Российский фонд
фундаментальных
исследований

Физический факультет
МГУ им. М.В.Ломоносова
 

Публикации Одесской астрономической обсерватории. 2017. 30

 

Bolotin Yu.L., Cherkaskiy V.A., Yanovsky V.V. «Limit values as an universal method of description of physical reality» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 6-12 (2017)

There are two main forms of cognition of Nature: empiric knowledge obtained from the experience, and theory as system of ideas and principles. Each of the two forms uses its own methods. While empirics or phenomenology is based on experiments, theory mostly deals with axiomatic approach. Every axiomatics starts from the principal question: what statements should be chosen as axioms? The present work uses the existence of limit values as the initial axiom. It is well known that the statement about the existence of minimum quantum of action ħ is sufficient to build all the Quantum Mechanics, likewise maxi-mum velocity value c – for the Special Relativity. Similar approach can be realized in General Relativity as well, which can be built on the postulated existence of limit (maximum) power η≪em>c/4G. It seems natural in context of this axiomatics to transit from the traditional Planck’s units to the modified ones, i.e. from the set (ħ, c, G) to (ħ, c, ħ), with the latter containing exclusively limit values. The approach considered in the present paper opens new exciting possibilities for interpretation of the known results and obtaining the new ones.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 6-12 (2017) | Рубрика: 18

 

Bolotin Yu.L., Zazunov L.G., Konchatnyi M.I., Lemets O.A. «The ABC of cosmography» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 13-15 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114129

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 13-15 (2017) | Рубрика: 18

 

Chernin A.D. «ΛGR centennial: cosmic web in dark energy background» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 16-18 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114218 The basic building blocks of the Cosmic Web are groups and clusters of galaxies, superclusters (pancakes) and filaments embedded in the universal dark energy background. The background produces antigravity, and the antigravity effect is strong in groups, clusters and superclusters. Antigravity is very weak in filaments where matter (dark matter and baryons) produces gravity dominating in the filament internal dynamics. Gravity-antigravity interplay on the large scales is a grandiose phenomenon predicted by ΛGR theory and seen in modern observations of the Cosmic Web.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 16-18 (2017) | Рубрика: 18

 

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 Ψemwith 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.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 19-22 (2017) | Рубрика: 18

 

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.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 23-26 (2017) | Рубрика: 18

 

Jenkovszky László, Szanyi István «High-energy diffraction and duality relations» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 27-34 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.115466 Relations between elastic and inelastic diffraction due to Regge factorisation and pomeron dominance are discussed in the light of the new phenomena discovered at the LHC in nearly forward scattering.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 27-34 (2017) | Рубрика: 18

 

Kotvytskiy A.T., Bronza S.D., Shablenko V.Yu. «Correlation of the number of images of an n-point gravitational lens and the number of solutions of its system» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 35-37 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114229. In this paper, we study the correlation between the number of solutions of a system of lens equations and the number of source images that a gravitational lens has. We defined the concept of an image in a gravitational lens. To find the set of solutions of a system of lens equations, we applied methods of algebraic geometry.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 35-37 (2017) | Рубрика: 18

 

Pankov A.A., Tsytrinov A.V. «Spin and model determination of extra neutral gauge bosons at LHC and ILC» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 38-40 (2017)

Heavy neutral gauge Z' bosons are predicted by many models of physics beyond the Standard Model. If a new neutral gauge boson is discovered at the LHC in the clean Drell–Yan channel, the characterization of its spin and couplings will proceed via measuring production rates and angular distributions of the decay products. We study the discrimination between a Z' boson (spin-1) against the Randall–Sundrum graviton resonance (spin-2) and spin-0 resonance (sneutrino) with the same mass and producing the same number of events in the cross section. The next step would be to measure its properties to identify the underlying theory that gave rise to the Z'. We discuss in this context the foreseeable sensitivity to Z's of fermion-pair production observables at the ILC with polarized beams, especially as regards the potential of distinguishing different Z' models once such deviations are observed.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 38-40 (2017) | Рубрики: 17 18

 

Rudakovskyi A.V. «Cores in dark matter haloes with anisotropic Osipkov–Merritt distribution and maximal phase-space density» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 41-44 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114259 This paper describes the developed model of dark matter cored density profiles. This model was recently proposed by Dmytro Iakubovskyi (Iakubovskyi and Rudakovskyi, in preparation). It has only one extra parameter – the maximal value fmax of phase-space distribution function – that turn a cusped Navarro–Frenk–White density profie into a cored one. This paper focuses on the estimation of the influence of velocity anisotropy on the cored density profile by using the Osipkov–Merritt model. The density profiles of the typical dwarf-spheroidal galaxy for different masses of fermionic dark matter particle and different anisotropy parameters ra was calculated. It was obtained that the influence of velocity anisotropy on the cored density profile is small.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 41-44 (2017) | Рубрика: 18

 

Shevchenko S.Yu., Tugay A.V. «Determination of the galaxy cluster orientation using x-ray images by FOCAS method» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 45-47 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114263 In our work we considered orientations of bright X-ray halos of the galaxy clusters (mainly Abell clusters). 78 appropriate clusters were selected using data from Xgal sample of extragalactic objects in XMM-Newton observation archive. Position angles and eccentricities of these halos were calculated applying FOCAS method. No privileged orientations were found.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 45-47 (2017) | Рубрика: 18

 

