Odesa Astronomical Publications

Постійне посилання зібрання

https://dspace.onu.edu.ua/handle/123456789/13200

ISSN 1810-4215
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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Зараз показуємо 1 - 20 з 233

Onomastics and Names of the Starry Sky. To the 95th anniversary of Professor, Corresponding Member of the Academy of Sciences of Ukraine Yu. O. Karpenko – the author of the book "Names of the Starry Sky"
(Odesa I. I. Mechnikov National University, 2024) Karpenko, Olena Yu.; Ryabov, Mykhailo I.; Карпенко, Олена Юріївна; Рябов, Михайло Іванович
In 2024, the 95th anniversary of the outstanding scientist, encyclopedist, Professor Yuriy Olexandrovich Karpenko is celebrated. Yu. O. Karpenko taught for many years at the Faculty of Philology Odesa Mechnikov National University. Yuriy Olexandrovich Karpenko, being a philologist, expanded the object of his research to include the entire Universe. The results of his research are reflected in the book "Names of the Starry Sky", which is still unique today. In the words of Yu. O. Karpenko himself: "The human path of knowledge has always been accompanied by words. Man denoted all his discoveries and victories by means of language – he named them. Without this, without such names, there would be no point in thinking about the accumulation of knowledge, about passing it on to subsequent generations." The authors of the report hope that the life of the wonderful book by Yu. O. Karpenko "Names of the Starry Sky" will be continued by its translation into English and Ukrainian.
Astrometry of NASA Lucy mission targets (617) Patroclus, (3548) Eurybates, and (21900) Orus at opposition 2021
(Odesa I. I. Mechnikov National University, 2024) Troianskyi, Volodymyr V.; Okhotko, Hanna K.; Kashuba, Volodymyr I.; Udovichenko, Serhii M.; Keir, Leonid E.; Romanyuk, Ya.; Savanevych, V.; Khlamov, S.; Briukhovetskyi, A.; Zhukov, V.; Lishchynskyi, I.; Poplavskyi, O.; Trunova, T.; Троянський, Володимир Володимирович; Охотко, Ганна Костянтинівна; Кашуба, Володимир Іванович; Удовіченко, Сергій Миколайович; Кейр, Леонід Едуардович; Романюк, Я.; Саваневич, В.; Хламов, С.; Брюховецький, О.; Жуков, В.; Ліщинський, І.; Поплавський, О.; Трунова, Т.
In this paper we present the result of the combined use of the OMT-800, AZT-3, KIT telescopes, and the Lemur software of the CoLiTec project. The paper considers in detail several of the astrometric observations of Jupiter Trojan asteroids: (617) Patroclus, (3548) Eurybates, and (21900) Orus from a long list of small bodies of the Solar System.
Using synthetic light curves of artificial satellite model to test the patterns method for determining the rotation axis orientation
(Odesa I. I. Mechnikov National University, 2024) Koshkin, Mykola I.; Shakun, Leonid S.; Korobeinikova, Olena O.; Melikyants, Seda M.; Strakhova, Svitlana L.; Kozhukhov, O. M.; Кошкін, Микола Іванович; Шакун, Леонід Сергійович; Коробейнікова, Олена Олександрівна; Мелікянц, Седа Мнацаканівна; Страхова, Світлана Леонідівна; Кожухов, О. М.
In this paper we test a new method for determining the rotation axis direction in space for various resident space objects (RSOs). This method (Koshkin et al., 2024) is based on the structural analysis of the light curves of such RSOs and the search for similar fragments, called "photometric patterns", in observations obtained from one or several observatories simultaneously or over a short period of time. The method does not require prior knowledge of the RSO shape and does not impose strict requirements on the quality of observations, and this is its main advantage. First of all, this method is certainly applicable to rapidly rotating objects of complex shape with smooth surfaces. As a result, such RSOs are capable to reflect sunlight in a specular manner, when short-term brightness flares are present in the light curves forming a unique pattern. Identical patterns are observed when the angle between the phase angle bisector (PAB) and the rotation axis reaches the same values. However, the light curves of many RSOs have a significant diffuse component in addition to the specular flares. This diffuse component depends on both the phase angle value and the orientation of the phase angle plane relative to the RSO’s plane of rotation. This paper is devoted to checking the assumption that the structure and shape of diffuse-specular patterns will remain similar to themselves within certain limits of variation of the value of these two angles at moments of equality of the PABs’ latitude. The analysis is based on simulation using synthetic light curves of the RSO model, observed from several points on the Earth's surface.
