Planet formation by pebble accretion in ringed disks

Abstract

Context: Pebble accretion is expected to be the dominant process for the formation of massive solid planets, such as the cores of giant planets and super-Earths. So, far, this process has been studied under the assumption that dust coagulates and drifts throughout the full protoplanetary disk. However, observations show that many disks are structured in rings that may be due to pressure maxima, preventing the global radial drift of the dust. Aims: We study how the pebble-accretion paradigm changes if the dust is confined in a ring. Results: Planet Type-I migration is stopped in a ring, but not necessarily at its center. If the entropy-driven corotation torque is desaturated, the planet is located in a region with a low density of dust, which severely limits its accretion rate. If instead the planet is near the ring's center, its accretion rate can be similar to the one it would have in a classic (ring-less) disk of equivalent dust density. However, the growth rate of the planet is limited by the diffusion of dust in the ring and the final planet's mass is bounded by the total ring's mass. The DSHARP rings are too far from the star to allow the formation of massive planets within the disk's lifetime. However, a similar ring rescaled to 5 AU could lead to the formation of a planet incorporating the full ring's mass in less than 1/2 My. Conclusions: The existence of rings may not be an obstacle to planet formation by pebble-accretion. However, for accretion to be effective the resting position of the planet has to be relatively near the ring's center and the ring needs to be not too far from the central star. The formation of planets in rings can explain the existence of giant planets with core masses smaller than the so-called pebble isolation mass.

Accepted for publication in Astronomy & Astrophysics

References in corpus (18)

• Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
• Gas- and dust evolution in protoplanetary disks
• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• Separating gas-giant and ice-giant planets by halting pebble accretion
• Comparing Jupiter interior structure models to Juno gravity measurements and the role of a dilute core
• Formation of planetary systems by pebble accretion and migration: How the radial pebble flux determines a terrestrial-planet or super-Earth growth mode
• New models of Jupiter in the context of Juno and Galileo
• Formation of planetary systems by pebble accretion and migration: Growth of gas giants
• Nine localised deviations from Keplerian rotation in the DSHARP circumstellar disks: Kinematic evidence for protoplanets carving the gaps
• 3D Radiation Non-ideal Magnetohydrodynamical Simulations Of The Inner Rim In Protoplanetary Disks
• The time evolution of dusty protoplanetary disc radii: observed and physical radii differ
• Planet formation and migration near the silicate sublimation front in protoplanetary disks
• Spontaneous ring formation in wind-emitting accretion discs
• Predicting the observational signature of migrating Neptune-sized planets in low-viscosity disks
• Exploring the conditions for forming cold gas giants through planetesimal accretion
• Influences of three-dimensional gas flow induced by protoplanets on pebble accretion --$\mathrm{I}$. shear regime
• Intermittent planet migration and the formation of multiple dust rings and gaps in protoplanetary disks
• Mapping the dark matter halo of early-type galaxy NGC 2974 through orbit-based models with combined stellar and cold gas kinematics

Cited by in corpus (23)

• Planetesimal rings as the cause of the Solar System's planetary architecture
• How dust fragmentation may be beneficial to planetary growth by pebble accretion
• Annular substructures in the transition disks around LkCa 15 and J1610
• Efficient planet formation by pebble accretion in ALMA rings
• Setting the Stage: Planet formation and Volatile Delivery
• How does the mass and activity history of the host star affect the population of low-mass planets?
• Migration processes in the Solar System and their role in the evolution of the Earth and planets
• Distant formation and differentiation of outer main belt asteroids and carbonaceous chondrite parent bodies
• The role of the drag force in the gravitational stability of dusty planet-forming disc -- II. Numerical simulations
• Migrating Low-Mass Planets in Inviscid Dusty Protoplanetary Discs
• Planet population synthesis: The role of stellar encounters
• Extreme Pebble Accretion in Ringed Protoplanetary Discs
• Ring Formation in Protoplanetary Disks Driven by an Eccentric Instability
• A Machine Learning model to infer planet masses from gaps observed in protoplanetary disks
• On the Estimation of Circumbinary Orbital Properties
• Accreting luminous low-mass planets escape from migration traps at pressure bumps
• The role of density perturbation on planet formation by pebble accretion
• On the interaction of pebble accreting embryos with the gaseous disc: importance of thermal forces
• Constraining giant planet formation with synthetic ALMA images of the Solar System's natal protoplanetary disk
• Increased isolation mass for pebble accreting planetary cores in pressure maxima of protoplanetary discs
• Planetesimal Growth in Evolving Protoplanetary Disks: Constraints from the Pebble Supply
• Eigenstates of Quasi-Keplerian Self-Gravitating Particle Discs
• Possible in situ formation of Uranus and Neptune via Pebble Accretion