发表机构
Pontificia Universidad Católica de Chile; Universidad de Alcalá; Centro de Astrobiología (CAB) CSIC-INTA; Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（智利天主教 Pontificia 大学; 阿尔卡拉大学; 天体生物学中心（CAB）西班牙高等科学研究理事会-国家航空航天技术研究所; 波兰科学院尼古拉·哥白尼天文台）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究结合银河化学演化模型与广义加性模型，推断系外行星宿主恒星的诞生半径，发现巨行星系统多源于内盘富金属环境，而径向迁移与行星多重性无关，展示了银河考古学对系外行星统计的补充价值。
AI 中文摘要
在太阳附近观测到的恒星不一定诞生于此。径向混合可以在银河系盘面上重新分布恒星族群，使其当前的位置与形成时的环境脱钩。我们总结了一个结合银河化学演化模型与广义加性模型来推断恒星诞生半径的框架。我们将该框架应用于1327颗以薄盘为主的、具有均匀年龄、\textit{Gaia} DR3天体测量数据和\texttt{SWEET-Cat}大气参数的系外行星宿主恒星。我们发现，巨行星系统优先示踪金属丰度较高的内盘诞生环境，而仅含岩石行星的系统则不那么集中于中心区域；并且径向位移与探测到的行星多重性之间没有明确关系。向银河系内部迁移的行星宿主恒星，其系统具有更大的轨道间距；然而，这可能部分反映了行星轨道性质对宿主恒星金属丰度的已知依赖性，而非银河恒星迁移的因果效应。这些结果展示了银河考古学如何通过将行星系统与其可能的诞生环境联系起来，补充系外行星统计特征的研究。
英文摘要
Stars observed in the solar vicinity were not necessarily born there. Radial mixing can redistribute stellar populations across the Galactic disc, decoupling their present-day locations from the environments in which they formed. We summarise a framework that combines Galactic chemical evolution models with a generalised additive model to infer stellar birth radii. We apply it to 1327 predominantly thin-disc planet hosts with homogeneous ages, \textit{Gaia} DR3 astrometry, and \texttt{SWEET-Cat} atmospheric parameters. We find that giant-planet systems preferentially trace metal-rich inner-disc birth environments, whereas rocky-only systems are less centrally concentrated; and no clear relation between radial displacement and detected planet multiplicity. Planet-host stars that migrate towards the inner parts of the Galaxy have systems with larger orbital separations; however, this may partly reflect the known dependence of planetary orbital properties on host-star metallicity rather than a causal effect of Galactic stellar migration. These results illustrate how Galactic archaeology can complement exoplanet demographics by linking planetary systems to their probable birth environments.
CommentsTo appear in the Proceedings of the IAU Symposium 408
