Pub Date : 2026-03-11DOI: 10.1038/s41550-026-02814-9
Zhihong He, Wenkang Pang, Kun Wang, Yangping Luo, Qian Cui
The accretion of metal-poor gas sustains galactic star formation. In the Milky Way, this process is fuelled by high-velocity clouds (HVCs), but their fundamental properties have remained elusive in the absence of stellar tracers. Here we report a binary open cluster within HVC Complex H. With an age of 11.2 ± 0.6 Myr and a subsolar metallicity of (0.0{5}_{-0.02}^{+0.05}) Z⊙, the clusters provide a direct stellar distance anchor to the cloud at 13.8 ± 0.6 kpc. Their proper motions indicate that Complex H is on a prograde, south-to-north orbit through the outer Galactic disk. The resulting interaction produces a ‘slow–fast–slow’ velocity gradient, with the cloud’s outer layers decelerating as they merge into the disk. Orbit integration suggests that the clusters formed from an internal cloud–cloud collision. This triggering mechanism implies that other HVCs could similarly produce high-velocity stars. The scarcity of previous stellar detections in HVCs is explained by the rapid escape of young stars (<20 Myr), whereas CO non-detections may stem from weak emission due to low metallicity and gas dispersal. This work reveals that the circumgalactic medium can sustain star formation, offering a tangible laboratory to probe the physical conditions of accreting gas before it merges with the Galactic disk.
{"title":"Star formation in the circumgalactic high-velocity cloud Complex H","authors":"Zhihong He, Wenkang Pang, Kun Wang, Yangping Luo, Qian Cui","doi":"10.1038/s41550-026-02814-9","DOIUrl":"https://doi.org/10.1038/s41550-026-02814-9","url":null,"abstract":"The accretion of metal-poor gas sustains galactic star formation. In the Milky Way, this process is fuelled by high-velocity clouds (HVCs), but their fundamental properties have remained elusive in the absence of stellar tracers. Here we report a binary open cluster within HVC Complex H. With an age of 11.2 ± 0.6 Myr and a subsolar metallicity of (0.0{5}_{-0.02}^{+0.05}) Z⊙, the clusters provide a direct stellar distance anchor to the cloud at 13.8 ± 0.6 kpc. Their proper motions indicate that Complex H is on a prograde, south-to-north orbit through the outer Galactic disk. The resulting interaction produces a ‘slow–fast–slow’ velocity gradient, with the cloud’s outer layers decelerating as they merge into the disk. Orbit integration suggests that the clusters formed from an internal cloud–cloud collision. This triggering mechanism implies that other HVCs could similarly produce high-velocity stars. The scarcity of previous stellar detections in HVCs is explained by the rapid escape of young stars (<20 Myr), whereas CO non-detections may stem from weak emission due to low metallicity and gas dispersal. This work reveals that the circumgalactic medium can sustain star formation, offering a tangible laboratory to probe the physical conditions of accreting gas before it merges with the Galactic disk.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"55 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2026-03-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147394042","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-03-09DOI: 10.1038/s41550-026-02790-0
Maosheng Yang (杨茂升), Jun Huang (黄俊), Wajiha Iqbal, Lukas Wueller, Carolyn H. van der Bogert, Harald Hiesinger, Sascha Mikolajewski, Minggang Xie (谢明刚), Sen Hu (胡森), Long Xiao (肖龙)
Characterizing landing sites for future lunar crewed missions is key to maximizing the science output. Here we use orbital data to look at the equatorial Rimae Bode region, which is at the mare–highlands boundary and is a high-priority candidate for the upcoming Chinese crewed mission. We identify four distinct geological units: a dark mantle deposit; the Sinus Aestuum mare area; the Rimae Bode unit proper, formed by two distinct areas; and the highlands. The dark mantle deposit is pyroclastic material with relatively low albedo, whose thickness ranges from 77 m to 136 m. Sinus Aestuum is an ancient impact basin filled with low-Ti basaltic lavas with a maximum thickness of 193 m and with a 4-m-thick regolith mostly composed of local materials. Rima Bode I includes volcanic rilles that are potential sources for the basalts in Sinus Aestuum, as they share its spectral characteristics, whereas Rima Bode II exhibits high abundances of Th and Ti. Based on this information, we propose four prospective landing sites in the traversable areas, which provide a range of diverse geological samples, including volcanic debris, mare basalts, Copernicus crater ejecta and high-Th materials. Such a collection may provide insights into the geological evolution of the region and enhance our understanding of the lunar mantle composition and volcanic processes.
