核坍缩和核振荡的直接N体模型
A direct N-body model of core-collapse and core oscillations
摘要：
我们报告的结果，一个星团，开始与N = 200 000，包括195 000单星和5 000原始双星的直接N体模拟。用于模拟的代码包括恒星演化、双星演化、外部潮汐场和两体弛豫效应。模型星团演化到12 Gyr，在此过程中失去了超过80%的恒星。它在10.5 Gyr时达到主核心崩溃阶段的结束，并从该点开始经历核心振荡-这一现象的直接数值确认。然而，我们发现，在进一步1 Gyr的核心振荡停止喷射的两个黑洞组成的大规模的二进制从核心，产生一个核心，没有显示出以前的核心崩溃的签名。我们还表明，以前的研究结果与N范围从500到100 000标度以及这个新的模型与更大的N。特别是，时间尺度的核心崩溃（在单位的松弛时间尺度），质量偏析，速度分散，和能源的二进制人口都表现出类似的行为在不同的N。
英文摘要：
We report on the results of a direct N-body simulation of a star cluster that started with N = 200 000, comprising 195 000 single stars and 5 000 primordial binaries. The code used for the simulation includes stellar evolution, binary evolution, an external tidal field and the effects of two-body relaxation. The model cluster is evolved to 12 Gyr, losing more than 80% of its stars in the process. It reaches the end of the main core-collapse phase at 10.5 Gyr and experiences core oscillations from that point onwards -- direct numerical confirmation of this phenomenon. However, we find that after a further 1 Gyr the core oscillations are halted by the ejection of a massive binary comprised of two black holes from the core, producing a core that shows no signature of the prior core-collapse. We also show that the results of previous studies with N ranging from 500 to 100 000 scale well to this new model with larger N. In particular, the timescale to core-collapse (in units of the relaxation timescale), mass segregation, velocity dispersion, and the energies of the binary population all show similar behaviour at different N.
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