Kinematics and Physics of Celestial Bodies最新文献

{"title":"Bay-Shaped Variations in the Geomagnetic Field that Accompanied the Catastrophic Explosion of the Tonga Volcano on January 15, 2022","authors":"L. F. Chernogor,&nbsp;M. Yu. Holub","doi":"10.3103/S0884591323050033","DOIUrl":"10.3103/S0884591323050033","url":null,"abstract":"<p>The Tonga volcano is among the five most powerful volcanoes in the world. The explosion of the Tonga volcano on January 15, 2022, was unique. It has led to disturbances in the lithosphere, World Ocean, atmosphere, ionosphere, magnetosphere, and all geophysical fields. A number of studies have been devoted to the disturbance of the Earth’s magnetic field. The transport of magnetic field disturbances by atmospheric gravity waves and tsunamis, disturbances in magnetically conjugated regions due to acoustic resonance, the effect on the equatorial electrojet, etc., have been studied. This is far from the end of the variety of magnetic effects of the Tonga volcano. This study is aimed at describing the results of the analysis of global bay disturbances in the geomagnetic field observed after the Tonga volcano explosion on January 15, 2022. The results of measuring the temporal variations in the level of the <i>X</i>, <i>Y</i>, and <i>Z</i> components by the INTERMAGNET world network of stations are used as initial data. The analysis of the magnetic data is preceded by an analysis of space weather conditions. A preliminary analysis of temporal variations in the level of the <i>X</i>-, <i>Y</i>-, and <i>Z</i>-components indicates that these variations on the reference days are smoother than on January 15, 2022. An analysis of the temporal variations in the level of the <i>X</i>-, <i>Y</i>-, and <i>Z</i>-components of the geomagnetic field and a statistical analysis of the disturbance parameters have shown the following. Bay disturbances of all components of the geomagnetic field are observed with a time delay that varies depending on the distance to the volcano from several tens of minutes to 100–200 min. The magnitude of the effect varies from approximately 10 to approximately 60 nT. The largest disturbances occur in the <i>Y</i> component. The delay time and duration of disturbances increase with an increase in the distance from the volcano, while their amplitude, on the contrary, decreases. The speed of propagation of bay disturbances is close to the speed of the blast wave. Bay disturbances are weakly expressed or completely absent on the night side of the planet. It is substantiated that bay disturbances are closely related to the occurrence of an ionospheric hole under the action of a blast wave from the volcano. The results of estimates of bay disturbances are in good agreement with the observation results.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"39 5","pages":"247 - 260"},"PeriodicalIF":0.5,"publicationDate":"2023-10-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"41086641","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":"Spectral Manifestations of Strong and Especially Strong Magnetic Fields in the Active Prominence on July 24, 1999","authors":"I. I. Yakovkin,&nbsp;M. A. Hromov,&nbsp;V. G. Lozitsky","doi":"10.3103/S0884591323050070","DOIUrl":"10.3103/S0884591323050070","url":null,"abstract":"<p>We present the results of the study of the magnetic field in the active prominence on July 24, 1999 at 07:00 UT, using the observational material obtained on the Echelle spectrograph of the horizontal solar telescope of the Astronomical Observatory of Taras Shevchenko Kyiv National University. Our analysis is based on the study of <i>I</i> ± <i>V</i> profiles of the Hα line, which were related to heights in the range of 11–20 Mm. It was found that the bisectors of the <i>I</i> ± <i>V</i> profiles are non-parallel to each other in majority of places of this prominence. This indicates the inhomogeneity of the magnetic field: with a uniform magnetic field, the named bisectors should be parallel. Moreover, the maximum splitting of bisectors is observed not only in the core of the line (which was found earlier by other authors), but also in its far wings, at distances of 1.5–2.5 Å from the line center. The specified maximum of splitting corresponds to magnetic field of about 3000 G, but this value should be considered only as a lower estimate of the true local magnetic fields. In particular, the second maximum of bisector splitting may indicate that the actual value of Zeeman splitting in small-scale structures with a small filling factor reaches the above value of 1.5–2.5 Å which corresponds to the field strength of almost 100 kG. From our study it follows that evidences on such extremely magnetic fields may not actually be a rare phenomenon, but a rather common one, which, however, can be recorded only under certain favorable observational conditions.