Probing the impact of varied migration and gas accretion rates for the formation of giant planets in the pebble accretion scenario
arXiv:2011.09146 · doi:10.1093/mnras/staa3629
Abstract
The final orbital position of growing planets is determined by their migration speed, which is essentially set by the planetary mass. Small mass planets migrate in type I migration, while more massive planets migrate in type II migration, which is thought to depend mostly on the viscous evolution rate of the disc. A planet is most vulnerable to inward migration before it reaches type II migration and can lose a significant fraction of its semi-major axis at this stage. We investigated the influence of different disc viscosities, the dynamical torque and gas accretion from within the horseshoe region as mechanisms for slowing down planet migration. Our study confirms that planets growing in low viscosity environments migrate less, due to the earlier gap opening and slower type II migration rate. We find that taking the gas accretion from the horseshoe region into account allows an earlier gap opening and this results in less inward migration of growing planets. Furthermore, this effect increases the planetary mass compared to simulations that do not take the effect of gas accretion from the horseshoe region. Moreover, combining the effect of the dynamical torque with the effect of gas accretion from the horseshoe region, significantly slows down inward migration. Taking these effects into account could allow the formation of cold Jupiters (a > 1 au) closer to the water ice line region compared to previous simulations that did not take these effects into account. We thus conclude that gas accretion from within the horseshoe region and the dynamical torque play crucial roles in shaping planetary systems.
arXiv comment13 pages, 8 figures, Accepted for publication in Monthly Notices of the Royal Astronomical Society (MNRAS)
References in corpus (72)
- Disk Frequencies and Lifetimes in Young Clusters
- Spectral Energy Distributions of T Tauri Stars With Passive Circumstellar Disks
- A low mass for Mars from Jupiter's early gas-driven migration
- The false positive rate of Kepler and the occurrence of planets
- Towards a Deterministic Model of Planetary Formation I: a Desert in the Mass and Semi Major Axis Distributions of Extra Solar Planets
- Rapid growth of gas-giant cores by pebble accretion
- Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
- Giant Planet Occurrence in the Stellar Mass-Metallicity Plane
- The Occurrence and Mass Distribution of Close-in Super-Earths, Neptunes, and Jupiters
- The effect of gas drag on the growth of protoplanets -- Analytical expressions for the accretion of small bodies in laminar disks
- On the width and shape of gaps in protoplanetary disks
- One or more bound planets per Milky Way star from microlensing observations
- Extrasolar planet population synthesis I: Method, formation tracks and mass-distance distribution
- Asteroids Were Born Big
- A torque formula for non-isothermal Type I planetary migration - II. Effects of diffusion
- Forming the cores of giant planets from the radial pebble flux in protoplanetary discs
- Separating gas-giant and ice-giant planets by halting pebble accretion
- Linear and nonlinear evolution of the vertical shear instability in accretion discs
- Toward a Deterministic Model of Planetary Formation V. Accumulation Near the Ice Line
- The Migration and Growth of Protoplanets in Protostellar Discs
- Pebble isolation mass --- scaling law and implications for the formation of super-Earths and gas giants
- The structure of protoplanetary discs around evolving young stars
- The TW Hya Disk at 870 microns: Comparison of CO and Dust Radial Structures
- Oligarchic growth of giant planets
- Planetesimal formation starts at the snow line
- The Exoplanet Mass-Ratio Function from the MOA-II Survey: Discovery of a Break and Likely Peak at a Neptune Mass
- Gas Flow Across Gaps in Protoplanetary Disks
- Planetesimal formation near the snowline: in or out?
