Astronomy & Astrophysics最新文献

{"title":"Optical observations of the peculiar high-mass X-ray binary 4U 2206+54","authors":"K. A. Stoyanov, M. Moyseev, Y. M. Nikolov, R. K. Zamanov, G. Y. Latev, K. Iłkiewicz, V. Hambaryan","doi":"10.1051/0004-6361/202554256","DOIUrl":"https://doi.org/10.1051/0004-6361/202554256","url":null,"abstract":"<i>Context.<i/> We present results from the high-resolution optical spectroscopy and spectropolarimetry of the peculiar high-mass X-ray binary 4U 2206+54.<i>Aims.<i/> We aim to estimate the size of the circumstellar disc and investigate the interaction between the compact object and the matter in the disc. We also study the interstellar polarisation towards 4U 2206+54.<i>Methods.<i/> We performed a periodogram analysis on the spectral data to identify periodicities. We estimated the radius of the circumstellar disc and the distance between the components at periastron. We used two methods to determine the interstellar polarisation towards 4U 2206+54, both of which yield similar results.<i>Results.<i/> We estimate that the outer radius of the H<i>α<i/>-emitting circumstellar disc varies between 7.9 and 15.2 <i>R<i/><sub>⊙<sub/> with an average value of 10.9 <i>R<i/><sub>⊙<sub/>. This suggests that when the disc is small, the neutron star does not reach the outer parts of the circumstellar disc. Based on our spectropolarimetric observations of 4U 2206+54, we can conclude that the dominant component of the polarisation is interstellar. A depolarisation effect is visible in the H<i>α<i/> emission line, which indicates intrinsic polarisation. We estimate that the intrinsic degree of polarisation in the synthetic <i>V<i/> band is <i>P<i/><sub>int<sub/> (<i>V<i/>) (%) = 0.5 ± 0.2 at the position angle PA<sub>int<sub/> (<i>V<i/>)≈47°.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"31 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144123047","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"The mass distribution of stars stripped in binaries: The effect of metallicity","authors":"B. Hovis-Afflerbach, Y. Götberg, A. Schootemeijer, J. Klencki, A. L. Strom, B. A. Ludwig, M. R. Drout","doi":"10.1051/0004-6361/202453185","DOIUrl":"https://doi.org/10.1051/0004-6361/202453185","url":null,"abstract":"Stars stripped of their hydrogen-rich envelopes through binary interaction are thought to be responsible for both hydrogen-poor supernovae and the hard ionizing radiation observed in low-<i>Z<i/> galaxies. A population of these stars was recently observed for the first time, but their prevalence remains unknown. In preparation for such measurements, we estimate the mass distribution of hot, stripped stars using a population synthesis code that interpolates over detailed single and binary stellar evolution tracks. We predict that for a constant star formation rate of 1 <i>M<i/><sub>⊙<sub/>/yr and regardless of metallicity, a scalable model population contains ∼30 000 stripped stars with mass <i>M<i/><sub>strip<sub/> > 1 <i>M<i/><sub>⊙<sub/> and ∼4000 stripped stars that are sufficiently massive to explode (<i>M<i/><sub>strip<sub/> > 2.6 <i>M<i/><sub>⊙<sub/>). Below <i>M<i/><sub>strip<sub/> = 5 <i>M<i/><sub>⊙<sub/>, the distribution is metallicity-independent and can be described by a power law with the exponent <i>α<i/> ∼ −2. At higher masses and lower metallicity (<i>Z<i/> ≲ 0.002), the mass distribution exhibits a drop. This originates from the prediction, frequently seen in evolutionary models, that massive low-metallicity stars do not expand substantially until central helium burning or later and therefore cannot form long-lived stripped stars. With weaker line-driven winds at low metallicity, this suggests that neither binary interaction nor wind mass loss can efficiently strip massive stars at low metallicity. As a result, a “helium-star desert” emerges around <i>M<i/><sub>strip<sub/> = 15 <i>M<i/><sub>⊙<sub/> at <i>Z<i/> = 0.002, covering an increasingly large mass range with decreasing metallicity. We note that these high-mass stars are those that potentially boost a galaxy’s He<sup>+<sup/>-ionizing radiation and that participate in the formation of merging black holes. This “helium-star desert” therefore merits further study.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"133 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144123051","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Anomalous cross-field motions of solar coronal loops","authors":"Sudip Mandal, Hardi Peter, James A. Klimchuk, Lakshmi Pradeep Chitta","doi":"10.1051/0004-6361/202553934","DOIUrl":"https://doi.org/10.1051/0004-6361/202553934","url":null,"abstract":"We present several examples of unusual evolutionary patterns in solar coronal loops that resemble cross-field drift motions. These loops were simultaneously observed from two vantage points by two different spacecraft: the High-Resolution Imager of the Extreme Ultraviolet Imager aboard the Solar Orbiter and the Atmospheric Imaging Assembly aboard the Solar Dynamics Observatory. Across all these events, a recurring pattern is observed: Initially, a thin, strand-like structure detaches and shifts several megameters away from a main or parent loop. During this period, the parent loop remains intact in its original position. After a few