论文标题
质量比，山丘机构和银河中心S-Star
Mass ratio, the hills mechanism, and the galactic centre S-stars
论文作者
论文摘要
银河中心包含其中央parsec中的几个年轻人群：$ \ sim $ \ sim $ 0.05和0.5 pc之间的磁盘，以及各向同性S-Star群集在半径内进一步延伸了一个数量级。最近的观察结果（即光谱和超速级别的星）表明某些S-Star源自磁盘。特别是，S-Star可能是潮汐破坏的磁盘二进制文件的残余物。但是，在这种情况下，显然存在不一致之处：磁盘包含巨大的O和狼 - 射线星 - 射线星，而S-Stars则是较低的质量，B星。我们探讨了这种明显差异的两个不同的解释：（i）二进制中断的内置偏见，其中主要恒星的能量与中部质量轨道的能量保持近距离，而不是次级轨道和（ii）S-Star群集内巨大恒星的选择性潮汐破坏。第一个解释是合理的。另一方面，潮汐破坏并未强烈影响过去几名MYR中S明星的质量分布。
The Galactic centre contains several young populations within its central parsec: a disk between $\sim$0.05 and 0.5 pc from the centre, and the isotropic S-star cluster extending an order of magnitude further inwards in radius. Recent observations (i.e. spectroscopy and hypervelocity stars) suggest that some S-stars originate in the disk. In particular, the S-stars may be remnants of tidally disrupted disk binaries. However, there is an apparent inconsistency in this scenario: the disk contains massive O and Wolf--Rayet stars while the S-stars are lower mass, B stars. We explore two different explanations for this apparent discrepancy: (i) a built-in bias in binary disruptions, where the primary star remains closer in energy to the centre-of-mass orbit than the secondary and (ii) selective tidal disruption of massive stars within the S-star cluster. The first explanation is plausible. On the other hand, tidal disruptions have not strongly affected the mass distribution of the S-stars over the last several Myr.
