发表机构
University of Birmingham; University of Cambridge; European Space Agency (ESA); European Space Research and Technology Centre (ESTEC); University of Groningen（伯明翰大学; 剑桥大学; 欧洲空间局（ESA）; 欧洲空间研究与技术中心（ESTEC）; 格罗宁根大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究分析45颗贫铁恒星及其64颗行星，发现恒星与行星成分间无统计学显著相关性，并指出不确定性是掩盖潜在关系的关键因素。
AI 中文摘要
行星及其宿主恒星的化学成分本质上是相互关联的，因为它们由相同的原恒星物质形成。表征这种关系为控制行星形成和演化的过程提供了关键约束。将研究重点集中在具有近太阳化学丰度的宿主恒星上，限制了我们对行星成分在更广泛化学参数空间中如何变化的理解。因此，扩大样本以包含化学成分与太阳显著不同的恒星，对于构建恒星-行星成分联系的完整图景至关重要。在此，我们特别关注贫铁宿主恒星，因为它们更可能富含α元素，并且代表了一些与太阳相比化学性质最独特的恒星（即厚盘恒星）。我们提出了一个包含45颗恒星、64颗行星的样本，这些行星位于超级地球和亚海王星区域，我们统一获得了新的恒星参数（包括丰度），重新推导了行星质量和半径，并对其行星伴星的体内部成分进行了建模。在我们的样本中，未发现恒星与行星成分之间存在统计学显著相关性的证据。我们认为，这一零结果主要归因于两种成分指标固有的较大不确定性，这些不确定性可能掩盖了潜在的关系。因此，量化这些不确定性是先前研究未完全解决的关键步骤。此外，即使提高了精度，揭示这种关系可能还需要更高维度的处理，以考虑行星平衡温度等额外参数。
英文摘要
The chemical compositions of planets and their hosts stars are intrinsically linked, having formed from the same protostellar material. Characterising this relationship provides key constraints on the processes governing planetary formation and evolution. Focusing on host stars with near-solar chemical abundances limits our understanding of how planetary composition varies across a broader chemical parameter space. Expanding the sample to include stars with compositions markedly different from the Sun is therefore essential for building a complete picture of star--planet compositional connections. Here, we focus specifically on iron-poor hosts since they are more likely to be alpha-enhanced and represent some of the most chemically distinct stars relative to the Sun (i.e., thick disc stars). We present a sample of 45 stars hosting 64 planets across the super-Earth and sub-Neptune regimes, for which we homogeneously obtain new stellar parameters including abundances, re-derive planetary mass and radius, and model the bulk interior compositions of their planetary companions. No statistically significant evidence for a correlation between stellar and planetary composition was found in our sample. We suggest that this null result is primarily driven by the large uncertainties inherent to both compositional proxies, which may obscure an underlying relationship. Quantifying these uncertainties is therefore a critical step that previous studies have not fully addressed. Furthermore, even with improved precision, uncovering such a relation may require a higher-dimensional treatment that accounts for additional parameters such as planetary equilibrium temperature.
Comments17 pages, 21 figures, accepted for publication in MNRAS
