填充银河系：结合星系形成模拟与行星族群合成模型刻画行星人口统计特征
Populating The Milky Way: Characterising Planet Demographics by Combining Galaxy Formation Simulations and Planet Population Synthesis Models
AI总结：
本文结合 HESTIA 星系形成模拟与行星族群合成模型，研究银河系不同区域的行星出现率差异，发现薄盘中巨行星出现率远高于厚盘，而低质量类地行星在厚盘更丰富，揭示了恒星金属丰度对行星人口统计特征的关键影响。
摘要：
银河系中恒星族群及其分布差异很大，这可能影响行星的人口统计特征。我们所在的本地邻域以银河系薄盘中年幼、富金属的恒星为主，而恒星晕和银河系核球则容纳了大量年老、贫金属的恒星。我们通过将高分辨率星系形成模拟与最先进的行星族群合成模型相结合，研究这些差异对银河系不同区域行星族群的影响。我们基于 Emsenhuber et al., 2021 提出的 New Generation Planet Population Synthesis 构建了一个族群模型，用于估计不同类型行星的出现率。我们将该模型应用于 HESTIA 星系形成模拟中的银河系类似物。我们研究了银河系内部富金属区域（即银河系核球和薄盘）中的行星出现率，并将其与更遥远、贫金属区域（如厚盘和恒星晕）中的出现频率进行对比。我们发现，银河系类似物中贫金属区域的行星人口统计特征与更遥远、贫金属区域的行星族群存在显著差异。巨行星（>300 M⊕）在薄盘中的出现率是厚盘中的 10 到 20 倍，这主要是由于贫金属恒星周围可用于行星形成的固态物质数量较少。类似地，类太阳恒星周围的低质量类地行星在厚盘中最为丰富，其出现频率是薄盘中的 1.5 倍。此外，低质量行星预计在整个银河系中都很丰富，从中心区域到外部晕，因为它们的形成过程对恒星金属丰度的依赖较小。与质量为 0.3 - 0.5 M⊙ 的矮星相比，类太阳恒星周围的行星族群差异更为显著。
英文摘要：
Stellar populations and their distribution differ widely across the Galaxy, which is likely to affect planet demographics. Our local neighbourhood is dominated by young, metal-rich stars in the galactic thin disc, while the stellar halo and galactic bulge host a large fraction of older, metal-poor stars. We study the impact of these variations on planet populations in different regions of the Galaxy by combining a high-resolution galaxy formation simulation with state-of-the-art planet population synthesis models. We construct a population model to estimate occurrence rates of different planet types, based on the New Generation Planet Population Synthesis by Emsenhuber et al., 2021. We apply this to a simulated Milky Way--Analogue in the HESTIA galaxy formation simulation. We study the planet occurrence rate in the metal-rich regions of the inner Galaxy, i.e. in the galactic bulge and thin disc, and contrast them to the frequencies in the more distant, metal-poor region like the thick disc and stellar halo. We find that the planet demographics in the metal-poor regions of the Milky Way-Analogue, differ strongly from the planet populations in the more distant, metal-poor regions. The occurrence rate of giant planets ($>300 M_\bigoplus$) is 10 to 20 times larger in the thin disc compared to the thick disc, driven by the low amounts of solid material available for planet formation around metal-poor stars. Similarly, low-mass Earth-like planets around Sun-like stars are most abundant in the thick disc, being 1.5 times more frequent than in the thin disc. Moreover, low-mass planets are expected to be abundant throughout the galaxy, from the central regions to the outer halo, due to their formation processes being less dependent on stellar metallicity. The planet populations differ more strongly around Sun-like stars compared to dwarfs with masses 0.3 - 0.5 $M_\odot$.
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