最近研究表明，小型近距离系外行星的半径分布呈双峰状。光蒸发模型预测这种双峰。在光蒸发的情况下，一些行星完全被剥夺了原始的H/He大气，而另一些则保留了它们。通过比较光蒸发模型和观测到的行星种群，可以揭示标准观测无法获得的行星种群细节，例如核心质量分布和核心组成。在这项工作中，我们提出了一个层次推理分析的分布接近的系外行星使用前向模型的光蒸发演化。我们使用这个模型来约束行星的核心组成，核心质量和初始大气质量分数的分布。我们发现核心质量分布是峰值的，峰值质量为$\sim 4$ M $_\oplus$。大体积岩芯成分与岩石/铁混合物一致，即贫冰和"类地球“;岩芯成分的分布范围很窄（在2 $σ$水平上铁质量分数的$\lesssim 16\%$变化），并与零一致。这一结果有利于在水/冰贫乏的环境中形成核心。我们发现，大多数行星吸积的H/He信封具有典型的质量分数$\sim 4\%$ ;只有一小部分没有吸积大量的H/He和“岩石”。我们发现，通过光蒸发形成的超级地球数量是没有大量H/He大气形成的超级地球数量的四倍。最后，我们发现核心吸积理论高估了H/He核心的吸积量，其系数为$\sim 5$，指向额外的质量损失机制（例如"蒸发“）或对核心吸积理论的修改。
英文摘要：
The radius distribution of small, close-in exoplanets has recently been shown to be bimodal. The photoevaporation model predicted this bimodality. In the photoevaporation scenario, some planets are completely stripped of their primordial H/He atmospheres, whereas others retain them. Comparisons between the photoevaporation model and observed planetary populations have the power to unveil details of the planet population inaccessible by standard observations, such as the core mass distribution and core composition. In this work, we present a hierarchical inference analysis on the distribution of close-in exoplanets using forward-models of photoevaporation evolution. We use this model to constrain the planetary distributions for core composition, core mass and initial atmospheric mass fraction. We find that the core-mass distribution is peaked, with a peak-mass of $\sim 4$M$_\oplus$. The bulk core-composition is consistent with a rock/iron mixture that is ice-poor and ``Earth-like''; the spread in core-composition is found to be narrow ($\lesssim 16\%$ variation in iron-mass fraction at the 2$σ$ level) and consistent with zero. This result favours core formation in a water/ice poor environment. We find the majority of planets accreted a H/He envelope with a typical mass fraction of $\sim 4\%$; only a small fraction did not accrete large amounts of H/He and were ``born-rocky''. We find four-times as many super-Earths were formed through photoevaporation, as formed without a large H/He atmosphere. Finally, we find core-accretion theory over-predicts the amount of H/He cores would have accreted by a factor of $\sim 5$, pointing to additional mass-loss mechanisms (e.g. ``boil-off'') or modifications to core-accretion theory.
The CO-Fuelled Time Machine: Tracing Birth Conditions and Terrestrial Planet Formation Outcomes in HD 163296 through Pebble Drift-induced CO Enhancements
A Dichotomy of the Mass-Metallicity Relation of Exoplanetary Atmospheres Demarcated by their Birthplace
Division of Science, National Astronomical Observatory of Japan（日本国立天文台科学部）；Graduate Institute for Advanced Studies, SOKENDAI（综合研究大学院大学）；Astrobiology Center（天体生物学中心）；Department of Earth and Planetary Science, The University of Tokyo（东京大学地球行星科学系）；Department of Earth and Planetary Sciences, Institute of Science Tokyo（东京科学大学地球行星科学系）；UTokyo Organization for Planetary Space Science (UTOPS), University of Tokyo（东京大学宇宙行星科学研究组织）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）
Host--Non-host Differences in Stellar Chemistry, Activity, and Birth Radius: Hints of Distinct Formation Environments for Earth-like Planets and Sub-Neptunes
School of Science, Hangzhou Dianzi University（杭州电子科技大学理学院）；National Astronomical Data Center Zhijiang Branch（国家天文台数据科学中心（紫金山））；CAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台光学天文重点实验室）；Department of Astronomy, The Ohio State University（俄亥俄州立大学天文学系）；Center for Cosmology and Astroparticle Physics (CCAPP), The Ohio State University（俄亥俄州立大学宇宙学与高能物理中心）；Department of Physics, Xiangtan University（湘潭大学物理系）；School of Physics and Astronomy, Beijing Normal University（北京师范大学物理与天文学院）
Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Universidad de Alcalá（阿尔卡拉大学）；Centro de Astrobiología (CAB) CSIC-INTA（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）；Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文台）
Bridging stellar evolution and planet formation: from birth, to survivors of the fittest, to the second generation of planets
European Southern Observatory（欧洲南方天文台）；KU Leuven（荷语鲁汶大学）；Chalmers University of Technology（查尔姆斯理工大学）；Macquarie University（麦考瑞大学）；Georgia State University（佐治亚州立大学）；University of Exeter（埃克塞特大学）；Konkoly Observatory（孔科利天文台）；Côte d’Azur Observatory（蔚蓝海岸天文台）；Universidad de Chile（智利大学）
Insights into the Exoplanet Radius Valley from Host-Star Ages, Activity, Chemistry, and Birth Radius
School of Science, Hangzhou Dianzi University（杭州电子科技大学理学院）；National Astronomical Data Center Zhijiang Branch（国家天文台紫江分中心）；CAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台光学天文重点实验室）；Department of Astronomy, The Ohio State University（俄亥俄州立大学天文学系）；Center for Cosmology and Astroparticle Physics (CCAPP), The Ohio State University（俄亥俄州立大学宇宙学与高能粒子物理中心）；School of Physics and Astronomy, Beijing Normal University（北京师范大学物理与天文学院）；School of Science, Xichang University（西昌学院理学院）
Unveiling What Makes Saturn Ring: Quantifying the Amplitudes of Saturn's Planetary Normal-Mode Oscillations and Trends in C-Ring Properties Using Kronoseismology (VII)
Probing the origins. III. Exoplanet demographics across Galactic birth radii
Universidad de Alcalá（阿尔卡拉大学）；Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Instituto de Astrofísica, Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学天体物理研究所）；Centro de Astrobiología (CAB) CSIC-INTA（CSIC-INTA 天体生物学中心）；European Space Agency (ESA), European Space Astronomy Centre (ESAC)（欧洲空间局（ESA）欧洲空间天文中心）；Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文中心）
Exploring the Sun's birth radius and the distribution of planet building blocks in the Milky Way galaxy: A multi-zone Galactic chemical evolution approach
Unveiling Complex Chemistry in Planet-forming Disks with the SKAO
University of Leeds（利兹大学）；Univ Toulouse, CNES, CNRS, IRAP（图卢兹大学，法国国家空间研究中心，法国国家科学研究中心，天体物理研究所）；Academia Sinica Institute of Astronomy and Astrophysics（中央研究院天文及天文物理研究所）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Tata Institute of Fundamental Research（塔塔基础研究所）；Institute for Research in Fundamental Sciences（伊朗基础科学研究院）；United Kingdom Astronomy Technology Centre（英国天文学技术研究中心）；National Institute of Science Education and Research（国家科学教育与研究学院）；Homi Bhabha National Institute（霍米·巴哈国立学院）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Monash University（蒙纳士大学）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；University of Leicester（莱斯特大学）
The Birth of Minor-Body Populations in the $β$ Pictoris System I: The First 25 Myr
Universidad de La Laguna (ULL)（拉古纳大学）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），CSIC-INTA）；Universidad Complutense de Madrid（马德里康普顿斯大学）；Lund University（隆德大学）
Active Galactic Nucleus Tori: Potential Birthplace to Millions of Planets
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文学中心）；New Mexico State University（新墨西哥州立大学）；CUNY Borough of Manhattan Community College（纽约市立大学曼哈顿社区学院）；American Museum of Natural History（美国自然历史博物馆）
Nautilus Space Observatory: Unveiling the Diversity and Origin of Sub-Neptunes with the Nautilus Space Observatory
Arizona State University（亚利桑那州立大学）；University of Arizona（亚利桑那大学）；Massachusetts Institute of Technology（麻省理工学院）；Harvard Paulson School of Engineering and Applied Sciences（哈佛保罗工程与应用科学学院）；Harvard University（哈佛大学）
