ALMA unveils rings and gaps in the protoplanetary system HD 169142: signatures of two giant protoplanets
Davide Fedele,M. T. Carney,Michiel R. Hogerheijde,Catherine Walsh,Catherine Walsh,Anna Miotello,Pamela Klaassen,Simon Bruderer,Th. Henning,E. F. van Dishoeck +9 more
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In this paper, the authors used ALMA observations of the dust continuum at 1.3 mm, 12 CO, 13 CO, and C18 O J = 2−1 emission from the system HD 169142 (which is observed almost face-on) at an angular resolution of ~ 35 × 20 au, revealing a double-ring structure with an inner ring between 20−35 au and an outer ring between 56−83 au.Abstract:
The protoplanetary system HD 169142 is one of the few cases where a potential candidate protoplanet has recently been detected by direct imaging in the near-infrared. To study the interaction between the protoplanet and the disk itself, observations of the gas and dust surface density structure are needed. This paper reports new ALMA observations of the dust continuum at 1.3 mm, 12 CO, 13 CO, and C18 O J = 2−1 emission from the system HD 169142 (which is observed almost face-on) at an angular resolution of ~ (~35 × 20 au). The dust continuum emission reveals a double-ring structure with an inner ring between (~20−35 au) and an outer ring between (~56−83 au). The size and position of the inner ring is in good agreement with previous polarimetric observations in the near-infrared and is consistent with dust trapping by a massive planet. No dust emission is detected inside the inner dust cavity (R ≲ 20 au) or within the dust gap (~35−56 au) down to the noise level. In contrast, the channel maps of the J = 2−1 line of the three CO isotopologs reveal gas inside the dust cavity and dust gap. The gaseous disk is also much larger than the compact dust emission; it extends to ~1 (~180 au) in radius. This difference and the sharp drop of the continuum emission at large radii point to radial drift of large dust grains (>μ m size). Using the thermo-chemical disk code dali, we modeled the continuum and the CO isotopolog emission to quantitatively measure the gas and dust surface densities. The resulting gas surface density is reduced by a factor of ~30−40 inward of the dust gap. The gas and dust distribution indicate that two giant planets shape the disk structure through dynamical clearing (dust cavity and gap) and dust trapping (double-ring dust distribution).read more
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Radiation Hydrodynamical Turbulence in Protoplanetary Disks: Numerical Models and Observational Constraints
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TL;DR: The European Research Council under the European Union's Seventh Framework Programme (FP7)/ERC, 258729 /672 /672 as mentioned in this paper, NASA Exoplanet Research program, 14XRP14_20153, 16-XRP16 20065 /672/672, STFC, St/P000592/1, ST/M001202/1/672/, CONICYT through FONDECYT, 3170657/672 /======
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Richard Teague,Richard Teague,Thomas Henning,Stéphane Guilloteau,Edwin A. Bergin,Dmitry Semenov,Anne Dutrey,Mario Flock,Uma Gorti,Tilman Birnstiel +9 more
TL;DR: In this article, the authors present an analysis of CS in TW~Hya using the $J=7-6, $5-4$ and $3-2$ transitions imaged at $\sim 0.5^{\prime\prime}$ spatial resolution, resulting in a temperature and column density profile of the CS emission region extending out to 230
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