Odessa Astronomical Publications最新文献

{"title":"FUNDAMENTAL PARAMETERS OF SUPERGIANT STAR HD 40589 (A0Iab)","authors":"Z. Samedov, U. Rustem, G. Hajiyeva, Z. F. Aliyeva","doi":"10.18524/1810-4215.2023.36.290802","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290802","url":null,"abstract":"The atmosphere of HD 40589 (A0Iab) supergiant star of A spectral class was studied using the model atmosphere and parallax methods. The effective temperatures (Teff) and surface of gravity (log g) were determined using a comparison of the observed and  calculated values of the photometric quantities [c1], Q and the equivalent widths of the hydrogen Balmer lines and parallax. Based on the Fe II lines the microturbulent velocity and metallicity [Fe/H] were determined. Metallicity of the program star is close to the metallicity of the Sun. This shows that our program star and the Sun are formed from the interstellar medium of a similar metallicity.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"61 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139011946","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}

{"title":"THE PROBLEM OF OBTAINING COMBINED GAMMA AND OPTICAL DETECTORS FOR THE REGISTRATION OF FAST NUCLEAR PROCESSES","authors":"Marko D. Doikov","doi":"10.18524/1810-4215.2023.36.290774","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290774","url":null,"abstract":"The physical and technical aspects of the registration of fast physical processes involving nuclear transformations with the help of binary detectors in the γ-and optical ranges are considered We chose a semiconducting perovskite crystal CsPbBr3 as the main element of the detector. Have been presented with geometrical and technologically usable parameters of the CsPbBr3 crystal for its implementations in nuclear medicine, geophysics and astrophysics. One of the objects that allow testing of the developed high-speed spectrographic equipment are lightning discharges in the atmospheres of planets, including the Earth. The thermonuclear nature of γ-bursts detected during thunderstorms was revealed by their spectra. The paper shows the role of the corresponding channels involving high-energy protons and α-particles, leading to the formation of 116C, 137 N, 158O isotopes. The registration of the γ-spectrum of the flash and its evolution allowed to estimate the character, energy and time scales of the processes necessary for the design and manufacture of multipurpose measuring complexes by us. The inclusion of γ-spectra in the consideration allowed to estimate the correlation between the maximum currents of particles and the productivity of γ-rays. In the experiments planned by us, the magnetic field fluctuations caused by currents are simultaneously recorded by highly sensitive magnetic field detectors. The height of the building of the Faculty of Physics in Smolyan, Bulgaria, is 900 meters above sea level. This makes it possible to place the measuring complex as close as possible to the sources of hard radiation and to carry out easurements in the immediate vicinity. Unlike distant space objects, the perovskite detector registers the positions themselves. This makes it possible to use the methods of positron γ-spectroscopy and accurately determine the parameters of local currents. The technological parameters of the device were determined. A simulation model was created in Simulink MATLAB, LabVIEW with synchronization of the operation of the listed spectrographs. The characteristic shape of the signal formed by individual γ-quanta with the parameters of the Gaussian function and the total number of these quanta are calculated. The degree of mathematical blinding of neighboring Gaussian functions and its influence on the structure of the final spectrogram in the form of an autocorrelation function is estimated. The similarity of the time scales of thermonuclear explosion processes on white dwarfs (WD) and the processes of synthesis of 116C, 137 N and 158O isotopes in the flash head is determined. It is concluded that it is expedient to create a robotic network of lightning observation stations similar to the meteor patrol at the I. I. Mechnikov National University of Ukraine.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"8 7","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012278","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}

