Final Masses of Giant Planets II: Jupiter Formation in a Gas-Depleted Disk

Abstract

Firstly, we study the final masses of giant planets growing in protoplanetary disks through capture of disk gas, by employing an empirical formula for the gas capture rate and a shallow disk gap model, which are both based on hydrodynamical simulations. The shallow disk gaps cannot terminate growth of giant planets. For planets less massive than 10 Jupiter masses, their growth rates are mainly controlled by the gas supply through the global disk accretion, rather than their gaps. The insufficient gas supply compared with the rapid gas capture causes a depletion of the gas surface density even at the outside of the gap, which can create an inner hole in the protoplanetary disk. Our model can also predict the depleted gas surface density in the inner hole for a given planet mass. Secondly, our findings are applied to the formation of our solar system. For the formation of Jupiter, a very low-mass gas disk with a few or several Jupiter masses is required at the beginning of its gas capture because of the non-stopping capture. Such a low-mass gas disk with sufficient solid material can be formed through viscous evolution from an initially $\sim$10AU-sized compact disk with the solar composition. By the viscous evolution with a moderate viscosity of $\alpha \sim 10^{-3}$, most of disk gas accretes onto the sun and a widely spread low-mass gas disk remains when the solid core of Jupiter starts gas capture at $t\sim 10^7$ yrs. The depletion of the disk gas is suitable for explaining the high metallicity in giant planets of our solar system. A very low-mass gas disk also provides a plausible path where type I and II planetary migrations are both suppressed significantly. In particular, we also show that the type II migration of Jupiter-size planets becomes inefficient because of the additional gas depletion due to the rapid gas capture by themselves.

36 pages, 10 figures, submitted to ApJ

References in corpus (12)

• 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
• The Migration of Gap-Opening Planets is not Locked to Viscous Disk Evolution
• Migration of massive planets in accreting disks
• Formation of a disc gap induced by a planet: Effect of the deviation from Keplerian disc rotation
• Evolution of Migrating Planets Undergoing Gas Accretion
• Massive planet migration: Theoretical predictions and comparison with observations
• On the gap-opening criterion of migrating planets in protoplanetary disks
• A Systematic Study of the Final Masses of Gas Giant Planets
• On the Viability of the Magnetorotational Instability in Circumplanetary Disks
• Dispersal of protoplanetary disks by central wind stripping
• Magnetic fields in gaps surrounding giant protoplanets

Cited by in corpus (83)

