Dust accretion onto high-mass planets

Abstract

We study the accretion of dust particles of various sizes onto embedded massive gas giant planets, where we take into account the structure of the gas disk due to the presence of the planet. The accretion rate of solids is important for the structure of giant planets: it determines the growth rate of the solid core that may be present as well as their final enrichment in solids. We use the RODEO hydrodynamics solver to solve the flow equations for the gas, together with a particle approach for the dust. The solver for the particles' equations of motion is implicit with respect to the drag force, which allows us to treat the whole dust size spectrum. We find that dust accretion is limited to the smallest particle sizes. The largest particles get trapped in outer mean-motion resonances with the planet, while particles of intermediate size are pushed away from the orbit of the planet by the density structure in the gas disk. Only particles smaller than approximately s_max =10 micron may accrete on a planet with the mass of Jupiter. For a ten times less massive planet s_max=100 micron. The strongly reduced accretion of dust makes it very hard to enrich a newly formed giant planet in solids.

15 pages, 18 figures, accepted for publication in A&A

References in corpus (17)

• Dust coagulation in protoplanetary disks: a rapid depletion of small grains
• Planetesimal Formation by Gravitational Instability
• Radial Flow of Dust Particles in Accretion Disks
• Disk Accretion Onto High-Mass Planets
• Mass Flow and Accretion through gaps in Accretion Discs
• Eccentricity Evolution for Planets in Gaseous Disks
• Orbital Migration and Mass Accretion of Protoplanets in 3D Global Computations with Nested Grids
• Gas Flow Across Gaps in Protoplanetary Disks
• Disk eccentricity and embedded planets
• Planets opening dust gaps in gas disks
• Dust flow in gas disks in the presence of embedded planets
• The evolution of gravitationally unstable protoplanetary disks: fragmentation and possible giant planet formation
• Nested-grid calculations of disk-planet interaction
• The interaction of planets with a disc with MHD turbulence III: Flow morphology and conditions for gap formation in local and global simulations
• Individual and collective behavior of dust particles in a protoplanetary nebula
• Planet - Disk Symbiosis
• RODEO: a new method for planet-disk interaction

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