Pub Date : 2026-01-22DOI: 10.1038/s41550-026-02772-2
Paul Woods
{"title":"Carbon-rich atmospheres hard to explain","authors":"Paul Woods","doi":"10.1038/s41550-026-02772-2","DOIUrl":"10.1038/s41550-026-02772-2","url":null,"abstract":"","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"10 1","pages":"10-10"},"PeriodicalIF":14.3,"publicationDate":"2026-01-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146016523","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 : 2026-01-22DOI: 10.1038/s41550-026-02773-1
Lindsay Oldham
{"title":"Finding a galaxy in a haystack","authors":"Lindsay Oldham","doi":"10.1038/s41550-026-02773-1","DOIUrl":"10.1038/s41550-026-02773-1","url":null,"abstract":"","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"10 1","pages":"11-11"},"PeriodicalIF":14.3,"publicationDate":"2026-01-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146016495","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 : 2026-01-21DOI: 10.1038/s41550-025-02767-5
Daxal H. Mehta, John A. Regan, Lewis Prole
Observations by the James Webb Space Telescope have uncovered supermassive black holes with masses exceeding 106 M⊙ at redshifts z > 8, posing serious challenges to existing models of early black hole formation and growth. Here we show, in a fully cosmological setting, that light seed black holes, remnants of population III stars, can grow rapidly to ~104 M⊙ in the early Universe. This growth is enabled by our new black hole seeding prescription and the unprecedented resolution of our zoom-in cosmological simulations, which resolve the dense environments necessary for efficient accretion. Our results provide robust evidence that light seed black holes can attain the masses required to serve as the dominant progenitors of the population of supermassive black holes observed at later cosmic epochs. These findings have far-reaching implications for the interpretation of observations by the James Webb Space Telescope and future gravitational wave detections with LISA.
{"title":"The growth of light seed black holes in the early Universe","authors":"Daxal H. Mehta, John A. Regan, Lewis Prole","doi":"10.1038/s41550-025-02767-5","DOIUrl":"https://doi.org/10.1038/s41550-025-02767-5","url":null,"abstract":"Observations by the James Webb Space Telescope have uncovered supermassive black holes with masses exceeding 106 M⊙ at redshifts z > 8, posing serious challenges to existing models of early black hole formation and growth. Here we show, in a fully cosmological setting, that light seed black holes, remnants of population III stars, can grow rapidly to ~104 M⊙ in the early Universe. This growth is enabled by our new black hole seeding prescription and the unprecedented resolution of our zoom-in cosmological simulations, which resolve the dense environments necessary for efficient accretion. Our results provide robust evidence that light seed black holes can attain the masses required to serve as the dominant progenitors of the population of supermassive black holes observed at later cosmic epochs. These findings have far-reaching implications for the interpretation of observations by the James Webb Space Telescope and future gravitational wave detections with LISA.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"45 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2026-01-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146006204","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 : 2026-01-20DOI: 10.1038/s41550-025-02765-7
Alfred Thomas Hopkinson, Ann Mary Wilson, Joe Pitfield, Alejandra Traspas Muiña, Richárd Rácz, Duncan V. Mifsud, Péter Herczku, Gergö Lakatos, Béla Sulik, Zoltán Juhász, Sándor Biri, Robert W. McCullough, Nigel J. Mason, Carsten Scavenius, Liv Hornekær, Sergio Ioppolo
The origin of the molecular building blocks of life is a central question in science. A few α-amino acids, such as glycine, the simplest proteinogenic amino acid, have been detected in meteorites and comets, indicating an extraterrestrial origin for some prebiotic molecules. However, the formation of peptides, short chains of α-amino acids linked by peptide bonds, has remained unresolved under astrophysical conditions. Here we show that the building blocks of proteins can form in interstellar ice analogues exposed to ionizing radiation without the presence of liquid water. Using isotopically labelled glycine irradiated with protons at cryogenic temperatures, we detect the formation of glycylglycine, the simplest dipeptide, along with deuterated and undeuterated water as by-products. The formation of peptide bonds is confirmed by infrared spectroscopy and high-resolution mass spectrometry, which also reveal the production of other complex organic species. These findings demonstrate a non-aqueous route to peptide formation under space-like conditions and suggest that such molecules could form in the cold interstellar medium and be incorporated into forming planetary systems. Our results challenge aqueous-centric models of early biochemical evolution and broaden potential settings for the origins of life.
