发表机构
University of Zurich; Rice University; Carnegie Institution for Science; SRON, Space Research Organisation Netherlands（苏黎世大学; 莱斯大学; 卡内基科学机构; 荷兰空间研究组织）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究针对小质量恒星周围巨型系外行星，利用GEMS观测数据结合模型分析其金属丰度，指出需借助JWST和Ariel望远镜的大气测量数据改善简并性，以约束行星形成理论。
AI 中文摘要
围绕小质量恒星运行的巨型行星是一类独特的巨型行星群体，可用于约束行星形成理论。对M型矮星周围凌日巨型系外行星的调查（GEMS）可测量其质量和半径，进而用于估算其整体密度。将这些观测结果与内部结构和演化模型相结合，可得出这些行星的整体金属丰度，但该过程存在简并性，而大气金属丰度的测量可改善这种简并性。整体金属丰度的估算对我们理解行星形成时标和质量预算至关重要，尤其在这些行星与恒星质量比极端的系统中。本文表明，GEMS的低整体金属丰度是行星形成过程以及形成后星子捕获效率低的自然结果。为从经验上验证这一点，我们需要更多拥有大气测量数据的GEMS样本，这可减少行星内部建模的部分简并性。利用詹姆斯·韦布空间望远镜（JWST）和Ariel望远镜测量GEMS的大气成分，对于更好理解这类处于标准行星形成条件末端的独特行星类型至关重要。
英文摘要
Giant planets orbiting low-mass stars represent a unique population of giant planets that can be studied to constrain planet formation theory. Surveys of transiting giant exoplanets around M-dwarfs (GEMS) allow for measurement of their masses and radii, which in turn can be used to estimate their bulk densities. Coupling these observations to interior structure and evolution models can yield the bulk metallicity of these planets, however there are degeneracies to this that are improved by measurements of atmospheric metallicity. Estimates of bulk metallicity can be crucial to our understanding of planet formation timescales and mass budgets, particularly in these extreme (planet-to-star) mass ratio systems. Here we show that GEMS are expected to have a low bulk metallicity as a natural result of the planet formation process, and the low efficiency of planetesimal capture post-formation. To test this empirically, we need a larger sample of GEMS with atmospheric measurements, which can reduce some of the degeneracies with the interior modelling of planets. Measuring the atmospheric composition of GEMS with JWST and Ariel will be crucial for better understanding this unique planetary type, which sits at the tail of standard planet formation conditions.
Commentssubmitted to RAS Techniques and Instruments, Special issue on "Ariel: mission, science & community engagement"