Investigation of the radioactive promethium lines in stellar spectra
(Odesa I. I. Mechnikov National University, 2024) Yushchenko, Volodymyr O.; Gopka, Vira F.; Yushchenko, A. V.; Pavlenko, Ya V.; Shavrina, A. V.; Demessinova, A.; Vasilieva, S. V.; Ющенко, Володимир Олександрович; Гопка, Віра Федорівна; Ющенко, О. В.; Павленко, Я. В.; Шавріна, А. В.; Демесінова, А.; Васильєва, С. В.
Eleven lines of promethium Pm II in the spectra of the magnetic peculiar A0 V star HD 25354 were analysed thoroughly in order to obtain information about how the short-lived element lines behave in spectra acquired on different observation dates. It has turned out that the intensity variations in time are typical for these lines with some of them being observed as emissive or absent at certain time intervals. The obtained list of Pm II lines in the spectra of the magnetic peculiar star HD 25354 has been employed to investigate promethium abundances in atmospheres of other stars, such as HR 465 (Teff = 111,840 K), HIP 13962 (Teff = 6,250 K) and BL 138 (Teff = 3,939 K). The investigation interval has been limited to the spectral range of 4000–5800 Å and oscillator strengths within –0.76 < log gf < 0.4.
Spectroscopic studies of Polaris: getting back to normal life of a Cepheid?
(Odesa I. I. Mechnikov National University, 2024) Usenko, Igor O.; Miroshnichenko, A. S.; Danford, S.; Vaidman, N. L.; Turner, D. G.; Majaess, D. J.; Protsyuk, S. V.; Усенко, Ігор Олександрович; Мірошніченко, А. С.; Данфорд, С.; Вайдман, Н. Л.; Тьорнер, Д.; Маджаєсс, Д. Дж.; Процюк, С. В.
Based on 583 radial velocity (RV) measurements we obtained at the Three College Observatory (TCO, North Carolina, USA) in 2015–2024, (including 396 not previously analyzed from 2020–2024) as well as on 236 RV data from the German amateur R. Bücke (2011–2022), we calculated the pulsation period and amplitude of the Cepheid Polaris Aa system (α UMi). The analysis showed that the pulsation period was stable within a few minutes in 2020–2024. During this time, the pulsation amplitude was increasing and reached the 1960s level (4–6 km s−1), when its sharp decline began. Since its new growth began after Polaris Ab, the system secondary component, passed a periastron, we concluded that the observed amplitude changes were due to its orbital motion. It is clear that Polaris Aa is returning to normal pulsating activity.
Specific features of the enrichment of metal-poor stars with neutron-capture (r-process) elements
(Odesa I. I. Mechnikov National University, 2024) Mishenina, Tamara V.; Gorbanova, Tetiana I.; Dmytrenko, A.; Pignatari, M.; Thielemann, F.-K.; Мішеніна, Тамара Василівна; Горбаньова, Тетяна Іванівна; Дмитренко, А.; Піньятарі, М.; Тілеманн, Ф.-К.
