Odessa Astronomical Publications最新文献

{"title":"MELTING HADRONS, BOILING QUAKRS AND GLUONS","authors":"István Szanyi, Tamás Biró, László Jenkovszky, Vladyslav Libov","doi":"10.18524/1810-4215.2023.36.289969","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.289969","url":null,"abstract":"Resonance spectra (Hagedorn distribution) are critically revised with emphasis on the saturation of hadron states and possible transition to a soup of quarks and gluons. Previous studies in this direction are extended by use of non-linear, complex Regge trajectories whose limited real part supports the idea of saturation of high-mass/spin resonance production.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"57 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139011951","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A NEW APPROACH TO THE ANALYSIS OF LIGHT CURVES OF PULSATING RR LYRAE STARS WITH THE BLAZHKO EFFECT","authors":"L. E. Keir","doi":"10.18524/1810-4215.2023.36.289990","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.289990","url":null,"abstract":"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). The study is based on the data obtained by S. 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.\u0000Our 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.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"141 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012334","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"SPECTROSCOPIC INVESTIGATIONS OF POLARIS FIELD STARS","authors":"I. Usenko, A. S. Miroshnichenko, S. Danford, D. G. Turner, D. J. Majaess, D. D. Balam","doi":"10.18524/1810-4215.2023.36.290534","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290534","url":null,"abstract":"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 “Spectral type – Luminosity” for MS stars. As a result, radii and distances for 9 stars were found overestimated compared to those determined photometrically. Therefore, the DR3 distances are unreliable and should be revisited. According 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 Polaris field at a distance ∼70–110pc, while two objects belong to the thick disk, and one belongs to a possible another star group located at a distance of 130 pc.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"77 3","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012538","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"NEW GALACTIC LITHIUM-RICH CLASSICAL CEPHEID: OGLE GD-CEP-0516","authors":"V. V. Kovtyukh","doi":"10.18524/1810-4215.2023.36.290038","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290038","url":null,"abstract":"We report the discovery of new super-lithium 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.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"50 12","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012008","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"FLAYERS IN THE PLANETS ATMOSPHERE","authors":"D. Doikov, M. D. Doikov","doi":"10.18524/1810-4215.2023.36.289978","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.289978","url":null,"abstract":"Planets of the Solar System or exoplanets with atmospheres are complicated to investigate because of the absence of sufficiently intense energy fluxes reflected by their atmospheres. At a sufficiently high brightness of the neighboring star, the atmosphere of the exoplanet gives the absorption spectra of some molecules with a high dissociation potential. If the star's surface temperature is low enough and its activity is low, then the presence of thunderstorm activity in the planet's atmosphere can make it possible to identify it. We show the processes that lead to the formation of flare spectra in the γ- and optical ranges and ways to identify them. It is important to note that current discharges initiate intense nuclear transformations with the formation of proton-rich C11, N13, and O15 nuclei. The spectrum of such a medium is specific and different from the spectra formed by the neighboring star. The statistical irregularity of the frequency of thunderstorms and the variety of conditions in the atmospheres of planets makes it possible to study them due to their illumination in the optical part of the spectrum. It is shown that the integrated optical flow and the detailed γ-spectrum make it possible to trace the time evolution of the lightning head current cord and obtain quantitative values of the current strength. Such fluctuations of the current give changes in the magnetic field of the filament, comparable with the value and even greater than the intrinsic magnetic fields of the planets. To carry out the proposed research, M. Doikov developed a multichannel spectrograph consisting of a γ- and optical spectrometer, a highly sensitive magnetometer, and a radio wave recorder. Its design is discussed in his report. We also note here that the calculations make it possible to determine the statistical parameter of time signals, the operating modes of the equipment, and the selection of the necessary nodes for designing the final working layout of the multichannel spectrometer. The value of the choice of observation site is indicated. In mountainous areas, these are heights of the order of a kilometer. In this case, the devices are near lightning.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"167 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012079","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"MOTIONS OF THE COMPONENTS OF AGNS ACCORDING TO VLBI MOJAVE DATA AS INDICATORS OF THE ACTIVITY AND SPATIAL STRUCTURE OF THE JET","authors":"D. Zabora, M. Ryabov, A. Sukharev, V. Bezrukovs, A. Bazyey","doi":"10.18524/1810-4215.2023.36.290586","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290586","url":null,"abstract":"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.\u0000The 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.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"10 12","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012378","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"FIRST REPORTED OBSERVATION OF ASTEROIDS 2017 SV39, 2017 ST39, AND 2017 TS7","authors":"A. Simon, V. V. Troianskyi","doi":"10.18524/1810-4215.2023.36.290927","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290927","url":null,"abstract":"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.