{"title":"Geology of Rimae Bode region as priority site candidate for China’s first crewed lunar mission","authors":"Maosheng Yang \u0000 (杨茂升), Jun Huang \u0000 (黄俊), Wajiha Iqbal, Lukas Wueller, Carolyn H. van der Bogert, Harald Hiesinger, Sascha Mikolajewski, Minggang Xie \u0000 (谢明刚), Sen Hu \u0000 (胡森), Long Xiao \u0000 (肖龙)","doi":"10.1038/s41550-026-02790-0","DOIUrl":"https://doi.org/10.1038/s41550-026-02790-0","url":null,"abstract":"Characterizing landing sites for future lunar crewed missions is key to maximizing the science output. Here we use orbital data to look at the equatorial Rimae Bode region, which is at the mare–highlands boundary and is a high-priority candidate for the upcoming Chinese crewed mission. We identify four distinct geological units: a dark mantle deposit; the Sinus Aestuum mare area; the Rimae Bode unit proper, formed by two distinct areas; and the highlands. The dark mantle deposit is pyroclastic material with relatively low albedo, whose thickness ranges from 77 m to 136 m. Sinus Aestuum is an ancient impact basin filled with low-Ti basaltic lavas with a maximum thickness of 193 m and with a 4-m-thick regolith mostly composed of local materials. Rima Bode I includes volcanic rilles that are potential sources for the basalts in Sinus Aestuum, as they share its spectral characteristics, whereas Rima Bode II exhibits high abundances of Th and Ti. Based on this information, we propose four prospective landing sites in the traversable areas, which provide a range of diverse geological samples, including volcanic debris, mare basalts, Copernicus crater ejecta and high-Th materials. Such a collection may provide insights into the geological evolution of the region and enhance our understanding of the lunar mantle composition and volcanic processes.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"1 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2026-03-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147381711","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-03-06DOI: 10.1038/s41550-026-02798-6
Yi-Kuan Chiang
Molecular gas, modest in mass yet pivotal within the cosmic inventory, regulates baryon cycling as the immediate fuel for star formation. Across most of cosmic history, its reservoir has remained elusive, with only the tip of the iceberg revealed by luminous CO-emitting galaxies. Here we report the detection of the mean cosmic CO background across its rotational ladder at 7σ, together with ionized carbon ([C II]) at 3σ, over 0 < z < 4.2. This uses tomographic clustering of diffuse broadband intensities with reference galaxies, directly probing aggregate emission in the cosmic web. From CO(1–0) we infer the total molecular gas density, ({varOmega }_{{{rm{H}}}_{2}}), finding it about twice that resolved in galaxy surveys. The global depletion time is ~1 Gyr, shorter than the Hubble time, requiring sustained inflow. CO excitation is linked to star-formation surface density and, with depletion time, yields a super-linear Kennicutt–Schmidt law that appears universal. Together these results establish a global picture of galaxy growth fuelled by a larger, short-lived molecular reservoir. The CO and [C II] detections mark a turning point for line-intensity mapping, replacing forecasts with empirical line strengths and defining sensitivity requirements for upcoming three-dimensional experiments poised to open new windows on galaxy formation and cosmology.
