论文标题
在原子碳发射中检测到的局部运动学结构在空间上与HD 163296磁盘中的拟议的原子星座一致
A localized kinematic structure detected in atomic carbon emission spatially coincident with a proposed protoplanet in the HD 163296 disk
论文作者
论文摘要
在过去的五年中，对原星磁盘的运动学的研究导致发现了新的原始球星候选者和与可能的行星盘相互作用相关的几种结构。我们在HD 163296磁盘中检测到一个局部的运动学双极结构，这是在原子碳线发射的48 au处最深的灰尘间隙内的。 HD 163296的恒星喷射和分子风在文献中详细描述了；但是，C I发射中的运动学异常与任何一个都不相关。此外，运动学结构点的速度表明成分足够快，可以将其与磁盘的开普勒轮廓区分开。它的原子性质暗示了足够强的局部紫外线源可以解离CO并发射C I流出，或者与磁盘上层的强极流相处。通过丢弃恒星射流并以前观察到的分子风，我们探索了C I发射中这种运动学特征的不同来源，该来源可能与原始球星流入/流出/流出或磁盘风有关。
Over the last five years, studies of the kinematics in protoplanetary disks have led to the discovery of new protoplanet candidates and several structures linked to possible planet-disk interactions. We detect a localized kinematic bipolar structure in the HD 163296 disk present inside the deepest dust gap at 48 au from atomic carbon line emission. HD 163296's stellar jet and molecular winds have been described in detail in the literature; however, the kinematic anomaly in C I emission is not associated with either of them. Further, the velocity of the kinematic structure points indicates a component fast enough to differentiate it from the Keplerian profile of the disk; and its atomic nature hints at a localized UV source strong enough to dissociate CO and launch a C I outflow, or a strong polar flow from the upper layers of the disk. By discarding the stellar jet and previously observed molecular winds, we explore different sources for this kinematic feature in C I emission that could be associated with a protoplanet inflow/outflow, or disk winds.