Stashko O.S., Zhdanov V.I. «Disconnected regions of stable circular orbits in presence of massive scalar field» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 48-50 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114270 We study circular orbits around a static spherically symmetric configuration of General Relativity in presence of a nonlinear massive scalar field (SF). The problem deals with a family of solutions to Einstein – SF equations with the SF potentials that are negative for some SF values in order to consider black hole configurations. We show that, for some parameters of the family, there can exist two disconnected regions of stable circular orbits around the configuration. Such regions can exist both for black hole and fornaked singularities.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 48-50 (2017) | Рубрика: 18

 

Tugay A.V. «Statistical analysis of large-scale structure of Universe» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 51-53 (2017)

While galaxy cluster catalogs were compiled many decades ago, other structural elements of cosmic web are detected at definite level only in the newest works. For example, extragalactic filaments were described by velocity field and SDSS galaxy distribution during the last years. Large-scale structure of the Universe could be also mapped in the future using ATHENA observations in X-rays and SKA in radio band. Until detailed observations are not available for the most volume of Universe, some integral statistical parameters can be used for its description. Such methods as galaxy correlation function, power spectrum, statistical moments and peak statistics are commonly used with this aim. The parameters of powerspectrum and other statistics are important for constraining the models of dark matter, dark energy, inflation and brane cosmology. In the present work we describe the growth of large-scale density fluctuations in one- and three-dimensional case with Fourier harmonics of hydrodynamical parameters. In result we get power-law relation for the matter power spectrum

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 51-53 (2017) | Рубрика: 18

 

Andrievsky S.M., Korotin S.A., Hill V., Zhukova A.V. «Zirconium abundances in the central part of the DsPH Fornax galaxy» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 54-56 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.117154 We derived LTE zirconium abundance in a sample of 81 giant stars in dwarf spheroidal Fornax galaxy. The LTE synthesis was used for this aim. We obtained the lower Zr abundance in Fornax galaxy comparing to the relevant value in the thick/thin disc of the Milky Way. We note that this result may be affected by the NLTE effects that decrease the real zirconium abundance.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 54-56 (2017) | Рубрика: 18

 

Andrych K.D., Andronov I.L., Chinarova L.L. «Statistically optimal modeling of flat eclipses and exoplanet transitions. The "Wall-Supported Polynomial" (WSP) algoritms» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 57-62 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.118521 The methods for determination of the characteristics of the extrema are discussed with an application to irregularly spaced data, which are characteristic for photometrical observations of variable stars. We introduce new special functions, which were named as the “Wall-Supported Polynomial” (WSP) of different orders. It is a parabola (WSP), constant line (WSL) or an “asymptotic” parabola (WSAP) with “walls” corresponding to more inclined descending and ascending branches of the light curve. As the interval is split generally into 3 parts, the approximations may be classified as a “nonpolynomial splines”. These approximations extend a parabolic/linear fit by adding the “walls” with a shape, which asymptotically corresponds to the brightness variations near phases of the inner contact. The fits are compared to that proposed by Andronov (2010, 2012) and Mikulasek (2015) and modified for the case of data near the bottom of eclipses instead of wider intervals of the light curve. The WSL method is preferred for total eclipses showing a brightness standstill. The WSP and WSAP may be generally recommended in a case of transit eclipses, especially by exoplanets. Other two methods, as well as the symmetrical polynomials of statistically optimal order, may be recommended in a general case of non-total eclipses. The method was illustrated by application to observations of a newly discovered eclipsing binary GSC 3692-00624 = 2MASS J01560160+5744488, for which the WSL method provides 12 times better accuracy

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 57-62 (2017) | Рубрика: 18

 

«Ionisation loss and shock excitation of 4420Ca I and 4420Ca II atoms in cold remnants of type II supernovae» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 63-68 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.118314 The light emission (“glow”) of cold dusty plasma of the remnant of SN 1987A was confirmed by the Hubble Space Telescope observations on 7th January, 1995. In particular, Ca I and Ca II lines were recorded and identified in the spectrum of the supernova’s envelope. The period of complete hydrogen recombination in the remnant is 800 days. Thus, it is only radioactive decay that could be a primary source of the plasma light emission at the moment of observation. This paper describes the conditions of shock excitation and recombination of 4420Ca resulted from the decay of radioactive 4422Ti travelling in the remnant’s cold dust. The overionisation in the remnant resulted from the motion of the 4420Ca recoil nucleus, as well as its impact on the spectrum formation, was studied. It has been shown that the calcium lines are formed by the 44Ca Ca II ion in the inner layers of the remnant. We have reached the conclusion that the Ca I/Ca II line strength ratio corresponds to the isotopic abundance ratio [4420Ca] /[4020Ca] in Type II supernova remnants.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 63-68 (2017) | Рубрика: 18

 

Doikov D.N., Savchuk N.V., Yushchenko A.V. «Radioactive molecules in SN1987a remnant» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 69-75 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114273

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 69-75 (2017) | Рубрика: 18

 

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.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 76-77 (2017) | Рубрика: 18

 

Ismailov N.Z., Adigezalzade A.N., Bashirova U.Z. «Circustellar matter activity in AE/BE Herbig star MWC 614» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 78-84 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.117155 The results of spectral observations of the Herbig Ae/Be type star HD 179218 are presented. Two wave-like cycles of variability in the parameters of hydrogen lines Hα and Hβ with a characteristic time of ∼40 days are revealed. The first wave of variations is deeper; the branches of decreasing and increasing the spectral parameters of the lines are more clearly expressed. At the time of the first minimum, in the profile of the emission line Hα the appearance and disappearance of additional blue and red emission components are observed. At the same time, narrow absorption components were discovered in the Hβ line. Possible mechanisms of the observed variability of the star are discussed.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 78-84 (2017) | Рубрика: 18

