Density streams in the disc winds of Classical T Tauri stars
Density streams in the disc winds of Classical T Tauri stars
复制标题
经典金牛座 T 星盘风中的密度流
DOI：
10.1093/mnras/stad2252
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发表时间：
2023
影响因子：
4.8
通讯作者：
Gameiro, J. F.
中科院分区：
文献类型：
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作者：
Petrov, P. P.;Grankin, K. N.;Babina, E. V.;Artemenko, S. A.;Romanova, M. M.;Gorda, S. Yu;Djupvik, A. A.;Gameiro, J. F.
分析了2013年至2022年经典金牛座T星RY Tau和SU Aur的光谱和光度变化。我们发现在苏与Hα线的通量径向速度房车=−50±7公里年代−1随P = 255±5 d。类似的效果之前发现RYτ与这些新数据证实:P = 21.6 d房车=−95±5公里。在这两个明星,这些变化的径向速度,,和明星的质量被开普勒定律相关,表明结构特点在圆盘平面轨道半径0.2 au在苏与RYτ和0.9 au,分别。两颗恒星的吸积盘对视线的倾斜度都很大，因此视线穿过了吸积盘风的区域。我们提出盘风的方位不对称，可能以“密度流”的形式存在，这是由吸积盘表面的子结构引起的。这些气流只有在穿过阿尔芬表面进入圆盘磁场后才会消散。这些发现为在小于1au的尺度上了解CTTS内部吸积盘的结构以及揭示与行星形成相关的轨道距离提供了可能性。
Spectral and photometric variability of the Classical T Tauri stars RY Tau and SU Aur from 2013 to 2022 is analysed. We find that in SU Aur the H α line’s flux at radial velocity RV = −50 ± 7 km s−1varies with a period P = 255 ± 5 d. A similar effect previously discovered in RY Tau is confirmed with these new data:P= 21.6 d at RV = −95 ± 5 km s. In both stars, the radial velocity of these variations, the period, and the mass of the star turn out to be related by Kepler’s law, suggesting structural features on the disc plane orbiting at radii of 0.2 au in RY Tau and 0.9 au in SU Aur, respectively. Both stars have a large inclination of the accretion disc to the line of sight – so that the line of sight passes through the region of the disc wind. We propose there is an azimuthal asymmetry in the disc wind, presumably in the form of ‘density streams,’ caused by substructures of the accretion disc surface. These streams cannot dissipate until they go beyond the Alfven surface in the disc’s magnetic field. These findings open up the possibility to learn about the structure of the inner accretion disc of CTTS on scales less than 1 au and to reveal the orbital distances related to the planet’s formation.