Odessa Astronomical Publications最新文献

{"title":"TWO TOOLS FOR ESTIMATING STAR CLUSTER PARAMETERS","authors":"E. Paunzen, M. Piecka, J. Supíková","doi":"10.18524/1810-4215.2023.36.291233","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.291233","url":null,"abstract":"A star cluster is a composition of stars held together by the overall gravitational field of the whole cluster. The stars of a given cluster are born in a giant molecular cloud and, as such, can be regarded as objects with almost equal ages. Furthermore, assuming that the initial material in the cloud is perfectly mixed, we may also say that the metallicity of all cluster members is the same. Four parameters (distance, extinction or reddening, age, and metallicity) are standardly used to describe star clusters. Their knowledge is essential for studying galaxies’ local and global properties (especially our own Galaxy). However, deriving these parameters may take time and effort. Thanks to the Gaia mission’s parallax measurements, we can determine the distances of stars (and clusters) within our Galaxy with unprecedented precision. Therefore, we can remove the distance from the list of free parameters. We developed two different tools for estimating cluster parameters: 1) Metalcode, an automatic tool focused on deriving metallicities of open clusters, and 2) Stellar Isochrone Fitting Tool (StIFT), a tool for fitting a grid of isochrones for any photometric system available. We present both tools in more detail.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"62 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139011945","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":"TOWARDS THEORETICAL MODELLING OF DISTRIBUTION OF MATTER IN UNIVERSE","authors":"O. I. Gerasymov, L. S. Kudashkina","doi":"10.18524/1810-4215.2023.36.290808","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290808","url":null,"abstract":"The description of the distribution of matter in the universe requires not only accurate observations but also adequate approaches to their theoretical interpretation. This paper proposes a method of parameterization of distributions with a morphologically complex topology using structural invariants (for example, Euler), based on which it is possible to distinguish clusters with different topologies (in the observation plane). Based on the introduced classification and appropriate scaling, it becomes possible to estimate the distribution of matter, for example, within the framework of the mean-field model. To study the kinetics of the evolution of matter distribution, it is proposed to introduce the appropriate ordering parameter, which is built based on the calibrating and current values of the Euler-Poincaré invariants. This approach, by constructing phase diagrams for the ordering parameter, allows you to track the details of the kinetics of the evolution of matter distributions, studying, in particular, the temporal hierarchy of relaxation times of intermediate states. The temporal kinetics of this approach are described using simple kinetic equations that describe the relaxation of the ordering parameter field, and the values of invariants determined with the help of appropriate measurements (observations) appear as initial conditions. This approach can be seen as an alternative to other approaches to parameterization of structurally complex systems, such as Voronoi methods, graphs, etc. A comparative analysis of the results of various alternative approaches to the parameterization of topologically complex distributions of matter, which will be conducted in the future, should contribute to the deepening of existing ideas about the nature of the distribution of matter in the Universe.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"15 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012242","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 THE TEMPERATURES OF THE CENTRAL STARS OF SELECTED PLANETARY NEBULAE","authors":"A. H. Alili, K. Alisheva, Kh. M. Mikailov","doi":"10.18524/1810-4215.2023.36.290929","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290929","url":null,"abstract":"In this work, for planetary nebulae İC 1295, İC 4191, Zanstra temperatures were calculated using the Hβ line of the central stars. Respectively, the temperatures 64252 K and 47663 K were determined. The flux in the Hβ radiative line used in the calculations, has been determined from the spectra retrieved from the archive of the European Southern Observatory. Our results have been compared with results of the other authors.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"328 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012254","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":"LIGHT CURVE ANALYSIS OF SIX MAIN BELT ASTEROIDS WITH EARTH MOID LESS THAN 1AU","authors":"I. Eglitis, K. Nagainis, A. Sokolova, G. Campbell","doi":"10.18524/1810-4215.2023.36.290220","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290220","url":null,"abstract":"Six main belt asteroids 1999 HK1 (11411), 1995 AM1 (30968), 1999 XC136 (53454), 1999 JN6 (70055), 1999 UQ9 (86280), 2000 SU2 (93041) with Earth MOID less than 1AU were studied at the Baldone Astrophysical Observatory of the Institute of Astronomy of the University of Latvia in the time span range 2020-2022. The obtained light curve data together with published Minor Planet Center data in the time range 1999-2022 were analyzed with Fourier series, Lomb-Scargle periodogram, and Phase dispersion minimization methods. A plan of analysis step by step is given. The results computed from different observatories' data are compared and mean-weighted periods are obtained. The rotation periods are for asteroids: N11411 P = 6.544 h, N30968 P = 8.330 h, N53454 P = 4.615 h, N70055 P = 74.364 h, N86280 P = 1.315 or 6.658 h and N93041 P = 30.645 h.