Linear growth of streaming instability in pressure bumps

Auffinger, Jérémy; Laibe, Guillaume

doi:10.1093/mnras/stx2395

Cited by 49 publications

(35 citation statements)

References 62 publications

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“…According to our results, the dust surface density at this position reaches ∼ 1 g cm −2 , which would imply dust-to-gas mass ratios ∼ 1 when compared with the gas surface density estimated by Fedele et al (2017). If confirmed, this inner ring would represent an ideal location to trigger the streaming instability and hence form the seeds for new young planets (Youdin & Goodman 2005;Auffinger & Laibe 2018). It is in fact possible that the streaming instability was triggered in the past at this ring, thus resulting in a run-away growth process responsible for the low values of p. Interestingly, the predicted a max at this position is not particularly high (∼ 5 mm), despite the low value of p (Abod et al 2018).…”

Section: Dust Grain Size Distributionmentioning

confidence: 93%

Characterization of Ring Substructures in the Protoplanetary Disk of HD 169142 from Multiwavelength Atacama Large Millimeter/submillimeter Array Observations

Macías

Espaillat

Osorio

et al. 2019

ApJ

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We present a detailed multi-wavelength characterization of the multi-ring disk of HD 169142. We report new ALMA observations at 3 mm and analyze them together with archival 0.89 and 1.3 mm data. Our observations resolve three out of the four rings in the disk previously seen in high-resolution ALMA data. A simple parametric model is used to estimate the radial profile of the dust optical depth, temperature, density, and particle size distribution. We find that the multiple ring features of the disk are produced by annular accumulations of large particles, probably associated with gas pressure bumps. Our model indicates that the maximum dust grain size in the rings is ∼ 1 cm, with slightly flatter power-law size distributions than the ISM-like size distribution (p ∼ 3.5) found in the gaps. In particular, the inner ring (∼ 26 au) is associated with a strong and narrow buildup of dust particles that could harbor the necessary conditions to trigger the streaming instability. According to our analysis, the snowlines of the most important volatiles do not coincide with the observed substructures. We explore different ring formation mechanisms and find that planet-disk interactions are the most likely scenario to explain the main features of HD 169142. Overall, our multi-wavelength analysis provides some of the first unambiguous evidence of the presence of radial dust traps in the rings of HD 169142. A similar analysis in a larger sample of disks could provide key insights on the impact that disk substructures have on the dust evolution and planet formation processes.

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Section: Dust Grain Size Distributionmentioning

confidence: 93%

Characterization of Ring Substructures in the Protoplanetary Disk of HD 169142 from Multiwavelength Atacama Large Millimeter/submillimeter Array Observations

Macías

Espaillat

Osorio

et al. 2019

ApJ

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“…Self-induced dust traps are a natural way of trapping dust in rings, where the dust-to-gas ratio is larger than the classic value of 1% by one or two orders of magnitude. With such enhancements of the dust density compared to the gas, it is possible that the streaming instability and self-induced dust traps could be working together to form planetesimals in pressure bumps (Auffinger & Laibe 2018). In particular, these authors found that the streaming instability can develop in a pressure bump for discs with a higher viscosity than previously thought (α 10 −3 ) at the cost of a slower growth rate.…”

Section: Planet(esimal) Formationmentioning

confidence: 94%

Self-induced dust traps around snow lines in protoplanetary discs

Vericel

Gonzalez

2019

Monthly Notices of the Royal Astronomical Society

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Dust particles need to grow efficiently from micrometre sizes to thousands of kilometres to form planets. With the growth of millimetre to meter sizes being hindered by a number of barriers, the recent discovery that dust evolution is able to create "self-induced" dust traps shows promises. The condensation and sublimation of volatile species at certain locations, called snow lines, is also thought to be an important part of planet formation scenarios. Given that dust sticking properties change across a snow line, this raises the question: how do snow lines affect the self-induced dust trap formation mechanism? The question is particularly relevant with the multiple observations of the carbon monoxide (CO) snow line in protoplanetary discs, since its effect on dust growth and dynamics is yet to be understood. In this paper, we present the effects of snow lines in general on the formation of self-induced dust traps in a parameter study, then focus on the CO snow line. We find that for a range of parameters, a dust trap forms at the snow line where the dust accumulates and slowly grows, as found for the water snow line in previous work. We also find that, depending on the grains sticking properties on either side of the CO snow line, it could either be a starting or braking point for dust growth and drift. This could provide clues to understand the link between dust distributions and snow lines in protoplanetary disc observations.

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“…Raettig et al (2015) showed that the accumulated pebbles could destroy a vortex in a disc, but in our case, the vortex is fed by the presence of the planet itself, which was not taken into account in their work. Auffinger & Laibe (2018) studied the linear growth regime of the streaming instability in pressure bumps in discs, and they found that streaming instability can occur within the pressure bump. The accumulated pebbles inside the pressure bump therefore turn into planetesimals, which do not affect the gas velocities and thus do not disrupt the pressure bump.…”

Section: Mass Loading In the Pressure Bumpmentioning

confidence: 99%

Pebble-isolation mass: Scaling law and implications for the formation of super-Earths and gas giants

Bitsch

Morbidelli

Johansen

et al. 2018

A&A

279

296

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The growth of a planetary core by pebble accretion stops at the so-called pebble isolation mass, when the core generates a pressure bump that traps drifting pebbles outside its orbit. The value of the pebble isolation mass is crucial in determining the final planet mass. If the isolation mass is very low, gas accretion is protracted and the planet remains at a few Earth masses with a mainly solid composition. For higher values of the pebble isolation mass, the planet might be able to accrete gas from the protoplanetary disc and grow into a gas giant. Previous works have determined a scaling of the pebble isolation mass with cube of the disc aspect ratio. Here, we expand on previous measurements and explore the dependency of the pebble isolation mass on all relevant parameters of the protoplanetary disc. We use 3D hydrodynamical simulations to measure the pebble isolation mass and derive a simple scaling law that captures the dependence on the local disc structure and the turbulent viscosity parameter α. We find that small pebbles, coupled to the gas, with Stokes number τ f < 0.005 can drift through the partial gap at pebble isolation mass. However, as the planetary mass increases, particles must be decreasingly smaller to penetrate the pressure bump. Turbulent diffusion of particles, however, can lead to an increase of the pebble isolation mass by a factor of two, depending on the strength of the background viscosity and on the pebble size. We finally explore the implications of the new scaling law of the pebble isolation mass on the formation of planetary systems by numerically integrating the growth and migration pathways of planets in evolving protoplanetary discs. Compared to models neglecting the dependence of the pebble isolation mass on the α-viscosity, our models including this effect result in higher core masses for giant planets. These higher core masses are more similar to the core masses of the giant planets in the solar system.

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Linear growth of streaming instability in pressure bumps

Cited by 49 publications

References 62 publications

Characterization of Ring Substructures in the Protoplanetary Disk of HD 169142 from Multiwavelength Atacama Large Millimeter/submillimeter Array Observations

Characterization of Ring Substructures in the Protoplanetary Disk of HD 169142 from Multiwavelength Atacama Large Millimeter/submillimeter Array Observations

Self-induced dust traps around snow lines in protoplanetary discs

Pebble-isolation mass: Scaling law and implications for the formation of super-Earths and gas giants

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