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Pebble Accretion
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abstract
Pebble accretion refers to the growth of planetary bodies through the accretion of pebble-sized particles. Pebbles are defined in terms of their aerodynamically size $\tau_s$, which describes the level of coupling to the disk gas. Observations confirms the presence of pebble-sized particles in both protoplanetary disks and the early solar system. Pebble accretion proceeds through the settling mechanism, where particles settle to the surface of the planet. This Chapter discusses the key aspects of the pebble accretion framework: the accretion regimes, the planet initiation mass, and the planet isolation masses. The accretion behavior of loosely coupled $\tau_s > 1$ particles, referred to as "large pebbles", is also examined. The pebble accretion probability, $\epsilon$, is shown to be a useful parameter for evaluating the efficiency of the process, though this quantity is not necessarily high. Distinctions between pebble and planetesimal accretion are outlined. Pebble accretion, in particular, can be a highly effective mechanism in dense rings, as witnessed with ALMA.
Forward citations
Cited by 5 Pith papers
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The Influence of Dust Composition on Accretion Outbursts
Using 1D simulations with dust evaporation and condensation, the paper shows that dead-zone accretion outbursts vaporize dust out to about 0.5 au and that higher dust sublimation temperatures produce stronger but less...
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Quantifying the Impact of the Dust Torque on the Migration of Low-mass Planets II: The Role of Pebble Accretion in Planet Growth within a Global Planet Formation Model
A global model that includes dust torque predicts that low-mass planets forming inside the water ice line can migrate outward, while planets forming beyond it are barely affected.
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Dust dynamics in radially convective regions of protoplanetary disks
Convective overstability zonal flows in protoplanetary disks trap dust only weakly, and dust feedback suppresses the flows when the dust-to-gas ratio reaches about 0.1.
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Partial Differentiation of Callisto as Possible Evidence for Pebble Accretion
Callisto's partially differentiated interior is more naturally explained by pebble accretion than by satellitesimal accretion, giving a potential fossil test of planet formation.
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Formation of Giant Planets
A comprehensive review argues that core accretion is the dominant pathway for giant planet formation, while gas disk fragmentation rarely produces planets.
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