Kinematics and Physics of Celestial Bodies最新文献

{"title":"Statistical Analysis of Flat-Spectrum and Steep-Spectrum Pulsars","authors":"Hongbing Cai,&nbsp;Siqi Li,&nbsp;Jingsong Xu,&nbsp;Hang Liu","doi":"10.3103/S0884591326020042","DOIUrl":"10.3103/S0884591326020042","url":null,"abstract":"<p>The radio spectra of pulsars are generally the power-law spectra shapes with a spectral index of approximately –1.6. But people have found that the spectra of some pulsars exhibit flat or steep spectra. Flat spectra refer to radio spectra with spectral indices ranging from –1 to 1, while steep spectra refer to radio spectra with spectral indices less than –2.5. We used the ATNF pulsar catalog and other literature to identify 239 flat-spectrum pulsars and 159 steep-spectrum pulsars, and conducted statistical analysis on the spatial position, magnetic field, spectral index, dispersion measure, and radio luminosity of these pulsars. The research results indicate that flat-spectrum and steep-spectrum pulsars are mainly concentrated near the galactic plane. The average spectral index of flat-spectrum pulsars is –0.62, with an average dispersion measure of 195.7 pc cm⁻³, while the average spectral index of steep-spectrum pulsars is –2.88, with an average dispersion measure of 96.5 pc cm⁻³. The characteristic age of flat-spectrum pulsars is also smaller than that of steepspectrum pulsars. There is a certain correlation between the dispersion measure of these two types of pulsars and their ages, rotation period changing rates, and surface magnetic fields, with the stronger correlations observed in flat-spectrum pulsars. In addition, there is a strong correlation between the dispersion measure of flat-spectrum pulsars and their rotational energy loss rates, while no such correlation has been found between the dispersion measure of steep-spectrum pulsars and their rotational energy loss rates. These correlations may indicate that the interstellar medium has a significant impact on the evolution process of flat-spectrum and steep-spectrum pulsars.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 2","pages":"62 - 79"},"PeriodicalIF":0.7,"publicationDate":"2026-03-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147559299","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}

{"title":"Comparative Analysis of Diurnal-Seasonal Variations of Ionospheric F2-Layer Parameters during the 24th Solar Activity Cycle","authors":"L. F. Chernogor,&nbsp;Y. Luo,&nbsp;Yu. B. Mylovanov","doi":"10.3103/S0884591326020029","DOIUrl":"10.3103/S0884591326020029","url":null,"abstract":"<p>The ionosphere serves as the primary natural medium for radio-wave propagation over wavelengths ranging from millimeters to tens of thousands of kilometers. Understanding regular and irregular ionospheric processes, therefore, remains a critical scientific objective. At present, empirical models of wave disturbances that capture diurnal, seasonal, and longer-term global variations in their parameters do not exist. Developing such models requires consistent, continuous observations worldwide; however, because such coverage is unattainable, researchers typically focus on measurements obtained during characteristic geophysical periods, including the spring and autumn equinoxes and the summer and winter solstices. The present study follows this approach. This work reports the results of an analysis of diurnal and seasonal variations in electron density and associated wave disturbances in the ionospheric F2 layer during the 24th solar activity cycle. To monitor ionospheric conditions, we employed a custom-built digital ionosonde developed at the V. N. Karazin Kharkiv National University. After constructing time series of critical frequencies, the trend and the difference between the original series and the trend were calculated. We determined the electron density and its increment from the critical frequency of the ordinary component of the reflected signal. Across all seasons, a dominant oscillation with a period of 140–250 min, an amplitude of (3.8–11.4) × 10¹⁰ m^–3, and a relative amplitude of 0.09–0.23 appeared in the F2 layer of the ionosphere. Depending on the season, this oscillation persisted for up to 12 h, whereas oscillations at other periods showed substantially smaller amplitudes. Through a comparative analysis of diurnal and seasonal variations in F2-layer electron density and its quasi-periodic disturbances, we established quantitative parameters that characterize these variations.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 2","pages":"47 - 61"},"PeriodicalIF":0.7,"publicationDate":"2026-03-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147559309","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}

