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This paper presents the results of acomparative analysis of the relationship between solarcosmic rays (SCR), coronal mass ejections (CME), andcoronal shock waves (CSW) with the parameters of solarcontinual type IV radio bursts, as well as with the parame-ters of type II radio bursts. The sample under study con-tains 147 proton events accompanied by type IV continu-um radio bursts in the 25-15400 MHz range, type II radiobursts in the 25-180 MHz range, as well as CME and cor-onal shock waves. For the analysis, we used original rec-ords of solar radio emission at 8 fixed frequencies in therange 245-15400 MHz according to data from RSTN (Ra-dio Solar Telescope Network), original records of dynam-ic spectra from SRS (Solar Radio Spectrograph) in therange of 25-180 MHz, as well as original records intensityof the flux of SCR protons with proton energies in therange> 1-100 MeV according to data from the GOESspacecraft. A comparative analysis showed that the rela-tionship between the intensity of the SCR proton flux andthe CME velocity is, on average, much stronger with theparameters of type IV radio bursts than with the parame-ters of type II radio bursts, which indicates the dominantrole of the SCR acceleration process in the flare region,rather than shock waves. However, detailed studies of thefine structure of type II radio bursts have shown that thereis a fairly strong relationship between the intensity of theflux of mean-relativistic protons I p and the frequency f min,1at the fundamental harmonic (at the 1-st harmonic) at thetime t min corresponding to the minimum relative distanceb min between the harmonics of type II radio bursts. De-tailed studies of the fine structure of type II radio burstshave also shown that there is a strong relationship betweenthe intensity of the SCR proton flux I p and parameter V II ,which characterizes the displacement of the shock frontwith time t i in a narrow frequency range of 25-60 MHz, This paper presents the results of acomparative analysis of the relationship between solarcosmic rays (SCR), coronal mass ejections (CME), andcoronal shock waves (CSW) with the parameters of solarcontinual type IV radio bursts, as well as with the parame-ters of type II radio bursts. The sample under study con-tains 147 proton events accompanied by type IV continu-um radio bursts in the 25-15400 MHz range, type II radiobursts in the 25-180 MHz range, as well as CME and cor-onal shock waves. For the analysis, we used original rec-ords of solar radio emission at 8 fixed frequencies in therange 245-15400 MHz according to data from RSTN (Ra-dio Solar Telescope Network), original records of dynam-ic spectra from SRS (Solar Radio Spectrograph) in therange of 25-180 MHz, as well as original records intensityof the flux of SCR protons with proton energies in therange> 1-100 MeV according to data from the GOESspacecraft. A comparative analysis showed that the rela-tionship between the intensity of the SCR proton flux andthe CME velocity is, on average, much stronger with theparameters of type IV radio bursts than with the parame-ters of type II radio bursts, which indicates the dominantrole of the SCR acceleration process in the flare region,rather than shock waves. However, detailed studies of thefine structure of type II radio bursts have shown that thereis a fairly strong relationship between the intensity of theflux of mean-relativistic protons I p and the frequency f min,1at the fundamental harmonic (at the 1-st harmonic) at thetime t min corresponding to the minimum relative distanceb min between the harmonics of type II radio bursts. De-tailed studies of the fine structure of type II radio burstshave also shown that there is a strong relationship betweenthe intensity of the SCR proton flux I p and parameter V II ,which characterizes the displacement of the shock frontwith time t i in a narrow frequency range of 25-60 MHz.

