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Meridional flows in the disk around a young star

机译:子午线在盘中流过一颗年轻恒星

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Protoplanetary disks are known to possess a variety of substructures in the distribution of their millimetre-sized grains, predominantly seen as rings and gaps(1), which are frequently interpreted as arising from the shepherding of large grains by either hidden, still-forming planets within the disk(2) or (magneto-)hydrodynamic instabilities(3). The velocity structure of the gas offers a unique probe of both the underlying mechanisms driving the evolution of the disk-such as movement of planet-building material from volatile-rich regions to the chemically inert midplane-and the details of the required removal of angular momentum. Here we report radial profiles of the three velocity components of gas in the upper layers of the disk of the young star HD 163296, as traced by emission from (CO)-C-12 molecules. These velocities reveal substantial flows from the surface of the disk towards its midplane at the radial locations of gaps that have been argued to be opened by embedded planets(4-7): these flows bear a striking resemblance to meridional flows, long predicted to occur during the early stages of planet formation(8-12). In addition, a persistent radial outflow is seen at the outer edge of the disk that is potentially the base of a wind associated with previously detected extended emission(12).
机译:众所周知,原行星盘在其毫米大小的颗粒分布中具有各种亚结构,主要被视为环和间隙(1),它们通常被解释为是由隐藏着但仍在形成中的行星将大颗粒切开而产生的。在磁盘(2)或(磁)流体动力学不稳定性(3)中。气体的速度结构提供了两种独特的方法来探究驱动盘演化的两种潜在机制,例如行星材料从富挥发分区域向化学惰性中平面的运动,以及所需去除角的细节。动量。在这里,我们报告了年轻恒星HD 163296盘的上层中气体的三个速度分量的径向分布,这是由(CO)-C-12分子的发射所跟踪的。这些速度揭示了从圆盘表面到其中平面在间隙的径向位置有大量流动,据认为是由嵌入行星打开的(4-7):这些流动与子午流非常相似,长期以来预计会发生在行星形成的早期阶段(8-12)。此外,在磁盘的外边缘看到持续的径向流出,这可能是与先前检测到的扩展排放相关的风的基础(12)。

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  • 来源
    《Nature》 |2019年第7778期|378-381|共4页
  • 作者单位

    Univ Michigan Dept Astron Ann Arbor MI 48109 USA;

    Carnegie Inst Sci Dept Terr Magnetism 5241 Broad Branch Rd NW Washington DC 20015 USA;

  • 收录信息 美国《科学引文索引》(SCI);美国《工程索引》(EI);美国《生物学医学文摘》(MEDLINE);美国《化学文摘》(CA);
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  • 正文语种 eng
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