HD 142527 B的轨道过于紧凑，无法解释许多盘结构特征
The orbit of HD 142527 B is too compact to explain many of the disc features
AI总结：
通过VLTI/GRAVITY天体测量确定HD 142527 B的紧凑轨道（半长轴10.80 au，偏心率0.47），结合三维流体动力学模拟，证明该低质量伴星无法产生观测到的约100 au空腔等盘结构。
摘要：
HD 142527 A是一颗年轻且大质量的Herbig Ae/Be恒星，周围环绕着一个具有高度结构的盘。该盘显示出众多形态结构，如旋臂、马蹄形的尘埃辐射区域、由内盘投射到外盘上的一组阴影，以及一个从约30 au延伸至约130 au的大空腔。HD 142527 A还有一个质量较低的伴星HD 142527 B（M = 0.13 ± 0.03 M☉），被认为对周围盘中观测到的大部分结构负有责任。我们收集了VLTI/GRAVITY对HD 142527的观测数据，这些数据来自我们自己的观测计划或ESO档案。我们利用这一组非均匀的数据，提取了总共七次HD 142527 A与B之间相对天体测量学的高精度测量结果，时间跨度从2017年中期到2021年初。结合文献中已有的数据，我们现在拥有对HD 142527长达9年的天体测量监测。我们使用轨道拟合工具来确定HD 142527 B的轨道参数，并将其作为三维流体动力学盘模型的输入，以判断该双星系统是否能够产生盘中观测到的结构。我们的VLTI/GRAVITY天体测量对HD 142527 B的轨道给出了极好的约束。我们表明，该伴星遵循一条半长轴a = 10.80 ± 0.22 au的轨道，具有中等偏心率（e = 0.47 ± 0.01）。对于如此紧凑的轨道，我们表明HD 142527 B只能在盘中产生约30 au的间隙和旋臂，这远小于观测所揭示的尺度。即使从理论角度来看，观测到的约100 au的空腔大小也远远超出了像HD 142527 B这样处于如此紧凑轨道上的伴星所能给出的最慷慨的预测。因此，我们得出结论，这颗低质量伴星不能单独对系统周围盘中观测到的形态负责。
英文摘要：
HD 142527 A is a young and massive Herbig Ae/Be star surrounded by a highly structured disc. The disc shows numerous morphological structures, such as spiral arms, a horseshoe region of dust emission, a set of shadows cast by an inner disc on the outer disc, and a large cavity extending from $\simeq{}$30 au to $\simeq{}$130 au. HD 142527 A also has a lower mass companion, HD 142527 B (M = 0.13 $\pm$ 0.03 $M_\odot{}$), which is thought to be responsible for most of the structures observed in the surrounding disc. We gathered VLTI/GRAVITY observations of HD 142527, either from our own programmes or from the ESO archive. We used this inhomogeneous set of data to extract a total of seven high-precision measurements of the relative astrometry between HD 142527 A and B, spread from mid-2017 to early 2021. Combined with what is available in the literature, we now have 9 yr of astrometric monitoring on HD 142527. We used orbit fitting tools to determine the orbital parameters of HD 142527 B, and used them as inputs for a 3D hydrodynamical model of the disc to determine whether or not the binary is able to create the structures observed in the disc. Our VLTI/GRAVITY astrometry gives excellent constraints on the orbit of HD 142527 B. We show that the secondary is following an orbit of semi-major axis a = 10.80 $\pm$ 0.22 au, with moderate eccentricity (e = 0.47 $\pm$ 0.01). With such a compact orbit, we show that HD 142527 B can only generate a gap and spiral arms of $\sim$30 au in the disc, which is much smaller than what is revealed by observations. Even from a theoretical standpoint, the observed cavity size of $\sim$100 au far exceeds even the most generous predictions for a companion like HD 142527 B on such a compact orbit. Thus, we conclude that the low-mass companion cannot be solely responsible for the observed morphology of the disc surrounding the system.
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