Kinematics and Physics of Celestial Bodies最新文献

{"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}

{"title":"Impact of a Disc and Drag Forces on the Existence Linear Stability of Equilibrium Points and Newton-Raphson Basins of Attraction","authors":"Saleem Yousuf,&nbsp;Ram Kishor","doi":"10.3103/S0884591322030060","DOIUrl":"10.3103/S0884591322030060","url":null,"abstract":"<p>This paper presents a study of zero velocity curves, linear stability analysis and basins of attraction corresponding to the equilibrium points in the Sun-Jupiter system with asteroid belt and β-Pictoris system with dust belt, respectively under the influence of perturbing factors in the form of Poynting-Robertson drag (P-R drag), solar wind drag and a disc, which is rotating about the common center of mass of the system. Zero velocity curves are obtained and it is observed that in the presence of perturbing factors, the prohibited regions of the motion of infinitesimal mass get disturbed. Again, linear stability and effects of perturbing factors are analyzed for the triangular equilibrium points. It is noticed that because of P-R drag, triangular equilibrium points become unstable within the stability range. Finally, the Newton-Raphson basins of attraction corresponding to the equilibrium points are computed and it is found that in the presence of the disc, geometry of the basins of attraction gets change, whereas the effects of remaining perturbing factors on the structure of basins of attraction are very small.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 3","pages":"166 - 180"},"PeriodicalIF":0.5,"publicationDate":"2022-06-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4937949","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":"Physical Effects of the Yushu Meteoroid: 1","authors":"L. F. Chernogor","doi":"10.3103/S0884591322030035","DOIUrl":"10.3103/S0884591322030035","url":null,"abstract":"<p>The purpose of this article was to evaluate the mechanical, optical, and gasdynamic effects that accompanied the passage and explosion of the Yushu meteoroid. The explosion occurred over a sparsely populated area, Qinghai Province (Tibetan Plateau, People’s Republic of China). According to NASA, the initial kinetic energy of the celestial body was approximately 9.5 kt TNT or 40 TJ. Approximately 4.9 TJ, i.e., 12.25% of the initial kinetic energy of the body, was converted into the energy of the light flash. The projections of the velocity of the meteoroid are as follows: <i>v</i>_<i>x</i> = –2.6 km/s, <i>v</i>_<i>y</i> = 5.9 km/s, and <i>v</i>_<i>z</i> = –12.1 km/s. They are used to estimate the angle of inclination of the trajectory to the horizon, which is approximately 5°. Using the explosion height of 35.5 km and the inclination angle, the density of the matter is estimated to be close to that of an ordinary chondrite (approximately 3.5 t/m³). Knowledge of the kinetic energy and velocity allows us to calculate the mass of the meteoroid (432 t) and its characteristic size (6.2 m). The energy of the processes, as well as mechanical, optical, and gasdynamic effects of the celestial body, are analyzed. The main release of energy accompanying the deceleration of fragments of the body destroyed at a dynamic pressure of ~1 MPa took place in a 17.2 km long area at a height of approximately 35 km. A quasi-continuous fragmentation and a power law of the distribution of the mass of the fragments are assumed. The main parameters of ballistic and explosive shock waves are estimated. With a Mach number of 45, the radius of the ballistic shock wave was approximately 280 m, and the fundamental period was 2.6 s, which increased from 9.5 to 30.1 s due to dispersion as the distance traveled by the wave increased from 50 to 5000 km. The radius of the cylindrical and spherical explosion waves was approximately 0.8 and 2 km, respectively, and the fundamental period was 7.5 and 18.8 s. This period increased from 21.1 to 66.7 s as the distance increased from 50 to 5000 km. Near the meteoroid terminal point, the relative overpressure was maximal. It decreased with decreasing height, and increased with increasing height until approximately 120–150 km, where it reached ~10–20 percent and then decreased to a few percent. The absolute value of the overpressure for the spherical wave was maximal near the explosion height, then it decreased as the height decreased to 15 km, then increased again. At the epicenter of the explosion, it was approximately 310 Pa for a cylindrical wave or ~48.5 Pa for a spherical wave, which is insufficient to damage ground objects. With increasing height, the overpressure decreased from many tens of pascals to micropascals. The average