{"title":"An interstellar energetic and non-aqueous pathway to peptide formation","authors":"Alfred Thomas Hopkinson, Ann Mary Wilson, Joe Pitfield, Alejandra Traspas Muiña, Richárd Rácz, Duncan V. Mifsud, Péter Herczku, Gergö Lakatos, Béla Sulik, Zoltán Juhász, Sándor Biri, Robert W. McCullough, Nigel J. Mason, Carsten Scavenius, Liv Hornekær, Sergio Ioppolo","doi":"10.1038/s41550-025-02765-7","DOIUrl":"https://doi.org/10.1038/s41550-025-02765-7","url":null,"abstract":"The origin of the molecular building blocks of life is a central question in science. A few α-amino acids, such as glycine, the simplest proteinogenic amino acid, have been detected in meteorites and comets, indicating an extraterrestrial origin for some prebiotic molecules. However, the formation of peptides, short chains of α-amino acids linked by peptide bonds, has remained unresolved under astrophysical conditions. Here we show that the building blocks of proteins can form in interstellar ice analogues exposed to ionizing radiation without the presence of liquid water. Using isotopically labelled glycine irradiated with protons at cryogenic temperatures, we detect the formation of glycylglycine, the simplest dipeptide, along with deuterated and undeuterated water as by-products. The formation of peptide bonds is confirmed by infrared spectroscopy and high-resolution mass spectrometry, which also reveal the production of other complex organic species. These findings demonstrate a non-aqueous route to peptide formation under space-like conditions and suggest that such molecules could form in the cold interstellar medium and be incorporated into forming planetary systems. Our results challenge aqueous-centric models of early biochemical evolution and broaden potential settings for the origins of life.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"94 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2026-01-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146006207","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 : 2026-01-19DOI: 10.1038/s41550-025-02709-1
Lucas Teinturier, Benjamin Charnay, Aymeric Spiga, Bruno Bézard
Brown dwarfs are massive, giant exoplanet analogues subject to variability and colour changes, known as the L/T transition, fundamental for their thermal evolution. The drivers of the L/T transition remain elusive, with atmospheric circulations and/or clouds usually suggested as potential mechanisms. Here, using a three-dimensional global climate model including cloud formation, transport and multiwavelength radiative effects, we show that clouds play a major role in shaping the atmospheric properties of brown dwarfs. The cloud radiative effect, which triggers atmospheric convection, leads to spectral, spatial and temporal variability in the modelled brown dwarfs, in agreement with the observed variability and L/T transition. Low latitudes are subject to sustained wave activity, whereas eddies dominate higher latitudes. Our results highlight that the role of clouds as a driver of atmospheric dynamics and climate, well known for giant exoplanets, extends to all substellar bodies. Brown dwarfs are substellar objects subject to variability and colour changes. A 3D general circulation model shows that clouds explain this observed behaviour and highlights their role as a driver of atmospheric dynamics and climate.
