The Astrophysical Journal Letters最新文献_第2页

The First Observation of a Polar Coronal Hole-like Fast Solar Wind Stream in the Sub-Alfvénic Solar Corona: An Analysis of Turbulence Properties 亚阿尔夫萨奇日冕中极冕洞样快速太阳风流的首次观测：湍流特性分析

The Astrophysical Journal Letters Pub Date : 2026-10-08 DOI: 10.3847/2041-8213/aeaae2

Riddhi Bandyopadhyay,Sujan Prasad Gautam,William H. Matthaeus,Yeimy J. Rivera,Samuel T. Badman

引用次数: 0

Collisionless Shock Driven by a Supersonic Velocity Shear 由超音速切变驱动的无碰撞冲击

The Astrophysical Journal Letters Pub Date : 2026-10-07 DOI: 10.3847/2041-8213/aeaba2

Kazuki Kamiido,Yutaka Ohira

引用次数: 0

Solar Soft X-Ray Coronal Dimming in a Failed Eruption Associated with Plasma Cooling 太阳软x射线日冕变暗与等离子体冷却有关的一次失败喷发

The Astrophysical Journal Letters Pub Date : 2026-10-07 DOI: 10.3847/2041-8213/aea099

Xinyue Wang,Astrid M. Veronig,Hechao Chen,Hui Tian

{"title":"Solar Soft X-Ray Coronal Dimming in a Failed Eruption Associated with Plasma Cooling","authors":"Xinyue Wang,Astrid M. Veronig,Hechao Chen,Hui Tian","doi":"10.3847/2041-8213/aea099","DOIUrl":"https://doi.org/10.3847/2041-8213/aea099","url":null,"abstract":"Abstract Coronal dimmings are observed as sudden and localized reductions in the extreme-ultraviolet and X-ray emission of the solar corona. Traditionally, significant dimmings of spectral lines formed at temperatures of 1–2 MK are regarded as indicators of coronal mass ejections (CMEs), reflecting the density depletion caused by plasma escaping into interplanetary space. In this Letter, we report a peculiar deep coronal dimming event predominantly observed in high-temperature spectral lines following an M8.8-class confined solar flare associated with a failed filament eruption. Sun-as-a-star measurements from the Geostationary Operational Environmental Satellite and the Extreme Ultraviolet Variability Experiment reveal intensity reductions exceeding 30% in soft X-ray (SXR) and measurable decreases in Fe xviii (6.5 MK) and Fe xx (9.3 MK). Spatially resolved observations from the Atmospheric Imaging Assembly demonstrate that the dimming originates from the active region core, while the Solar Terrestrial Relations Observatory-A shows no evidence for CME-driven mass loss. Differential emission measure analysis reveals plasma at temperatures >5 MK cooling into lower temperatures, supporting plasma cooling as the dominant contributor to the hot-band dimming rather than CME-associated plasma escape. This event demonstrates that deep hot SXR dimmings can occur without substantial CME-driven mass loss, suggesting that alternative physical mechanisms may also account for unresolved stellar dimmings in addition to the commonly inferred CME signatures.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"35 1","pages":"L16"},"PeriodicalIF":0.0,"publicationDate":"2026-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149089247","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}

引用次数: 0

Two Exciting High-redshift Galaxy Candidates Turn Out to Be Two Exciting Brown Dwarfs 两个令人兴奋的高红移星系候选者原来是两颗令人兴奋的褐矮星

The Astrophysical Journal Letters Pub Date : 2026-10-07 DOI: 10.3847/2041-8213/ae9085

Maruša Bradac,Chris Willott,Yoshihisa Asada,Loïc Albert,Gregor Rihtaršič,Anishya Harshan,Jon Judež,Nicholas S. Martis,Andrea Ferrara,Kevin Hainline,Abdurro’uf,Joseph F. V. Allingham,Volker Bromm,John Chisholm,Dan Coe,Guillaume Desprez,Jose M. Diego,Andreas L. Faisst,Seiji Fujimoto,Lukas J. Furtak,Tiger Yu-Yang Hsiao,Kohei Inayoshi,Anton M. Koekemoer,Vasily Kokorev,Brian C. Lemaux,Paulo A. A. Lopes,Ray A. Lucas,Danilo Marchesini,Vladan Markov,Gaël Noirot,Richard Pan,Scott W. Randall,Johan Richard,Luke Robbins,Ghassan T. E. Sarrouh,Marcin Sawicki,Tim Schrabback,Roberta Tripodi,Eros Vanzella,Rogier A. Windhorst

