Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): HD 34700 A unveils an inner ring
Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): HD 34700 A unveils an inner ring
复制标题
通过附近年轻恒星成像进行的盘演化研究 (DESTINYS)：HD 34700 A 揭开了内环的面纱
DOI：
10.1051/0004-6361/202347109
复制
发表时间：
2024
影响因子：
6.5
通讯作者：
Columba G
中科院分区：
文献类型：
--
作者：
Columba G
语境。原行星盘的研究对于理解它们的演化和与周围环境的相互作用以及限制行星形成机制至关重要。我们的目标是表征年轻的二进制系统 HD 34700 A，它显示了丰富的结构和方法。利用 VLT 的高对比度成像仪器 SPHERE、LBT 的 LMIRCam 以及 ALMA 观测，我们在多个波长下分析了该系统。我们研究环和旋臂的形态以及灰尘的散射特性。我们讨论所有观察到的特征的可能原因。结果。我们首次在 Hα 带中检测到一个从 ~65 au 延伸到 ~120 au 的环，该环内部从最近的研究中已经得知。这两者具有不同的物理和几何性质。根据散射特性，外环可能由典型尺寸 aout≥ 4 µm 的晶粒组成，而内环则具有较小的典型尺寸 ain≤ 0.4 µm。两个延伸的对数旋臂源自圆盘的相对两侧。外环本身就像一个螺旋臂，与中心和延伸的子结构具有可变的径向距离。 ALMA 数据证实存在位于外环外侧中心的毫米级灰尘子结构，并检测 HD 34700 A 和 B 的未对准气体旋转模式。结论。各种观察到的特征揭示了 HD 34700 A 的复杂性，表明存在一种或多种磁盘整形物理机制。我们的发现与盘内存在尚未被发现的几个木星质量的行星以及系统通过气体云捕获或飞越与周围环境的相互作用相一致。 JWST/MIRI 或 ALMA（气体运动学）的进一步观察可以为它们提供更多线索。
Context. The study of protoplanetary disks is fundamental to understand their evolution and interaction with the surrounding environment, and to constrain planet formation mechanisms.Aims. We aim to characterise the young binary system HD 34700 A, which shows a wealth of structures.Methods. Taking advantage of the high-contrast imaging instruments SPHERE at the VLT, LMIRCam at the LBT, and of ALMA observations, we analyse this system at multiple wavelengths. We study the morphology of the rings and spiral arms and the scattering properties of the dust. We discuss the possible causes of all the observed features.Results. We detect for the first time, in theHαband, a ring extending from ~65 au to ~120 au, inside the ring which is already known from recent studies. These two have different physical and geometrical properties. Based on the scattering properties, the outer ring may consist of grains with a typical size ofaout≥ 4 µm, while the inner ring has a smaller typical size ofain≤ 0.4 µm. Two extended logarithmic spiral arms stem from opposite sides of the disk. The outer ring appears as a spiral arm itself, with a variable radial distance from the centre and extended substructures. ALMA data confirm the presence of a millimetric dust substructure centred just outside the outer ring, and detect misaligned gas rotation patterns for HD 34700 A and B.Conclusions. The complexity of HD 34700 A, revealed by the variety of observed features, suggests the existence of one or more disk-shaping physical mechanisms. Our findings are compatible with the presence inside the disk of an as of yet undetected planet of several Jupiter masses and the system interaction with the surroundings, by means of gas cloudlet capture or flybys. Further observations with JWST/MIRI or ALMA (gas kinematics) could shed more light on them.