Kinematics and Physics of Celestial Bodies最新文献

{"title":"Properties of Acoustic-Gravity Waves at the Boundary of Two Isothermal Media","authors":"A. K. Fedorenko,&nbsp;E. I. Kryuchkov,&nbsp;O. K. Cheremnykh,&nbsp;S. V. Melnychuk,&nbsp;I. T. Zhuk","doi":"10.3103/S0884591322060022","DOIUrl":"10.3103/S0884591322060022","url":null,"abstract":"<div><p>The properties of evanescent acoustic-gravity waves that can propagate along the interface between two isothermal half-spaces with different temperatures are studied. In such a model, the condition of a simultaneous decrease in the wave energy density below and above the interface between the media is not satisfied for the known surface <i>f</i> mode. This study shows that it is possible to implement evanescent waves in the form of combinations of <i>f</i> modes and pseudo-modes (<i>f</i>_<i>p</i> modes) for both half-spaces at the interface between two isothermal media. The cross-linking of solutions at the interface depends on the wave spectral parameters and the magnitude of the temperature jump. At the interface, the wave properties change with an increase in the wavelength and their dispersion and polarization acquire features characteristic of acoustic-type waves. These differences are manifested not only in the dispersion dependence of the waves but also in the change in their amplitudes with height, polarization, and velocity divergence at the interface between the media. It is also found for large temperature differences between the lower and upper half-spaces that there is a spectral region in which the solutions satisfying the boundary condition cannot simultaneously decrease in energy below and above the interface. In this region of the spectrum, the <i>f</i>_<i>p</i> modes with a decreasing energy in the upper half-space and the <i>f</i> modes with an increasing energy in the lower half-space are joined at the interface. The considered waves at the interface between two media can be observed in the stratified atmosphere at altitudes with a sharp temperature change, for example, in the lower part of the Earth’s thermosphere or in the chromosphere–corona transition region on the Sun.</p></div>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 6","pages":"340 - 350"},"PeriodicalIF":0.5,"publicationDate":"2022-12-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4333216","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 Asymptotic Directions of Approach and the Magnetic Rigidity Cutoff of Cosmic Ray Particles for Airports at Different Latitudes and Longitudes","authors":"Witold Wozniak,&nbsp;Krzysztof Iskra,&nbsp;Marek Siluszyk","doi":"10.3103/S088459132206006X","DOIUrl":"10.3103/S088459132206006X","url":null,"abstract":"<p>The calculation of asymptotic directions of approach of cosmic ray particles is an important tool in the determination of the rigidity cutoff for a given geographical site. We present the results of computations of the asymptotic latitude and asymptotic longitude and the magnetic rigidity cutoff for the eight airports (Apatity, Oulu, Warsaw, Lae, Buenos Aires Wellington and Mc Murdo) located at different latitudes and longitudes based on the numerical integration of equations of motion of charged particles of cosmic radiation in the Earth’s magnetic field. The initial distance from the center of the Earth was taken as 20 km above the surface. At about this altitude, most cosmic rays undergo nuclear collisions. Calculations were made for the model of the International Geomagnetic Reference Field (IGRF) in 2015.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 6","pages":"300 - 315"},"PeriodicalIF":0.5,"publicationDate":"2022-12-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4333862","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":"Geospace Perturbations that Accompanied Rocket Launches from the Baikonur Cosmodrome","authors":"Y. Luo,&nbsp;L. F. Chernogor,&nbsp;Y. H. Zhdanko","doi":"10.3103/S0884591322060046","DOIUrl":"10.3103/S0884591322060046","url":null,"abstract":"<div><p>The launch of a rocket requires an energy comparable to the energy of many natural processes. For large rockets, the energy release reaches 10–100 TJ, and the power of engines reaches 0.1–1 TW. The energy release per unit volume is much higher than the specific energy content and energy release of all natural processes. During the launch and flight of a large rocket, disturbances in the substratum, the atmosphere, the ionosphere, and even in the magnetosphere occur. Effects from rocket engine burns have been studied for more than 60 years. Research results have been published in hundreds of articles, handbooks, and monographs. It turns out that the effects produced exhibit diverse geophysical phenomena. The effects near the rocket trajectory, namely, the regions of depressed electron density (ionospheric holes), and the generation of infrasound and atmospheric gravity waves (density waves) are investigated better than other effects. Great attention has been paid to studying the geomagnetic effect. The following methods have been used in studies: the Doppler effect, the Faraday, incoherent scattering, ionosonde, magnetometric methods, etc. The effects accompanying the launches and flights of rockets are being actively studied even now. For many years, large-scale (1 to 10 Mm) disturbances that occur after rocket launches have