Oknyansky V.L., Gaskell C.M., Huseynov N.A., Mikailov Kh.M., Lipunov V.M., Malanchev N.I., Tsygankov S.S., Gorbovskov E.S., Tatarnikov A.M., Metlov V.G., Shatsky K.L., Brotherton M.B., Kasper D., Du P., Chen X., Burlak M.A., Buckley D.A.H., Rebolo R., Serra-Ricart M., Podesta R., Levato H. «Ulti-wavelength monitoring of the changing-look AGN NGC 2617 during state changes» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 117-120 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114366 Optical and near-infrared photometry, optical spectroscopy, and soft X-ray and UV monitoring of the changing-look active galactic nucleus NGC 2617 show that it continues to have the appearance of a type-1 Seyfert galaxy. An optical light curve for 2010–2017 indicates that the change of type probably occurred between 2010 October and 2012 February and was not related to the brightening in 2013. In 2016 and 2017 NGC 2617 brightened again to a level of activity close to that in 2013 April. However, in 2017 from the end of the March to end of July 2017 it was in very low level and starting to change back to a Seyfert 1.8. We find variations in all passbands and in both the intensities and profiles of the broad Balmer lines. A new displaced emission peak has appeared in H_β. X-ray variations are well correlated with UV–optical variability and possibly lead by ∼2–3^d. The K band lags the J band by about 21.5±2.5^d and lags the combined B+J bands by ∼25^d. J lags B by about 3 d. This could be because J-band variability arises predominantly from the outer part of the accretion disc, while K-band variability is dominated by thermal re-emission by dust. We propose that spectral-type changes are a result of increasing central luminosity causing sublimation of the innermost dust in the hollow bi-conical outflow. We briefly discuss various other possible reasons that might explain the dramatic changes in NGC 2617.

Gladush V.D. «Quantum model of a charged black hole» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 19-22 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114219 A canonical approach for constructing of the classical and quantum description spherically-symmetric con guration gravitational and electromagnetic fields is considered. According to the sign of the square of the Kodama vector, space-time is divided into R-and T-regions. By virtue of the generalized Birkhoff theorem, one can choose coordinate systems such that the desired metric functions in the T-region depend on the time, and in the R-domain on the space coordinate. Then, the initial action for the configuration breaks up into terms describing the fields in the T- and R-regions with the time and space evolutionary variable, respectively. For these regions, Lagrangians of the configuration are constructed, which contain dynamic and non-dynamic degrees of freedom, leading to constrains. We concentrate our attention on dynamic T-regions. There are two additional conserved physical quantities: the charge and the total mass of the system. The Poisson bracket of the total mass with the Hamiltonian function vanishes in the weak sense. A classical solution of the field equations in the configuration space (minisuperspace) is constructed without fixing non-dynamic variable. In the framework of the canonical approach to the quantum mechanics of the system under consideration, physical states are found by solving the Hamiltonian constraint in the operator form (the DeWitt equation) for the system wave function Ψ. It also requires that Ψ is an eigenfunction of the operators of charge and total mass. For the symmetric of the mass operator the corresponding ordering of operators is carried out. Since the total mass operator commutes with the Hamiltonian in the weak sense, its eigenfunctions must be constructed in conjunction with the solution of the DeWitt equation. The consistency condition leads to the ansatz, with the help of which the solution of the DeWitt equation for the state Ψ_emwith a defined total mass and charge is constructed, taking into account the regularity condition on the horizon. The mass and charge spectra of the configuration in this approach turn out to be continuous. It is interesting that formal quantization in the R-region with a space evolutionary coordinate leads to a similar result.

Holovko M.G., Gladush V.D. «Quantization of the spherically symmetric configuration of the gravitational and electromagnetic fields» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 23-26 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114223 To construct a quantum model of a charged black hole (CBH), we introduce a modified description of the configuration of the electromagnetic and gravitational fields in a spherically symmetric space-time, which consists of T- and R- regions. We choose such coordinate system that the desired metric functions depend only on the time coordinate in the T-region, and on the space coordinate in the R-region. Then, the initial action for the configuration decays into terms which describe the fields in the T- and R-regions with the time and the space evolutionary coordinate respectively. We define new coordinates in the R- and T- regions, what allows us to unify the form of the Lagrangians, in each of them and carry out their uniform analysis. Then we construct the canonical formalism for obtained degenerate system according to the method of D.M. Gitman and I.V. Tyutin. It appears that system contains non-physical degrees of freedom. For their expicit separation we carry out the canonical transformation to new canonical variables. In these variables the constraints are reduced to the canonical form and physical part of the Hamilton function of the system is identically equal to zero. This leads to the fact that the desired wave function is determined only by the eigenvalue equations for the operators of observable physical quantities. According that considered system has only two observables – charge and mass of black hole – for further construction of quantum model of this system we introduce its mass and charge functions and find their expression in the new canonical variables. The solution of eigenvalue equations for corresponding operators leads to continuous spectra of charge and mass in considered model of CBH.

