具有双峰流体力学解的超星团：近似解析方法
Super stellar clusters with a bimodal hydrodynamic solution: an Approximate Analytic Approach
摘要：
我们寻找一个简单的分析模型来区分星团经历双峰流体动力学解决方案，从那些能够驱动只有一个固定的风。双峰星系团在密集的内部区域经历强烈的辐射冷却，这导致超新星和恒星风注入的物质积累，并最终形成更多的恒星世代，而它们的外部区域维持稳定的风。从基本的水动力学方程出发，导出了解析公式。我们的主要假设，即在星团表面的密度尺度几乎线性的停滞半径，是基于半解析和全数值计算的结果。的解析公式允许确定的阈值机械光度，分开集群在两个解决方案中的任何一个。可以通过简单的解析表达式来确定停滞半径，从而确定在双峰状态下演化的星团以风的形式吹出或再循环到下一代恒星中的沉积物质的比例。
英文摘要：
We look for a simple analytic model to distinguish between stellar clusters undergoing a bimodal hydrodynamic solution from those able to drive only a stationary wind. Clusters in the bimodal regime undergo strong radiative cooling within their densest inner regions, which results in the accumulation of the matter injected by supernovae and stellar winds and eventually in the formation of further stellar generations, while their outer regions sustain a stationary wind. The analytic formulae are derived from the basic hydrodynamic equations. Our main assumption, that the density at the star cluster surface scales almost linearly with that at the stagnation radius, is based on results from semi-analytic and full numerical calculations. The analytic formulation allows for the determination of the threshold mechanical luminosity that separates clusters evolving in either of the two solutions. It is possible to fix the stagnation radius by simple analytic expressions and thus to determine the fractions of the deposited matter that clusters evolving in the bimodal regime blow out as a wind or recycle into further stellar generations.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