In a recent paper, the model of thegalaxy with hot dark matter was considered. Thegalaxy is divided into the inner region with thedominant baryonic matter (the elliptic orbit of the testparticle) and the outer region with the dominant hotdark matter (the parabolic orbit of the test particle).It was assumed that the hot dark matter consists ofhypothetical Planck neutrinos arising in the decayof the protons at the Planck scale. Galaxies formedfrom the baryonic matter, and the hot dark matterappears in the galaxies later. The rotation curvesof the galaxies were studied in the model, includingMilky Way, M33, NGC 2366 and IC 2574. In thepresent paper, the hot dark matter model is furtherinvestigated, with the application to M31, the systemof M31 and the Milky Way, the globular clustersNGC 2419 and MGC1, the dwarf spheroidal galaxySculptor, ultra-massive quiescent galaxies from theCOSMOS and UDS fields. The baryonic matter massof M31 was estimated from the rotation curves, withthe average value 1.6 × 10 11 m ? . The gravitationalinteraction of the Milky Way and M31 is considered.In the hot dark matter model, the dynamical massesof the Milky Way and M31 are twice their baryonicmatter masses that gives the radial velocity of M31toward the Milky Way, 106 km s −1 . The hot darkmatter mass in the globular clusters NGC 2419 andMGC1 is estimated. The value is small comparedto the stellar mass in both the clusters. The hotdark matter mass within the half-light radius ofthe dwarf spheroidal galaxy Sculptor is estimated,0.5 × 10 6 m ? . The sum of the stellar and hot darkmatter mass within the half-light radius is consistentwith the dynamical mass within the half-light radiusof the Sculptor derived from the kinematics of themetal rich stars. The instability of the baryonicmatter due to the influence of the hot dark matterand some perturbations flattens the velocity profileof the metal poor stars which is unsuitable to derivethe dynamical mass. The evolution of ultra-massivequiescent galaxies from the COSMOS and UDS fieldsis considered. The dynamical to stellar mass relationis doubling during the evolution from z = 2 to 0 thatcan be explained by the absence of dark matter atz = 2 and the presence of the hot dark matter atz = 0., e outer region with the dominant hotdark matter (the parabolic orbit of the test particle).It was assumed that the hot dark matter consists ofhypothetical Planck neutrinos arising in the decayof the protons at the Planck scale. Galaxies formedfrom the baryonic matter, and the hot dark matterappears in the galaxies later. The rotation curvesof the galaxies were studied in the model, includingMilky Way, M33, NGC 2366 and IC 2574. In thepresent paper, the hot dark matter model is furtherinvestigated, with the application to M31, the systemof M31 and the Milky Way, the globular clustersNGC 2419 and MGC1, the dwarf spheroidal galaxySculptor, ultra-massive quiescent galaxies from theCOSMOS and UDS fields. The baryonic matter massof M31 was estimated from the rotation curves, withthe average value 1.6 × 10 11 m ? . The gravitationalinteraction of the Milky Way and M31 is considered.In the hot dark matter model, the dynamical massesof the Milky Way and M31 are twice their baryonicmatter masses that gives the radial velocity of M31toward the Milky Way, 106 km s −1 . The hot darkmatter mass in the globular clusters NGC 2419 andMGC1 is estimated. The value is small comparedto the stellar mass in both the clusters. The hotdark matter mass within the half-light radius ofthe dwarf spheroidal galaxy Sculptor is estimated,0.5 × 10 6 m ? . The sum of the stellar and hot darkmatter mass within the half-light radius is consistentwith the dynamical mass within the half-light radiusof the Sculptor derived from the kinematics of themetal rich stars. The instability of the baryonicmatter due to the influence of the hot dark matterand some perturbations flattens the velocity profileof the metal poor stars which is unsuitable to derivethe dynamical mass. The evolution of ultra-massivequiescent galaxies from the COSMOS and UDS fieldsis considered. The dynamical to stellar mass relationis doubling during the evolution from z = 2 to 0 thatcan be explained by the absence of dark matter atz = 2 and the presence of the hot dark matter atz = 0.

The URAN-4 decameter radio telescope, which is located in thevillageofMayakiof theOdessaregion, is an element of system of the URAN radio telescopes (Ukrainian Radiointerferometer of theAcademyofSciences). The radio telescope is used according to the following scientific programs: measurements in the composition of the Interferometer with the Super Large Base (VLBI), to study the angular structure of discrete radio sources; the study of the nonstationarity of the flux of cosmic radio sources and the study of the influence of the space environment on the characteristics of the received signals. RT URAN-4 operates at frequencies of 10-30 MHz and consists of an antenna and an equipment complex. A telescope antenna is an electrically controlled phased array of 128 turnstile vibrators. It identifies two linear signal components and is endowed with the possibility of changing the position of the antenna pattern in space (2048 discrete positions of the beam). The geometric dimensions of the array238 meters(West-East direction) and28 meters(North-South direction). The size of the antenna pattern in the modulation mode of signal reception at a frequency of 25 MHz is 2.7 x 22 degrees. In the VLBI interferometer mode, a resolution of about 2 seconds of arc is realized. The instrumental complex of the RT URAN-4 is represented by two types of modulation radiometers, which make it possible to measure the flux densities of radio sources and apparatus intended for VLBB measurements. The working frequency range in which RT URAN-4 operates has a high level of radio interference. The work gives definitions of interference acting in the decameter range. Considered methods of dealing with them. One of the methods to combat interference is the work of the radio telescope on the frequencies permitted and legally protected from interference, the list of which is given in the article. The paper deals with issues related to the organization of the security zone around the radio telescope. On its territory, the maximum allowable power for existing nearby transmitting radio facilities and interfering industrial facilities should be legitimized, in the designated working lanes. At the same time, a monitoring service for the radio spectrum should be organized. The paper deals with the developed and manufactured portable direction finder. Its characteristics are given, recommendations on its use are given.

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.

In addition to the formulas (1) and (2) from work of the author (Bezdenezhnyi, 1999, hereafter Paper I) alternative formulas (3)--(6) are derived for description of two sequences of magic numbers. Their properties are described. Dependences of some physical parameters as a function of the number of chemical element (Z), number of neutrons (N) and the mass number (A) are analyzed. It is shown that magic numbers of protons (Z) and neutrons (N) are displayed in them. The concept of magic mass numbers (A) is proposed, and it is shown that they are also present in some dependences. The list of magic and twice magic (on Z and N) elements is extended, as well as the list of twice magic ones on A and Z or N. We propose to refer a nucleus that contains magic numbers of protons and neutrons to thrice magic nucleus if their sum is a magic number too. It is suggested that during the decay of "double-uranium" super-nucleus one of three twice magic elements ( X(112,168), Y(126,184) and Z(168,258) or Z'(168,240) ) predicted (in Paper I) will be formed fragment accompanying in areas of twice magic nuclei: Yb(70,112), Sn(50,70) and S(16,16) respectively.

Numerical simulations of the cold supersonic flows in different astrophysical problems meets with the loss of precision difficulty. For to overcome the difficulty it was suggested earlier to use conservation entropy equation instead of energy conservation law. In the paper we analyse quantitatively the error what appears in the shocked flow when isoentropic equations are used. The isentropic equations of gas dynamics can be used only when there are no shocks in the solution or when they are weak and do not significantly affect the flow. The results described here were represented as a talk at the 16-th Gamow Summer School: ”Astronomy and beyond: Astrophysics, Cosmology, Cosmomicrophysics, Astroparticle Physics, Radioastronomy and Astrobiology” 14-20 August, 2016,Odessa,Ukraine. The complete paper is published in Bisnovatyi-Kogan & Moiseenko, 2016.