 

Kolotsey A., Atroschenco M., Dubrouski S.A., Baluk I.I «Updated light elements of 10 RRab stars in the Antlia, Caelum and Sculptor constellations» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 85-88 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.117671 This paper presents the results of verification of the periods and other characteristics of 10 variable stars. The All Sky Automated Survey (ASAS) data have been used in this verification study. 10 RRab stars in the Antlia, Caelum and Sculptor constellations have been investigated. The study was performed using the software package developed by S.A. Dubrouski and V.P. Goranski.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 85-88 (2017) | Рубрика: 18

 

Kondratyev V.N. «Short soft Γ-ray burst spectral evolution» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 89-90 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114279 Short Soft Gamma-Ray bursts are considered as neutron star crust magnetoemission. Statistics of temporal burst properties are shown to display universal features.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 89-90 (2017) | Рубрика: 18

 

Kondratyev V.N., Nurtayeva U.M., Zhomartova A.Zh., Mishenina T.V. «Synthesis of magnetized nuclei at supernova explosion» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 91-92 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114335 Influence of magnetorotational instabilities in astrophysical plasma at supernova explosion on synthesis of chemical elements is investigated. At field strength less than 10 teratesla nuclear magnetic susceptibility exhibits linear regime with enhanced nuclear binding energy for open shell nuclei. Effects of ultra-strong nuclear magnetization are demonstrated to enhance the portion of titanium product. The relation to an excess of titanium isotopes revealed from the Integral mission data and galactic chemical evolution is discussed.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 91-92 (2017) | Рубрика: 18

 

Kudashkina L.S., Andronov I.L. «Phase plane analysis of the photometrical variations of long-period variables» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 93-97 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114346 Using the phase plane diagrams, the phase light curves of a group of the Mira-type stars and semi-regular variables are analyzed. As generalized coordinates х and x-dot, we have used m – the brightness of the star and its phase derivative. We have used mean phase light curves using observations of various authors. The data typically span a large time interval (nearly a century). They were compiled from the databases of AAVSO, AFOEV, VSOLJ, ASAS and approximated using a trigonometric polynomial of statistically optimal degree. As the resulting approximation characterizes the auto oscillation process, which leads to a photometrical variability, the phase diagram corresponds to a limit cycle. For all stars studied, the limit cycles were computed. For a simple sine-like light curve, in e.g., L2 Pup, the limit cycle is a simple ellipse. In a case of more complicated light curve, in which harmonics are statistically significant, the limit cycle has deviations from the ellipse. In an addition to a classical analysis, we use the error estimates of the smoothing function and its derivative to constrain an “error corridor” in the phase plane.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 93-97 (2017) | Рубрика: 18

 

Kuratova A.K., Zakhozhay O.V., Kuratov K.S., Zakhozhay V.A., Miroshnichenko A.S. «Physical parameters of protoplanetary disk surrounding IRAS 22150+6109 young star» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 98-100 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114371

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 98-100 (2017) | Рубрика: 18

 

Maharramov Y.M. «Hα and Hβ profile variations in the spectra of the star 55 Cyg» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 101-107 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114351 We study the variability of the Hα and Hβ lines in the spectra of 55 Cyg based on observations acquired in 2014 on the 2-m telescope of Shamakhy Astrophysical Observatory. In this work line profiles of Hα and Hβ are described extensively and compared with early observations. The profile of Hα line vanishes or almost vanishes in the spectra on some epochs again. Our observations showed that when the Hα line disappeared or weaken sharply in the spectra, the HeI and Hβ line are redshifted, but no synchronous variabilities were observed in other spectral lines (CII and others) formed in deeper layers of the stellar atmosphere. In addition, the profiles of the Hα and Hβ lines have been analysed, as well as their relations with possible conditions of the atmosphere of 55 Cyg. We revealed that the structures of photospheric (CII, HeI etc.) absorption line profiles, as well as Hβ line, their radial velocities and equivalent widths are variable. These events may be associated with a manifestation of the non-stationarity of the atmosphere or non-sphericity of the stellar wind.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 101-107 (2017) | Рубрика: 18

 

Mishenina T., Klochkova V., Panchuk V., Basak N., Kovtyukh V., Korotin S., Velichko A. «Three giants – members of the open cluster M 67» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 108-112 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114355 We determined the atmospheric parameters and chemical composition of the three giants, which are members of the open cluster M 67. The high resolution spectra (R=60 000) were obtained with the echelle spectrograph NES mounted on the 6-metertelescope of the SAO RAS Obtained variations in Na and Zr abundances are within the determination errors. The Li abundance suggest a depletion of Li in the course ofstellar evolution. For studied giants, the iron abundances derived from the neutral and ionized iron lines have not shown any significant discrepancies. The [Ba/Fe] values are close to the solar ones.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 108-112 (2017) | Рубрика: 18

 

Nazarenko V.V., Nazarenko S.V. «3D numerical hydrodynamical models of the precessing thick accretion disk and on- and off-state generations in microquasars» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 113-116 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114365 The thick accretion disk and donor’s wind on the example of CYG X-1 are computed. The main aim of the present simulations is to calculate the precessing thick accretion disk and ON- and OFF-state generation by the methods of 3D numerical hydrodynamics. The main task of the present research is to investigate the dependencies of the central disk temperature and mass accretion rate versus time. Non-stationary Euler’s hydrodynamical equations are resolved by astrophysical variant of large-particle method by Belotserkovskii–Davydov. The ON- and OFF-state generation for the precessing thick accretion disk was setting. The correlation between radio flux and X-ray was setting. Our present calculations also show that in the cases of the thick accretion disk the jet velocities will be close to 0.24–0.26 of light speed (see for instance SS433) and on contrary in the cases of a thin accretion disk jet velocities will be close to 0.98–99 of light speed (see for instance CYG X-1).

