Streaming Instability in Turbulent Protoplanetary Disks

Umurhan, O. M.; Estrada, P. R.; Cuzzi, Jeffrey N.

doi:10.3847/1538-4357/ab899d

Cited by 91 publications

(107 citation statements)

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“…An alternative possibility is that these dust clumps result from the streaming instability (Youdin & Goodman 2005;Youdin & Johansen 2007) that tends to enhance the concentration of solids. Although our numerical resolution of ≈ 15 grid cells per scale-height is probably insufficient to resolve the streaming instability whose most unstable wavelength is typically ≈ ℎ𝐻, recent work (Chen & Lin 2020;Urmurhan et al 2020) has shown that in turbulent discs with 𝛼 ≈ 10 −3 , the most unstable wavelength might be shifted toward scales as large as 𝐻 (Johansen et al 2007;Umurhan et al 2020). In that case, our numerical resolution would be sufficient to witness the SI operating.…”

Section: Possible Formation Of Dusty Clumpsmentioning

confidence: 90%

Vertical settling of pebbles in turbulent circumbinary discs and the in situ formation of circumbinary planets

Nelson

McNally

2021

Monthly Notices of the Royal Astronomical Society

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The inner-most regions of circumbinary discs are unstable to a parametric instability whose non-linear evolution is hydrodynamical turbulence. This results in significant particle stirring, impacting on planetary growth processes such as the streaming instability or pebble accretion. In this paper, we present the results of three-dimensional, inviscid global hydrodynamical simulations of circumbinary discs with embedded particles of 1 cm size. Hydrodynamical turbulence develops in the disc, and we examine the effect of the particle back-reaction on vertical dust. We find that higher solid-to-gas ratios lead to smaller gas vertical velocity fluctuations, and therefore to smaller dust scale heights. For a metallicity Z = 0.1, the dust scale height near the edge of the tidally-truncated cavity is $\sim 80{{\ \rm per\ cent}}$ of the gas scale height, such that growing a Ceres-mass object to a 10 M⊕ core via pebble accretion would take longer than the disc lifetime. Collision velocities for small particles are also higher than the critical velocity for fragmentation, which precludes grain growth and the possibility of forming a massive planetesimal seed for pebble accretion. At larger distances from the binary, turbulence is weak enough to enable not only efficient pebble accretion but also grain growth to sizes required to trigger the streaming instability. In these regions, an in-situ formation scenario of circumbinary planets involving the streaming instability to form a massive planetesimal followed by pebble accretion on to this core is viable. In that case, planetary migration has to be invoked to explain the presence of circumbinary planets at their observed locations.

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Section: Possible Formation Of Dusty Clumpsmentioning

confidence: 90%

Vertical settling of pebbles in turbulent circumbinary discs and the in situ formation of circumbinary planets

Nelson

McNally

2021

Monthly Notices of the Royal Astronomical Society

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“…Over recent years, several works have shown that the generation of planetesimals via the SI in a smooth disk profile remains difficult. First, a large amount of solid material (Z > 0.02)larger than the typical ISM value -has to be provided in a single dust species of a particular Stokes number (Yang et al 2017;Johansen et al 2014), leaving a relatively narrow range of parameters (Umurhan et al 2020;Chen & Lin 2020), even more narrow when including the effect of turbulence (Jaupart & Laibe 2020). However such favorable conditions -a low amount of turbulence and a narrow range in mass distribution of large grains -is not expected from dust evolution models (Brauer et al 2008;Birnstiel et al 2011).…”

Section: Regions Of Planetesimal Formationmentioning

confidence: 99%

“…Recent studies emphasized again the importance of the level of gas turbulence when determining where the SI can operate (Jaupart & Laibe 2020; Umurhan et al 2020). So far, most simulations have been performed in local box simulations, and only recently did globally unstratified simulations come into use (Kowalik et al 2013;Mignone et al 2019), confirming the main characteristics of the SI.…”