Golovashchenko V.A., Kolomiyets S.V. «Meteor observational data visualisation in the equatorial coordinate system using information technology» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 166-169 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.115454 As a result of dynamic evolution of IT industry and astronomical research in the XXI century, which have resulted in obtaining large and complex data sets known as Big Data (e.g. data from the European Space Agency missions, such as GAIA mission, etc.), as well as due to rapid development of computer technologies, astronomy and computer science have become closely linked to each other. In the XXI century, Information technology has become an essential part of understanding the world around. This paper presents a solution to the problem of meteor data representation in the second equatorial coordinate (RA-Dec) system using Information Technology. Such a visualisation solution is needed to analyse the results of experiments based on the radar observations conducted in 1972–1978 (stage 1 – the data obtained in 1972 comprise 10,247 meteor orbits), which have been accumulated and stored in the Meteor Database of the Kharkiv National University of Radio Electronics (KNURE). A sample set of data with their characteristicsand details about their delivery has been presented by (Kashcheyev–Tkachuk, 1980). An electronic calculator application was developed by employing the model of data visualisation in the form of celestial hemispheres using the object-oriented programming language C#.

Andruk V., Yuldoshev Q., Eglitis I., Pakuliak L., Mullo-Abdolov A., Vaviliva I., Protsyuk Yu., Relke H., Golovnia V., Shatokhina S., Yizhakevych O., Ehgamberdiev Sh., Muminov M., Kokhirova G., Kazantseva L. «On the concept of the enhanced FON catalog compilation» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 159-162 (2017)

Golovnia V., Yizhakevych O., Shatokhina S., Andruk V. «Photographic observations of solar system bodies at the Main astronomical observatory of NAS of Ukraine: final results» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 170-173 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114463 Astrometric photographic observations of Solar system bodies in the frame of different programs were made at MAO NAN of Ukraine during 1950–2005. 9245 plates with the images of planets and their natural satellite, Moon, minor planets, comets and artificial satellites were obtained and processed in the late 20th century. At the beginning of the 21st century, the UkrVO Joint Digital Archive (JDA) was created, which is accessible at the МAO NAS resources (http://gua.db.ukr-vo.org/archivespecial.php). To digitize the plate archive for the JDA database, flat bed scanners were used and the software was specially developed on the basis of the LINUX/MIDAS/ROMAFOT software for the processing of wide-field images, as well as searching for the images of minor planets and comets on the Northern sky survey program plates. Up to the present time, the photographic plates with images of outer planets and their satellites have been re-processed. The final result of the long-lasting program of the photographic positional observations of Solar system bodies are summarized and presented in this publication.

Gorbanev Yu.M., Stogneeva I.A., Shestopalov V.A., Knyazkova E.F., Kimakovskaya I.I., Kimakovsky S.R., Golubaev A.V. «The effect of major meteor streams on the total ozone in the earth's atmosphere» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 209-218 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114643 The correlation between the total ozone and activity of major meteor streams, such as the Perseids, Geminids, Leonids and Orionids, has been found using the Total Ozone Mapping Spectrometer (TOMS) measurements of the global ozone distribution over the periods 1978–1993 and 1996–2001. The autocorrelation analysis of the total ozone time series for the period of about 20 years has confirmed the existence of regular changes in the ozone levels at the peaks of meteor shower activity. It has been established that TO decreases after the dates of peak activity of meteor streams (e.g. the Perseids) or during the whole periods of meteor shower activity (e.g. the Geminids, Orionids and Leonids). The analysis of the total ozone distribution (in the Southern and Northern Hemispheres), as well as the local distribution of ozone (over the selected surface area of several hundred square kilometres), was performed during the Leonid meteor shower in 1999. The atmospheric zones for which the ozone distribution pattern can be described as a result of interaction between the meteor shower material and the ozone layer were localised by applying the TOMS data. Such zones correspond to the regions where the highest Leonid activity has been observed. According to the radar observations (conducted in Kazan, Russian Federation), three activity maxima of the 1988 Geminid shower were reported: on the nights of 7, 12 and 14th December, 1988. The TO decrease was observed on the same dates. Thus, the analysis of the TO changes during the periods of intense meteor shower’s activity enables to preliminary assess the maximum overall decline in the total ozone concentration which makes about 5 DU over two weeks. From the results obtained it can be inferred that the ozone layer can be used as an indicator of the interaction between the meteoric material and the Earth’s atmosphere.

