Planetesimal formation at the gas pressure bump following a migrating planet I. Basic characteristics of the new formation model

Abstract

To avoid known difficulties in planetesimal formation such as the drift or fragmentation barriers, many scenarios have been proposed. However, in these scenarios, planetesimals form in general only at some specific locations in protoplanetary discs. On the other hand, it is generally assumed in planet formation models and population synthesis models, that planetesimals are broadly distributed in the protoplanetary disc. Here we propose a new scenario in which planetesimals can form in broad areas of the discs. Planetesimals form at the gas pressure bump formed by a first-generation planet (e.g. formed by pebble accretion) and the formation region spreads inward in the disc as the planet migrates. We use a simple 1D Lagrangian particle model to calculate the radial distribution of pebbles in the gas disc perturbed by a migrating embedded planet. We consider that planetesimals form by streaming instability at the points where the pebble-to-gas density ratio on the mid-plane becomes larger than unity. We also study the effect of some key parameters like the ones of the gas disc model, the pebble mass flux, the migration speed of the planet, and the strength of turbulence. We find that planetesimals form in wide areas of the discs provided the flux of pebbles is typical and the turbulence is not too strong. The planetesimal surface density depends on the pebble mass flux and the migration speed of the planet. The total mass of the planetesimals and the orbital position of the formation area depend strongly on the pebble mass flux. We also find that the profile of the planetesimal surface density and its slope can be estimated by very simple equations. We show that our new scenario can explain the formation of planetesimals in broad areas. The simple estimates we provide for the planetesimal surface density profile can be used as initial conditions for population synthesis models.

12 pages, 9 figures, 1 table, accepted for publication in Astronomy & Astrophysics

References in corpus (14)

• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• Separating gas-giant and ice-giant planets by halting pebble accretion
• Toward a Deterministic Model of Planetary Formation V. Accumulation Near the Ice Line
• Mass Estimates of a Giant Planet in a Protoplanetary Disk from the Gap Structures
• Four annular structures in a protostellar disk less than 500,000 years old
• Planetesimal formation around the snow line in MRI-driven turbulent protoplanetary disks
• Standing on the shoulders of giants: Trojan Earths and vortex trapping in low mass self-gravitating protoplanetary disks of gas and solids
• Formation of a disc gap induced by a planet: Effect of the deviation from Keplerian disc rotation
• Can dust coagulation trigger streaming instability?
• Including Dust Coagulation in Hydrodynamic Models of Protoplanetary Disks: Dust Evolution in the Vicinity of a Jupiter-mass Planet
• Planetesimal Population Synthesis: Pebble Flux Regulated Planetesimal Formation
• A Systematic Study of the Final Masses of Gas Giant Planets
• The impact of pebble flux regulated planetesimal formation on giant planet formation
• Pebble drift and planetesimal formation in protoplanetary discs with embedded planets

Cited by in corpus (12)

• How dust fragmentation may be beneficial to planetary growth by pebble accretion
• From Pebbles and Planetesimals to Planets and Dust: the Protoplanetary Disk--Debris Disk Connection
• Constraining planetesimal stirring: how sharp are debris disc edges?
• The fate of planetesimals formed at planetary gap edges
• The formation of wide exoKuiper belts from migrating dust traps
• Enrichment of Jupiter's atmosphere by late planetesimal bombardment
• The interplay between pebble and planetesimal accretion in population synthesis models and its role in giant planet formation
• Planetesimal and planet formation in transient dust traps
• Effective dust growth in laminar circumplanetary discs with magnetic wind-driven accretion
• The role of density perturbation on planet formation by pebble accretion
• Filament formation due to diffusive instabilities in dusty protoplanetary disks
• Planetesimal formation at the gas pressure bump following a migrating planet II. Effects of dust growth