Nature Astronomy最新文献

{"title":"Calcium in a supernova remnant as a fingerprint of a sub-Chandrasekhar-mass explosion","authors":"Priyam Das, Ivo R. Seitenzahl, Ashley J. Ruiter, Friedrich K. Röpke, Rüdiger Pakmor, Frédéric P. A. Vogt, Christine E. Collins, Parviz Ghavamian, Stuart A. Sim, Brian J. Williams, Stefan Taubenberger, J. Martin Laming, Janette Suherli, Ralph Sutherland, Nicolás Rodríguez-Segovia","doi":"10.1038/s41550-025-02589-5","DOIUrl":"https://doi.org/10.1038/s41550-025-02589-5","url":null,"abstract":"<p>Type Ia supernovae play a fundamental role as cosmological probes of dark energy and produce more than half of the iron in our Galaxy. Despite their central importance, a comprehensive understanding of their progenitor systems and triggering mechanism is still a long-standing fundamental problem. Here we present high-resolution integral field spectroscopic observations of the young supernova remnant SNR 0509-67.5 in the Large Magellanic Cloud. We uncover a double-shell morphology of highly ionized calcium [Ca XV] and a single shell of sulphur [S XII], observed in the reverse shocked ejecta. Our analysis reveals that the outer calcium shell originates from the helium detonation at the base of the outer envelope, while the inner shell is associated with the carbon–oxygen core detonation. This morphological distribution of intermediate-mass elements agrees qualitatively with the predicted signature of the double detonation of a sub-Chandrasekhar-mass white dwarf from a hydrodynamical explosion simulation. Our observations reveal two distinct, spatially separated peaks in surface brightness of [Ca XV] from the supernova remnant phase, providing substantial evidence that sub-Chandrasekhar-mass explosions through the double-detonation mechanism could occur in nature. They also highlight the importance of remnant tomography in understanding explosion mechanisms from the remnant phase.</p>","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"47 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-07-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144533768","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}

{"title":"A high mutual inclination system around KOI-134 revealed by transit timing variations","authors":"Emma Nabbie, Chelsea X. Huang, Judith Korth, Hannu Parviainen, Su Wang, Alexander Venner, Robert Wittenmyer, Allyson Bieryla, David W. Latham, Gongjie Li, Douglas N. C. Lin, George Zhou","doi":"10.1038/s41550-025-02594-8","DOIUrl":"https://doi.org/10.1038/s41550-025-02594-8","url":null,"abstract":"<p>Few planetary systems have measured mutual inclinations, and even fewer are found to be non-coplanar. Observing the gravitational interactions between exoplanets is an effective tool to detect non-transiting companions to transiting planets. Evidence of these interactions can manifest in the light curve through transit timing variations (TTVs) and transit duration variations (TDVs). Here, through analysis of Kepler photometry and joint TTV–TDV modelling, we confirm the detection of KOI-134 b, a transiting planet with mass and size similar to Jupiter on a period of ~67 days, and find that it exhibits high TTVs (20-h amplitude) and significant TDVs. We explain these signals with the presence of an innermost non-transiting planet in 2:1 resonance with KOI-134 b. KOI-134 c has a mass <span>(M=0.22{0}_{-0.011}^{+0.010}{M}_{{rm{Jup}}})</span> and a moderately high mutual inclination with KOI-134 b of <span>({i}_{{rm{mut}}}=15.{4}_{-2.5}^{+2.{8}^{circ }})</span>. Moreover, the inclination variations of KOI-134 b are so large that the planet is predicted to stop transiting in about 100 years. This system architecture cannot be easily explained by any one formation mechanism, with other dynamical effects needed to excite the planets’ mutual inclination while still preserving their resonance.</p>","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"17 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-06-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144500396","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}