{"title":"Analysis of Basins of Attraction in the Pseudo-Newtonian Photogravitational Restricted Four-Body Problem with Asteroid Belt Effects","authors":"Vinay Kumar,&nbsp;Rajiv Aggarwal,&nbsp;Nitesh Kumar","doi":"10.3103/S0884591326020030","DOIUrl":"10.3103/S0884591326020030","url":null,"abstract":"<p>In this study, we examine the convergence behavior of the Newton–Raphson basins of convergence in relation to the equilibrium points serving as attractors within the framework of the pseudo-Newtonian planar circular restricted four-body problem. This model accounts for the effects of both radiation pressure and the presence of a circular asteroid belt. Our focus lies on determining the positions and assessing the stability of these equilibrium points as the transition parameter, denoted by <span>(epsilon )</span>, is varied across the range [0, 1]. By employing a multivariate form of the Newton–Raphson iterative algorithm, we draw the basins of convergence across selected two-dimensional planes. A thorough numerical analysis is carried out to illustrate how changes in the transition parameter influence the structure and geometry of these convergence regions. Furthermore, we examine the relationship between the spatial extent of the attraction basins and the number of iterations needed to reach convergence. The results suggest that the behavior of these regions is complex yet deeply engaging, offering rich insights into the dynamics of the system.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 2","pages":"80 - 100"},"PeriodicalIF":0.7,"publicationDate":"2026-03-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147559310","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}

{"title":"Determination of Current Density in Magnetospheric Plasma: Multispacecraft and Particle Approaches","authors":"B. A. Petrenko,&nbsp;L. V. Kozak,&nbsp;N. O. Khalimonenko","doi":"10.3103/S0884591326010058","DOIUrl":"10.3103/S0884591326010058","url":null,"abstract":"<p>A comparative analysis of two methods for determining electric current density in the near-Earth magnetospheric plasma is presented: the multispacecraft curlometer technique and the particle-based (kinetic) approach relying on plasma moments. The study is based on data from the Magnetospheric Multiscale Mission (MMS) for six magnetic reconnection events in Earth’s magnetotail observed between 2019 and 2024. It is shown that the results of both methods agree well under conditions of stable spacecraft configuration and the absence of radiation contamination in the measurements. The particle-based approach systematically yields overestimated current densities, likely due to locally enhanced ion density near the spacecraft. Spectral analysis reveals that particle-derived data exhibit increased noise levels at frequencies above 1 Hz. The obtained results are important for refining our understanding of energy-dissipation mechanisms and the dynamics of magnetic reconnection processes.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 1","pages":"40 - 45"},"PeriodicalIF":0.7,"publicationDate":"2026-02-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147339316","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}

{"title":"Machine Learning Inference of Black Hole Spin from Simulated Quasi-Periodic Oscillations: A Gaussian Process Regression Approach","authors":"Debarshi Mukherjee","doi":"10.3103/S0884591326010046","DOIUrl":"10.3103/S0884591326010046","url":null,"abstract":"<p>Quasi-periodic oscillations (QPOs) in the X-ray light curves of accreting black holes provide a powerful, albeit complex, probe into the strong-field regime of General Relativity. Traditionally, constraints on black hole spin from QPOs have relied on phenomenological or relativistic precession models, each burdened by systematic uncertainties and observational limitations. In this work, we explore a complementary approach grounded in data-driven inference: using synthetic QPO datasets generated from theoretically motivated spin-frequency relations, we apply Gaussian Process Regression (GPR) to recover the underlying spin parameter of a stellar-mass black hole. Our method is tailored for computational accessibility, requiring minimal training data, no large-scale simulations, and modest hardware while retaining physical interpretability. The GPR model successfully reconstructs the spin parameter from noisy QPO signals with high confidence, highlighting the potential of non-parametric machine learning in extracting astrophysical parameters where traditional likelihoods fail or become intractable. We discuss the implications for future observations from next-generation X-ray observatories, and advocate for broader use of Bayesian non-parametric techniques in theoretical astrophysics. Our work serves as a prototype for applying modern statistical tools to long-standing theoretical questions in black hole physics, even in resource-constrained research settings.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 1","pages":"1 - 8"},"PeriodicalIF":0.7,"publicationDate":"2026-02-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147339320","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}

