Pebble accretion in class 0/I YSOs as a possible pathway for early planet formation

Abstract

Recent theoretical works suggest that the pebble accretion process is important for planet formation in protoplanetary disks, because it accelerates the growth of planetary cores. While several observations reveal axisymmetric sharp gaps in very young disks, which may be indicative of the existence of planets. We investigate the possibility of planet formation via pebble accretion in much earlier phases, the gravitationally unstable disks of class 0/I young stellar objects. We find that under the conditions of the class 0/I disks, the pebble accretion timescales can be shorter compared to the typical protoplanetary disks due to larger gas and dust accretion rate, but also find that the accretion timescale is not always a decreasing function of the gas accretion rate. By using estimated accretion timescales, we give a required initial mass to form cores of gas giants within the lifetime of class 0/I phases under several parameters, such as radial distances from the host star, gas accretion rates, and dust-to-gas mass ratio. In the most optimistic case, for example the dust-to-gas mass ratio is $f=3f_{\mathrm{solar}}$, $\sim 10^{-4}{M}_{\oplus }$ objects at 10 au can grow to $10M_{\oplus }$ cores during the typical lifetime of the class 0/I phases, 0.5 Myr.

15 pages, 10 figures, accepted for publication in MNRAS

References in corpus (17)

• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• Closed-form expressions for particle relative velocities induced by turbulence
• Separating gas-giant and ice-giant planets by halting pebble accretion
• Gaps, Rings, and Non-Axisymmetric Structures in Protoplanetary Disks - From Simulations to ALMA Observations
• The properties of brown dwarfs and low-mass hydrogen-burning stars formed by disc fragmentation
• The stickiness of micrometer-sized water-ice particles
• Grain Retention and Formation of Planetesimals near the Snow Line in MRI-driven Turbulent Protoplanetary Disks
• Mass Estimates of a Giant Planet in a Protoplanetary Disk from the Gap Structures
• Radiation Magnetohydrodynamic Simulations of Protostellar Collapse: Non-Ideal Magnetohydrodynamic Effects and Early Formation of Circumstellar Disks
• Can giant planets form by gravitational fragmentation of discs?
• 3D MHD Simulations of Planet Migration in Turbulent Stratified Disks
• Ice Grain Collisions in Comparison: CO${}_2$, H${}_2$O and their Mixtures
• Effects of radiation transfer on the structure of self-gravitating disks, their fragmentation and evolution of the fragments
• On the filtering and processing of dust by planetesimals 1. Derivation of collision probabilities for non-drifting planetesimals
• ALMA observations of Elias 2-24: a protoplanetary disk with multiple gaps in the Ophiuchus Molecular Cloud
• Non-linear Development of Secular Gravitational Instability in Protoplanetary Disks
• A photo-evaporative gap in the closest planet forming disc

Cited by in corpus (4)

• How dust fragmentation may be beneficial to planetary growth by pebble accretion
• Exploring the conditions for forming cold gas giants through planetesimal accretion
• The composition of hot Jupiter atmospheres assembled within chemically evolved protoplanetary discs
• Influences of three-dimensional gas flow induced by protoplanets on pebble accretion --$\mathrm{I}$. shear regime