MOCCA：具有多种恒星群体的潮汐填充和未填充球状星团的全局性质
MOCCA: Global properties of tidally filling and underfilling globular star clusters with multiple stellar populations
AI总结：
本研究使用MOCCA蒙特卡洛代码模拟了200多个多群体球状星团模型，发现第一代初始为潮汐填充或略微未填充的系统最能重现银河系球状星团当前观测到的恒星比例和半径性质，为未来构建特定模型奠定了基础。
摘要：
我们探索了多种群体球状星团（GCs）各种性质的演化，涵盖了广泛的初始条件范围。我们使用MOCCA蒙特卡洛代码模拟了200多个GC模型，发现这些模型的当前性质（核心半径和半光半径、第二代（SG）恒星数量与恒星总数之比，NSG/NTOT）覆盖了银河系GCs这些量的观测值。从相对较小的SG比例值（NSG/NTOT ~ 0.25）和集中在星团内部区域的SG系统开始，我们发现，与之前的研究一致，第一代（FG）初始为潮汐填充或略微潮汐未填充的系统最能重现观测到的NSG/NTOT比率，并且其核心半径和半光半径的值是许多银河系球状星团的典型值。FG初始为潮汐未填充的模型保留了接近其初始值的NSG/NTOT值。这些模拟扩展了先前的调查，并有助于进一步约束可行初始参数的范围，更好地理解它们对当前GC性质的影响。这项调查的结果还为我们未来的调查奠定了基础，该调查旨在建立特定模型，以重现多种恒星群体性质与其他星团性质之间观测到的趋势（或缺乏趋势）。
英文摘要：
We explore the evolution of various properties of multiple-population globular clusters (GCs) for a broad range of initial conditions. We simulated over 200 GC models using the MOCCA Monte Carlo code and find that present-day properties (core and half-light radii, ratio of the number of second-generation (SG) stars to the total number of stars, NSG/NTOT) of these models cover the observed values of these quantities for Milky Way GCs. Starting with a relatively small value of the SG fraction (NSG/NTOT ~ 0.25) and a SG system concentrated in the inner regions of the cluster, we find, in agreement with previous studies, that systems in which the first-generation (FG) is initially tidally filling or slightly tidally underfilling best reproduce the observed ratios of NSG/NTOT and have values of the core and half-light radii typical of those of many Galactic globular clusters. Models in which the FG is initially tidally underfilling retain values of NSG/NTOT close to their initial values. These simulations expand previous investigations and serve to further constrain the viable range of initial parameters and better understand their influence on present-day GC properties. The results of this investigation also provide the basis for our future survey aimed at building specific models to reproduce the observed trends (or lack thereof) between the properties of multiple stellar populations and other clusters properties.
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