{"title":"Clouds as the driver of variability and colour changes in brown dwarf atmospheres","authors":"Lucas Teinturier, Benjamin Charnay, Aymeric Spiga, Bruno Bézard","doi":"10.1038/s41550-025-02709-1","DOIUrl":"10.1038/s41550-025-02709-1","url":null,"abstract":"Brown dwarfs are massive, giant exoplanet analogues subject to variability and colour changes, known as the L/T transition, fundamental for their thermal evolution. The drivers of the L/T transition remain elusive, with atmospheric circulations and/or clouds usually suggested as potential mechanisms. Here, using a three-dimensional global climate model including cloud formation, transport and multiwavelength radiative effects, we show that clouds play a major role in shaping the atmospheric properties of brown dwarfs. The cloud radiative effect, which triggers atmospheric convection, leads to spectral, spatial and temporal variability in the modelled brown dwarfs, in agreement with the observed variability and L/T transition. Low latitudes are subject to sustained wave activity, whereas eddies dominate higher latitudes. Our results highlight that the role of clouds as a driver of atmospheric dynamics and climate, well known for giant exoplanets, extends to all substellar bodies. Brown dwarfs are substellar objects subject to variability and colour changes. A 3D general circulation model shows that clouds explain this observed behaviour and highlights their role as a driver of atmospheric dynamics and climate.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"10 2","pages":"224-233"},"PeriodicalIF":14.3,"publicationDate":"2026-01-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146006205","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 : 2026-01-16DOI: 10.1038/s41550-025-02759-5
Colin J. Burke, Priyamvada Natarajan
Between the groundbreaking detections of stellar-mass black holes by LIGO/Virgo/KAGRA and the James Webb Space Telescope’s revelation of a surprisingly abundant population of supermassive black holes, one crucial missing link remains: the elusive intermediate-mass black holes (IMBHs). IMBHs represent a key phase in the hierarchical growth of black holes, yet they have persistently evaded detection. Traditional methods, effective for both actively accreting and quiescent black holes, have largely failed to uncover this hidden population. Here, we argue that novel observational strategies—particularly time-domain variability studies of active galactic nuclei and tidal disruption events—provide a promising path forward. Finding IMBHs will resolve critical gaps in our understanding of black hole formation and the various mechanisms driving their subsequent growth. The upcoming Vera C. Rubin Observatory, with its unprecedented capacity to monitor the dynamic sky, stands to revolutionize our ability to detect these long-sought IMBHs, shedding new light on the assembly history of black holes across cosmic time. Though understood to exist in large numbers, intermediate-mass black holes are difficult to identify. This Perspective makes a case for the use of time-domain variability studies to increase the known intermediate-mass black hole population.
在LIGO/Virgo/KAGRA对恒星质量黑洞的突破性探测和詹姆斯·韦伯太空望远镜对大量超大质量黑洞的惊人发现之间，一个关键的缺失环节仍然存在：难以捉摸的中质量黑洞（IMBHs）。IMBHs代表了黑洞分层成长的关键阶段，但它们一直逃避探测。传统的方法对活跃的吸积黑洞和静止的黑洞都有效，但在很大程度上未能发现这个隐藏的群体。在这里，我们认为新的观测策略——特别是对活动星系核和潮汐破坏事件的时域变异性研究——提供了一条有希望的前进道路。发现IMBHs将解决我们对黑洞形成和推动其后续增长的各种机制的理解中的关键空白。即将到来的Vera C. Rubin天文台，以其前所未有的监测动态天空的能力，将彻底改变我们探测这些长期寻找的IMBHs的能力，为黑洞在宇宙时间内的聚集历史提供新的线索。中等质量黑洞虽然被认为大量存在，但很难识别。这一视角为使用时域变异性研究来增加已知的中等质量黑洞数量提供了一个案例。
{"title":"Variability as a new discovery channel for intermediate-mass black holes in the time-domain era","authors":"Colin J. Burke, Priyamvada Natarajan","doi":"10.1038/s41550-025-02759-5","DOIUrl":"10.1038/s41550-025-02759-5","url":null,"abstract":"Between the groundbreaking detections of stellar-mass black holes by LIGO/Virgo/KAGRA and the James Webb Space Telescope’s revelation of a surprisingly abundant population of supermassive black holes, one crucial missing link remains: the elusive intermediate-mass black holes (IMBHs). IMBHs represent a key phase in the hierarchical growth of black holes, yet they have persistently evaded detection. Traditional methods, effective for both actively accreting and quiescent black holes, have largely failed to uncover this hidden population. Here, we argue that novel observational strategies—particularly time-domain variability studies of active galactic nuclei and tidal disruption events—provide a promising path forward. Finding IMBHs will resolve critical gaps in our understanding of black hole formation and the various mechanisms driving their subsequent growth. The upcoming Vera C. Rubin Observatory, with its unprecedented capacity to monitor the dynamic sky, stands to revolutionize our ability to detect these long-sought IMBHs, shedding new light on the assembly history of black holes across cosmic time. Though understood to exist in large numbers, intermediate-mass black holes are difficult to identify. This Perspective makes a case for the use of time-domain variability studies to increase the known intermediate-mass black hole population.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"10 2","pages":"187-195"},"PeriodicalIF":14.3,"publicationDate":"2026-01-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146224538","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}
Gravitational-wave (GW) ringdown signals from black holes encode crucial information about the gravitational dynamics in the strong-field regime, which offers unique insights into the properties of black holes. Improving the sensitivity of GW detectors will enable the extraction of several quasi-normal modes from ringdown signals. However, incorporating several modes drastically enlarges the parameter space, posing computational challenges to data analysis. Inspired by the {mathcal{F}}{mathcal{F}}-statistic method in the continuous GW searches, here we develop an algorithm that enhances the parameter-marginalization scheme, dubbed FIREFLY, which is tailored for accelerating the ringdown signal analysis. FIREFLY analytically marginalizes the amplitude and phase parameters of quasi-normal modes to reduce the computational cost and to speed up the standard Bayesian inference with full parameters from hours to minutes while achieving consistent posterior and evidence. The acceleration becomes more pronounced when more quasi-normal modes are considered. Rigorously based on Bayesian inference and importance sampling, our method is statistically interpretable, flexible in prior choice and compatible with various advanced sampling techniques and, thus, provides a new perspective for accelerating future GW data analysis.
