Pub Date : 2024-03-01DOI: 10.31725/0367-7966-2024-232-1-7
I.A. Balyaev
Currently, there are many tools for calculating the trajectories of asteroids, comets, and meteor particles in the Solar System. However, only a portion of them are available to the astronomical community. Many of them do not always meet the requirements for accuracy and calculation speed. Since there is no universal solution here, the development of new methods that combine speed and accuracy following specific problems of celestial mechanics does not lose its importance. There is an attempt to combine the advantages of two trajectory calculation methods in this work. The first of them was developed at Saint Petersburg State University to quickly calculate the trajectories of a large number of particles and was implemented as a program R0. A significant disadvantage of this R0 realization is relatively low accuracy. The second one is designed to calculate the trajectory with maximum accuracy and is implemented in the form of the ASSIST software package. However, it provides lower performance. One of the reasons is the usage of complex motion equations. Some simplified models are compared with data obtained using NASA services. An assessment of the applicability of the upgraded R0 program is given. However, only part of them are available to the astronomical community. Many of them do not always meet the requirements for accuracy and calculation speed. Since there is no universal solution here, the development of new methods that combine speed and accuracy following specific problems of celestial mechanics does not lose its importance. There is an attempt to combine the advantages of two trajectory calculation methods in this work. The first of them was developed at Saint Petersburg State University to quickly calculate the trajectories of a large number of particles and was implemented as a program R0. A significant disadvantage of this R0 realization is relatively low accuracy. The second one is designed to calculate the trajectory with maximum accuracy and is implemented in the form of the ASSIST software package. However, it provides lower performance. One of the reasons is the usage of complex motion equations. Some simplified models are compared with data obtained using NASA services. An assessment of the applicability of the upgraded R0 program is given.
{"title":"Modernization of the R0 integrator for calculating asteroid ephemerides: accounting for relativistic and non-gravitational effects","authors":"I.A. Balyaev","doi":"10.31725/0367-7966-2024-232-1-7","DOIUrl":"https://doi.org/10.31725/0367-7966-2024-232-1-7","url":null,"abstract":"Currently, there are many tools for calculating the trajectories of asteroids, comets, and meteor particles in the Solar System. However, only a portion of them are available to the astronomical community. Many of them do not always meet the requirements for accuracy and calculation speed. Since there is no universal solution here, the development of new methods that combine speed and accuracy following specific problems of celestial mechanics does not lose its importance. There is an attempt to combine the advantages of two trajectory calculation methods in this work. The first of them was developed at Saint Petersburg State University to quickly calculate the trajectories of a large number of particles and was implemented as a program R0. A significant disadvantage of this R0 realization is relatively low accuracy. The second one is designed to calculate the trajectory with maximum accuracy and is implemented in the form of the ASSIST software package. However, it provides lower performance. One of the reasons is the usage of complex motion equations. Some simplified models are compared with data obtained using NASA services. An assessment of the applicability of the upgraded R0 program is given. However, only part of them are available to the astronomical community. Many of them do not always meet the requirements for accuracy and calculation speed. Since there is no universal solution here, the development of new methods that combine speed and accuracy following specific problems of celestial mechanics does not lose its importance. There is an attempt to combine the advantages of two trajectory calculation methods in this work. The first of them was developed at Saint Petersburg State University to quickly calculate the trajectories of a large number of particles and was implemented as a program R0. A significant disadvantage of this R0 realization is relatively low accuracy. The second one is designed to calculate the trajectory with maximum accuracy and is implemented in the form of the ASSIST software package. However, it provides lower performance. One of the reasons is the usage of complex motion equations. Some simplified models are compared with data obtained using NASA services. An assessment of the applicability of the upgraded R0 program is given.","PeriodicalId":500837,"journal":{"name":"Publications of the Pulkovo Observatory","volume":"216 S1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140270703","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-03-01DOI: 10.31725/0367-7966-2024-232-29-33
A. Devyatkin, D. Gorshanov, K. N. Naumov, S. N. Petrova, A. Martyusheva, V.V. Kouprianov, A.Kh. Aliev, S. Rusov
The astrometric observations of potentially hazardous asteroid 2001 QQ142 (139622) were made during its apparition after its close approach to the Earth. The observations were made using the mirror astrograph ZA-320M and D.D. Maksutov meniscus telescope MTM-500M of Pulkovo Observatory. The RMS of obtained series of the asteroid positions are σ = ±0''.21 for ZA-320M and σ = ±0''.07 for MTM-500M observations.
