ALMA unveils rings and gaps in the protoplanetary system HD 169142: signatures of two giant protoplanets

Fedele, D.; Carney, M. T.; Hogerheijde, M. R.; Walsh, Catherine; Miotello, A.; Klaassen, Pamela; Bruderer, S.; Henning, Thomas; Dishoeck, E. F. van

doi:10.1051/0004-6361/201629860

Cited by 224 publications

(275 citation statements)

References 56 publications

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“…Such gaps in the millimeter emission from the disk have been directly imaged previously in the young Class I/II object HL Tau (ALMA Partnership et al 2015) and the nearby older Class II TW Hya (Andrews et al 2016;Nomura et al 2016), as well as in the higher-mass Herbig Ae stars HD 163296 (Isella et al 2016) and HD 169142 (Fedele et al 2017). Modeling of ALMA continuum data at 0.87 and 1.3 mm of the young Class II star AA Tau also suggests multiple gaps in this star's disk (Loomis et al 2017).…”

Section: Transition and Gapped Disksmentioning

confidence: 59%

Protoplanetary Disks in ρ Ophiuchus as Seen from ALMA

Cox

Harris

Looney

et al. 2017

ApJ

105

144

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We present a high angular resolution ( 0. 2  ), high-sensitivity ( 0.2 s~mJy) survey of the 870 μm continuum emission from the circumstellar material around 49 pre-main-sequence stars in the ρ Ophiuchus molecular cloud. Because most millimeter instruments have resided in the northern hemisphere, this represents the largest highresolution, millimeter-wave survey of the circumstellar disk content of this cloud. Our survey of 49 systems comprises 63 stars; we detect disks associated with 29 single sources, 11 binaries, 3 triple systems, and 4 transition disks. We present flux and radius distributions for these systems; in particular, this is the first presentation of a reasonably complete probability distribution of disk radii at millimeter wavelengths. We also compare the flux distribution of these protoplanetary disks with that of the disk population of the Taurus-Auriga molecular cloud. We find that disks in binaries are both significantly smaller and have much less flux than their counterparts around isolated stars. We compute truncation calculations on our binary sources and find that these disks are too small to have been affected by tidal truncation and posit some explanations for this. Lastly, our survey found three candidate gapped disks, one of which is a newly identified transition disk with no signature of a dip in infrared excess in extant observations.

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Section: Transition and Gapped Disksmentioning

confidence: 59%

Protoplanetary Disks in ρ Ophiuchus as Seen from ALMA

Cox

Harris

Looney

et al. 2017

ApJ

105

144

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“…The technique of modeling of gas and dust simultaneously presented here can be applied to other systems with ringed structures (such as the HD 169142 disk (Fedele et al 2017)) to constrain the planet mass as well as the effective viscosity, which may provide a crucial benchmark to various evolutionary models of protoplanetary disks.…”

Section: Resultsmentioning

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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“…Recent high resolution observations of protoplanetary disks at millimeter wavelengths have revealed astonishing substructures in the thermal dust emission (ALMA Partnership et al 2015;Carrasco-González et al 2016;Andrews et al 2016;Isella et al 2016;Fedele et al 2017;Macías et al 2017). For the first time, the disk scale height is resolved in to 10 AU.…”

Section: Down To 10mentioning

confidence: 99%

Radiation Hydrodynamical Turbulence in Protoplanetary Disks: Numerical Models and Observational Constraints

Flock

Nelson

Turner

et al. 2017

ApJ

143

152

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Planets are born in protostellar disks, which are now observed with enough resolution to address questions about internal gas flows. Candidates for driving the flows include magnetic forces, but ionization state estimates suggest much of the gas mass decouples from magnetic fields. Thus, hydrodynamical instabilities could play a major role. We investigate disk dynamics under conditions typical for a T Tauri system, using global 3D radiation hydrodynamics simulations with embedded particles and a resolution of 70 cells per scale height. Stellar irradiation heating is included with realistic dust opacities. The disk starts in joint radiative balance and hydrostatic equilibrium. The vertical shear instability (VSI) develops into turbulence that persists up to at least 1600 inner orbits (143 outer orbits). Turbulent speeds are a few percent of the local sound speed at the midplane, increasing to 20%, or 100 m/s, in the corona. These are consistent with recent upper limits on turbulent speeds from optically thin and thick molecular line observations of TW Hya and HD 163296. The predominantly vertical motions induced by the VSI efficiently lift particles upwards. Grains 0.1 and 1 mm in size achieve scale heights greater than expected in isotropic turbulence. We conclude that while kinematic constraints from molecular line emission do not directly discriminate between magnetic and nonmagnetic disk models, the small dust scale heights measured in HL Tau and HD 163296 favor turbulent magnetic models, which reach lower ratios of the vertical kinetic energy density to the accretion stress.

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ALMA unveils rings and gaps in the protoplanetary system HD 169142: signatures of two giant protoplanets

Cited by 224 publications

References 56 publications

Protoplanetary Disks in ρ Ophiuchus as Seen from ALMA

Protoplanetary Disks in ρ Ophiuchus as Seen from ALMA

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

Radiation Hydrodynamical Turbulence in Protoplanetary Disks: Numerical Models and Observational Constraints

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