{"title":"GALAXY CLUSTER MERGERS: THE USE OF THE COMPUTER MODELING","authors":"M. Berkovskyi, E. Panko, N. Miroshnik","doi":"10.18524/1810-4215.2023.36.289962","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.289962","url":null,"abstract":"We show the possibilities of the methods of computer modeling of the galaxy cluster merger process with different initial parameters for the investigation of the features of the clusters after colliding.\u0000We considered the galaxy clusters as evolving objects including through collisions. Computer modeling of galaxy cluster mergers and comparing its results with observational data makes it possible to determine the evolutionary status of real clusters with complex internal structures. Within the study, we analyzed in detail a series of models of the galaxy clusters’ merger consequences by ZuHone under different initial conditions like mass ratio, initial collision parameter, or plasma coefficient β. The considered time intervals were from 0 to 4.8 billion years, from 0 to 6 billion years, and from 0 to 10 billion years, depending on the initial conditions.\u0000Based on the images of the simulated galaxy clusters, maps of the distribution of the total mass density and X-ray radiation were created and compared with observations. We showed a good perspective to use this catalog for studying galaxy clusters having compound inner structure.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"11 12","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012369","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}

{"title":"SPECTRAL OBSERVATIONS OF THE ALGOL - TYPE BINARY STAR δ LIBRAE","authors":"B. Rustamov, Kh. M. Mikailov, K. Alisheva, S. Mammadova, Sh. A. Agayeva, O. V. Maryeva","doi":"10.18524/1810-4215.2023.36.290121","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290121","url":null,"abstract":"The results of spectral observations of the Algol-type binary star δ Lib are presented. The behavior of Hα and Hβ lines in the star’s spectrum during the orbital period phase is described. Based on our measurements of the radial velocities of the Hα and Hβ lines and using published data, the radial velocity curves of both components of the δ Lib system were constructed. In some phases of the orbital period, an absorption component was detected in the blue, or red, part of the Hα and Hβ line profiles. The observed Hα and Hβ absorption lines are attributed to the main component of the binary system δ Lib. It is assumed that the appearance of absorption components at these lines is associated either with suspicion of a third component in the system, or at these phases of the Hα and Hβ lines, the primary and secondary components of the δ Lib system are observed simultaneously.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"278 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012394","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}

{"title":"THE EARTH’S MAGNETIC FIELD AND THE LARGE-SCALE MAGNETIC FIELD OF THE SUN: THE SOLAR-TERRESTRIAL CONNECTION","authors":"M. Orlyuk, A. Romenets","doi":"10.18524/1810-4215.2023.36.290538","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290538","url":null,"abstract":"The paper presents the results of a joint analysis of the Earth's main magnetic field (core field) BIGRF and the large-scale magnetic field (LSMF) of the Sun. Selected 11- and 22-year periods of LSMF and BIGRF variations are well manifested in both fields and are usually modulated by solar activity. Even 11-year cycles for which the direction of the Sun's magnetic field coincides with the direction of the Earth's magnetic field are characterized by the minimum values of sanspot numbers, and odd cycles with opposite directions of magnetic fields have larger values of sunspot numbers. The rotation rate of two- and four-sector structure of the Sun source of LSMF varied with about 11-year and 22-year cycle. Longer changes in the magnetic fields of the Sun and the Earth with a period of about 75 years have also been revealed.\u0000The rotation periods of the Sun source global field (28.0-28.5 days) were maximum at the middle of the 20th century in the period 1940÷1960 years. This maximum of solar activity corresponds to temporal gradient of geomagnetic field. It is shown that the gradient of the geomagnetic field BIGRF depends on the rate of change in the length of the day. So, according to the results of the study, the rotation modes of the Sun and the Earth cause different periodic changes in their magnetic fields.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"111 3","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012695","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}

