The Astrophysical Journal最新文献

Magnetogram-matching Biot–Savart Law and Decomposition of Vector Magnetograms 磁图匹配Biot-Savart定律与矢量磁图分解

The Astrophysical Journal Pub Date : 2025-07-15 DOI: 10.3847/1538-4357/add895

Viacheslav S. Titov, Cooper Downs, Tibor Török, Jon A. Linker, Michael Prazak and Jiong A. Qiu

{"title":"Magnetogram-matching Biot–Savart Law and Decomposition of Vector Magnetograms","authors":"Viacheslav S. Titov, Cooper Downs, Tibor Török, Jon A. Linker, Michael Prazak and Jiong A. Qiu","doi":"10.3847/1538-4357/add895","DOIUrl":"https://doi.org/10.3847/1538-4357/add895","url":null,"abstract":"We generalize a magnetogram-matching Biot–Savart law (BSl) from planar to spherical geometry. For a given coronal current density J, this law determines the magnetic field whose radial component vanishes at the surface. The superposition of with a potential field defined by a given surface radial field, Br, provides the entire configuration where Br remains unchanged by the currents. Using this approach, we (1) upgrade our regularized BSls for constructing coronal magnetic flux ropes (MFRs) and (2) propose a new method for decomposing a measured photospheric magnetic field as , where the potential, Bpot, toroidal, BT, and poloidal, , fields are determined by Br, Jr, and the surface divergence of B–Bpot, respectively, all derived from magnetic data. Our BT is identical to the one in the alternative Gaussian decomposition by P. W. Schuck et al., while Bpot and are different from their poloidal fields and , which are potential in the infinitesimal proximity to the upper and lower side of the surface, respectively. In contrast, our has no such constraints and, as Bpot and BT, refers to the same upper side of the surface. In spite of these differences, for a continuous J distribution across the surface, Bpot and are linear combinations of and . We demonstrate that, similar to the Gaussian method, our decomposition allows one to identify the footprints and projected surface-location of MFRs in the solar corona, as well as the direction and connectivity of their currents.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"95 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144640001","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 ALMA Study of Molecular Complexity in the Hot Core G336.99-00.03 MM1 热岩心G336.99-00.03 MM1分子复杂性的ALMA研究

The Astrophysical Journal Pub Date : 2025-07-15 DOI: 10.3847/1538-4357/addbd6

Chunguo Duan, Qian Gou, Tie Liu, Fengwei Xu, Xuefang Xu, Junlin Lan, Ke Wang, Laurent Pagani, Donghui Quan, Junzhi Wang, Xunchuan Liu and Mingwei He

{"title":"An ALMA Study of Molecular Complexity in the Hot Core G336.99-00.03 MM1","authors":"Chunguo Duan, Qian Gou, Tie Liu, Fengwei Xu, Xuefang Xu, Junlin Lan, Ke Wang, Laurent Pagani, Donghui Quan, Junzhi Wang, Xunchuan Liu and Mingwei He","doi":"10.3847/1538-4357/addbd6","DOIUrl":"https://doi.org/10.3847/1538-4357/addbd6","url":null,"abstract":"High-mass star formation involves complex processes, with the hot core phase playing a crucial role in chemical enrichment and the formation of complex organic molecules. However, molecular inventories in hot cores remain limited. Using data from the Atacama Large Millimeter/submillimeter Array Three-millimeter Observations of Massive Star-forming regions survey, the molecular composition and evolutionary stages of two distinct millimeter continuum sources in the high-mass star-forming region G336.99-00.03 have been characterized. MM1, with 19 distinct molecular species detected, along with eight isotopologues and several vibrationally/torsionally excited states, has been identified as a hot core. MM2, with only five species identified, was defined as a H ii region. Isotopic ratios in MM1 were derived, with 12C/13C ranging from 16.0 to 29.2, 16O/18O at 47.7, and 32S/34S at 19.2. Molecular abundances in MM1 show strong agreement with other sources and three-phase warm-up chemical models within an order of magnitude for most species. Formation pathways of key molecules were explored, revealing chemical links and reaction networks. This study provides a detailed molecular inventory of two millimeter continuum sources, shedding light on the chemical diversity and evolutionary processes in high-mass star-forming regions. The derived molecular parameters and isotopic ratios offer benchmarks for astrochemical models, paving the way for further investigation into the formation and evolution of complex organic molecules during the hot core phase.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"10 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144640002","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

