The effect of a planet on the dust distribution in a 3D protoplanetary disk

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

doi:10.1051/0004-6361:20077586

Cited by 79 publications

(110 citation statements)

References 59 publications

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“…Rice et al 2006;Fouchet et al 2007;Pinilla et al 2012a;Zhu et al 2012), although with different shape and location in small and large grains depending on the planet mass and disk viscosity (e.g. de Juan Ovelar et al 2013.…”

Section: Discussion Of the Scattered Light Gapsmentioning

confidence: 99%

Direct detection of scattered light gaps in the transitional disk around HD 97048 with VLT/SPHERE

Ginski

Stolker

Pinilla

et al. 2016

A&A

132

158

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Aims. We studied the well-known circumstellar disk around the Herbig Ae/Be star HD 97048 with high angular resolution to reveal undetected structures in the disk which may be indicative of disk evolutionary processes such as planet formation. Methods. We used the IRDIS near-IR subsystem of the extreme adaptive optics imager SPHERE at the ESO/VLT to study the scattered light from the circumstellar disk via high resolution polarimetry and angular differential imaging. Results. We imaged the disk in unprecedented detail and revealed four ring-like brightness enhancements and corresponding gaps in the scattered light from the disk surface with radii between 39 au and 341 au. We derived the inclination and position angle as well as the height of the scattering surface of the disk from our observational data. We found that the surface height profile can be described by a single power law up to a separation ∼270 au. Using the surface height profile we measured the scattering phase function of the disk and found that it is consistent with theoretical models of compact dust aggregates. We discuss the origin of the detected features and find that low mass (≤1 M Jup ) nascent planets are a possible explanation.

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Section: Discussion Of the Scattered Light Gapsmentioning

confidence: 99%

Direct detection of scattered light gaps in the transitional disk around HD 97048 with VLT/SPHERE

Ginski

Stolker

Pinilla

et al. 2016

A&A

132

158

View full text Add to dashboard Cite

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“…Previous studies also found a clear dependence of the gap width with the core mass, where larger planets open wider gaps (Paardekooper & Mellema 2006;Zhu et al 2014). Finally, there are some contrasting results regarding the dependence of the gap width on the particle size (Paardekooper & Mellema 2006), but it seems that for less coupled particles the gap is wider for larger particles (Fouchet et al 2007). …”

Section: Dust Gapmentioning

confidence: 91%

How do giant planetary cores shape the dust disk?

Picogna

Kley

2015

A&A

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Context. We have been observing, thanks to ALMA, the dust distribution in the region of active planet formation around young stars. This is a powerful tool that can be used to connect observations with theoretical models and improve our understanding of the processes at play. Aims. We want to test how a multiplanetary system shapes its birth disk and to study the influence of the planetary masses and particle sizes on the final dust distribution. Moreover, we apply our model to the HL Tau system in order to obtain some insights on the physical parameters of the planets that are able to create the observed features. Methods. We follow the evolution of a population of dust particles, treated as Lagrangian particles, in two-dimensional locally isothermal disks where two equal-mass planets are present. The planets are kept in fixed orbits and they do not accrete mass.Results. The outer planet plays a major role in removing the dust particles in the co-orbital region of the inner planet and in forming a particle ring which have a steeper density gradient close to the gap edge respect to the single-planet scenario, promoting the development of vortices. The ring and gap width depend strongly on the planetary mass and particle stopping times, and for the more massive cases on the ring clumps in few stable points that are able to collect a high mass fraction. The features observed in the HL Tau system can be explained through the presence of several massive cores that shape the dust disk where the inner planet(s) have a mass of the order of 0.07 M Jup and the outer one(s) of the order of 0.35 M Jup . These values can be significantly lower if the disk mass turns out to be less than previously estimated. By decreasing the disk mass by a factor of 10, we obtain similar gap widths for planets with a mass of 10 M ⊕ and 20 M ⊕ for the inner and outer planets, respectively. Although the particle gaps are prominent, the expected gaseous gaps are barely visible.

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“…While this could adequately be tested in 2D, our ultimate goal is to study the observational signatures of grain growth in protoplanetary disks and apply the code to various non-axisymmetric problems, like disks with embedded planets. Thus we will be able to extend our previous work on the formation of planetary gaps in the dust layers of protoplanetary disks Fouchet et al 2007) to include grain growth, and study the stratification of growing dust grains in disks (see, e.g., Pinte et al 2007).…”

Section: Grain Growth In a 3d Sph Codementioning

confidence: 96%

SPH simulations of grain growth in protoplanetary disks

Laibe

Gonzalez

Fouchet³

et al. 2008

A&A

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Aims. In order to understand the first stages of planet formation, when tiny grains aggregate to form planetesimals, one needs to simultaneously model grain growth, vertical settling and radial migration of dust in protoplanetary disks. In this study, we implement an analytical prescription for grain growth into a 3D two-phase hydrodynamics code to understand its effects on the dust distribution in disks. Methods. Following the analytic derivation of Stepinski & Valageas (1997, A&A, 319, 1007, which assumes that grains stick perfectly upon collision, we implement a convenient and fast method of following grain growth in our 3D, two-phase (gas+dust) SPH code. We then follow the evolution of the size and spatial distribution of a dust population in a classical T Tauri star disk. Results. We find that the grains go through various stages of growth due to the complex interplay between gas drag, dust dynamics, and growth. Grains initially grow rapidly as they settle to the mid-plane, then experience a fast radial migration with little growth through the bulk of the disk, and finally pile-up in the inner disk where they grow more efficiently. This results in a bimodal distribution of grain sizes. Using this simple prescription of grain growth, we find that grains reach decimetric sizes in 10 5 years in the inner disk and survive the fast migration phase.

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The effect of a planet on the dust distribution in a 3D protoplanetary disk

Cited by 79 publications

References 59 publications

Direct detection of scattered light gaps in the transitional disk around HD 97048 with VLT/SPHERE

Direct detection of scattered light gaps in the transitional disk around HD 97048 with VLT/SPHERE

How do giant planetary cores shape the dust disk?

SPH simulations of grain growth in protoplanetary disks

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