minutes, the shifted strand reverses its direction and returns to the location of the parent loop. Key features of this “split-drift” type evolution are: (i) the presence of kink oscillations in the loops before and after the split events and (ii) a sudden split motion at about 30 km s<sup>−1<sup/>, with additional slow drifts, either away from or back to the parent loops, at around 5 km s<sup>−1<sup/>. Co-temporal photospheric magnetic field data obtained from the Helioseismic and Magnetic Imager reveal that during such split-drift evolution, one of the loop points in the photosphere moves back and forth between nearby magnetic polarities. While the exact cause of this split drift phenomenon is still unclear, the consistent patterns observed in its characteristics indicate that there may be a broader physical mechanism at play. This underscores the need for further investigation through both observational studies and numerical simulations.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"9 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144123046","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Propagation of coronal large-amplitude Alfvén-type waves to the solar photosphere","authors":"I. Živanović, V. V. Smirnova, Yu. T. Tsap, Y. Chen","doi":"10.1051/0004-6361/202452849","DOIUrl":"https://doi.org/10.1051/0004-6361/202452849","url":null,"abstract":"<i>Context.<i/> We present a study of the propagation of magnetohydrodynamic (MHD) Alfvén-type waves from the solar corona to the photosphere, generated by the large-amplitude velocity pulse.<i>Aims.<i/> We aim to estimate the energy flux and the propagation time of Alfvén-type waves, which can be responsible for the white-light flare emission caused by solar photospheric heating.<i>Methods.<i/> The ideal MHD equations were solved with the PLUTO code for the two-dimensional force-free magnetic configuration in the stratified solar atmosphere. We consider the evolution of the electromagnetic energy flux maximum caused by the non-linear large-amplitude velocity pulse launched in the solar corona.<i>Results.<i/> We find that the Alfvén energy flux is about a few orders of magnitude less than the required values. It cannot heat the flare photosphere, due to the energy losses from the non-linear effects, the solar atmosphere stratification, and the influence of the magnetic configuration. The calculated characteristic propagation time of the energy flux from the corona to the photosphere was about 2 min which does not match some time delays between hard X-ray and white-light flare emissions. The results obtained suggest that Alfvén waves can make a significant contribution to the continuum optical emission generated in the chromosphere.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"19 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144104732","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Discovery of resonating integration modes in triple-mode high-amplitude δ Scuti stars: A new evolutionary phase indicator","authors":"Jia-Shu Niu, Hui-Fang Xue","doi":"10.1051/0004-6361/202554170","DOIUrl":"https://doi.org/10.1051/0004-6361/202554170","url":null,"abstract":"High-amplitude <i>δ<i/> Scuti stars (HADS) that pulsate in their first three radial modes are rare in current samples. Here, we analyse five such triple-mode HADS observed by the Transiting Exoplanet Survey Satellite (TESS) and report that the previously considered second overtone mode (<i>f<i/><sub>2<sub/>) is actually the non-radial component of a resonating integration mode (RI mode, resulting from resonance between a radial <i>p<i/>-mode and a non-radial <i>p<i/>-<i>g<i/> mixed mode), which shows significant amplitude and frequency variations over short timescales (approximately 20 days). This RI mode appears to be widespread among these stars. Notably, all five stars are in the post-main sequence evolutionary phase, actively crossing the Hertzsprung gap. These stars offer valuable insights into stellar evolution during the Hertzsprung gap, which is one of the most rapid evolutionary stages in a star’s life.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"33 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144104728","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Binary evolution pathways to blue large-amplitude pulsators: Insights from HD 133729","authors":"Zhengyang Zhang, Chengyuan Wu, Xianfei Zhang, Zhanwen Han, Bo Wang","doi":"10.1051/0004-6361/202553749","DOIUrl":"https://doi.org/10.1051/0004-6361/202553749","url":null,"abstract":"Blue large-amplitude pulsators (BLAPs) are a recently identified class of pulsating stars distinguished by their short pulsation periods (2–60 minutes) and asymmetric light curves. This study investigated the evolutionary channel of HD 133729, which is the first confirmed BLAP in a binary system. Using the binary evolution code MESA, we explored various mass ratios and initial orbital periods. Our simulations suggest that a system with a mass ratio <i>q<i/> = 0.30 undergoing non-conservative mass transfer (<i>β<i/> = 0.15) can reproduce the observed characteristics through the pre-white-dwarf Roche lobe overflow channel. Meanwhile, we postulate that there are significant helium and nitrogen enhancements on the surface of the main sequence (MS) star. The system will eventually undergo the common envelope phase, leading to a stellar merger. HD 133729 is a unique case, providing crucial insights into the formation mechanism and evolutionary fate of BLAPs with MS companions. This work constrains the elemental abundances of the MS star and has advanced our understanding of non-conservative mass transfer in binary evolution.