{"title":"Observations of potentially hazardous asteroid 2001 QQ142 (139622) with mirror astrograph ZA-320M and D.D. Maksutov meniscus telescope MTM-500M of Pulkovo Observatory","authors":"A. Devyatkin, D. Gorshanov, K. N. Naumov, S. N. Petrova, A. Martyusheva, V.V. Kouprianov, A.Kh. Aliev, S. Rusov","doi":"10.31725/0367-7966-2024-232-29-33","DOIUrl":"https://doi.org/10.31725/0367-7966-2024-232-29-33","url":null,"abstract":"The astrometric observations of potentially hazardous asteroid 2001 QQ142 (139622) were made during its apparition after its close approach to the Earth. The observations were made using the mirror astrograph ZA-320M and D.D. Maksutov meniscus telescope MTM-500M of Pulkovo Observatory. The RMS of obtained series of the asteroid positions are σ = ±0''.21 for ZA-320M and σ = ±0''.07 for MTM-500M observations.","PeriodicalId":500837,"journal":{"name":"Publications of the Pulkovo Observatory","volume":"42 10","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140268000","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-03-01DOI: 10.31725/0367-7966-2024-232-49-53
Z.M. Malkin
The prediction of the Earth’s rotation parameters, including the coordinates of the celestial pole (precession-nutation angles), is necessary for many practical applications. This work is devoted to the study of changes in the accuracy of the prediction of precession-nutation angles over time over the past 16 years. This study was conducted on the basis of real predictions computed in 2007–2022 at the U.S. Naval Observatory, which serves as the Center of Rapid Service and Predictions of the International Earth Rotation and Reference Systems Service (IERS), and at the Pulkovo Observatory. As a result, it turned out that the accuracy of IERS predictions has improved significantly over time, whereas there is no obvious improvement in the accuracy of predictions of the Pulkovo Observatory. For both analysis centers, there is a noticeable decrease in the dependence of prediction errors on its length. It can also be concluded that the predictions of the Pulkovo predictions are more accurate.
{"title":"Analysis of progress in improving the prediction accuracy of Celestial Pole coordinates over the past 16 years","authors":"Z.M. Malkin","doi":"10.31725/0367-7966-2024-232-49-53","DOIUrl":"https://doi.org/10.31725/0367-7966-2024-232-49-53","url":null,"abstract":"The prediction of the Earth’s rotation parameters, including the coordinates of the celestial pole (precession-nutation angles), is necessary for many practical applications. This work is devoted to the study of changes in the accuracy of the prediction of precession-nutation angles over time over the past 16 years. This study was conducted on the basis of real predictions computed in 2007–2022 at the U.S. Naval Observatory, which serves as the Center of Rapid Service and Predictions of the International Earth Rotation and Reference Systems Service (IERS), and at the Pulkovo Observatory. As a result, it turned out that the accuracy of IERS predictions has improved significantly over time, whereas there is no obvious improvement in the accuracy of predictions of the Pulkovo Observatory. For both analysis centers, there is a noticeable decrease in the dependence of prediction errors on its length. It can also be concluded that the predictions of the Pulkovo predictions are more accurate.","PeriodicalId":500837,"journal":{"name":"Publications of the Pulkovo Observatory","volume":"209 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140278834","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-03-01DOI: 10.31725/0367-7966-2024-232-54-61
V.V. Pashkevich
In May of this year (May 22, 2024), the distinguished scientist, the candidate of physical and mathematical sciences (Ph.D.) Georgy Ivanovich Eroshkin would have turned 80 years old. Georgy Ivanovich was one of the leading experts in the field of classical and relativistic celestial mechanics. He was the leading researcher at the Central Pulkovo Astronomical Observatory of the Russian Academy of Sciences (GAO RAS), in 2000-2010 years he was the deputy director of the GAO RAS and head of the Department of Celestial Mechanics at the GAO RAS. He obtained a number of fundamental results in the field of mathematical modeling of the motion of large bodies of the Solar System and the construction of high-precision methods of numerical integration. Georgy Ivanovich’s scientific results have received international recognition. He died five years ago.