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"39 5","pages":"287 - 293"},"PeriodicalIF":0.5,"publicationDate":"2023-10-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"41086649","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":"Acoustic Gravity Waves with Height-Independent Amplitude in the Isothermal Atmosphere","authors":"O. K. Cheremnykh,&nbsp;A. K. Fedorenko,&nbsp;S. O. Cheremnykh,&nbsp;E. A. Kronberg","doi":"10.3103/S0884591323050021","DOIUrl":"10.3103/S0884591323050021","url":null,"abstract":"<p>Acoustic gravity wave modes in the Earth’s thermosphere, the amplitude of which does not depend on height, are theoretically investigated. These studies are stimulated by satellite observations, according to which the amplitudes of acoustic gravity waves in the polar thermosphere do not show dependence on height in the altitude range of 250–450 km. It is shown that the propagation of acoustic gravity wave modes with the height-independent amplitude should be considered as an oscillatory process that occurs simultaneously at two natural frequencies. The dispersion equation for these waves is obtained. According to the frequency–wave vector diagnostic diagram, the dispersion dependence of waves with the constant amplitude is in the region that is prohibited for free propagation. It separates the waves propagating horizontally, in which the amplitude in the vertical direction increases from waves with the amplitude decreasing in the vertical direction. Solutions are found for the perturbed quantities in the two-frequency mode of oscillations. It is noted that the superposition of a few of such modes can lead to the emergence of complex resulting motions close to turbulent ones. It is shown that there is a selected quasi-harmonic mode with the constant amplitude, which is characterized by a fixed frequency and wavelength. It is concluded that this kind of wave mode with the height-independent amplitude of the perturbed values prevails in the observations in the Earth’s polar thermosphere.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"39 5","pages":"280 - 286"},"PeriodicalIF":0.5,"publicationDate":"2023-10-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"41086648","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":"Multiscale Dissipative Processes in the Earth’s Magnetotail","authors":"B. Petrenko","doi":"10.3103/S0884591323050069","DOIUrl":"10.3103/S0884591323050069","url":null,"abstract":"<p>The dissipation in the geomagnetic tail is a process that stops the cascade transfer of energy in the inertial turbulent range and transforms the energy of turbulent motions into heating. In the case of kinetic turbulence with the dominance of the thermal pressure over the magnetic field pressure, dissipation is also possible in the inertial range. This study considers an approach for obtaining the distribution of the energy-conversion rate (multiscale spectrum) of the electromagnetic field with the preliminary involvement of the multispacecraft method for calculating the current density. For the first time, a multiscale spectrum of the energy conversion rate in the tail of the Earth’s magnetosphere is obtained and analyzed. The results of measuring the magnetic and electric fields by the MMS mission spacecraft in the region of the current stratum and during high-speed plasma flows in the plasma layer during September 8, 2021 are used.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"39 5","pages":"300 - 303"},"PeriodicalIF":0.5,"publicationDate":"2023-10-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"41086651","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":"Electron Density Reduction Caused by the Tonga Volcano Eruption on January 15, 2022","authors":"L. F. Chernogor,&nbsp;Yu. B. Mylovanov","doi":"10.3103/S0884591323040037","DOIUrl":"10.3103/S0884591323040037","url":null,"abstract":"<p>The explosive Tonga volcano is among the unique ones. Its order of magnitude is the same as Krakatoa (1883), St. Helens (1980), El Chichón (1982), and Pinatubo (1991) volcanoes. The uniqueness of the Tonga volcano lies in the fact that the products of eruption of the Tonga volcano rose to a record height of 50–58 km, whereas the height of eruption of the most powerful Krakatoa volcano reached only 40–55 km. The Tonga volcano has estimates of 3.9 × 10¹⁸ J for thermal energy, approximately 5.8 for volcanic explosive index <i>VEI</i>, approximately 5.5 for volcano magnitude <i>M</i>, and approximately 10.8 for eruption intensity <i>I</i>. We have estimated the explosion energy to be 16–18 Mt TNT. The problems of proving that a decrease in the total electron content (TEC), which was observed on January 15, 2022, in the ionosphere, was caused by the Tonga volcano explosion, and determining the principal parameters of the ionospheric hole are very urgent problems. This study is aimed at analyzing the parameters of the ionospheric hole created by the Tonga volcano explosion on January 15, 2022. Well-known GPS technologies are used to obtain data on time variations of the ionospheric TEC in the vertical column by measuring the pseudo-range and the integrated phase data at two frequencies along the path to each GPS satellite. The space weather conditions were favorable for observing the ionospheric effects caused by the explosion of the Tonga volcano. The calendar dates of January 13 and 17, which are