Self-induced dust traps around snow lines in protoplanetary discs

Vericel, Arnaud; Gonzalez, Jean-François

doi:10.1093/mnras/stz3444

Cited by 23 publications

(21 citation statements)

References 71 publications

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“…Astrophysical mass distributions are expected to be dominated by large grains. Hence, the CFL condition for fragmentation should be similar to the one for growth (Vericel & Gonzalez 2020). If so, numerical integration will be performed explicitly.…”

Section: Discussionmentioning

confidence: 99%

Grain growth for astrophysics with discontinuous Galerkin schemes

Lombart

Laibe

2020

Monthly Notices of the Royal Astronomical Society

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Depending on their sizes, dust grains store more or less charges, catalyse more or less chemical reactions, intercept more or less photons and stick more or less efficiently to form embryos of planets. Hence the need for an accurate treatment of dust coagulation and fragmentation in numerical modelling. However, existing algorithms for solving the coagulation equation are over-diffusive in the conditions of 3D simulations. We address this challenge by developing a high-order solver based on the Discontinuous Galerkin method. This algorithm conserves mass to machine precision and allows to compute accurately the growth of dust grains over several orders of magnitude in size with a very limited number of dust bins.

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Section: Discussionmentioning

confidence: 99%

Grain growth for astrophysics with discontinuous Galerkin schemes

Lombart

Laibe

2020

Monthly Notices of the Royal Astronomical Society

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“…Indeed, when the pressure gradient is zero, the difference of speed between gas and dust vanishes and no radial drift occurs. Several mechanisms have been proposed to form dust traps, such as gaps made by planets (Pinilla et al 2012), magnetic winds (Suriano et al 2018), spirals induced by gravitational instabilities (Dipierro et al 2015a) or self-induced dust traps (Gonzalez et al 2017;Vericel & Gonzalez 2020).…”

Section: Introductionmentioning

confidence: 99%

Dynamical dust traps in misaligned circumbinary discs: analytical theory and numerical simulations

Longarini

Lodato

Toci

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Recent observations have shown that circumbinary discs can be misaligned with respect to the binary orbital plane.The lack of spherical symmetry, together with the non-planar geometry of these systems, causes differential precession which might induce the propagation of warps. While gas dynamics in such environments is well understood, little is known about dusty discs. In this work, we analytically study the problem of dust traps formation in misaligned circumbinary discs. We find that pile-ups may be induced not by pressure maxima, as the usual dust traps, but by a difference in precession rates between the gas and dust. Indeed, this difference makes the radial drift inefficient in two locations, leading to the formation of two dust rings whose position depends on the system parameters. This phenomenon is likely to occur to marginally coupled dust particles (St ≳ 1) as both the effect of gravitational and drag force are considerable. We then perform a suite of three-dimensional SPH numerical simulations to compare the results with our theoretical predictions. We explore the parameter space, varying stellar mass ratio, disc thickness, radial extension, and we find a general agreement with the analytical expectations. Such dust pile-up prevents radial drift, fosters dust growth and may thus promote the planet formation in circumbinary discs.

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“…& Wurm 2019;Ros et al 2019;Vericel & Gonzalez 2020;Ziampras et al 2020). In future studies, we plan to improve our model by introducing H 2 O, CO, and CO 2 snow lines and adopting dust fragmentation velocity (u frag ) depending on the position of dust particle relative to the snow line.…”

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confidence: 99%

Gravitoviscous protoplanetary disks with a dust component

Elbakyan

Johansen²,

Lambrechts³

et al. 2020

A&A

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Aims. We study the dynamics and growth of dust particles in circumstellar disks of different masses that are prone to gravitational instability during the critical first Myr of their evolution. Methods. We solved the hydrodynamics equations for a self-gravitating and viscous circumstellar disk in a thin-disk limit using the FEOSAD numerical hydrodynamics code. The dust component is made up of two different components: micron-sized dust and grown dust of evolving size. For the dust component, we considered the dust coagulation, fragmentation, momentum exchange with the gas, and dust self-gravity. Results. We found that the micron-sized dust particles grow rapidly in the circumstellar disk, reaching a few cm in size in the inner 100 au of the disk during less than 100 kyr after the disk formation, provided that fragmentation velocity is 30 ms−1. Due to the accretion of micron dust particles from the surrounding envelope, which serves as a micron dust reservoir, the approximately cm-sized dust particles continue to be present in the disk for more than 900 kyr after the disk formation and maintain a dust-to-gas ratio close to 0.01. We show that a strong correlation exists between the gas and pebble fluxes in the disk. We find that radial surface density distribution of pebbles in the disk shows power-law distribution with an index similar to that of the Minimum-mass solar nebula regardless the disk mass. We also show that the gas surface density in our models agrees well with measurements of dust in protoplanetary disks of AS 209, HD 163296, and DoAr 25 systems. Conclusions. Pebbles are formed during the very early stages of protoplanetary disk evolution. They play a crucial role in the planet formation process. Our disc simulations reveal the early onset (<105 yr) of an inwards-drifting flux of pebble-sized particles that makes up approximately between one hundredth and one tenth of the gas mass flux, which appears consistent with mm-observations of discs. Such a pebble flux would allow for the formation of planetesimals by streaming instability and the early growth of embryos by pebble accretion. We conclude that unlike the more common studies of isolated steady-state protoplanetary disks, more sophisticated global numerical simulations of circumstellar disk formation and evolution, including the pebble formation from the micron dust particles, are needed for performing realistic planet formation studies.

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Self-induced dust traps around snow lines in protoplanetary discs

Cited by 23 publications

References 71 publications

Grain growth for astrophysics with discontinuous Galerkin schemes

Grain growth for astrophysics with discontinuous Galerkin schemes

Dynamical dust traps in misaligned circumbinary discs: analytical theory and numerical simulations

Gravitoviscous protoplanetary disks with a dust component

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