Research in Astronomy and Astrophysics最新文献_第4页

Are Solar Active Regions Born with Neutralized Currents? 太阳活动区是否诞生于中和电流？

IF 1.8 4区物理与天体物理

Research in Astronomy and Astrophysics Pub Date : 2024-06-30 DOI: 10.1088/1674-4527/ad50b6

Aiying Duan, Yaoyu Xing and Chaowei Jiang

{"title":"Are Solar Active Regions Born with Neutralized Currents?","authors":"Aiying Duan, Yaoyu Xing and Chaowei Jiang","doi":"10.1088/1674-4527/ad50b6","DOIUrl":"https://doi.org/10.1088/1674-4527/ad50b6","url":null,"abstract":"Solar active regions (ARs) are formed by the emergence of current-carrying magnetic flux tubes from below the photosphere. Although for an isolated flux tube the direct and return currents flowing along the tube should balance with each other, it remains controversial whether such a neutralization of currents is also maintained during the emergence process. Here we present a systematic survey of the degrees of the current neutralization in a large sample of flux-emerging ARs which appeared on the solar disk around the central meridian from 2010 to 2022. The vector magnetograms taken by Helioseismic and Magnetic Imager onboard Solar Dynamic Observatory are employed to calculate the distributions of the vertical current density at the photosphere. Focusing on the main phase of flux emergence, i.e., the phase in which the total unsigned magnetic flux is continuously increased, we statistically examined the ratios of direct to return currents in all the ARs. Such a large-sample statistical study suggests that most of the ARs were born with currents close to neutralization. The degree of current neutralization seems to be not affected by the active-region size, the active-region growing rate, and the total unsigned current. The only correlation of significance as found is that the stronger the magnetic field nonpotentiality is, the further the AR deviates from current neutrality, which supports previous event studies that eruption-productive ARs often have non-neutralized currents.","PeriodicalId":54494,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"14 1","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-06-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141518208","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0

Supernova 1987A’s Keyhole: A Long-lived Jet-pair in the Final Explosion Phase of Core-collapse Supernovae 超新星1987A的钥匙孔：核心坍缩超新星最后爆发阶段的长寿命喷流对

IF 1.8 4区物理与天体物理

Research in Astronomy and Astrophysics Pub Date : 2024-06-26 DOI: 10.1088/1674-4527/ad4fc2

Noam Soker

{"title":"Supernova 1987A’s Keyhole: A Long-lived Jet-pair in the Final Explosion Phase of Core-collapse Supernovae","authors":"Noam Soker","doi":"10.1088/1674-4527/ad4fc2","DOIUrl":"https://doi.org/10.1088/1674-4527/ad4fc2","url":null,"abstract":"I further study the manner by which a pair of opposite jets shape the “keyhole” morphological structure of the core-collapse supernova (CCSN) SN 1997A, now the CCSN remnant (CCSNR) 1987A. By doing so, I strengthen the claim that the jittering-jet explosion mechanism accounts for most, likely all, CCSNe. The “keyhole” structure comprises a northern low-intensity zone closed with a bright rim on its front and an elongated low-intensity nozzle in the south. This rim-nozzle asymmetry is observed in some cooling flow clusters and planetary nebulae that are observed to be shaped by jets. I build a toy model that uses the planar jittering jets pattern, where consecutive pairs of jets tend to jitter in a common plane, implying that the accreted gas onto the newly born neutron star at the late explosion phase flows perpendicular to that plane. This allows for a long-lived jet-launching episode. This long-lasting jet-launching episode launches more mass into the jets that can inflate larger pairs of ears or bubbles, forming the main jets’ axis of the CCSNR that is not necessarily related to a possible pre-collapse core rotation. I discuss the relation of the main jets’ axis to the neutron star’s natal kick velocity.","PeriodicalId":54494,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"34 1","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-06-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141509081","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0

The First Ground-based White Light Lunar Polarization Imaging: A New Kind of FeO Observation on the Near Side of the Moon 首次地基白光月球偏振成像：月球近侧的新型氧化铁观测