{"title":"In memory of Georgy Ivanovich Eroshkin","authors":"V.V. Pashkevich","doi":"10.31725/0367-7966-2024-232-54-61","DOIUrl":"https://doi.org/10.31725/0367-7966-2024-232-54-61","url":null,"abstract":"In May of this year (May 22, 2024), the distinguished scientist, the candidate of physical and mathematical sciences (Ph.D.) Georgy Ivanovich Eroshkin would have turned 80 years old. Georgy Ivanovich was one of the leading experts in the field of classical and relativistic celestial mechanics. He was the leading researcher at the Central Pulkovo Astronomical Observatory of the Russian Academy of Sciences (GAO RAS), in 2000-2010 years he was the deputy director of the GAO RAS and head of the Department of Celestial Mechanics at the GAO RAS. He obtained a number of fundamental results in the field of mathematical modeling of the motion of large bodies of the Solar System and the construction of high-precision methods of numerical integration. Georgy Ivanovich’s scientific results have received international recognition. He died five years ago.","PeriodicalId":500837,"journal":{"name":"Publications of the Pulkovo Observatory","volume":"73 3","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140275896","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-03-01DOI: 10.31725/0367-7966-2024-232-34-43
V.L. Gorshkov, N.V. Scherbakova, S.S. Smirnov
The paper presents the composition and main characteristics of the velocity database (VDB) for about 900 GNSS stations. The VDB is developed and maintained in Pulkovo observatory for stations which are in the territory approximately coinciding with the East European Craton (EEC). More than 70% of stations belong to Russian GNSS networks. The comparison of the VDB velocities with a similar global database of the Nevada Geodetic Laboratory (NGL, USA) for 171 common stations does not detect any systematic discrepancies between them. This fact allows us to use combined data from both DB for geodynamic studies in the EEC region. The kinematic parameters of rotation of some structural blocks of the EEC have been determined. The boundaries of these blocks varied within several degrees, and within these boundaries, stations were selected according to the duration of observations to minimize errors in the least squares solution.
{"title":"Pulkovo’s velocity database of the GNSS station and its scientific potential: geodynamics","authors":"V.L. Gorshkov, N.V. Scherbakova, S.S. Smirnov","doi":"10.31725/0367-7966-2024-232-34-43","DOIUrl":"https://doi.org/10.31725/0367-7966-2024-232-34-43","url":null,"abstract":"The paper presents the composition and main characteristics of the velocity database (VDB) for about 900 GNSS stations. The VDB is developed and maintained in Pulkovo observatory for stations which are in the territory approximately coinciding with the East European Craton (EEC). More than 70% of stations belong to Russian GNSS networks. The comparison of the VDB velocities with a similar global database of the Nevada Geodetic Laboratory (NGL, USA) for 171 common stations does not detect any systematic discrepancies between them. This fact allows us to use combined data from both DB for geodynamic studies in the EEC region. The kinematic parameters of rotation of some structural blocks of the EEC have been determined. The boundaries of these blocks varied within several degrees, and within these boundaries, stations were selected according to the duration of observations to minimize errors in the least squares solution.","PeriodicalId":500837,"journal":{"name":"Publications of the Pulkovo Observatory","volume":"49 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140272375","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-03-01DOI: 10.31725/0367-7966-2024-232-44-48
N. Ikhsanov, N. Beskrovnaya
We consider the accretion-driven spin-up of a magnetized degenerate star in a close binary system under different assumptions about the accretion scenario. We have estimated the minimum possible spin period which the star can achieve in the course of such spin-up. We show that the star can achieve the minimum possible value of the spin period if the interchange instabilities of its magnetospheric boundary are suppressed.
