On the accumulation of planetesimals near disc gaps created by protoplanets

Ayliffe, Ben; Laibe, Guillaume; Price, Daniel J.; Bate, Matthew R.

doi:10.1111/j.1365-2966.2012.20967.x

Cited by 92 publications

(86 citation statements)

References 71 publications

(140 reference statements)

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“…Furthermore, as observed in Ayliffe et al (2012) there is a strong correlation between particle size and particle gap, where the most coupled particles reach regions closer to the planet and can be accreted by the planet or can migrate to the inner disk, while less coupled particles are effectively filtrated by the planet.…”

Section: Comparison With Previous Workmentioning

confidence: 84%

How do giant planetary cores shape the dust disk?

Picogna

Kley

2015

A&A

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Context. We have been observing, thanks to ALMA, the dust distribution in the region of active planet formation around young stars. This is a powerful tool that can be used to connect observations with theoretical models and improve our understanding of the processes at play. Aims. We want to test how a multiplanetary system shapes its birth disk and to study the influence of the planetary masses and particle sizes on the final dust distribution. Moreover, we apply our model to the HL Tau system in order to obtain some insights on the physical parameters of the planets that are able to create the observed features. Methods. We follow the evolution of a population of dust particles, treated as Lagrangian particles, in two-dimensional locally isothermal disks where two equal-mass planets are present. The planets are kept in fixed orbits and they do not accrete mass.Results. The outer planet plays a major role in removing the dust particles in the co-orbital region of the inner planet and in forming a particle ring which have a steeper density gradient close to the gap edge respect to the single-planet scenario, promoting the development of vortices. The ring and gap width depend strongly on the planetary mass and particle stopping times, and for the more massive cases on the ring clumps in few stable points that are able to collect a high mass fraction. The features observed in the HL Tau system can be explained through the presence of several massive cores that shape the dust disk where the inner planet(s) have a mass of the order of 0.07 M Jup and the outer one(s) of the order of 0.35 M Jup . These values can be significantly lower if the disk mass turns out to be less than previously estimated. By decreasing the disk mass by a factor of 10, we obtain similar gap widths for planets with a mass of 10 M ⊕ and 20 M ⊕ for the inner and outer planets, respectively. Although the particle gaps are prominent, the expected gaseous gaps are barely visible.

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Section: Comparison With Previous Workmentioning

confidence: 84%

How do giant planetary cores shape the dust disk?

Picogna

Kley

2015

A&A

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“…It is therefore necessary to take a critical look at the fidelity of the method. While many code comparisons exist in the case of purely gaseous discs (Meru & Bate 2011, 2012Paardekooper, Baruteau & Meru 2011), the dust implementation has been hitherto untested in this context (although, for studies of dust in general see Laibe & Price 2011, 2012Ayliffe et al 2012;Lorén-Aguilar & Bate 2014).…”

Section: Discussionmentioning

confidence: 99%

“…They found that using the gas smoothing length partially resolves the issue, since the gas has lower density and a larger smoothing length. We suspect that both error in the dust density and requirement that the gas is resolved on length scales present in the dust distribution are important for resolving the issue (Ayliffe et al 2012).…”

Section: Discussionmentioning

confidence: 99%

Smoothed particle hydrodynamics simulations of gas and dust mixtures

Booth¹,

Sijacki²,

Clarke³

2015

Mon. Not. R. Astron. Soc.

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We present a 'two-fluid' implementation of dust in smoothed particle hydrodynamics (SPH) in the test particle limit. The scheme is able to handle both short and long stopping times and reproduces the short friction time limit, which is not properly handled in other implementations. We apply novel tests to verify its accuracy and limitations, including multi-dimensional tests that have not been previously applied to the drag-coupled dust problem and which are particularly relevant to self-gravitating protoplanetary discs. Our tests demonstrate several key requirements for accurate simulations of gas-dust mixtures. Firstly, in standard SPH particle jitter can degrade the dust solution, even when the gas density is well reproduced. The use of integral gradients, a Wendland kernel and a large number of neighbours can control this, albeit at a greater computational cost. Secondly, when it is necessary to limit the artificial viscosity we recommend using the Cullen & Dehnen (2010) switch, since the alternative, using α ∼ 0.1, can generate a large velocity noise up to σ v 0.3c s in the dust particles. Thirdly, we find that an accurate dust density estimate requires > 400 neighbours, since, unlike the gas, the dust particles do not feel regularization forces. This density noise applies to all particlebased two-fluid implementations of dust, irrespective of the hydro solver and could lead to numerically induced fragmentation. Although our tests show accurate dusty gas simulations are possible, care must be taken to minimize the contribution from numerical noise.

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“…Another approach is to model the dust population as a continuous, pressureless fluid (Barrière-Fouchet et al 2005;Paardekooper & Mellema 2006;Ayliffe et al 2012;Meheut et al 2012;Fu et al 2014;Lorén-Aguilar & Bate 2014;Surville et al 2016). The hydrodynamic equations are evolved for two fluids: the gas and dust, with density and velocity r g , v g and r d , v d , respectively.…”

Section: Introductionmentioning

confidence: 99%

A Thermodynamic View of Dusty Protoplanetary Disks

Lin

Youdin

2017

ApJ

123

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Small solids embedded in gaseous protoplanetary disks are subject to strong dust-gas friction. Consequently, tightly coupled dust particles almost follow the gas flow. This near conservation of the dust-to-gas ratio along streamlines is analogous to the near conservation of entropy along flows of (dust-free) gas with weak heating and cooling. We develop this thermodynamic analogy into a framework to study dusty gas dynamics in protoplanetary disks. We show that an isothermal dusty gas behaves like an adiabatic pure gas, and that finite dust-gas coupling may be regarded as effective heating/cooling. We exploit this correspondence to deduce that (1) perfectly coupled, thin dust layers cannot cause axisymmetric instabilities; (2) radial dust edges are unstable if the dust is vertically well-mixed; (3) the streaming instability necessarily involves a gas pressure response that lags behind dust density; and (4) dust-loading introduces buoyancy forces that generally stabilize the vertical shear instability associated with global radial temperature gradients. We also discuss dusty analogs of other hydrodynamic processes (e.g., Rossby wave instability, convective overstability, and zombie vortices) and how to simulate dusty protoplanetary disks with minor tweaks to existing codes for pure gas dynamics.

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On the accumulation of planetesimals near disc gaps created by protoplanets

Cited by 92 publications

References 71 publications

How do giant planetary cores shape the dust disk?

How do giant planetary cores shape the dust disk?

Smoothed particle hydrodynamics simulations of gas and dust mixtures

A Thermodynamic View of Dusty Protoplanetary Disks

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