (${\alpha }_{\mathrm{acc}}$) as well as that on the pebble-to-gas mass flux ($F_{p/g}$). We derive the sublimation width of drifting icy pebbles which is a critical parameter to characterize the pile-up of silicate dust and pebbles around the snow line. We identify a parameter space (in the $F_{p/g}-{\alpha }_{\mathrm{acc}}-{\alpha }_{\mathrm{Dz}}(={\alpha }_{\mathrm{Dr}})$ space) where pebbles no longer drift inward to reach the snow line due to the back-reaction that slows down radial velocity of pebbles. We show that the pile-up of solids around the snow line occurs in a broader range of parameters for ${\alpha }_{\mathrm{acc}}=10^{-3}$ than for ${\alpha }_{\mathrm{acc}}=10^{-2}$. Above a critical $F_{p/g}$ value, the runaway pile-up of silicate dust inside the snow line is favored for ${\alpha }_{\mathrm{Dr}}/{\alpha }_{\mathrm{acc}}\ll 1$, while that of pebbles outside the snow line is favored for ${\alpha }_{\mathrm{Dr}}/{\alpha }_{\mathrm{acc}}\sim 1$. Our results imply that a distinct evolutionary path could produce a diversity of outcomes in terms of planetesimal formation around the snow line.

arXiv comment18 pages, 6 Figures, 3 Figures in Appendix, accepted for publication in Astronomy & Astrophysics (A&A)

References in corpus (38)

• Streaming Instabilities in Protoplanetary Disks
• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• Wind-driven Accretion in Protoplanetary Disks. I: Suppression of the Magnetorotational Instability and Launching of the Magnetocentrifugal Wind
• Planetesimal Formation by Gravitational Instability
• Rapid Coagulation of Porous Dust Aggregates Outside the Snow Line: A Pathway to Successful Icy Planetesimal Formation
• Forming Planetesimals in Solar and Extrasolar Nebulae
• The Evolution of the Water Distribution in a Viscous Protoplanetary Disk
• Concentrating small particles in protoplanetary disks through the streaming instability
• Sintering-induced Dust Ring Formation in Protoplanetary Disks: Application to the HL Tau Disk
• Global simulations of protoplanetary disks with ohmic resistivity and ambipolar diffusion
• Planetesimal formation starts at the snow line
• How to form planetesimals from mm-sized chondrules and chondrule aggregates
• The great dichotomy of the Solar System: small terrestrial embryos and massive giant planet cores
• Planetesimal formation near the snowline: in or out?
• Magneto-thermal Disk Wind from Protoplanetary Disks
• Contacts of Water Ice in Protoplanetary Disks - Laboratory Experiments
• Evolution of Snow Line in Optically Thick Protoplanetary Disks: Effects of Water Ice Opacity and Dust Grain Size
• Magnetically driven accretion in protoplanetary discs
• The radial dependence of pebble accretion rates: A source of diversity in planetary systems I. Analytical formulation
• Formation of dust-rich planetesimals from sublimated pebbles inside of the snow line
• Super-Earth masses sculpted by pebble isolation around stars of different masses
• Cohesion of Amorphous Silica Spheres: Toward a Better Understanding of the Coagulation Growth of Silicate Dust Aggregates
• Diffusion and Concentration of Solids in the Dead Zone of a Protoplanetary Disk
• Sticking Properties of Silicates in Planetesimal Formation Revisited
• Vertical Shearing Instabilities in Radially Shearing Disks: The Dustiest Layers of the Protoplanetary Nebula
• Dust Transport in MRI Turbulent Disks: Ideal and Non-ideal MHD with Ambipolar Diffusion
• Global Modeling of Nebulae with Particle Growth, Drift and Evaporation Fronts. I: Methodology and Typical Results
• Two timescale dispersal of magnetized protoplanetary disks
• Requirements for gravitational collapse in planetesimal formation --- the impact of scales set by Kelvin-Helmholtz and nonlinear streaming instability
• Effect of nucleation on icy pebble growth in protoplanetary discs
• Effect of dust radial drift on viscous evolution of gaseous disk
• Formation of rocky and icy planetesimals inside and outside the snow line: Effects of diffusion, sublimation and back-reaction
• Magnetically Induced Disk Winds and Transport in the HL Tau Disk
• Formulas for Radial Transport in Protoplanetary Disks
• Gas accretion damped by dust back-reaction at the snow line
• Planetesimal formation around the snow line: I. Monte Carlo simulations of silicate dust pile-up in a turbulent disk
• Electron Heating and Saturation of Self-regulating Magnetorotational Instability in Protoplanetary Disks
• A "no-drift" runaway pile-up of pebbles in protoplanetary disks in which midplane turbulence increases with radius

Cited by in corpus (14)

• Forming pressure-traps at the snow-line to isolate isotopic reservoirs in the absence of a planet
• An inflationary disk phase to explain extended protoplanetary dust disks
• A global two-layer radiative transfer model for axisymmetric, shadowed protoplanetary disks
• Enrichment of Jupiter's atmosphere by late planetesimal bombardment
• Modeling the Evolution of Silicate/Volatile Accretion Discs around White Dwarfs
• Planetesimal formation around the snow line: I. Monte Carlo simulations of silicate dust pile-up in a turbulent disk
• Dust Accumulation near the Magnetospheric Truncation of Protoplanetary Discs around T Tauri Stars
• Solving for the 2D Water Snowline with Hydrodynamic Simulations. Emergence of gas outflow, water cycle and temperature plateau
• Constraints on PDS 70 b and c from the dust continuum emission of the circumplanetary discs considering in situ dust evolution
• A "no-drift" runaway pile-up of pebbles in protoplanetary disks in which midplane turbulence increases with radius
• Effective dust growth in laminar circumplanetary discs with magnetic wind-driven accretion
• Formation of super-Earths and mini-Neptunes from rings of planetesimals
• C/O ratios in self-gravitating protoplanetary discs with dust evolution
• A "no-drift" runaway pile-up of pebbles in protoplanetary disks II. Characteristics of the resulting planetesimal belt