In contrast to stars with near-solar metallicity (Galactic disk stars), metal-deficient stars show an abundance scatter of up to 3 dex in the enrichment with neutron-capture elements, in particular the r-process elements. The reasons of such a large variation in the in the r-process nucleosynthesis is currently matter of debate. Possible scenarios could be the presence of various r-process stellar and mechanisms in the early unevenly mixed Galaxy, as well as different stellar origin, either galactic or extragalactic, that reflect entering the Galaxy after the capture or coalescence of both individual stars and more complex stellar associations and star formations. In order to study differences in the enrichment with the r-process elements, we selected 20 metal-deficient stars, the spectra of which were collected in the UVES/VLT archive. We employed earlier determined atmospheric parameters to calculate the abundances of about 20 neutron-capture elements via the synthetic spectrum method, taking into account the hyperfine structure for a number of elements. We performed an analysis of the enrichment with the r-process elements grounded on multiple levels of enrichment intensity – namely, limited r-process, r-I and r-II – and the arrangement of stars by their belonging to different populations of the Galaxy, based on the stars’ spatial velocity components.
The R-band observations and comparison with results in the V-band of FI Sge
(Odesa I. I. Mechnikov National University, 2024) Keir, Leonid E.; Udovichenko, Serhii M.; Кейр, Леонід Едуардович; Удовіченко, Сергій Миколайович
We present the result of the processing of our observations of the FI Sge, the pulsating RR Lyrae type variable with the Blazhko effect in the R-band. The data were obtained during 36 nights in 2018 as well as during 13 nights in 2021. We used the period and initial epoch obtained from our observations in V-band. We confirmed the presence of the Blazhko effect, the bi-cyclicity effect, and also the effect of discrete displacement of the light curves along the phase curve detected firstly in the V-band. We detect some differences in the dynamic of the light curve variability in different photometrical bands, possibly related to the Blazhko effect.
The inner structure of galaxy clusters in the triplets
(Odesa I. I. Mechnikov National University, 2024) Panko, Olena O.; Yemelianov, Sviatoslav I.; Панько, Олена Олексіївна; Ємельянов, Святослав Ігорович
The inner structure of galaxy clusters is determined by the interaction of baryon matter with the surrounding structures and the influence of the underlying dark matter. For the search of the results of such interaction, we select the 18 triplets (11 elongated and 7 rounded ones) of galaxy clusters from the triplets founded in the PF Catalogue of Galaxy Clusters and Groups (Panko & Flin). The shape of the all founded triplets vary from practically regular triangle to straight chain, i.e., the ellipticity of the best-fitted ellipse of the triplets ranged from 0.12 to 0.92. We select the triplets with ellipticities in the range 0.8−1.0 as the first subset and with the ellipticities in the range 0.1−0.4 as the second one. The comparison the results obtained for two subsets allowed to conclude the elongated triplets arise along the filament. Binggeli effect was detected in a major part of clusters. In the linear substructure L11 in PF 0369–7499 galaxies show also perpendicular alignment in contrast to other galaxies of this cluster. We suppose the substructures in the galaxy clusters of our data set must be connected with the influence of other triplet members.
Motions of the components of AGNS according to VLBI MOJAVE data as indicators of the activity and spatial structure of the jet
(Одеський національний університет імені І. І. Мечникова, 2023) Zabora, D.; Ryabov, Myhaylo I. ; Sukharev, A.; Bezrukovs, V.; Bazyey, Oleksandr A.; Базєй, Олександр Анатолійович; Рябов, Михайло Іванович
The system of ten radio telescopes VLBA (Very Large Baseline Array), with a maximum baseline of about 8,600 km, of the National Radio Astronomy Observatory of the USA (NRAO USA) carries out systematic monitoring observations of about 500 active galactic nuclei (AGN), the results are presented in the MOJAVE database. The resulting angular resolution (~0.47 arcseconds at a frequency of 15.4 GHz) is enough to separate the close surroundings of the AGN and its jet. The results of corresponding observations make it possible to compare the features of movement in the jet with the processes of activity of the AGN, as well as to study its spatial structure. The MOJAVE database contains the spectral densities of the radio fluxes of the AGN, radio images for each epoch of observations at the frequency of 15.4 GHz, and "Separation jet" diagrams (showing the angular separation of the jet components over time). This information makes it possible to study the movement of these components. In this work, a general analysis of movement patterns of the components of the 3C 273 jet was performed. In the published papers of the MOJAVE team, a similar analysis wasn’t presented for all jet’s features.
