The Astrophysical Journal Letters最新文献

{"title":"Magnetically Driven Neutron-rich Ejecta Unleashed: Global 3D Neutrino–General Relativistic Magnetohydrodynamic Simulations of Collapsars Probe the Conditions for r-process Nucleosynthesis","authors":"Danat Issa, Ore Gottlieb, Brian D. Metzger, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Goni Halevi and Alexander Tchekhovskoy","doi":"10.3847/2041-8213/adc694","DOIUrl":"https://doi.org/10.3847/2041-8213/adc694","url":null,"abstract":"Collapsars—rapidly rotating stellar cores that form black holes—can power gamma-ray bursts and are proposed to be key contributors to the production of heavy elements in the Universe via the rapid neutron capture process (r-process). Previous neutrino-transport collapsar simulations have been unable to unbind neutron-rich material from the disk. However, these simulations have not included sufficiently strong magnetic fields and the black hole (BH), both of which are essential for launching mass outflows. We present νh-amr, a novel neutrino-transport general relativistic magnetohydrodynamic (νGRMHD) code, which we use to perform the first 3D global νGRMHD collapsar simulations. We find a self-consistent formation of a weakly magnetized dense accretion disk, which has sufficient time to neutronize. Eventually, substantial magnetic flux accumulates near the BH, becomes dynamically important, leads to a magnetically arrested disk (MAD), and unbinds some of the neutron-rich material. However, the strong flux also hinders accretion, lowers density, and increases neutrino-cooling timescale, which prevents further disk neutronization. Typical collapsar progenitors with mass accretion rates, , do not produce significant neutron-rich (Ye < 0.25) ejecta. However, we find that MADs at higher mass accretion rates, (e.g., for more centrally concentrated progenitors), can unbind Mej ≲ M⊙ of neutron-rich ejecta. The outflows inflate a shocked cocoon that mixes with the infalling neutron-poor stellar gas and raises the final outflow Ye; however, the final r-process yield may be determined earlier at the point of neutron capture freeze-out. Future work will explore under what conditions more typical collapsar engines become r-process factories.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"19 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144104553","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"First Detection of Low-frequency Striae in Interplanetary Type III Radio Bursts","authors":"Vratislav Krupar, Eduard P. Kontar, Jan Soucek, Lynn B. Wilson, Adam Szabo, Oksana Kruparova, Hamish A. S. Reid, Mychajlo Hajos, David Pisa, Ondrej Santolik, Milan Maksimovic and Jolene S. Pickett","doi":"10.3847/2041-8213/add688","DOIUrl":"https://doi.org/10.3847/2041-8213/add688","url":null,"abstract":"We report the first detection of type III solar radio burst striae in the 30–80 kHz range, observed by the Cluster-4 spacecraft during an exceptionally quiet solar period. These low-frequency fine structures, which drift slowly in frequency and exhibit narrow bandwidths, provide a novel diagnostic of plasma processes in the inner heliosphere. The detected striae, interpreted as fundamental plasma emission, exhibit a frequency drift rate of 0.328 Hz s−1 and a bandwidth of 1.3 kHz. By combining high-resolution radio observations with well-calibrated in situ electron velocity distribution function data from the Wind spacecraft, we characterized the plasma properties of the burst source region near 0.32 au. Our analysis estimates relative density fluctuations, at the effective turbulence scale length, as approximately 3.4% (inferred from striae bandwidths), 0.62% (from intensity fluctuations), and 3.5% (from a heliocentric distance-based empirical model). These findings offer critical insights into small-scale density inhomogeneities and turbulence that affect electron beam propagation. This study underscores the potential of combining well-calibrated in situ electron data with radio burst measurements to probe the physical conditions of the solar wind and to refine our understanding of solar radio bursts across a broad frequency range.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"31 1","pages":"L27"},"PeriodicalIF":0.0,"publicationDate":"2025-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144114062","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Starspot Area Coverage: Correlation with Age and Spectral Type in FGK and M Stars","authors":"Alexandre Araújo, Ciria Lima, Fabian Menezes and Adriana Valio","doi":"10.3847/2041-8213/add338","DOIUrl":"https://doi.org/10.3847/2041-8213/add338","url":null,"abstract":"Starspots, analogous to sunspots, are surface manifestations of stellar magnetic activity. Their study provides crucial insights into stellar dynamo processes and the evolution of magnetic phenomena. However, due to limited data on magnetic activity across stellar lifetimes, the relationship between starspot area coverage and stellar properties remains underexplored. This work investigates the correlation between starspot area coverage and stellar age, effective temperature, and rotation period in FGK and M stars using data