been studied. Their study makes it possible to better understand the mechanisms of the propagation of disturbances from a rocket over global distances, the interaction of subsystems in the Earth–atmosphere–ionosphere–magnetosphere system, and the ecological consequences of rocket engine burns. Disturbances occurring in the atmosphere and geospace substantially depend on the state of the atmospheric–space weather, time of day, season, and phase of the solar cycle. Even with the launch of two identical rockets, disturbances in the mentioned system can be very different. It should be borne in mind that rockets differ in power, trajectories, fuel composition, and the location of cosmodromes. Therefore, studying the response of subsystems to rocket launches and flights remains an urgent problem. The purpose of this study is to describe the results of an analysis of the ionospheric effects of the Soyuz and Proton rockets launched during the 24th cycle of solar activity from the Baikonur Cosmodrome. To observe the effects in the ionosphere caused by the launch of the Soyuz and Proton rockets from the Baikonur Cosmodrome, a vertical sounding Doppler radar was used. As a rule, measurements are carried out at two fixed frequencies of 3.2 and 4.2 MHz. The smaller of them is effective when studying the dynamic processes in the E and F1 layers, and the larger one is effective when studying the F1 and F2 layers. The parameters of ionospheric disturbances that followed the launches of 81 Soyuz rockets and 53 Proton rockets from the Baikonur Cosmodrome in 2009–2021 are analyzed. It is confirmed that there are several groups of delay ","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 6","pages":"287 - 299"},"PeriodicalIF":0.5,"publicationDate":"2022-12-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4328699","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":"Quantitative Analysis of the Spectrum of HD 108564","authors":"Y. V. Pavlenko","doi":"10.3103/S0884591322060058","DOIUrl":"10.3103/S0884591322060058","url":null,"abstract":"<p>A quantitative analysis of the spectrum of HD 108564 is performed. It is a star of the main sequence of spectral class K5V, the atmosphere of which is depleted in metals. The high-quality observed HARPS spectra are downloaded from the ESO archive. Abundances of elements in the atmosphere are obtained by fit of observational profiles of the C I lines and selected lines of the C₂ molecules, and the O I, Ca I, Si I, Sc II, Cr I, CI, OI, Na I, Mg I, Si I, Ca I, Sc II, Ti I, Ti II, Cr I, Mn I, Fe I, Fe II, Co I, Ni I, Cu I, and Zn I. Abundances are determined iteratively, with a recalculation of the input parameters, which are effective temperature <i>T</i>_eff  at a fixed value of gravity log<i>g</i> (or log <i>g</i> for a fixed <i>T</i>_eff value). The effect of variations of <i>T</i>_eff  or log <i>g</i>, which provide the same abundances of <i>A</i>(Fe I) and <i>A</i>(Fe II), on the abundances of other elements are determined. The obtained results indicate an excess of light elements (C, O, and Si) compared to the group of iron. The absence of the lithium line at 670.8 nm is confirmed with an estimate of <i>A</i>(Li) &lt; –12.5 for the upper limit of lithium abundance in the abundance scale, in which the sum of all abundances is 1.0. The determined radial velocity equal to <i>V</i>_rad = 111.21 km/s is consistent with the known estimates of other researchers. Apparent rotation velocity <i>V</i> sin <i>i</i> = 1.12 ± 0.5 km/s is determined.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 6","pages":"316 - 327"},"PeriodicalIF":0.5,"publicationDate":"2022-12-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4650240","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":"Properties of Acoustic-Gravity Waves at the Boundary of Two Isothermal Media","authors":"A. Fedorenko, E. I. Kryuchkov, O. Cheremnykh, S. Melnychuk, I. Zhuk","doi":"10.15407/kfnt2022.06.079","DOIUrl":"https://doi.org/10.15407/kfnt2022.06.079","url":null,"abstract":"The properties of evanescent acoustic-gravity waves that can propagate along the interface between two isothermal half-spaces with different temperatures are studied. In such a model, the condition of a simultaneous decrease in the wave energy density below and above the interface between the media is not satisfied for the known surface f mode. This study shows that it is possible to implement evanescent waves in the form of combinations of f modes and pseudo-modes ( f p modes) for both half-spaces at the interface between two isothermal media. The cross-linking of solutions at the interface depends on the wave spectral parameters and the magnitude of the temperature jump. At the interface, the wave properties change with an increase in the wavelength and their dispersion and polarization acquire features characteristic of acoustic-type waves. These differences are manifested not only in the dispersion dependence of the waves but also in the change in their amplitudes with height, polarization, and velocity divergence at the interface between the media. It is also found for large temperature differences between the lower and upper half-spaces that there is a spectral region in which the solutions satisfying the boundary condition cannot simultaneously decrease in energy below and above the interface. In this region of the spectrum, the