Context. Semi-grey atmospheric models (with one opacity for the visible and one opacity for the infrared) are useful to understand the global structure of irradiated atmospheres, their dynamics and the interior structure and evolution of planets, brown dwarfs and stars. But when compared to direct numerical radiative transfer calculations for irradiated exoplanets, these models systematically overestimate the temperatures at low optical depth, independently of the opacity parameters. We wish to understand why semi-grey models fail at low optical depths, and provide a more accurate approximation to the atmospheric structure by accounting for the variable opacity in the infrared. Our analytical irradiated non-grey model is found to provide a range of temperatures that is consistent with that obtained by numerical calculations. We find that even for slightly non-grey thermal opacities the temperature structure differs significantly from previous semi-grey models. For small values of beta (expected when lines are dominant), we find that the non-grey effects are confined to low-optical depths. However, for beta larger than 0.5 (appropriate in the presence of bands with a wavelength-dependence smaller or comparable with the width of the Planck function), we find that the temperature structure is affected even down to infrared optical depths unity and deeper as a result of the so-called blanketing effect. The expressions that we derive may be used to provide a proper functional form for algorithms that invert the atmospheric properties from spectral information. Because a full atmospheric structure can be calculated directly, these expressions should be useful for simulations of the dynamics of these atmospheres and of the thermal evolution of the planets. Finally, they should be used to test full radiative transfer models and improve their convergence.
Irradiated Atmospheres VII. Effect of Mixing Energy Flux on Atmosphere-Interior Coupling
Institute of Science and Technology for Deep Space Exploration, Nanjing University（南京大学深空探测科学与技术研究院）；School of Physics and Astronomy, Sun Yat-Sen University（中山大学物理学院）；CSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area（粤港澳大湾区空间望远镜科学中心）；State Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology（澳门科技大学月与行星科学国家重点实验室）；Atmospheric, Oceanic, and Planetary Physics Department, University of Oxford（牛津大学大气、海洋与行星物理系）；Department of Physics and Astronomy, University of Exeter（埃克塞特大学物理与天文系）；Tsung-Dao Lee Institute & School of Physics and Astronomy, Shanghai Jiao Tong University（上海交通大学李政道研究所及物理与天文学院）
Irradiated Atmospheres IV: Effect of Mixing Heat Flux on Chemistry
School of Physics and Astronomy, Sun Yat-Sen University（中山大学物理学院）；CSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area（粤港澳大湾区空间望远镜科学中心）；State Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology（澳门科技大学月面与行星科学国家重点实验室）；Institute of Science and Technology for Deep Space Exploration, Nanjing University（南京大学深空探测科学与技术研究院）；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）；Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；University of CAS（中国科学院大学）；Key Laboratory for the Structure and Evolution of Celestial Objects, CAS（中国科学院天体结构与演化重点实验室）；Electric Information School, Wuhan University（武汉大学电气信息学院）；International Centre of Supernovae, Yunnan Key Laboratory（云南省超新星国际研究中心）
Exploring deep and hot adiabats as a potential solution to the radius inflation problem in brown dwarfs: Long-timescale models of the deep atmospheres of KELT-1b, Kepler-13Ab, and SDSS1411B
