Exoplanet discoveries have reached into the realm of terrestrial planets that are becoming the subject of atmospheric studies. One such discovery is LHS 3844b, a 1.3 Earth radius planet in a 0.46 day orbit around an M4.5-5 dwarf star. Follow-up observations indicate that the planet is largely devoid of substantial atmosphere. This lack of significant atmosphere places astrophysical and geophysical constraints on LHS 3844b, primarily the degree of volatile outgassing and the rate of atmosphere erosion. We estimate the age of the host star as $7.8\pm1.6$ Gyrs and find evidence of an active past comparable to Proxima Centauri. We use geodynamical models of volcanic outgassing and atmospheric erosion to show that the apparent lack of atmosphere is consistent with a volatile-poor mantle for LHS 3844b. We show the core is unlikely to host enough C to produce a sufficiently volatile-poor mantle, unless the bulk planet is volatile-poor relative to Earth. While we cannot rule out a giant impact stripping LHS 3844b's atmosphere, we show this mechanism would require significant mantle stripping, potentially leaving LHS 3844b as an Fe-rich "super-Mercury". Atmospheric erosion by smaller impacts is possible, but only if the planet has already begun degassing and is bombarded by $10^3$ impactors of radius 500-1000 km traveling at escape velocity. We discuss formation and migration scenarios that could account for a volatile poor origin, including the potential for an unobserved massive companion planet. A relatively volatile-poor composition of LHS 3844b suggests that the planet formed interior to the system snow-line.
A Thick Volatile Atmosphere on the Ultrahot Super-Earth TOI-561 b
Carnegie Institution for Science（卡内基科学研究所）；The University of Birmingham（伯明翰大学）；University of Waterloo（滑铁卢大学）；Université de Montréal（蒙特利尔大学）；University of Groningen（格罗宁根大学）；University of Toronto（多伦多大学）；University of Oxford（牛津大学）；Stanford University（斯坦福大学）
TOI-561 b 被发现拥有厚挥发大气层，挑战了超短周期行星大气脱水的传统观念，揭示了其可能的地质演化过程。
Physicochemical Controls on the Compositions of the Earth and Planets
ETH Zürich（苏黎世联邦理工学院）；Consiglio Nazionale delle Ricerche (CNR)（意大利国家研究委员会）；Max Planck Institute for Solar System Research（马普太阳系研究所）；Université Côte d’Azur（蔚蓝海岸大学）；Collège de France（法兰西学院）；University of California Santa Cruz（加州大学圣克鲁兹分校）
Enriched volatiles and refractories but deficient titanium on the dayside atmosphere of WASP-121b revealed by JWST/NIRISS
Observatoire astronomique de l’Université de Genève（日内瓦大学天文台）；Trottier Institute for Research on Exoplanets, Department of Physics, Université de Montréal（蒙特利尔大学物理系特罗蒂尔系外行星研究所）；Trottier Space Institute at McGill（麦吉尔大学特罗蒂尔太空研究所）；Department of Earth & Planetary Sciences, McGill University（麦吉尔大学地球与行星科学系）；Department of Earth, Planetary, and Space Sciences, University of California, Los Angeles（加州大学洛杉矶分校地球、行星与空间科学系）；Department of Astronomy, University of Michigan（密歇根大学天文学系）；School of Physics and Astronomy, University of St Andrews（圣安德鲁斯大学物理与天文学学院）
Late infall of molecular cloud material reshaped the outer Solar System
Centre for Star and Planet Formation, Globe Institute, University of Copenhagen（哥本哈根大学环球学院恒星与行星形成中心）；School of Earth Sciences, University of Bristol（布里斯托大学地球科学学院）
Super-Earth Interiors Shrink by About 10% as They Crystallise
Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）；Department of Earth and Planetary Sciences, ETH Zurich（苏黎世联邦理工学院地球与行星科学系）
Planetesimal Formation Across the Stellar Mass Spectrum and its Influence on Exoplanet-Inherited Volatile Budgets
University of Exeter（埃克塞特大学）；Max Planck Institute for Solar System Research（马克斯·普朗克太阳系研究所）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）
Geophysical and atmospheric implications of $f$O$_{2}$-dependent melting on rocky exoplanets
Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；Netherlands eScience Center（荷兰e科学中心）；Interuniversity Micro Electronics Centre（跨大学微电子中心）；Institute of Geochemistry and Petrology, Department of Earth and Planetary Sciences, ETH Zürich（苏黎世联邦理工学院地球与行星科学系地球化学与岩石学研究所）；Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）
Universität Bern（伯尔尼大学）；Institut für Geologie, Universität Bern（伯尔尼大学地质研究所）；Universität Münster（明斯特大学）；Institut für Planetologie, Universität Münster（明斯特大学行星研究所）；Max Planck Institute for Solar System Research（马克斯·普朗克太阳系统研究所）；Thermo Fisher Scientific（赛默飞世尔科技）
Evolutionary pathways toward survival of a thick CO2- or SO2-rich atmosphere on the lava world TOI-561 b
Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡佩恩天文研究所）；Earth and Planets Laboratory, Carnegie Institution for Science（卡内基科学机构地球与行星实验室）；The Observatories of the Carnegie Institution for Science（卡内基科学机构天文台）；Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）；School of Physics & Astronomy, University of Birmingham（伯明翰大学物理与天文学院）；Waterloo Centre for Astrophysics and Department of Physics and Astronomy, University of Waterloo（滑铁卢大学天体物理学中心及物理与天文学系）
Jupiter-like uniform metal enrichment in a system of multiple giant exoplanets
University of California San Diego（加州大学圣迭戈分校）；California Institute of Technology（加州理工学院）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；IPAC, Caltech（加州理工学院IPAC）；University of Hawaii, Institute for Astronomy（夏威夷大学天文学研究所）；Johns Hopkins University（约翰斯·霍普金斯大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Division of Geological and Planetary Sciences, California Institute of Technology（加州理工学院地质与行星科学系）
Hot and cloudy: High temperature clouds in super-Earths and sub-Neptunes
Leiden Observatory（莱顿天文台）；SRON Netherlands Institute for Space Research（荷兰空间研究所）；Tsinghua University（清华大学）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）
