Modeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog
Modeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog
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DOI：
10.3847/1538-4365/ab7919
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发表时间：
2019-10
期刊：
影响因子：
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通讯作者：
K. Kremer;Claire S. Ye;N. Z. Rui;Newlin C. Weatherford;S. Chatterjee;G. Fragione;C. Rodriguez;
中科院分区：
文献类型：
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作者：
K. Kremer;Claire S. Ye;N. Z. Rui;Newlin C. Weatherford;S. Chatterjee;G. Fragione;C. Rodriguez;
我们提出了一套148个独立的N体模拟球状星团（GC）计算使用的代码CMC（集群蒙特卡罗）。在10 - 13 Gyr的年龄，所产生的模型几乎涵盖了银河系GC所展示的星系团性质的全部范围，包括总质量，核心和半光半径，金属丰度和银河系距离。我们使用我们的模型来研究恒星质量黑洞在核心坍缩过程中的作用。此外，我们还研究了动力学相互作用如何影响GC中几种重要类型源的形成和演化，包括低质量X射线双星、毫秒双星、蓝离散星、激变变星、Ia型超新星、富钙瞬变和合并致密双星。虽然我们在这里的重点是旧的，低金属丰度GC，我们的CMC模拟遵循哈勃时间的集群演化，它们包括广泛的金属丰度（直到太阳），因此我们的结果也可以用于研究年轻和高金属丰度的星星集群。最后，这些模拟的输出可在www.example.com下载。
We present a set of 148 independent N-body simulations of globular clusters (GCs) computed using the code CMC (Cluster Monte Carlo). At an age of ∼10–13 Gyr, the resulting models cover nearly the full range of cluster properties exhibited by the Milky Way GCs, including total mass, core and half-light radii, metallicity, and galactocentric distance. We use our models to investigate the role that stellar-mass black holes play in the process of core collapse. Furthermore, we study how dynamical interactions affect the formation and evolution of several important types of sources in GCs, including low-mass X-ray binaries, millisecond pulsars, blue stragglers, cataclysmic variables, Type Ia supernovae, calcium-rich transients, and merging compact binaries. While our focus here is on old, low-metallicity GCs, our CMC simulations follow the evolution of clusters over a Hubble time, and they include a wide range of metallicities (up to solar), so that our results can also be used to study younger and higher-metallicity star clusters. Finally, the output from these simulations is available for download at https://cmc.ciera.northwestern.edu/home/.