根据Gaia和PCRV数据研究B-F星的动力学与其去红颜色的关系
Kinematics of B-F Stars as a Function of Their Dereddened Color from Gaia and PCRV Data
摘要：
精度优于10%的视差和来自Gaia DR 1 TGAS星表的自行，来自PCRV，Tycho-2测光，PARSEC，MIST，YaPSI，BaSTI等时线的径向速度，以及最精确的红化和消光估计已被用来分析9543个薄盘B-F星的运动学作为其去红化颜色的函数。这些恒星在赫罗图上相对于等时线的位置非常精确。这使我得出结论，在其他作者的一些运动学研究中，红化和灭绝被大大低估了。在这项研究中的速度分量U，V，W的中位精度为1.7公里/秒，虽然在范围$-0.1<(B_T-V_T)_0<0.5$之外的运动学特征是明显的偏见，由于样本的不完整性。我们已经证实了恒星相对于太阳的平均速度和恒星速度色散的变化，作为其从依巴谷数据已知的去红颜色的函数。根据TRILEGAL模型和日内瓦-哥本哈根巡天对恒星年龄的估计，这些变化可以被认为是年龄的函数。将我们的结果与太阳附近恒星运动学的其他研究结果进行比较表明，选择和红化低估几乎完全解释了结果之间的差异。可靠研究结果的频散和平均速度符合$\pm2$ km/s走廊，而比值$σ_V/σ_U$和$σ_W/σ_U$符合$\pm0.05$。基于$-0.1<(B_T-V_T)_0<0.5$范围内的所有可靠研究，即，对于年龄为0.23 - 2.4 Gyr的恒星，我们发现以km/s为单位的恒星速度色散与以Gyr为单位的年龄的$β_U=0.33$、$β_V=0.285$和$β_W=0.37$的幂成正比。
英文摘要：
Parallaxes with an accuracy better than 10% and proper motions from the Gaia DR1 TGAS catalogue, radial velocities from the PCRV, Tycho-2 photometry, PARSEC, MIST, YaPSI, BaSTI isochrones, and the most accurate reddening and extinction estimates have been used to analyze the kinematics of 9543 thin-disk B-F stars as a function of their dereddened color. These stars are located on the Hertzsprung-Russell diagram relative to the isochrones with a high accuracy. This has allowed me to conclude that the reddening and extinction were significantly underestimated in some kinematic studies of other authors. The median accuracy of the velocity components U, V, W in this study is 1.7 km/s, although outside the range $-0.1<(B_T-V_T)_0<0.5$ the kinematic characteristics are noticeably biased due to the incompleteness of the sample. We have confirmed the variations in the mean velocity of stars relative to the Sun and the stellar velocity dispersion as a function of their dereddened color known from the Hipparcos data. Given the age estimates for the stars under consideration from the TRILEGAL model and the Geneva-Copenhagen survey, these variations may be considered as variations as a function of the age. A comparison of our results with the results of other studies of the stellar kinematics near the Sun has shown that selection and reddening underestimation explain almost completely the discrepancies between the results. The dispersions and mean velocities from the results of reliable studies fit into a $\pm2$ km/s corridor, while the ratios $σ_V/σ_U$ and $σ_W/σ_U$ fit into $\pm0.05$. Based on all reliable studies in the range $-0.1<(B_T-V_T)_0<0.5$, i.e., for an age from 0.23 to 2.4 Gyr, we have found that the stellar velocity dispersions in km/s are proportional to the age in Gyr raised to the power $β_U=0.33$, $β_V=0.285$, and $β_W=0.37$.
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