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. 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":"Characteristic Features of the Magnetic and Ionospheric Storms on December 21–24, 2016","authors":"Y. Luo,&nbsp;L. F. Chernogor","doi":"10.3103/S0884591322050051","DOIUrl":"10.3103/S0884591322050051","url":null,"abstract":"<p>Solar storms accompanied by solar flares, coronal mass ejections, and high-speed flows result in considerable disturbances in the Sun–interplanetary medium–magnetosphere–ionosphere–atmosphere–Earth (internal geospheres) system. As a result, geospace storms with synergistically interacting magnetic, ionospheric, atmospheric, and electrical storms arise in our planet. Magnetic and ionospheric storms have been studied for a long time, but atmospheric storms and electrical storms have been studied considerably to a less extent. Geospace storms and their components exhibit significant variability. It may be asserted that no identical two storms exist. Therefore, a comprehensive study of each new geospace storm and its manifestations and features is an urgent scientific issue. This will contribute to a process of their adequate simulation and, in the long term, forecasting. The purpose of this article is to describe the observed features of the ionospheric and magnetic storms accompanying the geospace storm on December 21–24, 2016. The state of the geomagnetic field has been observed via the fluxgate magnetometer located at the Magnetometer Observatory of the Karazin Kharkiv National University (49°38′ N, 36°56′ E). The dynamics of the ionospheric plasma has been monitored by a vertical incidence Doppler radar and a digisonde located at the Radio Physics Observatory of the Karazin Kharkiv National University (49°38′ N, 36°20′ E). The Doppler radar operate at 3.2 and 4.2 MHz; however, only measurements performed at 3.2 MHz are given below, since a frequency of 4.2 MHz turned out to be inefficient at nighttime when F2 layer critical frequency median <i>f</i>_{0 F2} ≈ 2 MHz, which prevented signal reflection from the ionosphere even at 3.2 MHz. Prior to the beginning of the magnetic storm on December 20, 2016, the level of the <i>H</i> and <i>D</i> components rarely exceeded 0.2–0.7 nT. The sudden commencement of a storm between 06:00 and 10:00 UTC virtually did not affect this level. During the second half of the day on December 21, 2016, the level of exhibited sporadic fluctuations increased from approximately 1 to 3–4 nT. During the next few days, up to December 25, 2016, their level showed variations mostly from approximately 1 nT to approximately 2 nT. Increases in the level were predominantly observed in the period from 05:00 to 15:00 UTC for the <i>H</i> component and from 10:00 to 20:00 UTC for the <i>D</i> component. The weak (power 20 GJ/s and energy approximately 0.45 PJ) geospace storm in the period of December 21–24, 2016, was accompanied by a moderate positive ionospheric storm, as well as by three negative ionospheric storms, one of which was very strong, and the other two were strong and moderate. The geospace storm was accompanied by a moderate magnetic storm with an energy of approximately 2 PJ and a power of approximately 56 GW. The positive ionospheric storm barely affects the level of the signal reflected from the ionospher","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 5","pages":"262 - 278"},"PeriodicalIF":0.5,"publicationDate":"2022-09-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4776689","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":"Ionospheric Effects of the June 10, 2021, Solar Eclipse in the Arctic","authors":"L. F. Chernogor,&nbsp;Yu. B. Mylovanov","doi":"10.3103/S088459132204002X","DOIUrl":"10.3103/S088459132204002X","url":null,"abstract":"<div><div><h3>\u0000 <b>Abstract</b>—</h3><p>Solar eclipses (SEs) cause a variety of processes in all geospheres. There is a decrease of electron density, as well as electron, ion, and neutral temperature, in the ionosphere; the dynamics of ionospheric plasma changes significantly, wave disturbances are generated, and the interaction between subsystems in the Earth–atmosphere–ionosphere–magnetosphere system increases. It has been proven that SE effects depend on the solar eclipse magnitude, geographical coordinates, time of day, season, atmospheric and space weather conditions, position in the solar cycle, and other factors. In addition to recurring or regular effects, there are effects specific to a given SE. For this reason, the study of physical processes in all geospheres caused by SEs is an urgent interdisciplinary problem. The purpose of this work is to present the results of the observation and analysis of time disturbances of the vertical total electron content (TEC) in the Arctic. The data