{"title":"Two Exciting High-redshift Galaxy Candidates Turn Out to Be Two Exciting Brown Dwarfs","authors":"Maruša Bradac,Chris Willott,Yoshihisa Asada,Loïc Albert,Gregor Rihtaršič,Anishya Harshan,Jon Judež,Nicholas S. Martis,Andrea Ferrara,Kevin Hainline,Abdurro’uf,Joseph F. V. Allingham,Volker Bromm,John Chisholm,Dan Coe,Guillaume Desprez,Jose M. Diego,Andreas L. Faisst,Seiji Fujimoto,Lukas J. Furtak,Tiger Yu-Yang Hsiao,Kohei Inayoshi,Anton M. Koekemoer,Vasily Kokorev,Brian C. Lemaux,Paulo A. A. Lopes,Ray A. Lucas,Danilo Marchesini,Vladan Markov,Gaël Noirot,Richard Pan,Scott W. Randall,Johan Richard,Luke Robbins,Ghassan T. E. Sarrouh,Marcin Sawicki,Tim Schrabback,Roberta Tripodi,Eros Vanzella,Rogier A. Windhorst","doi":"10.3847/2041-8213/ae9085","DOIUrl":"https://doi.org/10.3847/2041-8213/ae9085","url":null,"abstract":"Abstract From the onset of observations of JWST we have discovered unexpectedly luminous galaxies at redshifts z > 10 and as high as z = 14. With their discovery, the question immediately followed as to where their progenitors are, since such progenitors should be within reach of existing surveys. However, the discovery of several bright candidates at z > 15 may indicate further discrepancies between pre-JWST model predictions and current observations. Progenitors of the bright z ∼ 14 galaxies should be visible at redshifts as high as z ∼ 20–30, showing in the data as F277W and F356W dropouts. We identify two such candidates in the Bullet Cluster JWST data; however, subsequent NIRSpec follow-up data show spectra that can be well fit with Y dwarf templates with temperatures 272–351 K and and 445–525 K (using ATMO2020 and Sonora Elf Owl models) and distances of ∼150–650 pc. The first is one of the lowest-temperature brown dwarfs known, and the lowest-temperature brown dwarf detected spectroscopically outside the solar neighborhood. With additional NIRCam imaging taken ∼1 yr later, we also detect their proper motions of (49 ± 8) mas yr −1 and (24 ± 3) mas yr −1 , further indicating that at least some F277W and F356W dropouts are substellar cold Milky Way objects such as brown dwarfs.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"67 1","pages":"L13"},"PeriodicalIF":0.0,"publicationDate":"2026-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149089199","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}

引用次数: 0

Is Dark Matter Really Matter? 暗物质真的是物质吗？

The Astrophysical Journal Letters Pub Date : 2026-10-07 DOI: 10.3847/2041-8213/aeaa2a