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 113-116 (2017) | Рубрика: 18

 

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 Hβ. X-ray variations are well correlated with UV–optical variability and possibly lead by ∼2–3d. The K band lags the J band by about 21.5±2.5d and lags the combined B+J bands by ∼25d. 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.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 117-120 (2017) | Рубрика: 18

 

Panko E.A., Emelyanov S.I. «The peculiarities in O-type galaxy clusters» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 121-123 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114369 We present the results of analysis of 2D distribution of galaxies in galaxy cluster fields. The Catalogue of Galaxy Clusters and Groups PF (Panko–Flin) was used as input observational data set. We selected open rich PF galaxy clusters, containing 100 and more galaxies for our study. According to Panko classification scheme open galaxy clusters (O-type) have no concentration to the cluster center. The data set contains both pure O-type clusters and O-type clusters with overdence belts, namely OL and OF types. According to Rood–Sastry and Struble–Rood ideas, the open galaxy clusters are the beginning stage of cluster evolution. We found in the O-type clusters some types of statistically significant regular peculiarities, such as two crossed belts or curved strip. We suppose founded features connected with galaxy clusters evolution and the distribution of DM inside the clusters.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 121-123 (2017) | Рубрика: 18

 

Plachinda S.I., Butkovskaya V.V. «Stellar activity cycles: why do we need in the long-term measurements of the magnetic field?» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 124-125 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114374 Solution of the two important problems requires a study of long-term behavior of the magnetic field on stars with nondegenerate matter: firstly, to define the role of the magnetic field on different evolutionary stages of stars; secondly, to know the influence of the star’s activity on space weather in the habitable zone. This brief review summarizes the first results of the long-term magnetic field measurements on selected stars.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 124-125 (2017) | Рубрика: 18

 

Savastru S.V., Marsakova V.I., Andrych K.D., Dubovsky P. «Improved ephemeris of poorly studied eclipsing binary GSC 3950-00707 = 2mass J20355082+5242136» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 126-127 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.115819 We made our CCD-observations of GSC 3950-00707 by using the telescope Celestron-14 of Vihorlat Observatory and Astronomical Observatory on Kolonica Saddle. The moments of minima were calculated by using the symmetrical polynomial fit. We also analyzed the observations from automated surveys ASAS-SN and found 3 mean minima by using trigonometrical polynomial fit. The analysis of our observations and data from the surveys allows to conclude that it is the W UMa-type variable and its published period value is not accurate. We analyzed the O–C curve and corrected the elements.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 126-127 (2017) | Рубрика: 18

 

Smerechynskyi S.V., Dzikovskyi D.V. «Model of magnetic degenerate dwarf» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 128-134 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114380 Ключевые слова: degenerate dwarf, critical mass, relativistic parameter, spin-polarization

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 128-134 (2017) | Рубрика: 18

 

Tvardovskyi D.E., Marsakova V.I., Andronov I.L. «Effects of the mass transfer and presence of the third components in close binary stellar systems» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 135-139 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.115463 n our research, we have studied 6 close binary stellar systems which are eclipsing variables of β Lyrae and W Ursae Majoris types of variability. We have studied their O–C curves. To build them, we used moments of minima, listed in the BRNO database. Also, we used ones, which we obtained as the result of processing of observational data taken from AAVSO database. As the result of the O–C analysis, we detected that all of these stars have parabolic O–C curves, which might be caused by mass transfer from one component to another. In an addition, 3 from researched stars (U Peg,V0523 Cas and WZ Cyg) have superimposed parabolic and cyclic O–C changes that could be caused by presence of the third components in the systems. Also, we calculated minimal possible masses of third components, rates of the mass transfer for these systems and corrected the ephemerides.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 135-139 (2017) | Рубрика: 18

 

Udovichenko S.N., Keir L.E. «Photometry and Blazhko effect in RR Lyr-type star AE Leo» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 140-142 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114381 The photometric observations for the RR Lyr-type star AE Leo in the Astronomical station near Odessa using the 48-cm reflector AZT-3 and the CCD photometer equipped with the V filter have been carried out. The light curves shows variable amplitude of light maxima and the moderate Blazhko effect. The analysis of the O–C light maxima for our observations and the ASAS, NSVS data indicates the secular period changes.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 140-142 (2017) | Рубрика: 18

 

Usenko I.A., Kniazev A.Yu., Kovtyukh V.V., Belik S.I., Berdnikov L.N. «Spectroscopical study of faint southern Cepheids with Southern African large telescope (SALT). first results» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 143-145 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.117156 First Cepheids observations using echelle-spectrograph HRS fed by Southern African Large Telescope (SALT) were realized during 2016. All spectra have been obtained in the medium resoltion mode (R≈31000–41000) with high S/N ratio near 50–220. All data were processed using package developed by authors based on the standard system of astronomical data reduction MIDAS. Using new echelle data we found the atmosphere parameters and chemical composition for 30 faint Cepheids of southern hemisphere, where for the most of theses stars these results we obtained for the first time. 28 stars are Cepheids after the first-dredge up stage, while ASAS 075842-25336.1 and ASAS 1131714-6605.0 having remarkable Li I 6707.8 A absorption line and anomalous CNO and Na content could be consider as first crossing of the Cepheids instability strip.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 143-145 (2017) | Рубрика: 18

