论文标题
银河全球簇的物理和化学特性，具有从Gaia DR2数据中鉴定出的各种起源
Physical and Chemical Properties of Galactic Global Clusters with Various Origins Identified from the Gaia DR2 Data
论文作者
论文摘要
已经研究了物理参数与化学元素丰度之间的关系差异的差异，而在星系中形成的球状恒星簇中的化学元素丰度之间的差异。基于Gaia〜DR2数据的集群所假定的地层位点的信息是从文献中借来的。这些来源估计了属于银河凸起和磁盘的概率，以及与银河系合并的六个已知事件，以银河系为151〜球形簇。结果表明，所有金属贫困（$ \ rm {[fe/h]} <-1.0 $）遗传相关的球状簇具有$α$ - 元素的较高相对丰度。根据现代观点，由于II型超新星释放更多的$α$元素，并增加了质量增加的星际介质，因此建议银河系中的II型超新星质量大于增生星系中的质量。事实证明，被认为是积聚的低能基团的簇在遗传上与单个杂构云相关，与未分层的簇UKS 〜1和Liller〜1相同，很可能属于凸起。结果表明，不仅较低，而且不仅会随着轨道平均半径的增加而减小簇的质量的上限。后一个事实是由新兴簇的质量减少，其宿主星系的质量减少。已经证明，仅在具有初始质量$> 10^{6} m _ {\ odot} $的吸收球状簇中观察到一个极其多组分的恒星总体。有人提出，这些簇保留了其不断发展的恒星弹出的所有物质，由于远离我们的星系，新一代恒星形成了新一代的恒星。
The differences in the relationships between the physical parameters and the chemical-element abundances in accreted globular star clusters and those formed inside the Galaxy have been investigated. The information on the supposed formation sites of the clusters based on the Gaia~DR2 data is borrowed from the literature. Those sources estimate the probability of belonging to the Galactic bulge and disk, as well as to six known events of the merger of dwarf satellite galaxies with the Milky Way, for 151~globular clusters. It is shown that all metal-poor ($\rm{[Fe/H]}<-1.0$) genetically related globular clusters have high relative abundances of $α$-elements. According to modern views, since type II supernovae release more $α$-elements into the interstellar medium with increasing mass, it has been suggested that masses of type II supernovae in the Galaxy were greater than in the accreted galaxies. It is proved that the clusters of the low-energy group, which were considered accreted, are genetically related to a single protogalactic cloud, same as the unstratified clusters UKS~1 and Liller~1, which most likely belong to the bulge. It is shown that not only the lower but also the upper limits of the clusters' masses decrease with an increase in the average radius of their orbits. The latter fact is explained by a decrease in the masses of emerging clusters with a decrease in the masses of their host galaxies. It is demonstrated that an extremely multicomponent stellar population is observed only in accreted globular clusters with an initial mass $>10^{6}M_{\odot}$. It has been suggested that these clusters retained all the matter ejected by their evolved stars, from which new generations of stars formed due to long evolution far from our Galaxy.