{"title":"AN ENIGMA OF THE PRZYBYLSKI STAR","authors":"S. M. Andrievsky","doi":"10.18524/1810-4215.2022.35.268673","DOIUrl":"https://doi.org/10.18524/1810-4215.2022.35.268673","url":null,"abstract":"A new scenario to explain the Przybylski star phenomenon is proposed. It is based on the supposition that this star is a component of a binary system with a neutron star (similar to the hypothesis proposed earlier by Gopka, Ul’yanov & Andrievskii). The main difference with previous scenario is as following. The orbits of the stars of this system lie in the plane of the sky (or very close to this plane). Thus, we see this star (and its companion) nearly polar-on, and therefore we cannot detect the orbital motion (spectral line based) from the Przybylski star spectrum. In relation to the Przybylski star, the neutron star is a γ-ray pulsar for it. A neutron star is a source of relativistic particles and radiation emitted from the certain parts of its surface. The topology of this radiation strongly depends on the the magnetic field configuration of the neutron star. Existing models suppose that 1) high-energy electronpositron pairs and hard radiation are produced in the (magnetic) polar zones. Accelerated charge particles that move along magnetic lines emit electromagnetic quanta. In this model the radio-emission is genetically linked with the emission of the γ-quanta. 2) Another model of the outer gap is based on the assumption that there is a vacuum gap in the outer magnetosphere of the neutron star, which arises due to the constant escape of charged particles through the light cylinder along the open magnetic field lines. The direction of such escape may be roughly orthogonal to the rotation axis. If the rotational axes of the Przybylski star and the neutron star are close in direction (or even aligned), charged particles and hard radiation ejected in the approximately orthogonal direction at a large solid angle can enter the Przybylski star atmosphere, causing there different physical processes. As a possible source of the free neutrons could be the nuclear reactions between high-energy γ-quanta and nuclei of some atoms in the Przybylski star atmosphere gas. As a result, photoneutrons can be generated. Large enough neutron flux can be produced in the reactions with quite abundant element of the atmosphere gas (for example, helium). The photoneutrons produced in these reactions are rapidly thermalized and, as resonant neutrons, react with seed nuclei in the s-process. It should be also noted that together with s-process elements, the deuterium nuclei could be formed as a result of the interactions of the free resonant neutrons with the hydrogen atoms, but this issue has not yet been worked out.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":" ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2022-12-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"44218161","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}

{"title":"COMPARATIVE ANALYSIS OF OBSERVATIONS OF THE SELECTED EXOPLANET TRANSITS OBTAINED AT THE KYIV COMET STATION WITH THE DATABASE OF THE ORBITAL TELESCOPES TESS AND KEPLER","authors":"M. Lobodenko, Y. Pavlenko, I. Kulyk, A. Nahurna, M. Solomakha, O. Baransky","doi":"10.18524/1810-4215.2022.35.268007","DOIUrl":"https://doi.org/10.18524/1810-4215.2022.35.268007","url":null,"abstract":"We present a comparative analysis of observations of the selected exoplanet transits obtained at the Kyiv Comet station with the database of the TESS (Transiting Exoplanet Survey Satellite) and Kepler space telescopes. The light curves obtained by the TESS and Kepler orbital telescopes were processed using a program based on the Python package Lightcurve 2.3v which is freely available in the MUST archive (Barbara A. Mikulski Archive for Space Telescopes). The ground based observations were carried out with the 70-cm telescope AZT- 8 (Lisnyky). Photometric processing of the ground based observation was performed by using the Muniwin program. The light curves and parameters of the observed transits as well as the exoplanet orbital parameters obtained from ground based observations were published in the ETD (Exoplanet Transit Database). Determined transit parameters were compared with the results of the TESS command, which are stored in the MUST archive. Here we presents a comparison of the parameters of transit phenomena (period, depth, transit duration) and some orbital parameters obtained from two independent sets of observations, terrestrial and orbital, performed in different epochs.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":" ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2022-12-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"42773349","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}

