Planetary Desert around Compact Binaries: Dynamical Instability Triggered by Resonance-Induced Eccentricity Excitation
Institute for Astronomy, School of Physics, Zhejiang University（浙江大学物理学院天体物理研究所）；Center for Cosmology and Computational Astrophysics, Institute for Advanced Study in Physics, Zhejiang University（浙江大学物理高等研究院宇宙学与计算天体物理中心）；Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交通大学李政道研究所）；Department of Astronomy, Center for Astrophysics and Planetary Science, Cornell University（康奈尔大学天文学系天文与行星科学中心）
Compact binaries with orbital periods shorter than about 7 days show an absence of transiting planets, a feature known as the ``circumbinary planet desert". The physical mechanism behind this desert remains unclear. We investigate its origin by simulating the long-term dynamics of multi-planet circumbinary systems with evolving inner binaries. Our simulations are based on the single-averaged secular equations that average only over the binary orbital period and fully incorporate planet-planet interactions. When an eccentric binary decays via tides, an outer planet can be captured into resonance advection in eccentricity, a state in which its apsidal precession locks with that of the binary, driving extreme eccentricity growth. While such growth can occur in a binary-single planet system, the parameter space is limited and may not necessarily induce instability. In a multi-planet system, however, the excited orbit inevitably crosses those of its neighbors, which triggers violent planet-planet scatterings and produces collisions or ejections. Crucially, these mutual gravitational interactions amplify the ``localized" instability of a single planet into a system-wide chain reaction, drastically reshaping the orbital architecture and potentially clearing out the inner regions of planetary systems. Our results suggest that the resonance-induced instability provides a natural explanation for the observed circumbinary planet desert.
The Neptunian ridge as a natural outcome of high-eccentricity tidal migration
Observatoire Astronomique de l’Université de Genève（日内瓦大学天文台）；University of Warwick（华威大学）；Universidade de Coimbra（科英布拉大学）；Sorbonne Université（索邦大学）；CNRS（法国国家科学研究中心）
Revealing the Origin of Desert Dwellers via Stellar Obliquities
MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理与空间研究所，麻省理工学院）；Imperial Astrophysics, Department of Physics, Imperial College London（帝国理工学院物理学系天体物理组，帝国理工学院）；Department of Physics, Massachusetts Institute of Technology（麻省理工学院物理学系）
Very Low Mass Stellar and Substellar Companions to Solar-Like Stars From MARVELS V: A Low Eccentricity Brown Dwarf from the Driest Part of the Desert, MARVELS-6b
A universal brown dwarf desert formed between planets and stars
Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交大李政道研究所）；Department of Physics, University of Warwick（华威大学物理系）；Centre for Exoplanets and Habitability, University of Warwick（华威大学系外行星与宜居性中心）；School of Physics and Astronomy, Shanghai Jiao Tong University（上海交通大学物理与天文学院）；Institute for Astronomy, School of Physics, Zhejiang University（浙江大学物理学院天体物理研究所）；Center for Cosmology and Computational Astrophysics, Institute for Advanced Study in Physics, Zhejiang University（浙江大学物理学高等研究院宇宙学与计算天体物理中心）；School of Physics and Astronomy, University of Leicester（莱斯特大学物理与天文学院）；Department of Physics and Astronomy, The University of Georgia（佐治亚大学物理与天文系）；Center for Simulational Physics, The University of Georgia（佐治亚大学模拟物理中心）
Two extremely irradiated volatile-rich sub-Neptunes with companions in the TOI-426 and TOI-1839 systems: Insights into arrival and survival near the lower edge of the Neptunian desert