IF 1.8 4区物理与天体物理

Research in Astronomy and Astrophysics Pub Date : 2024-06-23 DOI: 10.1088/1674-4527/ad44f1

Wei-Nan Wang, Jin-Song Ping, Ming-Yuan Wang, Wen-Zhao Zhang, Han-Lin Ye, Xing-Wei Han and Song-Feng Kou

引用次数: 0

Can near-to-mid Infrared Spectral Energy Distribution Quantitatively Trace Protoplanetary Disk Evolution? 近中红外光谱能量分布能否定量追踪原行星盘的演化？

IF 1.8 4区物理与天体物理

Research in Astronomy and Astrophysics Pub Date : 2024-06-23 DOI: 10.1088/1674-4527/ad4b5c

Mingchao Liu, 明超刘, Jinhua He, 金华何, Zhen Guo, Jixing Ge, 继兴葛, Yuping Tang and 雨平唐

{"title":"Can near-to-mid Infrared Spectral Energy Distribution Quantitatively Trace Protoplanetary Disk Evolution?","authors":"Mingchao Liu, 明超刘, Jinhua He, 金华何, Zhen Guo, Jixing Ge, 继兴葛, Yuping Tang and 雨平唐","doi":"10.1088/1674-4527/ad4b5c","DOIUrl":"https://doi.org/10.1088/1674-4527/ad4b5c","url":null,"abstract":"Infrared (IR) spectral energy distribution (SED) is the major tracer of protoplanetary disks. It was recently proposed to use the near-to-mid IR (or K-24) SED slope α defined between 2 and 24μm as a potential quantitative tracer of disk age. We critically examine the viability of this idea and confront it with additional statistics of IR luminosities and SED shapes. We point out that, because the statistical properties of most of the complicated physical factors involved in disk evolution are still poorly understood in a quantitative sense, the only viable way is to assume them to be random so that an idealized “average disk” can be defined, which allows the α histogram to trace its age. We confirm that the statistics of the zeroth order (luminosity), first order (slope α), and second order characteristics (concavity) of the observed K-24 SEDs indeed carry useful information upon the evolutionary processes of the “average disk”. We also stress that intrinsic diversities in K-24 SED shapes and luminosities are always large at the level of individual stars so that the application of the evolutionary path of the “average disk” to individual stars must be done with care. The data of most curves in plots are provided on GitHub (Disk-age package https://github.com/starage/disk-age/).","PeriodicalId":54494,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"146 1","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-06-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141529813","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0

Toward a Direct Measurement of the Cosmic Acceleration: The Pilot Observation of HI 21 cm Absorption Line at FAST 实现对宇宙加速度的直接测量：在 FAST 上对 HI 21 厘米吸收线的试验性观测

IF 1.8 4区物理与天体物理

Research in Astronomy and Astrophysics Pub Date : 2024-06-18 DOI: 10.1088/1674-4527/ad48d1

Jiangang Kang, Chang-Zhi Lu, Tong-Jie Zhang and Ming Zhu

{"title":"Toward a Direct Measurement of the Cosmic Acceleration: The Pilot Observation of HI 21 cm Absorption Line at FAST","authors":"Jiangang Kang, Chang-Zhi Lu, Tong-Jie Zhang and Ming Zhu","doi":"10.1088/1674-4527/ad48d1","DOIUrl":"https://doi.org/10.1088/1674-4527/ad48d1","url":null,"abstract":"This study presents results on detecting neutral atomic hydrogen (H i) 21 cm absorption in the spectrum of PKS PKS1413+13 at redshift z = 0.24670041. The observation was conducted by FAST, with a spectral resolution of 10 Hz, using 10 minutes of observing time. The global spectral profile is examined by modeling the absorption line using a single Gaussian function with a resolution of 10 kHz within a 2 MHz bandwidth. The goal is to determine the rate of the latest cosmic acceleration by directly measuring the redshift evolution of the H i 21 cm absorption line with Hubble flow toward a common background quasar over a decade or longer time span. This will serve as a detectable signal generated by the accelerated expansion of the Universe at redshift z < 1, referred to as redshift drift or the SL effect. The measured H i gas column density in this DLA system is approximately equivalent to the initial observation value, considering uncertainties of the spin temperature of a spiral host galaxy. The high signal-to-noise ratio of 57, obtained at a 10 kHz resolution, strongly supports the feasibility of using the H i 21 cm absorption line in DLA systems to accurately measure the redshift drift rate at a precision level of around 10−10 per decade.","PeriodicalId":54494,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"223 1","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-06-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141518209","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0

