论文标题
Masers，Radio Stars和T Tauri星星的Radcliffe浪潮的参数
Parameters of the Radcliffe wave from masers, radio stars and T Tauri stars
论文作者
论文摘要
radcliffe波的存在在属于当地臂的Masers和无线电星的位置和垂直速度中显示。这给人的印象是，在单词的全部意义上，radcliffe波的结构不是波浪。它更像是当地的高振幅爆发，迅速消失。此外，这种结构在太阳附近的幅度最大，其中主要``贡献''是古尔德皮带恒星。 Based on the spectral analysis of masers, the following estimates of the geometric and kinematic characteristics of the wave were obtained: the largest value of the vertical coordinate $z_{max}=87\pm4$ pc and the wavelength $λ=2.8\pm0.1$ kpc, the vertical velocity perturbation amplitude reaches $W_{max}=5.1\pm0.7$ km s $^{ - 1} $和垂直速度的波长为$λ= 3.9 \ pm1.6 $ kpc。拉德克利夫（Radcliffe）波还体现在尚未达到主序列阶段的非常年轻的恒星的位置。我们从Gaia Dr2 $ \ times $ allwise数据库中提取了此类恒星的样本，并从它们中获得了以下估计：$ z_ {max} = 118 \ pm3 $ pc和ewavelength $λ= 2.0 \ pm0.1 $ kpc。
The presence of the Radcliffe wave is shown both in the positions and in the vertical velocities of masers and radio stars belonging to the Local Arm. This gives the impression that the structure of the Radcliffe wave is not a wave in the full sense of the word. It is more like a local high-amplitude burst, rapidly fading away. Moreover, this structure has the largest amplitude in the immediate vicinity of the Sun, where the main ``contributors'' are the Gould Belt stars. Based on the spectral analysis of masers, the following estimates of the geometric and kinematic characteristics of the wave were obtained: the largest value of the vertical coordinate $z_{max}=87\pm4$ pc and the wavelength $λ=2.8\pm0.1$ kpc, the vertical velocity perturbation amplitude reaches $W_{max}=5.1\pm0.7$ km s$^{-1}$ and the wavelength found from vertical velocities is $λ=3.9\pm1.6$ kpc. The Radcliffe wave also manifests itself in the positions of very young stars that have not reached the main sequence stage. We extracted a sample of such stars from the Gaia DR2$\times$AllWISE database and obtained the following estimates from them: $z_{max}=118\pm3$ pc and wavelength $λ=2.0\pm0.1$ kpc.
