Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region

Long, Feng; Pinilla, P.; Herczeg, Gregory J.; Harsono, Daniel; Dipierro, Giovanni; Pascucci, Ilaria; Hendler, Nathanial P.; Tazzari, Marco; Ragusa, Enrico; Salyk, Colette; Edwards, Suzan; Lodato, Giuseppe; Plas, Gerrit van de; Johnstone, Doug; Liu, Yao; Boehler, Yann; Cabrit, S.; Manara, C. F.; Ménard, F.; Mulders, Gijs D.; Nisini, B.; Fischer, William J.; Rigliaco, E.; Banzatti, Andrea; Avenhaus, H.; Gully-Santiago, Michael

doi:10.3847/1538-4357/aae8e1

Cited by 528 publications

(622 citation statements)

References 108 publications

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“…(ii) Planet formation simulations are missing some important ingredients regarding gas accretion (see also Nayakshin et al (2019)) and planet migration. The survey by Long et al (2018) in the Taurus star-forming region and the survey by Cieza et al (2019) in the Ophiuchus starforming region, on the other hand, found a significant population of very compact discs (outer disc radii ¡ 30 au). These discs are not pictured within the DSHARP sample, due to the selection biases in the DSHARP campaign (Andrews et al 2018).…”

Section: Discussionmentioning

confidence: 96%

Are the observed gaps in protoplanetary discs caused by growing planets?

Ndugu

Bitsch

Jurua

2019

Monthly Notices of the Royal Astronomical Society

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Recent detailed observations of protoplanetary discs revealed a lot of sub-structures which are mostly ring-like. One interpretation is that these rings are caused by growing planets. These potential planets are not yet opening very deep gaps in their discs. These planets instead form small gaps in the discs to generate small pressure bumps exterior to their orbits that stop the inflow of the largest dust particles. In the pebble accretion paradigm, this planetary mass corresponds to the pebble isolation mass, where pebble accretion stops and efficient gas accretion starts. We perform planet population synthesis via pebble and gas accretion including type-I and type-II migration. In the first stage of our simulations, we investigate the conditions necessary for planets to reach the pebble isolation mass and compare their position to the observed gaps. We find that in order to match the gap structures 2000 M E in pebbles is needed, which would be only available for the most metal rich stars. We then follow the evolution of these planets for a few My to compare the resulting population with the observed exoplanet populations. Planet formation in discs with these large amounts of pebbles result in mostly forming gas giants and only very little super-Earths, contradicting observations. This leads to the conclusions that either (i) the observed discs are exceptions, (ii) not all gaps in observed discs are caused by planets or (iii) that we miss some important ingredients in planet formation related to gas accretion and/or planet migration.

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Section: Discussionmentioning

confidence: 96%

Are the observed gaps in protoplanetary discs caused by growing planets?

Ndugu

Bitsch

Jurua

2019

Monthly Notices of the Royal Astronomical Society

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“…Tidal interaction can be effective in removing dust mass from a disk even in later stages when the disk is in a binary system (e.g. Artymowicz & Lubow 1994), as proposed to explain the low mm flux of some objects in Taurus by Long et al (2018). A higher than usual binary fraction could therefore explain the low disk masses observed in CrA.…”

Section: Is Cra Young?mentioning

confidence: 99%

ALMA survey of Class II protoplanetary disks in Corona Australis: a young region with low disk masses

