Within the birth environment of a massive globular cluster, the combination of a luminous young stellar population and a high column density induces a state in which the thermal optical depth and radiation pressure are both appreciable. In this state, the sonic mass scale, which influences the peak of the stellar mass function, is tied to a fundamental scale composed of the Planck mass and the mass per particle. Thermal feedback also affects the opacity-limited minimum mass and how protostellar outflows and binary fragmentation modify stellar masses. Considering the regions that collapse to form massive stars, we argue that thermal stabilization is likely to flatten the high-mass slope of the initial mass function. Among regions that are optically thick to thermal radiation, we expect the stellar population to become increasingly top-heavy at higher column densities, although this effect can be offset by lowering the metallicity. A toy model is presented that demonstrates these effects and in which radiation pressure leads to gas dispersal before all of the mass is converted into stars.

中文翻译：

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强烈的星团形成：恒星质量、质量函数和基本质量尺度


在大质量球状星团的诞生环境中，发光的年轻恒星群和高柱密度的结合导致了一种热光学深度和辐射压力都相当可观的状态。在这种状态下，影响恒星质量函数峰值的声质量尺度与由普朗克质量和每个粒子的质量组成的基本尺度相关联。热反馈还会影响不透明度限制的最小质量以及原恒星流出和双星碎裂如何改变恒星质量。考虑到坍缩形成大质量恒星的区域，我们认为热稳定可能会使初始质量函数的高质量斜率变平。在对热辐射光学较厚的区域中，我们预计恒星种群在较高的柱密度下会变得越来越头重脚轻，尽管这种影响可以通过降低金属丰度来抵消。提出了一个玩具模型来演示这些效应，其中辐射压力导致气体扩散，然后所有质量都转化为恒星。