 

Usenko I.A., Kovtyukh V.V., Miroshnichenko A.S., Danford S. «Pulsational activity of the small-amplitude Cepheid Polaris (α UMi) in 2016–2017» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 146-148 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114382 We present the results of an analysis of 49 spectra of α UMi (Polaris) obtained during August–December 2016 and January–March 2017. Frequency analysis displays an unexpected decrease of the pulsational period up to 17.3min in comparison to the 2015 observational set. The radial velocity amplitude was reduced to 3.43 km s–1 in 2016 and to 3.31km s–1 in the beginning of 2017 in comparison with 4.16 km s–1 in 2015. This result is also unexpected, because during the last decade a gradual amplitude growth has been observed. The average Teff=6021 K determined from the 2016–2017 data is close to the values determined for the 2001–2015 set.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 146-148 (2017) | Рубрика: 18

 

Vavrukh M.V., Dzikovskyi D.V. «The characteristics of electron-nuclear model in the degenerate dwarfs theory. Equation of state» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 149-158 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114384 Within the microscopic theory the ground state energy of spatially homogeneous degenerate relativistic subsystem of electrons in the field of stationary nuclei of l-th sorts with charges z1, . . . , zl was calculated. In the two- and three-particle electron correlations approximation the contributions of Coulomb interactions to the equation of model state at low temperatures was analyzed.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 149-158 (2017) | Рубрика: 18

 

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)

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 159-162 (2017) | Рубрика: 18

 

Dmytrenko A.M., Akhmetov V.S. «Astronomical image processing for high-accurate astrometry data» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 163-165 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114458 This article presents the main results of the initial processing of some of the astronomical images obtained from the archive of the digitized photographic survey of the whole sky SuperCOSMOS. Using of the median filtering and gaussian convolution procedure with the adaptive kernel allows to carry out the initial processing of astronomical images without calibration frames. After the initial processing, the photo centers of the celestial objects were identified by various methods. It has been concluded that after the use of the mathematical methods for the initial processing of the digitized photographic images, the position of objects is calculated with a higher random and systematic precision.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 163-165 (2017) | Рубрика: 18

 

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#.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 166-169 (2017) | Рубрика: 18

 

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.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 170-173 (2017) | Рубрика: 18

 

Kashuba S., Andruk V., Kashuba V. «On the digitisation of Odessa collection of astronomical negatives. Examination of the Epson perfection V 700 photo scanner» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 174-177 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114277 Ключевые слова: astronegative, scanning, processing of digitized plates

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 174-177 (2017) | Рубрика: 18

 

Khramtsov V., Akhmetov V. «Supervised automatic identification of extragalactic sources in the WISExSuperCOSMOS catalogue» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 178-181 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114465 We present new catalogue of ∼8,500,000 extragalactic objects as a result of automatic classification of WISE and SuperCOSMOS (SCOS) cross-identification product. The main goal is to create a set of candidates in extragalactic objects due to colour (photometric) features through machine learning techniques. Extragalactic sources were separated from stars in high-dimensional colour space using Support Vector Machine (SVM) classifier. Construction of catalogue of the extragalactic objects is based on the four important procedures: 1. Cross-identification of the WISExSCOS catalogues. 2. Training set creation (Gaia DR1 and 2MASX\XSC data). 3. Feature engineering and colour-space constructing for further learning and classification. 4. Fine-tuning of SVM and separation and classification processes. In result we got high-accuracy (∼98%) algorithm for extragalactic source identification in built colour space. Product of algorithm realization is presented as photometric catalogue of the extragalactic objects and can be used for further astronomical investigations.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 178-181 (2017) | Рубрика: 18

 

Maigurova N.V., Pomazan A.V., Bodryagin D.V., Bondarchuk L.E. «Accuracy of Mykolaiv asteroid observations with different reference catalogues» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 182-185 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114488 The results of astrometric reductions of main belt asteroid observations with usage of 3 different reference catalogues are presented. The high precision catalogs CMC15, UCAC4 and GAIA DR1 were used as reference catalogues for calculation asteroid equatorial coordinates. The asteroid observations were carried out at KT-50 telescope of the RI “MAO” Mobitel complex during 2016. The array contains 1666.positions of 68 asteroids mainly in range of (11–15) magnitudes. The differences (O–C) were calculated by comparing the obtained topocentric positions with the HORIZONS ephemeredes of the JPL laboratory. The mean square errors of the (O–C) values were used for comparison of the different reductions model. The influence of the choice of the reference catalog on the random and systematic asteroid position errors is shown.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 182-185 (2017) | Рубрика: 18

 

Mullo-Abdolov A., Kokhirova G., Relke H., Yuldoshev Q., Protsyuk Yu., Andruk V. «Investigation of the Microtek ScanMaker 1000XL PLUS scanner of the Institute of astrophysics of the Academy of Sciences of the Republic of Tajikistan» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 186-189 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114407 This work was done to estimate the accuracy of the processing method of photographic plates and the detailed study of the Microtek ScanMaker 1000XL Plus scanner, which plans to be used for the digitizing of about 1600 photographic plates of the Astrophysics Institute of the Academy of Sciences of the Republic of Tajikistan (Dushanbe) recorded for the FON project. For the processing of these photographic plates will be used software created in the LINUX/MIDAS/ROMAFOT environment. Six sequential scans of a single plate (1150, the Pleiades cluster) with a spatial resolution of 1200 dpi were processed to evaluate the repeatability of the scanner's astrometric and photometric errors. The size of photographic plates is 8×8 degrees (30×30 cm or 13000×13000 pixels). The estimated errors of the scanner for the stars brighter than B<13.5m are σxy=±0.054 pixels for the rectangular coordinates and σm=±0.020m for the instrumental magnitudes. The estimated astrometric accuracy of the processing of stellar fields of photographic plates in the system of the Tycho-2 catalogue is σαδ=±0.13".