from Kepler and CoRoT. We utilized the starspot transit mapping method to analyze 11 stars, calculating starspot area coverage by integrating spot areas on the stellar surface. The average starspot coverage ranged from 4% to 29%, consistent with theoretical models of stellar magnetic evolution. Our analysis revealed a strong anticorrelation with stellar age (Spearman ρ = −0.80), confirming a significant decline in magnetic activity over time, but a weak anticorrelation between starspot coverage and rotation period. Regarding the relationship between absolute starspot area coverage and effective temperature, we found a moderate positive correlation (Spearman ρ = 0.40), with the majority of stars with an absolute area coverage of (2–4 ± 0.6) × 1010 km2. Incorporating starspot coverage into isochrone models could significantly improve stellar age estimates, especially for young stars. Moreover, these measurements are crucial for refining stellar dynamo models and advancing our understanding of magnetic field generation.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"16 1","pages":"L28"},"PeriodicalIF":0.0,"publicationDate":"2025-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144114060","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"First Detections of PN, PO, and PO+ toward a Shocked Low-mass Starless Core","authors":"Samantha Scibelli, Andrés Megías, Izaskun Jiménez-Serra, Yancy Shirley, Jennifer Bergner, Judit Ferrer Asensio, Robin T. Garrod, Mélisse Bonfand and Anissa Pokorny-Yadav","doi":"10.3847/2041-8213/add344","DOIUrl":"https://doi.org/10.3847/2041-8213/add344","url":null,"abstract":"Phosphorus is a key element that plays an essential role in biological processes important for living organisms on Earth. The origin and connection of phosphorus-bearing molecules to early solar system objects and star-forming molecular clouds is therefore of great interest, yet there are limited observations throughout different stages of low-mass (M < a few solar masses) star formation. Observations from the Yebes 40 m and IRAM 30 m telescopes detect for the first time in the 7 mm, 3 mm, and 2 mm bands multiple transitions of PN and PO, as well as a single transition of PO+, toward a low-mass starless core. The presence of PN, PO, and PO+ is kinematically correlated with bright SiO(1–0) emission. Our results reveal not only that shocks are the main driver of releasing phosphorus from dust grains and into the gas phase but that the emission originates from gas not affiliated with the shock itself but quiescent gas that has been shocked in the recent past. From radiative transfer calculations, the PO/PN abundance ratio is found to be , consistent with other high-mass and low-mass star-forming regions. This first detection of PO+ toward any low-mass star-forming region reveals a PO+/PO ratio of , a factor of 10 lower than previously determined from observations of a Galactic center molecular cloud, suggesting its formation can occur under more standard Galactic cosmic-ray ionization rates. These results motivate the need for additional observations that can better disentangle the physical mechanisms and chemical drivers of this precursor of prebiotic chemistry.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"14 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-05-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144104608","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The Striated Solar Photosphere Observed at 0 . ...","authors":"David Kuridze, Friedrich Wöger, Han Uitenbroek, Matthias Rempel, Alexandra Tritschler, Thomas Rimmele, Catherine Fischer and Oskar Steiner","doi":"10.3847/2041-8213/add470","DOIUrl":"https://doi.org/10.3847/2041-8213/add470","url":null,"abstract":"Striated granular edges observed in the solar photosphere represent one of the smallest-scale phenomena on the Sun. They arise from the interaction of strongly coupled hydrodynamic, magnetic, and radiative properties of the plasma. In particular, modulations in the photospheric magnetic field strength cause variations in density and opacity along the line of sight, leading to their formation. Therefore, the striation patterns can be used as valuable diagnostics for studying the finest-scale structure of the photospheric magnetic field. The Daniel K. Inouye Solar Telescope (DKIST) allows observations of the solar atmosphere with a spatial resolution of better than 0 03 with its current instrumentation. We analyze images acquired with the Visible Broadband Imager using the G-band channel to investigate the characteristics of fine-scale striations in the photosphere and compare them with state-of-the-art radiation-MHD simulations at similar spatial resolution. Both observed and synthetic images reveal photospheric striae with widths of approximately 20−50 km, suggesting that at least 4 m class solar telescopes are necessary to resolve this ultrafine structure. Analysis of the numerical simulations confirms that the striation observed in the filtergrams is associated with spatial variations in photospheric magnetic flux concentrations, which cause shifts in the geometrical height where the emergent intensity forms. Some fine-scale striations in the synthetic images originate from magnetic field variations of approximately 100 G, resulting in Wilson depressions as narrow as 10 km. This suggests that DKIST G-band images can trace the footprints of magnetic field variations and Wilson depressions at a similar scale.