Статті та доповіді НДІ "АО"

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https://dspace.onu.edu.ua/handle/123456789/13174

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Перегляд Статті та доповіді НДІ "АО" за Автор "Andrievsky, Serhii M."

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    Astronegative archive of Odessa observatory. Large surveys with small telescopes
    (2019) Kashuba, S. V.; Bazyey, N. V.; Kashuba, V. I.; Andrievsky, Serhii M.; Андрієвський, Сергій Михайлович; Андриевский, Сергей Михайлович
    Currently Observatory of I. I. Mechnikov Odessa National University owns collections of astronegatives obtained with its own instruments (about 100000 glass plates), as well as those obtained with instruments from other observatories (about 10000 plates). According to Bulgarian web-page WFPDB (wfpdb.org) Odessa collection of astroplates is second in Europe (after Sonneberg collection) and third in the world (after Harvard and Sonneberg). In this poster we describe the current condition of our collection and consider our plans for how to maintain this important astronomical heritage. We are also discussing our first steps in digitizing part of a collection in accordance with the decision of the world virtual observatory and WFPDB standards.
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    Coopération Franco-Ukrainienne dans dans l'étude de l'évolution chimique de Notre Galaxie
    (2019) Andrievsky, Serhii M.; Андрієвський, Сергій Михайлович; Андриевский, Сергей Михайлович
    Notre Galaxie comprend différentes sous-structures : disques minces et épais, renflement, halo, etc. Ces sous-structures contiennent des étoiles de types différents, en particulier de niveau de métallicité différente. Une étude de la composition chimique de ces étoiles fournit une information cruciale sur l'évolution chimique de notre système stellaire dans son ensemble. Jusqu'à présent, nous n'avions pas de solution définitive au problème de la formation de la Voie Lactée : s'agit-il d'un processus hiérarchique allant de la grande structure aux plus petites sous-structures, ou bien notre galaxie s'est-elle formée à la suite de processus de fusion impliquant des systèmes stellaires plus petits, tels que des galaxies naines et des amas globulaires ? L'étude des propriétés chimiques des étoiles de différentes sous-structures de la Voie Lactée peut éclairer cette énigme astrophysique.
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    Monitoring of space objects using Odessa Observatory network of telescope
    (2019) Andrievsky, Serhii M.; Bazyey, N. V.; Zhukov, V. V.; Koshkin, Nikolay I.; Kashuba, V. I.; Kashuba, S. V.; Gorbanev, Yuriy M.; Sukhov, P. P.; Podlesnyak, S. V.; Udovichenko, S. N.; Keir, L. E.; Андрієвський, Сергій Михайлович; Андриевский, Сергей Михайлович; Кошкін, Микола Іванович; Кошкин, Николай Иванович; Горбаньов, Юрій Михайлович; Горбанёв, Юрий Михайлович
    In this paper we are presenting optical telescopes of Astronomical Observatory of I. I. Mechnikov Odessa National University. We are describing technical characteristics and scientific program for each telescope. Here we also present a description of the tools with which the unique collections of astroplates were obtained under the program “The Sky Service”. Odessa Observatory (46°.28 N, 30°.45 E, altitude 64 m, observation code 086) it has several observational stations. Among them: Mayaki (46.39° N, 30°.27 E, altitude 25 m, observation code 583) and Kryzhanovka (46°.37 N, 30°.48 E, altitude 40 m, observation code A85). Both stations have a good geographical location, as well as good astroclimate (up to 200 clear nights or part of the night). Telescopes are equipped with modern CCDs and photometric light detectors. Odessa Observatory has its own mechanical and optical workshops that are used for construction the new telescopes and manufacture and repair other astronomical equipment.
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    Systematic investigation of chemical abundances derived using IR spectra obtained with GIANO
    (2019) Caffau, E.; Bonifacio, P.; Oliva, E.; Korotin, S.; Capitanio, L.; Andrievsky, Serhii M.; Collet, R.; Sbordone, L.; Duffau, S.; Sanna, N.; Tozzi, A.; Origlia, L.; Ryde, N.; Ludwig, H.-G.; Андрієвський, Сергій Михайлович; Андриевский, Сергей Михайлович
    ontext. Detailed chemical abundances of Galactic stars are needed in order to improve our knowledge of the formation and evolution of our galaxy, the Milky Way. Aims. We took advantage of the GIANO archive spectra to select a sample of Galactic disc stars in order to derive their chemical inventory and to compare the abundances we derived from these infrared spectra to the chemical pattern derived from optical spectra. Methods. We analysed high-quality spectra of 40 stars observed with GIANO. We derived the stellar parameters from the photometry and the Gaia data-release 2 (DR2) parallax; the chemical abundances were derived with the code MyGIsFOS. For a subsample of stars we compared the chemical pattern derived from the GIANO spectra with the abundances derived from optical spectra. We derived P abundances for all 40 stars, increasing the number of Galactic stars for which phosphorus abundance is known. Results. We could derive abundances of 14 elements, 8 of which are also derived from optical spectra. The comparison of the abun-dances derived from infrared and optical spectra is very good. The chemical pattern of these stars is the one expected for Galactic disc stars and is in agreement with the results from the literature. Conclusions. GIANO is providing the astronomical community with an extremely useful instrument, able to produce spectra with high resolution and a wide wavelength range in the infrared.