- Radial migration of gap-opening planets in protoplanetary disks. I. The case of a single planet
- Toward a Deterministic Model of Planetary Formation VII: Eccentricity Distribution of Gas Giants
- On the Minimum Core Mass for Giant Planet Formation at Wide Separations
- Cavity opening by a giant planet in a protoplanetary disc and effects on planetary migration
- Planet heating prevents inward migration of planetary cores
- Modeling the Formation of Giant Planet Cores I: Evaluating Key Processes
- Extrasolar planet population synthesis III. Formation of planets around stars of different masses
- Impact Craters on Pluto and Charon Indicate a Deficit of Small Kuiper Belt Objects
- Vertical shear instability in accretion disc models with radiation transport
- Planet formation models: the interplay with the planetesimal disc
- Global Models of Planet Formation and Evolution
- New Jupiter and Saturn formation models meet observations
- Formation of dust-rich planetesimals from sublimated pebbles inside of the snow line
- A giant exoplanet orbiting a very low-mass star challenges planet formation models
- Dynamical corotation torques on low-mass planets
- How much does turbulence change the pebble isolation mass for planet formation?
- How planetary growth outperforms migration
- Impacts of planet migration models on planetary populations. Effects of saturation, cooling and stellar irradiation
- A reassessment of the in situ formation of close-in super-Earths
- HST measures of Mass Accretion Rates in the Orion Nebula Cluster
- Stellar irradiated discs and implications on migration of embedded planets II: accreting-discs
- Planet population synthesis driven by pebble accretion in cluster environments
- Transport and Accretion in Planet-Forming Disks
- Possible Stellar Metallicity Enhancements from the Accretion of Planets
- The opacity of grains in protoplanetary atmospheres
- Planet-Disc Interactions and Early Evolution of Planetary Systems
- Effects of Type I Migration on Terrestrial Planet Formation
- Planet formation and migration near the silicate sublimation front in protoplanetary disks
- Slowing Down Type II Migration of Gas Giants to Match Observational Data
- Prograde rotation of protoplanets by accretion of pebbles in a gaseous environment
- Connecting planet formation and astrochemistry: Refractory carbon depletion leading to super-stellar C/O in giant planetary atmospheres
- Gas Accretion onto a Protoplanet and Formation of a Gas Giant Planet
- Tidal Downsizing model. I. Numerical methods: saving giant planets from tidal disruptions
- Formation of solar system analogs I: looking for initial conditions through a population synthesis analysis
- Runaway gas accretion and gap opening versus type~I migration
- Influence of planetary gas accretion on the shape and depth of gaps in protoplanetary discs
- Planet Formation: An Optimized Population-Synthesis Approach
- Metallicity effect and planet mass function in pebble-based planet formation models
- Influence of grain growth on the thermal structure of protoplanetary discs
- Disentangling Hot Jupiters formation location from their chemical composition
- Are the observed gaps in protoplanetary discs caused by growing planets?
- The role of the initial surface density profiles of the disc on giant planet formation: comparing with observations
- Influence of migration models and thermal torque on planetary growth in the pebble accretion scenario
- Isotropic non-Gaussian -like toy models that reproduce the cosmic microwave background anomalies
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- How drifting and evaporating pebbles shape giant planets I: Heavy element content and atmospheric C/O
- How drifting and evaporating pebbles shape giant planets II: Volatiles and refractories in atmospheres
- Dry or water world? How the water contents of inner sub-Neptunes constrain giant planet formation and the location of the water ice line
- Understanding planet formation using microgravity experiments
- How drifting and evaporating pebbles shape giant planets III: The formation of WASP-77A b and Boötis b
- How to make giant planets via pebble accretion
- Composition of giant planets: the roles of pebbles and planetesimals
- Forming super-Mercuries: The role of stellar abundances
- How does accretion of planet-forming disks influence stellar abundances?
- Implications of Jupiter Inward Gas-Driven Migration for the Inner Solar System
- Planetary core formation via multi-species pebble accretion
- Planet population synthesis: The role of stellar encounters
- There is no disk mass budget problem of planet formation
- Simultaneous gas accretion onto a pair of giant planets: Impact on their final mass and on the protoplanetary disk structure
- The role of density perturbation on planet formation by pebble accretion
- How disc initial conditions sculpt the atmospheric composition of giant planets
- Constraining the formation history of the HAT-P-11 system by atmospheric abundances
- A High-Resolution Spectroscopic Survey of Directly Imaged Companion Hosts: II. Diversity in C/O Ratios among Host Stars
- Exploring the conditions for forming planetesimals by the streaming instability and planetary systems by pebble accretion