Formation and Evolution of Clumpy Tidal Tails around Globular Clusters
Formation and Evolution of Clumpy Tidal Tails around Globular Clusters
复制标题
球状星团周围块状潮汐尾的形成和演化
DOI：
10.1086/426006
复制
发表时间：
2004
期刊：
影响因子：
--
通讯作者：
P. Miocchi
中科院分区：
文献类型：
--
作者：
P. D. Matteo;R. Capuzzo;P. Miocchi
本文给出了一个球状星团在一组“圈”轨道上绕三轴星系中心区运行的数值模拟结果。大约在球状星团轨道周期的四分之一之后，尾部开始形成，并且在大多数情况下，沿着星团轨道发展，显示出星团的子结构，例如在Palomar 5中观察到的。如果完全可检测到，则每个团块可含有约7000 M的β-内酰胺，即，大约是那个时期星系团质量的10%研究了尾和团簇的形态以及尾中恒星的运动学性质，并与现有的观测数据进行了比较。我们的发现是恒星速度色散在大半径处趋于平稳，与M15和ω Cen的发现一致。
We present some results of numerical simulations of a globular cluster orbiting in the central region of a triaxial galaxy on a set of "loop" orbits. Tails start forming after about a quarter of the globular cluster orbital period and develop, in most cases, along the cluster orbit, showing clumpy substructures as observed, for example, in Palomar 5. If completely detectable, clumps can contain about 7000 M⊙ each, i.e., about 10% of the cluster mass at that epoch. The morphology of tails and clumps and the kinematical properties of stars in the tails are studied and compared with available observational data. Our finding is that the stellar velocity dispersion tends to level off at large radii, in agreement with that found for M15 and ω Cen.