f p modes with a decreasing energy in the upper half-space and the f modes with an increasing energy in the lower half-space are joined at the interface. The considered waves at the interface between two media can be observed in the stratified atmosphere at altitudes with a sharp temperature change, for example, in the lower part of the Earth’s thermosphere or in the chromosphere–corona transition region on the Sun.","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 1","pages":"340-350"},"PeriodicalIF":0.5,"publicationDate":"2022-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"67115862","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":"Kinetic Alfvén Waves’ Generation in Front of the Earth’s Main Shock Wave","authors":"P. P. Malovichko,&nbsp;Yu. V. Kyzyurov","doi":"10.3103/S0884591322050063","DOIUrl":"10.3103/S0884591322050063","url":null,"abstract":"<p>We investigated the possibility of generating kinetic Alfvén waves by beams of high-speed protons in front of the Earth’s main shock wave. An analytical solution is obtained for the hose-type instability of kinetic Alfvén waves caused by the beam’s dynamic pressure. The effect of the temperature of high-speed beams and the temperature of solar wind protons on the characteristics of the generated disturbances is studied. The temperature has a significant effect on the transverse scales of disturbances: the higher the temperature of the beam protons and the lower the temperature of the surrounding plasma, the more stringent the restrictions imposed on the transverse wavelength scales. The development of instability during the propagation of beams of reflected, intermediate, and diffused protons in the region ahead of the Earth’s main shock wave is considered. The dynamics of the movement of disturbances in this region are analyzed.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 5","pages":"231 - 239"},"PeriodicalIF":0.5,"publicationDate":"2022-09-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4780151","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":"Hyades Kinematics and the Relationship Between Galactic Coordinates and its Angular Distance from the Apex with Gaia EDR3","authors":"Amnah S. Al-Johani,&nbsp;W. H. Elsanhoury,&nbsp;Afaf Al-Juhani,&nbsp;Ghada Al-Qadhi,&nbsp;Manar Al-Anazi,&nbsp;Sarah Al-Balwi,&nbsp;Sarah Al-Hamdi,&nbsp;Shorouq Al-Qahtani,&nbsp;Wejdan Al-Shehri","doi":"10.3103/S0884591322050026","DOIUrl":"10.3103/S0884591322050026","url":null,"abstract":"<p>In this paper, we have improved the Hyades members with aid of the Gaia EDR3 source. We have studied their kinematics, including computations of the convergent point with AD-diagram method such as <span>(left( {{{A}_{0}},~{{D}_{0}}} right) = left( {79^circ .48 pm 0^circ .11,~,,6^circ .85 pm 0^circ .38} right))</span>, their spatial velocities <span>(U,~V,~W,{text{(km}};{{{text{s}}}^{{ - 1}}}{text{)}})</span>, their morphology with 3D. A relation was established for Hyades stars between their Galactic coordinates <span>(left( {l,~b} right))</span> and the angular distances <span>(left( {{lambda }} right))</span> from the vertex. The precision criteria of this relation are very satisfactory and a correlation coefficient of value <span>( approx 0.90)</span> was found which proves that the attributes are completely related linearly.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 5","pages":"240 - 247"},"PeriodicalIF":0.5,"publicationDate":"2022-09-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"5073079","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 Viscosity and Oblateness on the Perturbed Robe’s Problem with Non-Spherical Primaries","authors":"B. Kaur,&nbsp;S. Kumar,&nbsp;R. Aggarwal","doi":"10.3103/S088459132205004X","DOIUrl":"10.3103/S088459132205004X","url":null,"abstract":"<p>We here analyzed the effects of viscosity, oblateness of the primary <i>m</i>₁, length parameter <i>l</i>, and perturbations in the Coriolis and centrifugal forces on the stability of the equilibrium points of the Robe’s problem. In the setting, it is assumed that the two primaries <i>m</i>₁, an oblate spheroid of incompressible homogeneous viscous fluid of density ρ₁ and <i>m</i>₂, a finite straight segment of length 2<i>l</i> revolve around their common center of mass in circular orbits while third body <i>m</i>₃ (a small solid sphere of density ρ₃) moves inside <i>m</i>₁. Two collinear {<i>L</i>₁, <i>L</i>₂} and infinite non-collinear equilibrium points are evaluated and found that the location of equilibrium points remain unaffected by viscosity. However, the effects of oblateness and perturbation in the centrifugal force are quite noticeable from the expressions of the equilibrium points. The stability criterion for <i>L</i>₁ and <i>L</i>₂ are stated whereas the non-collinear equilibrium points are found to be unstable. It is observed that the viscosity has a substantial effect on the stability as it changes the nature of stability from marginal stability to asymptotic stability. The perturbations do not affect the stability of <i>L</i>₁ but affect the stability of <i>L</i>₂. Moreover, the effect of oblateness on the stability of the equilibrium points is quite evident. A very important observation of the study is that the oblateness parameter A neutralizes the effects of the length parameter <i>l</i> and perturbation ε₂, on the stability of equilibrium point <i>L</i>₁. The results obtained are applied on Earth-Moon, Jupiler-Amalthea, Jupiler-Ganymede systems (astrophysical problems) to predict the stability of <i>L</i>₁.