{"title":"OBSERVATION OF AN OCCULTATION OF THE UCAC4 488-082551 STAR BY ASTEROID (76228) 2000 EH 75 ON 31 MAY 2022","authors":"Y. Gorbanev, V. Kleshchonok, S. Kimakovsky","doi":"10.18524/1810-4215.2022.35.268213","DOIUrl":"https://doi.org/10.18524/1810-4215.2022.35.268213","url":null,"abstract":"Observations of an occultation of the UCAC4 488-082551 star by asteroid (76228) 2000 EH 75 were carried out on 31 May 2022 at Kryzhanivka observation station of Odesa I. I. Mechnykov National University (the observatory code A85). A set of instruments, which included a Schmidt telescope (the primary mirror diameter D = 271.25 mm; the corrector plate diameter D k = 223.9 mm; the focal length F = 440 mm), a GPS receiver and Videoscan-415-2001 CCD camera, was used to perform observations. The observing conditions were as follows: clear sky, the star’s altitude 49 0 south, the Moon was below the local horizon. The target star from the UCAC4 catalogue (Zacharias et al. 2013) has the following photometric parameters: m B = 14.008; m V = 12.720; m r = 12.284; m i = 11.813. The diameter of the star has not been determined. Asteroid (76228) is a Main Belt asteroid with an orbital period of 4.17178 years. It has an absolute magnitude of 14.93, the visible geometric albedo of 0.123±0.013 and diameter of 5.00±0.23 km (Masiero et al. 2011). The time of occultation predicted using ephemerides was 23:52:44±4 sec. The maximum duration of the occultation was 0.4 sec, provided that the observing site was located at the centre of the occultation track (strip). A drop in the star’s brightness observed during occultation was about 8 m . The occultation event was recorded as a sequence of GIF images with the exposure time of 0.5 sec per frame. The system clock of the computer used for the occultation recording was controlled with a GPS receiver in a fashion similar to that described in the paper by Karbovsky et al. (2017). The data processing yielded an estimate of the occultation duration of 0.46±0.04 sec. The uncertainty of the occultation start time within exposure results in the total estimate of accuracy in timing the maximum phase of occultation 23:52:44.06±0.10 sec. The chord length across the asteroid estimated by timing the occultation is L = 9.2±0.8. This chord length is close to the estimates of the asteroid diameter reported in the paper by Masiero et al. (2011).","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2022-12-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"41409607","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}

{"title":"SPHERICALLY SYMMETRIC SYSTEM OF GRAVITATIONAL AND ELECTROMAGNETIC FIELDS AND THE STRUCTURE OF ITS CONFIGURATION SPACE","authors":"V. Gladush","doi":"10.18524/1810-4215.2022.35.268190","DOIUrl":"https://doi.org/10.18524/1810-4215.2022.35.268190","url":null,"abstract":"Geometrodynamics of charged black holes (BH) described by the system of Maxwell Einstein equations is considered. We start from a spherically symmetric metric, a reduced action, and a Lagrangian written in characteristic variables. The configuration space (CS) metric, Hamiltonian, momentum and electromagnetic constraints are constructed. The system has conservation laws of charge q and mass m. The action functional is transformed into a Jacobi-type functional in CS with a metric conformal to the CS metric. A transformation of field variables is introduced which brings the CS metric to the \"Lorentzian\"form. The resulting CS metric is the metric of a flat nonholonomic section of a 4-dimensional space. In the new variables, the squared momenta of the system has the Lorentz form. On this basis, quantization is considered. Thanks to the structure of the CS, the momentum operators, the DeWitt equations, and the mass and charge operators are constructed. The equations system of CBH quantum states with certain q and m is constructed. For comparison, we consider the CBH reduced model limited in the T-region. In such the simplified formulation, the T-model equations are integrated and lead to the CBH with continuous spectrum of m and q.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":" ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2022-12-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49509078","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}

{"title":"DETERMINATION OF EXTERNAL GSS PAYLOAD FROM LIGHT CURVES","authors":"P. Sukhov, V. Yepishev, K. Sukhov","doi":"10.18524/1810-4215.2022.35.268799","DOIUrl":"https://doi.org/10.18524/1810-4215.2022.35.268799","url":null,"abstract":"They are offered reflective features to external surface geostationary satellites on which possible identify the separate external construction geostationary satellites. Such constructions can be; the type and forms radio antennas, solar panels, thermo film on surfaces of the platform. They are given to recommendations and specified moments of time, condition, under which possible find the external payload. The paper presents the results of colorimetric observations of 5 GSS of multipurpose operation, on the platform of which an external payload in the form of several radio antennas was found, and in some cases the orientation and technical characteristics of the GSS were estimated","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":" ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2022-12-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"45453497","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}