Effect of Different Angular Momentum Transport mechanisms on the Distribution of Water in Protoplanetary Disks

Abstract

The snow line in a protoplanetary disk demarcates regions with H${}_2$O ice from regions with H${}_2$O vapor. Where a planet forms relative to this location determines how much water and other volatiles it forms with. Giant planet formation may be triggered at the water snow line if vapor diffuses outward and is cold-trapped beyond the snow line faster than icy particles can drift inward. In this study we investigate the distribution of water across the snow line, considering three different radial profiles of the turbulence parameter $\alpha (r)$, corresponding to three different angular momentum transport mechanisms. We consider the radial transport of water vapor and icy particles by diffusion, advection, and drift. We show that even for similar values of $\alpha$, the gradient of $\alpha$(r) across the snow line significantly changes the snow line location, the sharpness of the volatile gradient across the snow line, and the final water/rock ratio in planetary bodies. A profile of radially decreasing $\alpha$, consistent with transport by hydrodynamic instabilities plus magnetic disk winds, appears consistent with the distribution of water in the solar nebula, with monotonically-increasing radial water content and a diverse population of asteroids with different water content. We argue that $\Sigma (r)$ and water abundance $N_{{\mathrm{H}}_2\mathrm{O}}(r)/N_{{\mathrm{H}}_2}(r)$ are likely diagnostic of $\alpha (r)$ and thus the mechanism for angular momentum transport in inner disks.

Accepted to ApJ (Mar 7, 2019)

References in corpus (26)

• Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
• Protoplanetary Disk Structures in Ophiuchus
• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• Solar System evolution from compositional mapping of the asteroid belt
• Evidence of fast pebble growth near condensation fronts in the HL Tau protoplanetary disk
• The stickiness of micrometer-sized water-ice particles
• Global simulations of protoplanetary disks with ohmic resistivity and ambipolar diffusion
• A Three-Dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk using DCO${}^{+}$
• Analytical protostellar disk models 1: the effect of internal dissipation and surface irradiation on the structure of disks and the location of the snow line around Sun-like stars
• Dust size distributions in coagulation/fragmentation equilibrium: Numerical solutions and analytical fits
• Grain Retention and Formation of Planetesimals near the Snow Line in MRI-driven Turbulent Protoplanetary Disks
• Imaging the water-snow line during a protostellar outburst
• Evolution of Protoplanetary Discs with Magnetically Driven Disc Winds
• Hall-effect Controlled Gas Dynamics in Protoplanetary Disks: II. Full 3D Simulations toward the Outer Disk
• Convective Overstability in radially stratified accretion disks under thermal relaxation
• Ice Lines, Planetesimal Composition and Solid Surface Density in the Solar Nebula
• Vertical shear instability in accretion disc models with radiation transport
• Formation of dust-rich planetesimals from sublimated pebbles inside of the snow line
• Can dead zones create structures like a transition disk?
• Radiation Hydrodynamical Turbulence In Protoplanetary Disks: Numerical Models and Observational Constraints
• Convective overstability in accretion disks: 3D linear analysis and nonlinear saturation
• Protoplanetary Disks as (Possibly) Viscous Disks
• Turbulent diffusion in protoplanetary discs: the effect of an imposed magnetic field
• Candidate Water Vapor Lines to Locate the H${}_2$O Snowline through High-Dispersion Spectroscopic Observations II. The Case of a Herbig Ae Star
• Pebble Accretion in Turbulent Protoplanetary Disks
• FUV Irradiation and the Heat Signature of Accretion in Protoplanetary Disk Atmospheres

Cited by in corpus (4)

• Hybrid accretion of carbonaceous chondrites by radial transport across the Jupiter barrier
• Resolved molecular line observations reveal an inherited molecular layer in the young disk around TMC1A
• Global Modeling of Nebulae With Particle Growth, Drift, and Evaporation Fronts. III. Redistribution of Refractories and Volatiles
• Models and Observational Predictions of Dust Traps in Protoplanetary Discs