论文标题
通过模拟的H-R图，探索银河系和乳清星簇的起源
Exploration about the origin of galactic and extragalactic star clusters through simulated H-R diagrams
论文作者
论文摘要
目前的工作通过模拟的H-R图探索了我们星系中恒星簇的形成的起源，并在小麦哲伦云（SMC）中探讨了与观察到的星形簇进行比较。模拟研究使用恒星形成历史记录（SFH），光度函数（LF），重金属（Z）的丰度（Z）和同色库作为基本输入作为基本输入，并将它们与观察到的H-R SAT簇的H-R DAUGRAM进行比较，使用恒星形成历史（SFH），亮度函数（LF），重金属（Z）的丰度（LF），重金属（Z）和大量的等环群库来生产Markov Chain Carlo（MCMC）技术的合成H-R图。这两个图之间的基于距离的比较是通过在最佳选择bin尺寸和适当距离函数的最佳选择后通过颜色磁性图（CMD）的二维匹配来进行的。发现较重的元素（Z = 0.0004），Gaia LF以及SFH多个高斯分布的混合物可能是球状簇（GCS）形成的起源。相反，富集的培养基（z = 0.019）与GAIA LF以及双功率定律（即单峰）SFH有利。对于SMC群集，指数LF和指数SFH的选择是较差的培养基的合适组合，而beta型SFH的GAIA LF在富集的培养基中首选，用于形成星形簇。
The present work explores the origin of the formation of star clusters in our Galaxy and in Small Magellanic Cloud (SMC) through simulated H-R diagrams and compare those with observed star clusters. The simulation study produces synthetic H-R diagrams by Markov Chain Monte Carlo (MCMC) technique using star formation history (SFH), luminosity function (LF), abundance of heavy metal (Z) and a big library of isochrones as basic inputs and compares them with observed H-R diagrams of various star clusters. The distance based comparison between those two diagrams is carried out through two dimensional matching of points in Color-Magnitude Diagram (CMD) after optimal choice of bin size and appropriate distance function. It is found that a poor medium of heavy elements (Z = 0.0004), Gaia LF along with mixture of multiple Gaussian distributions of SFH may be the origin of formation of globular clusters (GCs). On the contrary, enriched medium (Z = 0.019) is favoured with Gaia LF along with double power law (i.e. unimodal) SFH. For SMC clusters, the choice of exponential LF and exponential SFH is a proper combination for poor medium whereas Gaia LF with Beta type SFH is preferred in an enriched medium for the formation of star clusters.