分子气体虽然质量不大，但在宇宙中起着关键作用，它调节重子循环，作为恒星形成的直接燃料。在宇宙历史的大部分时间里，它的储藏库仍然是难以捉摸的，只有发光的co发射星系揭示了冰山一角。在这里，我们报告了在其旋转阶梯上探测到的平均宇宙CO背景在7σ，以及电离碳（[C II]）在3σ，大于0 < z < 4.2。它使用参考星系的漫射宽带强度的层析成像聚类，直接探测宇宙网中的聚集发射。从CO（1-0）我们推断出总分子气体密度，({varOmega }_{{{rm{H}}}_{2}})，发现它大约是星系调查中分辨率的两倍。全球耗竭时间为1gyr，比哈勃时间短，需要持续的流入。CO激发与恒星形成的表面密度有关，随着耗尽时间的推移，产生了一个似乎普遍存在的超线性kennicut - schmidt定律。总之，这些结果建立了一个更大的、寿命较短的分子储存库推动的星系增长的全球图景。CO和[C II]探测标志着线强度测绘的转折点，用经验线强度取代预测，并为即将到来的三维实验确定灵敏度要求，准备打开星系形成和宇宙学的新窗口。
{"title":"Cosmic CO and [C II] backgrounds and the fuelling of star formation over 12 Gyr","authors":"Yi-Kuan Chiang","doi":"10.1038/s41550-026-02798-6","DOIUrl":"https://doi.org/10.1038/s41550-026-02798-6","url":null,"abstract":"Molecular gas, modest in mass yet pivotal within the cosmic inventory, regulates baryon cycling as the immediate fuel for star formation. Across most of cosmic history, its reservoir has remained elusive, with only the tip of the iceberg revealed by luminous CO-emitting galaxies. Here we report the detection of the mean cosmic CO background across its rotational ladder at 7σ, together with ionized carbon ([C II]) at 3σ, over 0 < z < 4.2. This uses tomographic clustering of diffuse broadband intensities with reference galaxies, directly probing aggregate emission in the cosmic web. From CO(1–0) we infer the total molecular gas density, ({varOmega }_{{{rm{H}}}_{2}}), finding it about twice that resolved in galaxy surveys. The global depletion time is ~1 Gyr, shorter than the Hubble time, requiring sustained inflow. CO excitation is linked to star-formation surface density and, with depletion time, yields a super-linear Kennicutt–Schmidt law that appears universal. Together these results establish a global picture of galaxy growth fuelled by a larger, short-lived molecular reservoir. The CO and [C II] detections mark a turning point for line-intensity mapping, replacing forecasts with empirical line strengths and defining sensitivity requirements for upcoming three-dimensional experiments poised to open new windows on galaxy formation and cosmology.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"53 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2026-03-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147371128","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-03-03DOI: 10.1038/s41550-026-02803-y
Gibor Basri
One of the most active areas in current astrophysics is the search for clues to answering the ancient question: are we alone? This Perspective focuses on where most of the life in our Galaxy might reside over the very long haul, taking a freer viewpoint than is typical for astrobiology. The astrophysical discussion includes stellar numbers and longevity, planetary numbers and conditions, and the effects of stellar magnetic activity. I support the position that exoplanets in habitable zones around stars of between 0.5 and 0.8 solar masses might be the dominant habitats for surface life. However, the primary habitat in the Galaxy could easily be salty oceans under thick ice shells instead. These are probably much more numerous than planets with Earth-like conditions and have little dependence on stellar properties. In both cases, exoplanets of a few Earth masses are favoured for several reasons. These conclusions are based on terrestrial life, but there is no reason to think that nature is confined to that paradigm, so I discuss some other speculative possibilities. Finally, I suggest that the classical Drake equation should be made dynamic to reflect galactic evolution, and discuss the importance of survival times for life and civilizations.