used as reference days, were the least disturbed ones. The main results are as follows. It was found that the TEC on the reference days varied almost monotonically. Aperiodic and quasi-periodic variations of TEC were observed on the day of volcano eruption. Aperiodic variations are associated with a decrease in the TEC. This effect is called the ionospheric hole. It has been proven that the ionospheric hole is caused by a volcanic explosion. The delay time of the hole increases with an increase in the distance between the volcano and the observation site, while both the absolute value of the TEC and the relative value of its decrease are reduced. According to estimates, the horizontal size of the ionospheric hole did not exceed 10 Mm, and the time delay of its appearance did not exceed 122 min. The vertical speed of disturbance propagation was 36–72 m/s, and the horizontal speed was 2.2 km/s. The lifetime of the ionospheric hole was 120–200 min. The TEC in the ionospheric hole was reduced by approximately 2.5–10 TECU, which is a function of the distance from the volcano to the observation site, and the relative decrease ranged from –17 to –34%.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"39 4","pages":"204 - 216"},"PeriodicalIF":0.5,"publicationDate":"2023-08-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4152956","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":"Acoustic-Gravity Wave Spectrum Filtering in the Horizontally Inhomogeneous Atmospheric Flow","authors":"A. K. Fedorenko,&nbsp;E. I. Kryuchkov,&nbsp;O. K. Cheremnykh,&nbsp;I. T. Zhuk","doi":"10.3103/S0884591323040049","DOIUrl":"10.3103/S0884591323040049","url":null,"abstract":"<div><div><h3>\u0000 <b>Abstract</b>—</h3><p>The properties of acoustic-gravity waves (AGWs) in the atmosphere can be determined to a greater extent by the features of the propagation medium than by the sources of these disturbances. In the presence of spatial inhomogeneities of atmospheric parameters, significant deviations of AGW characteristics from theory are observed. This complicates the experimental diagnosis of waves and the search for a connection with their potential sources. AGW observations from the Dynamics Explorer 2 satellite indicates the predominance of waves with certain spectral characteristics in the polar thermosphere. It has been found that AGWs with large amplitudes are spatially consistent with areas of strong winds, while AGWs move mainly toward the wind. In order to explain the observed AGW properties, we investigate the filtering of the spectrum of these waves in the presence of a spatially inhomogeneous wind. It is shown that the direction and magnitude of the wave vector change in a special way in the oncoming inhomogeneous wind. In this case, with an increase in the speed of the headwind, the wave vector gradually tilts toward the horizontal plane. The vertical component of the wave vector decreases rapidly, and its horizontal component tends to some threshold value, which is predominant in observations. In addition, in the oncoming inhomogeneous flow, the frequencies and amplitudes of the waves increase. As a result, high-frequency wave harmonics with a small angle of inclination of the wave vector to the horizontal plane and a characteristic horizontal wavelength will prevail in a strong headwind from the continuous spectrum of atmospheric AGWs that can be generated by a hypothetical source. Since the wave vector and the group velocity vector in AGWs are almost perpendicular to each other, such waves provide efficient energy transfer in the vertical direction. In this regard, AGWs play an important role in the energy balance of the polar atmosphere by redistributing the energy of horizontal wind currents in the vertical direction.</p></div></div>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"39 4","pages":"217 - 224"},"PeriodicalIF":0.5,"publicationDate":"2023-08-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4150199","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":"Predicting the Maximum of Solar Cycle 25: Total Power at the Cycle’s Beginning and in the Previous Cycle as Precursor","authors":"M. I. Pishkalo,&nbsp;I. E. Vasiljeva","doi":"10.3103/S0884591323040062","DOIUrl":"10.3103/S0884591323040062","url":null,"abstract":"<div><div><h3>\u0000 <b>Abstract</b>—</h3><p>Solar activity, the most famous manifestation of which is sunspots, varies with a period of approximately 11 years. Two 11-year cycles form the 22-year magnetic cycle of the Sun. Changes in solar activity lead to changes in the interplanetary and the near-Earth space and affect the Earth and the human environment. The ability to predict solar activity in advance is important both for some practical tasks of cosmonautics and for a better understanding of the nature of those physical processes at the Sun which are responsible for the solar activity. In the work, the interrelationship of the powers (sum of the monthly sunspot numbers in the cycle) of pairs of “even-numbered to odd-numbered” and “odd-numbered to even-numbered” cycles was investigated, and an attempt was made to forecast the