Owing to technological advances, the number of exoplanets discovered has risen dramatically in the last few years. However, when trying to observe Earth analogs, it is often difficult to test the veracity of detection. We have developed a new approach to the analysis of exoplanetary spectral observations based on temporal multifractality, which identifies time scales that characterize planetary orbital motion around the host star, and those that arise from stellar features such as spots. Without fitting stellar models to spectral data, we show how the planetary signal can be robustly detected from noisy data using noise amplitude as a source of information. For observation of transiting planets, combining this method with simple geometry allows us to relate the time scales obtained to primary and secondary eclipse of the exoplanets. Making use of data obtained with ground-based and space-based observations we have tested our approach on HD 189733b. Moreover, we have investigated the use of this technique in measuring planetary orbital motion via Doppler shift detection. Finally, we have analyzed synthetic spectra obtained using the SOAP 2.0 tool, which simulates a stellar spectrum and the influence of the presence of a planet or a spot on that spectrum over one orbital period. We have demonstrated that, so long as the signal-to-noise-ratio $\ge$ 75, our approach reconstructs the planetary orbital period, as well as the rotation period of a spot on the stellar surface.
Young M dwarfs flare activity model: Towards better exoplanetary atmospheric characterisation
University of Oslo（奥斯陆大学）；National Solar Observatory, University of Colorado Boulder（美国国家太阳天文台，科罗拉多大学博尔德分校）；Department of Astrophysical and Planetary Sciences, University of Colorado（科罗拉多大学天体物理与行星科学系）；Laboratory for Atmospheric and Space Physics, University of Colorado Boulder（科罗拉多大学博尔德分校大气与空间物理实验室）；Rosseland Centre for Solar Physics, University of Oslo（奥斯陆大学罗斯兰太阳物理中心）；Institute of Theoretical Astrophysics, University of Oslo（奥斯陆大学理论天体物理研究所）
Non-Local Thermodynamic Equilibrium Transmission Spectrum Modelling of HD209458b
系外行星上层大气是低密度环境，辐射过程可以与碰撞过程竞争，并将非局部热力学平衡（NLTE）效应引入透射光谱。目的-我们开发了一个NLTE辐射转移框架，能够在广泛的行星特性范围内模拟系外行星传输光谱。方法-我们适应的NLTE光谱合成代码多云产生的大气结构和原子透射光谱在NLTE和当地的热力学平衡（LTE）的热木星HD209458 b，给出了一个公布的T-P配置文件，并假设太阳金属丰度。选定的光谱特征，包括H $α$，Na I D，He I $λ$ 10830，Fe I和II紫外（UV）带，和C，O和Si UV线，与文献观测和模型进行比较。针对各个谱线测量NLTE效应的强度，以识别哪些特征受到最强烈的影响。结果-开发的建模框架计算NLTE合成光谱再现文献结果的He I $λ$ 10830三重态，Na I D线，和森林的Fe I线的光学。相对于LTE光谱，NLTE光谱中的各个谱线表现出高达40%的更强吸收。
Analysis of Habitability and Stellar Habitable Zones from Observed Exoplanets
Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Lakeside School（湖畔学校）；Pacific Academy（太平洋学院）；Burke Institute for Theoretical Physics, California Institute of Technology（加州理工学院伯克理论物理研究所）
POSTELLAR: Posterior Stellar Spectrum Sampling - An Alternative to Approximate Stellar Spectra for Exoplanetary Analysis
McGill University（麦吉尔大学）；Trottier Space Institute, McGill University（麦吉尔大学特罗蒂尔太空研究所）；Ciela Institute（Ciela研究所）；Department of Earth and Planetary Sciences, McGill University（麦吉尔大学地球与行星科学系）；Université de Montréal（蒙特利尔大学）；Mila—Quebec Artificial Intelligence Institute（Mila-魁北克人工智能研究所）；Institut Trottier de Recherche sur les Exoplanètes, Université de Montréal（蒙特利尔大学特罗蒂尔系外行星研究所）；Observatoire du Mont-Mégantic, Université de Montréal（蒙特利尔大学梅格尼克山天文台）
JWST Exoplanetary Worlds and Elemental Survey (JEWELS) II: Condensation Temperature Trends and Galactic Chemical Evolution in JWST Planet-Hosting Stars
Tsung-Dao Lee Institute, School of Physics and Astronomy, & State Key Laboratory of Dark Matter Physics, Shanghai Jiao Tong University（上海交通大学物理与天文学院、汤川研究所、暗物质物理国家重点实验室）；Department of Physics, King’s College London（伦敦国王学院物理系）；Department of Astronomy, Tsinghua University（清华大学天文系）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）
The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. VII. Molecular Mapping Performance with JWST/MIRI MRS: VHS 1256 b as a case study
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）；Observatoire de Paris（巴黎天文台）；CNRS（法国国家科学研究中心）；Sorbonne Université（索邦大学）；Laboratoire d’Astrophysique de Bordeaux（波尔多天体物理学实验室）
The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems VIII: patchy forsterite and enstatite clouds in the atmosphere of VHS 1256 b, retrieval lessons learned and outlook to the future
American Museum of Natural History（美国自然历史博物馆）；University of Hertfordshire（赫特福德大学）；Trinity College Dublin, The University of Dublin（都柏林三一学院，都柏林大学）；Universidad de Valparaíso（瓦尔帕莱索大学）；Millennium Nucleus on Young Exoplanets and their Moons (YEMS)（系外行星及其卫星年轻世代千年核（YEMS））；Universidad de Santiago de Chile（智利圣地亚哥大学）；ETH Zurich（苏黎世联邦理工学院）
Large Interferometer For Exoplanets (LIFE): XII. The Detectability of Capstone Biosignatures in the Mid-Infrared -- Sniffing Exoplanetary Laughing Gas and Methylated Halogens
本文利用 LIFE 任务概念和 LIFEsim 模拟器，研究在中红外波段探测系外行星大气中 N₂O、CH₃Cl 和 CH₃Br 等关键生物标志物所需的观测时间，并据此定义任务科学要求，证明多数场景下这些标志物可被探测。
Probing Exoplanetary Chemistry with Ariel: Scientific Priorities and Observational Strategies
Univ. Grenoble Alpes CNRS IPAG（格勒诺布尔阿尔卑斯大学法国国家科学研究中心IPAG实验室）；Université Paris Cité and Univ Paris Est Creteil CNRS LISA（巴黎西岱大学和巴黎东 Créteil大学法国国家科学研究中心LISA实验室）；SRON Netherlands Institute for Space Research（荷兰空间研究所）；Leiden Observatory Leiden University（莱顿大学莱顿天文台）；Anton Pannekoek Institute for Astronomy University of Amsterdam（阿姆斯特丹大学安东·潘内克天文学研究所）；IRAP Université de Toulouse CNRS/UMR 5277 UPS-OMP（图卢兹大学法国国家科学研究中心IRAP研究所）；Institute（研究所）