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"8 12","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012274","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 Hα AND Hβ LINES IN THE SPECTRUM OF CH CYG IN 2016","authors":"Kh. M. Mikailov, B. Rustamov, A. B. Rustamova, A. J. Orujova","doi":"10.18524/1810-4215.2023.36.290040","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290040","url":null,"abstract":"We present the results of spectral observations of the symbiotic star CH Cyg, carried out at the Cassegrain focus of the 2-m telescope of the ShAO named after N. Tusi, by using the Shamakhy Fiber Echelle Spectrograph (ShAFES). The spectra of star CH Cyg were obtained with the spectral resolution of R = 28000, between June and November 2016. We also present the results of the comparative analysis of the brightness curve of the star with the main parameters of Hα and Hβ emission lines. During the observation period, both lines exhibited changing profiles characterized by complex structures, predominantly with double peaks. The ratio of the intensities of the blue and red components was typically IB/IR < 1 for the Hα line and IB/IR ≥ 1 for the Hβ line. A quasi-period of 241 days was found in the variation of the equivalent widths of Hα and Hβ emission lines as well as in the intensities of their components.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"41 13","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139011964","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 RELATIONSHIP OF THE INTENSITY OF THE SCR PROTON FLUX WITH THE PARAMETERS OF TYPE II SOLAR RADIO BURSTS","authors":"E. A. Isaeva","doi":"10.18524/1810-4215.2023.36.290196","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290196","url":null,"abstract":"112 solar proton events (SPEs) were processed for the period from November 24, 2000 to December 20, 2014, which were accompanied by type II radio bursts. For the analysis, used original records of solar radio emission from a solar radio spectrograph in the range of 25-180 MHz, as well as original records of the flux intensity proton of solar cosmic rays (SCR) protons Ip with energy Ep in the range > 0.8-850 MeV according to data from the GOES series of devices. In this case, superimposed proton events were always separated and identified with the corresponding solar proton flares, and the maximum proton flux intensity Ip of superimposed proton events was determined from the level of the previous proton event.\u0000Based on data from the solar radio spectrograph, regression models were obtained for 91 type II bursts that established the relationship between the frequency drift velocity Vi,j and the frequency of type II bursts fi,j, and for 73 type II bursts it was possible to obtain regression models which established the relationship between the intensity of type II bursts Ii,j and type II burst frequency fi,j in the range 25-180 MHz. Detailed studies have shown that the intensity of type II bursts Ii,j, as well as the frequency drift velocity Vi,j, strongly depends on the frequency of type II burst fi,j and monotonically changes with time ti along the harmonics of type II bursts.\u0000As a result, the relationship between the maximum values of the SCR proton flux intensity Ip and the calculated values of the frequency drift velocity Vi,j and intensity of type II bursts Ii,j was investigated. A comparative analysis showed that the relationship between the intensity of the SCR proton flux Ip and the intensity of type II bursts Ii,j is much stronger than with the frequency drift velocity Vi,j, where the correlation coefficient r is 0.82 and 0.71, respectively, for protons with energies Ep > 30 MeV. The relationship between the proton flux intensity Ip and the frequency drift velocity Vi,j and the intensity of type II bursts Ii,j was also studied as a function of the proton energy Ep and the frequency fi,j of type II radio bursts. It was shown that the strongest relationship between the intensity of the SCR proton flux Ip with the frequency drift velocity Vi and with the intensity of type II bursts Ii,j is observed with subrelativistic SCR protons with energies Ep in the range > 30-100 MeV and for type II radio bursts at a frequency fi,j in the range 40-160 MHz.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"137 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012403","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":"ANOMALOUS MAGNETIC REGIONS ON THE SUN","authors":"N. N. Kondrashova, V. Krivodubskij","doi":"10.18524/1810-4215.2023.36.290216","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290216","url":null,"abstract":"We studied the anomalous magnetic regions observed near the minima of solar cycles 24 and 25. The peculiarity of these areas was the deviation of their configuration from Hale's law of magnetic polarity and Joy's law about the inclination of the axes of bipolar groups to the latitudinal direction. Therefore, they belong to the class of so-called anti-Hale active regions. We paid special attention to the flare activity of anti-Hale regions, as this is important for forecasting space weather and magnetic storms in the Earth's atmosphere.\u0000The detected anomalies of the surface magnetism of the active regions studied by us may indicate the influence of the mechanisms of the deep small-scale dynamo on their evolution. In this regard we analyzed the possible mechanisms of the formation of anti-Hale magnetic regions. In particular, such mechanisms can be the mechanisms of a small-scale magnetic dynamo. In connection with this an urgent problem today is the search for observed evidence of the existence of the theoretically proposed by Brandenburg A. et al. (2012) of a new physical entity – a small-scale magnetic field hidden in the solar depths, excited by two qualitatively different mechanisms of a small-scale dynamo (SSD). The first mechanism is the SSD of macroscopic MHD (SSD1), while the second is the diffusion SSD of classical MHD (SSD2). However, the small contributions of these sources are very difficult to distinguish observationally. To solve this complication, Sokoloff, Khlystova and Abramenko (2015) proposed a test for separating the contributions of two sources based on a statistical probabilistic model. Such an important feature of the differences between of the two SSD is the behavior of the percentage of anti-Hail groups of sunspots (in relation to the total number of spots) in the minima of solar cycles. According to statistical studies of long series of observations Sokoloff, Khlystova and Abramenko (2015) found that the percentage of anti-Haile groups of spots increases during minima of the solar cycles, suggesting in favor of SSD2.