Cazzoletti

Manara

Liu

et al. 2019

A&A

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Context. In recent years, the disk populations in a number of young star-forming regions have been surveyed with the Atacama Large Millimeter/submillimeter Array (ALMA). Understanding the disk properties and their correlation with the properties of the central star is critical to understand planet formation. In particular, a decrease of the average measured disk dust mass with the age of the region has been observed, consistent with grain growth and disk dissipation. Aims. We want to compare the general properties of disks and their host stars in the nearby (d = 160 pc) Corona Australis (CrA) star forming region to those of the disks and stars in other regions. Methods. We conducted high-sensitivity continuum ALMA observations of 43 Class II young stellar objects in CrA at 1.3 mm (230 GHz). The typical spatial resolution is ∼ 0.3 . The continuum fluxes are used to estimate the dust masses of the disks, and a survival analysis is performed to estimate the average dust mass. We also obtained new VLT/X-Shooter spectra for 12 of the objects in our sample for which spectral type information was missing.Results. 24 disks are detected, and stringent limits have been put on the average dust mass of the non-detections. Taking into account the upper limits, the average disk mass in CrA is 6 ± 3 M ⊕ . This value is significantly lower than that of disks in other young (1-3 Myr) star forming regions (Lupus, Taurus, Chamaeleon I, and Ophiuchus) and appears to be consistent with the average disk mass of the 5-10 Myr old Upper Sco. The position of the stars in our sample on the Herzsprung-Russel diagram, however, seems to confirm that that CrA has age similar to Lupus. Neither external photoevaporation nor a lower than usual stellar mass distribution can explain the low disk masses. On the other hand, a low-mass disk population could be explained if the disks are small, which could happen if the parent cloud has a low temperature or intrinsic angular momentum, or if the the angular momentum of the cloud is removed by some physical mechanism such as magnetic braking. Even in detected disks, none show clear substructures or cavities. Conclusions. Our results suggest that in order to fully explain and understand the dust mass distribution of protoplanetary disks and their evolution, it may also be necessary to take into consideration the initial conditions of star and disk formation process. These conditions at the very beginning may potentially vary from region to region, and could play a crucial role in planet formation and evolution.

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“…The morphological characterization of dust grains in protoplanetary disks is much more advanced than that of molecular species. In fact, high-resolution images at either near-IR or (sub)millimeter wavelengths are currently available for more than a hundred sources (e.g., Garufi et al 2017;Avenhaus et al 2018;Andrews et al 2018;Long et al 2018). The vast majority of these objects are Class II sources (following Lada 1987), namely stars older than ∼1 Myr that are visible at optical wavelengths and show a spectral energy distribution (SED) composed of a stellar blackbody plus a substantial IR excess from the surrounding disk.…”

Section: Introductionmentioning

confidence: 99%

ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT)

Garufi

Podio

Codella

et al. 2020

A&A

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The chemical composition of planets is determined by the distribution of the various molecular species in the protoplanetary disk at the time of their formation. To date, only a handful of disks have been imaged in multiple spectral lines with high spatial resolution. As part of a small campaign devoted to the chemical characterization of disk-outflow sources in Taurus, we report on new ALMA Band 6 (∼1.3 mm) observations with ∼0.15 (20 au) resolution toward the embedded young star DG Tau B. Images of the continuum emission reveals a dust disk with rings and, putatively, a leading spiral arm. The disk, as well as the prominent outflow cavities, are detected in CO, H 2 CO, CS, and CN; instead, they remain undetected in SO 2 , HDO, and CH 3 OH. From the absorption of the back-side outflow, we inferred that the disk emission is optically thick in the inner 50 au. This morphology explains why no line emission is detected from this inner region and poses some limitations toward the calculation of the dust mass and the characterization of the inner gaseous disk. The H 2 CO and CS emission from the inner 200 au is mostly from the disk, and their morphology is very similar. The CN emission significantly differs from the other two molecules as it is observed only beyond 150 au. This ring-like morphology is consistent with previous observations and the predictions of thermochemical disk models. Finally, we constrained the disk-integrated column density of all molecules. In particular, we found that the CH 3 OH/H 2 CO ratio must be smaller than ∼2, making the methanol non-detection still consistent with the only such ratio available from the literature (1.27 in TW Hya).

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Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region

Cited by 528 publications

References 108 publications

Are the observed gaps in protoplanetary discs caused by growing planets?

Are the observed gaps in protoplanetary discs caused by growing planets?

ALMA survey of Class II protoplanetary disks in Corona Australis: a young region with low disk masses

ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT)

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