Searching for Axion Dark Matter Gegenschein of the Vela Supernova Remnant with FAST 用FAST寻找船帆座超新星遗迹的轴子暗物质成因机制

The Astrophysical Journal Pub Date : 2025-07-15 DOI: 10.3847/1538-4357/adde48

Wenxiu Yang, Yitian Sun, Yougang Wang, Katelin Schutz, Yichao Li, Calvin Leung, Wenkai Hu, Shuanghao Shu, Kiyoshi Masui and Xuelei Chen

{"title":"Searching for Axion Dark Matter Gegenschein of the Vela Supernova Remnant with FAST","authors":"Wenxiu Yang, Yitian Sun, Yougang Wang, Katelin Schutz, Yichao Li, Calvin Leung, Wenkai Hu, Shuanghao Shu, Kiyoshi Masui and Xuelei Chen","doi":"10.3847/1538-4357/adde48","DOIUrl":"https://doi.org/10.3847/1538-4357/adde48","url":null,"abstract":"Axions are one of the leading dark matter candidates. If we are embedded in a Milky Way dark matter halo comprised of axions, their stimulated decay would enable us to observe a counterimage (“axion gegenschein”) with a frequency equal to half the axion mass in the opposite direction of a bright radio source. This spectral line emission will be broadened to Δν/ν ∼ σd/c ∼ 10−3 due to the velocity dispersion of dark matter, σd. In this pilot study, we perform the first search for the expected axion gegenschein image of Vela supernova remnant with 26.4 hr of effective ON–OFF data from the Five-hundred-meter Aperture Spherical radio Telescope (FAST) L-band (1.0–1.5 GHz) 19 beam receiver. Our null detection limits the axion–photon coupling strength to be gaγγ ≲ 2 × 10−10 GeV−1 in the mass ranges of 8.7 μeV ≤ ma ≤ 9.44 μeV and 10.85 μeV ≤ ma ≤ 12.01 μeV. These results provide a stronger constraint on gaγγ in this axion mass range than the current limits obtained by the direct search of an axion decay signal from a dwarf galaxy that uses FAST observations, but are a factor of ∼3 times weaker than the current CERN Axion Solar Telescope limit. Based on our observation strategy, data processing methods, and results, the expected sensitivity will reach ∼10−11 GeV−1 with ∼2000 hr of observation in the future.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"84 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144640004","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

Magnetic Fields in the Pillars of Creation 创造之柱中的磁场

The Astrophysical Journal Pub Date : 2025-07-15 DOI: 10.3847/1538-4357/ade544

Adwitiya Sarkar, Leslie W. Looney, Marc W. Pound, Zhi-Yun Li, Ian W. Stephens, Manuel Fernández-López, Simon Coudé, Zhe-Yu Daniel Lin, Haifeng Yang and Reid Faistl