Section: Introductionmentioning

confidence: 99%

Streaming instability in a global patch simulation of protoplanetary disks

Flock

Mignone

2021

A&A

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Aims. In recent years, sub-millimeter (mm) observations of protoplanetary disks have revealed an incredible diversity of substructures in the dust emission. An important result was the finding that dust grains of mm size are embedded in very thin dusty disks. This implies that the dust mass fraction in the midplane becomes comparable to that of the gas, increasing the importance of the interaction between the two components there. Methods. We use numerical 2.5D simulations to study the interaction between gas and dust in fully globally stratified disks. To this end, we employ the recently developed dust grain module of the PLUTO code. Our model focuses on a typical T Tauri disk model, simulating a short patch of the disk at 10 au which includes grains of a constant Stokes number of St = 0.01 and St = 0.1, corresponding to grains with sizes of 0.9 cm and 0.9 mm, respectively, for the given disk model. Results. By injecting a constant pebble flux at the outer domain, the system reaches a quasi-steady state of turbulence and dust concentrations driven by the streaming instability. For our given setup, and using resolutions up to 2500 cells per scale height, we resolve the streaming instability that leads to local dust clumping and concentrations. Our results show dust density values of around 10–100 times the gas density with a steady-state pebble flux of between 3.5 × 10−4 and 2.5 × 10−3 MEarth yr−1 for the models with St = 0.01 and St = 0.1. Conclusions. Grain size and pebble flux for model St = 0.01 compare well with dust evolution models of the first million years of disk evolution. For those grains, the scatter opacity dominates the extinction coefficient at mm wavelengths. These types of global dust and gas simulations are a promising tool for studies of the gas and dust evolution at pressure bumps in protoplanetary disks.

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“…Indeed, a distribution of grains has been shown to strongly impede the growth of the streaming instability in the low-dust-to-gasratio regime (Krapp et al 2019), while turbulence and/or viscosity can significantly limit the applicability of the instability in many scenarios (e.g. Squire & Hopkins 2018b;Umurhan, Estrada & Cuzzi 2019;Chen & Lin 2020;Jaupart & Laibe 2020;Krapp et al 2020;Zhuravlev 2020). Our models could, nonetheless, prove useful as the basis for more complex models of instabilities in systems with distributions of grain sizes, while turbulence, viscosity, or dust diffusion could likely be straightforwardly added, if desired (for example, viscosity will impede the growth of modes below some scale).…”

Section: The Philosophy Of This Articlementioning

confidence: 99%

Physical models of streaming instabilities in protoplanetary discs

Squire

Hopkins

2020

Monthly Notices of the Royal Astronomical Society

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We develop simple, physically motivated models for drag-induced dust-gas streaming instabilities, which are thought to be crucial for clumping grains to form planetesimals in protoplanetary disks. The models explain, based on the physics of gaseous epicyclic motion and dust-gas drag forces, the most important features of the streaming instability and its simple generalisation, the disk settling instability. Some of the key properties explained by our models include the sudden change in the growth rate of the streaming instability when the dust-to-gas-mass ratio surpasses one, the slow growth rate of the streaming instability compared to the settling instability for smaller grains, and the main physical processes underlying the growth of the most unstable modes in different regimes. As well as providing helpful simplified pictures for understanding the operation of an interesting and fundamental astrophysical fluid instability, our models may prove useful for analysing simulations and developing nonlinear theories of planetesimal growth in disks.

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Streaming Instability in Turbulent Protoplanetary Disks

Cited by 91 publications

References 100 publications

Vertical settling of pebbles in turbulent circumbinary discs and the in situ formation of circumbinary planets

Vertical settling of pebbles in turbulent circumbinary discs and the in situ formation of circumbinary planets

Streaming instability in a global patch simulation of protoplanetary disks

Physical models of streaming instabilities in protoplanetary discs

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