{"title":"Formation of Mercury by a grazing giant collision involving similar-mass bodies","authors":"Patrick Franco, Fernando Roig, Othon C. Winter, Rafael Sfair, Christoph Burger, Christoph M. Schäfer","doi":"10.1038/s41550-025-02582-y","DOIUrl":"https://doi.org/10.1038/s41550-025-02582-y","url":null,"abstract":"<p>The origin of Mercury still remains poorly understood compared with the other rocky planets of the Solar System. To explain its internal structure, it is usually considered to be the product of a giant impact. However, most studies assume a binary collision between bodies of substantially different masses, which seems to be unlikely according to <i>N</i>-body simulations. Here, we perform smoothed-particle hydrodynamics simulations to investigate the conditions under which collisions of similar-mass bodies are able to form a Mercury-like planet. Our results show that such collisions can fulfil the necessary constraints in terms of mass (0.055 <i>M</i>_{<span>⊕</span>}) and composition (30/70 silicate-to-iron mass ratio) within less than 5%, as long as the impact angles and velocities are properly adjusted according to well established scaling laws. With these results, we broaden the scope of plausible formation scenarios by presenting those that are more frequent in numerical simulations, less constrained in planetary contexts and thus more likely to happen.</p>","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"18 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-06-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144500394","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}

{"title":"Probable impact scenarios reproduce the structure of Mercury","authors":"","doi":"10.1038/s41550-025-02583-x","DOIUrl":"https://doi.org/10.1038/s41550-025-02583-x","url":null,"abstract":"Identifying viable impact scenarios that can reproduce the internal structure of Mercury, which is mainly composed of an iron core, is a long-standing problem. Hydrodynamic simulations show that collisions between two growing planets with comparable masses and appropriate speed and angle configurations could form Mercury’s unique structure.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"22 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-06-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144500398","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}

{"title":"Astronomy as a strategic driver for sustainable development","authors":"Joyful E. Mdhluli, Charles Takalana, Ramasamy Venugopal, Kevin Govender, Eslam Hussein, Dominic Vertue","doi":"10.1038/s41550-025-02602-x","DOIUrl":"https://doi.org/10.1038/s41550-025-02602-x","url":null,"abstract":"The ethos of the International Astronomical Union’s Office of Astronomy for Development is to direct astronomy towards addressing urgent societal needs. It does this by funding and managing hundreds of projects across the world.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"21 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-06-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144500392","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}

{"title":"An imaging spectrometer for a 4 m solar telescope","authors":"T. J. Kentischer, M. Schubert, C. Halbgewachs","doi":"10.1038/s41550-025-02604-9","DOIUrl":"https://doi.org/10.1038/s41550-025-02604-9","url":null,"abstract":"The Visible Tunable Filter (VTF) has recently been installed on the Daniel K. Inouye Solar Telescope in Hawai‘i. When complete, the instrument will offer high-resolution observations of the solar surface.","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"7 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-06-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144488362","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}