{"title":"Magnetic Fields in the Pillars of Creation","authors":"Adwitiya Sarkar, Leslie W. Looney, Marc W. Pound, Zhi-Yun Li, Ian W. Stephens, Manuel Fernández-López, Simon Coudé, Zhe-Yu Daniel Lin, Haifeng Yang and Reid Faistl","doi":"10.3847/1538-4357/ade544","DOIUrl":"https://doi.org/10.3847/1538-4357/ade544","url":null,"abstract":"Due to dust grain alignment with magnetic fields, dust polarization observations of far-infrared emission from cold molecular clouds are often used to trace magnetic fields, allowing a probe of the effects of magnetic fields on the star formation process. We present inferred magnetic field maps of the Pillars of Creation region within the larger M16 emission nebula, derived from dust polarization data in the 89 and 154 μm continuum using the Stratospheric Observatory For Infrared Astronomy/High-resolution Airborne Wideband Camera. We derive magnetic field strength estimates using the Davis–Chandrasekhar–Fermi method. We compare the polarization and magnetic field strengths to column densities and dust continuum intensities across the region to build a coherent picture of the relationship between star-forming activity and magnetic fields in the region. The projected magnetic field strengths derived are in the range of ∼50–130 μG, which is typical for clouds of similar n(H2), i.e., molecular hydrogen volume density on the order of 104–105 cm−3. We conclude that star formation occurs in the finger tips when the magnetic fields are too weak to prevent radial collapse due to gravity but strong enough to oppose OB stellar radiation pressure, while in the base of the fingers the magnetic fields hinder mass accretion and consequently star formation. We also support an initial weak-field model (<50 μG) with subsequent strengthening through realignment and compression, resulting in a dynamically important magnetic field.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"40 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144640072","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

Leaky Dust Traps in Planet-embedded Protoplanetary Disks 嵌入行星的原行星盘中的漏尘陷阱

The Astrophysical Journal Pub Date : 2025-07-15 DOI: 10.3847/1538-4357/addd1f

Pinghui Huang, Fangyuan Yu, Eve J. Lee, Ruobing Dong and Xue-Ning Bai

{"title":"Leaky Dust Traps in Planet-embedded Protoplanetary Disks","authors":"Pinghui Huang, Fangyuan Yu, Eve J. Lee, Ruobing Dong and Xue-Ning Bai","doi":"10.3847/1538-4357/addd1f","DOIUrl":"https://doi.org/10.3847/1538-4357/addd1f","url":null,"abstract":"From the survival of dust disks for a few Myr to the establishment of chemical dichotomy, dust traps are expected to play a pivotal role in sculpting protoplanetary disks and the early planet formation process. These traps may not be perfect, as evidenced by both numerical simulations and the observations of disks with gaps and cavities, inside which we detect some amounts of both gas and dust. Using two-fluid hydrodynamic global simulations in both 2D and 3D, we directly compute the dynamics of dust grains as they aerodynamically interact with the disk gas that is being perturbed by an embedded planet. In both 2D and 3D, we find the dust trap to be more leaky for a lower-mass planet and for a more turbulent disk. More crucially, we find that the fraction of dust mass that remains trapped within the pressure bump can be up to an order of magnitude more reduced in 3D compared to 2D, with all else being equal. Our simulations show a complex behavior of dust radial motion that is both azimuthally and poloidally nonuniform, with the overall dynamics dominated by the dust coupling to the gas flow even for Stokes number 0.1. The leaky traps we find suggest that the pebble isolation mass is likely not truly isolating and that gap-opening planets do not establish an unconditional impermeable barrier. Our findings have implications for recent JWST MINDS results, which show that volatiles, including water, are present in the inner regions of disks hosting outer dust rings.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"54 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144640003","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

Steady-state Heating of Diffuse Coronal Plasma in a Solar Active Region 太阳活动区漫射日冕等离子体的稳态加热

The Astrophysical Journal Pub Date : 2025-07-15 DOI: 10.3847/1538-4357/ade3dd

Gregory D. Fleishman, Alexey A. Kuznetsov and Gelu M. Nita

引用次数: 0

The Impact of Applying Black Hole–Host Galaxy Scaling Relations to Large Galaxy Populations 将黑洞-宿主星系尺度关系应用于大星系群的影响

