A panoptic model for planetesimal formation and pebble delivery

Abstract

The journey from dust particle to planetesimal involves physical processes acting on scales ranging from micrometers (the sticking and restructuring of aggregates) to hundreds of astronomical units (the size of the turbulent protoplanetary nebula). Considering these processes simultaneously is essential when studying planetesimal formation. We develop a novel, global, semi-analytical model for the evolution of the mass-dominating dust particles in a turbulent protoplanetary disk that takes into account the evolution of the dust surface density while preserving the essential characteristics of the porous coagulation process. This panoptic model is used to study the growth from submicron to planetesimal sizes in disks around Sun-like stars. For highly porous ices, unaffected by collisional fragmentation and erosion, rapid growth to planetesimal sizes is possible in a zone stretching out to $\sim 10\mathrm{AU}$ for massive disks. When porous coagulation is limited by erosive collisions, the formation of planetesimals through direct coagulation is not possible, but the creation of a large population of aggregates with Stokes numbers close to unity might trigger the streaming instability (SI). However, we find that reaching conditions necessary for SI is difficult and limited to dust-rich disks, (very) cold disks, or disks with weak turbulence. Behind the snow-line, porosity-driven aggregation of icy grains results in rapid ($\sim 10^4\mathrm{yr}$) formation of planetesimals. If erosive collisions prevent this, SI might be triggered for specific disk conditions. The numerical approach introduced in this work is ideally suited for studying planetesimal formation and pebble delivery simultaneously and will help build a coherent picture of the start of the planet formation process.

13 pages, 7 figures. Accepted for publication in Astronomy & Astrophysics

References in corpus (16)

• Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
• Protoplanetary Disk Structures in Ophiuchus
• Gas- and dust evolution in protoplanetary disks
• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• Closed-form expressions for particle relative velocities induced by turbulence
• Ring shaped dust accumulation in transition disks
• The stickiness of micrometer-sized water-ice particles
• The structure of protoplanetary discs around evolving young stars
• How to form planetesimals from mm-sized chondrules and chondrule aggregates
• Dust size distributions in coagulation/fragmentation equilibrium: Numerical solutions and analytical fits
• Dust coagulation in protoplanetary disks: porosity matters
• Dust sedimentation and self-sustained Kelvin-Helmholtz turbulence in protoplanetary disk mid-planes. I. Radially symmetric simulations
• Can dust coagulation trigger streaming instability?
• A representative particle approach to coagulation and fragmentation of dust aggregates and fluid droplets
• Erosion and the limits to planetesimal growth
• Challenges in Forming the Solar System's Giant Planet Cores via Pebble Accretion

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• Efficiency of radial transport of ices in protoplanetary disks probed with infrared observations: the case of CO${}_2$
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• Evolution of porous dust grains in protoplanetary discs -- I. Growing grains
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• Atmospheric Recyling of Volatiles by Pebble-Accreting Planets
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