Kinematics and Physics of Celestial Bodies最新文献

{"title":"Features of the Evolution of Remnants of Supernova SN 1987A Based on Published Studies Obtained with the Hubble and James Webb Space Telescopes","authors":"A. P. Vidmachenko","doi":"10.3103/S0884591326060061","DOIUrl":"10.3103/S0884591326060061","url":null,"abstract":"<p>The Supernova SN 1987A in the Large Magellanic Cloud can be considered a natural testbed for testing hypotheses about the evolution of massive stars and the formation of compact remnants around them. Photometric, spectral, and polarimetric observations of this Supernova, conducted by us in February-December 1987 at the Tarija Astronomical Observatory in the Republic of Bolivia, showed that in May 1987 its brightness reached a maximum with an apparent magnitude of +3.5^<i>m</i>. The spectra obtained by us in March 1987 showed emission features in the range of 397…589 nm, the wavelength shift of which corresponded to the values of the expansion velocity of the Supernova envelope of 5500…8900 km/s. Images obtained with the help of the Hubble Space Telescope (HST) revealed a system of three ionized gas rings surrounding the explosion site. The central ring, about one light-year in diameter, lies in the plane of the equator of the star of the Supernova’s progenitor, and two large outer rings are located in parallel planes in front and behind it. The outer rings could have been formed not by a direct mass ejection, but by a high-energy plasma jet that precesses around its axis. The source of such a jet could be such a compact object as a neutron star or a black hole that is part of a binary system. Analysis of the spots on these rings showed that the thickenings located on the opposite rings are symmetrical about some point that does not coincide with the geometric center of the explosion. It is believed that the precursor of Supernova SN 1987A, the star Sanduleak –69°202, with a mass of up to 20 solar masses, could have been the product of the merger of two stars in a close binary system about 20 000 years ago. The search for a neutron star at the center of the supernova SN 1987A received a new impetus with the start of operations of the James Webb Space Telescope (JWST) in 2022. Since argon and sulfur are synthesized in the deep layers of a massive star immediately before the explosion, their presence in a highly ionized state in the center of the Supernova remnant became a strong argument for the presence of a young neutron star there. Experience in studying SN 1987A may be important for interpreting the structures of other planetary nebulae, such as the “Hourglass” Nebula MyCn 18, DM Taurus, etc.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 6","pages":"294 - 301"},"PeriodicalIF":0.4,"publicationDate":"2026-11-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149367409","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":"The Recovery of Parameters of the Multimode Atmospheric Aerosol Component Based on Polarization Measurements of the Sky over Kyiv","authors":"O. S. Ovsak,&nbsp;A. P. Vid’machenko","doi":"10.3103/S088459132606005X","DOIUrl":"10.3103/S088459132606005X","url":null,"abstract":"<p>According to the data of spectral polarimetric measurements of the sky at the zenith above the observation site GAO, Holosiiv, Kyiv, the vectors of probable values of the parameters of the three main aerosol modes were restored. The quantitative ratio of these modes in the aerosol component of the atmosphere was determined. By comparing those results with the characteristics of atmospheric aerosols determined in the previous work of the authors, changes in the number and magnitudes of the parameters of the main aerosol modes were revealed between the two observation dates and the possible reasons for this were considered. The parameters of the two main coarse modes were determined. For the first coarse mode the geometric mean radius of particles <i>r</i>₀ = 20.4 µm, the real part of the refractive index <i>n</i>_<i>r</i> = 1.44, the dispersion σ² = 0.15. A second aerosol coarse mode in the form of water mist was detected. The recovered parameters of this mode are: <i>r</i>₀ = 18.4 µm, <i>n</i>_<i>r</i> = 1.38, σ² = 0.49. The parameters of the third main finely dispersed aerosol mode remained unchanged: <i>r</i>₀ = 0.11 µm, <i>n</i>_<i>r</i> = 1.45, σ² = 0.11. But a significant decrease in the share of this fine mode in the total value of the degree of linear polarization of the atmospheric aerosol component was detected. A sign of a slight presence of the fourth aerosol mode in the atmosphere was noted. Additions have been made to the description of the Method for recovering the characteristics of the multimode aerosol component of the atmosphere based on spectral polarimetric measurements of a cloudless blue sky, which was developed by the authors. The formulas for analyzing measurement data and determining the characteristics of the aerosol component of the atmosphere with three or more main modes are represented. A procedure for performing the analysis in sequential stages with corresponding model calculations and evaluations of their results is proposed. Recommendations are provided for organizing and performing polarization measurements of the sky in order to obtain data acceptable for correct reconstruction of the parameters of the main modes of atmospheric aerosols. Problems of using other methods for determining the characteristics of the aerosol component in the atmosphere, when using them for arbitrarily selected observation positions, with significant changes in the saturation of air with aerosols and the presence of complex multimode aerosol compositions, are noted.