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 186-189 (2017) | Рубрика: 18

 

Pomazan A.V., Maigurova N.V., Shulga O.V. «The astrometric results of observations of periodical comets at KT-50 telescope in RI “MAO”» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 190-193 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114490 The astrometric results of the observations of 10 periodical comets in 2017 are presented. The observations were made with telescope KT-50 telescope in RI «Mykolaiv Astronomical Observatory». The differences between the measured from observations (O) and calculated from ephemeris (C) positions and their mean square errors (MSE) were calculated. The ephemeris positions were taken from online computation service HORIZONS (JPL NASA, USA). For the measured positions the average MSE values are 0.17" in right ascension and 0.18" in declination respectively. Analysis of the values (О–C) before and after additions of obtained positions to Minor Planet Center (MPC) database revealed a gradual decrease of these differences with respect to the ephemeris. This indicates that the using of the new high-precision positions allows us to refine the calculated ephemeris. As well improvement and lengthening of the astrometric datasets play important role in the modeling of the cometary nongravitational effects.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 190-193 (2017) | Рубрика: 18

 

Savanevych V.E., Briukhovetskyi O.B., Khlamov S.V., Pohorelov A.V., Vlasenko V.P., Dubovsky P.A., Kudzej I., Parimucha Š. «COLITECVS – new tool for automated reduction of photometric observations» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 194-197 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114495 The capabilities of telescopes allow us to make the plotting of light curves a routine task. This one shifts the main attention of astronomer from the plotting to research. To achieve this goal, we developed a new tool for automated reduction of photometric observations, which includes the computational method for the brightness assessment of the investigated and comparison stars; brightness equalization of astronomical images using inverse median filter; light curve plotting and its processing using different tools.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 194-197 (2017) | Рубрика: 18

 

Shatokhina S.V., Kazantseva L.V., Yizhakevych O.M., Eglitis I., Andruk V.M. «Asteroids search results in large photographic Sky Surveys» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 198-200 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114510 Photographic observations of XX century contained numerous and varied information about all objects and events of the Universe fixed on plates. The original and interesting observations of small bodies of the Solar system in previous years can be selected and used for various scientific tasks. Existing databases and online services can help make such selection easily and quickly. The observations of chronologically earlier positions, photometric evaluation of brightness for long periods of time allow refining the orbits of asteroids and identifying various non-stationaries. Photographic observations of Northern Sky Survey project and observations of clusters in UBVR bands were used for global search for small bodies of Solar system. Total we founded 2486 positions of asteroids and 13 positions of comets. All positions were compared with ephemeris. It was found that 80 positions of asteroids have a moment of observation preceding their discovery, and 19 of them are chronologically the earliest observations of these asteroids in the world.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 198-200 (2017) | Рубрика: 18

 

Yizhakevych O., Andruk V., Pakuliak L. «Catalogue of astrometric positions of Jupiter’s outer satellites on photographic observations in MAO NAS of Ukraine in 1987–1993» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 201-204 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114529 The catalog of 33 topocentric positions of Jupiter’s moons J6, J7, J8 has been created on photographic observations made in MAO NASU in 1987–1993. Positions are referred to the system of TYCHO-2 using the program package INUX/MIDAS/ROMAFOT. The comparison of observed positions was made online with their theoretical data of IMCCE (www.imcce.fr/sat).

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 201-204 (2017) | Рубрика: 18

 

Yuldoshev Q.H., Muminov M.M., Ehgamberdiev Sh.A., Relke H., Protsyuk Yu.I., Kovylianska O.E., Protsyuk S.V., Andruk V.M. «Catalogue of coordinates and B-magnitudes in –20° – +2° zone based on the Ulugh Beg Astronomical institute part of the FON project» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 205-208 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114443 Catalogue of 13.4 million stars down to 17.5m was obtained in 2017 by using plates from the Kitab Observatory of Ulugh Beg Astronomical Institute (UBAI) of the Uzbek Academy of Sciences. Kitab's part of Photographic Sky Survey (Russian abbreviation is FON, in next contexts) project include more than 2600 photographic plates, exposed on the Double Astrograph of Zeiss (DAZ, D/F=40/300, 69"/mm) from 1981 to 1996. Digitizationof these plates was made by using Epson Expression 10000XL scanner with the 1200 dpi resolution. Catalogue includes objects from the 1963 plates in declination zone between –20° and +2° for middle epoch 1984.97. The equatorial coordinates of objects were determined in the Tycho-2 reference system and the B-magnitudes in the system of the photoelectric standards. Five participants from Uzbekistan, Germany and Ukraine have taken part in the processing of the digitized images. The average internal accuracy of the catalogue for one observation are 0.23" and 0.15m for the equatorial coordinates and B-magnitudes respectively. For the stars brighter than 14m the errors are 0.09" and 0.05m respectively. The analysis of the catalogue and its comparison with the several astrometric catalogues was done.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 205-208 (2017) | Рубрика: 18

 

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.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 209-218 (2017) | Рубрика: 18

 

