Stellar mass

For each type of galaxy , the size distribution at given luminosity ( or stellar mass ) is well described by a log-normal function , characterized by its median R and dispersion InR .

对于给定形态的星系，在给定光度（或恒星质量）处其大小的分布较好的遵从一对数正态函数，因此可由其中值R和弥散σ（lnR）两个参数加以定量描述。

The correlation between metallicity and stellar mass of cluster galaxies is also confirmed . It is concluded that galaxy cluster Abell 2255 is formed by the gravitational interaction after the individual galaxies are formed , which supports the hierarchical model of cluster formation .

此外还确认了团星系的金属丰度与恒星质量之间的相关性，并推断星系团Abell2255是在单个星系形成后，经过引力相互作用而形成的，这一结果支持了等级成团理论。

In this paper , the properties and classifications of the stars , clusters and galaxies are described , and the distributions of stellar mass in clusters are discussed firstly .

本文首先对恒星、星团和星系的特征、分类及星团内的恒星分布情况进行简单的描述。

In fact , the process otherwise appears to be just like the accretion process feeding M81 's stellar mass black holes , even though the central black hole is millions of times more massive .

事实上，这个过程看上去就像给M81内恒星量级的黑洞吸积过程，尽管中央黑洞质量要大上数百万倍。

Also the reasonable model parameters , such as the metal yield and the stellar initial mass function , make it possible to re-produce the observed bimodal distribution of the color-magnitude diagram .

我们选取的合理的参数，如金属产率，恒星初始质量函数等使得我们能预言星系颜色分布的双峰结构。