The accretion of migrating giant planets

Abstract

Most studies concerning the growth and evolution of massive planets focus either on their accretion or their migration only. In this work we study both processes concurrently to investigate how they might mutually affect each other. We modeled a 2-dimensional disk with a steady accretion flow onto the central star and embed a Jupiter mass planet at 5.2 au. The disk is locally isothermal and viscosity is modeled using a constant $\alpha$. The planet is held on a fixed orbit for a few hundred orbits to allow the disk to adapt and carve a gap. After this period, the planet is released and free to move according to the gravitational interaction with the gas disk. The mass accretion onto the planet is modeled by removing a fraction of gas from the inner Hill sphere, and the removed mass and momentum can be added to the planet. Our results show that a fast migrating planet is able to accrete more gas than a slower migrating planet. Utilizing a tracer fluid we analyzed the origin of the accreted gas which comes predominantly originating from the inner disk for a fast migrating planet. In case of slower migration the fraction of gas from the outer disk increases. We also found that even for very high accretion rates in some cases gas crosses the planetary gap from the inner to the outer disk. Our simulations show that the crossing of gas changes during the migration process as the migration rate slows down. Therefore classical type II migration where the planet migrates with the viscous drift rate and no gas crosses the gap is no general process but may only occur for special parameters and at a certain time during the orbital evolution of the planet.

arXiv comment9 pages, 14 figures, accepted for publication in A&A

References in corpus (16)

• Planet-disk interaction and orbital evolution
• Disk Accretion Onto High-Mass Planets
• Mass Flow and Accretion through gaps in Accretion Discs
• The Migration and Growth of Protoplanets in Protostellar Discs
• Orbital Migration and Mass Accretion of Protoplanets in 3D Global Computations with Nested Grids
• How Empty are Disk Gaps Opened by Giant Planets?
• Nested-grid calculations of disk-planet interaction
• The Migration of Gap-Opening Planets is not Locked to Viscous Disk Evolution
• Migration of massive planets in accreting disks
• Dynamical corotation torques on low-mass planets
• Final Masses of Giant Planets II: Jupiter Formation in a Gas-Depleted Disk
• A Systematic Study of the Final Masses of Gas Giant Planets
• Do Giant Planets Survive Type II Migration?
• Recent developments in planet migration theory
• Giant Planet Migration in Viscous Power-Law Discs
• Migration of accreting planets in radiative discs from dynamical torques

Cited by in corpus (38)

• New Horizons for Fundamental Physics with LISA
• The Quest for Dual and Binary Supermassive Black Holes: A Multi-Messenger View
• Formation of planetary systems by pebble accretion and migration: Growth of gas giants
• On the orbital evolution of supermassive black hole binaries with circumbinary accretion discs
• An Ideal Testbed for Planet-disk Interaction: Two Giant Protoplanets in Resonance Shaping the PDS 70 Protoplanetary Disk
• Probing gas disc physics with LISA: simulations of an intermediate mass ratio inspiral in an accretion disc
• Toward a new paradigm for Type II migration
• Quasi-static contraction during runaway gas accretion onto giant planets
• Dry or water world? How the water contents of inner sub-Neptunes constrain giant planet formation and the location of the water ice line
• Final Masses of Giant Planets III: Effect of Photoevaporation and a New Planetary Migration Model
• Effect of wind-driven accretion on planetary migration
• Global 3D radiation-hydrodynamic simulations of gas accretion: The opacity dependent growth of Saturn-mass planets
• Three-dimensional Global Simulations of Type-II Planet-disk Interaction with a Magnetized Disk Wind: I. Magnetic Flux Concentration and Gap Properties
• How Consumption and Repulsion Set Planetary Gap Depths and the Final Masses of Gas Giants
• Accretion of Gas Giants Constrained by the Tidal Barrier
• The comparative effect of FUV, EUV and X-ray disc photoevaporation on gas giant separations
• Is There a Temperature Limit in Planet Formation at 1000 K?
• Retention of Long-Period Gas Giant Planets: Type II Migration Revisited
• The diverse lives of massive protoplanets in self-gravitating discs
• A Theoretical Framework for the Mass Distribution of Gas Giant Planets forming through the Core Accretion Paradigm
• Constraining the initial planetary population in the gravitational instability model
• Radial migration of gap-opening planets in protoplanetary disks. II. The case of a planet pair
• Planet formation in the PDS 70 system: Constraining the atmospheric chemistry of PDS 70b and c
• A brief overview of planet formation
• Termination of an inward migration of a gap-opening planet triggered by dust feedback
• Model of a gap formed by a planet with fast inward migration
• Dust rings as a footprint of planet formation in a protoplanetary disk
• Non-steady-state long-term evolution of supermassive black hole binaries surrounded by accretion discs
• Simultaneous gas accretion onto a pair of giant planets: Impact on their final mass and on the protoplanetary disk structure
• Migration jumps of planets in transition disks
• Migration of Accreting Planets and Black Holes in Disks
• Photoevaporation Does Not Create a Pileup of Giant Planets at 1 AU
• Feedback-limited Accretion: Variable Luminosity from Growing Planets
• On the importance of wave planet interactions for the migration of two super-Earths embedded in a protoplanetary disk
• Calibrated Gas Accretion and Orbital Migration of Protoplanets in 1D Disc Models
• The interplay between forming planets and photoevaporating discs II: Wind-driven gas redistribution
• Adapting a gas accretion scenario for migrating planets in FARGO3D
• Adapting a solid accretion scenario for migrating planets in FARGO3D