In this paper, we study the distribu- tion of images from a point source in N - point gravi- tational lenses. It is well known that in a Schwarzschild lens (N = 1) from a point source, there are always two images. Moreover, one of them is always inside the Einstein ring, and the second outside it. It follows that: a) the image plane is divided into two areas; b) in each area there is always only one image; c) the source plane, with the exception of the caustic point (origin), is uniquely mapped onto each of the two areas of the image plane. In our study, we describe an algorithm that allows us to determine the single-valued regions in a 2-point gravitational lens and demonstrate it using an exam- ple of a binary symmetric lens in which the distance between the point masses is 1. We have shown that in this case the full prototype of the caustic divides the image plane into eight simply connected areas that have the following properties: a) if the point source is inside the caustic, then it has five images in five (internal) areas; b) if the point source is outside the caustic, then it has three images in three (external) areas; c) in each area there can be no more than one image; d) if the image of a point source is located in one of the five internal areas, then the remaining four also have images, while none of the three external areas have images of the source; e) if the image of the source is located in one of the three external areas, then its images also exist in the remaining two, while none of the five internal areas contains a prototype of this source; f) a caustic is a continuous, piecewise smooth, closed Jordan curve that has a finite number of singular points; each smooth, open part of the caustic, the ends of which are singular points (the caustic arc) has four inverse images, of which only one belongs to the critical set, the caustic arcs are positively oriented (when going around, the interior of the caustic remains to the left; g) the boundaries of the regions consist of arcs (closure of the image of arcs) with a hereditary orien- tation; all eight regions are divided into the following two classes: four regions in which the orientation of the boundary coincides with the orientation on the caustic and four regions in which the orientation of the bound- ary is opposite to the orientation on the caustic.

This paper presents the results of the study of evolution of Jupiter-family comet-like orbits of six meteorite-producing groups, including sporadic fireballs from the IAU MDC database 2007 [1], sporadic meteors from the SonataCo database [2], instrumentally observed H5 and L3.5 ordinary chondrites, as well as near-Earth asteroids which are potential parents of the examined groups. In order to verify the relationship between meteorite-producing groups and their potential parents, we performed backward numerical integration of the orbital motion of these groups’ members over several millennia. The numerical integration was carried out using the Halley software [3]. The equations of motion factored in gravitational perturbations due to the major planets, radiation pressure effects and the Poynting-Robertson drag. The equations of motion were numerically integrated using the 11 th -order Everhart method applicable to studying the motion of Jupiter-approaching short-period comets. The numerical integration of the mean orbital elements of a group, as well as those of the relevant meteorite and potential parent asteroid, over 5,000 years has shown that the respective perihelia, eccentricities and arguments of perihelion evolved in a similar manner over the specified period. The D SH -criterion of Southworth and Hawkins [4], which is a quantitative measure of orbital similarity, has remained below 0.3 [5] for about 5,000 years in the groups of Neuschwanstein and Mason Gully meteorites and for about 3,500 to 4,500 years in the groups of Benesov and Park Forest meteorites. In the groups of the Kosice and Pribram meteorites, the mean orbits and those of their potential parents remained similar as defined in terms of the D SH -criterion over a relatively short period of about 2,000 to 3,000 years. We can infer from our findings that meteorite-producing sporadic fireballs and sporadic meteors are related to the H5 and L3.5 ordinary chondrites and their potential parents, i.e. near-Earth asteroids, in the investigated groups. The estimated time intervals, over which the evolving orbits of the groups’ members have shown good similarity, are indicative of relatively recent formation of meteorite-producing groups as a result of fragmentation of their parent bodies.

Population studies of the extragalactic objects are a major part of the universe large-scale structure study. Apart from radio, infrared, and visible wavelength bands, observations and further identification of extragalactic objects such as galaxies, quasars, blazers, liners, and active star burst regions are also conducted in the X-ray and gamma bands. In this paper we make identification and cross-correlate of the infrared and X-ray observational data, build a distribution of a selected sample sources by types and attempted to analyze types of the extragalactic objects at distances up to z = 0.1 using observational data of relevant space observatories. Data from a leading X-ray space observatory XMM-Newton were used to compile the largest catalog of X-ray sources. Current version of XMM SSC (Serendipitous Source Catalog) contains more than half a million sources. In our previous works we selected and analyzed a sample of 5021 X-ray galaxies observed by XMM-Newton. Identification and classification of these sources is essential next step of the study. In this study we used infrared apparent magnitudes from WISE catalog of AGN candidates. In 2010 space telescope WISE performed full sky survey in four infrared bands and detected 747 million sources. WISE catalog of AGN candidates amounts 4 million of possible extragalactic sources. We built infrared color-color diagram for our sample of X-ray galaxies and assessed their types using WISE telescope data. In this study we also analyzed large scale structure of the universe (distances up to z=0.1). This analysis revealed Coma galaxy cluster and SDSS Sloan Great Wall. In the further studies we are planning to investigate the distribution of different types of X-ray galaxies within the large-scale structures of the Universe., 8 pages, 5 figures

