标题： 银河系盘的翘曲和波纹的运动学特征 显示英文标题

标题： The Kinematic Signature of the Warp and Waves in the Milky Way Disk

摘要： 使用来自LAMOST和APOGEE选择的超过170,000颗红团簇（RC）恒星，我们对不同盘族在不同$\phi$区间内的恒星$V_{Z}$随$L_{Z}$（或$R_{g}$）的变化进行了详细分析。整个RC样本恒星的$V_{Z}$表现出叠加在指数增长趋势上的波动模式，表明来自盘扭曲、盘膨胀和盘波的贡献。我们对各种群体的结果表明，薄盘的行为与整个RC样本相似，而厚盘则表现出叠加在线性增长趋势上的波动模式，这意味着盘扭曲和波动特征存在于薄盘和厚盘中，而盘膨胀特征仅存在于薄盘中。这些结果表明，盘扭曲可能由如星际磁场对盘的扰动和不对齐的暗晕等长期过程驱动。 盘弯曲的节点线在不同星族中显示略有差异，整体RC样本恒星的$\phi_{0}$ = 5.68 $\pm$ 2.91 度，薄盘恒星的$\phi_{0}$ = 5.78 $\pm$ 2.89 度，厚盘恒星的$\phi_{0}$ = 4.10 $\pm$ 3.43 度。 显示英文摘要

摘要： Using over 170,000 red clump (RC) stars selected from LAMOST and APOGEE, we conduct a detailed analysis of the stellar $V_{Z}$ as a function of $L_{Z}$ (or $R_{g}$) across different $\phi$ bins for various disk populations. The $V_{Z}$ of the whole RC sample stars exhibits a wave-like pattern superimposed on an exponentially increasing trend, indicating the contribution from disk warp, disk flare and disk waves. Our results across various populations suggest that the thin disk is similar to the whole RC sample behavior, while the thick disk displays a wave-like pattern superimposed on a linearly increasing trend, meaning that the features of disk warp and waves are present in both thin and thick disks, and the disk flare feature is only present in the thin disk. These results indicate that the disk warp is potentially driven by secular processes like disk perturbations from intergalactic magnetic fields and a misaligned dark halo. The line-of-node of the disk warp of various populations displays a slight difference, with $\phi_{0}$ = 5.68 $\pm$ 2.91 degree for the whole RC sample stars, $\phi_{0}$ = 5.78 $\pm$ 2.89 degree for the thin disk stars, and $\phi_{0}$ = 4.10 $\pm$ 3.43 degree for the thick disk stars.