{"title":"Recurrent Magnetic Storms of January 2–8, 2015","authors":"L. F. Chernogor,&nbsp;Y. Luo","doi":"10.3103/S0884591326010022","DOIUrl":"10.3103/S0884591326010022","url":null,"abstract":"&lt;p&gt;Solar storms, accompanied by flares, coronal mass ejections, and the generation of high-speed solar wind streams, cause a set of physical processes in the geospace environment and on Earth. The collective manifestation of these processes is referred to as a geospace storm. Geospace storms are associated with intense disturbances of the geomagnetic field, the ionosphere, the upper atmosphere (thermosphere), the geoelectric field of magnetospheric-ionospheric-atmospheric origin, the troposphere, and telluric currents. All these disturbances are closely interconnected. Therefore, a geospace storm can be understood as a synergistically interacting system of magnetic, ionospheric, atmospheric, and electrical storms. Every geospace storm is a unique phenomenon. In addition to general patterns, each storm has its own individual characteristics. For this reason, the study of each new storm remains a relevant scientific task. An interesting event occurred in early January 2015: a recurrent sequence of three geomagnetic storms over the course of 1 week. The purpose of this study is to describe the features of fluctuations in the level and spectral composition of the geomagnetic field during these three successive storms from January 2 to 8, 2015. The core of the magnetometric system located at the magnetometric observatory of the V. N. Karazin Kharkiv National University (geographic coordinates: 49.65° N, 36.93° E) is the IM-II induction magnetometer-fluxmeter. It offers high sensitivity (0.5…500 pT for periods of 1–1000 s, respectively). The signal output from the magnetometer, initially in relative units and accounting for the instrument’s amplitude-frequency characteristics, is first converted into absolute units (in nanoteslas). Time series of the amplitudes of the horizontal components of the geomagnetic field are then constructed. Subsequently, a system spectral analysis is performed across the period range of 1–1000 s. Analysis of the three recurrent geospace and magnetic storms observed near the maximum of the 24th solar activity cycle revealed the following. During January 2/3, 4/5, and 7/8, 2015, severe magnetospheric storms occurred, with corresponding powers of 180, 240, and 530 GJ/s and energies of approximately 1920, 4800, and 10 500 TJ, respectively. The magnetic storms during January 2/3, 4/5, and 7/8, 2015, were classified as rather moderate, moderate, and strong, with associated energies of 2.5, 3.1, and 4.9 PJ, and power &lt;i&gt;P&lt;/i&gt;&lt;sub&gt;1&lt;/sub&gt; of approximately 200, 50, and 600 GW. At the same time, the &lt;i&gt;P&lt;/i&gt;&lt;sub&gt;2&lt;/sub&gt; power reached 32, 12, and 23 GW, respectively. During January 2/3, 4/5, and 7/8, 2015, the fluctuation level of the horizontal components of the geomagnetic field increased from 0.5 nT by factors of approximately 4–5, 2–3, and 8–10, respectively. These increases correlated with the average power of the geomagnetic storm during its main phase. During the magnetic storms, fluctuations in the geomagnetic field were domin","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 1","pages":"9 - 23"},"PeriodicalIF":0.7,"publicationDate":"2026-02-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147339319","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}

