论文标题
银河中心S群的运动学结构
Kinematic Structure of the Galactic Center S-cluster
论文作者
论文摘要
我们对112颗恒星的运动学进行了详细分析，其中主要包括高速S群，并在银河系中心绕了超大的黑洞Sgra*。对于其中39个轨道元素而言，是已知的，其余的我们知道适当的动作。倾斜的分布和适当的运动飞行方向显着偏离统一分布，如果轨道的方向是随机的，人们期望这是人们期望的。在中央弧秒上，S簇恒星在两个圆盘上排列在两个圆盘上，其位置角度相对于银河平面，位置角度约为 +-45 o。两个方向上每个磁盘点中恒星的角动量向量，即给定磁盘中的恒星以相反的方式旋转。该结构的两极距离视线仅约25 o。该结构可能是共振过程的结果，该过程始于大约6 Myr ogo中的群集中年轻的B型恒星的形成。或者，它表明在与紧凑型恒星缔合IRS13的距离的距离处的距离处存在干扰器。
We present a detailed analysis of the kinematics of 112 stars that mostly comprise the high velocity S-cluster and orbit the super massive black hole SgrA* at the center of the Milky Way. For 39 of them orbital elements are known, for the remainder we know proper motions. The distribution of inclinations, and proper motion flight directions deviate significantly from a uniform distribution which one expects if the orientation of the orbits are random. Across the central arcseconds the S-cluster stars are arranged in two almost edge on disks that are located at a position angle approximately +-45 o with respect to the Galactic plane. The angular momentum vectors for stars in each disk point in both directions, i.e. the stars in a given disk rotate in opposite ways. The poles of this structure are located only about 25 o from the line of sight. This structure may be the result of a resonance process that started with the formation of the young B-dwarf stars in the cluster about 6 Myr ago. Alternatively, it indicated the presence of a disturber at a distance from the center comparable to the distance of the compact stellar association IRS13.