First reported observation of asteroids 2017 SV39, 2017 ST39, and 2017 TS7
(Одеський національний університет імені І. І. Мечникова, 2023) Simon, A.; Troianskyi, V. V.
In this paper, we show the result of the joint use of the AZT-8 telescope, the Astrometrica software, and the Väisälä method. The paper considers in detail several of the discovered (rediscovered) asteroids: SV39, 2017 ST39, and 2017 TS7 from a long list of small bodies of the Solar System.
Spectroscopic investigations of Polaris field stars
(Одеський національний університет імені І. І. Мечникова, 2023) Usenko, I. A.; Miroshnichenko, A. S.; Danford, S.; Turner, D. G.; Majaess, D. J.; Balam, D. D.
We present the results of an analysis of 28 spectra of 18 Polaris ﬁeld A–G V stars obtained in 2016–2023. Derived radial velocities and Teﬀ along with distances and reddenings from the Gaia DR3 catalog allowed us to calculate radii of the stars and compare them with calibration relationships “Specral type – Luminosity” for MS stars. As a result, radii and distances for 9 stars were found overestimated compred to those determined photometrically. Therefore, the DR3 distances are unreliable and should be revisited. Accordring to our data for these stars and their photometric distances, 15 objects belong to a possible old open cluster that is currently dissolved in the Polarisﬁeldatadistance∼70–110pc, whiletwoobjectsbelong to the thick disk, and one belongs to a possible another star group located at a distance of 130 pc.
Manifestation of stellar evolution in metal-deficient stars
(Одеський національний університет імені І. І. Мечникова, 2023) Mishenina, Tamara V.; Usenko, I. A.; Kniazev, A. Yu.; Gorbaneva, T. N.; Мішеніна, Тамара Василівна
Metal-poor stars allow us to establish the early history of the Milky Way, furthermore the stars on advanced evolution stage (e.g. giants, AGB stars etc.) give the opportunity to research the peculiarities of stellar evolution at low metallicity. On the base of the 11m Southern African Large Telescope (SALT) spectra obtained using HRS fibre-fed echelle-spectrograph during 2018 -2020, the atmospheric parameters and elemental abundances of four metal-poor stars HE 1523-0901, HD 6268, HD 121135, and HD 195636 ( [Fe/H] ~ -1.5 – -3.0) have been obtained. The iron abundance was determined based on the equivalent widths of absorption lines. The carbon abundance was obtained using the molecular synthesis fitting for the CH (4300-4330 ÅÅ) region, nitrogen from CN at 3883 Å, oxygen from [O] line at 6300 Å and IR triplet at 7770 Å The relationship between the chemical enrichment of stars and their stellar evolution is considered. It may be associated with the processes of mixing inside the stars, and the mechanisms of matter transfer during stellar evolution.
New galactic lithium-rich classical Cepheid: OGLE GD-CEP-0516
(Одеський національний університет імені І. І. Мечникова, 2023) Kovtyukh, Valery V.; Ковтюх, Валерій В.
We report the discovery new superlithium rich beat Cepheid OGLE GD-CEP-0516 which has a lithium abundance of logA(Li)≈3.6 dex. It is the sixth known Cepheid of such type in the Galaxy. OGLE GD-CEP-0516 can be considered as the Cepheid which is presently crossing the instability strip for the ﬁrst time.
A new approach to the analysis of light curves of pulsating RR Lyrae stars with the Blazhko effect
(Одеський національний університет імені І. І. Мечникова, 2023) Keir, Leonid E.; Кейр, Леонід Е.
We discuss the new approach for the analysis of the long-term dense series of observations of RR Lyr-type pulsating stars with the Blazhko eﬀect. The standard way, namely The frequency analysis of the O–C values for the times of maxima does not allow for to detection of the complex nature of the periodic changes in the shape of the light curves, including bi-cyclicity. We have shown the perspectives of a new approach on the example of the analysis of FISge variable observations containing a total of 55 observational nights during a period of ﬁve years (AZT-3 Telescope, Mayaki Observational Station, SRI “Astronomical Observatory”, I.I. Mechnikov ONU). ThestudyisbasedonthedataobtainedbyS.N.Udovichenko during the 2013 and 2014 observational seasons as well as on data obtained by S.N. Udovichenko and the author during the 2018 observational season. Our results show that in order to understand the features in the shape of the light curve variations for RR Lyr type pulsating stars with the Blazhko eﬀect, it is necessary to have data for full cycles of variability over a long time, and not just the moments of maxima.
