论文标题
来自Young Open Star簇的银河系的运动学，以及来自GAIA EDR3目录的数据
Kinematics of the Galaxy from Young Open Star Clusters with Data from the Gaia EDR3 Catalogue
论文作者
论文摘要
我们已经分析了Hao等人计算的适当运动和距离的开放型星团（OSC）的运动学。基于Gaia EDR3数据。平均视线速度以此列表中的许多簇而闻名。我们表明，从不同年龄的OSC的样本确定的银河旋转参数之间是良好的一致性。最有趣的结果是从平均18 Myr的967个最年轻的OSC的样本中获得的结果。特别是，我们发现了仅使用其适当的运动和距离的银河旋转角速度的以下参数： $ω__0= 28.01 \ pm0.15 $ km s $^{ - 1} $ kpc $^{ - 1}，$ $ω^{'} _ 0 = -3.674 \ pm0.040 $ km s $^{ - 1} $ kpc $^{ - 2}，$和$ and $ $ω^{''} _ 0 = 0.565 \ pm0.023 $ km s $^{ - 1} $ kpc $^{ - 3} $。银河中心周围太阳能社区的圆形旋转速度是$ v_0 = 226.9 \ pm3.1 $ km s $ s $^{ - 1} $，用于所采用的太阳的半乳酸距离$ r_0 = 8.1 = 8.1 \ pm0.1 $ kpc。螺旋密度波的参数已从233个年轻簇的空间速度确定。螺旋密度波产生的径向和切向速度扰动的振幅为$ f_r = 9.1 \ pm0.8 $ km s $ s $^{ - 1} $和$f_θ= 4.6 \ pm1.2 $ km s $ s $ s $ s $^{ - 1} $，分别为;扰动波长为$λ_r= 3.3 \ pm0.5 $ kpc和$λ_θ= 2.6 \ pm0.6 $ kpc，用于采用的四臂螺旋模式。发现太阳在螺旋密度波中的相位为$（χ_\ odot）_r \ oft-180^\ circ $。
We have analyzed the kinematics of open star clusters (OSCs) with the proper motions and distances calculated by Hao et al. based on Gaia EDR3 data. The mean line-of-sight velocities are known for a number of clusters from this list. We show that the Galactic rotation parameters determined from samples of OSCs with various ages are in good agreement between themselves. The most interesting results have been obtained from a sample of 967 youngest OSCs with a mean age of 18 Myr. In particular, we have found the following parameters of the angular velocity of Galactic rotation using only their proper motions and distances: $Ω_0 =28.01\pm0.15$ km s$^{-1}$ kpc$^{-1},$ $Ω^{'}_0=-3.674\pm0.040$ km s$^{-1}$ kpc$^{-2},$ and $Ω^{''}_0=0.565\pm0.023$ km s$^{-1}$ kpc$^{-3}$. The circular rotation velocity of the solar neighborhood around the Galactic center here is $V_0=226.9\pm3.1$ km s$^{-1}$ for the adopted Galactocentric distance of the Sun $R_0=8.1\pm0.1$ kpc. The parameters of the spiral density wave have been determined from the space velocities of 233 young clusters. The amplitudes of the radial and tangential velocity perturbations produced by the spiral density wave are $f_R=9.1\pm0.8$ km s$^{-1}$ and $f_θ=4.6\pm1.2$ km s$^{-1}$, respectively; the perturbation wavelengths are $λ_R=3.3\pm0.5$ kpc and $λ_θ=2.6\pm0.6$ kpc for the the adopted four-armed spiral pattern. The Sun's phase in the spiral density wave has been found to be $(χ_\odot)_R\approx-180^\circ$.