{"title":"A broad perspective on Galactic life","authors":"Gibor Basri","doi":"10.1038/s41550-026-02803-y","DOIUrl":"https://doi.org/10.1038/s41550-026-02803-y","url":null,"abstract":"One of the most active areas in current astrophysics is the search for clues to answering the ancient question: are we alone? This Perspective focuses on where most of the life in our Galaxy might reside over the very long haul, taking a freer viewpoint than is typical for astrobiology. The astrophysical discussion includes stellar numbers and longevity, planetary numbers and conditions, and the effects of stellar magnetic activity. I support the position that exoplanets in habitable zones around stars of between 0.5 and 0.8 solar masses might be the dominant habitats for surface life. However, the primary habitat in the Galaxy could easily be salty oceans under thick ice shells instead. These are probably much more numerous than planets with Earth-like conditions and have little dependence on stellar properties. In both cases, exoplanets of a few Earth masses are favoured for several reasons. These conclusions are based on terrestrial life, but there is no reason to think that nature is confined to that paradigm, so I discuss some other speculative possibilities. Finally, I suggest that the classical Drake equation should be made dynamic to reflect galactic evolution, and discuss the importance of survival times for life and civilizations.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"58 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2026-03-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147507825","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-03-03DOI: 10.1038/s41550-026-02812-x
Caroline Morley
Spectra of temperate sub-Neptunes reveal strikingly different atmospheric chemistries, hinting at diverse origins and interiors.
温带亚海王星的光谱揭示了截然不同的大气化学成分，暗示了不同的起源和内部结构。
{"title":"Worlds between Earth and Neptune defy a simple story","authors":"Caroline Morley","doi":"10.1038/s41550-026-02812-x","DOIUrl":"https://doi.org/10.1038/s41550-026-02812-x","url":null,"abstract":"Spectra of temperate sub-Neptunes reveal strikingly different atmospheric chemistries, hinting at diverse origins and interiors.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"1 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2026-03-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147507941","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-03-03DOI: 10.1038/s41550-026-02807-8
Nitin Shukla, Geray S. Karademir, Luciano Rezzolla, Fabio Bacchini, Stefano Truzzi, Andrea Mignone, Alessandro Romeo, Klaus Dolag, Luca Tornatore, Lubomir Riha, Giuliano Taffoni
From early particle calculations to today’s models, numerical simulations have reshaped the way physicists investigate the Universe. This overview examines how the next generation of high-performance computing systems — characterized by unprecedented scale and substantial technical complexity —will create opportunities for astronomical discovery, from plasma physics to cosmological structure formation.
{"title":"Exascale computing to accelerate discoveries in astrophysics and space plasma physics","authors":"Nitin Shukla, Geray S. Karademir, Luciano Rezzolla, Fabio Bacchini, Stefano Truzzi, Andrea Mignone, Alessandro Romeo, Klaus Dolag, Luca Tornatore, Lubomir Riha, Giuliano Taffoni","doi":"10.1038/s41550-026-02807-8","DOIUrl":"https://doi.org/10.1038/s41550-026-02807-8","url":null,"abstract":"From early particle calculations to today’s models, numerical simulations have reshaped the way physicists investigate the Universe. This overview examines how the next generation of high-performance computing systems — characterized by unprecedented scale and substantial technical complexity —will create opportunities for astronomical discovery, from plasma physics to cosmological structure formation.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"12 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2026-03-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147507887","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-02-27DOI: 10.1038/s41550-026-02795-9
Mu-Tian Wang, Fei Dai, Hui-Gen Liu, Howard Chen, Zhecheng Hu, Erik Petigura, Steven Giacalone, Eve Lee, Max Goldberg, Adrien Leleu, Andrew W. Mann, Madyson G. Barber, Joshua N. Winn, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Howard M. Relles, Francis P. Wilkin, Enric Palle, Felipe Murgas, Avi Shporer, Ramotholo Sefako, Keith Horne, Hugh P. Osborn, Yann Alibert, Luca Fossati, Andrea Fortier, Sérgio Sousa, Alexis Brandeker, Pierre Maxted, Alexia Goldenberg
Young exoplanets provide vital insights into the early dynamical and atmospheric evolution of planetary systems. Many multi-planet systems younger than 100 Myr exhibit mean-motion resonances, probably established through convergent disk migration. Over time, however, these resonant chains are often disrupted, mirroring the Nice model proposed for the Solar System. Here we present a detailed characterization of the ~200-Myr-old TOI-2076 system, which contains four sub-Neptune planets between 1.4 and 3.5 Earth radii. We demonstrate that its planets are near to but not locked in mean-motion resonances, making the system dynamically fragile. The four planets have comparable core masses but display a monotonic increase in hydrogen and helium (H/He) envelope mass fractions (from stripped to 1%, 5% and 5%) with decreasing stellar insolation. This trend is consistent with atmospheric mass loss due to photoevaporation, which predicts that the envelopes of irradiated planets either erode completely or stabilize at a residual level of ~1% by mass within the first few hundred million years, with more distant, less-irradiated planets retaining most of their primordial envelopes. Additionally, previous detections of metastable helium outflows rule out a pure water-world scenario for the TOI-2076 planets. Our finding provides direct observational evidence that the dynamical and atmospheric reshaping of compact planetary systems begins early and offers an empirical anchor for models of their long-term evolution.
