Gaps and rings carved by vortices in protoplanetary dust

Barge, P.; Ricci, Luca; Carilli, Christopher L.; Ratnasingam, R. P.

doi:10.1051/0004-6361/201629918

Cited by 29 publications

(23 citation statements)

References 35 publications

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“…With this assumption we obtain the dust surface density as a function of the grain radius and the gas surface density. We have applied this model to the disk vortex obtained in the numerical simulations of Barge et al (2017). Due to dust segregation inside the vortex, the local dust to gas mass ratio l increases significantly and the slope of the size distribution p decreases.…”

Section: Discussionmentioning

confidence: 99%

Dust Concentration and Emission in Protoplanetary Disks Vortices

Sierra¹,

Lizano²,

Barge

2017

ApJ

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We study the dust concentration and emission in protoplanetary disks vortices. We extend the Lyra-Lin solution for the dust concentration of a single grain size to a power-law distribution of grain sizes n(a) ∝ a −p . Assuming dust conservation in the disk, we find an analytic dust surface density as a function of the grain radius. We calculate the increase of the dust to gas mass ratio and the slope p of the dust size distribution due to grain segregation within the vortex. We apply this model to a numerical simulation of a disk containing a persistent vortex. Due to the accumulation of large grains towards the vortex center, increases by a factor of 10 from the background disk value, and p decreases from 3.5 to 3.0. We find the disk emission at millimeter wavelengths corresponding to synthetic observations with ALMA and VLA. The simulated maps at 7 mm and 1 cm show a strong azimuthal asymmetry. This happens because, at these wavelengths, the disk becomes optically thin while the vortex remains optically thick. The large vortex opacity is mainly due to an increase in the dust to gas mass ratio. In addition, the change in the slope of the dust size distribution increases the opacity by a factor of 2. We also show that the inclusion of the dust scattering opacity substantially changes the disks images.

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Section: Discussionmentioning

confidence: 99%

Dust Concentration and Emission in Protoplanetary Disks Vortices

Sierra¹,

Lizano²,

Barge

2017

ApJ

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“…There are currently two classes of scenarios that have been proposed to explain their origin, differing from one another by the presence of a planet embedded in the disc. According to the first scenario, rings originate from self-induced dust pile-ups (Gonzalez et al 2015), dead zones (Ruge et al 2016), rapid pebble growth around condensation fronts (Zhang et al 2015), aggregate sintering (Okuzumi et al 2016), large scale instabilities due to dust settling (Lorén-Aguilar & Bate 2016), secular gravitational instabilities (Takahashi & Inutsuka 2016) or large-scale vortices (Barge et al 2017). In some of the previous models, the evidence of a gap in the emission disc maps might be the sign of a variation of the optical properties of the dust, which in turn might be related to a variation of the sticking efficiency of dust grains.…”

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confidence: 99%

Rings and gaps in the disc around Elias 24 revealed by ALMA

Dipierro

Ricci

Pérez

et al. 2018

Monthly Notices of the Royal Astronomical Society

110

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We present Atacama Large Millimeter/sub-millimeter Array (ALMA) Cycle 2 observations of the 1.3 mm dust continuum emission of the protoplanetary disc surrounding the T Tauri star Elias 24 with an angular resolution of ∼ 0.2 ′′ (∼ 28 au). The dust continuum emission map reveals a dark ring at a radial distance of 0.47 ′′ (∼ 65 au) from the central star, surrounded by a bright ring at 0.58 ′′ (∼ 81 au). In the outer disc, the radial intensity profile shows two inflection points at 0.71 ′′ and 0.87 ′′ (∼ 99 and 121 au respectively). We perform global three-dimensional smoothed particle hydrodynamic gas/dust simulations of discs hosting a migrating and accreting planet. Combining the dust density maps of small and large grains with three dimensional radiative transfer calculations, we produce synthetic ALMA observations of a variety of disc models in order to reproduce the gap-and ring-like features observed in Elias 24. We find that the dust emission across the disc is consistent with the presence of an embedded planet with a mass of ∼ 0.7 M J at an orbital radius of ∼ 60 au. Our model suggests that the two inflection points in the radial intensity profile are due to the inward radial motion of large dust grains from the outer disc. The surface brightness map of our disc model provides a reasonable match to the gap-and ring-like structures observed in Elias 24, with an average discrepancy of ∼ 5% of the observed fluxes around the gap region. Key words: protoplanetary discs -planet-disc interactions -dust, extinction 1 INTRODUCTIONWith the advent of the new generation of radio interferometers and improvements in near-infrared imaging, the field of protoplanetary discs is currently being revolutionized. Our ability to image star formation regions has dramatically increased, offering us an unprece-⋆ giovanni.dipierro@leicester.ac.uk dented opportunity to gain insight into protoplanetary disc evolution and planet formation. A recent active topic of research in this field is the characterization of substructures within protoplanetary discs. Among the wide range of morphologies of substructures imaged recently, the most fascinating and elementary ones are gapand ring-like structures, that might be linked to ongoing and/or a subsequent formation of one or more planets.Dust rings have been detected in a number of young and

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“…We just note that different physical process may give large disc perturbations. Among them, there are disc atmosphere vortices (see, e. g., Surville & Barge 2015; Barge et al 2017), charged dust grains rising above the disc due to magneto-rotational turbulence (Turner et al 2014), and accretion and disc wind instability and asymmetry.…”

Section: Introductionmentioning

confidence: 99%

UX Ori Stars Eclipses by Large-Scale Disc Perturbations

Shulman,

Grinin

2021

Preprint

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The eclipses of UX Ori type stars by large-scale disc humps are studied in detail. The influence of the hump extension on the eclipse depth and parameters of the linear polarization is modelled and compared with a compact cloud eclipse model. Eclipses were investigated both for the flared disc and for the disc with a puffing-up in the dust sublimation zone. It is shown that the large-scale hump eclipse may be significantly deeper than a compact cloud eclipse and show a greater linear polarization degree compared to it. It is also demonstrated that the hump extension together with the disc puffing-up can strongly affect the degree of polarization and colour index of the star during the eclipse. The position angle of the linear polarization may also change markedly during and after an eclipse by a large scale hump for the model with a puffed-up inner rim. Also, in this model, the maximum degree of the linear polarization can be achieved not at the brightness minimum, but closer to the end of the eclipse.

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Gaps and rings carved by vortices in protoplanetary dust

Cited by 29 publications

References 35 publications

Dust Concentration and Emission in Protoplanetary Disks Vortices

Dust Concentration and Emission in Protoplanetary Disks Vortices

Rings and gaps in the disc around Elias 24 revealed by ALMA

UX Ori Stars Eclipses by Large-Scale Disc Perturbations

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