Odesa Astronomical Publications
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ISSN 1810-4215
eISSN 2786-5215
eISSN 2786-5215
Журнал «Одеські астрономічні публікації» публікує наукові статі з питань астрономії, астрофізики, космічних досліджень, а також матеріали конференцій, які організовуються й проводяться за участю НДІ «Астрономічна обсерваторія» Одеського національного університету імені І. І. Мечникова.
Повні тексти видання доступні на сайті Наукової бібліотеки ОНУ імені І. І. Мечникова за посиланням:
https://lib.onu.edu.ua/ukrayinska-odessa-astronomical-publications/
Сайт видання: http://oap.onu.edu.ua/
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Перегляд Odesa Astronomical Publications за Автор "Andrievsky, Serhii M."
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Документ A new 800 mm automatic telescope(Astroprint, 2013) Andrievsky, Serhii M.; Molotov, I. E.; Fashchevsky, N. N.; Podlesnyak, S. V.; Zhukov, V. V.; Kouprianov, V. V.; Kashuba, S. G.; Kashuba, V. I.; Mel’nichenko, V. F.; Gorbanev, Juri M.; Андрієвський, Сергій Михайлович; Андриевский, Сергей МихайловичABSTRACT. A new automatic telescope, a 800-millimeter main mirror catadioptric anastigmatic aplanat, was constructed by specialists of Odessa National University Astronomical observatory (Ukraine) in cooperation with their colleagues from the ISON project (Russia), and was recently put into operation. The telescope is mounted at Mayaki station in suburb of Odessa. It is equipped with a focal corrector and a professional CCD camera. The telescope is used now for observations of geostationary objects, asteroids, and comets. In addition, this telescope can be used for the high precision photometric observations of faint objects up to 20m.Документ About chemical composition of supergiant PMMR145 in Small Magellanic cloud. Osmium.(Astroprint, 2012) Gopka, Vera F.; Shavrina, Angelina V.; Vasilyeva, S. V.; Andrievsky, Serhii M.; Андрієвський, Сергій Михайлович; Андриевский, Сергей МихайловичABSTRACT. The abundance analysis of six Ksupergiants of the Small Magellanic (Hill 1997) showed that the heavier elements (La, Ce, Nd, Eu) have the excess relative to iron [El/Fe]=+0.4 dex, on average, for the sample of five stars (PMMR23, PMMR27, PMMR48, PMMR102, PMMR145). We made the identification of spectral lines in the spectrum of PMMR145 based on the comparison of synthetic and observed spectra. The absorption lines of elements heavier than lanthanides including osmium were identified and abundance of osmium was found ([Os/Fe]=0.59 dex).Документ An enigma of the Przybylski star(Одеський національний університет імені І. І. Мечникова, 2022) Andrievsky, Serhii M.; Андрієвський, Сергій МихайловичA new scenario to explain the Przybylski star phenomenon is proposed. It is based on the supposition that this star is a component of a binary system with a neutron star (similar to the hypothesis proposed earlier by Gopka, Ul’yanov & Andrievskii). The main difference with previous scenario is as follows. The orbits of the stars of this system lie in the plane of the sky (or very close to this plane). Thus, we see this star (and its companion) nearly polar-on, and therefore we cannot detect the orbital motion (spectral line based) from the Przybylski’s star spectrum. In relation to the Przybylski star, the neutron star is a γ-ray pulsar for it. A neutron star is a source of relativistic particles and radiation emitted from the certain parts of its surface. The topology of this radiation strongly depends on the the magnetic field configuration of the neutron star. Existing models suppose that 1) high-energy electron-positron pairs and hard radiation are produced in the (magnetic) polar zones. Accelerated charge particles that move along magnetic lines emit electromagnetic quanta. In this model the radio-emission is genetically linked with the emission of the γ-quanta. 2) Another model of the outer gap is based on the assumption that there is a vacuum gap in the outer magnetosphere of the neutron star, which arises due to the constant escape of charged particles through the light cylinder along the open magnetic field lines. The direction of such escape may be roughly orthogonal to the rotation axis. If the rotation axes of the Przybylski star and the neutron star are close in direction (or even aligned), charged particles and hard radiation ejected in the approximately orthogonal direction at a large solid angle can enter the Przybylski’s star atmosphere, causing there different physical processes. As a possible source of the free neutrons could be the nuclear reactions between high-energy γ-quanta and nuclei of some atoms in the Przybylski’s star atmosphere gas. As a result, photoneutrons can be generated. Large enough neutron flux can be produced in the reactions with quite abundant element of the atmosphere gas (for example, helium). The photoneutrons produced in these reactions are rapidly thermalized and, as resonant neutrons, react with seed nuclei in the s-process. It should be also noted that together with s-process elements, the deuterium nuclei could be formed as a result of the interactions of the free resonant neutrons with the hydrogen atoms, but this issue has not yet been worked out.