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 5","pages":"248 - 261"},"PeriodicalIF":0.5,"publicationDate":"2022-09-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4774368","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":"Activity of the Astronomical Observatory of Kharkiv University and Its Employees during the German–Soviet War (1941–1945)","authors":"M. A. Balyshev","doi":"10.3103/S0884591322050038","DOIUrl":"10.3103/S0884591322050038","url":null,"abstract":"<p>A historical research study devoted to the elucidation of the historical facts about the activity of the Kharkiv Astronomical Observatory during the German–Soviet War is carried out. The astronomical community of Kharkiv suffered heavy losses: Professors O.I. Razdol’skii, M.S. Savron, and S.M. Semiletov, Researcher G.L. Strashnii, Yu.M. Fadeev, and V.O. Balanskii, and calculation specialist L.M. Kostirya died; young representatives of the Kharkiv astronomical community M. Azbel’, F. Berezovskii, I. Tymoshenko, and O. Ubiivovk gave their lives in the battle with the enemy. During warfare, many observatory buildings, together with astronomical instruments and devices, were seriously damaged. The peculiarities of observatory operation during the studied period have been documented, and the biographical data of most of the employees of the Kharkiv Astronomical Observatory during the Nazi occupation of the city in 1941–1943 have been clarified. The stages of restoration of the observatory after the liberation of Kharkiv from the invaders were considered.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 5","pages":"279 - 285"},"PeriodicalIF":0.5,"publicationDate":"2022-09-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4775444","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":"Magneto-Ionospheric Effects of the Geospace Storm of March 21–23, 2017","authors":"Y. Luo,&nbsp;L. F. Chernogor,&nbsp;K. P. Garmash","doi":"10.3103/S0884591322040055","DOIUrl":"10.3103/S0884591322040055","url":null,"abstract":"<div><div><h3>\u0000 <b>Abstract</b>—</h3><p>Geospace storms develop in the Sun–interplanetary medium–magnetosphere–ionosphere–Earth (inner spheres) (SIMMIAE) system. The study of the physical effects of geospace storms is the most important scientific direction in space geophysics. The problem of interaction between the SIMMIAE subsystems during geospace storms is interdisciplinary and requires a systematic approach to solve it. The problem is multifactorial in nature. The response of the subsystems is determined by the simultaneous (synergetic) effect of a number of perturbing factors. It is important that the SIMMIAE system is open, nonlinear, and nonstationary. It has direct and inverse, positive and negative relationships. Given the multifaceted manifestations of geospace storms, because of the unique nature of each storm, the study of the physical effects of geospace storms is an urgent scientific problem. In addition to the problems of a comprehensive study of the physical effects of geospace storms, the problems of their detailed adequate modeling and forecasting are highly important. Their solution will contribute to the survival and sustainable development of our civilization, which is mastering more and more perfect and complex technologies. The greater the people’s technological advances, the more vulnerable the civilization’s infrastructure to the effects of solar and geospace storms. The purpose of this article is to present the results of the analysis of the magneto-ionospheric effects that accompanied the geospace storm of March 21 to 23, 2017. The following tools were used to observe effects in the ionosphere and in the magnetic field caused by the geospace storm of March 21 to 23, 2017: a custom-made digital ionosonde and a Doppler vertical sounding radar located at the V.N. Karazin Kharkiv National University Radiophysical Observatory (49°38′ N, 36°20′ E) and a fluxmeter-magnetometer at the Magnetometer Observatory of the Kharkiv National University (49°38′ N, 36°56′ E). As a rule, the Doppler vertical sounding radar makes measurements at two fixed frequencies, 3.2 and 4.2 MHz. The smaller of them is effective when studying dynamic processes in E- and F1-layers and the larger one, in F1 and F2-layers. The fluxmeter-magnetometer is intended for monitoring the variations of horizontal <i>H-</i> and <i>D-</i>components of the geomagnetic field in the time range 1…1000 s. Ionospheric processes are analyzed using ionograms. The dependences of the virtual height <i>z</i>´ on frequency are first converted to dependences of the electron density <i>N</i> on the true height <i>z</i>. The temporal dependences <i>N</i>(<i>t</i>) are then constructed for fixed altitudes in the 140…260 km range. Then, the periods <i>T</i> and absolute amplitudes Δ<i>N</i>_<i>a</i> of quasi-periodic variations <i>N</i>(<i>t</i>), as well as their relative variations δ<i>N</i>_<i>a</i> = Δ<i>N</i>_<i>a</i>/<i>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 4","pages":"210 - 229"},"PeriodicalIF":0.5,"publicationDate":"2022-08-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4069177","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}