Dust size distributions in coagulation/fragmentation equilibrium: numerical solutions and analytical fits

Birnstiel, T.; Ormel, Chris W.; Dullemond, C. P.

doi:10.1051/0004-6361/201015228

Cited by 231 publications

(99 citation statements)

References 48 publications

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“…The grain size distribution up to the maximum grain size can be reasonably fit with a power law (i.e. Birnstiel et al (2011)),…”

Section: Dust Evolutionmentioning

confidence: 97%

“…where f f is an order-unity parameter, Σg is the gas surface density, and ρs is the volume-density of solids. Analytical models of grain size distributions in Birnstiel, Ormel & Dullemond (2011) find that most of the mass in large grains is contained in sizes slightly below the maximum fragmentation-limited grain size. The fragmentation parameter f f in equation 3 is used to correct this offset.…”

Section: Dust Evolutionmentioning

confidence: 99%

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Formation of planetary populations − II. Effects of initial disc size and radial dust drift

Alessi

Cridland

2020

Monthly Notices of the Royal Astronomical Society

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Recent ALMA observations indicate that while a range of disk sizes exist, typical disk radii are small, and that radial dust drift affects the distribution of solids in disks.Here we explore the consequences of these features in planet population synthesis models. A key feature of our model is planet traps -barriers to otherwise rapid type-I migration of forming planets -for which we include the ice line, heat transition, and outer edge of the dead zone. We find that the ice line plays a fundamental role in the formation of warm Jupiters. In particular, the ratio of super Earths to warm Jupiters formed at the ice line depend sensitively on the initial disk radius. Initial gas disk radii of ∼50 AU results in the largest super Earth populations, while both larger and smaller disk sizes result in the ice line producing more gas giants near 1 AU. This transition between typical planet class formed at the ice line at various disk radii confirms that planet formation is fundamentally linked to disk properties (in this case, disk size), and is a result that is only seen when dust evolution effects are included in our models. Additionally, we find that including radial dust drift results in the formation of more super Earths between 0.1 -1 AU, having shorter orbital radii than those produced in models where dust evolution effects are not included.

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“…The grain size distribution up to the maximum grain size can be reasonably fit with a power law (i.e. Birnstiel et al (2011)),…”

Section: Dust Evolutionmentioning

confidence: 97%

Section: Dust Evolutionmentioning

confidence: 99%

Formation of planetary populations − II. Effects of initial disc size and radial dust drift

Alessi

Cridland

2020

Monthly Notices of the Royal Astronomical Society

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“…The complexity of the problem is illustrated by, for example, Birnstiel et al (2011) and references therein. In this work, based on transitional disk SEDs, we suggest that small dust needs to grow in the inner disk.…”

Section: Observational Implications For Almamentioning

confidence: 99%

Dust Filtration by Planet-Induced Gap Edges: Implications for Transitional Disks

Zhu

Nelson

Dong

et al. 2012

ApJ

408

447

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By carrying out two-dimensional two-fluid global simulations, we have studied the response of dust to gap formation by a single planet in the gaseous component of a protoplanetary disk-the so-called dust filtration mechanism. We have found that a gap opened by a giant planet at 20 AU in an α = 0.01,Ṁ = 10 −8 M yr −1 disk can effectively stop dust particles larger than 0.1 mm drifting inward, leaving a submillimeter (submm) dust cavity/hole. However, smaller particles are difficult to filter by a gap induced by a several M J planet due to (1) dust diffusion and (2) a high gas accretion velocity at the gap edge. Based on these simulations, an analytic model is derived to understand what size particles can be filtered by the planet-induced gap edge. We show that a dimensionless parameter T s /α, which is the ratio between the dimensionless dust stopping time and the disk viscosity parameter, is important for the dust filtration process. Finally, with our updated understanding of dust filtration, we have computed Monte Carlo radiative transfer models with variable dust size distributions to generate the spectral energy distributions of disks with gaps. By comparing with transitional disk observations (e.g., GM Aur), we have found that dust filtration alone has difficulties depleting small particles sufficiently to explain the near-IR deficit of moderateṀ transitional disks, except under some extreme circumstances. The scenario of gap opening by multiple planets studied previously suffers the same difficulty. One possible solution is to invoke both dust filtration and dust growth in the inner disk. In this scenario, a planet-induced gap filters large dust particles in the disk, and the remaining small dust particles passing to the inner disk can grow efficiently without replenishment from fragmentation of large grains. Predictions for ALMA have also been made based on all these scenarios. We conclude that dust filtration with planet(s) in the disk is a promising mechanism to explain submm observations of transitional disks but it may need to be combined with other processes (e.g., dust growth) to explain the near-IR deficit of some systems.