maximum of the current solar cycle 25, which began in December 2019, using the value of the total power of the previous solar cycle 24. It was found that there is a significant correlation between the power and amplitude of the odd-numbered cycle and the power of the previous even-numbered cycle (<i>r</i> = 0.897, <i>p</i> = 0.00043 and <i>r</i> = 0.785, <i>p</i> = 0.00715, respectively; if excluding the pair of cycles four to five). A slightly smaller correlation is observed between the amplitude of the odd-numbered cycle and the amplitude of the previous even-numbered cycle (<i>r</i> = 0.712, <i>p</i> = 0.0209). Regression equations between the relevant parameters were found. The calculated predicted amplitude of solar cycle 25 is 155.6 ± 42.4 for August 2024 or 172.1 ± 46.5 for June 2024 if the power of solar cycle 24 or its maximal amplitude is used as precursor, respectively. For solar cycles 12 to 24, the relationship of the same parameters was investigated separately in the <i>N</i>- and <i>S</i>-hemispheres. It was also found that the southern hemisphere will be slightly more active than the northern one in solar cycle 25; the predicted maximal amplitudes in the <i>N</i>- and <i>S</i>-hemispheres are 86.9 ± 41.1 and 91.7 ± 29.7, respectively. The power of the solar cycle for the first 30 months from its start is closely correlated (<i>r</i> = 0.83, <i>р</i> = 5 × 10^–7) both with the amplitude of the next maximum of the cycle and with the duration of the rising phase of the cycle. This makes it possible to obtain, in the authors' opinion, the most probable forecast of the maximum of solar cycle 25 for today, i.e., 136 ± 36 for February 2025. All predictions obtained in this work indicate that solar cycle 25 will be stronger than the previous solar cycle 24.</p></div></div>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"39 4","pages":"225 - 238"},"PeriodicalIF":0.5,"publicationDate":"2023-08-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4152954","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":"Assessment of the Astroclimatic Conditions of the Observation Complex at the Institute of Astronomy of Kharkiv National University","authors":"A. V. Golubaev,&nbsp;A. P. Zheleznyak,&nbsp;V. G. Kaydash","doi":"10.3103/S0884591323040050","DOIUrl":"10.3103/S0884591323040050","url":null,"abstract":"<div><div><h3>\u0000 <b>Abstract</b>—</h3><p>The article is devoted to the comparison of modern astroclimatic conditions (light pollution and the number of cloudless nights) of 14 Ukrainian astronomical observatories. The aim of the work is to assess the prospects for further development of the observational complex of the Chuhuiv Observational Station (COS) at the Institute of Astronomy of Kharkiv National University (IA KNU). The level of light pollution at the selected observation stations is studied using the Global Light Pollution Map databank. The Weather Archive database is used to analyze the statistics of cloudless skies at these locations. An independent measurement of the integral brightness of the sky background is carried out using a portable integrated photometer. It is found that, in terms of light pollution, the COS of the Institute of Astronomy has the most favorable conditions for astronomical observations among other observatories in Ukraine. The results of measurements of the integrated brightness of the sky background at the COS of the Institute of Astronomy using a portable integrated photometer showed a rather dark sky background for a plain observatory; the levels of indicators are similar to the Crimean Astrophysical Observatory. A selective analysis of the weather archive database for the period 2017–2019 for the southern, western, eastern, and central regions of Ukraine showed that, on average, the statistical indicators of cloudless skies in these locations differ little. Taking into account the results of astroclimatic studies and the absence of sources of significant light pollution at distances of 15…20 km from the COS (and the low probability of their appearance in the near future), it can be concluded that it is advisable to modernize the observatory complex of the IA KNU, in particular, to build a modern telescope of 1…2-m class on its territory.</p></div></div>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"39 4","pages":"239 - 245"},"PeriodicalIF":0.5,"publicationDate":"2023-08-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4153470","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 Variations of the Total Electron Content in the Equatorial Ionosphere during the Annular Solar Eclipse of June 21, 2020","authors":"L. F. Chernogor,&nbsp;Yu. B. Mylovanov","doi":"10.3103/S0884591323040025","DOIUrl":"10.3103/S0884591323040025","url":null,"abstract":"<p>A solar eclipse (SE) causes recordable disturbances in all subsystems of the Earth–atmosphere–ionosphere–magnetosphere system and in geophysical fields. The response of the system to an SE substantially depends on the eclipse magnitude, the solar cycle phase, the atmospheric and space weather, the season, the time, and the observation coordinates. Manifestations