Jun-Qian Jiang,Arman Shafieloo

{"title":"Is Dark Matter Really Matter?","authors":"Jun-Qian Jiang,Arman Shafieloo","doi":"10.3847/2041-8213/aeaa2a","DOIUrl":"https://doi.org/10.3847/2041-8213/aeaa2a","url":null,"abstract":"Abstract In the standard model of cosmology, it is assumed that dark matter is pressureless with equation of state w = 0 and dark energy has w = −1. We test these assumptions jointly using DESI DR2 distance measurements, including the recent Ly α Alcock–Paczynski (AP) information, Dark Energy Survey (DES) supernovae, and two complementary cosmic microwave background (CMB) treatments. When constant w DM and w DE are varied together, we find w DM = 0.00096 8 − 0.000496 + 0.000501 and w DE = − 0.938 0 − 0.0262 + 0.0259 (68%). With an alternative CMB treatment that marginalizes over the lensing spectrum, the corresponding constraints are w DM = 0.00087 0 − 0.000410 + 0.000408 and w DE = − 0.935 3 − 0.0254 + 0.0258 . Both standard ΛCDM values are disfavored at approximately 2 σ in the joint extension. Neither parameter departs significantly from its standard value when only that parameter is varied. This behavior arises because late-time distances favor w DE > −1, while maintaining the early-Universe physical matter density requires a compensating positive w DM , which changes the mapping to the matter density today. Allowing dynamical dark energy further highlights the complexity of the situation: phantom crossing for dark energy makes w DM = 0 consistent with the data, whereas a positive w DM preference persists when crossing is forbidden. Interestingly, the Padé- w parameterization that provides a flexible description of a class of quintessence models (with no phantom crossing), along with w DM free, is even mildly favored over the phantom-crossing w 0 w a model according to both the best-fit χ 2 and the deviance information criterion (DIC) under both CMB treatments. One can conclude that the apparent preference for phantom crossing may instead reflect deviations in the dark-matter sector rather than dark-energy dynamics alone. With future high-redshift distance measurements, particularly improved Ly α observations, together with growth and lensing probes, these possibilities may be further clarified.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"11 1","pages":"L12"},"PeriodicalIF":0.0,"publicationDate":"2026-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149089202","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}

引用次数: 0

Negative and Positive Cascade Rates of Slow Alfvénic Turbulence in Switchback and Nonswitchback Intervals: Wind Observations 在折返和非折返区间慢alfv<s:1>湍流负和正级联速率：风观测

The Astrophysical Journal Letters Pub Date : 2026-10-07 DOI: 10.3847/2041-8213/aea90c

Sofiane Bourouaine

{"title":"Negative and Positive Cascade Rates of Slow Alfvénic Turbulence in Switchback and Nonswitchback Intervals: Wind Observations","authors":"Sofiane Bourouaine","doi":"10.3847/2041-8213/aea90c","DOIUrl":"https://doi.org/10.3847/2041-8213/aea90c","url":null,"abstract":"Abstract We estimate the turbulent cascade rate in imbalanced Alfvénic turbulence in the slow solar wind using a Politano–Pouquet-based approach that does not require an isotropic assumption. We analyze selected 8 hr intervals provided by the Wind spacecraft. These intervals are characterized by near-homogeneity, weak velocity shear, and imbalanced Alfvénic fluctuations, and are classified as switchback or nonswitchback depending on the angular spread of the magnetic field relative to the mean field. Switchback intervals are identified by large magnetic-field rotations, whereas nonswitchback intervals exhibit only small angular deviations. Our results show that nonswitchback intervals exhibit a positive total cascade rate and power spectra consistent with a −3/2 scaling, indicative of a forward energy cascade. In contrast, switchback intervals are characterized by a negative total cascade rate, and by steeper power spectra with a spectral index of approximately −1.6. This indicates that large magnetic-field rotations can substantially modify the scale-to-scale energy transfer in Alfvénic slow solar wind. The results suggest that switchbacks may be associated with additional physical processes, such as local instabilities or reconnection-related structures, that alter the direction and magnitude of the turbulent cascade. These findings may help explain previous reports of negative cascade rates in imbalanced Alfvénic solar-wind turbulence.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"36 1","pages":"L1"},"PeriodicalIF":0.0,"publicationDate":"2026-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149089200","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}

引用次数: 0

Deep HST/STIS Coronagraphic Imaging of the β Pictoris Debris Disk: On the Scattered Light Component of the Cat’s Tail 绘形星β碎片盘的深HST/STIS日冕成像：关于猫尾的散射光成分

The Astrophysical Journal Letters Pub Date : 2026-10-07 DOI: 10.3847/2041-8213/aeac4a

Arin M. Avsar,Kevin Wagner,Dániel Apai,Isabel Rebollido,Antranik A. Sefilian,Marshall D. Perrin,Christopher C. Stark,Gabriel Weible,András Gáspár

