核团簇形成的模拟
Simulations of Nuclear Cluster formation
摘要：
本文给出了一个由四个大质量球状星团组成的样本的完全自洽N体模拟的初步结果。星系团和星系的N体表象（总共N=1.5x10^6个粒子）允许以自然和自洽的方式包括动力学摩擦和潮汐相互作用。结果证实了球状星团的衰变和合并是形成/吸积致密核团簇的可行方案。具体而言：结果表明：（1）摩擦轨道的衰减比广义Krasekhar公式预测的快2倍;（2）先驱星系团在小于20个星系核穿越时间内发生合并;（3）NC组态至少在70个星系核穿越时间内保持准稳定状态。
英文摘要：
Preliminary results are presented about a fully self-consistent N-body simulation of a sample of four massive globular clusters in close interaction within the central region of a galaxy. The N-body representation (with N=1.5x10^6 particles in total) of both the clusters and the galaxy allows to include in a natural and self-consistent way dynamical friction and tidal interactions. The results confirm the decay and merging of globulars as a viable scenario for the formation/accretion of compact nuclear clusters. Specifically: i) the frictional orbital decay is about 2 times faster than that predicted by the generalized Chandrasekhar formula; ii) the progenitor clusters merge in less than 20 galactic core-crossing time; iii) the NC configuration keeps a quasi-stable state at least within 70 galactic core-crossing times.
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