of the response are also influenced by the observation technique. Despite the fact that the effect of a solar eclipse on the ionosphere has been studied for approximately 100 years, a number of unresolved issues remain. The purpose of this study is to describe the results of our analysis of temporal total electron content (TEC) variations caused by the annular solar eclipse on June 21, 2020, in the equatorial ionosphere. The authors analyzed 132 time dependences of the TEC that covered an extensive region with an eclipse. The maximum magnitude (<i>M</i>_max = 0.9940) of the eclipse, which began at 06:39:59 UT, was observed in northern India in Uttarakhand and lasted 38 s. Space weather conditions on June 21, 2020, were favorable for studying the effects associated with the SE. To reveal the response of the ionosphere to the annular SE on June 21, 2020, the GPS signal recordings were processed. Time variations of the TEC in the ionosphere on reference days and on the SE day of June 21, 2020, were analyzed on a global scale. For this purpose, the results of measurements at twelve stations and eleven GPS satellites were used. The dependences of the absolute and relative TEC value decreases caused by the SE on a time of day are studied. The lowest value of the TEC decrease (–2…–3 TECU) was observed in the morning. In the daytime and in the evening hours, it reached –4…–6 TECU. The relative decrease in the TEC barely depended on a time of day and reached –30…–35%. No stable dependence of the TEC decrease on the eclipse magnitude was found. The relative value of the TEC decrease depended on the SE magnitude, i.e., smaller values of the SE magnitude corresponded to smaller values of the relative TEC decrease. The duration of the TEC reduction exceeded the duration of the eclipse by 1.5–2.5 h. The time of reaching the minimum TEC values in the daytime and the evening hours delayed by 10–20 min with respect to the time of reaching the maximum SE magnitude. Wave-like disturbances of the TEC were practically absent. Undisturbed TEC values and the TEC values disturbed by the eclipse substantially depended on the location of stations and the trajectory of satellites, which was associated with the influence of equatorial ionization anomaly. This is the main peculiarity of ionospheric effects of the SE at latitudes 0°–30° N.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"39 4","pages":"181 - 203"},"PeriodicalIF":0.5,"publicationDate":"2023-08-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4153466","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Analysis of GNSS Observations (GPS Weeks 1934–2105) for the Propagation of the IGS14 Reference Frame on the Territory of Ukraine","authors":"O. Khoda","doi":"10.3103/S0884591323030054","DOIUrl":"10.3103/S0884591323030054","url":null,"abstract":"<p>From January 29, 2017 to May 16, 2020 (GPS weeks 1934–2105) all products of the International GNSS Service (IGS)–precise ephemerides of GPS and GLONASS satellites, coordinates and velocities of permanent GNSS stations, etc.–were based on the IGS14 reference frame, the first IGS realization of the release of the International Terrestrial Reference Frame ITRF2014. Observations of GNSS satellites at permanent stations located in Ukraine and in the Eastern Europe for this period were processed in the GNSS Data Analysis Centre of the Main Astronomical Observatory NAS of Ukraine (MAO). The processing was carried out with the <i>Bernese GNSS Software ver. 5.2</i> according to the requirements of the EUREF Permanent GNSS Network (EPN), that were relevant at that time. In total, observations on 277 GNSS stations, including 205 Ukrainian stations belonging to the following operators of GNSS networks: MAO NAS of Ukraine, StateGeoCadastre of Ukraine (UPN GNSS), NU Lviv Polytechnic (GeoTerrace), PJSC System Solutions (System.NET), TNT TPI company (TNT TPI GNSS Network), Navigation and Geodetic Center (NGC.net), UA-EUPOS/ZAKPOS, E.P.S. LLC, Coordinate navigation maintenance system of Ukraine (NET.Spacecenter), Kiev Institute of Land Relations (KyivPOS), KMC LLC, were processed. The IGS14 reference frame was realized by applying No-Net-Translation conditions on the coordinates of the EPN Class A stations from the EPN C2100 catalogue. As result, the stations’ coordinates in the IGS14 reference frame and the zenith tropospheric delays for all stations were estimated. The mean repeatabilities for components of GNSS stations’ coordinates for all weeks (the characteristics of the precision of the obtained daily and weekly solutions) are in the following ranges: for the northern and eastern components – from 0.6 to 1.4 mm (average values are 0.93 and 1.00 mm respectively) with outliers for the eastern component of 2.02 and 1.55 mm for GPS weeks 2085 and 2091 respectively, for height component – from 2.0 to 5.5 mm (average value is 3.51 mm).</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"39 3","pages":"173 - 179"},"PeriodicalIF":0.5,"publicationDate":"2023-06-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4688488","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}