Feedback of Efficient Shock Acceleration on Magnetic-field Structure Inside Young Type Ia Supernova Remnants 高效冲击加速对年轻 Ia 型超新星残留物内部磁场结构的反馈作用

IF 1.8 4区物理与天体物理

Research in Astronomy and Astrophysics Pub Date : 2024-06-07 DOI: 10.1088/1674-4527/ad4598

Jun-Yu Shen, Bi-Wen Bao, Li Zhang

{"title":"Feedback of Efficient Shock Acceleration on Magnetic-field Structure Inside Young Type Ia Supernova Remnants","authors":"Jun-Yu Shen, Bi-Wen Bao, Li Zhang","doi":"10.1088/1674-4527/ad4598","DOIUrl":"https://doi.org/10.1088/1674-4527/ad4598","url":null,"abstract":"Using an effective adiabatic index <italic toggle=\"yes\">γ</italic>\u0000eff to mimic the feedback of efficient shock acceleration, we simulate the temporal evolution of a young type Ia supernova remnant (SNR) with two different background magnetic field (BMF) topologies: a uniform and a turbulent BMF. The density distribution and magnetic-field characteristics of our benchmark SNR are studied with two-dimensional cylindrical magnetohydrodynamic simulations. When <italic toggle=\"yes\">γ</italic>\u0000eff is considered, we find that: (1) the two-shock structure shrinks and the downstream magnetic-field orientation is dominated by the Rayleigh–Taylor instability structures; (2) there exists more quasi-radial magnetic fields inside the shocked region; and (3) inside the intershock region, both the quasi-radial magnetic energy density and the total magnetic energy density are enhanced: in the radial direction, with <italic toggle=\"yes\">γ</italic>\u0000eff = 1.1, they are amplified about 10–26 times more than those with <italic toggle=\"yes\">γ</italic>\u0000eff = 5/3. While in the angular direction, the total magnetic energy densities could be amplified about 350 times more than those with <italic toggle=\"yes\">γ</italic>\u0000eff = 5/3, and there are more grid cells within the intershock region where the magnetic energy density is amplified by a factor greater than 100.","PeriodicalId":54494,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"32 1","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-06-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141518210","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0

Analysis of the Impact of the Blazhko Effect Both on the Van Hoof Effect and Radial Velocity Amplitude in the Star RR Lyr 分析布拉兹科效应对RR Lyr星的范霍夫效应和径向速度振幅的影响

IF 1.8 4区物理与天体物理

Research in Astronomy and Astrophysics Pub Date : 2024-06-03 DOI: 10.1088/1674-4527/ad44f0

