Phase-dependent chemistry of WASP-43 b revealed with a suite of one-, two-, and three-dimensional models
Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安顿·潘内科克天文学研究所）；Space Science Institute（空间科学研究所）；Department of Physics, New York University Abu Dhabi（阿布扎比纽约大学物理系）；Center for Astrophysics and Space Science (CASS), New York University Abu Dhabi（阿布扎比纽约大学天体物理学与空间科学中心）；Center for Space and Habitability, University of Bern（伯尔尼大学太空与宜居性中心）；LIRA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris Cité（巴黎天文台LIRA实验室，PSL大学，法国国家科学研究中心，索邦大学，巴黎西岱大学）；Laboratoire de Météorologie Dynamique, IPSL, CNRS, Sorbonne Université, Ecole Normale Supérieure, Université PSL, Ecole Polytechnique, Institut Polytechnique de Paris（动态气象实验室，IPSL，法国国家科学研究中心，索邦大学，巴黎高等师范学院，PSL大学，巴黎综合理工学院，巴黎理工学院）；Institute of Astronomy & Astrophysics, Academia Sinica（中央研究院天文学及天体物理学研究所）；Department of Astronomy and Astrophysics, The University of Chicago（芝加哥大学天文学与天体物理学系）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Atmospheric, Oceanic and Planetary Physics, Department of Physics, University of Oxford（牛津大学物理系大气、海洋和行星物理组）
Robin Baeyens, Julianne I. Moses, Jasmina Blecic, Elspeth K. H. Lee, Lucas Teinturier, Shang-Min Tsai, Jeehyun Yang, Jingxuan Yang, Ludmila Carone, Renyu Hu, Sv… 展开作者
Robin Baeyens, Julianne I. Moses, Jasmina Blecic, Elspeth K. H. Lee, Lucas Teinturier, Shang-Min Tsai, Jeehyun Yang, Jingxuan Yang, Ludmila Carone, Renyu Hu, Sven Kiefer, Anjali A. A. Piette, Taylor J. Bell, Nicolas Crouzet, Ian Dobbs-Dixon, Christiane Helling, Nicolas Iro, Dominic Samra, Olivia Venot, Jean-Michel Désert
备注：
25 pages, 18 figures, accepted for publication in A&A
Our goal is to investigate the chemistry of the hot Jupiter WASP-43 b in detail using theoretical models, considering the constraints of the James Webb Space Telescope MIRI phase curve. With a suite of pseudo-two-dimensional and three-dimensional photochemical models, we simulate the composition of WASP-43 b in various configurations, and compare them with atmospheric retrieval models. We confirm that disequilibrium chemistry in our theoretical models reduces the methane concentration on the planet night side for wind jet speeds > 500 m/s. Varying the metallicity in the models induces large changes in the CO$_2$ and SO$_2$ concentrations, with SO$_2$ producing mid-infrared absorption features in synthetic emission spectra of the night side at atmospheric metallicities > 10x solar. Our models provide evidence for pole-to-equator circulation enhancing the CH$_4$, NH$_3$, and HCN abundances, which is nonetheless insufficient for detectable spectral features. Finally, we show that H$_2$O, CO, and CO$_2$ are robustly modeled, but species affected by photochemistry are more sensitive to model-specific assumptions and pathways. We conclude that horizontal quenching is the prime mechanism that explains the non-detection of methane in the MIRI phase-curve of WASP-43 b. This mechanism requires only moderate wind speeds and is operative at various thermal structures and atmospheric metallicities. Furthermore, coupled carbon-sulfur chemistry leads to an additional decrease in methane compared to previous models in the literature that did not contain sulfur chemistry. We do not favor a high metallicity as it would have led to observable SO$_2$ features in the MIRI spectra. Our study shows that phase-dependent photochemistry models are essential tools in the interpretation of hot-Jupiter phase curves, but benchmarking is needed to improve the accuracy of photochemical models in the future.