{"title":"Critical period of a star in the scenario of accretion-driven spin-up","authors":"N. Ikhsanov, N. Beskrovnaya","doi":"10.31725/0367-7966-2024-232-44-48","DOIUrl":"https://doi.org/10.31725/0367-7966-2024-232-44-48","url":null,"abstract":"We consider the accretion-driven spin-up of a magnetized degenerate star in a close binary system under different assumptions about the accretion scenario. We have estimated the minimum possible spin period which the star can achieve in the course of such spin-up. We show that the star can achieve the minimum possible value of the spin period if the interchange instabilities of its magnetospheric boundary are suppressed.","PeriodicalId":500837,"journal":{"name":"Publications of the Pulkovo Observatory","volume":"85 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140276650","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-03-01DOI: 10.31725/0367-7966-2024-232-8-28
I. V. Chugunov, A. Marchuk
Various problems concerning the origin and evolution of spiral arms in galaxies are still remain unsettled. Also, only few studies are devoted to the parameters of the spiral structure in distant galaxies. To investigate this, we have performed decomposition with spiral arms of 138 distant galaxies from COSMOS and CEERS surveys, located at redshift 0.1 < z < 2.2 (up to 10.5 Gyr ago). For all 9 galaxies from CEERS, multi-band images are utilized. As a result, different parameters dependence on redshift and wavelength are studied. In particular, we confirm that pitch angle of spiral arms increases with redshift. For the spiral arm width, we find relationship with redshift, but this value depends much stronger on wavelength. A
{"title":"Decomposition of 138 galaxies at 0.1 < z < 2.2 with spiral structure","authors":"I. V. Chugunov, A. Marchuk","doi":"10.31725/0367-7966-2024-232-8-28","DOIUrl":"https://doi.org/10.31725/0367-7966-2024-232-8-28","url":null,"abstract":"Various problems concerning the origin and evolution of spiral arms in galaxies are still remain unsettled. Also, only few studies are devoted to the parameters of the spiral structure in distant galaxies. To investigate this, we have performed decomposition with spiral arms of 138 distant galaxies from COSMOS and CEERS surveys, located at redshift 0.1 < z < 2.2 (up to 10.5 Gyr ago). For all 9 galaxies from CEERS, multi-band images are utilized. As a result, different parameters dependence on redshift and wavelength are studied. In particular, we confirm that pitch angle of spiral arms increases with redshift. For the spiral arm width, we find relationship with redshift, but this value depends much stronger on wavelength. A","PeriodicalId":500837,"journal":{"name":"Publications of the Pulkovo Observatory","volume":"9 14","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140270051","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-01DOI: 10.31725/0367-7966-2023-230-1
I.V. Chugunov, A.A. Marchuk
For the first time we perform the decomposition of 29 galaxies from S4G survey considering spiral arms as a separate component. We analyze the contribution of spiral arms to the azimuthally-averaged profiles of galaxies’ surface brightness using our models, using models obtained with decomposition. We show that spiral arms’ contribution varies strongly with distance to the center, usually reaching its highest value at the radius of about 1,5 exponential scale of the disk and decreasing to zero at the center and on the periphery of the galaxy. We obtain the characteristic values of the «bump» height on the galaxy’s azimuthally-averaged profile which is caused by the spiral arms. Spiral arms’ contribution to the overall luminosity of the galaxy is investigated, its connection with the Hubble type is also confirmed. Our results can be applied, for the rough estimates of axisymmetric components’ share in galaxy’s light, which is important for determination of disk parameters based on azimuthally-averaged surface brightness profiles, or for analysis of the spectral energy distribution in galaxy.
