Torques Induced by Scattered Pebble-flow in Protoplanetary Disks

Abstract

Fast inward migration of planetary cores is a common problem in the current planet formation paradigm. Even though dust is ubiquitous in protoplanetary disks, its dynamical role in the migration history of planetary embryos has not been assessed. In this Letter, we show that the scattered pebble-flow induced by a low-mass planetary embryo leads to an asymmetric dust-density distribution that is able to exert a net torque. By analyzing a large suite of multifluid hydrodynamical simulations addressing the interaction between the disk and a low-mass planet on a fixed circular orbit, and neglecting dust feedback onto the gas, we identify two different regimes, gas- and gravity-dominated, where the scattered pebble-flow results in almost all cases in positive torques. We collect our measurements in a first torque map for dusty disks, which will enable the incorporation of the effect of dust dynamics on migration into population synthesis models. Depending on the dust drift speed, the dust-to-gas mass ratio/distribution and the embryo mass, the dust-induced torque has the potential to halt inward migration or even induce fast outward migration of planetary cores. We thus anticipate that dust-driven migration could play a dominant role during the formation history of planets. Because dust torques scale with disk metallicity, we propose that dust-driven outward migration may enhance the occurrence of distant giant planets in higher-metallicity systems.

7 pages, 4 figures - Accepted for publication in ApJL

References in corpus (23)

• The NumPy array: a structure for efficient numerical computation
• A comparative study of disc-planet interaction
• Halting Type I planet migration in non-isothermal disks
• FARGO3D: A new GPU-oriented MHD code
• On the corotation torque in a radiatively inefficient disk
• Challenges in Planet Formation
• Hot super-Earths and giant planet cores from different migration histories
• Treating gravity in thin disk simulations
• Coorbital thermal torques on low-mass protoplanets
• Improved torque formula for low and intermediate mass planetary migration
• Saturated torque formula for planetary migration in viscous disks with thermal diffusion: recipe for protoplanet population synthesis
• Characterizing the variable dust permeability of planet-induced gaps
• An opening criterion for dust gaps in protoplanetary discs
• A thermodynamic view of dusty protoplanetary disks
• On the width and shape of the corotation region for low-mass planets
• Planetesimal-driven planet migration in the presence of a gas disk
• Numerical simulations of the type III migration:I. Disc model and convergence tests
• Eccentricity excitation and merging of planetary embryos heated by pebble accretion
• Dynamical friction on hot bodies in opaque, gaseous media
• The effect of planetary migration on the corotation resonance
• Long-term and large-scale hydrodynamical simulations of migrating planets
• Planetary Torque in 3D Isentropic Disks
• Type I Planet Migration in a Magnetized Disk. I. Effect of Large-Scale Vertical and Azimuthal Field Components

Cited by in corpus (32)

• Formation of planetary systems by pebble accretion and migration: How the radial pebble flux determines a terrestrial-planet or super-Earth growth mode
• Asymptotically stable numerical method for multispecies momentum transfer: gas and multifluid-dust test suite and implementation in FARGO3D
• Super-Earth masses sculpted by pebble isolation around stars of different masses
• How planetary growth outperforms migration
• Dust unveils the formation of a mini-Neptune planet in a protoplanetary ring
• Streaming Instability for Particle-Size Distributions
• Efficient planet formation by pebble accretion in ALMA rings
• Rapid Formation of Massive Planetary Cores in a Pressure Bump
• Predicting the observational signature of migrating Neptune-sized planets in low-viscosity disks
• Dusty disc-planet interaction with dust-free simulations
• Torques felt by solid accreting planets
• The 3D dust and opacity distribution of protoplanets in multi-fluid global simulations
• Vortex instabilities triggered by low-mass planets in pebble-rich, inviscid protoplanetary discs
• Quantifying the Impact of the Dust Torque on the Migration of Low-mass Planets
• Morphological signatures induced by dust back reaction in discs with an embedded planet
• Migrating Low-Mass Planets in Inviscid Dusty Protoplanetary Discs
• Pebble-driven migration of low-mass planets in the 2D regime of pebble accretion
• Growth after the streaming instability: The radial distance dependence of the planetary growth
• Extreme Pebble Accretion in Ringed Protoplanetary Discs
• Giant planet migration during the disc dispersal phase
• Model of a gap formed by a planet with fast inward migration
• Erosion driven size-redistribution of protoplanetary disk solids and the onset of streaming Instability and Pebble Accretion
• Dynamics of multiple protoplanets embedded in gas/pebble disks and its dependence on $\Sigma$ and $\nu$ parameters
• Binary planet formation by gas-assisted encounters of planetary embryos
• Increased isolation mass for pebble accreting planetary cores in pressure maxima of protoplanetary discs
• Planet formation: key mechanisms and global models
• Dust-void evolution driven by turbulent dust flux can induce runaway migration of Earth-mass planets
• Exploring the conditions for forming planetesimals by the streaming instability and planetary systems by pebble accretion
• Dust back-reaction on gas around planets modifies the cold thermal torque
• How stellar mass and disc size shape the formation and migration of super-Earths
• Single Fluid vs. Multifluid: Comparison between single fluid and multifluid dust models for disc planet interactions
• Not Just Gas: How Solid-Driven Torques Shaped the Migration of the Galilean Moons