{"title":"Dynamics of Equatorial and Low-Latitude TEC Fluctuations during the April 2023 Geomagnetic Storm","authors":"Efrem Amanuel Data,&nbsp;Dejene Ambisa Terefe,&nbsp;Solomon Gunta Gutulo,&nbsp;Ayalew Lemma Teklemariam,&nbsp;Gebre Kalute Gebino,&nbsp;Melaku Belayneh Bagaje","doi":"10.3103/S0884591326010034","DOIUrl":"10.3103/S0884591326010034","url":null,"abstract":"<p>This study investigates the ionospheric response to the April 2023 geomagnetic superstorm by analyzing Total Electron Content (TEC) variations over equatorial and low-latitude regions. TEC data derived from GNSS were processed and compared with estimates from the NeQuick model. Geomagnetic indices (<i>D</i>_st, <i>AE</i>, <i>K</i>_p), magnetometer data, and thermospheric <span>({{text{O}} mathord{left/ {vphantom {{text{O}} {{{{text{N}}}_{2}}}}} right. kern-0em} {{{{text{N}}}_{2}}}})</span> ratios from GUVI/TIMED observations were used to track storm-time ionospheric changes. TEC was computed from dual-frequency GNSS signals, corrected for biases, and validated using statistical metrics such as RMSE and the Pearson correlation coefficient (<i>R</i>), which ranged from 0.66 to 0.96 across stations and storm phases. The study found both positive and negative storm-time ionospheric effects, with significant regional differences. A notable depletion in the <span>({{text{O}} mathord{left/ {vphantom {{text{O}} {{{{text{N}}}_{2}}}}} right. kern-0em} {{{{text{N}}}_{2}}}})</span> ratio corresponded with TEC decreases, emphasizing thermosphere-ionosphere coupling during disturbed periods. This integrated observational and model-based approach highlights complex ionospheric dynamics triggered by geomagnetic superstorms and the value of multi-instrument analysis in space weather research.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 1","pages":"24 - 39"},"PeriodicalIF":0.7,"publicationDate":"2026-02-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147339321","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}

{"title":"Possible Signatures of Extremely Strong Magnetic Fields Observed in a Sunspot Based on Spectropolarimetry near the D3 Line","authors":"V. G. Lozitsky","doi":"10.3103/S0884591325060054","DOIUrl":"10.3103/S0884591325060054","url":null,"abstract":"<p>The main goal of the study is to search for super-strong magnetic fields in “quiet” sunspots without flares. The authors’ method is based on Stokes <i>V</i> spectropolarimetry in a wide spectral range, from –5 to +2.5 nm relative to the D₃ He I line. The objects of the study are two simple sunspots with diameters of 35–40 Mm, observed on 17 and 24 July, 2023, near the center of the solar disk, at heliocentric angles of approximately 18°. Novelty of the study consists in the fact that characteristic spectral features are detected in the second sunspot at distances of approximately –1.88 and –0.84 nm from the D₃ He I line, which can be strongly split sigma-components in the Zeeman effect of the mentioned line for the following principal reasons: (a) their Stokes <i>V</i> signs are opposite, and the amplitudes reach 5%, which significantly exceeds the measurement errors, (b) the amplitudes of the blue and red peaks vary synchronously in different places of the sunspot, and (c) the spectral profiles of both peaks have similar shapes and are mutually antisymmetric. If the indicated spectral features are interpreted as a manifestation of the combined action of the Zeeman and Doppler effects, then one can assume the presence of very fine-structured (spatially unresolved) jets in the sunspot that have a magnetic field on the order of 10⁵ G and a plasma ascent speed at the level of 700 km/s. Within this interpretation, it becomes possible to address two current problems in heliophysics: the anomalously rapid rotation of the corona at low latitudes and the occurrence of super-strong magnetic fields at chromospheric and coronal levels.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"41 6","pages":"259 - 267"},"PeriodicalIF":0.7,"publicationDate":"2025-11-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145493328","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}

