Dust flow in gas disks in the presence of embedded planets

By Sijme-Jan Paardekooper, G. Mellema. 2006

158 citations recorded by the source corpus.

Aims. We study the dynamics of gas and dust in a protoplanetary disk in the presence of embedded planets. We investigate the conditions for dust-gap formation in terms of particle size and planetary mass. We also monitor the amount of dust that is accreted by the planet relative to the amount of gas, which is an important parameter in determining the enrichment of solids in giant planets compared to the solid content of the central star. Methods. We use a new two-fluid hydrodynamics code to solve the flow equations for both gas and dust. For the gas, we use a Godunov-type scheme with an approximate Riemann solver (the Roe solver). The dust is treated as a pressureless fluid by essentially the same numerical method as is used for the gas. Results. We find that it only takes a planet of 0.05 Jupiter masses to open up a gap in a disk with a significant population of mm-sized particles. Dust particles larger than 150 $\mu{\rm m}$ participate in gap formation. We also find that the formation of the gap severely slows down dust accretion compared to that in the gas. Therefore, it is not possible to enrich a newly formed giant planet in solids, if these solids are contained in particles with sizes from 150 $\mu{\rm m}$ to approximately 10 cm.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ae7672be66d6137865b018507db2fe9f09d5cd21

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Citations in the corpus

Planet-Disk Interaction and Orbital Evolution (2012, background): “…from disk shadowing and illumination variations in the presence of a planet (Jang-Condell & Sasselov, 2005); stochastic migration induced by disk turbulence (Nelson & Papaloizou, 2004; Laughlin, Steinacker & Adams, 2004); and corotation torques in radiative disks (Paardekooper & Mellema, 2006b).”
DUST FILTRATION BY PLANET-INDUCED GAP EDGES: IMPLICATIONS FOR TRANSITIONAL DISKS (2012, methodology): “By considering dust dynamics independently, one promising mechanism to explain these wide and deep (dust) gaps/holes is dust filtration by the gap outer edge opened by planet(s) (Paardekooper & Mellema 2006, Rice et al. 2006).”
GIANT PLANET MIGRATION, DISK EVOLUTION, AND THE ORIGIN OF TRANSITIONAL DISKS (2009, background): “Planets less massive than∼ 0.5MJup are unlikely to open gaps in their parent gas disks, but the presence of even a low-mass planet can cause significant perturbations to the dust distribution (Paardekooper & Mellema 2006).”
Cavity opening by a giant planet in a protoplanetary disc and effects on planetary migration (2007, background): “Hence, the planet appears opening a wide and deep gap in the dust distribution (Paardekooper & Mellema 2006), rather than a cavity.”
The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview (2018, background): “…particle trapping capabilities of even modest pressure maxima should substantially amplify the associated local mm/cm-sized particle density (e.g., Paardekooper & Mellema 2006; Rice et al. 2006; Pinilla et al. 2012b; Zhu et al. 2012), generating a bright signature in the broadband (sub-)mm…”
Dust filtration at gap edges: Implications for the spectral energy distributions of discs with embedded planets (2006, background): “The pressure gradient leads to super-Keplerian rotation of the gas, which in turn allows standard aerodynamic coupling to solid bodies (Weidenschilling 1977; Paardekooper & Mellema 2006) to inject angular momentum and hold back the inward flow of all but the smallest solid particles.”
On planet formation in HL Tau (2015, background): “We assume a physical drag prescription where the drag regimeis chosen automatically depending on the ratio of the grain size to the gas mean free path (Kwok 1975; Paardekooper & Mellema 2006; Laibe & Price 2012b).”
The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation (2018, background): “…at various wavelengths, only dust thermal emission at (sub) millimeter wavelengths allows us to probe low-mass planets, because a small change in the gas surface density due to the low-mass planet can cause dramatic changes in the dust surface density (Paardekooper & Mellema 2006; Zhu et al. 2014).”
Observational Signatures of Planets in Protoplanetary Disks I: Gaps Opened by Single and Multiple Young Planets in Disks (2014, background): “Zhu et al. (2012) and Pinilla et al. (2012) have shown that the “dust filtration” effect (Paardekooper & Mellema 2006; Rice et al. 2006) may allow the cavity in the gas and 0.3-3 mm wavelengths “mm observations” 7 In this work, we call both “transitional” and “pretransitional” disks as defined in…”
Pebble-isolation mass: Scaling law and implications for the formation of super-Earths and gas giants (2018, background): “Paardekooper & Mellema (2006) included diffusion into the motion of dust particles in gas discs in the presence of 30 ME planets and estimated this effect to be of the order of 1%, indicating that diffusion of dust particles does not play a role in opening a gap in dust distribution of…”
Multiple Disk Gaps and Rings Generated by a Single Super-Earth (2017, methodology): “Note that our 10M⊕ planet is not massive enough to trap dust effectively at its 2:1 resonance at r = 1.6rp, by contrast to the higher mass planet considered by Paardekooper & Mellema (2004, 2006).”
Dust dynamics during protoplanetary disc clearing (2007, result): “…by the same physical process (a reversal in the direction of the pressure gradient close to the disc edge), have been found by other authors (e.g. Paardekooper & Mellema 2004, 2006), so although we are unable to make detailed predictions we are satisfied that the formation of the dust-rich ring…”
Rapid growth of gas-giant cores by pebble accretion (2012, background): “Dust gaps can open up before the core is massive enough to create a gap in the gas disc itself (Paardekooper & Mellema 2006).”
RINGED SUBSTRUCTURE AND A GAP AT 1 au IN THE NEAREST PROTOPLANETARY DISK (2016, background): “…even relatively low-mass (∼several M⊕) planets can open narrow gaps (Zhu et al. 2013; Duffell & MacFadyen 2013; Fung et al. 2014) and trap solid particles (Paardekooper & Mellema 2006; Zhu et al. 2014; Picogna & Kley 2015) to produce features similar to the substructure that we observe here.”
Separating gas-giant and ice-giant planets by halting pebble accretion (2014, background): “A planet can perturb the gas-disc enough to make the gas velocity in a narrow ring just outside the orbit of the planet super-Keplerian (Paardekooper & Mellema 2006; Morbidelli & Nesvorny 2012).”
TRANSITIONAL AND PRE-TRANSITIONAL DISKS: GAP OPENING BY MULTIPLE PLANETS? (2010, background): “This gas may be substantially depleted of small dust because of significant grain growth at large radii, combined with filtration of dust at the outer edge of the gap (Paardekooper & Mellema 2006; Rice et al. 2006).”
RESOLVED IMAGES OF LARGE CAVITIES IN PROTOPLANETARY TRANSITION DISKS (2011, background): “Any companion that can open a gap will generate wakes just outside its orbit, creating a pressure bump that may act like a dust filter on the flow across the gap (Rice et al. 2006; Paardekooper & Mellema 2006).”