Laboratory Experiments on the Motion of Dense Dust Clouds in Protoplanetary Disks

Schneider, Niclas; Wurm, Gerhard

doi:10.3847/2041-8213/ab55e0

Cited by 7 publications

(1 citation statement)

References 23 publications

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“…2.4), the particle collision timescale becomes even shorter. However, for large values of f dust the stirring of dust by turbulent diffusion in the gas is reduced by their collective inertia (see Schneider & Wurm 2019 for laboratory experiments and Sect. 4 of Batygin & Morbidelli 2020 for an analytic derivation).…”

Section: Once In the Gap: Accretion On The Planetmentioning

confidence: 99%

In situ enrichment in heavy elements of hot Jupiters

Morbidelli¹,

Batygin²,

Lega³

2023

A&A

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Context. Radius and mass measurements of short-period giant planets reveal that many of these planets contain a large amount of heavy elements. Although the range of inferred metallicities is broad, planets with more than 100 M⊕ of heavy elements are not rare. This is in sharp contrast with the expectations of the conventional core-accretion model for the origin of giant planets. Aims. The proposed explanations for the heavy-element enrichment of giant planets fall short of explaining the most enriched planets. We look for additional processes that can explain the full envelope of inferred enrichments. Methods. We revisited the dynamics of pebbles and dust in the vicinity of giant planets using analytic estimates and published results on the profile of a gap opened by a giant planet, the radial velocity of the gas with respect to the planet, the Stokes number of particles in the different parts of the disk, and the consequent dust/gas ratio. Although our results are derived in the framework of a viscous α-disk, we also discuss the case of disks driven by angular momentum removal in magnetized winds. Results. When giant planets are far from the star, dust and pebbles are confined to a pressure bump at the outer edge of the planet-induced gap. When the planets reach the inner part of the disk (rp ≪ 2 au), dust instead penetrates into the gap together with the gas. The dust/gas ratio can be enhanced by more than an order of magnitude if the radial drift of dust is not impeded farther out by other barriers. Thus, hot planets undergoing runaway gas accretion can swallow a large amount of dust, acquiring ~100 M⊕ of heavy elements by the time they reach Jupiter masses. Conclusions. Whereas the gas accreted by giant planets in the outer disk is very dust-poor, that accreted by hot planets can be extremely dust-rich. Thus, provided that a large fraction of the atmosphere of hot Jupiters is accreted in situ, a large amount of dust can be accreted as well. We draw a distinction between this process and pebble accretion (i.e., the capture of dust without the accretion of gas), which is ineffective at small stellocentric radii, even for super-Earths. Giant planets farther out in the disk are extremely effective barriers against the flow of pebbles and dust across their gap. Saturn and Jupiter, after locking into a mutual mean motion resonance and reversing their migration, could have accreted small pebble debris.

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Section: Once In the Gap: Accretion On The Planetmentioning

confidence: 99%

In situ enrichment in heavy elements of hot Jupiters

Morbidelli¹,

Batygin²,

Lega³

2023

A&A

View full text Add to dashboard Cite

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Experimental study of clusters in dense granular gas and implications for the particle stopping time in protoplanetary disks

Schneider

Musiolik

Kollmer

et al. 2021

Icarus

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Understanding planet formation using microgravity experiments

Wurm

Teiser

2021

Nat Rev Phys

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In 2018, images were released of a planet being formed around the star PDS 70, offering a tantalizing glimpse into how planets come into being. However, many questions remain about how dust evolves into planets, and astrophysical observations are unable to provide all the answers. It is therefore necessary to perform experiments to reveal key details and, to avoid unwanted effects from the Earth's gravitational pull, it is often necessary to perform such experiments in microgravity platforms. This Review sketches current models of planet formation and describes the experiments needed to test the models.

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Laboratory Experiments on the Motion of Dense Dust Clouds in Protoplanetary Disks

Cited by 7 publications

References 23 publications

In situ enrichment in heavy elements of hot Jupiters

In situ enrichment in heavy elements of hot Jupiters

Experimental study of clusters in dense granular gas and implications for the particle stopping time in protoplanetary disks

Understanding planet formation using microgravity experiments

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