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 6","pages":"279 - 293"},"PeriodicalIF":0.4,"publicationDate":"2026-11-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149367404","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":"Global TEC Variations during the Unique Geospace Storm of May 10–12, 2024","authors":"L. F. Chernogor,&nbsp;Yu. B. Mylovanov,&nbsp;T. K. Hrabko","doi":"10.3103/S0884591326060048","DOIUrl":"10.3103/S0884591326060048","url":null,"abstract":"<p>This study provides a detailed comparative analysis of the global spatiotemporal variations of the ionospheric total electron content (TEC) during the extreme geospace storm of May 10–12, 2024. The analysis was conducted using data from 40 global GNSS stations located in Eastern and Western hemispheres near the 68° W and 112° E meridians. This approach allowed for a direct comparison of the ionospheric response in the western and eastern sectors with high spatial and temporal resolution, avoiding the methodological limitations of global smoothing. In the Western Hemisphere, the geospace storm triggered a strong positive ionospheric storm with a TEC enhancement of over 125 TECU at low and mid-latitudes, as well as an intense super-fountain effect that led to a significant expansion of the equatorial ionization anomaly and an equatorial TEC depletion in the trough region of up to 80 TECU. This positive storm was followed by a widespread negative storm, during which the TEC depletion exceeded 60 TECU. In the Eastern Hemisphere, the ionospheric response was characterized by pronounced latitudinal asymmetry, especially during the recovery phase. At latitudes of 15–60° N, a continuous strong negative storm was observed with a TEC depletion of over 40 TECU, whereas at latitudes of 0°–40° S, following an initial brief drop, a steady TEC enhancement was recorded. Furthermore, over the northern mid-latitudes of the Asian sector, localized westward-moving plasma blobs of enhanced electron density were observed, within which TEC values exceeded the background level by more than 50 TECU. The obtained results compellingly emphasize that the global impact of this unique geospace storm was fundamentally asymmetric: the Western Hemisphere experienced the most extreme primary disturbances, while the Eastern Hemisphere demonstrated a structurally distinct response with strong latitudinal divergence.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 6","pages":"255 - 278"},"PeriodicalIF":0.4,"publicationDate":"2026-11-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149367406","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":"Mathematical Methods of Analytical Description of Wave Disturbances in the Stratified Atmosphere","authors":"O. K. Cheremnykh,&nbsp;A. K. Fedorenko,&nbsp;S. O. Cheremnykh,&nbsp;D. I. Vlasov,&nbsp;O. N. Kryshtal","doi":"10.3103/S0884591326060036","DOIUrl":"10.3103/S0884591326060036","url":null,"abstract":"<p>Wave disturbances are an important component of the dynamics of the Earth’s atmosphere. They propagate throughout the entire atmosphere: from the lower surface layers, where they can be generated by ground and tropospheric sources, such as earthquakes, volcanoes, tsunamis, anthropogenic sources, etc., and up to the rarefied upper layers (~500 km), where their sources are solar wind disturbances, magnetic storms, and charged particle showers. The paper considers two main methods for analytically solving the system of differential equations describing linear wave processes in a model of a stratified non-isothermal atmosphere. It is noted that the equations for linear disturbances describe the following types of waves: acoustic and internal gravity waves freely propagating at an angle to the horizon, as well as horizontal (evanescent) waves. It is shown that acoustic and gravitational waves are described within the framework of the standard method, which consists in reducing the system of linear equations to a single second-order differential equation for one of the components of the perturbed velocity. The solution of this equation allows us to determine other perturbed quantities. Analysis of this method showed that it allows us to satisfactorily describe waves in the isothermal part of the Earth’s atmosphere (thermosphere). The limitation of the specified method for considering evanescent waves is due to the fact that in this case we do not obtain a solution for all values of the horizontal wave vector. Another method, developed by us in previous works, is more acceptable for describing evanescent waves for arbitrary values of the horizontal component of the wave vector. The essence of this method is to use additional relations between the velocity components. This allows us to obtain easily integrated differential equations and find their solutions for each of the components, that is, to actually fully consider the problem of evanescent wave propagation. However, a limitation of this method is that it does not allow finding solutions in a non-isothermal atmosphere, except for the fundamental <i>f</i>-mode.