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"15 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-05-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144104609","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Modeling Galaxies in the Early Universe with Supernova Dust Attenuation","authors":"Jed McKinney, Olivia R. Cooper, Caitlin M. Casey, Julian B. Muñoz, Hollis Akins, Erini Lambrides and Arianna S. Long","doi":"10.3847/2041-8213/add15d","DOIUrl":"https://doi.org/10.3847/2041-8213/add15d","url":null,"abstract":"Supernovae (SNe) may be the dominant channel by which dust grains accumulate in galaxies during the first Gyr of cosmic time as formation channels important for lower-redshift galaxies, e.g., asymptotic giant branch stars and grain growth, may not have had sufficient time to take over. SNe produce fewer small grains, leading to a flatter attenuation law. In this work, we fit observations of 138 spectroscopically confirmed z > 6 galaxies adopting standard spectral energy distribution (SED) modeling assumptions and compare standard attenuation law prescriptions to a flat attenuation law. Compared to SMC dust, flat attenuation close to what may be expected from dust produced in SNe yields up to 0.5 mag higher AV and 0.4 dex larger stellar masses. It also finds better fits to the rest-frame UV photometry with lower , allowing the observed UV luminosities taken from the models to be fainter by 0.2 dex on average. The systematically fainter observed UV luminosities for fixed observed photometry could help resolve current tension between the ionizing photon production implied by JWST observations and the redshift evolution of the neutral hydrogen fraction. Given these systematic effects and the physical constraint of cosmic time itself, fairly flat attenuation laws that could represent the properties of dust grains produced by SNe should be a standard consideration in fitting to the SEDs of z > 6 galaxies.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"18 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-05-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144097504","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"XRISM Forecast for the Coma Cluster: Stormy, with a Steep Power Spectrum","authors":"XRISM Collaboration, Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto,..","doi":"10.3847/2041-8213/add2f6","DOIUrl":"https://doi.org/10.3847/2041-8213/add2f6","url":null,"abstract":"The XRISM Resolve microcalorimeter array measured the velocities of hot intracluster gas at two positions in the Coma galaxy cluster: squares at the center and at 6 (170 kpc) to the south. We find the line-of-sight velocity dispersions in those regions to be σz = 208 ± 12 km s−1 and 202 ± 24 km s−1, respectively. The central value corresponds to a 3D Mach number of M = 0.24 ± 0.015 and a ratio of the kinetic pressure of small-scale motions to thermal pressure in the intracluster plasma of only 3.1% ± 0.4%, at the lower end of predictions from cosmological simulations for merging clusters like Coma, and similar to that observed in the cool core of the relaxed cluster A2029. Meanwhile, the gas in both regions exhibits high line-of-sight velocity differences from the mean velocity of the cluster galaxies, Δvz = 450 ± 15 km s−1 and 730 ± 30 km s−1, respectively. A small contribution from an additional gas velocity component, consistent with the cluster optical mean, is detected along a sight line near the cluster center. The combination of the observed velocity dispersions and bulk velocities is not described by a Kolmogorov velocity power spectrum of steady-state turbulence; instead, the data imply a much steeper effective slope (i.e., relatively more power at larger linear scales). This may indicate either a very large dissipation scale, resulting in the suppression of small-scale motions, or a transient dynamic state of the cluster, where large-scale gas flows generated by an ongoing merger have not yet cascaded down to small scales.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"12 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-05-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144097592","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Galactic Accelerations from the GD-1 Stream Suggest a Tilted Dark Matter Halo","authors":"Jacob Nibauer and Ana Bonaca","doi":"10.3847/2041-8213/add0a9","DOIUrl":"https://doi.org/10.3847/2041-8213/add0a9","url":null,"abstract":"Cold dark matter halos are expected to be triaxial and often tilted relative to the stellar disk. Stellar streams provide a sensitive tracer of the Milky Way’s halo shape though models for the Galactic potential are typically limited to simple, symmetric functional forms. Here, we measure the Galactic acceleration field along the GD-1 stream using a direct differentiation of the stream’s track in phase space. Using a fully