Y. El jariri, F.L. Sefyani, A. Benhida, Z. Benkhaldoun, K. Kolenberg, K. Chafouai, A. Habib and M. Sabil

{"title":"Analysis of the Impact of the Blazhko Effect Both on the Van Hoof Effect and Radial Velocity Amplitude in the Star RR Lyr","authors":"Y. El jariri, F.L. Sefyani, A. Benhida, Z. Benkhaldoun, K. Kolenberg, K. Chafouai, A. Habib and M. Sabil","doi":"10.1088/1674-4527/ad44f0","DOIUrl":"https://doi.org/10.1088/1674-4527/ad44f0","url":null,"abstract":"The Van Hoof effect is a phase shift existing between the radial velocity curves of hydrogen and metallic lines within the atmosphere of pulsating stars. In this article, we present a study of this phenomenon through the spectra of the brightest pulsating star RR Lyr of RR Lyrae stars recorded for 22 yr. We based ourselves, on the one hand, on 1268 spectra (41 nights of observation) recorded between the years 1994 and 1997 at the Observatory of Haute Provence (OHP, France) previously observed by Chadid and Gillet, and on the other hand on 1569 spectra (46 nights of observation) recorded at our Oukaimeden Observatory (Morocco) between 2015 and 2016. Through this study, we have detected information on atmospheric dynamics that had not previously been detected. Indeed, the Van Hoof effect which results in a clear correlation between the radial velocities of hydrogen and those of the metallic lines has been observed and analyzed at different Blazhko phases. A correlation between the radial velocities of different metallic lines located in the lower atmosphere has been observed as well. For the first time, we were able to show that the amplitude of the radial velocity curves deduced from the lines of hydrogen and that of Fe ii (λ4923.921 Å) increases toward the minimum of the Blazhko cycle and decreases toward the maximum of the same Blazhko cycle. Furthermore, we found that the Van Hoof effect is also modulated by the Blazhko effect. Thus, toward the minimum of the Blazhko cycle the Van Hoof effect is more visible and at the maximum of the Blazhko cycle, this effect is minimal. We also observed the temporal evolution of the amplitudes of the radial velocities of the lower and upper atmosphere. When observed over a long time, we can interpret it as a function of the Blazhko phases.","PeriodicalId":54494,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"24 1","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-06-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141255752","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0

Temporal and Spectral Characteristics of Persistent Emission and Special Bursts of Magnetar SGR J1935+2154 Based on Insight-HXMT 基于 Insight-HXMT 的磁星 SGR J1935+2154 持续发射和特殊爆发的时间和光谱特征

IF 1.8 4区物理与天体物理

Research in Astronomy and Astrophysics Pub Date : 2024-05-28 DOI: 10.1088/1674-4527/ad4599

Xue-Feng Lu, Li-Ming Song, Ming-Yu Ge, Shuang-Nan Zhang, Jin-Lu Qu, Ce Cai, Cong-Zhan Liu, Cheng-Kui Li, Yu-Cong Fu and Ying-Chen Xu

{"title":"Temporal and Spectral Characteristics of Persistent Emission and Special Bursts of Magnetar SGR J1935+2154 Based on Insight-HXMT","authors":"Xue-Feng Lu, Li-Ming Song, Ming-Yu Ge, Shuang-Nan Zhang, Jin-Lu Qu, Ce Cai, Cong-Zhan Liu, Cheng-Kui Li, Yu-Cong Fu and Ying-Chen Xu","doi":"10.1088/1674-4527/ad4599","DOIUrl":"https://doi.org/10.1088/1674-4527/ad4599","url":null,"abstract":"In October 2022, the magnetar SGR J1935+2154 entered the active outburst state. During the episode, the Insight-HXMT satellite carried out a long observation that lasted for 20 days. More than 300 bursts were detected, and a certain amount of persistent radiation signals were also accumulated. This paper mainly introduces the results of persistent radiation profile folding and period search based on Insight-HXMT data. At the same time, the burst phase distribution characteristics, spectral lag results of burst, the spectral characteristics of zero-lag bursts and the time-resolved spectral evolution characteristics of high-flux bursts are reported. We found that there is no significant delay feature during different energy bands for the bursts of SGR J1935+2154. The observed zero-lag burst does not have a unique spectrum. The time-resolved spectrum of the individual burst has consistent spectral types and spectral parameters at different time periods of the burst. We also find that the burst number phase distribution and the burst photon phase distribution have the same tendency to concentrate in specific regions of the persistent emission profile.","PeriodicalId":54494,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"6 1","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-05-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141190192","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0

What is the Role of Gravity, Turbulence and Magnetic Fields in High-mass Star Formation Clouds? 重力、湍流和磁场在大质量恒星形成云中的作用是什么？