Shakun L., Koshkin N., Korobeynikova E., Strakhova S., Dragomiretsky V., Ryabov A., Melikyants S., Golubovskaya T., Terpan S. «Accuracy of satellite optical observations and precise orbit determination» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 242-245 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.117660 The monitoring of low-orbit space objects (LEO-objects) is performed in the Astronomical Observatory of Odessa I.I. Mechnikov National University (Ukraine) for many years. Decades-long arсhives of these observations are accessible within Ukrainian network of optical observers (UMOS). In this work, we give an example of orbit determination for the satellite with the 1500-km height of orbit based on angular observations in our observatory (Int. No. 086). For estimation of the measurement accuracy and accuracy of determination and propagation of satellite position, we analyze the observations of Ajisai satellite with the well-determined orbit. This allows making justified conclusions not only about random errors of separate measurements, but also to analyze the presence of systematic errors, including external ones to the measurement process. We have shown that the accuracy of one measurement has the standard deviation about 1 arcsec across the track and 1.4 arcsec along the track and systematical shifts in measurements of one track do not exceed 0.45 arcsec. Ajisai position in the interval of the orbit fitting is predicted with accuracy better than 30 m along the orbit and better than 10 m across the orbit for any its point.

Gorbanev Yu.M., Stogneeva I.A., Shestopalov V.A., Knyazkova E.F., Kimakovskaya I.I., Kimakovsky S.R., Golubaev A.V. «The effect of major meteor streams on the total ozone in the earth's atmosphere» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 209-218 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114643 The correlation between the total ozone and activity of major meteor streams, such as the Perseids, Geminids, Leonids and Orionids, has been found using the Total Ozone Mapping Spectrometer (TOMS) measurements of the global ozone distribution over the periods 1978–1993 and 1996–2001. The autocorrelation analysis of the total ozone time series for the period of about 20 years has confirmed the existence of regular changes in the ozone levels at the peaks of meteor shower activity. It has been established that TO decreases after the dates of peak activity of meteor streams (e.g. the Perseids) or during the whole periods of meteor shower activity (e.g. the Geminids, Orionids and Leonids). The analysis of the total ozone distribution (in the Southern and Northern Hemispheres), as well as the local distribution of ozone (over the selected surface area of several hundred square kilometres), was performed during the Leonid meteor shower in 1999. The atmospheric zones for which the ozone distribution pattern can be described as a result of interaction between the meteor shower material and the ozone layer were localised by applying the TOMS data. Such zones correspond to the regions where the highest Leonid activity has been observed. According to the radar observations (conducted in Kazan, Russian Federation), three activity maxima of the 1988 Geminid shower were reported: on the nights of 7, 12 and 14th December, 1988. The TO decrease was observed on the same dates. Thus, the analysis of the TO changes during the periods of intense meteor shower’s activity enables to preliminary assess the maximum overall decline in the total ozone concentration which makes about 5 DU over two weeks. From the results obtained it can be inferred that the ozone layer can be used as an indicator of the interaction between the meteoric material and the Earth’s atmosphere.

Gorbaneva T.I., Mishenina T.V. «Molybdenum and ruthenium abundances in cool stars of the galactic disc» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 76-77 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114274 We revise the molybdenum and ruthenium abundances in FGK stars with metallicities ranging from –1.0 < [Fe/H] < +0.3. The observed stars belong to the substructures of the Galaxy. The observations were conducted using the 1.93 m telescope at Observatoire de Haute–Provence (OHP, France) equipped with the echelle type spectrographs ELODIE and SOPHIE. The results are based on analyses of spectra that have a typical S/N ∼100–300 and a resolution of 42 000. These estimates were obtained using synthetic spectra computed with LTE model atmosphere.

Oknyansky V.L., Gaskell C.M., Huseynov N.A., Mikailov Kh.M., Lipunov V.M., Malanchev N.I., Tsygankov S.S., Gorbovskov E.S., Tatarnikov A.M., Metlov V.G., Shatsky K.L., Brotherton M.B., Kasper D., Du P., Chen X., Burlak M.A., Buckley D.A.H., Rebolo R., Serra-Ricart M., Podesta R., Levato H. «Ulti-wavelength monitoring of the changing-look AGN NGC 2617 during state changes» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 117-120 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114366 Optical and near-infrared photometry, optical spectroscopy, and soft X-ray and UV monitoring of the changing-look active galactic nucleus NGC 2617 show that it continues to have the appearance of a type-1 Seyfert galaxy. An optical light curve for 2010–2017 indicates that the change of type probably occurred between 2010 October and 2012 February and was not related to the brightening in 2013. In 2016 and 2017 NGC 2617 brightened again to a level of activity close to that in 2013 April. However, in 2017 from the end of the March to end of July 2017 it was in very low level and starting to change back to a Seyfert 1.8. We find variations in all passbands and in both the intensities and profiles of the broad Balmer lines. A new displaced emission peak has appeared in H_β. X-ray variations are well correlated with UV–optical variability and possibly lead by ∼2–3^d. The K band lags the J band by about 21.5±2.5^d and lags the combined B+J bands by ∼25^d. J lags B by about 3 d. This could be because J-band variability arises predominantly from the outer part of the accretion disc, while K-band variability is dominated by thermal re-emission by dust. We propose that spectral-type changes are a result of increasing central luminosity causing sublimation of the innermost dust in the hollow bi-conical outflow. We briefly discuss various other possible reasons that might explain the dramatic changes in NGC 2617.