Dust distribution in protoplanetary disks

Barrière-Fouchet, Laure; Gonzalez, Jean-François; Murray, J. R.; Humble, Robin; Maddison, Sarah

doi:10.1051/0004-6361:20042249

Cited by 89 publications

(105 citation statements)

References 21 publications

(34 reference statements)

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“…It is known that grain growth occurs in this disk, as reported by Isella et al (2007) based on the slope of the dust opacity law in the interval 0.87−7 mm. Related to the inward migration, models predict the gas drag to be more efficient in intermediate sized dust particles, with small grains remaining coupled to the gas (as seen in scattered light) and boulders following marginally perturbed Keplerian orbits (e.g., Barrière-Fouchet et al 2005). Models predict a sharp cutoff of the submillimeter continuum emission when both grain growth and inward migration are considered (e.g., Laibe et al 2008), in agreement with our observations.…”

Section: Origin Of the Different Surface Brightness Profilessupporting

confidence: 83%

Unveiling the gas-and-dust disk structure in HD 163296 using ALMA observations

Gregorio-Monsalvo

Ménard

Dent

et al. 2013

A&A

169

206

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Aims. The aim of this work is to study the structure of the protoplanetary disk surrounding the Herbig Ae star HD 163296. Methods. We used high-resolution and high-sensitivity ALMA observations of the CO(3-2) emission line and the continuum at 850 μm, as well as the three-dimensional Monte Carlo radiative transfer code, MCFOST, to model the data presented in this work.Results. The CO(3-2) emission unveils for the first time at submillimeter frequencies the vertical structure details of a gaseous disk in Keplerian rotation, showing the back and front sides of a flared disk. Continuum emission at 850 μm reveals a compact dust disk with a 240 AU outer radius and a surface brightness profile that shows a very steep decline at radius larger than 125 AU. The gaseous disk is more than two times larger than the dust disk, with a similar critical radius but with a shallower radial profile. Radiative transfer models of the continuum data confirm the need for a sharp outer edge to the dust disk. The models for the CO(3-2) channel map require the disk to be slightly more geometrically thick than previous models suggested, and that the temperature at which CO gas becomes depleted (i.e., frozen out) from the outer regions of the disk midplane is T < 20 K, in agreement with previous studies.

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Section: Origin Of the Different Surface Brightness Profilessupporting

confidence: 83%

Unveiling the gas-and-dust disk structure in HD 163296 using ALMA observations

Gregorio-Monsalvo

Ménard

Dent

et al. 2013

A&A

169

206

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“…We compared our results qualitatively with theoretical models for the evolution of dust in circumstellar disks by , , Barrière-Fouchet et al (2005), and Garaud (2007), for example. The Butterfly Star is characterized as a Class I YSO and is surrounded by a circumstellar disk that is optically thick even at submm wavelengths and by a substantial envelope.…”

Section: Comparison With Theoretical Modelsmentioning

confidence: 98%

“…Sub-micron-sized dust particles, which are strongly coupled to the motion of the gas in the disk via gas drag, agglomerate through low-velocity collisions to eventually form planetesimals of several kilometers in size (e.g., Beckwith et al 2000;Dominik et al 2007;Natta et al 2007). During this coagulation process, larger particles decouple from the turbulent gas motion, settle toward the disk midplane and radially drift toward the inner parts of the disk as a result of the impact of stellar gravity and gas drag (e.g., Weidenschilling 1977;Barrière-Fouchet et al 2005;Fromang & Papaloizou 2006;D'Alessio et al 2006). The growth beyond planetesimals occurs via direct collisions, with an increasing role for gravitational focusing as masses become larger, leading to the gravitational agglomeration of these bodies to rocky planets (Safronov & Zvjagina 1969).…”

Section: Introductionmentioning

confidence: 99%

Vertical settling and radial segregation of large dust grains in the circumstellar disk of the Butterfly Star

Gräfe¹,

Wolf²,

Guilloteau³

et al. 2013

A&A

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Context. Circumstellar disks are considered to be the environment for the formation of planets. The growth of dust grains in these disks is the first step in the core accretion-gas capture planet formation scenario. Indicators and evidence of disk evolution can be traced in spatially resolved images and the spectral energy distribution (SED) of these objects. Aims. We develop a model for the dust phase of the edge-on oriented circumstellar disk of the Butterfly Star which allows one to fit observed multi-wavelength images and the SED simultaneously. Methods. Our model is based on spatially resolved high angular resolution observations at 1.3 mm, 894 μm, 2.07 μm, 1.87 μm, 1.60 μm, and 1.13 μm and an extensively covered SED ranging from 12 μm to 2.7 mm, including a detailed spectrum obtained with the Spitzer Space Telescope in the range from 12 μm to 38 μm. A parameter study based on a grid search method involving the detailed analysis of every parameter was performed to constrain the disk parameters and find the best-fit model for the independent observations. The individual observations were modeled simultaneously, using our continuum radiative transfer code. Results. We derived a model that is capable of reproducing all of the observations of the disk at the same time. We find quantitative evidence for grain growth up to ∼100 μm-sized particles, vertical settling of larger dust grains toward the disk midplane, and radial segregation of the latter toward the central star. Within our best-fit model the large grains have a distribution with a scale height of 3.7 AU at 100 AU and a radial extent of 175 AU compared to a hydrostatic scale height of 6.9 AU at 100 AU and an outer disk radius of 300 AU. Our results are consistent with current theoretical models for the evolution of circumstellar disks and the early stages of planet formation.

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“…The presence of grains with Stokes number of order unity and dust-to-gas ratios of order unity (ie.. ǫ ≃ 0.5) is expected (e.g. Barrière-Fouchet et al 2005;Zsom et al 2011). In such a situation, the right panel of Fig.…”

Section: Outward Migration Of Dust Particlesmentioning

confidence: 99%

Dust and gas mixtures with multiple grain species – a one-fluid approach

Laibe

Price

2014

Monthly Notices of the Royal Astronomical Society

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We derive the single-fluid evolution equations describing a mixture made of a gas phase and an arbitrary number of dust phases, generalising the approach developed in Laibe & Price (2014a). A generalisation for continuous dust distributions as well as analytic approximations for strong drag regimes are also provided. This formalism lays the foundation for numerical simulations of dust populations in a wide range of astrophysical systems while avoiding limitations associated with a multiple-fluid treatment.The usefulness of the formalism is illustrated on a series of analytical problems, namely the dustybox, dustyshock and dustywave problems as well as the radial drift of grains and the streaming instability in protoplanetary discs. We find physical effects specific to the presence of several dust phases and multiple drag timescales, including non-monotonic evolution of the differential velocity between phases and increased efficiency of the linear growth of the streaming instability. Interestingly, it is found that under certain conditions, large grains can migrate outwards in protoplanetary discs. This may explain the presence of small pebbles at several hundreds of astronomical units from their central star.

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Dust distribution in protoplanetary disks

Cited by 89 publications

References 21 publications

Unveiling the gas-and-dust disk structure in HD 163296 using ALMA observations

Unveiling the gas-and-dust disk structure in HD 163296 using ALMA observations

Vertical settling and radial segregation of large dust grains in the circumstellar disk of the Butterfly Star

Dust and gas mixtures with multiple grain species – a one-fluid approach

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