{"title":"A fast X-ray transient from a weak relativistic jet associated with a type Ic-BL supernova","authors":"H. Sun, W.-X. Li, L.-D. Liu, H. Gao, X.-F. Wang, W. Yuan, B. Zhang, A. V. Filippenko, D. Xu, T. An, S. Ai, T. G. Brink, Y. Liu, Y.-Q. Liu, C.-Y. Wang, Q.-Y. Wu, X.-F. Wu, Y. Yang, B.-B. Zhang, W.-K. Zheng, T. Ahumada, Z.-G. Dai, J. Delaunay, N. Elias-Rosa, S. Benetti, S.-Y. Fu, D. A. Howell, Y.-F. Huang, M. M. Kasliwal, V. Karambelkar, R. Stein, W.-H. Lei, T.-Y. Lian, Z.-K. Peng, D. D. Frederiks, A. V. Ridnaia, D. S. Svinkin, X.-Y. Wang, A.-L. Wang, D.-M. Wei, J. An, M. Andrews, J.-M Bai, C.-Y. Dai, S. A. Ehgamberdiev, Z. Fan, J. Farah, H.-C. Feng, J. P. U. Fynbo, W.-J. Guo, Z. Guo, M.-K. Hu, J.-W. Hu, S.-Q. Jiang, J.-J. Jin, A. Li, J.-D. Li, R.-Z. Li, Y.-F. Liang, Z.-X. Ling, X. Liu, J.-R. Mao, C. McCully, D. Mirzaqulov, M. Newsome, E. Padilla Gonzalez, X. Pan, G. Terreran, S. Tinyanont, B.-T. Wang, L.-Z. Wang, X.-D. Wen, D.-F. Xiang, S.-J. Xue, J. Yang, Z.-P. Zhu, Z.-M. Cai, A. J. Castro-Tirado, F.-S. Chen, H.-L. Chen, T.-X. Chen, W. Chen, Y.-H. Chen, Y.-F. Chen, Y. Chen, H.-Q. Cheng, B. Cordier, C.-Z. Cui, W.-W. Cui, Y.-F. Dai, D.-W. Fan, H. Feng, J. Guan, D.-W. Han, D.-J. Hou, H.-B. Hu, M.-H. Huang, J. Huo, S.-M. Jia, Z.-Q. Jia, B.-W. Jiang, C.-C. Jin, G. Jin, E. Kuulkers, C.-K. Li, D.-Y. Li, J.-F. Li, L.-H. Li, M.-S. Li, W. Li, Z.-D. Li, C.-Z. Liu, H.-Y. Liu, H.-Q. Liu, M.-J. Liu, F.-J. Lu, L.-D. Luo, J. Ma, X. Mao, K. Nandra, P. O’Brien, H.-W. Pan, A. Rau, N. Rea, J. Sanders, L.-M. Song, S.-L. Sun, X.-J. Sun, Y. -Y. Tan, Q.-J. Tang, Y.-H. Tao, H. Wang, J. Wang, L. Wang, W.-X. Wang, Y.-L. Wang, Y.-S. Wang, D.-R. Xiong, H.-T. Xu, J.-J. Xu, X.-P. Xu, Y.-F. Xu, Z. Xu, C.-B. Xue, Y.-L. Xue, A.-L. Yan, H.-N. Yang, X.-T. Yang, Y.-J. Yang, C. Zhang, J. Zhang, M. Zhang, S.-N. Zhang, W.-D. Zhang, W.-J. Zhang, Y.-H. Zhang, Z. Zhang, Z. Zhang, Z.-L. Zhang, D.-H. Zhao, H.-S. Zhao, X.-F. Zhao, Z.-J. Zhao, Y.-L. Zhou, Y.-X. Zhu, Z.-C. Zhu, H. Zou","doi":"10.1038/s41550-025-02571-1","DOIUrl":"https://doi.org/10.1038/s41550-025-02571-1","url":null,"abstract":"<p>Massive stars end their lives as core-collapse supernovae, among which some extremes are broad-lined type Ic supernovae from Wolf–Rayet stars associated with long-duration gamma-ray bursts (LGRBs) with powerful relativistic jets. Their less-extreme brethren make unsuccessful jets that are choked inside the stars, appearing as X-ray flashes or low-luminosity GRBs. However, there exists a population of extragalactic fast X-ray transients with timescales ranging from seconds to thousands of seconds, whose origins remain obscure. Here we report the discovery of the bright X-ray transient EP240414a detected by the Einstein Probe, which is associated with the type Ic supernova SN 2024gsa at a redshift of 0.401. The X-ray emission evolution is characterized by a very soft energy spectrum peaking at &lt;1.3 keV, which makes it different from known LGRBs, X-ray flashes or low-luminosity GRBs. Follow-up observations at optical and radio bands revealed the existence of a weak relativistic jet that interacts with an extended shell surrounding the progenitor star. Located on the outskirts of a massive galaxy, this event reveals a population of explosions of Wolf–Rayet stars characterized by a less powerful engine that drives a successful but weak jet, possibly owing to a progenitor star with a smaller core angular momentum than in traditional LGRB progenitors.</p>","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"16 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-06-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144488424","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}

