Nine Localized Deviations from Keplerian Rotation in the DSHARP Circumstellar Disks: Kinematic Evidence for Protoplanets Carving the Gaps

Pinte, C.; Price, Daniel J.; Ménard, F.; Duchêne, Gaspard; Christiaens, Valentin; Andrews, Sean M.; Huang, Jane; Hill, T.; Plas, G. van der; Pérez, Laura; Isella, Andrea; Boehler, Yann; Dent, W. R. F.; Mentiplay, Daniel; Loomis, Ryan A.

doi:10.3847/2041-8213/ab6dda

Cited by 194 publications

(189 citation statements)

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“…Thus, the growth of the first generation of planets would have rapidly stalled due to the absence of solid material. These conclusions are in apparent conflict with Pinte et al (2020), who claim the detection of velocity "kinks" in eight of 18 circumstellar disks observed by the DSHARP program, which could be due to the presence of planets. However, we note that, if confirmed, these kinks would require the existence of planets of multiple Jupiter masses; massive planets at such large distances could have been formed by gravitational instability (see e.g., Kratter & Lodato 2016 for a recent review) rather than core-accretion.…”

Section: Discussionmentioning

confidence: 66%

Planet formation by pebble accretion in ringed disks

Morbidelli

2020

A&A

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Context. Pebble accretion is expected to be the dominant process for the formation of massive solid planets, such as the cores of giant planets and super-Earths. So far, this process has been studied under the assumption that dust coagulates and drifts throughout the full protoplanetary disk. However, observations show that many disks are structured in rings that may be due to pressure maxima, preventing the global radial drift of the dust. Aims. We aim to study how the pebble-accretion paradigm changes if the dust is confined in a ring. Methods. Our approach is mostly analytic. We derived a formula that provides an upper bound to the growth of a planet as a function of time. We also numerically implemented the analytic formulæ to compute the growth of a planet located in a typical ring observed in the DSHARP survey, as well as in a putative ring rescaled at 5 AU. Results. Planet Type I migration is stopped in a ring, but not necessarily at its center. If the entropy-driven corotation torque is desaturated, the planet is located in a region with low dust density, which severely limits its accretion rate. If the planet is instead near the ring’s center, its accretion rate can be similar to the one it would have in a classic (ringless) disk of equivalent dust density. However, the growth rate of the planet is limited by the diffusion of dust in the ring, and the final planet mass is bounded by the total ring mass. The DSHARP rings are too far from the star to allow the formation of massive planets within the disk’s lifetime. However, a similar ring rescaled to 5 AU could lead to the formation of a planet incorporating the full ring mass in less than 1/2 My. Conclusions. The existence of rings may not be an obstacle to planet formation by pebble-accretion. However, for accretion to be effective, the resting position of the planet has to be relatively near the ring’s center, and the ring needs to be not too far from the central star. The formation of planets in rings can explain the existence of giant planets with core masses smaller than the so-called pebble isolation mass.

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Section: Discussionmentioning

confidence: 66%

Planet formation by pebble accretion in ringed disks

Morbidelli

2020

A&A

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“…Recent ALMA observations have revealed protoplanetary discs with many diverse features in the gas (Teague et al 2018;Pinte et al 2020) or in the dust (Andrews et al 2018). An important question considers whether these features can be explained by the presence of planets.…”

Section: Introductionmentioning

confidence: 99%

Influence of planetary gas accretion on the shape and depth of gaps in protoplanetary discs

Bergez-Casalou

Bitsch

Pierens

et al. 2020

A&A

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It is widely known that giant planets have the capacity to open deep gaps in their natal gaseous protoplanetary discs. It is unclear, however, how gas accretion onto growing planets influences the shape and depth of their growing gaps. We performed isothermal hydrodynamical simulations with the Fargo-2D1D code, which assumes planets accreting gas within full discs that range from 0.1 to 260 AU. The gas accretion routine uses a sink cell approach, in which different accretion rates are used to cope with the broad range of gas accretion rates cited in the literature. We find that the planetary gas accretion rate increases for larger disc aspect ratios and greater viscosities. Our main results show that gas accretion has an important impact on the gap-opening mass: we find that when the disc responds slowly to a change in planetary mass (i.e., at low viscosity), the gap-opening mass scales with the planetary accretion rate, with a higher gas accretion rate resulting in a larger gap-opening mass. On the other hand, if the disc response time is short (i.e., at high viscosity), then gas accretion helps the planet carve a deep gap. As a consequence, higher planetary gas accretion rates result in smaller gap-opening masses. Our results have important implications for the derivation of planet masses from disc observations: depending on the planetary gas accretion rate, the derived masses from ALMA observations might be off by up to a factor of two. We discuss the consequences of the change in the gap-opening mass on the evolution of planetary systems based on the example of the grand tack scenario. Planetary gas accretion also impacts stellar gas accretion, where the influence is minimal due to the presence of a gas-accreting planet.

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“…Matrà et al (2018) suggested there may be a link between CO snow lines in protoplanetary discs and the subsequent locations of planetesimal belts (e.g. Andrews et al 2018;Pinte et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Multi-wavelength, spatially resolved modelling of HD 48682’s debris disc

Hengst

Marshall

Horner

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Abstract Asteroids and comets (planetesimals) are created in gas- and dust-rich protoplanetary discs. The presence of these planetesimals around main-sequence stars is usually inferred from the detection of excess continuum emission at infrared wavelengths from dust grains produced by destructive processes within these discs. Modelling of the disc structure and dust grain properties for those discs is often hindered by the absence of any meaningful constraint on the location and spatial extent of the disc. Multi-wavelength, spatially resolved imaging is thus invaluable in refining the interpretation of these systems. Observations of HD 48682 at far-infrared (Spitzer, Herschel) and sub-millimetre (JCMT, SMA) wavelengths indicated the presence of an extended, cold debris disc with a blackbody temperature of 57.9 ± 0.7 K. Here, we combined these data to perform a comprehensive study of the disc architecture and its implications for the dust grain properties. The deconvolved images revealed a cold debris belt, verified by combining a 3D radiative transfer dust continuum model with image analysis to replicate the structure using a single, axisymmetric annulus. A Markov chain Monte Carlo analysis calculated the maximum likelihood of HD48682’s disc radius ($R_{disc} = 89^{+17}_{-20}~$au), fractional width ($\Delta R_{\rm disc} = 0.41^{+0.27}_{-0.20}$), position angle ($\theta = 66{_{.}^{\circ}} 3^{+4.5}_{-4.9}$), and inclination ($\phi = 112{_{.}^{\circ}} 5^{+4.2}_{-4.2}$). HD 48682 has been revealed to host a collisionally active, broad disc whose emission is dominated by small dust grains, smin ∼ 0.6 μm, and a size distribution exponent of 3.60 ± 0.02.

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Nine Localized Deviations from Keplerian Rotation in the DSHARP Circumstellar Disks: Kinematic Evidence for Protoplanets Carving the Gaps

Cited by 194 publications

References 50 publications

Planet formation by pebble accretion in ringed disks

Planet formation by pebble accretion in ringed disks

Influence of planetary gas accretion on the shape and depth of gaps in protoplanetary discs

Multi-wavelength, spatially resolved modelling of HD 48682’s debris disc

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