used in this study include the parameters of signals received by a network of stations from navigation satellites passing over the Moon’s shadow, where the SE magnitude was approximately 0.9 in the latitude range 70…80° N. The annular solar eclipse of June 10, 2021, began at 08:12:20 UT and ended at 13:11:19 UT. The Moon’s shadow appeared first over Canada then moved across Greenland, the Arctic Ocean, the North Pole, and the New Siberian Island. The Moon’s shadow covered the northern part of the Russian Federation. Partial SE was observed in northern and middle parts of Europe, most of the Russian Federation, Mongolia, and China. Using 11 ground stations that received GPS signals from 8 satellites, the authors studied the spatial and temporal variations of the TEC during the maximum coverage of the solar disk, which was observed in the Arctic, and found the following. The decrease in electron density for each station and each satellite was observed almost immediately after the beginning of SE and lasted approximately 60…100 min. The minimum TEC value was then detected, followed by an increase to the initial value or higher. The average TEC was 6.4…10.4 TECU. The average decrease in TEC was 2.3 ± 0.6 TECU from 8.4 ± 1.6 TECU. In relative units, the decrease ranged –16.5…–46% (average value –30 ± 9.7%). The time delay between the start of the minimum TEC value relative to the maximum SE magnitude was determined. It varied within 5…30 min (mean value was 18.3 ± 8.5 min). In some cases, quasi-periodic variations in TEC with a period of 9…15 min and a relative amplitude of 3…5% were observed during the SE.</p></div></div>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 4","pages":"197 - 209"},"PeriodicalIF":0.5,"publicationDate":"2022-08-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4420055","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":"Modulation of Galactic Cosmic Ray Intensity in the Approximation of Small Anisotropy","authors":"Yu. I. Fedorov,&nbsp;B. O. Shakhov,&nbsp;Yu. L. Kolesnyk","doi":"10.3103/S0884591322040043","DOIUrl":"10.3103/S0884591322040043","url":null,"abstract":"<div><div><h3>\u0000 <b>Abstract</b>—</h3><p>The propagation of cosmic rays in the interplanetary medium based on the transport equation is considered. The solution of the cosmic ray transport equation is obtained for the known energy distribution of high-energy charged particles at the heliospheric boundary. The spectrum of galactic cosmic rays in the local interstellar medium is taken on the basis of the data from the Voyager 1 and 2 spacecraft. The flux of galactic cosmic rays in different periods of solar activity is calculated. Cosmic ray intensity gradients are estimated, and these calculations are compared to the data from space missions. The anisotropy of the angular distribution of cosmic rays is calculated. It is shown that the flux of galactic cosmic rays in the Earth’s orbit has an azimuthal direction, and the value of the anisotropy of protons with energies from 1 MeV to 1 Gev is of the order of 0.5%.</p></div></div>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 4","pages":"181 - 189"},"PeriodicalIF":0.5,"publicationDate":"2022-08-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4069171","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}

{"title":"Energy Balance of Evanescent Acoustic-Gravity Waves","authors":"A. K. Fedorenko,&nbsp;O. K. Cheremnykh,&nbsp;E. I. Kryuchkov,&nbsp;D. I. Vlasov","doi":"10.3103/S0884591322040031","DOIUrl":"10.3103/S0884591322040031","url":null,"abstract":"<p>The features of the energy balance of evanescent acoustic-gravity waves in the atmosphere are investigated. In the case of freely propagating AGWs in an ideal isothermal atmosphere without dissipation, the period-average densities of kinetic and potential energy are equal to each other. This is true for the acoustic and gravity regions of the AGW spectrum. It is shown that the period-average kinetic and potential AGW energy densities are not equal to each other in the general case in the evanescent spectral region. The exceptions are the Lamb wave and the Brunt–Väisälä oscillations, in which the particles oscillate only along one coordinate (horizontally or vertically). Also, the densities of kinetic and potential energy are equal for the evanescent f- and γ-modes at the points where they touch the regions of freely propagating waves. An assumption is made that the evanescent modes for which the average values of kinetic and potential energies are equal are implemented first.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 4","pages":"190 - 196"},"PeriodicalIF":0.5,"publicationDate":"2022-08-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4069185","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}