Документ Are the s-Cepheids crossing the instability strip for the first time?(Astroprint, 2012) Andrievsky, Serhii M.; Harbuzov H. O.; Doikov, D. N.; Андрієвський, Сергій Михайлович; Андриевский, Сергей МихайловичUsing the literature data on secular period changes reported for the small-amplitude Cepheids (s-Cepheids) it is shown that these stars are not crossing the instability strip for the first time. After correction of the observed pulsational chracteristics of s-Cepheids, in the diagram ”log(dP/P)100 - log P” they become indistinguishable from usual classic Cepheids, which are supposed to have already crossed the instability strip more than (or at least) once.Документ Diffuse interstellar band 6202 ˚a as an indicator of organic matter in cosmos: cepheid spectra(Одеський національний університет імені І. І. Мечникова, 2019) Andrievsky, Serhii M.; Shereta, E. P.; Khrapaty, S. V.; S. A. Korotin; Kovtyukh, Valery V.; Kashuba, V. I.; Андрієвський, Сергій Михайлович; Андриевский, Сергей Михайлович; Ковтюх, Валерій В.We have described the method of investigation of the diffuse interstellar band (DIB) at 6202 ˚A. This DIB is seen in the spectra of cepheid stars, and it is blended with two stellar lines of Ce II (6201.773 ˚A) and Ni I (6204.6 ˚A). After removal of the blending lines of ionized cerium and neutral nickel, we can determine the equivalent widths (EW) of the DIB. This procedure can be applied for the sample of cepheids (with well known distances), which enables one to construct the map of the organic matter distribution in the Galactic disc and use these values to investigate the E(B–V)–DIB EW relation. The relation found from Cepheids matches that found in B stars. This relation can help to find the reddening for newly discovered Cepheids without extensive photometric data, and thus determine their distances. The relation between E(B–V) and the DIB EW does not yield precise reddening values. It is not a substitute for better photometric or spectroscopic methods. At best, it is indicative, but it provides some information that may not be otherwise available.Документ Investigation of diffuse interstellar bands of organic molecules in the spectra of cepheid stars(Одеський національний університет імені І. І. Мечникова, 2015) Kashuba, S. V.; Andrievsky, Serhii M.; Chekhonadskikh, F. A.; Korotin, S. A.; Kovtyukh, Valery V.; Luck, R. E.; Андрієвський, Сергій Михайлович; Андриевский, Сергей МихайловичWe describe an effective method of investigation of the Diffuse Interstellar Bands (DIBs) in the spectra of Cepheid stars. DIBs are believed to originate from the absorption of such carriers as polycyclic aromatic hydrocarbons in the interstellar gaseous clouds located between an observer and the stars whose spectra were recorded. We performed a detailed consideration of the DIB at 6613 A in our sample of spectra for more than 250 stars. The quantitative characteristics of the DIB absorption features will be studied in connection with the interstellar absorption data, and after that, they will be used in the mapping of the Galactic disc.Документ Ionisation loss and shock excitation of 44/20 Са I and 44/20 Са II atoms in cold remnants of type II supernovae(Одеський національний університет імені І. І. Мечникова, 2017) Doikov, D. N.; Andrievsky, Serhii M.; Андрієвський, Сергій Михайлович; Андриевский, Сергей МихайловичThe light emission (“glow”) of cold dusty plasma of the remnant of SN1987A 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 44/20 Ca resulted from the decay of radioactive 44/20 Ti travelling in the remnant’s cold dust. The overionisation in the remnant resulted from the motion of the 44/20 Ca 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 44/20 Ca II ion in the inner layers of the remnant. We have reached the conclusion that the Ca I/Ca II lines strength ratio corresponds to the isotopic abundance ratio [44/20 Ca] /[44/20 Ca ] in type II supernova remnants.Документ Isolated clusters of PF catalogue(Astroprint, 2012) Panko, Olena O.; Andrievsky, Serhii M.; Андрієвський, Сергій Михайлович; Андриевский, Сергей Михайлович; Панько, Елена Алексеевна; Панько, Олена ОлексіївнаThe properties of isolated galaxy clusters are discussed. The clusters were found among 1746 PF clusters inclusive 50 and more galaxies in structure field. For 19 clusters with distances to the nearest neighbour larger than 68.5 h-1 Mpc we assigned the morphological types of these clusters according to Abell and Bauts & Morgan. The existence of preferential planes and angular momenta of isolated clusters was assumed. We connect evolution of isolated clusters with common large-scale characteristics.