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摘要
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, (CO)-C-12, (CO)-C-13, and (CO)-O-18 J = 2-1 emission from the system HD 169142 (which is observed almost face-on) at an angular resolution of similar to 1.'' 3 x 0.'' 2 (similar to 35 x 20 au). The dust continuum emission reveals a double-ring structure with an inner ring between 0.'' 17-0.'' 28 (similar to 20-35 au) and an outer ring between 0.'' 48-0.'' 64 (similar to 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 less than or similar to 20 au) or within the dust gap (similar to 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 similar to 1.'' 15 (similar to 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 (mu 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 similar to 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).
- 出版日期2017-4