{"title":"A practical Bayesian method for gravitational-wave ringdown analysis with multiple modes","authors":"Yiming Dong, Ziming Wang, Hai-Tian Wang, Junjie Zhao, Lijing Shao","doi":"10.1038/s41550-025-02766-6","DOIUrl":"https://doi.org/10.1038/s41550-025-02766-6","url":null,"abstract":"Gravitational-wave (GW) ringdown signals from black holes encode crucial information about the gravitational dynamics in the strong-field regime, which offers unique insights into the properties of black holes. Improving the sensitivity of GW detectors will enable the extraction of several quasi-normal modes from ringdown signals. However, incorporating several modes drastically enlarges the parameter space, posing computational challenges to data analysis. Inspired by the {mathcal{F}}{mathcal{F}}-statistic method in the continuous GW searches, here we develop an algorithm that enhances the parameter-marginalization scheme, dubbed FIREFLY, which is tailored for accelerating the ringdown signal analysis. FIREFLY analytically marginalizes the amplitude and phase parameters of quasi-normal modes to reduce the computational cost and to speed up the standard Bayesian inference with full parameters from hours to minutes while achieving consistent posterior and evidence. The acceleration becomes more pronounced when more quasi-normal modes are considered. Rigorously based on Bayesian inference and importance sampling, our method is statistically interpretable, flexible in prior choice and compatible with various advanced sampling techniques and, thus, provides a new perspective for accelerating future GW data analysis.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"5 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2026-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145968751","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 : 2026-01-15DOI: 10.1038/s41550-025-02729-x
Miki Nakajima, Sarah K. Harter, Alex V. Jasko, Danae N. Polsin, Ian Szumila, Kim A. Cone, Victor Lherm, Eric G. Blackman, Francis Dragulet, Lars Stixrude, Dustin Trail, Margaret F. Huff, J. Ryan Rygg, Angel Paz, Gilbert W. Collins, Alexa LaPierre, Zaire Sprowal
During planet formation, planets undergo many impacts that can generate magma oceans. When these crystallize, part of the magma densifies via iron enrichment and migrates to the core–mantle boundary, forming an iron-rich basal magma ocean (BMO). The BMO could generate a dynamo in early Earth and super-Earths if the electrical conductivity of the BMO, which is thought to be sensitive to its Fe content, is sufficiently high. To test this hypothesis, here we conduct laser-driven shock experiments on ferropericlase (Mgx,Fe1−x)O (0.95 ≤ x ≤ 1) as an Fe-rich BMO analogue, perform density functional theory molecular dynamics simulations on MgO and calculate the long-term evolution of super-Earths. We find that the d.c. conductivities of MgO and (Mg,Fe)O are indistinguishable between 467 GPa and 1,400 GPa, despite previous predictions. We predict that super-Earths larger than 3–6 Earth masses can produce BMO-driven dynamos that are almost one order of magnitude stronger than core-driven dynamos for several billion years. High-pressure measurements of the electrical conductivity of (Mg,Fe)O, used as an analogue for basal magma ocean material, indicate that the conductivity is high enough to produce a dynamo much stronger than a core-driven dynamo for super-Earths larger than 3–6 Earth masses.