{"title":"Deep HST/STIS Coronagraphic Imaging of the\u0000 β\u0000 Pictoris Debris Disk: On the Scattered Light Component of the Cat’s Tail","authors":"Arin M. Avsar,Kevin Wagner,Dániel Apai,Isabel Rebollido,Antranik A. Sefilian,Marshall D. Perrin,Christopher C. Stark,Gabriel Weible,András Gáspár","doi":"10.3847/2041-8213/aeac4a","DOIUrl":"https://doi.org/10.3847/2041-8213/aeac4a","url":null,"abstract":"Abstract The β Pictoris debris disk is a unique system where mid-infrared coronagraphic imaging with JWST/Mid-Infrared Imager (MIRI) revealed a new spatially resolved substructure known as the Cat’s Tail. We present deep Hubble Space Telescope (HST)/Space Telescope Imaging Spectrograph (STIS) coronagraphic imaging of β Pic in scattered light, combining six epochs of observations between 2012 and 2025, in search of the scattered light component of the Cat’s Tail. We detect the disk out to a projected separation of 500 au for the first time with HST/STIS, achieving a signal-to-noise ratio (SNR) > 100 across much of the midplane between 50 and 200 au. We report the detection of the visible/near-infrared scattered light component of the Cat’s Tail substructure. We find through injection-recovery analysis that the scattered light component of the Cat’s Tail has a total flux of 0.1%–0.4% of the MIRI F1550C flux. Using the measured STIS-to-MIRI flux ratio, we model the Cat’s Tail grain properties and find that the grains are highly porous and almost entirely composed of organic refractory material, which is in agreement with findings with JWST/MIRI. We use the organics content of solar system dwarf planets and dust in the local ISM as a proxy to estimate the size of the colliding progenitors that can produce enough organic refractory material seen in the Cat’s Tail. We find that each colliding progenitor must have a mass of at least 1–3 × 10 21 kg, comparable to Charon and Makemake in our Kuiper Belt. Additionally, we find a prominent warped morphology and surface brightness asymmetry in the outer dust halo of β Pic. We compare the observed halo morphology and asymmetry to predicted vertical structures, which may arise from planet–disk interactions.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"3 1","pages":"L10"},"PeriodicalIF":0.0,"publicationDate":"2026-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149089198","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}

引用次数: 0

First Light of Neutron Star Mergers: Off-axis Cocoon Cooling X-Ray Emission from Short Gamma-Ray Burst Jets 中子星合并的第一束光：短伽马射线爆发射流的离轴茧冷却x射线发射

The Astrophysical Journal Letters Pub Date : 2026-10-06 DOI: 10.3847/2041-8213/aeac25

Jian-He Zheng,Wenbin Lu

{"title":"First Light of Neutron Star Mergers: Off-axis Cocoon Cooling X-Ray Emission from Short Gamma-Ray Burst Jets","authors":"Jian-He Zheng,Wenbin Lu","doi":"10.3847/2041-8213/aeac25","DOIUrl":"https://doi.org/10.3847/2041-8213/aeac25","url":null,"abstract":"Abstract Neutron star mergers (NSMs) are confirmed gravitational wave sources. Identifying an early electromagnetic counterpart for these events is therefore crucial for rapid localization and multimessenger follow-up. However, the associated gamma-ray bursts (GRBs) are highly collimated and are therefore easily missed by off-axis observers. An early, less beamed counterpart is essential for identifying the majority of mergers. In this Letter, we investigate the cooling emission from jet-driven cocoons produced by short gamma-ray burst jets propagating through merger ejecta. We perform hydrodynamic simulations and radiative postprocessing to calculate the early X-ray emission over a wide range of viewing angles. We find that the mildly relativistic cocoon produces bright soft X-ray transients for off-axis observers, with luminosities of 10 46−48 erg s −1 and durations of a few to ten seconds. The X-ray spectra are quasi-thermal with characteristic temperatures of 0.1–1 keV. For observers at θ v = 10 ∘ , the cocoon emission is detectable by the Einstein Probe (EP) out to z ≃ 0.3. For nearby events like GW170817, it remains detectable up to θ v ≃ 45 ∘ . The predicted detection rate for EP is 0.5 yr −1 in the canonical model. In future multimessenger campaigns, rapid UV/optical/IR follow-up of such X-ray triggers can subsequently identify the associated kilonova and jet afterglow emission, which can confirm their origin.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"8 1","pages":"L7"},"PeriodicalIF":0.0,"publicationDate":"2026-10-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149089204","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}

引用次数: 0

An Open Cluster Origin for Most Solar-type Binaries in the Solar Neighborhood and Implications for Primordial Planet Stability 太阳附近大多数太阳型双星的疏散星团起源及其对原始行星稳定性的影响