Dynamically Coupled Three-dimensional Cloud-Chemistry in Rapidly Rotating Irradiated Atmospheres: an Application to the Compact White Dwarf-Brown Dwarf system ZTFJ0038+2030
Tsung-Dao Lee Institute, Shanghai Jiao Tong University（李政道研究所，上海交通大学）；School of Physics and Astronomy, Shanghai Jiao Tong University（物理与天文学院，上海交通大学）；State Key Laboratory of Dark Matter Physics, Shanghai Jiao Tong University（暗物质物理全国重点实验室，上海交通大学）；Department of Astronomy, University of Virginia（天文学系，弗吉尼亚大学）；School of Physics and Astronomy, University of Leicester（物理与天文学院，莱斯特大学）；School of Physics and Astronomy, University of Birmingham（物理与天文学院，伯明翰大学）；Center for Space and Habitability, University of Bern（太空与宜居性中心，伯尔尼大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Université de la Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange（蔚蓝海岸大学，蔚蓝海岸天文台，法国国家科学研究中心，拉格朗日实验室）
Irradiated Atmosphere V: Effects of Vertical-Mixing induced Energy Transport on the Inhomogeneity
Institute of Science and Technology for Deep Space Exploration, Nanjing University（南京大学深空探测科学与技术研究院）；School of Physics and Astronomy, Sun Yat-Sen University（中山大学物理学院）；CSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area（粤港澳大湾区空间望远镜科学中心）；State Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology（澳门科技大学月球与行星科学国家重点实验室）；International Centre of Supernovae, Yunnan Key Laboratory（云南省超新星国际研究中心）
Atmospheric mass loss from hot Jupiters irradiated by stellar superflares
由于它们的活动，晚型恒星被认为拥有强大的耀斑，在短时间内产生强烈的高能辐射，可能会对附近行星的大气层产生重大影响。我们采用一维空气动力学模型来研究热木星HD 209458 b的上层大气对恒星耀斑引起的额外高能辐射的反应。大气吸收耀斑期间产生的额外能量导致局部大气加热，并伴随着两个传播冲击波的形成。我们提出的额外的大气损失发生在响应耀斑的估计。我们发现，与不活跃恒星的质量损失率（2*10^10 g s-1）相比，外底水平的质量损失率显著增加（分别为安静恒星高能通量的10倍、100倍和1000倍时的3.8*10^10 g s-1、8*10^10 g s-1和3.5*10^11 g s-1）。
Quantifying the differences in transmission and emission spectra for hot irradiated gaseous exoplanet atmospheres: A comparison of 1D and 3D modeling using JWST
National Institute of Science Education and Research（印度科学教育研究所）；Homi Bhabha National Institute（霍米·巴巴国立研究所）
Helium escaping from the atmosphere of a nearby rocky exoplanet orbiting in a habitable zone
Harvard University（哈佛大学）；Carnegie Science Observatories（卡内基科学天文台）；Center for Astrophysics, Harvard & Smithsonian（哈佛-史密森天体物理中心）；School of Engineering and Applied Sciences, Harvard University（哈佛工程学院与应用科学学院）；Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理学与空间研究所）；Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology（麻省理工学院地球、大气和行星科学系）；Earth and Planets Laboratory, Carnegie Institution for Science（卡内基科学机构地球与行星实验室）；Space Telescope Science Institute（太空望远镜科学研究所）；Department of Physics & Astronomy, Johns Hopkins University（约翰斯·霍普金斯大学物理与天文系）；Department of Physics, Washington University（华盛顿大学物理系）
Phase-resolved Hubble Space Telescope WFC3 Spectroscopy of Weakly-Irradiated Brown Dwarf GD 1400 and Energy Redistribution-Irradiation Trends in Six WD$-$BD Binaries
Is pi Men c's atmosphere hydrogen-dominated? Insights from a non-detecton of Hy Ly-alpha absorption
限制超级地球到次海王星大小的行星的组成是理解行星形成和演化过程的优先事项。pi Men c代表了此类行星大气和成分特征的独特目标，因为它受到强烈照射，并且其体积密度与丰富的H2O一致。我们用哈勃太空望远镜的STIS仪器通过H i Ly-alpha透射光谱在pi Men c的高层大气中寻找来自光解H2/H2O的氢，但没有探测到它。我们设定1（3）个上限，有效行星与恒星的大小比RLy-alpha/Rearth=0.13（0.24）和0.12（0.20）。我们重建了恒星光谱，并估计Men c接收到约1350 erg cm-2 s-1的5-912-Angstroms能量，足以引起快速的大气逃逸。一个有趣的解释是，Men c的大气层主要是H2O或其他重分子，而不是H2/He。根据我们的模型，丰富的氧气导致更少的大气层，从中性过渡到离行星更近的电离氢。我们将我们的未探测与其他探测尝试进行了比较，并初步确定了两种行为：密度<2 g cm-3的行星（可能是氢主导的大气）导致H i Ly-alpha吸收，而密度>3 g cm-3的行星（可能是非氢主导的大气）不会导致可测量的吸收。研究一个强辐射的亚海王星样本可能会提供一些统计学上的确认，如果它表明它们通常不会形成扩展的大气层。
