Investigating the Early Evolution of Planetary Systems with ALMA and the Next Generation Very Large Array

Ricci, Luca; Liu, Shang-Fei; Isella, Andrea; Li, Hui

doi:10.3847/1538-4357/aaa546

Cited by 49 publications

(53 citation statements)

References 67 publications

(70 reference statements)

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“…These features are more apparent than those in the gas ( Figure 1). As pointed out by Ricci et al (2018), such features may be observable. On the other hand, we want to emphasize that the dust concentration at Lagrangian points is not in a steady state, and the amount of dust at those points decreases with time.…”

Section: Axisymmetric and Non-axisymmetric Featuresmentioning

confidence: 82%

The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation

Zhang

Zhu

Huang

et al. 2018

ApJL

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450

607

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The Disk Substructures at High Angular Resolution Project (DSHARP) provides a large sample of protoplanetary disks having substructures which could be induced by young forming planets. To explore the properties of planets that may be responsible for these substructures, we systematically carry out a grid of 2-D hydrodynamical simulations including both gas and dust components. We present the resulting gas structures, including the relationship between the planet mass and 1) the gaseous gap depth/width, and 2) the sub/super-Keplerian motion across the gap. We then compute dust continuum intensity maps at the frequency of the DSHARP observations. We provide the relationship between the planet mass and 1) the depth/width of the gaps at millimeter intensity maps, 2) the gap edge ellipticity and asymmetry, and 3) the position of secondary gaps induced by the planet. With these relationships, we lay out the procedure to constrain the planet mass using gap properties, and study the potential planets in the DSHARP disks. We highlight the excellent agreement between observations and simulations for AS 209 and the detectability of the young Solar System analog. Finally, under the assumption that the detected gaps are induced by young planets, we characterize the young planet population in the planet mass-semimajor axis diagram. We find that the occurrence rate for > 5 M J planets beyond 5-10 au is consistent with direct imaging constraints. Disk substructures allow us probe a wide-orbit planet population (Neptune to Jupiter mass planets beyond 10 au) that is not accessible to other planet searching techniques.

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Section: Axisymmetric and Non-axisymmetric Featuresmentioning

confidence: 82%

The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation

Zhang

Zhu

Huang

et al. 2018

ApJL

Self Cite

450

607

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“…One possibility to explain the offset might be that PDS 70 b smm traces dust particles trapped at the Lagrangian point L5, about 60 • behind PDS 70 b in azimuth along its orbit. Numerical simulations predict that if the disk viscosity is low (α < 10 −4 ) solid particles might be trapped at this Lagrangian point for more than 1000 orbits (Lyra et al 2009;Ricci et al 2018;Zhang et al 2018). In the case of PDS 70 b, this would imply particle lifetimes larger than about 10 5 years.…”

Section: Discussionmentioning

confidence: 99%

Detection of Continuum Submillimeter Emission Associated with Candidate Protoplanets

Isella

Benisty

Teague

et al. 2019

ApJL

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185

172

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We present the discovery of a spatially unresolved source of sub-millimeter continuum emission (λ = 855 µm) associated with a young planet, PDS 70 c, recently detected in Hα emission around the 5 Myr old T Tauri star PDS 70. We interpret the emission as originating from a dusty circumplanetary disk with a dust mass between 2×10 −3 M ⊕ and 4.2×10 −3 M ⊕ . Assuming a standard gas-to-dust ratio of 100, the ratio between the total mass of the circumplanetary disk and the mass of the central planet would be between 10 −4 − 10 −5 . Furthermore, we report the discovery of another compact continuum source located 0.074 ± 0.013 South-West of a second known planet in this system, PDS 70 b, that was previously detected in near-infrared images. We speculate that the latter source might trace dust orbiting in proximity of the planet, but more sensitive observations are required to unveil its nature.

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“…Carr et al (2004) find evidence for transonic turbulence within 0.3 au of the disk around the young star SVS 13 based on the broadening of the water lines at infrared wavelengths, while Najita & Ádámko-vics (2017) suggest that mechanical heating from turbulence in the inner disk may be observable at UV wavelengths. On the other hand, future radio interferometers such as the Next Generation Very Large Array (Carilli et al 2015;Isella et al 2015) might allow us to study the planet-disk interaction on a scale as small as 1 au (Ricci et al 2018), and, through an analysis similar to what presented in this paper, information about the effect of Ohmic dissipation might be inferred.…”

Section: Non-ideal Mhd Effects and Disk Turbulencementioning

confidence: 99%

New Constraints on Turbulence and Embedded Planet Mass in the HD 163296 Disk from Planet–Disk Hydrodynamic Simulations

Liu

Jin

et al. 2018

ApJ

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Recent Atacama Large Millimeter and Submillimeter Array (ALMA) observations of the protoplanetary disk around the Herbig Ae star HD 163296 revealed three depleted dust gaps at 60, 100, and 160 au in the 1.3 mm continuum as well as CO depletion in the middle and outer dust gaps. However, no CO depletion was found in the inner dust gap. To examine the planet-disk interaction model, we present results of 2D two fluid (gas + dust) hydrodynamic simulations coupled with 3D radiative transfer simulations. To fit the high gas-to-dust ratio of the first gap, we find that the Shakura-Sunyaev viscosity parameter α must be very small ( 10 4  -) in the inner disk. On the other hand, a relatively large α ( 7.5 10 3´-) is required to reproduce the dust surface density in the outer disk. We interpret the variation of α as an indicator of the transition from an inner dead zone to the outer magnetorotational instability (MRI) active zone. Within ∼100 au, the HD 163296 disk's ionization level is low, and non-ideal magnetohydrodynamic effects could suppress the MRI, so the disk can be largely laminar. The disk's ionization level gradually increases toward larger radii, and the outermost disk (r 300 > au) becomes turbulent due to MRI. Under this condition, we find that the observed dust continuum and CO gas line emissions can be reasonably fit by three half-Jovian-mass planets (0.46, 0.46, and M 0.58 J ) at 59, 105, and 160 au, respectively.

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Investigating the Early Evolution of Planetary Systems with ALMA and the Next Generation Very Large Array

Cited by 49 publications

References 67 publications

The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation

The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation

Detection of Continuum Submillimeter Emission Associated with Candidate Protoplanets

New Constraints on Turbulence and Embedded Planet Mass in the HD 163296 Disk from Planet–Disk Hydrodynamic Simulations

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