Galaxy Cluster Mergers: the use of the computer modeling
(Одеський національний університет імені І. І. Мечникова, 2023) Berkovskyi, M.; Panko, Olena O.; Miroshnik, N.; Панько, Олена Олексіївна
We show the possibilities of the methods of computer modeling of the galaxy cluster merger process with diﬀerent initial parameters for the investigation of the features of the clusters after colliding. Weconsideredthegalaxyclustersasevolvingobjects including through collisions. Computer modeling of galaxy cluster mergers and comparing its results with observational data makes it possible to determine the evolutionary status of real clusters with complex internal structures. Within the study, we analyzed in detail a series of models of the galaxy clusters’ merger consequences by ZuHone under diﬀerent initial conditions like mass ratio, initial collision parameter, or plasma coeﬃcient β. The considered time intervals were from 0 to 4.8 billion years, from 0 to 6 billion years, and from 0 to 10 billion years, depending on the initial conditions. Basedontheimagesofthesimulatedgalaxyclusters, maps of the distribution of the total mass density and X-ray radiation were created and compared with observations. We showed a good perspective to use this catalog for studying galaxy clusters having compound inner structure.
Determination of external GSS payload from light curves
(Одеський національний університет імені І. І. Мечникова, 2022) Sukhov, P. P.; Yepishev, Vitaly P.; Sukhov, Konstantin P.; Сухов, Петро Петрович
They are offered reflective features to external surface geostationary satellites on which possible identify the separate external construction geostationary satellites. Such constructions can be; the type and forms radio antennas, solar panels, thermo film on surfaces of the platform. They are given to recommendations and specified moments of time, condition, under which possible find the external payload. The paper presents the results of colorimetric observations of 5 GSS of multipurpose operation, on the platform of which an external payload in the form of several radio antennas was found, and in some cases the orientation and technical characteristics of the GSS were estimated.
Determination degradation of satellite surface optical features by photometric method
(Одеський національний університет імені І. І. Мечникова, 2022) Sukhov, P. P.; Yepishev, V. P.; Sukhov, K. P.; Pavlovskyi, Alexei L.; Mamrai, Sergei A.; Сухов, Петро Петрович
A method is described for using photometric data to estimate the reflective properties of a satellite's surface material under conditions of its long stay in space. The technique of multicolour photometric B,V,R observations of several geostationary satellites built on different types of tires is shown, and the results obtained over a period of 3 to 9 years. These are geostationary satellites Astra 2E (on the Eurostar E3000 bus), Azerspace- 2/Intelsat 38 (on the SSL-1300 bus), Sicral 2 (on the Spacebus-4000B2 platform) and Blagovest 11L (the Ekspress-2000 bus). It has been revealed that a pattern of change in the reflectivity of different geostationary satellites is dissimilar. Spacecraft materials used for the surfaces of geostationary satellites manufactured in the second decade of the 21st century are more resistant to the harsh space environment than those used for the satellites built in the late 20th century. We have proposed several ways of improving the method for identifying the spacecraft material type based on multicolour photometric observations. The presented results show that the proposed photometric method works and can be used for detecting spacecraft surface degradation.
Physical properties of “hot population” objects in the Kuiper belt
(Одеський національний університет імені І. І. Мечникова, 2022) Okhotko, H.; Troianskyi, V. V.; Bazyey, O.