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 6","pages":"245 - 254"},"PeriodicalIF":0.4,"publicationDate":"2026-11-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149367405","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":"The Scientific Legacy of Mykola Bobrovnikoff in the Development of Comet Physics and Spectroscopy in the 20th Century","authors":"M. Balyshev","doi":"10.3103/S0884591326060024","DOIUrl":"10.3103/S0884591326060024","url":null,"abstract":"<p>This article is devoted to a comprehensive analysis of the scientific legacy of Mykola Bobrovnikoff in the context of the emergence of comet physics and the development of spectroscopic research in the 20th century. The paper traces the evolution of the scientist’s research interests—from his early observations and professional training to his fundamental research at leading observatories in the United States. Particular attention is paid to his contribution to the spectrophotometric study of comets, specifically the establishment of dependencies between changes in their brightness and heliocentric distance, and the analysis of molecular lines (CN, C₂, CO₂) in cometary spectra. By synthesizing a large body of observational data, Bobrovnikoff was able to formulate approaches to the physical interpretation of processes in cometary atmospheres, emphasizing the role of non-equilibrium phenomena and interactions with solar radiation. It is shown that the scientist’s works laid the empirical foundation for the further development of cometary astrophysics, influenced the modeling of cometary comas, and refined photometric methods. At the same time, his research in the field of spectroscopy of stars and small bodies of the Solar System is examined, which expands our understanding of the physical nature of the asteroid-comet continuum. It is argued that the scientist’s body of work is systematic in nature and remains significant for modern astrophysical research.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 6","pages":"302 - 310"},"PeriodicalIF":0.4,"publicationDate":"2026-11-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"149367407","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":"Geomagnetic Shielding in the Spectra of High-Energy Particles","authors":"L. V. Kozak,&nbsp;O. Yu. Mylka,&nbsp;B. A. Petrenko,&nbsp;N. O. Khalimonenko,&nbsp;I. Ballai","doi":"10.3103/S0884591326050041","DOIUrl":"10.3103/S0884591326050041","url":null,"abstract":"<p>The Earth’s magnetosphere acts as an energy- and direction-selective filter for high-energy charged particles and, thus, modifies the nonthermal radiation spectrum observed at the ground. The authors developed a physically motivated description of geomagnetic shielding in terms of an effective phase-space potential barrier, introduced the magnetospheric transmission function <i>T</i>(<i>R</i>, <i>t</i>), and formulated a criterion for the transition to the spectral-modulation regime by the magnetic field. To quantify <i>T</i>(<i>R</i>, <i>t</i>) and the temporal evolution of the cutoff rigidity <i>R</i>_<i>c</i>(<i>t</i>), Monte Carlo trajectory tracing in realistic magnetic-field configurations (IGRF internal field plus external current systems) is employed. Using the June 7–8, 2024, event, we compared the model with neutron monitor data (Apatity, Oulu, South Pole) and calibrated the linear parameterization <i>R</i>_<i>c</i>(<i>t</i>) = <i>R</i>_<i>c</i>,0 + α<i>D</i>_st(<i>t</i>). It was found that α = (4 ± 0<i>.</i>6) × 10⁻⁵ GV/nT within the event window, implying very small cutoff variations (≲1<i>.</i>5 × 10⁻³ GV) under modest <i>D</i>_st changes (tens of nT). This separation of magnetospheric filtering from source-driven processes (acceleration/transport) suggests that the observed spectral evolution in this event is predominantly of solar/heliospheric origin.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 5","pages":"199 - 209"},"PeriodicalIF":0.4,"publicationDate":"2026-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148859866","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":"Variations in Solar Wind Parameters during the Extreme Geospace Storm of May 10–11, 2024","authors":"L. F. Chernogor,&nbsp;D. R. Novytska,&nbsp;M. B. Shevelev","doi":"10.3103/S0884591326050016","DOIUrl":"10.3103/S0884591326050016","url":null,"abstract":"<p>This paper investigates the dynamics of the main parameters of the solar wind and the interplanetary magnetic field based on satellite observations during the extreme geospace storm of May 10–11, 2024. It was found that there was a significant increase in the number density, velocity, temperature, and dynamic pressure of solar wind particles and a sharp increase in the variability of the interplanetary magnetic field components during the storm. These changes contributed to the development of powerful disturbances in the Earth’s magnetosphere. A systems spectral analysis revealed that the spectra of the solar wind and interplanetary magnetic field parameters were dominated by components with periods of 150–190 min.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 5","pages":"210 - 218"},"PeriodicalIF":0.4,"publicationDate":"2026-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148859870","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":"Main Types of Energy Losses of Ultrarelativistic Pulsar Plasma in the Upper Layers of a Companion Star’s Atmosphere","authors":"O. M. Ulyanov,&nbsp;M. V. Skoryk,&nbsp;A. I. Shevtsova,&nbsp;A. O. Skoryk","doi":"10.3103/S0884591326050053","DOIUrl":"10.3103/S0884591326050053","url":null,"abstract":"<p>The main types of energy losses experienced by ultrarelativistic electron-positron pulsar plasma in the upper atmosphere of a companion star are considered. These energy-loss mechanisms include ionization losses due to interactions with atoms of the medium, excitation losses associated with the energy transferred to plasma particles, losses resulting from the production of δ electrons, Cherenkov radiation losses, bremsstrahlung losses, synchrotron radiation losses, and inverse Compton losses. It is shown that the fastest component of the pulsar plasma can reach the top of the convection zone of the nearby companion star. The kinetic energy range of the plasma particles reaching the upper boundary of the convection zone corresponds to the energy range of the giant dipole resonance (GDR). As a result of the interaction between the pulsar plasma and the upper atmosphere of the companion star, localized regions of the photosphere and of the photosphere-convection zone boundary at different depths undergo nonuniform (spot-like) heating. This interaction may also produce neutron-rich isotopes, which are subsequently transported into the upper layers of the photosphere.