论文标题
部分可观测时空混沌系统的无模型预测
Self-similar orbit-averaged Fokker-Planck equation for isotropic spherical dense clusters (iii) application of pre-collapse solution to Galactic globular clusters
论文作者
论文摘要
This is the third paper of a series of our works on the self-similar orbit-averaged Fokker-Planck (OAFP) equation.第一篇论文提供了各向同性前星形簇的方程式的精确光谱解决方案，第二篇详细介绍了模型的物理特征。 Based on the works, the present work applies the solution to the observed structural profiles of Galactic globular clusters.为了适应剖面，最基本的（准）固定模型，国王模型和变体显示了成功的结果，而它们在放松演变的后期无法应用于核心堆肥和核心堆的簇。 We propose an energy-truncated self-similar OAFP model that can apply to clusters at both the early and late stages of the evolution.该新模型符合至少一半的银河球状簇的结构曲线，同时也适用于带有分辨岩心的核心恒星。 As a main result, we provide the completion rate of core collapse against concentration for the clusters. Also, we show our new model can apply to the globular clusters even in a broad range of radii (0.01$\sim$10 arcminutes).但是，由于我们的模型包括多晶型（细长的外晕），因此对于某些簇而言，模型的潮汐半径变得不切实际。 To avoid the issue, we also propose an approximated form of the new model.最后，我们报告说，银河系具有低浓度的球状簇具有与恒星多层性相同的空间结构，并讨论了这种多趋于群集是否是一个合理的概念。
This is the third paper of a series of our works on the self-similar orbit-averaged Fokker-Planck (OAFP) equation. The first paper provided an accurate spectral solution of the equation for isotropic pre-collapse star clusters and the second detailed the physical feature of the model. Based on the works, the present work applies the solution to the observed structural profiles of Galactic globular clusters. For fitting to the profiles, the most fundamental (quasi-)stationary model, the King model, and the variants have shown successful results while they can not apply to core-collapsing and core-collapsed clusters at the late stage of the relaxation evolution. We propose an energy-truncated self-similar OAFP model that can apply to clusters at both the early and late stages of the evolution. This new model fits the structural profiles of at least half of Galactic globular clusters while it also applies to core-collapsed stars with resolved cores. As a main result, we provide the completion rate of core collapse against concentration for the clusters. Also, we show our new model can apply to the globular clusters even in a broad range of radii (0.01$\sim$10 arcminutes). However, since our model includes polytrope (elongated outer halo), the tidal radius of the model becomes unrealistically large for some clusters. To avoid the issue, we also propose an approximated form of the new model. Lastly, we report that Milky Way globular clusters with low concentrations have the same spatial structures as stellar polytropes and discuss whether such polytropic cluster is a reasonable concept.