The paper discusses the construction of characteristic curves for various astronegatives with a single exposure. Particular attention is paid to the question of extrapolation of the characteristic curve for the region of the weakest stars in the absence of standards. A new method for constructing an individual characteristic curve for digitized films and plates in the UBVR system has been proposed and implemented. The processing of frames of digitized plates and films with sky areas is car- ried out using LINUX/MIDAS/ROMAFOT software tools. ROMAFOT application allows us to extract astro- metric rectangular coordinates X,Y and photometric char- acteristics such as instrumental photometric magnitudes m, FWHM, and the intensity in the center of the star im- age I c for all fixed objects on each astronegative. For all frames, the connection between instrumental photometric values m with stellar magnitudes in any system (Johnson UBVR, Tycho-2 or GAIA catalogs, etc.) is not linear and multipurpose. It is presented as the characteristic curve for each astronegative. Currently, the determination of U, B, V, R magnitudes of stars and other space objects is in pro- gress for astronegatives with the single exposure obtained in the frameworks of selected observational projects.

In this paper, we studied the incompre- hensible fading of a continuum of noise storms and type IV continual bursts in the decameter range, coinciding in time with coronal mass ejections (CMEs) for solar proton events (SPE). A comparative analysis showed that about 60% of the CMEs are accompanied by the fading of the continuum of noise storms and type IV continual bursts in the range of 25-30 MHz. It is shown that the fading of the continuum of a noise storm associated with a CME is distinguished by the intensity and duration of fading, as well as the width of the fading band and the frequency at which the maximum fading depth is observed. Moreover, detailed studies have shown that, against the background of a general decline in the radiation flux, a fine temporal structure at adjacent fre- quencies remains. This may indicate that the radiation is shielded by an external region in the path of radiation prop- agation. It can be a cold and dense cloud of the CME itself or absorption in the ionosphere. Absorption at low frequen- cies in the Earth's ionosphere is quite possible, since the x- ray and ultraviolet radiation of the flare can cause addi- tional short-term ionization. In this regard, studies have been conducted on the relationship of the fading of the con- tinuum of noise storms with x-ray flares. A comparative analysis showed that there is a fairly strong relationship be- tween the integral flux and the effective duration of x-ray flares with the integral flux and the effective duration of the decrease in the continuum of noise storms, respectively. Moreover, the relationship between the effective durations is slightly higher, where the correlation coefficient between the studied values is ≈ 0.71. It was also shown that short- term impulse fading is associated with impulse x-ray flares, and long-term with gradual long-term x-ray flares. It was noted above that absorption can also occur in the body of the CME itself, therefore, the relationship between the pa- rameters for lowering the continuum of noise storms at a given frequency and the speed of the CME was investi- gated. A comparative analysis showed that there is a fairly strong relationship between the maximum fading depth and the CME speed, where the correlation coefficient between the studied values is ≈ 0.65.

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#.

This paper presents the results of determination of the molybdenum abundances in 13 G, K type stars in the open clusters NGC 2477 and NGC 2506. The abundances of molybdenum were determined using stellar atmosphere models by Castelli & Kurucz (2004), as well as a modified STARSP LTE spectral synthesis code (Tsymbal, 1996). For the used Mo I lines 5506 and 5533 Å the oscillator strengths log gf were adopted from the latest version of the VALD database dated 2016 (Kupka et al., 1999). The high resolution spectra were obtained with a VLT telescope at the European Southern observatory (ESO, Chile).We used atmospheric parameters of the investigated stars which we had obtained earlier. We have found out that the molybdenum abundances depend on metallicity [Fe/H] in giants of NGC 2506 and NGC 2477. For the stars in NGC 2506, molybdenum is slightly overabundant as compared to the solar abundance; such an overabundance is slightly higher in the stars of the second investigated cluster NGC 2477. Further investigation of the Mo abundance in larger number of open clusters is required to draw reliable conclusions.

Exactly 25 years ago, Santiago Tapia has detected circular and linear polarization of AM Her varying with the same period as the photometric and spectral characteristics. This had lead to a discovery of unprecedentedly exotic binary systems, in which the strength of the magnetic field is large enough to keep the white dwarf in a synchronism, dominating the accretion torque. Nowadays, about 70 representatives of this class of polars have been registered. We review the history of study of polars, starting with a "standard model", according to which, the red dwarf fills its Roche lobe and the is captured and channelized by a magnetic field of the white dwarf in the vicinities of the inner Lagrangian point. The models of the "propeller", "idling", "magnetic valve", "swinging dipole", "boiling asymmetric rainbow column" are reviewed, with a special attention to the unsolved problems of this study - contradiction between the observed synchronism of spin and orbital periods of the white dwarf with a possible presence of the partially ballistic trajectory of the accretion and possibly important contributions of the dipole and multipole components of the magnetic fields; presence of few mechanisms of luminosity variations; various types and mechanisms of variability at different time scales from seconds to decades. The monitoring of AM Her (and later on other objects) has started inOdessain 1978 and was regularly continued in the Crimean Astrophysical observatory since 1989. The results will be published in the "Atlas and catalogue of the polarimetric and photometric characteristics" by N.M.Shakhovskoy, I.L.Andronov and S.V.Kolesnikov. Other papers absent in the ADS are available via http://il-a.pochtamt.ru or www.paco.odessa.ua/~il-a. Despite 25 years have passed, these stars still exhibit new observational surprizes challenging theoretical models.