{"title":"Influence of Turbulence on Electric-Field Intensity Variations in the Earth’s Atmosphere","authors":"L. V. Kozak,&nbsp;B. A. Petrenko,&nbsp;N. O. Khalimonenko,&nbsp;E. A. Kronberg,&nbsp;I. Ballai","doi":"10.3103/S0884591325060042","DOIUrl":"10.3103/S0884591325060042","url":null,"abstract":"<p>The influence of turbulent mixing on the vertical profile of electric-field intensity in the atmospheric boundary layer is investigated. The effects of meteorological conditions and thermodynamic stratification on the electrical conductivity and structure of the electric field are analyzed. It is shown that the turbulent diffusion coefficient <i>K</i>(<i>z</i>), which determines the vertical transport of electric charge, can vary significantly with altitude depending on atmospheric stratification. Several models for describing <i>K</i>(<i>z</i>) are considered, including empirical and theoretically grounded approaches (the Monin–Obukhov model). Calculations based on radiosonde data from the Norderney station (WMO 10 113) for the winter and summer seasons have made it possible to trace seasonal differences in the distributions of the turbulent diffusion coefficient and electric-field intensity. Additionally, data from station 2TDJJ8J aboard the research vessel Polarstern RV, which operates near the Earth’s poles during polar summer, are analyzed. This makes it possible to compare changes in the electric field and the turbulent diffusion coefficient for high-latitude regions of both hemispheres. The similarity of exponential field decay with altitude is established, and differences indicating regional characteristics of atmospheric stratification are identified.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"41 6","pages":"249 - 258"},"PeriodicalIF":0.7,"publicationDate":"2025-11-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145493325","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}

{"title":"Effects of the Solar Eclipse on June 21, 2020, in Low-Latitude Ionosphere Total Electron Content","authors":"L. F. Chernogor,&nbsp;Y. Luo,&nbsp;Yu. B. Mylovanov,&nbsp;V. L. Dorokhov","doi":"10.3103/S0884591325060030","DOIUrl":"10.3103/S0884591325060030","url":null,"abstract":"<p>Solar eclipses (SEs) are accompanied by both regular and a number of irregular effects as well as individual effects inherent in a particular SE. The following questions remain unanswered: can there be effects prior to an SE? How long do they last after the end of an SE? Do they appear on the night side of the planet? What effects occur in the magnetically conjugate region? What is the role of dynamic processes and geophysical fields in the interaction of subsystems in the Earth–atmosphere–ionosphere–magnetosphere system during an SE? These questions need to be addressed. The aim of this paper is to present the results of observations of temporal variations of total electron content (TEC) in the ionosphere over China obtained using Global Navigation Satellite System during the SE and reference days. The low-latitude ionosphere has certain features that could not fail to manifest themselves in the effects of the SE. Estimation of the ionospheric response to the annular SE was performed using recordings of GPS satellite signals obtained on dual-frequency receivers. The error of the TEC calculation technique used in the study does not exceed 0.1 TECU. To obtain acceptable results, the mutual motions of the TEC measurement point, lunar shadow, and Earth’s rotation were taken into account. The ionospheric effect of the SE, which consisted in a significant reduction in TEC, was confidently observed at all five stations and for all seven satellites. It was found that the deficit of TEC clearly followed the maximum magnitude value of the SE. The maximum TEC depletion reached 6–7 TECU at a magnitude of <i>M</i>_max ≈ 0.976–0.986. In this case, the relative TEC depletion was 35–37%. The time delay of the maximum reduction in TEC relative to the maximum magnitude of the SE was close to 15 min. This result is in good agreement with the known data. The moments of the beginning and end of the TEC depletion, in general, did not coincide with the changes in the SE magnitude. The duration of the ionospheric effect was usually longer than the duration of the eclipse. There was no clear dependence of the ionospheric effect on latitude and longitude. No increase in the wave activity during the SE was detected. The effects of the annular SE, which took place in the low-latitude ionosphere near the summer solstice, had a number of features.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"41 6","pages":"228 - 248"},"PeriodicalIF":0.7,"publicationDate":"2025-11-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145493329","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}