{"title":"Examination of azimuthally-averaged surface brightness profiles of the spiral arms using decomposition.","authors":"I.V. Chugunov, A.A. Marchuk","doi":"10.31725/0367-7966-2023-230-1","DOIUrl":"https://doi.org/10.31725/0367-7966-2023-230-1","url":null,"abstract":"For the first time we perform the decomposition of 29 galaxies from S4G survey considering spiral arms as a separate component. We analyze the contribution of spiral arms to the azimuthally-averaged profiles of galaxies’ surface brightness using our models, using models obtained with decomposition. We show that spiral arms’ contribution varies strongly with distance to the center, usually reaching its highest value at the radius of about 1,5 exponential scale of the disk and decreasing to zero at the center and on the periphery of the galaxy. We obtain the characteristic values of the «bump» height on the galaxy’s azimuthally-averaged profile which is caused by the spiral arms. Spiral arms’ contribution to the overall luminosity of the galaxy is investigated, its connection with the Hubble type is also confirmed. Our results can be applied, for the rough estimates of axisymmetric components’ share in galaxy’s light, which is important for determination of disk parameters based on azimuthally-averaged surface brightness profiles, or for analysis of the spectral energy distribution in galaxy.","PeriodicalId":500837,"journal":{"name":"Publications of the Pulkovo Observatory","volume":"71 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136161924","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-01DOI: 10.31725/0367-7966-2023-230-2
N.R. Ikhsanov, N.G. Beskrovnaya
We consider the accretion process in the X-ray binary systems with neutron stars as relativistic components. We focus our investigation at the question of magnetospheres formation in the process of mass accretion onto the neutron stars in these systems. We note that the answer to this question depends, in particular, on the geometry and physical parameters of the accretion flow. We show that magnetospheres are the most likely to form in the systems with spherical (quasi-spherical) accretion. Formation of a magnetosphere is less likely in the case of accretion through the Keplerian disk or in the MAD-accretion scenario. This findings should be taken into account in the estimation of expected number of accreting X-ray pulsars in the low-mass X-ray binaries.
{"title":"On criteria for the magnetospheric accretion in X-ray binary systems","authors":"N.R. Ikhsanov, N.G. Beskrovnaya","doi":"10.31725/0367-7966-2023-230-2","DOIUrl":"https://doi.org/10.31725/0367-7966-2023-230-2","url":null,"abstract":"We consider the accretion process in the X-ray binary systems with neutron stars as relativistic components. We focus our investigation at the question of magnetospheres formation in the process of mass accretion onto the neutron stars in these systems. We note that the answer to this question depends, in particular, on the geometry and physical parameters of the accretion flow. We show that magnetospheres are the most likely to form in the systems with spherical (quasi-spherical) accretion. Formation of a magnetosphere is less likely in the case of accretion through the Keplerian disk or in the MAD-accretion scenario. This findings should be taken into account in the estimation of expected number of accreting X-ray pulsars in the low-mass X-ray binaries.","PeriodicalId":500837,"journal":{"name":"Publications of the Pulkovo Observatory","volume":"57 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136161921","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-01DOI: 10.31725/0367-7966-2023-230-3
Z.M. Malkin
Galactic aberration in proper motions (GA) has an amplitude (also known as the Galactic aberration constant) of about 5 µas/yr, which is substantial for the modern highly accurate astrometric observations such as Gaia and radio astrometry. There are several determination of the GA constant, but they don’t agree well. The estimates derived from radio astrometry (VLBI) and Gaia observations differ significantly, so it would be very desirable to involve another independent method to solve the problem of inconsistency between these two methods. In this paper, determination of the GA constant from the Galactic rotation parameters determined by methods of stellar astronomy is carried out. Obtained result showed that the GA constant estimate obtained from stellar astronomy agrees within errors with the estimate obtained from Gaia and does not agree well with the estimate based on VLBI observations of extragalactic radio sources.
{"title":"On determination of the Galactic aberration constant","authors":"Z.M. Malkin","doi":"10.31725/0367-7966-2023-230-3","DOIUrl":"https://doi.org/10.31725/0367-7966-2023-230-3","url":null,"abstract":"Galactic aberration in proper motions (GA) has an amplitude (also known as the Galactic aberration constant) of about 5 µas/yr, which is substantial for the modern highly accurate astrometric observations such as Gaia and radio astrometry. There are several determination of the GA constant, but they don’t agree well. The estimates derived from radio astrometry (VLBI) and Gaia observations differ significantly, so it would be very desirable to involve another independent method to solve the problem of inconsistency between these two methods. In this paper, determination of the GA constant from the Galactic rotation parameters determined by methods of stellar astronomy is carried out. Obtained result showed that the GA constant estimate obtained from stellar astronomy agrees within errors with the estimate obtained from Gaia and does not agree well with the estimate based on VLBI observations of extragalactic radio sources.","PeriodicalId":500837,"journal":{"name":"Publications of the Pulkovo Observatory","volume":"34 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136161922","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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