In this paper, we present the results of a study of the variability of the prototype polar AM Her using one of the complementary mathematical methods. Results of modeling of the auto-correlation analysis of a 24117 second long Chandra observation are discussed. The data have been binned to 1-second intervals. The corresponding auto-correlation func- tion has been modeled to take into account the nonsinusoidal orbital variability of the object, onto which a strong flickering is added. The model of a second order trigonometric polynomial (orbital) + a first-order Auto-Regressive process (”shot-noise” flickering) does not seem to be not sufficient. A much better approximation can be achieved With a a four-parameter fit With exponential decay times t1 : 174s and t-2 : 9.8s. A possible physical mechanism may be attributed to the longer time of the flare of the plasma blob (” spaghetti”) falling onto the White dwarf as compared to flares corresponding to smaller blobs resulting from magneto- hydrodynamical instabilities. The results are compared vvith numerical models. .

During their life galaxies exchange in matter and energy with the intergalactic medium (IGM). This complex process is a most important factor in galactic evolution as well in evolution of the IGM. In this paper recent progress in the IGM studies and mechanisms of mass gain and mass loss from galaxies are briefly reviewed. Using a model of chemo-dynamical evolution of galaxies I discuss enrichment of the IGM with metals and origin of the radial gradients of chemical composition in disk galaxies as possible consequence of heavy elements loss. The general conclusion is simple: many problems remain unsolved but we are under way to understanding of consistent evolution of galaxies - IGM system.

No abstract, In this paper we analyse the evolutionary status of He-rich stars in order to draw some conclusions on internal processes which determine the chemical anomalies presently observed in stars of this type.

Physical mechanisms and corresponding mathematical models for different types of stellar variability are reviewed with applications to concrete stars. Special attention is attributed to the following topics: cataclysmic variables (synchronous and synchronizing magnetic systems, non-magnetic novalike stars, dwarf novae; magnetic activity of the red companion, third body around), pulsating variables (additional classification criteria of variability, multiparameter correlation analysis of the characteristics of the mean light curves of groups of long-period stars and of the multi- parameter correlation analysis of the individual characteristics of their pulsations), mathematical models (multi-periodic, multi-harmonic, multi-shift variations with possible trends, mono- and multi- cyclic variations of low coherence and the frequency changing/switching signals, "red noise" variability. Some original papers and links may be found at http://ila.webjump.com

In the present paper we analyze the anomalies in the atmospheres of HgMn stars. The abundance anomalies include both overabundances and underabundances of heavy elements. Recent observations show strongly anomalous isotopic composition of Hg, Pt, Tl and of He. Generation of abundance anomalies in quiescent atmospheres of CP stars is successfully explained by the mechanism of diffusional segregation of elements due to oppositing gravitational and radiative forces, but the formation of isotopic anomalies is not yet well explained. New diffusion mechanism called light-induced drift (LID), added to the one of radiative acceleration, successfully explains the observed isotopic anomalies. We have refined the theory of LID and applied it to CP star atmospheres. The results of computations confirm the important role of LID for diffusive segregation of isotopes.

The current Big Bang Model had its origin in Einstein's attempt to model a static cosmos, based on his general theory of relativity. Friedmann and Lemaitre, as well as de Sitter, further developed the model to cover other options, including nonstatic behavior. Lemaitre in the 1930s and, particularly, Gamow in 1946 first put physics into the nonstatic model. By 1946 there had been significant developments in the mathematics of the model due to Robertson, Walker, Tolman and many others. The Hubble law had given an essential observational basis for the Big Bang, as did the attribution of cosmic significance to element abundances by Goldschmidt. Following early suggestions by George Gamow, the first attempt to explain nucleosynthesis in a hot, dense, early universe was done by Alpher, Bethe and Gamow in 1948, a paper whose principal importance was that it suggested that the early universe was in fact hot and dense, and that hydrogen and helium and perhaps other light elements were primeval. In that same year Alpher and Herman first predicted a cosmic background radiation at 5 kelvin as an essential feature of the model. The Hubble expansion rate, the primordial and stellar abundances of the elements, and the cosmic microwave background are major pillars today for the Big Bang model.

Currently representation of solar cycles on average monthly data and smoothed values on various indexes from the full solar disk is generally accepted. Such representation creates an illusion of monotone change and perceptions of simultaneity of manifestations of solar activity for all solar disc. At the same time, daily monitoring data reveal the presence of discrete properties of manifestations of solar cycle. They are associated with absence of spots on the Sun in the northern and southern hemispheres at different intervals. This phenomenon is defined as anti-cycle of solar activity. Properties of discreteness of anti-cycles are presented in this paper on "spotless days’ periods". On their basis the appropriate monthly and annual data was received. The basic characteristics of the manifestations of the discreteness of activity anti-cycles had been determined. It noted the «switch effect» of the existence of the solar dynamo. It manifests itself in the rapid transition from a regime of «spotless days» to the regime of continuous generation.

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.

In the paper one from little known pages of Prof. V.P.Tsessevich' life and scientific activity as an organizer and scientifics supervisor of expedition on the determination of coordinates of site, where BTA would be placed, is described. V.P.Tsessevich have formed a staff of expedition, scientific problems and have taken direct part of the first and final stages of the expedition. As a result of expedition coordinates which corresponded to requirements of astroplace of the second class (expeditionary) have been obtained and axes of BTA have been traced on the locality.