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“…growth and fragmentation balance each other. The resulting grain size distributions tend to be power-laws or broken power-laws, which do not necessarily follow the MRN-distribution (see, Birnstiel et al, 2011). A common feature of these distributions is the fact that most of the dust mass is concentrated in the largest grains.…”

Section: Recent Growth Models and Growth Barriersmentioning

confidence: 99%

“…Below a few micrometers, the main source of collision velocities switches from turbulence to Brownian motion (see Fig. 3), which leads to a kink in the size distribution, such that particles much smaller than a micrometer do not contribute much to the total grain surface area (see, Birnstiel et al, 2011;Ormel and Okuzumi, 2013).…”

Section: Recent Growth Models and Growth Barriersmentioning

confidence: 99%

Dust Evolution in Protoplanetary Disks

Testi¹,

Birnstiel²,

Ricci³

et al. 2014

Protostars and Planets VI

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294

271

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In the core accretion scenario for the formation of planetary rocky cores, the first step toward planet formation is the growth of dust grains into larger and larger aggregates and eventually planetesimals. Although dust grains are thought to grow from the submicron sizes typical of interstellar dust to micron size particles in the dense regions of molecular clouds and cores, the growth from micron size particles to pebbles and kilometre size bodies must occur in the high densities reached in the mid-plane of protoplanetary disks. This critical step in the formation of planetary systems is the last stage of solids evolution that can be observed directly in young extrasolar systems before the appearance of large planetary-size bodies.Tracing the properties of dust in the disk mid-plane, where the bulk of the material for planet formation resides, requires sensitive observations at long wavelengths (sub-mm through cm waves). At these wavelengths, the observed emission can be related to the dust opacity, which in turns depend on to the grain size distribution. In recent years the upgrade of the existing (sub-)mm arrays, the start of ALMA Early Science operations and the upgrade of the VLA have significantly improved the observational constraints on models of dust evolution in protoplanetary disks. Laboratory experiments and numerical simulations led to a substantial improvement in the understanding of the physical processes of grain-grain collisions, which are the foundation for the models of dust evolution in disks.In this chapter we review the constraints on the physics of grain-grain collisions as they have emerged from laboratory experiments and numerical computations. We then review the current theoretical understanding of the global processes governing the evolution of solids in protoplanetary disks, including dust settling, growth, and radial transport. The predicted observational signatures of these processes are summarized.We discuss the recent developments in the study of grain growth in molecular cloud cores and in collapsing envelopes of protostars as these likely provide the initial conditions for the dust in protoplanetary disks. We then discuss the current observational evidence for the growth of grains in young protoplanetary disks from millimeter surveys, as well as the very recent evidence of radial variations of the dust properties in disks. We also include a brief discussion of the constraints on the small end of the grain size distribution and on dust settling as derived from optical, near-, and mid-IR observations. The observations are discussed in the context of global dust evolution models, in particular we focus on the emerging evidence for a very efficient early growth of grains in disks and the radial distribution of maximum grain sizes as the result of growth barriers in disks. We will also highlight the limits of the current models of dust evolution in disks including the need to slow the radial drift of grains to overcome the migration/fragmentation barrier.

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Dust size distributions in coagulation/fragmentation equilibrium: numerical solutions and analytical fits

Cited by 231 publications

References 48 publications

Formation of planetary populations − II. Effects of initial disc size and radial dust drift

Formation of planetary populations − II. Effects of initial disc size and radial dust drift

Dust Filtration by Planet-Induced Gap Edges: Implications for Transitional Disks

Dust Evolution in Protoplanetary Disks

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