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"2 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144088293","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Size and shape of the trans-Neptunian object (470316) 2007 OC10: Comparison with thermal data","authors":"J. M. Gómez-Limón, R. Leiva, J. L. Ortiz, N. Morales, M. Kretlow, M. Vara-Lubiano, P. Santos-Sanz, A. Álvarez-Candal, J. L. Rizos, R. Duffard, E. Fernández-Valenzuela, Y. Kilic, S. Cikota, B. Sicardy, F. Bragas-Ribas, M. R. Alarcon, S. Aliş, Z. Benkhaldoun, A. Burdanov, J. de Wit, S. Calavia Belloc, J. Calvo Fernández, O. Canales Moreno, G. Catanzaro, S. Fişek, A. Frasca, R. Iglesias-Marzoa, R. Infante-Sainz, A. Jiménez-Guisado, S. Kaspi, T. Kuutma, D. Lafuente Aznar, J. Licandro, J. L. Maestre, P. Martorell, A. Nastasi, G. Occhipinti, C. Perelló, C. Rinner, B. Samper-Doménech, A. San Segundo, T. Santana-Ros, M. Serra-Ricart","doi":"10.1051/0004-6361/202453540","DOIUrl":"https://doi.org/10.1051/0004-6361/202453540","url":null,"abstract":"<i>Context.<i/> The shapes of only 12 trans-Neptunian objects have been directly measured, offering crucial insights into their internal structure. These properties are strongly connected to the processes that shaped the early Solar System, and provide important clues about its evolution.<i>Aims.<i/> The aim of the present work is to characterise the size, shape, geometric albedo, and beaming parameter of the TNO (470316) 2007 OC10. We compared these values to the effective diameter and geometric albedo obtained from thermal data by the TNOs are Cool survey. We also combined occultation and thermal data to constrain the size of a putative unresolved satellite.<i>Methods.<i/> We predicted an occultation of the star <i>Gaia<i/> DR3 2727866328215869952 by 2007 OC10 on 2022 August 22. Four stations detected the occultation. We implemented an elliptical shape model for the projection of 2007 OC10. Following a Bayesian approach, we obtained the posterior probability density in the model parameter space using a Markov chain Monte Carlo method.<i>Results.<i/> The elliptical limb of 2007 OC 10 has semi-axes of 215<sub>-7<sub/><sup>+10<sup/> × 141<sub>-23<sub/><sup>+24<sup/> km, and thus the projected axis ratio is <i>b/a<i/> = 0.58<sub>-0.16<sub/><sup>+0.16<sup/>. The area-equivalent diameter is 330<sub>-55<sub/><sup>+56<sup/> km. From our own absolute magnitude value of <i>H<sub>V<sub/><i/> = 5.40 ± 0.02, the geometric albedo is <i>p<sub>V<sub/><i/> = 11.2<sub>-5.0<sub/><sup>+2.1<sup/>%. Combining the occultation results with thermal data, we constrain the beaming parameter to <i>η<i/> = 1.42<sub>-0.58<sub/><sup>+0.75<sup/>. Occultation data reveal that the star is double. The secondary star has a position angle with respect to the primary of 56<sub>-17<sub/><sup>+3<sup/> degrees, has an angular separation of 57<sub>-11<sub/><sup>+4<sup/> mas, and is 1.18<sub>-0.07<sub/><sup>+0.07<sup/> magnitudes fainter than the primary.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"55 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144088303","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Search for γ-ray emission from supernova remnants in the Large Magellanic Cloud: A new cluster analysis at energies above 4 GeV","authors":"A. Tramacere, R. Campana, E. Massaro, F. Bocchino, M. Miceli, S. Orlando","doi":"10.1051/0004-6361/202553665","DOIUrl":"https://doi.org/10.1051/0004-6361/202553665","url":null,"abstract":"<i>Context.<i/> A search for <i>γ<i/>-ray emission from supernova remnants (SNRs) in the Large Magellanic Cloud (LMC) based on the detection of concentrations in the arrival direction <i>Fermi<i/>-LAT images of photons at energies higher than 10 GeV found significant evidence for nine sources. This analysis was based on data collected in the time window from August 4, 2008, to August 4, 2020 (12 years).<i>Aims.<i/> In the present contribution, we report the results of a new search extended using a 15-year long (up to August 4, 2023) dataset and to a broad energy range (higher than 4 GeV). The longer baseline and the softer energy lower limit are required to further understand the relation between the X-ray and gamma ray SNRs in the LMC and to investigate the completeness of the sample at low luminosities.<i>Methods.<i/> Two different methods of clustering analysis were applied: minimum spanning tree (MST) and a combination of density-based spatial clustering of applications with noise (DBSCAN) and DENsity-based CLUstEring (DENCLUE) algorithms.<i>Results.<i/> We confirm all previous detections and found positive indications for at least eight new clusters with a spatial correspondence with other SNRs, thus increasing the number of candidate remnants in the LMC or detected in the high-energy <i>γ<i/>-rays to 16 sources.<i>Conclusions.