{"title":"An adolescent and near-resonant planetary system near the end of photoevaporation","authors":"Mu-Tian Wang, Fei Dai, Hui-Gen Liu, Howard Chen, Zhecheng Hu, Erik Petigura, Steven Giacalone, Eve Lee, Max Goldberg, Adrien Leleu, Andrew W. Mann, Madyson G. Barber, Joshua N. Winn, Karen A. Collins, Cristilyn N. Watkins, Richard P. Schwarz, Howard M. Relles, Francis P. Wilkin, Enric Palle, Felipe Murgas, Avi Shporer, Ramotholo Sefako, Keith Horne, Hugh P. Osborn, Yann Alibert, Luca Fossati, Andrea Fortier, Sérgio Sousa, Alexis Brandeker, Pierre Maxted, Alexia Goldenberg","doi":"10.1038/s41550-026-02795-9","DOIUrl":"https://doi.org/10.1038/s41550-026-02795-9","url":null,"abstract":"Young exoplanets provide vital insights into the early dynamical and atmospheric evolution of planetary systems. Many multi-planet systems younger than 100 Myr exhibit mean-motion resonances, probably established through convergent disk migration. Over time, however, these resonant chains are often disrupted, mirroring the Nice model proposed for the Solar System. Here we present a detailed characterization of the ~200-Myr-old TOI-2076 system, which contains four sub-Neptune planets between 1.4 and 3.5 Earth radii. We demonstrate that its planets are near to but not locked in mean-motion resonances, making the system dynamically fragile. The four planets have comparable core masses but display a monotonic increase in hydrogen and helium (H/He) envelope mass fractions (from stripped to 1%, 5% and 5%) with decreasing stellar insolation. This trend is consistent with atmospheric mass loss due to photoevaporation, which predicts that the envelopes of irradiated planets either erode completely or stabilize at a residual level of ~1% by mass within the first few hundred million years, with more distant, less-irradiated planets retaining most of their primordial envelopes. Additionally, previous detections of metastable helium outflows rule out a pure water-world scenario for the TOI-2076 planets. Our finding provides direct observational evidence that the dynamical and atmospheric reshaping of compact planetary systems begins early and offers an empirical anchor for models of their long-term evolution.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"228 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2026-02-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147320172","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-02-25DOI: 10.1038/s41550-026-02792-y
Hassen M. Yesuf, Connor Bottrell
{"title":"Galaxy and black hole co-evolution in dark matter haloes not captured by cosmological simulations","authors":"Hassen M. Yesuf, Connor Bottrell","doi":"10.1038/s41550-026-02792-y","DOIUrl":"https://doi.org/10.1038/s41550-026-02792-y","url":null,"abstract":"","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"52 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2026-02-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147279118","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-02-24DOI: 10.1038/s41550-026-02794-w
Shravan Hanasoge, Christopher Hanson
{"title":"Evidence for global-scale magnetically modified Rossby waves in the Sun","authors":"Shravan Hanasoge, Christopher Hanson","doi":"10.1038/s41550-026-02794-w","DOIUrl":"https://doi.org/10.1038/s41550-026-02794-w","url":null,"abstract":"","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"340 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2026-02-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147279119","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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