The CBA (Center for Backyard Astrophysics) Belgium Observatory belongs to a global network of small photometric telescopes, that study periodic phenomena in Cataclysmic Variables (CVs). This network is among the leading examples of successful partnerships between professional and amateur astronomers. In a few occasions. CBA stations operate on a stand-alone basis on some selected CVs. This paper reports the results of such an individual photometry campaign. The dwarf nova PV Per was observed for three nights during its outburst in September 1996 at the CBA Belgium Observatory. Unfiltered differential CCD photometry revealed superhumps with a period of 0.oSO5:I:0.00ol days. This finding establishes PV Per as being a new member of the SU UMa-type dwarf novae.

This paper reports on the theoretical investigation of evolution of the Galaxy. The spiral arms and radial gas flows can be considered as some kind of indicators of the dynamical processes in the disc. Investigation the surface density of gas. The velocity profiles of radial gas flows were selected in such a way to have an agreement between the model predictions and observational data. The model with the radial gas flows gives the results that appear to be in the better agreement with the observations. The results of the model predictions differ significantly comparing to the case of the standard Galactic evolutionary model.

Recently we proposed a new method of mode identification based on spectroscopic nonadiabatic diagrams (Cugier & Daszynska 2001, As.Ap., 377, 113). Our results are for β Cephei models. These diagram involve the amplitude ratios and phase differences calculated from various oscillating parameters measured from line profiles. We found that the spectroscopic observables are especially useful to determine m values. In this paper we investigate the case of multimodal pulsating models.

The paper is devoted to elaboration of the new optimized methods, algorithms and programs for the solution of problems of the remote control of near-earth space (CS), which are related to investigation of cosmic objects (CO) based on the photometric and coordinate measurements. It is shown, that for these determination of satellite's rotation period around center of mass, the orientation of rotation axis, and also its color, polarization and others characteristics can be used. The main principles of a system of the CO identification based on their light curves are elaborated. A new algorithm of CO orbit determination using the network station data is created. Its accuracy is by 3-4 orders at magnitude higher than that of algorithms based on the well-known methods of celestial mechanics.

Sunlight scattered by surfaces of atmosphere less bodies carry information about details of these surfaces. Burns and Tedesco in 1979 published formula for estimations of dimensions of details located on surfaces of asteroids. Authors of this paper show that using of frequency methods for analysing of light curves or curves of colour index allows receiving of optimal information. Experiments confirm this statement. Estimations of dimensions of details located on the surface of the asteroid 1620 Geographos are in good agreements with facts receiving with radar observations. Analysis of synthetic colour indexes B-V and V-R of the asteroid 4 Vesta show estimations of dimensions of colour spots on its surface in the interval 660-9 km. Conclusion are made that investigations of high frequency modulations of light curves or curves of colour indexes of asteroids allow us to receive information about dimensions of details on its surfaces.

The astronomical observations of the last years show that there are the regions in the Universe with much lower density of matter, than their surroundings. Theoretical studies of the regions (voids) in the model of the expanding Universe are carried on different directions. In this paper the voids have been built by means of matching Tolman and Friedman solutions. The Lichnerovich-Darmois matching conditions are used. It is shown that in expanding Universe with at space the voids can not exist. So we have Friedman Universe with voids, with described by the Tolman solution. The models of voids in the Friedman Universe with negative spatial curvature have been built.

We search for variable stars and study them using our CCD observations, observations available in the CSS, NSVS, ASAS-3 and Super-WASP online public archives.Our CCD observations were performed using the Zeiss- 1000 telescope of the V.G. Fesenkov Astrophysical Institute’s Tien-Shan Astronomical Observatory. Earlier, as a result of our search using CCD images, we detected 27 new variable stars; using the NSVS and SuperWASP databases, we detected 12 new red semiregular and irregular variable stars.In this paper, we present our study of seven known variables based on the ASAS-3 and SuperWASP databases. All these stars remained poorly studied, their light elements were unknown, variability types were considered preliminary only. We studied two eclipsing variables (FY And and V2250 Sgr) and five Mira-stars (BZ Sco, CZ Sco, FK Sco, V880 Sco and V1818 Sgr).

Stars with high proper motions, for the most part, are objects located in the solar neighborhood within 100 parsecs. These stars are important targets for a wide range of astrophysical problems, but the accuracy of the results depends on the completeness of the star samples. The uniform distribution over the celestial sphere is also important for kinematic studies. There are two catalogs of the fast stars in northern hemisphere, while only scattered lists of such stars are available for southern hemisphere. This paper presents the results of analysis of samples of stars with proper motions exceeding 150 mas/year from the modern catalogs of astronomical database CDS (PPMXL, SPM4, UCAC4, XPM, APOP, LSPM, Tycho2, URAT1 and WISE). Results of pairwise mutual crossidentification of the samples have shown that modern astrometric catalogs contain a significant number of false identifications of stars with large proper motions, and the total number of common stars in the resulting samples is extremely small and is not more than 20% on average.

Today the following types of resonances in the rotation of celestial bodies in the solar system are known, namely orbital, spin-orbit and spin-spin resonances. This paper presents our computations of these types of resonances for the known binary and multiple asteroid systems.