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"104 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012446","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"ABOUT RESEARCH PROGRAMS AT THE RADIO TELESCOPE \"URAN-4\" IRA NASU – MONITORING OF FLUXES OF POWERFUL RADIO SOURCES, STUDY OF THE SUN'S SUPERCORONA, OBSERVATIONS OF SOLAR ECLIPSE","authors":"A. Sukharev, M. Ryabov, V. V. Galanin, V. G. Komendant","doi":"10.18524/1810-4215.2023.36.290143","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290143","url":null,"abstract":"During 2020–2023, an initiative series of observation programs was carried out on a radiometer designed and manufactured by V.V. Galanin. Among them are observations of ionospheric scintillations of powerful radio sources Cas A, Cyg A, Vir A, Tau A, Per A, on the URAN-4 radio telescope (IRA NASU) at frequencies of 20 and 25 MHz. The observations were carried out at various states of Solar and geomagnetic activity and allow us to analyze the response of the ionosphere in the region of the Odessa Magnetic Anomaly to disturbing events. It was found that the radio source 3C 84 (Per A) is the least noisy at the location of the URAN-4 antenna and is well suited for studying the ionospheric response during magnetic storms. The recorded scintillation periods of the studied radio sources, on \"calm\" days, are in the range of 1-2 minutes. During magnetic storms, the periods of scintillations are reduced to 10-30 seconds. The paper considers the features of the response of scintillations of different radio sources to a magnetic storm, since they shine through different spatial regions of the ionosphere. Of particular interest are observations of the radio source Tau A (3C 144), which annually, in June, shines through the Solar Supercorona. Processing scans of such observations of the 3C 144 source shows an increase flux variations with an average \"period\" of about 5-10 seconds. Observations were also made to record the features of radio background variations during partial Solar eclipse. It is shown that during a Solar eclipse, the level of background radio noise increases significantly. At the same time, the background level on the next day after the eclipse was still quite high. A more detailed analysis of this effect is planned and, if possible, repeated observations.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"49 13","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012051","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"TRAPPED HOT DARK MATTER IN THE SHELL AROUND THE COMPACT OBJECT","authors":"D. L. Khokhlov","doi":"10.18524/1810-4215.2023.36.289964","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.289964","url":null,"abstract":"The model of the compact object is considered, being alternate to the black hole. In the model, the accreting protons decay at the Planck scale into positrons and hypothetical Planck neutrinos. The energy of the particles is split in two modes, low and high. The electrons, positrons and Planck neutrinos with the high energy move away. The electrons and positrons with the low energy form the compact object. The Planck neutrinos with the low energy form the shell around the compact object. The Planck neutrinos moving away may be interpreted as the hot dark matter (HDM). The Planck neutrinos in the shell around the compact object may be interpreted as the trapped hot dark matter (THDM). In a recent paper, the concept of the free fall pressure was introduced. In the effective gravity, including the Newton gravity and the free fall pressure, the THDM is hidden for the massive particles but makes deflection of the massless particles. The THDM can be seen in the gravitational interaction of two shells. The gravitational interaction of the galaxies in the Virgo cluster (M60, M87, M84, M86, M49) is studied. The motion of the galaxies is defined by the THDM masses in the shells around the compact objects in the centres of the galaxies, the stellar masses of the galaxies and the HDM mass in the galaxies. The velocities of M60 and M49 toward M87 are estimated to be 678 km s−1 and 445 km s−1 which are 66% and 59% of the observational values respectively.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"169 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012077","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"INTERFEROMETRIC OBSERVATIONS OF THE QUIET SUN AT DECAMETER WAVELENGTHS UNDER STRONG RADIO FREQUENCY INTERFERENCE","authors":"V. Shepeliev, R. Vashchishin, V. Dorovskyy, V. Melnik, M. Shevchuk","doi":"10.18524/1810-4215.2023.36.290141","DOIUrl":"https://doi.org/10.18524/1810-4215.2023.36.290141","url":null,"abstract":"Studies of the quiet Sun radio emission were carried out in a wide range of wavelengths from extremely short up to decameter ones. At the longest wavelengths, the measurements of angular sizes of the solar corona were previously carried out using the UTR-2 radio telescope in the scanning mode.\u0000We have developed a simple interferometric technique for measuring the angular diameter of an extended radio source. It uses a set of interferometers formed from the antenna sections of the north-south and east-west arms of the UTR-2 radio telescope to measure the size of the quiet Sun in the equatorial and polar directions. The first interferometric observations with this approach were carried out using the receivers and software of the URAN interferometers back in 2014. That study allowed us to determine equatorial and polar solar sizes at the fixed frequencies of 20 and 25 MHz. To expand the frequency range of the studies in the following observations, we used broadband digital DSPZ receivers in the correlation mode. However, in the daytime, broad-band observations are complicated by radio frequency interference of various types, which often significantly exceed the level of wanted signals. To limit the effect of RFI, software has been developed that automatically detects and mitigates narrowband and impulse interference in a recorded signal.\u0000The paper describes the methods of RFI mitigation and criteria for the degree of signal clearing, which are used in this software. We also present the measurement results of the angular parameters of the quiet Sun radio emission, which were obtained by the interferometric method in the frequency range of 10 – 30 MHz. The observations were carried out during the minimum of solar activity in 2018 – 2020.","PeriodicalId":34039,"journal":{"name":"Odessa Astronomical Publications","volume":"46 9","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139012161","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}