Документ Some evolutionary aspects of the binary stellar systems containing neutron star(Astroprint, 2012) Ulyanov, Oleg O.; Andrievsky, Serhii M.; Gopka, Vera F.; Shavrina, Angelina V.; Андрієвський, Сергій Михайлович; Андриевский, Сергей МихайловичThe obvious lack of the binary stellar systems that contain neutron stars (NS) is observed at present. Partly it is caused by the fact that it is very di cult to detect neutron star in a binary system if this relativistic component does not manifest itself as a radio pulsar. Among 1879 pulsars that are listed in the ATNF pulsar catalogue, only 141 pulsars are known to be the companions in binary systems. Only 81 objects having median mass estimation of more than 0.2 M⊙ constitute the binary systems with pulsars. Nevertheless, such systems should be much more numerous and their investigation is of the great interest because thier structure and evolution can certainly help in our understanding of many unique properties that are seen in some stars.Документ Some statistical picture of magnetic CP stars evolution(Astroprint, 2010-07) Gopka, Vera F.; Ulyanov, O. M.; Andrievsky, Serhii M.; Shavrina, Angelina V.; Yushchenko, V. A.; Андрієвський, Сергій Михайлович; Андриевский, Сергей МихайловичWe discuss some statistical results on the evolution of magnetic CP stars in the framework of the supposition about their binary nature.Документ Spherical primary mirror in telescopes with complex (multi-element) optical designs(Одеський національний університет імені І. І. Мечникова, 2021) Podlesnyak, S. V.; Fashchevsky, N. N.; Bondarenko, Yu. N.; Andrievsky, Serhii M.; Андрієвський, Сергій Михайлович; Андриевский, Сергей МихайловичAn optical design for telescope with spherical primary mirror, planoidal surface and two-lens corrector is discussed. The spherical mirror has an aperture ratio 1/2.69. After reflection from the spherical mirror, the wave front falls on a planoidal surface and “forms” the reflected wave front from a virtual mirror with e2 = 1.576. After passing the two-lens corrector, the light is collected in the focal plane. A dot diagram in the focal plane shows that all three-order aberrations are successfully corrected. The effective field of view is 2 degrees. The aperture ratio is 1/2.28.Документ The abundances of heavy elements in red supergiants of Magellanic Clouds(Astroprint, 2013) Gopka, Vera F.; Yushchenko, A. V.; Kovtyukh, Valery V.; Shavrina, Angelina V.; Yushchenko, V. A.; Vasilyeva, S. V.; Pavlenko, Y.; Andrievsky, Serhii M.; Андрієвський, Сергій Михайлович; Андриевский, Сергей МихайловичABSTRACT. The spectra of Magellanic Clouds (MC) supergiants PMMR 23, PMMR 144 and RM 1- 667 with resolving power R=30,000 and signal to noise ratio near 100 obtained at 3.6 meter telescope in Chile were analysed. We present a report on the detailed investigation of MC supergiants, with spesial attention to the thorium abundance in these stars. The abundance patterns of three supergiants show that r-process elements are clearly detected in the atmospheres of investigated stars, but the abundances of s-processes elements can vary from star to star.Документ THE QUANTITY AND QUALITY OF OBSERVATIONAL NIGHTS MONITORED WITH USING THE ASTRONOMICAL INSTRUMENTS AT THE SUBURBAN OBSERVATION STATIONS OF ASTRONOMICAL OBSERVATORY OF ODESSA NATIONAL UNIVERSITY(Astroprint, 2015) Kashuba, S. G.; Gorbanev, Juri M.; Andrievsky, Serhii M.; Marsakova, V. I.; Troianskyi, V. V.; Андрієвський, Сергій Михайлович; Андриевский, Сергей МихайловичThe Astronomical Observatory of Odessa National University named after I.I. Mechnikov is one of the four astronomical observatories which exist in classical universities. The Observatory has a main office in the T.G. Shevchenko Park that located near historical center of Odessa. The Observatory also has several observation stations: in the Odessa suburb Mayaki and Kryzhanovka villages.Документ Zirconium abundances in the Central part of the dSph Fornax galaxy(Одеський національний університет імені І. І. Мечникова, 2017) Andrievsky, Serhii M.; Korotin, S. A.; Hill, V.; Zhukova, A. V.; Андрієвський, Сергій Михайлович; Андриевский, Сергей МихайловичWe 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.Документ Одесской астрономической обсерватории 140 лет(Астропринт, 2011) Андриевский, Сергей Михайлович; Andrievsky, Serhii M.; Андрієвський, Сергій МихайловичВ 2011 году Астрономической обсерватории в Одессе исполняется 140 лет. Астрономическая обсерватория (ныне Научно-исследовательский институт «Астрономическая обсерватория») – одно из старейших научных учреждений нашего города. Большую часть времени своего существования она была неразрывно связана с Новороссийским (впоследствии Одесским государственным, а затем национальным) университетом. В начале ХХ века 12 лет была самостоятельной организацией, причем некоторое время – Главная государственная астрономическая обсерватория Украины.