The Astrophysical Journal Pub Date : 2025-07-15 DOI: 10.3847/1538-4357/ade30a

Maggie C. Huber, Joseph Simon and Julia M. Comerford

{"title":"The Impact of Applying Black Hole–Host Galaxy Scaling Relations to Large Galaxy Populations","authors":"Maggie C. Huber, Joseph Simon and Julia M. Comerford","doi":"10.3847/1538-4357/ade30a","DOIUrl":"https://doi.org/10.3847/1538-4357/ade30a","url":null,"abstract":"Supermassive black holes (SMBHs) with dynamically measured masses have shown empirical correlations with host galaxy properties. These correlations are often the only method available to estimate SMBH masses and gather statistics for large galaxy populations across a range of redshifts, even though the scaling relations themselves are derived from a small subset of nearby galaxies. Depending on the scaling relation used, estimated SMBH masses can vary significantly. The most widely used scaling relations are the MBH–Mbulge and MBH–σ relations, where Mbulge is galaxy bulge mass and σ is the bulge velocity dispersion. In this paper, we determine how severely the choice of scaling relation impacts SMBH mass estimates for different subsets of a large galaxy population. For this analysis, we use a sample of ∼400,000 galaxies, including 1240 Type 1 active galactic nuclei from the Sloan Digital Sky Survey. We calculate SMBH masses from MBH–Mbulge and MBH–σ and compare to single-epoch virial SMBH masses from broad-line Hβ, which are derived independently of black hole–host galaxy scaling relations. We find that SMBH masses derived from the single-epoch virial relation for Hβ are better reproduced by MBH–σ than MBH–Mbulge. Finally, in cases where σ and Mbulge cannot be measured directly, we show that it is possible to infer σ from photometry with more accuracy than we can infer Mbulge.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"20 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144640007","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

Rapid Change in the Orbital Period of the Remnant of Nova Scorpii AD 1437 (IGR J17014-4306) 天蝎座新星AD 1437遗迹（IGR J17014-4306）轨道周期的快速变化

The Astrophysical Journal Pub Date : 2025-07-15 DOI: 10.3847/1538-4357/ade788

Lei Zang, Shengbang Qian, Li Zhang, Qibin Sun, Linfeng Chang, Berto Monard, Gordon Myers and Franz-Josef Hambsch

{"title":"Rapid Change in the Orbital Period of the Remnant of Nova Scorpii AD 1437 (IGR J17014-4306)","authors":"Lei Zang, Shengbang Qian, Li Zhang, Qibin Sun, Linfeng Chang, Berto Monard, Gordon Myers and Franz-Josef Hambsch","doi":"10.3847/1538-4357/ade788","DOIUrl":"https://doi.org/10.3847/1538-4357/ade788","url":null,"abstract":"IGR J17014-4306 is the longest orbital period (12.8 hr) deep-eclipsing intermediate polar known, where a massive white dwarf (WD) accretes matter from its companion star via an accretion disk. Based on photometric observations from the Transiting Exoplanet Survey Satellite space telescope and the American Association of Variable Star Observers database, 70 eclipse timings were determined. It was also confirmed that the spin pulse profile of the WD does change, which is due to the amplitude variation with opposite trends in spin frequency and its first harmonic. This may be related to fluctuations in the accretion rate. The spin period shows slight fluctuations but no significant changing trends. We constructed the O–C diagram and discovered that the orbital period is increasing at a high rate of , which is comparable to those detected in compact binary supersoft X-ray sources and recurrent novae. This continuous increase in the orbital period is caused by the mass transfer from the less-massive companion to the WD on its thermal timescale at a high rate. All these findings suggest that IGR J17014-4306 is an interesting target to investigate nova eruption, the real angular momentum loss mechanism, and the overall evolution of cataclysmic variables.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"94 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144640074","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