The introduction of the automatic measuring machines into the astronomical investigations a little more then a quarter of the century ago has increased essentially the range and the scale of projects which the astronomers could capable to realize since then. During that time, there have been dozens photographic sky surveys, which have covered all of the sky more then once. Due to high accuracy and speed of automatic measuring machines the photographic astrometry has obtained the opportunity to create the high precision catalogs such as CpC2. Investigations of the structure and kinematics of the stellar components of our Galaxy has been revolutionized in the last decade by the advent of automated plate measuring machines. But in an age of rapidly evolving electronic detectors and space-based catalogs, expected soon, one could think that the twilight hours of astronomical photography have become. On opposite of that point of view such astronomers as D.Monet (U.S.N.O.), L.G.Taff (STScI), M.K.Tsvetkov (IA BAS) and some other have contended the several ways of the photographic astronomy evolution. One of them sounds as: "...special efforts must be taken to extract useful information from the photographic archives before the plates degrade and the technology required to measure them disappears". Another is the minimization of the systematic errors of ground-based star catalogs by employment of certain reduction technology and a dense enough and precise space-based star reference catalogs. In addition to that the using of the higher resolution and quantum efficiency emulsions such as Tech Pan and some of the new methods of processing of the digitized information hold great promise for future deep (B < 25) surveys (Bland-Hawthorn et al. 1993, AJ, 106, 2154). Thus not only the hard working of all existing automatic measuring machines is apparently needed but the designing, development and employment of a new generation of portable, mobile scanners is very necessary. The classification, main parameters of some modern automatic measuring machines, developed with them scientific researches and some of the used methods of high accuracy, reliability and certainly ensuring are reported in that paper. This workare supported by Grant N U4I000 from International Science Foundation.

In the paper some ways of the improvement (changes in the optical-mechanical part and improvement in the electronical part) the electrophotometric instruments are described. The apparatus which were constracted at Lviv astronomical observatory were taken as the examples.

The light curves of EGS Ajisai with temporal resolution of 20 ms referred to the time scale UTC (GPS) with an error of at most 0.1 ms were obtained. The observed flashes are produced when the mirrors which cover the spinning satellite’s surface reflect off the sunlight. In previous paper the analysis of sequence of flashes allowed of reconstructing the arrangement and orientation of the mirrors, i.e. developing an optogeometric model of the satellite (Korobeynikova et al., 2012), and to apply that model along with new photometric observations to determine the satellite’s sidereal rotational period with an accuracy that was previously unachievable. A new technique for determination of the spin-axis orientation during each passage of the satellite over an observation site was developed. The secular slowdown of the satellite’s spin rate (Рsid = 1.4858·EXP(0.000041099·T), where Т is measured in days counted from the date of the satellite launch) and its variations correlating with the average duration of the satellite orbit out of the Earth’s shadow were refined. New parameters of the spin-axis precession were estimated: the period Pprec = 116.44 days, αprec = 18.0h, δprec = 87.66°, the nutation angle θ = 1.78°.

Variable polarization of ρ Cassiopeae is found, with an amplitude of about 0.2 in the V band and up to 1 in R. It is drew attention on a conflict of luminosity from a spectral analysis (about -8 magnitude) and from a trigonometrical parallax (an average from four measurings corresponds to +0.5 magnitude). The paper submitted to Astronomische Nachrichten.

Measurements of brightness of 29 red dwarf stars and 3 stars of other types were made on time scales of 5 - 90 years using plates archives of Sternberg State Astronomical Institute (Moscow), Astronomical Observatory of Odessa State University and Sonneberg Observatory (Germany). The sensitivity of plates are close to B band. The long- term changes in yearly mean magnitude have been detected or suspected for 10 dKe-dMe objects. Two stars, V833 Tau and PZ Mon, show high amplitude of variability up to 0.6 - 1.0 mag. The range of variability in mean light of the other eight stars is of 0.2 - 0.5 mag. The light curves show typical times of long-term variability of about 30-60 years. Changes of the mean light of the remained dKe-dMe stars and three other stars of other types - FK Com, V654 Her, AE Aqr - do not exceed 0.2 mag. Complete paper is to be published in: Izvestija Krymskoy Astrofizicheskoy Observatorii, v.91.

It is proposed to evaluate, on the basis of H and He radio recombination line observations, the number ratio of stellar photons, capable to ionize helium, to those capable to ionize hydrogen. Then, comparing this ratio with a prediction of model stellar atmospheres, the effective temperature and other stellar parameters are determined. Thus to the information about a total number of Ly-c quanta it adds the information about a spectrum slope in Ly-c wavelength range, which is not directly observable, but information about it is special importance for O-B stars. The choice of an object and angular radio telescope resolution needs to make so that ionizing photons (Ly-c) should be absorbed completely in a region of investigation and beam should cover enough this region. Therefore it is proposed to usecompact HII regions and a central part (core) of such HII regions which have a " blister" -type structure. This way is applied to the galactic HII regions: Orion A (38500), DR-21 (36000), S106 (35300), Sgr B2(N3) (35100), W48 (38700), Orion B (36100), W3A (43000), there the obtained effective temperature of exciting stars are in parentheses. Results of it are discussed and compared with different model stellar atmospheres. For sources S106 and Sgr B2(N3) it has obtained the strong difference of total number of Ly-c photons between its determination by radio flux density and that by radio lines. Possibly this difference is needed to take into account in further study of these objects. Full paper was published in Astronomicheskii Zhurnal (1993, 70, 72).