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    The CEMP star SDSSJ0222–0313: the first evidence of proton ingestion in very low-metallicity AGB stars?
    (2019) Caffau, E.; Monaco, L.; Bonifacio, P.; Korotin, S.; Andrievsky, Serhii M.; Cristallo, S.; Spite, M.; Spite, F.; Sbordone, L.; François, P.; Cescutti, G.; Salvadori, S.; Андрієвський, Сергій Михайлович; Андриевский, Сергей Михайлович
    Context. Carbon-enhanced metal-poor (CEMP) stars are common objects in the metal-poor regime. The lower the metallicity we look at, the larger the fraction of CEMP stars with respect to metal-poor stars with no enhancement in carbon. The chemical pattern of CEMP stars is diversified, strongly suggesting a different origin of the C enhancement in the different types of CEMP stars. Aims. We selected a CEMP star, SDSS J0222–0313, with a known high carbon abundance and, from a low-resolution analysis, a strong enhancement in neutron-capture elements of the first peak (Sr and Y) and of the second peak (Ba). The peculiarity of this object is a greater overabundance (with respect to iron) of the first s-process peak than the second s-process peak. Methods. We analysed a high-resolution spectrum obtained with the Mike spectrograph at the Clay Magellan 6.5m telescope in order to derive the detailed chemical composition of this star. Results. We confirmed the chemical pattern we expected; we derived abundances for a total of 18 elements and significant upper limits. Conclusions. We conclude that this star is a carbon-enhanced metal-poor star enriched in elements produced by s-process (CEMP-s), whose enhancement in heavy elements is due to mass transfer from the more evolved companion in its asymptotic giant branch (AGB) phase. The abundances imply that the evolved companion had a low main sequence mass and it suggests that it experienced a proton ingestion episode at the beginning of its AGB phase.
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    The Gaia RVS benchmark stars I. Chemical inventory of the first sample of evolved stars and its Rb NLTE investigation
    (2021) Caffau, E.; Bonifacio, P.; Korotin, S. A.; François, P.; Lallement, R; Matas Pinto, A. M.; Di Matteo, P.; Steffen, M.; Mucciarelli, A.; Katz, D.; Haywood, M.; Chemin, L.; Sartoretti, P.; Sbordone, L.; Andrievsky, Serhii M.; Андрієвський, Сергій Михайлович; Андриевский, Сергей Михайлович; Kovtyukh, V. V.; Spite, M.; Spite, F.; Panuzzo, P.; Royer, F.; Thévenin, F.; Ludwig, H.-G.; Marchal, O.; Plum, G.
    Context. The Radial Velocity Spectrometer (RVS) on board the Gaia satellite is not provided with a wavelength calibration lamp. It uses its observations of stars with known radial velocity to derive the dispersion relation. To derive an accurate radial velocity calibration, a precise knowledge of the line spread function (LSF) of the RVS is necessary. Good-quality ground-based observations in the wavelength range of the RVS are highly desired to determine the LSF. Aims. Several radial velocity standard stars are available to the Gaia community. The highest possible number of calibrators will surely allow us to improve the accuracy of the radial velocity. Because the LSF may vary across the focal plane of the RVS, a large number of high-quality spectra for the LSF calibration may allow us to better sample the properties of the focal plane. Methods. We selected a sample of stars to be observed with UVES at the Very Large Telescope, in a setting including the wavelength range of RVS, that are bright enough to allow obtaining high-quality spectra in a short time. We also selected stars that lack chemical investigation in order to increase the sample of bright, close by stars with a complete chemical inventory. Results. We here present the chemical analysis of the first sample of 80 evolved stars. The quality of the spectra is very good, therefore we were able to derive abundances for 20 elements. The metallicity range spanned by the sample is about 1 dex, from slightly metalpoor to solar metallicity.We derived the Rb abundance for all stars and investigated departures from local thermodynamical equilibrium (NLTE) in the formation of its lines. Conclusions. The sample of spectra is of good quality, which is useful for a Gaia radial velocity calibration. The Rb NLTE effects in this stellar parameters range are small but sometimes non-negligible, especially for spectra of this good quality.
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    Науково-дослідний інститут "Астрономічна обсерваторія" Одеського національного університету (до 140-річчя з дня заснування)
    (Астрономічна обсерваторія, 2011) Драгунова, Алина Викторовна; Каретников, Валентин Григорьевич; Андриевский, Сергей Михайлович; Andrievsky, Serhii M.; Андрієвський, Сергій Михайлович; Драгунова, Аліна Вікторівна; Drahunova, Alina V.; Karetnikov, Valentyn H.; Каретніков, Валентин Григорович
    Днем заснування Одеської Астрономічної обсерваторії в складі Імператорського Новоросійського університету є 3 (15) серпня 1871 року