The Astrophysical Journal Letters Pub Date : 2026-10-06 DOI: 10.3847/2041-8213/aeaae1

Anna C. Childs,Aaron M. Geller

{"title":"An Open Cluster Origin for Most Solar-type Binaries in the Solar Neighborhood and Implications for Primordial Planet Stability","authors":"Anna C. Childs,Aaron M. Geller","doi":"10.3847/2041-8213/aeaae1","DOIUrl":"https://doi.org/10.3847/2041-8213/aeaae1","url":null,"abstract":"Abstract We present the first Gaia-calibrated estimate of the contribution of dynamically processed open clusters (OCs) to the nearby solar-type field binary population and investigate the implications for primordial planet stability. We combine Gaia DR3 observations, empirical models of cluster formation and dissolution, and direct N -body simulations to constrain the fraction of field FGK-type binaries within 1 kpc that originated in OCs over the past 5 Gyr. We find that at least ∼53% of solar-type field binaries formed in OCs with initial masses ≥200 M ⊙ , where dynamical processing becomes significant. We quantify the effects of stellar encounters and binary orbital evolution on the stability of both circumbinary and circumstellar planets by deriving empirical prescriptions for circumbinary planet destabilization as a function of binary separation and for the fractional reduction of stable circumstellar coplanar phase space. These results provide a framework for evaluating how OC dynamical evolution may influence the stability of planets in binary systems and therefore contribute to observed exoplanet demographics.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"221 1","pages":"L5"},"PeriodicalIF":0.0,"publicationDate":"2026-10-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149089203","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}

引用次数: 0

Just a Phase? Weakening Vertical Shear Instability Explains Class II Disk Morphologies: Simulations with Dust Coagulation, Sedimentation, Thermal Relaxation, and Backreaction 只是一个阶段？减弱的垂直剪切不稳定性解释了II类圆盘形态：粉尘凝聚、沉降、热松弛和反反应的模拟

The Astrophysical Journal Letters Pub Date : 2026-10-06 DOI: 10.3847/2041-8213/aeab96

Thomas Pfeil,Alexandros Ziampras,Shangjia 尚嘉 Zhang 张,Philip J. Armitage,Yan-Fei 燕飞 Jiang 姜

{"title":"Just a Phase? Weakening Vertical Shear Instability Explains Class II Disk Morphologies: Simulations with Dust Coagulation, Sedimentation, Thermal Relaxation, and Backreaction","authors":"Thomas Pfeil,Alexandros Ziampras,Shangjia 尚嘉 Zhang 张,Philip J. Armitage,Yan-Fei 燕飞 Jiang 姜","doi":"10.3847/2041-8213/aeab96","DOIUrl":"https://doi.org/10.3847/2041-8213/aeab96","url":null,"abstract":"Abstract The vertical shear instability (VSI) is known to create turbulence and strong vertical mixing in protoplanetary disks if thermal relaxation is sufficiently fast. In simulations where this condition is met, VSI can loft dust particles to large altitudes, creating a vertically extended appearance in mock millimeter-wavelength observations, which is inconsistent with the morphology of the majority of observed Class II disks. We present simulations of protoplanetary disks with VSI that are consistent with the observed thin-disk geometries, while maintaining the commonly observed bowl-shaped morphology in scattered light images at micrometer wavelengths. We show that this outcome arises naturally when the effects of dust coagulation, sedimentation, and dust–gas thermal accommodation are taken into account. Sedimentation-driven coagulation removes large amounts of dust from the disk atmosphere, in the process slowing down the dust-driven cooling of the gas. At the same time, a dense midplane layer of millimeter-sized grains forms, which exerts aerodynamic drag on the gas. This results in the termination of the VSI’s corrugation mode. Only weak VSI activity remains in the upper and lower hemispheres. These processes occur on the typical dust growth timescale and suppress strong VSI-induced turbulence within a few hundred thousand years. VSI could thus generally be restricted to the Class I evolutionary stages of protoplanetary disks.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"14 1","pages":"L6"},"PeriodicalIF":0.0,"publicationDate":"2026-10-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149089235","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}

引用次数: 0