{"title":"Determination of the mass distribution of the first stars from the 21-cm signal","authors":"T. Gessey-Jones, N. S. Sartorio, H. T. J. Bevins, A. Fialkov, W. J. Handley, E. de Lera Acedo, G. M. Mirouh, R. G. Izzard, R. Barkana","doi":"10.1038/s41550-025-02575-x","DOIUrl":"https://doi.org/10.1038/s41550-025-02575-x","url":null,"abstract":"<p>The formation of the first stars and the subsequent population of X-ray binaries represents a fundamental transition in the state of the Universe as it evolves from near homogeneity to being abundant in collapsed structures such as galaxies. Due to a lack of direct observations, the properties of these stars remain highly uncertain. Here, by considering the impact of the first stars and their remnant X-ray binaries on the cosmological 21-cm signal, we demonstrate that upcoming observations have the potential to improve our understanding of these objects. We find that a 25 mK sensitivity measurement of the 21-cm global signal by a wide-beam radiometer, such as REACH, or 3,000 h of foreground avoidance observations of the 21-cm power spectrum by SKA-Low, could provide 3<i>σ</i> constraints on the mass distribution of the first stars. Such measurements will fill a critical gap in our understanding of the early Universe and aid in interpreting high-redshift galaxy observations.</p>","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"24 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-06-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144329002","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}

{"title":"Co-precession of a curved jet and compact accretion disk in M87","authors":"Yuzhu Cui, Weikang Lin","doi":"10.1038/s41550-025-02580-0","DOIUrl":"https://doi.org/10.1038/s41550-025-02580-0","url":null,"abstract":"<p>Observational constraints on the configuration of the black hole (BH)–accretion disk–jet system are crucial to understanding BH spin, accretion disk physics and jet formation. The recently reported variation in the position angle of the M87 jet provides a new avenue for exploring these long-standing issues. The observed ~11-year periodicity, spanning over two cycles, is consistent with the Lense–Thirring precession of a compact, tilted accretion disk. However, how such a compact region decouples from the larger-scale accretion flow remains an open question in current numerical simulations. The jet precession challenges the traditional view of a strictly collimated jet by revealing a subtle curvature in the inner regions of the jet that dynamically links the jet to the spinning BH and successfully accounts for its unexpectedly wide inner projected profile. Although continued long-term observations are needed to distinguish coherent precession from stochastic fluctuations in the disk or jet orientation, these results open a new window for probing BH systems through coordinated multiscale observations and follow-on theoretical models.</p>","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"25 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-06-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144329004","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}

{"title":"Fermi detection of gamma-ray emission from the hot coronae of radio-quiet active galactic nuclei","authors":"Jun-Rong Liu, Jian-Min Wang","doi":"10.1038/s41550-025-02538-2","DOIUrl":"https://doi.org/10.1038/s41550-025-02538-2","url":null,"abstract":"<p>Relativistic jets around supermassive black holes are well-known powerful γ-ray emitters. In the absence of the jets in radio-quiet active galactic nuclei, how the supermassive black holes work in γ-ray bands is still unknown despite great observational efforts in the past three decades. Here, considering the previous efforts, we carefully select an active galactic nucleus sample composed of 37 nearby Seyfert galaxies with ultrahard X-rays for γ-ray detection by excluding all potential contamination in this band. Adopting a stacking technique, we report the significant γ-ray detection (test statistic 30.6, or 5.2<i>σ</i>) from the sample using 15-year Fermi-LAT observations. We find the average γ-ray luminosity of the sample to be (1.5 ± 1.0) × 10⁴⁰ erg s⁻¹ at energies of 1–300 GeV. Limited by the well-known pair production from the interaction of γ-rays with low-energy photons, γ-rays of more than several giga-electronvolts are found to originate from an extended corona (~2.7 × 10⁶ gravitational radii), whereas the canonical much more compact X-ray corona (~10 gravitational radii) is responsible for γ-rays of one to several giga-electronvolts. The finding of the compact region lends strong support to the long-time theoretical expectations, but the extended corona is an unexpected finding. One promising scenario is that the electron–positron pairs produced in the compact X-ray corona would expand as a fireball, similar to that in γ-ray bursts, forming the structure of extended corona.</p>","PeriodicalId":18778,"journal":{"name":"Nature Astronomy","volume":"19 1","pages":""},"PeriodicalIF":14.1,"publicationDate":"2025-06-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144329005","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}