Isaeva E.A., Lytvynenko O.A., Shepelev V.A. «Software for adapting DSPZ receivers to the URAN interferometer network» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 219-221 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.115456 More than 10 years ago, URAN interferometer network (Megn A.V.,1997; Konovalenko A.A., 2014) had been equipped with newly designed receivers with a pass band extended up to 250 kHz and software rejection of interferences (Rashkovskii, 2012). The broadening of bandwidth of received signal increase the sensitivity of the receivers significantly and let us to investigate the angular structure about one hundred radio sources. A software package had been developed that allows: preparing a program of observations, carrying out observations automatically, making data cross-correlation, calculating visibility functions for all pairs of antennae, and fitting models of an angular structure of the sources. Data storage formats were elaborated for each stage of recording or processing. At present, new digital radio astronomy receiver DSPZ have been developed by IRA NASU (Zakharenko, 2016). The receiver allows recording an entire bandwidth of signals of a decameter range from 8 to 32 MHz. It is used at UTR-2 and URAN radio telescopes operated in a single dish mode. Application of the receivers for interferometer observation with the URAN network provides additional advantages in accuracy and sensitivity of studies. In this report we consider the data formats and synchronization methods used in URAN equipment and DSPZ receivers, and discuss algorithms of their transformation. Newly elaborated software is described, that allows selecting a set of frequency bands of signals recorded with DSPZ and converting them to the form used by the URAN software. This approach allows us to carry out the interferometer observations in an the extended frequency range provided by DSPZ and to use as much as possible the software package developed for the URAN network for data reduction.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 219-221 (2017) | Рубрика: 18

 

Isaeva E.A., Tsap Yu.T. «Microwave emission of solar flares: coronal mass ejections and shock waves» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 222-225 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114670 Coronal mass ejections (CMEs) mostly affect the geomagnetic field. These structures are observed and studied with coronagraphic images therefore we don’t see the corona in the plane of the sky and the measurements of the propagation speed for solar disk events are not accessible to coronagraphic observations. This suggests that microwave emission of solar flares that can be attributed to the gyrosynchrotron mechanism of mildly relativistic electrons can be used. In turn, the relationship between coronal shock waves and CMEs also remains unclear. The data set that we use in this study is based on microwave (μ) observations of spectral fluxes Fμ at 8.8 GHz obtained with the Radio Solar Telescope Network for the 124 proton solar events . The correlation coefficient r between the CME velocities VCME and integral fluxes of microwave emission ∫Fμdt achieves of about 0.8 while it does not exceed 0.36 between VCME and the shock wave velocities. It has been found the quite strong correlation between the growth rate of microwave emission and the deceleration of frequency drift in the frequency range of 25–180 GHz (r≈0.66). The obtained results suggest that microwave observation can be used to predict VCME and the shock wave generation occurs in the region of flare energy release.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 222-225 (2017) | Рубрика: 18

 

Koshkin N.I., Savanevich V., Pohorelov A., Shakun L., Zhukov V., Korobeynikova E., Strakhova S., Moskalenko S., Kashuba V., Krasnoshchokov A. «Ukrainian database and atlas of light curves of artificial space objects» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 226-229 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.117655 This paper describes the Ukrainian database of long-term photometric observations of resident space objects (RSO). For the purpose of using this database for the outer space monitoring and space situational awareness (SSA) the open internet resource has been developed. The paper shows examples of using the Atlas of light curves of RSO's for analyzing the state of rotation around the center of mass of several active and non-functioning satellites in orbit.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 226-229 (2017) | Рубрика: 18

 

Kulichenko M.O., Shulga O.V., Shulga O.V. «Double station observation of meteors with low baseline in Mykolaiv» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 230-231 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114685 Results of single and double station observations of meteors using TV CCD techniques which were conducted in 2013–2016 in Mykolaiv astronomical observatory (RI MAO) are shown in the article.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 230-231 (2017) | Рубрика: 18

 

Lozitsky V.G., Baranovsky E.A., Lozitska N.I., Tarashchuk V.P. «Estimations of local magnetic fields in solar flares: basic methods and some results» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 232-235 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114690 We consider three methods for estimations of local magnetic fields in solar flares: (1) analysis of bisectors of I±V profiles (Lozitsky, 2015); (2) search for Zeeman-like effects in cores of spectral lines with very low Lande factors, geff≈0.01 (Lozitsky, 1993, 1998); (3) semi-empirical modeling using many spectral lines and two-component models (see, e.g., Lozitsky et al., 2000). We illustrate the application of named methods to different observational data and to different spectral lines. Our main conclusions are following: (a) upper limit of local magnetic fields in solar flares is, at least, ∼104G, (b) such extremely strong fields can occur in very small, spatially unresolved scales, (c) lifetime of such fields is, at least, a few minutes.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 232-235 (2017) | Рубрика: 18

 

Miroshnichenko A.P. «Evolution features of giant sources with linear and break steep radio spectra» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 236-239 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114640 In the framework of the cosmological model ΛM the features of properties of giant radio sources with steep low-frequency spectra of linear (S) and break (C+) types are examined. Our estimates of characteristic age of galaxies and quasars with steep spectrum from the UTR-2 catalogue have values 107–108 years. We consider that steep radio spectra may be formed at the transient injection by synchrotron losses of relativistic electrons. Earlier we have determined two evolution branches in relation of the characteristic age and ratio of emission of torus and accretion disk crown for sources with steep spectra S and C+. To further examination of evolution features of giant sources with steep spectra we consider ratio of emission of radio lobes and accretion disk (and disk crown) versus velocity of jet propagation and characteristic age of these objects. Analysis of obtained relations testifies to periodical activity of giant low frequency steep spectrum radio sources.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 236-239 (2017) | Рубрика: 18