Most planetesimals formed at distances of 15 - 30 a.u. were gravitationally ejected from the Solar system as a result of the migration of the giant planets, but a small part remained, captured by Jupiter and the Kuiper belt. As a result, we can now observe such a variety, in terms of physical and dynamic characteristics, in the Trojan asteroids of Jupiter and in the Kuiper belt. Planetesimals captured by the Kuiper Belt are a "hot population" now. The term "hot" does not refer to the temperature of bodies, but characterizes the orbit of objects. ~120,000 objects larger than 100 km. in diameter are known in the "hot population". This population is characterized by an orbital inclination greater than 5 degrees and a large eccentricity. The main task of the work, based on physical and dynamic characteristics, is to search for the same properties Trojan asteroids of Jupiter and objects from the "hot population" of the Kuiper belt, which supposedly migrated earlier from the region of the original orbit of Neptune. The data from ground-based observations and space missions is used in the work.
Observation of an occultation of the UCAC4 488-082551 star by asteroid (76228) 2000 EH 75 on 31 May 2022
(Одеський національний університет імені І. І. Мечникова, 2022) Gorbanev, Yuriy M.; Kleshchonok, V. V.; Kimakovsky, S. R.; Горбаньов, Юрій Михайлович
Observations of an occultation of the UCAC4 488-082551 star by asteroid (76228) 2000 EH 75 were carried out on 31 May 2022 at Kryzhanivka observation station of Odesa I. I. Mechnykov National University (the observatory code A85). A set of instruments, which included a Schmidt telescope (the primary mirror diameter D = 271.25 mm; the corrector plate diameter Dk = 223.9 mm; the focal length F = 440 mm), a GPS receiver and Videoscan-415-2001 CCD camera, was used to perform observations. The observing conditions were as follows: clear sky, the star’s altitude 490 south, the Moon was below the local horizon. The target star from the UCAC4 catalogue (Zacharias et al. 2013) has the following photometric parameters: mB = 14.008; mv = 12.720; mr = 12.284; m, = 11.813. The diameter of the star has not been determined. Asteroid (76228) is a Main Belt asteroid with an orbital period of 4.17178 years. It has an absolute magnitude of 14.93, the visible geometric albedo of 0.123±0.013 and diameter of 5.00±0.23 km (Masiero et al. 2011). The time of occultation predicted using ephemerides was 23:52:44±4 sec. The maximum duration of the occultation was 0.4 sec, provided that the observing site was located at the centre of the occultation track (strip). A drop in the star’s brightness observed during occultation was about 8m. The occultation event was recorded as a sequence of GIF images with the exposure time of 0.5 sec per frame. The system clock of the computer used for the occultation recording was controlled with a GPS receiver in a fashion similar to that described in the paper by Karbovsky et al. (2017). The data processing yielded an estimate of the occultation duration of 0.46±0.04 sec. The uncertainty of the occultation start time within exposure results in the total estimate of accuracy in timing the maximum phase of occultation 23:52:44.06±0.10 sec. The chord length across the asteroid estimated by timing the occultation is L = 9.2±0.8. This chord length is close to the estimates of the asteroid diameter reported in the paper by Masiero et al. (2011).
Refined physical properties of the HD 327083 binary system
(Одеський національний університет імені І. І. Мечникова, 2022) Nodyarov, A. S.; Miroshnichenko, A. S.; Khokhlov, S. A.; Zharikov, S. V.; Manset, N.; Usenko, Igor O.; Усенко, Ігор Олександрович
HD 327083 is a member of a small group of supergiants exhibiting the B[e] phenomenon. It was found to be a binary system with an early-B and an early-F supergiant components. However the fundamental and orbital parameters of the system were not accurately known. We determined a new set of the system parameters that include the orbital period and the components’ masses using a combination of photometric and spectroscopic data. A new orbital period of 107.7 days was found from both the spectral line positional variations and the visual light curve. Absorption lines of the cool component show a radial velocity semi-amplitude of 48.3 kms-1 , similar to that of emission lines that originate around the hot component. The system shows partial eclipses. We estimated the components’ masses to be nearly equal and close to 6-8 Mq . The masses turned out to be smaller then the evolutionary masses that may be a consequence of a recent mass-transfer.

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