Molecules with ALMA at Planet-forming Scales (MAPS). XVI. Characterizing the Impact of the Molecular Wind on the Evolution of the HD 163296 System
Molecules with ALMA at Planet-forming Scales (MAPS). XVI. Characterizing the Impact of the Molecular Wind on the Evolution of the HD 163296 System
复制标题
DOI：
10.3847/1538-4365/ac1ad4
复制
发表时间：
2021-09
期刊：
影响因子：
--
通讯作者：
A. Booth;B. Tabone;J. Ilee;C. Walsh;Y. Aikawa;S. Andrews;J. Bae;E. Bergin;J. Bergner;A. Bos
中科院分区：
文献类型：
--
作者：
A. Booth;B. Tabone;J. Ilee;C. Walsh;Y. Aikawa;S. Andrews;J. Bae;E. Bergin;J. Bergner;A. Bos
在原行星盘演化的主要阶段，吸积调节盘内的性质，如温度和质量分布，进而调节与行星形成相关的物理条件。吸积背后的驱动机制仍然不确定;然而，一个有希望的机制是通过磁流体动力学（MHD）盘风从盘的内部几十个天文单位发射来去除一部分角动量。本文利用CO同位素发射研究独特的分子流出源的HD 163296原行星盘获得的阿塔卡马大毫米/亚毫米阵列。HD 163296是研究最充分的II类盘之一，被认为拥有多颗气体巨行星。我们在12 CO J = 2 − 1和13 CO J = 2 − 1和J = 1 − 0跃迁中稳健地探测到大尺度旋转外流。我们约束了分子气体的运动学、激发温度和质量损失率。喷射与吸积的高比率（5-50），以及气流的旋转特征，为MHD盘风提供了坚实的证据。我们发现，角动量去除风是足够的驱动吸积通过内部区域的磁盘，因此，吸积驱动湍流粘性是不需要解释HD 163296的吸积。分子风的低温及其整体运动学表明，MHD盘风可能受到先前观察到的高速原子射流的扰动和冲击。本文是《天体物理学杂志增刊》MAPS特刊的一部分。
During the main phase of evolution of a protoplanetary disk, accretion regulates the inner-disk properties, such as the temperature and mass distribution, and in turn, the physical conditions associated with planet formation. The driving mechanism behind accretion remains uncertain; however, one promising mechanism is the removal of a fraction of angular momentum via a magnetohydrodynamic (MHD) disk wind launched from the inner tens of astronomical units of the disk. This paper utilizes CO isotopologue emission to study the unique molecular outflow originating from the HD 163296 protoplanetary disk obtained with the Atacama Large Millimeter/submillimeter Array. HD 163296 is one of the most well-studied Class II disks and is proposed to host multiple gas-giant planets. We robustly detect the large-scale rotating outflow in the 12CO J = 2 − 1 and the 13CO J = 2 − 1 and J = 1 − 0 transitions. We constrain the kinematics, the excitation temperature of the molecular gas, and the mass-loss rate. The high ratio of the rates of ejection to accretion (5–50), together with the rotation signatures of the flow, provides solid evidence for an MHD disk wind. We find that the angular momentum removal by the wind is sufficient to drive accretion though the inner region of the disk; therefore, accretion driven by turbulent viscosity is not required to explain HD 163296's accretion. The low temperature of the molecular wind and its overall kinematics suggest that the MHD disk wind could be perturbed and shocked by the previously observed high-velocity atomic jet. This paper is part of the MAPS special issue of the Astrophysical Journal Supplement.