\u0000We believe that the detected magnetic anomalies of the studied regions may be caused by the influence of a SSD2 in the depths of the convective zone of the Sun, since this source gives the most noticeable contribution to the surface magnetism near cycle minima.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"27 11","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012571","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":"MANIFESTATION OF STELLAR EVOLUTION IN METAL-DEFICIENT STARS","authors":"T. Mishenina, I. Usenko, A. Kniazev, T. Gorbaneva","doi":"10.18524/1810-4215.2023.36.290042","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290042","url":null,"abstract":"Metal-poor stars allow us to establish the early history of the Milky Way, furthermore the stars on advanced evolution stage (e.g. giants, AGB stars etc.) give the opportunity to research the peculiarities of stellar evolution at low metallicity. On the base of the 11-m Southern African Large Telescope (SALT) spectra obtained using HRS fibre-fed echelle-spectrograph during 2018–2020, the atmospheric parameters and elemental abundances of four metal-poor stars HE 1523-0901, HD 6268, HD 121135, and HD 195636 ( [Fe/H] ~ -1.5 – -3.0) have been obtained. The iron abundance was determined based on the equivalent widths of absorption lines. The carbon abundance was obtained using the molecular synthesis fitting for the CH (4300-4330 ÅÅ) region, nitrogen from CN at 3883 Å, oxygen from [O] line at 6300 Å and IR triplet at 7770 Å The relationship between the chemical enrichment of stars and their stellar evolution is considered. It may be associated with the processes of mixing inside the stars, and the mechanisms of matter transfer during stellar evolution.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"9 11","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012205","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 JET KINETIC LUMINOSITIES FOR THE UTR-2 SOURCES WITH THE STEEP LOW-FREQUENCY SPECTRA","authors":"A. P. Miroshnichenko","doi":"10.18524/1810-4215.2023.36.290137","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290137","url":null,"abstract":"Earlier we have determined that the UTR-2 radio sources with steep linear spectra possess greater jet propagation velocity and lesser characteristic age than the UTR-2 radio sources with steep break spectra. Also examined galaxies and quasars with steep break spectra display greater mean values of the central black hole masses and mass accretion rates, than corresponding these for galaxies and quasars with steep linear spectra. Besides, as we have determined, the radio structure of the UTR-2 steep-spectrum sources is giant, its linear size has Mpc-scale. The source’s giant structure is formed by jets with enveloped radio lobes. So, this indicates on the powerful jets of the radio sources with the steep low-frequency spectra. Since the source jets are connected with the accretion disk of the source, it is important to examine relations of their physical characteristics. With this purpose we obtain estimates of the jet kinetic luminosity for the UTR-2 steep-spectrum sources on the assumption of the equality of the corresponding mass accretion rate and the jet matter flux. Using our calculated values of the jet propagation velocity and the mass accretion rate for the UTR-2 steep-spectrum galaxies and quasars, we estimate their jet kinetic luminosities. The obtained values of the jet kinetic luminosities are ~ 1045 erg/s, pointing out the great power of jets for the examined steep-spectrum sources. It is essential, that the examined objects display the relation of their kinetic luminosity and corresponding redshift (cosmological evolution).","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"312 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012289","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":"COLOR-INDEX DETERMINATION OF LEO SATELLITES USING COLOR IP-CAMERAS","authors":"M. O. Kulichenko, Y. Kozyryev, N. Maigurova, O. Shulga","doi":"10.18524/1810-4215.2023.36.290925","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290925","url":null,"abstract":"The study is devoted to determining the color characteristics of the structural surfaces of artificial satellites. Observations of satellites were carried out in automatic mode using software for detection fast moving object, developed at RI “MAO”. The satellite observations equipment consists of Canon EF 85mm f/1.8 USM photographic lens and professional VIVOTEK IP816A-HP network camera. The camera is directed to the zenith and has a field of view (4.9°х2.8°). The camera has progressive CMOS sensor with Bayer color filter⁰₀ array for producing RGB color image. Coordinate and photometric processing of saved images is carried out using SExtractor and Astrometry.net software along with additional Python scripts. In this paper, we present first results of our LEO satellites observations using network IP-cameras with RGB Bayer filter. To convert the instrumental magnitudes from RGB Bayer system into standard bp/rp magnitudes of the Gaia EDR3 photometric system, a system of equations was solved, where the calculated magnitudes in the bp/rp photometric system were represented as functions of magnitudes and colors in the instrumental RGB system. The mean differences between the calculated magnitudes and the catalog magnitudes are (0.03±0.15)mag and (0.01±0.16)mag for bp and rp band, respectively. The calculated Brjb_bp and Rrjb_rp magnitudes using obtained transformation coefficients show a good linear correlation with the bp and rp Gaia EDR3 magnitudes. Only main sequence’s stars in the range of (5-13)mag were used as reference stars for determining the transformation coefficients. The results of determining the color indexes (Brjb_bp - Rrjb_rp) for 8 LEO satellites with the obtained transformation coefficients were received. The average accuracy of the obtained values of color indexes is about 0.2mag.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"5 9","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012337","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}