%B It is shown that there are certain rules which connect a height of previous solar activity cycle with the entropy of the next one. For even and odd cycles these rules are asymmetrical. So if it is known height of the previous cycle one can make estimation for entropy of the next one according to one of these rules. It has been shown also, that entropy (ES) of a cycle has good correlation with its height. On the other hand height of a cycle (Wmax) correlates with duration of its rise branch (Waldmeier's rule), and it allows to get the estimation of epoch of maximum (Tmax) of future cycle. Epignosis shows that the reliability of such forecasts is about 83%. Below we present the values of main parameters of future 24 cycle obtained according to these rules: Shannon's entropy ES = 5.0 ± 0.2; height of the cycle Wmax = 95± 20 (in monthly Wolf numbers); duration of arise branch Ta = 4.5 ± 0.5 years; epoch of the cycle maximum Tmax = 2012.25 ± 0.5 year. Full version of the paper is prepared to be published in Solar System Research.

In this paper we consider dynamical behavior of the astrophysical objects in the Local Group. The motion of Andromed and The Milky Way is studied. We distinguish two different models: for the first one we do not take into account the influence of the Intra-Group Matter (IGrM), for the second one we take into account the dynamical friction due to the IGrM. We obtained some characteristic IGrM parametres such as particle masses for principle cases of the collision between the giant galaxies and the situation when the merger becomes problematic. We also define the region in the vicinity of our Local Group where the formation of the Hubble Flows starts.

This paper describes a simplified numerical model of passive artificial Earth satellite (AES) motion. The model accuracy is determined using the International Laser Ranging Service (ILRS) highprecision coordinates. Those data are freely available on http://ilrs.gsfc.nasa.gov. The differential equations of the AES motion are solved by the Everhart numerical method of 17th and 19th orders with the integration step automatic correction. The comparison between the AES coordinates computed with the motion model and the ILRS coordinates enabled to determine the accuracy of the ephemerides obtained. As a result, the discrepancy of the computed Etalon-1 ephemerides from the ILRS data is about 10″ for a one-year ephemeris.

We present a review of observations of the stellar longitudinal (effective) magnetic field ($B_e$) and its properties. This paper also discusses contemporary views on the origin, evolution and structure of $B_e$., Comment: Plenary report, The Gamov International Astronomical Conference, XIII ODESSA, 19-25 August, 2013, Odessa, Ukraine

This paper studies the capabilities of the all-sky weather (meteorological) cameras in investigation of bright variable stars and determination of apparent radiants of meteor showers.

This paper is a brief introduction to the new physical conception - holographic dynamics. Formulated in the early 90's of the last century, the holographic principle helped to overcome some fundamental challenges facing the traditional cosmology.

Alexander Ya. Orlov is a well-known astronomer and geophysicist as well as a worldrecognized organizer of scientific research in Russia, the USSR, and Ukraine. Orlov has formulated his main scientific ideas during the Odesa's period of life. He studied a tidal deformation of the Earth and its polar motion using the gravity and latitude observations. He has proposed new defenitions of a mean pole and a mean latitude, as wel as a new method for determing the Earth pole coordinates. To the end of 1940-ties, the Orlov's scientific ideas were implemented and stimulated a development of a research field, which is now called as Astrogeodynamics or Space Geodynamics. Among the representatives of the Orlov's scientific school are about 20 Doctors of Sciences and more than 40 Candidates of Sciences, including the members of Academy of Sciences of Ukraine and other countries. Among them are N.Stoyko-Radilenko (France), J.Witkowski (Poland), V.Zhardetsky (Yugoslavia-Austria-USA), D.Pyaskovsky, Z.Aksent'eva, E.Lavrentieva, N.Popov, E.Fedorov and A.Korol in Ukraine. The deserved followers of the Orlov's scientific ideas were also I.Androsov, I.Dyukov, K.Mansurova, B.Novopashennyj, N.V.Zimmerman in Russia and M.Bursa (Chesh Republic), who worked with him, as well as his sons, A.A.Orlov and B.A. Orlov. The Orlov's life and scientific activity were fully described in many articles. For that reason in this paper we will focus on the little-known facts of the Orlov's scientific-organizational activity, for example, the Orlov's appointments as a director of observatories in Odesa, Poltava, m.Pip-Ivan, Pulkovo, and Kyiv; interesesting facts related to his membership in the Academies of Sciences of the USSR and Ukrainian SSR; organization of a large-scale program on the latitude observations and gravimetric survey. We describe briefly his life and his astrogeodynamic scientific school.

Three criteria of the periodicity are discussed in the paper and their properties are investigated. These criteria are applied to investigate the periodicity properties of a variable star GX Pegasi. A number of periodic components are extracted.

Light curves and spectrum of Geminga in a hard gamma region are investigated in this paper and their properties are discussed. The geometric parameters of pulsar rotation, such as the inclination angle of rotational axis, the angle between rotational and magnetic axes and the cone spread angle of gamma radiation are evaluated. All the results are based on the data of EGRET instrument.

A historic review of the 293 papers, contained as the results of observations and the description of the processes of production and destruction of the light elements Li, Be, B are presented.

We present in this paper a description for various types of the apparent variations of stellar magnetic fields, which we actually recognise.

The problem of cosmic ray origin comes to two main questions: were and how cosmic particles are accelerated up to very high energies. In this paper, arguments in favor of two basic sources of cosmic rays (Galaxy and Metagalaxy) are considered and consequences for observed parameters of cosmic rays (energy spectrum and mass composition) are analyzed. Model of cosmic ray generation in plasma pinches is discussed.