IF 1.8 4区物理与天体物理

Research in Astronomy and Astrophysics Pub Date : 2024-05-19 DOI: 10.1088/1674-4527/ad3ec8

An-Xu Luo, Hong-Li Liu, Guang-Xing Li, Sirong Pan and Dong-Ting Yang

{"title":"What is the Role of Gravity, Turbulence and Magnetic Fields in High-mass Star Formation Clouds?","authors":"An-Xu Luo, Hong-Li Liu, Guang-Xing Li, Sirong Pan and Dong-Ting Yang","doi":"10.1088/1674-4527/ad3ec8","DOIUrl":"https://doi.org/10.1088/1674-4527/ad3ec8","url":null,"abstract":"To explore the potential role of gravity, turbulence and magnetic fields in high-mass star formation in molecular clouds, this study revisits the velocity dispersion–size (σ–L) and density–size (ρ–L) scalings and the associated turbulent energy spectrum using an extensive data sample. The sample includes various hierarchical density structures in high-mass star formation clouds, across scales of 0.01–100 pc. We observe σ ∝ L0.26 and ρ ∝ L−1.54 scalings, converging toward a virial equilibrium state. A nearly flat virial parameter–mass (αvir−M) distribution is seen across all density scales, with αvir values centered around unity, suggesting a global equilibrium maintained by the interplay between gravity and turbulence across multiple scales. Our turbulent energy spectrum (E(k)) analysis, based on the σ–L and ρ–L scalings, yields a characteristic E(k) ∝ k−1.52. These findings indicate the potential significance of gravity, turbulence, and possibly magnetic fields in regulating dynamics of molecular clouds and high-mass star formation therein.","PeriodicalId":54494,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"67 1","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-05-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141149815","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0

Inelastic Scattering of Dark Matter with Heavy Cosmic Rays 暗物质与重宇宙射线的非弹性散射

IF 1.8 4区物理与天体物理

Research in Astronomy and Astrophysics Pub Date : 2024-05-19 DOI: 10.1088/1674-4527/ad3c6f

Keyu Lu, Yue-Lin Sming Tsai, Qiang Yuan and Le Zhang

{"title":"Inelastic Scattering of Dark Matter with Heavy Cosmic Rays","authors":"Keyu Lu, Yue-Lin Sming Tsai, Qiang Yuan and Le Zhang","doi":"10.1088/1674-4527/ad3c6f","DOIUrl":"https://doi.org/10.1088/1674-4527/ad3c6f","url":null,"abstract":"We investigate the impact of inelastic collisions between dark matter (DM) and heavy cosmic ray (CR) nuclei on CR propagation. We approximate the fragmentation cross-sections for DM-CR collisions using collider-measured proton-nuclei scattering cross-sections, allowing us to assess how these collisions affect the spectra of CR boron and carbon. We derive new CR spectra from DM-CR collisions by incorporating their cross-sections into the source terms and solving the diffusion equation for the complete network of reactions involved in generating secondary species. In a specific example with a coupling strength of bχ = 0.1 and a DM mass of mχ = 0.1 GeV, considering a simplified scenario where DM interacts exclusively with oxygen, a notable modification in the boron-to-carbon spectrum due to the DM-CR interaction is observed. Particularly, the peak within the spectrum, spanning from 0.1 to 10 GeV, experiences an enhancement of approximately 1.5 times. However, in a more realistic scenario where DM particles interact with all CRs, this peak can be amplified to twice its original value. Utilizing the latest data from AMS-02 and DAMPE on the boron-to-carbon ratio, we estimate a 95% upper limit for the effective inelastic cross-section of DM-proton as a function of DM mass. Our findings reveal that at mχ ≃ 2 MeV, the effective inelastic cross-section between DM and protons must be less than .","PeriodicalId":54494,"journal":{"name":"Research in Astronomy and Astrophysics","volume":"28 1","pages":""},"PeriodicalIF":1.8,"publicationDate":"2024-05-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141149810","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0