data-driven catalog of stream members from Gaia, Sloan Digital Sky Survey, LAMOST, and DESI, we map the stream in 6D phase space. We fit splines to the stream track and infer cylindrical acceleration components , az = −1.8 ± 0.1, and aϕ = 0.2 ± 0.1 km s−1 Myr−1 at (R, z, ϕ) = (11.9 kpc, 7.3 kpc, 171 1). We measure mass enclosed within 14 kpc of 1.4 ± 0.1 × 1011 M⊙ and z-axis density flattening of , both consistent with previous estimates. However, we find a 2σ deviation from an axisymmetric acceleration field, which can be explained by a triaxial dark matter halo with axis ratios 1:0.75:0.70. The major axis of the halo is consistent with a tilt of 18° above the Galactic plane in the direction of the Sun. The magnitude and direction of the tilt are consistent with measurements of the stellar halo from Gaia and the Hectochelle in the Halo at High Resolution survey. A tilted triaxial halo has important consequences for orbit-integration-based studies of the Galaxy and can be further tested by deriving acceleration constraints from multiple streams.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"316 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-05-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144088301","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Mars Gravity Field Determination Using Tianwen-1 Orbiter Tracking Data","authors":"Chongyang Wang, Jianguo Yan, Shanhong Liu, Shangbiao Sun, Jianfeng Cao, Denggao Qiu, Xie Li and Jean-Pierre Barriot","doi":"10.3847/2041-8213/adce6d","DOIUrl":"https://doi.org/10.3847/2041-8213/adce6d","url":null,"abstract":"The Martian gravity field is a key data set for studying the internal structure of Mars. For this purpose, we processed all the two-way Doppler tracking data of the Tianwen-1 orbiter from 2021 June to 2024 October and determined a new degree and order 80 Martian static gravity field model, TW80. The Tianwen-1 orbiter tracking data show high accuracy, with approximately 90% of arcs achieving an rms of residuals of less than 0.1 mm s–1. We evaluated this model in terms of gravity anomaly errors, gravity/topography correlation, and orbit determination performance. The TW80 gravity field model reaches a global resolution of degree and order 74, corresponding to a spatial resolution of approximately 140 km. The rms of the gravity anomaly errors is approximately 35.8 mGal, with notably smaller errors near the south pole region in the southern hemisphere and larger errors in mid- and low-latitude regions. The TW80 model shows a high correlation with topography and is consistent with the MRO120D gravity field model up to degree 40. Due to the highly elliptical orbit geometry, the orbit determination performance of the TW80 model for the Tianwen-1 orbiter is comparable to that of the MRO120D model, with radial differences less than 100 m and total position differences less than 500 m. Further improvements in orbit determination accuracy will focus on precise modeling of orbital maneuvers and the solar radiation pressure model, as well as extending the tracking duration of individual arcs.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"4 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-05-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144088300","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The Giant Eruption in Solar Cycle 25 Caused by Collisional Shearing","authors":"Tao Ding, Jun Zhang and Yijun Hou","doi":"10.3847/2041-8213/add32c","DOIUrl":"https://doi.org/10.3847/2041-8213/add32c","url":null,"abstract":"On 2024 October 3, solar active region (AR) 13842 produced an X9.0 flare, which is the largest one in Solar Cycle 25 so far. Our study is to answer the question of what process caused this flare. Based on the magnetic field observations from the Solar Dynamics Observatory (SDO), we find that the nonconjugated sunspots of opposite polarities of the AR core region underwent a persistent collision process with strong shearing motions. Moreover, flux cancellation was observed at the collision region, e.g., 1021 Mx of unsigned flux canceled at the local area within 2 hr, suggesting the occurrence of collisional shearing. Meanwhile, a collisional polarity inversion line (PIL) was produced in the AR core region as a result of the collision of the nonconjugated polarities during flux emergence. The SDO/Atmospheric Imaging Assembly extreme-ultraviolet observations show that two flux ropes formed above the PIL. Due to the photospheric magnetic field evolution, the two flux ropes destabilized and then erupted simultaneously. Using nonlinear force-free field modeling, we notice that there were three flux ropes at the PIL, including the two ropes mentioned above and another unobserved one. We suggest that the formation of flux ropes that carry massive accumulated free energy by the collisional shearing process and the eruption of the flux rope system are responsible for the giant flare in Solar Cycle 25.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"122 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-05-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144066825","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}