ALMA continuum observations of the protoplanetary disk AS 209. Evidence of multiple gaps opened by a single planet

By D. Fedele, M. Tazzari, R. Booth, L. Testi, C. Clarke, Ilaria Pascucci, Á. Kóspál, D.Semenov, Simon Bruderer, Th. Henning and 12 more. 2017

133 citations recorded by the source corpus.

The paper presents new high angular resolution ALMA 1.3 mm dust continuum observations of the protoplanetary system AS 209 in the Ophiuchus star forming region. The dust continuum emission is characterized by a main central core and two prominent rings at $r = 75\,$au and $r = 130\,$au intervaled by two gaps at at $r = 62\,$au and $r = 103\,$au. The two gaps have different widths and depths, with the inner one being narrower and shallower. We determined the surface density of the millimeter dust grains using the 3D radiative transfer disk code \textsc{dali}. According to our fiducial model the inner gap is partially filled with millimeter grains while the outer gap is largely devoid of dust. The inferred surface density is compared to 3D hydrodynamical simulations (FARGO-3D) of planet-disk interaction. The outer dust gap is consistent with the presence of a giant planet ($M_{\rm planet} \sim 0.8\,M_{\rm Staturn}$); the planet is responsible for the gap opening and for the pile-up of dust at the outer edge of the planet orbit. The simulations also show that the same planet can give origin to the inner gap at $r = 62\,$au. The relative position of the two dust gaps is close to the 2:1 resonance and we have investigated the possibility of a second planet inside the inner gap. The resulting surface density (including location, width and depth of the two dust gaps) are in agreement with the observations. The properties of the inner gap pose a strong constraint to the mass of the inner planet ($M_{\rm planet} < 0.1\,M_{\rm J}$). In both scenarios (single or pair of planets), the hydrodynamical simulations suggest a very low disk viscosity ($\alpha < 10^{-4}$). Given the young age of the system (0.5 - 1 Myr), this result implies that the formation of giant planets occurs on a timescale of $\lesssim$ 1\,Myr.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/87aad70bc0d033f8dc62e15c4174aacf37edfde3

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In Astronomy and Astrophysics

1. T. Birnstiel
2. D. Wilner
3. S. Andrews
4. Xue-Ning Bai
5. Zhaohuan Zhu
6. C. Dullemond
7. A. Hughes
8. L. Ricci

In Spectroscopy

1. T. Birnstiel
2. D. Wilner
3. S. Andrews
4. C. Dullemond
5. A. Hughes
6. Xue-Ning Bai
7. C. Qi
8. Zhaohuan Zhu

Citations in the corpus

• Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region (2018, background): “…et al. 2015; Andrews et al. 2016; Isella et al. 2016; Walsh et al. 2016; Zhang et al. 2016; Cieza et al. 2017; Loomis et al. 2017; van der Plas et al. 2017; Dipierro et al. 2018; Fedele et al. 2018; van Terwisga et al. 2018), in both young and evolved systems around T Tauri and Herbig stars.”
• The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview (2018, background): “…disk population frequently exhibits substructures in the forms of rings/gaps (Zhang et al. 2016; Isella et al. 2016; Cieza et al. 2016, 2017; Loomis et al. 2017; Huang et al. 2017; Cox et al. 2017; Dipierro et al. 2018; Fedele et al. 2018; van Terwisga et al. 2018) and spirals (Pérez et al. 2016).”
• Compact Disks in a High-resolution ALMA Survey of Dust Structures in the Taurus Molecular Cloud (2019, background): “…they are imaged with sufficient angular resolution (van der Marel et al. 2013; Isella et al. 2016; Cieza et al. 2017; Loomis et al. 2017; van der Plas et al. 2017; Hendler et al. 2018; Fedele et al. 2018; Boehler et al. 2018; Dong et al. 2018; van Terwisga et al. 2018; van der Marel et al. 2019).”
• The Disk Substructures at High Angular Resolution Project (DSHARP). II. Characteristics of Annular Substructures (2018, methodology): “Of the DSHARP sample, millimeter continuum substructures have previously been reported for the disks around AS 209 (Huang et al. 2017; Fedele et al. 2018), DoAr 25 (Cox et al. 2017), Elias 24 (Cieza et al. 2017; Cox et al. 2017; Dipierro et al. 2018), Elias 27 (Pérez et al. 2016), HD 142666…”
• The Disk Substructures at High Angular Resolution Project (DSHARP). VI. Dust Trapping in Thin-ringed Protoplanetary Disks (2018, background): “…multi-ringed disk observation of HL Tau (ALMA Partnership et al. 2015) a number of such multi-ringed disks have been detected (Andrews et al. 2016; Isella et al. 2016; Cieza et al. 2017; Fedele et al. 2017, 2018; Dipierro et al. 2018; van Terwisga et al. 2018; Clarke et al. 2018; Long et al. 2018).”
• The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation (2018, background): “Previously, hydrodynamical simulations have been carried out to explain features in individual sources (e.g., Jin et al. 2016; Dipierro et al. 2018; Fedele et al. 2018).”
• A Kinematical Detection of Two Embedded Jupiter-mass Planets in HD 163296 (2018, background): “Massive planets are able to excite spiral waves which open up secondary and tertiary gaps (Bae, et al. 2017; Fedele et al. 2018), while grain growth around ice lines (Zhang et al. 2015) and the shepherding of dust by (magneto-)hydrodynamic instabilities have also been shown to produce ring like…”
• Molecules with ALMA at Planet-forming Scales (MAPS). I. Program Overview and Highlights (2021, background): “The disk is highly structured in millimeter continuum emission with at least 7 nested rings (Andrews et al. 2009; Fedele et al. 2018; Andrews et al. 2018; Huang et al. 2018b; Guzmán et al. 2018), some of which have been associated with ongoing planet formation (Guzmán et al. 2018; Favre et al.…”
• The Disk Substructures at High Angular Resolution Project (DSHARP). V. Interpreting ALMA Maps of Protoplanetary Disks in Terms of a Dust Model (2018, background): “…that protoplanetary disks do not have simple monotonically decreasing surface density profiles, but consist of multiple narrow rings (e.g., ALMA Partnership et al. 2015; Andrews et al. 2016; Isella et al. 2016; Fedele et al. 2017, 2018; Huang et al. 2018), apparently single mas- ar X iv :1 81 2.”