Polydisperse streaming instability – III. Dust evolution encourages fast instability

McNally, Christopher A.; Lovascio, Francesco; Paardekooper, Sijme-Jan

doi:10.1093/mnras/stab112

Cited by 31 publications

(33 citation statements)

References 79 publications

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“…Specifically, for smaller grain sizes, (Krapp et al 2019) found that growth rates were a strong function of the number of species N d used to discretize the grain distribution, in some cases being unconverged even for N d > 2048. Subsequent works (Paardekooper et al 2020;Zhu & Yang 2021;McNally et al 2021) have explored this further, showing that the instability is robust only for large stopping times or µ 1, also depending somewhat on the size distribution of grains. Similar non-convergent behavior is seen for some mode angles of the acoustic RDI discussed below.…”

Section: Data Availabilitymentioning

confidence: 99%

“…Cursory lower-resolution tests of different grain-mass distributions (e.g., small-grain dominated, dµ/d ln grain ∝ −0.5 grain ) have not revealed significant differences, so we shall not explore this in detail. It is, however, worth noting that for the gas of the protoplanetary-disk streaming instability, the grain distribution can affect important details of the linear instability (Paardekooper et al 2020;McNally et al 2021;Zhu & Yang 2021), so this issue may be worth revisiting in more detail in future work.…”

Section: Grain Mass Distributionmentioning

confidence: 99%

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The Acoustic Resonant Drag Instability with a Spectrum of Grain Sizes

Squire,

Moroianu,

Hopkins

2021

Preprint

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We study the linear growth and nonlinear saturation of the "acoustic Resonant Drag Instability" (RDI) when the dust grains, which drive the instability, have a wide, continuous spectrum of different sizes. This physics is generally applicable to dusty winds driven by radiation pressure, such as occurs around red-giant stars, star-forming regions, or active galactic nuclei. Depending on the physical size of the grains compared to the wavelength of the radiation field that drives the wind, two qualitatively different regimes emerge. In the case of grains that are larger than the radiation's wavelength -termed the constant-drift regime -the grain's equilibrium drift velocity through the gas is approximately independent of grain size, leading to strong correlations between differently sized grains that persist well into the saturated nonlinear turbulence. For grains that are smaller than the radiation's wavelength -termed the non-constant-drift regime -the linear instability grows more slowly than the single-grainsize RDI and only the larger grains exhibit RDI-like behavior in the saturated state. A detailed study of grain clumping and grain-grain collisions shows that outflows in the constant-drift regime may be effective sites for grain growth through collisions, with large collision rates but low collision velocities.

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Section: Data Availabilitymentioning

confidence: 99%

Section: Grain Mass Distributionmentioning

confidence: 99%

The Acoustic Resonant Drag Instability with a Spectrum of Grain Sizes

Squire,

Moroianu,

Hopkins

2021

Preprint

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“…distribution, in some cases being unconverged even for N d > 2048. Subsequent w orks (Paardek ooper et al 2020 ;McNally et al 2021 ;Zhu & Yang 2021 ) hav e e xplored this further, showing that the instability is robust only for large stopping times or μ 1, also depending somewhat on the size distribution of grains. Similar nonconvergent behaviour is seen for some mode angles of the acoustic RDI discussed belo w. Ho we ver, such behaviour is not by any means generic to all RDIs.…”

Section: Ac K N Ow L E D G E M E N T Smentioning

confidence: 94%

The acoustic resonant drag instability with a spectrum of grain sizes

Squire

Moroianu

Hopkins

2021

Monthly Notices of the Royal Astronomical Society

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We study the linear growth and nonlinear saturation of the ‘acoustic Resonant Drag Instability’ (RDI) when the dust grains, which drive the instability, have a wide, continuous spectrum of different sizes. This physics is generally applicable to dusty winds driven by radiation pressure, such as occurs around red-giant stars, star-forming regions, or active galactic nuclei. Depending on the physical size of the grains compared to the wavelength of the radiation field that drives the wind, two qualitatively different regimes emerge. In the case of grains that are larger than the radiation’s wavelength – termed the constant-drift regime – the grain’s equilibrium drift velocity through the gas is approximately independent of grain size, leading to strong correlations between differently sized grains that persist well into the saturated nonlinear turbulence. For grains that are smaller than the radiation’s wavelength – termed the non-constant-drift regime – the linear instability grows more slowly than the single-grain-size RDI and only the larger grains exhibit RDI-like behaviour in the saturated state. A detailed study of grain clumping and grain-grain collisions shows that outflows in the constant-drift regime may be effective sites for grain growth through collisions, with large collision rates but low collision velocities.

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“…streaming instability with local box simulations, or magneto-hydrodynamic simulations where magnetic effects influencing the dust (e.g. Johansen et al 2007;Chi-ang & Youdin 2009;Flock et al 2020;Krapp et al 2019;Paardekooper et al 2020Paardekooper et al , 2021McNally et al 2021;Zhu & Yang 2021;Lin 2021). There is a need for 3D dust-gas hydrodynamical simulations with embedded planets to understand how the dust flows and -processes change in this case.…”

Section: Introductionmentioning

confidence: 99%

Meridional Circulation of Dust and Gas in the Circumstellar Disk: Delivery of Solids onto the Circumplanetary Region

Szulágyi,

Binkert,

Surville

2021

Preprint

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We carried out 3D dust+gas radiative hydrodynamic simulations of forming planets. We investigated a parameter grid of Neptune-, Saturn-, Jupiter-, and 5 Jupiter-mass planets at 5.2, 30, 50 AU distance from their star. We found that the meridional circulation (Szulágyi et al. 2014;Fung & Chiang 2016) drives a strong vertical flow for the dust as well, hence the dust is not settled in the midplane, even for mm-sized grains. The meridional circulation will deliver dust and gas vertically onto the circumplanetary region, efficiently bridging over the gap. The Hill-sphere accretion rates for the dust are ∼ 10 −8 to 10 −10 M Jup /yr, increasing with planet-mass. For the gas component, the gain is 10 −6 to 10 −8 M Jup /yr. The difference between the dust and gas accretion rates is smaller with decreasing planetary mass. In the planet vicinity, the mm-grains can get trapped easier than the gas, which means the circumplanetary disk might be enriched with solids in comparison to the circumstellar disk. We calculated the local dust-to-gas ratio (DTG) everywhere in the circumstellar disk and identified the altitude above the midplane where the DTG is 1, 0.1, 0.01, 0.001. The larger is the planetary mass, the higher the mm-sized dust is delivered and a larger fraction of the dust disk is lifted by the planet. The stirring of mm-dust is negligible for Neptune-mass planets or below, but significant above Saturn-mass. We also examined the formation of dust rings (similar to ALMA observations) and we found that they are formed by the merging of the spiral arms of planets.

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Polydisperse streaming instability – III. Dust evolution encourages fast instability

Cited by 31 publications

References 79 publications

The Acoustic Resonant Drag Instability with a Spectrum of Grain Sizes

The Acoustic Resonant Drag Instability with a Spectrum of Grain Sizes

The acoustic resonant drag instability with a spectrum of grain sizes

Meridional Circulation of Dust and Gas in the Circumstellar Disk: Delivery of Solids onto the Circumplanetary Region

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