power of a light flash with a duration of approximately 1.26 s was 3.9 TW, the power flux density near the fireball, more precisely, a 3.4 km long cone with a diameter ","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 3","pages":"132 - 147"},"PeriodicalIF":0.5,"publicationDate":"2022-06-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4941824","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":"Bands of NaH lines in Spectra of Late Type Stars","authors":"Yu. P. Lyubchyk,&nbsp;Ya. V. Pavlenko,&nbsp;O. K. Lyubchyk,&nbsp;H. R. A. Jones","doi":"10.3103/S0884591322030059","DOIUrl":"10.3103/S0884591322030059","url":null,"abstract":"<p>The absorption of radiation by systems of NaH molecule bands in the atmospheres of late-type stars is modeled. Calculations of synthetic spectra with model atmosphere parameters, which corresponds to M stars, show that the lines of this molecule form notable spectral details approximately the same intensity at wavelengths from λ ≈ 380 nm to almost ~1100 nm. The recently calculated parameters of the NaH molecule from the Exomol database, as well as a new value of the dissociation potential of this molecule <i>D</i>₀ = 1.975, were used in the calculations. The dependences of the calculated spectral energy distributions on the dissociation potential of the NaH molecule and on the parameters of the stellar atmospheres (<i>T</i>_eff, log <i>g</i>, [Fe/H]) were considered. Analysis of synthetic spectra shows that the lines of the NaH molecule become weak with temperature increasing and gravity decreasing in the stellar atmosphere. Thus, sodium hydride lines cannot be observed either in stars with effective temperatures corresponding to early M stars nor in M giants. NaH lines should appear only in the spectra of cold dwarfs, although the strong absorption of other molecules (TiO, CrH, and FeH) in visible and near-infrared region of the spectrum and absorption by atoms in the blue region make the NaH lines' detection a very complicated task. The energy distribution in the spectrum of the red dwarf VB 10 (M8V) in the blue region of the spectrum is modeled. The results of the analysis show that, under normal conditions and close to the solar chemical composition, NaH molecules provide only an additional component in the opacity of the spectra of cold dwarfs and substellar objects.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 3","pages":"159 - 165"},"PeriodicalIF":0.5,"publicationDate":"2022-06-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4936736","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":"On the Nonlinear Interaction of Low-Frequency Kinetic Plasma Waves in the Preflare Atmosphere of the Solar Active Region","authors":"O. N. Kryshtal,&nbsp;A. D. Voitsekhovska","doi":"10.3103/S0884591322030047","DOIUrl":"10.3103/S0884591322030047","url":null,"abstract":"<p>Necessary conditions for the appearance of decay instability of low-frequency kinetic Alfven waves in loop structures of an active region on the Sun before a flare are obtained. On the basis of the transcendental dispersion equation obtained using the synchronism conditions and additional conservation laws, an expression is obtained for the nonlinear growth rate of the decay instability of the initial kinetic Alfven wave (KAW) to the secondary KAW and the kinetic ion-acoustic wave (KIAW). Boundary values of the reduced amplitude of the initial KAW in the preflare atmosphere of an active region (AR) are obtained. It was assumed in the calculations that the waves involved in the process in the AR under study appear due to the development of instability caused by the presence of a weak large-scale (sub-Dreicer) electric field and drift motions of the plasma due to spatial inhomogeneities of its temperature and density. It is shown that, for a certain type of semiempirical model of the solar atmosphere, kinetic Alfven and kinetic ion-acoustic waves can be generated during the linear stage of instability development. In this case, the process of wave generation can take place both in plasma with purely Coulomb conductivity and in the presence of small-scale Bernstein turbulence in it. To “trigger” the instability, relatively low values of plasma nonisothermality and a very low threshold value of the reduced amplitude of the sub-Dreicer electric field are required. The possibility of the appearance of undamped kinetic waves of small amplitude in the region under study is proven.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"38 3","pages":"148 - 158"},"PeriodicalIF":0.5,"publicationDate":"2022-06-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4936737","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}