<i/> This study extends previous analyses of <i>γ<i/>-ray emission from SNRs in the LMC by incorporating a longer observational baseline and a broader energy range. The improved dataset and advanced clustering techniques enhance our understanding of the connection between X-ray and <i>γ<i/>-ray SNRs, providing new insights into their high-energy properties and contributing to the assessment of the completeness of the sample at lower luminosities.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"38 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144088310","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"Simulation of the distribution of radio pulsar nulling fractions","authors":"R. Yuen","doi":"10.1051/0004-6361/202553813","DOIUrl":"https://doi.org/10.1051/0004-6361/202553813","url":null,"abstract":"<i>Aims.<i/> In this work, we aim to simulate the observed distribution of the pulse nulling fractions (NFs) in radio pulsars and to investigate the associated properties of the emission region.<i>Methods.<i/> We identified three conditions related to the occurrence of pulse nulling. From the traditional approach for correlation of the pulsed radio intensity and plasma density, a pulse cessation results from switching in the plasma density to zero. Second, recent observations have shown that the occurrence of a pulse cessation appears to favor certain emission conditions. Third, the observation of specific emission properties across different parts of a profile indicates that the emission region may be segmented. A detectable null would then correspond to the presence of a favorable condition, whereby the switching to zero plasma density occurs in all the emission segments visible to the observer. By dividing the emission region into equal segments around the magnetic axis, we simulated the distribution of NFs based on 5000 pulsar samples, each with 1000 rotations.<i>Results.<i/> Our results show that an emission region with 16 ± 4 segments gives the best-fit NF distribution for the recent observations. We find that while the number of nulling pulsars increases as their age increases, the NFs do not demonstrate a strong correlation with the obliquity angle, measured between the rotation and the magnetic axes. We show that the former relationship is related to the emission geometry, whereas the latter may be due to an additional mechanism on top of the traditional radio emission generation. The model predicts that nulling is expected to occur in all pulsars, although it is more common in pulsars of older ages.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"10 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144088309","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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":"High energy time lags of gamma-ray bursts","authors":"C. Maraventano, G. Ghirlanda, L. Nava, T. Di Salvo, W. Leone, R. Iaria, L. Burderi, A. Tsvetkova","doi":"10.1051/0004-6361/202554053","DOIUrl":"https://doi.org/10.1051/0004-6361/202554053","url":null,"abstract":"<i>Context.<i/> Positive lags between the arrival time of different photon energies are commonly observed in the prompt phase of gamma-ray bursts (GRBs), where soft photons lag behind harder ones. However, a fraction of GRBs display the opposite behavior. In particular, <i>Fermi<i/> Large Area Telescope (LAT) observations revealed that high-energy photons are often characterized by a delayed onset.<i>Aims.<i/> We explore the potential of spectral lags as a diagnostic tool to identify distinct emission components or processes. By analyzing data from the <i>Fermi<i/> Gamma-ray Burst Monitor (GBM) and the LAT Low Energy (LLE) technique, we explore the connection between lag behavior and high-energy spectral properties.<i>Methods.<i/> We analyze a sample of 70 GRBs from the LLE catalog. Spectral lags are computed using the discrete correlation function method, considering light curves extracted in four different energy bands, from 10 keV to 100 MeV. Additionally, we compare LLE time lags with properties of the prompt emission and with the spectral behavior at high energies.<i>Results.<i/> Time lags computed across different energy bands distributed between 10 keV and 1 MeV are predominantly positive (76%) as a possible consequence of a hard-to-soft spectral evolution of the prompt spectrum. Lags between the LLE (30–100 MeV) and the GBM (10–100 keV) bands show a variety of behaviors: 40% are positive, while 37% are negative. Such negative lags may suggest the delayed emergence of an additional emission component dominating at high energies. Indeed, the spectral analysis of LLE data for 56 GRBs shows that negative lags are associated with an LLE spectral index typically harder than the high-energy power law identified in GBM data.<i>Conclusions.<i/> Spectral lags of LLE data can be exploited as a diagnostic tool to identify and characterize emission components in GRBs, highlighting the importance of combining temporal and spectral analyses to advance our understanding of GRB emission mechanisms.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"32 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-05-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144088304","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"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}