{"title":"Electrical conductivities of (Mg,Fe)O at extreme pressures and implications for planetary magma oceans","authors":"Miki Nakajima, Sarah K. Harter, Alex V. Jasko, Danae N. Polsin, Ian Szumila, Kim A. Cone, Victor Lherm, Eric G. Blackman, Francis Dragulet, Lars Stixrude, Dustin Trail, Margaret F. Huff, J. Ryan Rygg, Angel Paz, Gilbert W. Collins, Alexa LaPierre, Zaire Sprowal","doi":"10.1038/s41550-025-02729-x","DOIUrl":"10.1038/s41550-025-02729-x","url":null,"abstract":"During planet formation, planets undergo many impacts that can generate magma oceans. When these crystallize, part of the magma densifies via iron enrichment and migrates to the core–mantle boundary, forming an iron-rich basal magma ocean (BMO). The BMO could generate a dynamo in early Earth and super-Earths if the electrical conductivity of the BMO, which is thought to be sensitive to its Fe content, is sufficiently high. To test this hypothesis, here we conduct laser-driven shock experiments on ferropericlase (Mgx,Fe1−x)O (0.95 ≤ x ≤ 1) as an Fe-rich BMO analogue, perform density functional theory molecular dynamics simulations on MgO and calculate the long-term evolution of super-Earths. We find that the d.c. conductivities of MgO and (Mg,Fe)O are indistinguishable between 467 GPa and 1,400 GPa, despite previous predictions. We predict that super-Earths larger than 3–6 Earth masses can produce BMO-driven dynamos that are almost one order of magnitude stronger than core-driven dynamos for several billion years. High-pressure measurements of the electrical conductivity of (Mg,Fe)O, used as an analogue for basal magma ocean material, indicate that the conductivity is high enough to produce a dynamo much stronger than a core-driven dynamo for super-Earths larger than 3–6 Earth masses.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"10 2","pages":"248-257"},"PeriodicalIF":14.3,"publicationDate":"2026-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145968770","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 : 2026-01-15DOI: 10.1038/s41550-025-02731-3
The generation mechanism of planetary magnetic fields in massive Earth-like planets (super-Earths) is uncertain. Now, shock experiments on a magma ocean analogue (Mg,Fe)O suggest that magma becomes metallic and electrically conductive under high pressures. This finding indicates that deep magma oceans in super-Earths might be metallic enough to produce strong magnetic fields.
{"title":"Magma oceans could host dynamos in massive Earth-like planets","authors":"","doi":"10.1038/s41550-025-02731-3","DOIUrl":"10.1038/s41550-025-02731-3","url":null,"abstract":"The generation mechanism of planetary magnetic fields in massive Earth-like planets (super-Earths) is uncertain. Now, shock experiments on a magma ocean analogue (Mg,Fe)O suggest that magma becomes metallic and electrically conductive under high pressures. This finding indicates that deep magma oceans in super-Earths might be metallic enough to produce strong magnetic fields.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"10 2","pages":"183-184"},"PeriodicalIF":14.3,"publicationDate":"2026-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146224548","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 : 2026-01-13DOI: 10.1038/s41550-026-02779-9
The calendar for 2026 looks set to be busy for the scientific and human exploration of the Solar System, the Galaxy and the wider Universe. From long-awaited planetary rendez-vous to cutting-edge telescope launches, these events will define the frontiers of astronomy, this year and beyond.
{"title":"The astronomical year ahead","authors":"","doi":"10.1038/s41550-026-02779-9","DOIUrl":"10.1038/s41550-026-02779-9","url":null,"abstract":"The calendar for 2026 looks set to be busy for the scientific and human exploration of the Solar System, the Galaxy and the wider Universe. From long-awaited planetary rendez-vous to cutting-edge telescope launches, these events will define the frontiers of astronomy, this year and beyond.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"10 1","pages":"1-2"},"PeriodicalIF":14.3,"publicationDate":"2026-01-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.nature.comhttps://www.nature.com/articles/s41550-026-02779-9.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146016498","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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