 

Parshina S.S., Tokayeva L.K., Dolgova E.M., Afanas'yeva T.N., Samsonov S.N., Petrova V.D., Vodolagina E.S., Kaplanova T.I., Potapova M.V. «Erythrocytes functional features in the 11-year solar cycle» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 240-241 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114691 There had been studied features of rheological blood failures in patients with unstable angina (UA) in periods of the high (HSA) and low solar activity (LSA) in the 23rd 11-year solar cycle. This category of patients is characterized by prethrombotic blood state, although they don’t have coronary thrombosis. The research aimed to study compensatory mechanisms which block thrombosis development at the solar activity increase. There had been established that the period of the solar activity increasing in the 11-year solar cycle is characterized by an increase of a blood viscosity, comparing with the period of a low solar activity. Though, erythrocytes functional features in this case are compensatory mechanisms – erythrocyte aggregation paradoxically reduced and their deformability increases. It is probably connected with the revealed fibrinogen decrease in the period of the high solar activity. We can see that the change of a solar activity is accompanied not only by the progressing of pathologic processes, but also by an activation of adaptive changes in erythrocyte membrane so0 as to prevent thrombosis. Though, the required compensatory mechanisms were found invalid, which were shown in the decrease of an oxygen delivery to tissues, and the effectiveness decrease of the medical treatment in the period of a HSA.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 240-241 (2017) | Рубрика: 18

 

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.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 242-245 (2017) | Рубрика: 18

 

Sidorenkov N.S., Wilson Ian «Influence of solar retrograde motion on terrestrial processes» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 246-249 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114695 The influence of solar retrograde motion on secular minima of solar activity, volcanic eruptions, climate changes, and other terrestrial processes is investigated. Most collected data suggest that secular minima of solar activity, powerful volcanic eruptions, significant climate changes, and catastrophic earthquakes occur around events of solar retrograde motion.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 246-249 (2017) | Рубрика: 18

 

Voitko A.S., Troianskyi V.V. «Resonances in Saturn's system» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 250-251 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.117157 One of principal tasks of celestial mechanics is study of motion of natural satellites of planets. In this work, the authors have examined resonances in system of satellites and rings of Saturn. They have showed presence of resonances between all the regular satellites and satellites – rings.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 250-251 (2017) | Рубрика: 18

 

Andronov I.L. «Odessa scientific school of researchers of variable stars: from V.P. Tsesevich (1907–1983) to our days» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 252-255 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.118686 The biography of Vladimir Platonovich Tsesevich (11.11.1907–28.10.1983), a leader of the astronomy in Odessa from 1944 to 1983, is briefly reviewed, as well as the directions of study, mainly the highlights of the research of variable stars carried out by the members of the scientific school founded by him. The directions of these studies cover a very wide range of variability types – “magnetic” and “non-magnetic” cataclysmic variables, symbiotic, X-Ray and other interacting binaries, classical eclipsers and “extreme direct impactors”, pulsating variables from DSct and RR through C and RV to SR and M. Improved algorithms and programs have been elaborated for statistically optimal phenomenological and physical modeling. Initially these studies in Odessa were inspired by ("with a capital letter") Vladimir Platonovich Tsesevich. who was a meticulous Scientist and brilliant Educator, thorough Author and the intelligibly explaining Popularizer, persevering Organizer and cheerful Joker – a true Professor and Teacher. He was “the Poet of the Starry Heavens”.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 252-255 (2017) | Рубрика: 18

 

Vavilova I.B. «Scientific astronomical school by professor Volodymyr P. Tsesevich on the physics of variable stars» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 256-262 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.118718 This paper is dedicated to the Prof. Volodymyr Platonovych Tsesevich (1907–1983), an outstanding scientist and legendary personality of the XX century. We describe briefly the Kyiv period of his life and activity taken from his Personal Dossier from the Archive of the Presidium of the NAS of Ukraine. A particular attention is paid to the role by V.P. Tsesevich in the development of astrophysical research at the Main Astronomical Observatory of the Academy of Sciences of UkrSSR, when he served as the Director (19.11.1948–03.05.1951), and to the fruitful cooperation between Kyiv and Odesa astronomers. We present briefly a “tree” of the scientific astronomical school by Prof. V.P. Tsesevich on the physics of stars. The data were obtained from different archives (Astronomical Observatory of the I.I. Mechnikov National University of Odessa, Main Astronomical Observatory of the NAS of Ukraine, Archive of the Vernadsky National Library, Archive of the Russian AS, and other institutions). The full database contains of a brief information on the about 100 representatives of this school as follows: name, title and year of thesis’s defense, past/present affiliation). The scientific school is formed since 1950-s till now having its greatest continuation in the work of such astronomers as N.S. Komarov, V.G. Karetnikov, Yu.S. Romanov, and I.L. Andronov (a branch of this school after V.P. Tsesevich), as well as S.M. Andrievsky as the follower by V.G. Karetnikov and T.V. Mishenina, V.F. Gopka, V.V. Kovtykh as the followers by N.S. Komarov. The given information on the school by V.P. Tsesevich is not absolutely full, for example, 1) there are no the data on thesis’s defense under his supervision before 1948; 2) information on the astronomical school developed by A.M. Stafeev and some other scientists is a very poor; 3) some inaccuracies may be present. We will grateful for all the additions and corrections to update a tree of this scientific school, which played and plays a prominent role in the development of our knowledge on physics of stars.

Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 256-262 (2017) | Рубрики: 03 18