Implementation of disequilibrium chemistry to spectral retrieval code ARCiS and application to sixteen exoplanet transmission spectra: Indication of disequilibrium chemistry for HD 209458b and WASP-39b
JWST-TST DREAMS: The Nightside Emission and Chemistry of WASP-17b
JHU Applied Physics Laboratory（约翰·霍普金斯大学应用物理实验室）；University of California, Riverside（加州大学河滨分校）；Academia Sinica（中央研究院）；Cornell University（康奈尔大学）；National Institute of Science Education and Research (NISER)（国家科学教育与研究研究所）；Catholic University of America（美利坚天主教大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Center for Research and Exploration in Space Science and Technology II, NASA/GSFC（NASA/GSFC空间科学与技术探索研究中心II）；University of Bristol（布里斯托大学）；Johns Hopkins University（约翰·霍普金斯大学）；American University（美利坚大学）；NASA GSFC Sellers Exoplanet Environments Collaboration（NASA戈达德太空飞行中心塞勒斯系外行星环境合作组织）；Massachusetts Institute of Technology（麻省理工学院）；Space Telescope Science Institute（太空望远镜科学研究所）；Washington University, St. Louis（华盛顿大学（圣路易斯））；University of Maryland, Baltimore County（马里兰大学巴尔的摩县分校）；Association of Universities for Research in Astronomy（天文学研究大学协会）
A Next-Generation Exoplanet Atmospheric Retrieval Framework NEXOTRANS for Emission Spectroscopy: New Constraints and Atmospheric Characterization of WASP-69b Using JWST NIRCam and MIRI Observations
National Institute of Science Education and Research（印度科学教育研究国家研究所）；Homi Bhabha National Institute（霍米·巴巴国立学院）
Exploring the ultra-hot Jupiter WASP-178b. Constraints on atmospheric chemistry and dynamics from a joint retrieval of VLT/CRIRES$^+$ and space photometric data
Chemical Tracers for 3D Atmospheric Asymmetries on WASP-69 b
Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）；Institute for Theoretical and Computational Physics, Graz University of Technology（格拉茨工业大学理论与计算物理研究所）；Space Research and Planetary Sciences, Physics Institute, University of Bern（伯尔尼大学物理学院空间研究与行星科学系）；Cavendish Laboratory, University of Cambridge（剑桥大学卡文迪许实验室）
A Next-Generation Exoplanet Atmospheric Retrieval Framework for Transmission Spectroscopy (NEXOTRANS): Comparative Characterization for WASP-39 b Using JWST NIRISS, NIRSpec PRISM, and MIRI Observations
Modelling the effect of 3D temperature and chemistry on the cross-correlation signal of transiting ultra-hot Jupiters: A study of 5 chemical species on WASP-76b
Limb Asymmetries on WASP-39b: A Multi-GCM Comparison of Chemistry, Clouds, and Hazes
University of Chicago（芝加哥大学）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；University of Maryland（马里兰大学）；Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）；University of California, Riverside（加州大学河滨分校）；Academia Sinica（中央研究院）；University of Bern（伯尔尼大学）；Universitäts-Sternwarte München, Fakultät für Physik der Ludwig-Maximilians-Universität（慕尼黑大学天文台，物理学院）；University of Michigan（密歇根大学）；KU Leuven（荷语鲁汶大学）
The GAPS Programme at TNG XXXIX -- Multiple molecular species in the atmosphere of the warm giant planet WASP-80 b unveiled at high resolution with GIANO-B
From pre-transit to post-eclipse: investigating the impact of 3D temperature, chemistry, and dynamics on high-resolution emission spectra of the ultra-hot Jupiter WASP-76b
Institut Trottier de Recherche sur les Exoplanètes, Université de Montréal（特罗提尔系外行星研究所，蒙特利尔大学）；Université 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）；Center for Space and Habitability, University of Bern（太空与宜居性中心，伯尔尼大学）
Inclusion of sulfur chemistry in a validated C/H/O/N chemical network: identification of key C/S coupling pathways
Université Paris Cité and Univ Paris Est Creteil, CNRS, LISA（巴黎西岱大学与巴黎东克雷泰伊大学，法国国家科学研究中心，LISA）；Astrophysics Group, University of Exeter（埃克塞特大学天体物理学组）；Université de Lorraine, CNRS, LRGP（洛林大学，法国国家科学研究中心，LRGP）；Department of Physics and Astronomy, University College London（伦敦大学学院物理与天文系）
Detection of CO, H$_2$O, and OH in WASP-18b with JWST/NIRISS using Direct-Extracted Spectra and Cross-Correlation
University of Science and Technology of China（中国科学技术大学）；Chinese Academy of Sciences（中国科学院）；Purple Mountain Observatory（紫金山天文台）；Instituto de Astrofísica de Canarias（加那利天体物理研究所）；Universidad de La Laguna（拉各拉纳大学）
A Physically Driven Parameterisation of Multidimensional Atmospheres: Application to the JWST Phase Curve of WASP-121b
CAS Key Laboratory of Planetary Sciences, Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院行星科学重点实验室，紫金山天文台）；University of Science and Technology of China（中国科学技术大学）；Tsung-Dao Lee Institute & School of Physics and Astronomy, Shanghai Jiao Tong University（上海交大李政道研究所与物理与天文学院）；University of Oxford（牛津大学）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；University of Newcastle（纽卡斯尔大学）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）；Universidad de La Laguna（拉各纳大学）；University of Hawai‘i（夏威夷大学）