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 5","pages":"185 - 198"},"PeriodicalIF":0.4,"publicationDate":"2026-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148859869","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 TEC Estimation Models over Ethiopia: Case Study during 2015 St. Patrick’s Day Storm","authors":"Nigussie Mezgebe Giday","doi":"10.3103/S088459132605003X","DOIUrl":"10.3103/S088459132605003X","url":null,"abstract":"<p>The ionosphere, a vital layer of Earth’s atmosphere, undergoes dynamic changes influenced by solar and geomagnetic activities. This study evaluates the Multi-Instrument Data Analysis System (MIDAS) for estimating ionospheric total electron content (TEC) in the data-scarce East African longitude sector, focusing on the 2015 St. Patrick’s Day geomagnetic storm. TEC maps from MIDAS are compared with those from the Global Ionospheric Map (GIM) and the AfriTEC neural network-based model, revealing temporal and spatial TEC variations during both quiet and storm conditions. Validation is performed using ground GPS station data. MIDAS and GIM successfully captured TEC enhancements during the storm, while AfriTEC, relying on quiet-condition data, showed limited responsiveness. GIM showed a high correlation coefficient (<i>R</i> = 0.99) with observational data, while MIDAS (<i>R</i> = 0.97) better captured transient diurnal variations. MIDAS outperformed AfriTEC in capturing transient TEC fluctuations, such as diurnal variations and storm-induced enhancements, though it showed occasional variability compared to GIM. The results demonstrate the potential of tomographic techniques in regional ionospheric studies, especially in data-scarce regions, and underscore the importance of model adaptability to geomagnetic variations.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 5","pages":"219 - 231"},"PeriodicalIF":0.4,"publicationDate":"2026-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148859867","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":"Regional Assessment of the Applicability of IRI-2016, IRI-2020, and AfriTEC Models over East Africa during the Ascending Phase of Solar Cycle 25","authors":"Efrem Amanuel Data,&nbsp;Emmanuel Daudi Sulungu,&nbsp;Daniel Izuikedinachi Okoh,&nbsp;Melaku Belayneh Bagaje","doi":"10.3103/S0884591326050028","DOIUrl":"10.3103/S0884591326050028","url":null,"abstract":"<p>Reliable estimation of ionospheric Total Electron Content (TEC) is essential for mitigating signal delays and positioning errors in satellite-based communication and navigation systems. In low-latitude regions such as East Africa, TEC variability is strongly influenced by equatorial electrodynamics, seasonal asymmetry, and solar-cycle evolution, posing persistent challenges for both global and regional ionospheric models. This study presents a regional assessment of the IRI-2016, IRI-2020, and AfriTEC models in reproducing TEC variability over East Africa during the ascending phase of Solar Cycle 25 (2021–2022), a period marked by increasing solar and geomagnetic activity. Model outputs are systematically evaluated against GNSS-derived vertical TEC observations from selected International GNSS Service (IGS) stations, with analyses conducted across four representative seasons corresponding to the March and September equinoxes and the June and December solstices. Model performance is quantified using root mean square error (RMSE), Pearson correlation coefficients, and residual distribution analysis to examine error magnitude and bias under varying geophysical conditions. Results reveal pronounced seasonal dependence, with all models showing larger errors during solstice periods, particularly December. AfriTEC demonstrates improved agreement during equinoxes, with reduced variance and near-zero mean residuals, indicating balanced performance under moderate geomagnetic activity. However, its tendency to overestimate TEC during solstices and underestimate peak values during disturbed intervals highlights limitations in representing thermospheric winds and pre-reversal enhancement variability. IRI-2020 shows modest improvements over IRI-2016 in stability and correlation, yet both global models struggle to capture equinoctial and storm-time TEC extremes during the ascending solar cycle. These findings confirm that model performance over East Africa is strongly modulated by seasonal forcing and solar-cycle phase, underscoring the importance of region-specific validation. Integrating regional GNSS observations with enhanced electrodynamic parameterizations is crucial for improving ionospheric predictions and supporting reliable GNSS-based applications across the African sector.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"42 5","pages":"232 - 244"},"PeriodicalIF":0.4,"publicationDate":"2026-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"148859868","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}