Hot rocky super-Earths are thought to be sufficiently irradiated by their host star to melt their surface and thus allow for long-lasting magma oceans. Some processes have been proposed for such planets to have retained primordial hydrogen captured during their formation while moving inward in the planetary system. The new generation of space telescopes such as the JWST may provide observations precise enough to characterize the atmospheres and perhaps the interiors of such exoplanets. We use a vaporization model that calculates the gas-liquid equilibrium between the atmosphere (including hydrogen) and the magma ocean, to compute the elemental composition of a variety of atmospheres for different quantities of hydrogen. The elemental composition is then used in a steady-state atmospheric model to compute the atmospheric structure and generate synthetic emission spectra. With this method, we confirm previous results showing that silicate atmospheres exhibit a thermal inversion, with notably an emission peak of SiO at 9~$μm$. We compare our method to the literature on the inclusion of hydrogen in the atmosphere, and show hydrogen reduces the thermal inversion, because of the formation of H2O which has a strong greenhouse potential. However planets that are significantly irradiated by their host star are sufficiently hot to dissociate H2O and thus also maintain a thermal inversion. The observational implications are twofold: 1) H2O is more likely to be detected in colder atmospheres; 2) Detecting a thermal inversion in hotter atmospheres does not a priori exclude the presence of H (in its atomic form). Due to the impact of H on the overall chemistry and atmospheric structure, and therefore observations, we emphasize the importance of including volatiles in the calculation of the gas-liquid equilibrium. Finally, we provide a criterion to determine potential targets for observation.
Sensitivity of Dry Lava Planet Atmospheric Emission Spectra to Changes in Lava Compositions
Leiden Observatory, Leiden University（莱顿天文台，莱顿大学）；Department of Earth Sciences, Vrije Universiteit Amsterdam（地球科学系，阿姆斯特丹自由大学）；Astrophysics Research Institute, Liverpool John Moores University（天体物理研究所，利物浦约翰摩尔斯大学）；SRON Netherlands Institute for Space Research（荷兰空间研究研究所）；Center for Astrophysics, Harvard & Smithsonian（天体物理中心，哈佛大学与史密森尼学会）
Evidence for an Atmosphere on the Ultra-Short Period super-Earth HD 3167 b
University of Chicago（芝加哥大学）；University of Maryland, College Park（马里兰大学帕克分校）；Center for Astrophysics | Harvard & Smithsonian（哈佛与史密森尼天体物理中心）；University of Birmingham（伯明翰大学）
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）
Thermal Evolution of Lava Planets Across System Ages: Predictions for Hell of a Survey
Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；Waterloo Centre for Astrophysics and Department of Physics and Astronomy, University of Waterloo（滑铁卢大学天体物理中心及物理与天文学系）；School of Physics and Astronomy, University of Birmingham（伯明翰大学物理与天文学院）；Center for Star and Planet Formation, Globe Institute, University of Copenhagen（哥本哈根大学全球研究所恒星与行星形成中心）；Space Telescope Science Institute（太空望远镜科学研究所）；Department of Physics, University of Warwick（华威大学物理系）；Department of Physics and Astronomy, York University（约克大学物理与天文学系）；Trottier Space Institute, McGill University（麦吉尔大学特罗蒂尔空间研究所）
A general machine learning model of aluminosilicate melt viscosity and its application to the surface properties of dry lava planets
Université Paris Cité（巴黎城市大学）；Institut de physique du globe de Paris（巴黎地球物理研究所）；CNRS-UMR 7154（法国国家科学研究中心-7154联合研究单位）；Institut Universitaire de France（法国大学研究院）；York University（约克大学）；ETH Zürich（苏黎世联邦理工学院）；Institute of Geochemistry and Petrology（地球化学与岩石学研究所）
An Evolving Cosmic Shoreline and Sandbar Bounding the Rocky Airless Valley
Stanford University（斯坦福大学）；The University of Chicago（芝加哥大学）；University of California, San Diego（加州大学圣地亚哥分校）；University of Hawai‘i（夏威夷大学）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；University of Maryland, College Park（马里兰大学帕克分校）