Observatoire Astronomique de l’Université de Genève（日内瓦大学天文台）；University of Warwick（华威大学）；University of Oxford（牛津大学）；Centre for Exoplanets and Habitability, University of Warwick（华威系外行星与宜居性中心）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；Universidad Nacional Autónoma de México（墨西哥国立自治大学）；European Space Agency (ESA)（欧洲空间局）；Universidade do Porto（波尔图大学）；Keele University（基尔大学）；NASA Ames Research Center（美国宇航局艾姆斯研究中心）；NASA Exoplanet Science Institute, Caltech/IPAC（NASA系外行星科学研究所/加州理工学院IPAC）；Stephen F. Austin State University（斯蒂芬·F·奥斯汀州立大学）；Princeton University（普林斯顿大学）
The Hot Neptune Initiative (HONEI) III. An ultra-hot super Neptune orbiting the metal-rich subgiant star TOI-5646: the largest host for a desert dweller
University of Rome “Tor Vergata”（罗马第二大学）；INAF – Turin Astrophysical Observatory（意大利国家天体物理研究所都灵天文台）；Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）；University of Bern（伯尔尼大学）；Leiden University（莱顿大学）；INAF – Astronomical Observatory of Rome（意大利国家天体物理研究所罗马天文台）
Confirmation of the hot super-Neptune TOI-672 b with NIRPS and HARPS and Insights into the Neptunian desert around M dwarfs
Univ. Grenoble Alpes（格勒诺布尔阿尔卑斯大学）；CNRS（法国国家科学研究中心）；McMaster University（麦克马斯特大学）；The University of Warwick（华威大学）；Observatoire de Genève, Département d’Astronomie, Université de Genève（日内瓦大学天文学系天文台）；Institut Trottier de recherche sur les exoplanètes（特罗蒂埃系外行星研究所）
The discovery of WASP-151b, WASP-153b, WASP-156b: Insights on giant planet migration and the upper boundary of the Neptunian desert
To investigate the origin of the features discovered in the exoplanet population, the knowledge of exoplanets' mass and radius with a good precision is essential. In this paper, we report the discovery of three transiting exoplanets by the SuperWASP survey and the SOPHIE spectrograph with mass and radius determined with a precision better than 15 %. WASP-151b and WASP-153b are two hot Saturns with masses, radii, densities and equilibrium temperatures of 0.31^{+0.04}_{-0.03} MJ, 1.13^{+0.03}_{-0.03} RJ, 0.22^{-0.03}_{-0.02} rhoJ and 1, 290^{+20}_{-10} K, and 0.39^{+0.02}_{-0.02} MJ, 1.55^{+0.10…
Episodic planetesimal disruptions triggered by dissipation of gas disk
Nanjing University（南京大学）；Key Laboratory of Modern Astronomy and Astrophysics in Ministry of Education, Nanjing University（教育部现代天文与天体物理重点实验室，南京大学）；State Key Laboratory of Critical Earth Material Cycling and Mineral Deposits & Lunar and Planetary Science Institute, School of Earth Sciences and Engineering, Nanjing University（南京大学地球科学与工程学院关键地球物质循环与矿床国家重点实验室及月球与行星科学研究所）；CAS Center for Excellence in Comparative Planetology（中国科学院比较行星学卓越创新中心）
The GAPS Programme at TNG LXXIV. A reanalysis of the planetary systems TOI-1272 and TOI-1694 with HARPS-N and retraction of the planetary interpretation of TOI-1272 c
University of Rome “Tor Vergata”（罗马托尔维加塔大学）；INAF – Turin Astrophysical Observatory（意大利国家天体物理研究所都灵天文台）；INAF – Astronomical Observatory of Rome（意大利国家天体物理研究所罗马天文台）；INAF – Astrophysical Observatory of Catania（意大利国家天体物理研究所卡塔尼亚天文台）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CSIC-INTA））；Fundacion Galileo Galilei（伽利略基金会）；INAF – Astronomical Observatory of Trieste（意大利国家天体物理研究所的里雅斯特天文台）
TOI-1259Ab: A Warm Jupiter Orbiting a K-dwarf White-Dwarf Binary is on a Well-aligned Orbit
University of Amsterdam（阿姆斯特丹大学）；Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Millennium Institute for Astrophysics（天体物理学千年研究所）；Vanderbilt University（范德堡大学）；Tufts University（塔夫茨大学）；The Pennsylvania State University（宾夕法尼亚州立大学）；Princeton University（普林斯顿大学）；University of Pennsylvania（宾夕法尼亚大学）
BEBOP VIII. SOPHIE radial velocities reveal an eccentric, circumbinary brown dwarf
University of Birmingham（伯明翰大学）；Institut d’astrophysique de Paris, UMR 7095 CNRS université Pierre et Marie Curie（巴黎天体物理研究所）；Aix Marseille Univ, CNRS, CNES, LAM（艾克斯-马赛大学）；Queen Mary University of London（伦敦玛丽女王大学）；Universidade de Coimbra（科英布拉大学）；Observatoire de Paris, PSL Université（巴黎天文台）；Tufts University（塔夫茨大学）；Keele University（基尔大学）；University of Cambridge（剑桥大学）；Thüringer Landessternwarte Tautenburg（图林根州陶滕堡州立天文台）；European Space Agency (ESA)（欧洲空间局）；Observatoire Astronomique de l’Université de Genève（日内瓦大学天文台）
