沿着球状星团红巨星分支的质量损失是急剧的吗？M3的案例
Is mass loss along the red giant branch of globular clusters sharply peaked? The case of M3
摘要：
越来越多的证据表明，几个球状星团必须包含多个恒星世代，氦含量不同。这一假说有助于解释其水平分支中无法解释的特殊特征。在这个框架中，我们模拟了M3中RR Lyr周期的峰值分布，这一点到目前为止还没有得到解释。同时，我们还试图再现M3水平支星的颜色分布。我们发现，只有一个非常小的分散在沿红巨星分支的质量损失再现了良好的精度的观测数据。星团恒星之间氦含量的增强和变化是水平分支颜色延伸的起源，而尖锐的峰值质量损失是必要的，以重现RR Lyr变量的尖锐峰值周期分布。质量损失的分散度必须<~ 0.003 Msun，以与通常假设的~0.02 Msun值进行比较。这一要求代表了对调节球状星团恒星演化的物理机制的解释的实质性变化。
英文摘要：
There is a growing evidence that several globular clusters must contain multiple stellar generations, differing in helium content. This hypothesis has helped to interpret peculiar unexplained features in their horizontal branches. In this framework we model the peaked distribution of the RR Lyr periods in M3, that has defied explanation until now. At the same time, we try to reproduce the colour distribution of M3 horizontal branch stars. We find that only a very small dispersion in mass loss along the red giant branch reproduces with good accuracy the observational data. The enhanced and variable helium content among cluster stars is at the origin of the extension in colour of the horizontal branch, while the sharply peaked mass loss is necessary to reproduce the sharply peaked period distribution of RR Lyr variables. The dispersion in mass loss has to be <~ 0.003 Msun, to be compared with the usually assumed values of ~0.02 Msun. This requirement represents a substantial change in the interpretation of the physical mechanisms regulating the evolution of globular cluster stars.
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