• The imprint of exoplanet formation history on observable present-day spectra of hot Jupiters
• Evidence of an Upper Bound on the Masses of Planets and its Implications for Giant Planet Formation
• How planetary growth outperforms migration
• Gap Opening in 3D: Single Planet Gaps
• WASP-107b's density is even lower: a case study for the physics of planetary gas envelope accretion and orbital migration
• Keck/NIRC2 $L$'-Band Imaging of Jovian-Mass Accreting Protoplanets around PDS 70
• Revelations on Jupiter's Formation, Evolution and Interior: Challenges from Juno Results
• The Boundary between Gas-rich and Gas-poor Planets
• Accretion Properties of PDS 70b with MUSE
• The origin of the high metallicity of close-in giant exoplanets: Combined effect of the resonant and aerodynamic shepherding
• Slowing Down Type II Migration of Gas Giants to Match Observational Data
• Quasi-static contraction during runaway gas accretion onto giant planets
• Outflow Bubbles from Compact Binary Mergers Embedded in Active Galactic Nuclei: Cavity Formation and the Impact on Electromagnetic Counterparts
• Creating the Radius Gap without Mass Loss
• Planet Formation in Disks with Inclined Binary Companions: Can Primordial Spin-Orbit Misalignment be Produced?
• Predicted diversity in water content of terrestrial exoplanets orbiting M dwarfs
• Clouds of Fluffy Aggregates: How They Form in Exoplanetary Atmospheres and Influence Transmission Spectra
• Final Masses of Giant Planets III: Effect of Photoevaporation and a New Planetary Migration Model
• The accretion of migrating giant planets
• Capture of Solids by Growing Proto-gas Giants: Effects of Gap Formation and Supply-limited Growth
• Can stellar-mass black hole growth disrupt disks of active galactic nuclei? The role of mechanical feedback
• The Galilean Satellites Formed Slowly from Pebbles
• Meridional Circulation of Dust and Gas in the Circumstellar Disk: Delivery of Solids onto the Circumplanetary Region
• Influence of planetary gas accretion on the shape and depth of gaps in protoplanetary discs
• The End of Runaway: How Gap Opening Limits the Final Masses of Gas Giants
• Accreting protoplanets: Spectral signatures and magnitude of gas and dust extinction at H alpha
• Envelopes of embedded super-Earths II. Three-dimensional isothermal simulations
• Terrestrial planet formation: Dynamical shake-up and the low mass of Mars
• Rapid Formation of Jupiter and Wide-Orbit Exoplanets in Disks with Pressure Bumps
• wdwarfdate: A Python Package to Derive Bayesian Ages of White Dwarfs
• How Consumption and Repulsion Set Planetary Gap Depths and the Final Masses of Gas Giants
• The Origin of Heavy Element Content Trend in Giant Planets via Core Accretion
• The maximum accretion rate of a protoplanet: how fast can runaway be?
• Spin Evolution of Stellar-mass Black Holes Embedded in AGN disks: Orbital Eccentricity Produces Retrograde Circumstellar Flows
• Accretion of Gas Giants Constrained by the Tidal Barrier
• The Role of Outflow Feedback on Accretion of Compact Objects in Accretion Disk of Active Galactic Nuclei
• N-body simulations of planet formation via pebble accretion II. How various giant planets form
• The Spiral Wave Instability Induced by a Giant Planet: I. Particle Stirring in the Inner Regions of Protoplanetary Disks
• Breaking the centrifugal barrier to giant planet contraction by magnetic disc braking
• TOI-216: Resonant Constraints on Planet Migration
• Retention of Long-Period Gas Giant Planets: Type II Migration Revisited
• ALMA observations require slower Core Accretion runaway growth
• Unified simulations of planetary formation and atmospheric evolution: Effects of pebble accretion, giant impacts, and stellar irradiations on super-Earth formation
• Satellitesimal Formation via Collisional Dust Growth in Steady Circumplanetary Disks
• The Endgame of Gas Giant Formation: Accretion Luminosity and Contraction Post-Runaway
• Sequential giant planet formation initiated by disc substructure
• Planet formation throughout the Milky Way: Planet populations in the context of Galactic chemical evolution
• Chemical footprints of giant planet formation. Role of planet accretion in shaping the C/O ratio of protoplanetary disks
• Unified simulations of planetary formation and atmospheric evolution II: Rapid disk clearing by photoevaporation yields low-mass super-Earth atmospheres
• Eccentric gap induced by a super-Jupiter mass planet
• A Theoretical Framework for the Mass Distribution of Gas Giant Planets forming through the Core Accretion Paradigm
• A localized kinematic structure detected in atomic carbon emission spatially coincident with a proposed protoplanet in the HD 163296 disk
• Radial migration of gap-opening planets in protoplanetary disks. II. The case of a planet pair
• Formation of Planetary Populations II: Effects of Initial Disk Size & Radial Dust Drift
• Formation of wide-orbit giant planets in protoplanetary disks with a decreasing pebble flux
• Multiple Populations of Extrasolar Gas Giants
• Constraining accretion signatures of exoplanets in the TW Hya transitional disk
• Analytic Approach to the Late Stages of Giant Planet Formation
• Super-Earths as Failed Cores in Orbital Migration Traps
• Can Large-Scale Migration Explain the Giant Planet Occurrence Rate?
• On the suppression of giant planet formation around low-mass stars in clustered environments
• Feasibility of detecting and characterizing embedded low-mass giant planets in gaps in the VIS/NIR wavelength range
• A low accretion efficiency of planetesimals formed at planetary gap edges
• Magnetic Fields and Accreting Giant Planets around PDS 70
• OGLE-2013-BLG-0911Lb: A Secondary on the Brown-Dwarf Planet Boundary around an M-dwarf
• A limit on gas accretion onto close-in super-Earth cores from disk accretion
• Delivery of gas onto the circumplanetary disk of giant planets: Planetary-mass dependence of the source region of accreting gas and mass accretion rate
• Dust rings as a footprint of planet formation in a protoplanetary disk
• Simultaneous gas accretion onto a pair of giant planets: Impact on their final mass and on the protoplanetary disk structure
• The Heavy-element Content Trend of Planets: A Tracer of their Formation Sites
• Feedback-limited Accretion: Variable Luminosity from Growing Planets
• Architecture of three-planet systems predicted from the observed protoplanetary disk of HL Tau
• Super-Earth formation in systems with cold giants
• Testing planet formation from the ultraviolet to the millimeter
• On the origin of transition disk cavities: Pebble-accreting protoplanets vs Super-Jupiters
• Emerging population of gap-opening planets around type-A stars -- Long-term evolution of the forming planets around HD 163296
• Estimating the depth of gaps opened by planets in eccentric orbit
• Solid Accretion onto Neptune-Mass Planets I: In-Situ Accretion and Constraints from the metallicity of Uranus and Neptune
• Architecture of planetary systems predicted from protoplanetary disks observed with ALMA II: evolution outcomes and dynamical stability
• Long-term evolution of the temperature structure in magnetized protoplanetary disks and its implication for the dichotomy of planetary composition
• Oxygen Isotope Exchange Between Molten Silicate Spherules and Ambient Water Vapor with Nonzero Relative Velocity: Implication for Chondrule Formation Environment
• Planetesimal formation at the gas pressure bump following a migrating planet II. Effects of dust growth
• A break in planet occurrence near the pebble isolation mass should be observable by the Roman microlensing survey