We investigate the evolution of the abundance of fluorine in the Milky Way thick and thin discs by means of detailed chemical evolution models compared with recent observational data. The chemical evolution models adopted here have already been shown to fit the observed abundance patterns of CNO and $\alpha$-elements as well as the metallicity distribution functions for the Galactic thick and thin disc stars. We apply them here to the study of the origin and evolution of fluorine, which is still a matter of debate. First, we study the importance of the various sites proposed for the production of fluorine. Then, we apply the reference models to follow the evolution of the two different Galactic components. We conclude that rotating massive stars are important producers of F and they can set a plateau in F abundance below [Fe/H]=-0.5 dex, though its existence for [Fe/H]<-1 has yet to be confimed by extensive observations of halo stars. In order to reproduce the F abundance increase in the discs at late times, instead, a contribution from lower mass stars - single asymptotic giant branch stars and/or novae - is required. The dichotomy between the thick and thin discs is more evident in the [F/O] vs. [O/H] plot than in the [F/Fe] vs. [Fe/H] one, and we confirm that the thick disc has evolved much faster than the thin disc, in agreement with findings from the abundance patterns of other chemical elements.

中文翻译：

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太阳附近的氟：模拟银河厚盘和薄盘

与最近的观测数据相比，我们通过详细的化学演化模型研究了银河系厚圆盘和薄圆盘中氟丰度的演变。这里采用的化学演化模型已经被证明适合观测到的 CNO 和 $\alpha$ 元素的丰度模式以及银河厚盘星和薄盘星的金属丰度分布函数。我们在这里将它们应用于氟的起源和演化的研究，这仍然是一个有争议的问题。首先，我们研究了拟用于生产氟的各个地点的重要性。然后，我们应用参考模型来跟踪两个不同的银河组成部分的演变。我们得出结论，旋转的大质量恒星是 F 的重要生产者，它们可以使 F 丰度低于 [Fe/H]=-0.5 dex，尽管 [Fe/H]<-1 的存在尚未被对晕星的广泛观测所证实。相反，为了在后期重现盘中 F 丰度的增加，需要来自较低质量的恒星——单个渐近巨星分支星和/或新星——的贡献。[F/O] 与 [O/H] 图中的厚盘和薄盘之间的二分法比 [F/Fe] 与 [Fe/H] 图中的更明显，我们确认厚盘比薄圆盘进化得快得多，这与其他化学元素丰度模式的发现一致。