On Convective Turnover Times and Dynamos in Low-mass Stars 关于低质量恒星的对流周转时间和发电机

The Astrophysical Journal Pub Date : 2025-07-15 DOI: 10.3847/1538-4357/adde4d

Seth Gossage, Rocio Kiman, Kristina Monsch, Amber A. Medina, Jeremy J. Drake, Cecilia Garraffo, Yuxi(Lucy) Lu, Joshua D. Wing and Nicholas J. Wright

{"title":"On Convective Turnover Times and Dynamos in Low-mass Stars","authors":"Seth Gossage, Rocio Kiman, Kristina Monsch, Amber A. Medina, Jeremy J. Drake, Cecilia Garraffo, Yuxi(Lucy) Lu, Joshua D. Wing and Nicholas J. Wright","doi":"10.3847/1538-4357/adde4d","DOIUrl":"https://doi.org/10.3847/1538-4357/adde4d","url":null,"abstract":"The relationship between magnetic activity and Rossby number is one way through which stellar dynamos can be understood. Using measured rotation rates and X-ray to bolometric luminosity ratios of an ensemble of stars, we derive empirical convective turnover times based on recent observations and reevaluate the X-ray activity–Rossby number relationship. In doing so, we find a sharp rise in the convective turnover time for stars in the mass range of 0.35−0.4 M⊙, associated with the onset of a fully convective internal stellar structure. Using MESA stellar evolution models, we infer the location of dynamo action implied by the empirical convective turnover time. The empirical convective turnover time is found to be indicative of dynamo action deep within the convective envelope in stars with masses 0.1–1.2 M⊙, crossing the fully convective boundary. Our results corroborate past works suggesting that partially and fully convective stars follow the same activity–Rossby relation, possibly owing to similar dynamo mechanisms. Our stellar models also give insight into the dynamo mechanism. We find that empirically determined convective turnover times correlate with properties of the deep stellar interior. These findings are in agreement with global dynamo models that see a reservoir of magnetic flux accumulates deep in the convection zone before buoyantly rising to the surface.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"29 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144640005","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

A Possible Common Physics Picture Reflected by the Gamma-Ray Emission of the Galactic Center 银河系中心伽玛射线发射所反映的可能的共同物理图像

The Astrophysical Journal Pub Date : 2025-07-15 DOI: 10.3847/1538-4357/ade3ce

Lin Nie, Yi-Qing Guo and Si-Ming Liu

{"title":"A Possible Common Physics Picture Reflected by the Gamma-Ray Emission of the Galactic Center","authors":"Lin Nie, Yi-Qing Guo and Si-Ming Liu","doi":"10.3847/1538-4357/ade3ce","DOIUrl":"https://doi.org/10.3847/1538-4357/ade3ce","url":null,"abstract":"Long-term observations of the Galactic center by Fermi and HESS have revealed a novel phenomenon: the high-energy gamma-ray spectrum from the gamma-ray source HESS J1745-290 exhibits a double power-law structure. In this study, we propose a new explanation for this phenomenon. We suggest that the low-energy (GeV) power-law spectrum originates from interactions between trapped background “sea” cosmic ray particles and the dense gaseous environment near the Galactic center. In contrast, the bubble-like structure in the high-energy (TeV) spectrum is produced by protons accelerated during active phases of the Galactic center, through the same physical process. Based on this framework, we first calculate the gamma-ray emission generated by cosmic ray protons accelerated in the Galactic center. Then, using a spatially dependent cosmic ray propagation model, we compute the energy spectrum of background “sea” cosmic ray protons and their associated diffuse gamma-ray emission in the Galactic center region. The results closely reproduce the observations from Fermi-LAT and HESS, suggesting that their long-term data support this picture: high-energy cosmic rays in the local region originate from nearby cosmic ray sources, while low-energy cosmic rays are a unified contribution from distant cosmic ray sources. We anticipate that this double power-law structure may be widely present in the halo of a Galactic cosmic-ray source or a slow-diffusion region. We hope that future observations will detect more such sources, allowing us to further test and validate our model.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"669 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144640065","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