原行星的运动学探测：HD100546盘中的多普勒翻转
Kinematic detections of protoplanets: a Doppler-flip in the disk of HD100546
摘要：
原行星和环行星盘的热红外辐射相当难以捉摸。然而，它们是在气体和尘埃密度场中观察到的原行星盘结构的最流行解释的基石，尽管存在其他理论。气体速度场也应该带有行星-盘相互作用的印记，在分子线通道图中具有非开普勒精细结构。这种扭结或摆动的光学深度结构和合成成像的限制的影响，但它们的细节可以在原则上连接到扰动相比，流体动力学模拟。这些预测似乎已经在HD 163296和HD 97048中观察到，其中最明显的摆动被解释为嵌入行星。速度质心地图可以允许对嵌入式行星进行更鲁棒的间接检测。沿着行星尾流的非开普勒速度在原行星上经历了突然的符号反转。在减去圆盘旋转曲线之后，扰动的位置应该被识别为速度质心图中的多普勒翻转。在这里，我们改进我们的旋转曲线在扩展到磁盘与中间倾角，我们适用于深和细角分辨率CO同位素数据集。HD 163296和HD 97048中的试验未检出。然而，在HD 100546中，我们发现了一个明显的多普勒翻转，其中一个重要部分可能是由于径向流。它与连续环内一个穿过环形槽的细脊的巧合表明了一个复杂的动力学场景，其中假定的原行星可能最近经历了卵石吸积。
英文摘要：
Protoplanets and circumplanetary disks are rather elusive in their thermal IR emission. Yet they are cornerstone to the most popular interpretations for the protoplanetary disks structures observed in the gas and dust density fields, even though alternative theories exist. The gaseous velocity field should also bear the imprint of planet-disk interactions, with non-Keplerian fine structure in the molecular line channel maps. Such kinks or wiggles are affected by the optical depth structure and synthesis imaging limitations, but their detail could in principle be connected to the perturber by comparison with hydrodynamical simulations. These predictions appear to have been observed in HD163296 and HD97048, where the most conspicuous wiggles are interpreted in terms of embedded planets. The velocity centroid maps may allow for more robust indirect detections of embedded planets. The non-Keplerian velocity along the planetary wakes undergoes an abrupt sign reversal across the protoplanet. After subtraction of the disk rotation curve, the location of the perturber should be identifiable as a Doppler-flip in velocity centroid maps. Here we improve our rotation curves in an extension to disks with intermediate inclinations, which we apply to deep and fine angular resolution CO isotopologue datasets. Trials in HD163296 and in HD97048 yield non-detections. However, in HD100546 we pick-up a conspicuous Doppler-flip, an important part of which is likely due to radial flows. Its coincidence with a fine ridge crossing an annular groove inside the continuum ring suggests a complex dynamical scenario, in which the putative protoplanet might have recently undergone pebble accretion.
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