European Economic and Monetary Union: 20 Years After
In: Mirovaja ėkonomika i meždunarodnye otnošenija: MĖMO, Band 63, Heft 9, S. 76-85
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In: Mirovaja ėkonomika i meždunarodnye otnošenija: MĖMO, Band 63, Heft 9, S. 76-85
In: Vestnik Permskogo universiteta: Perm University Herald. Seriya Filosofia Psikhologiya Sotsiologiya = Series "Philosophy, psychologie, sociology", Heft 2, S. 251-267
ISSN: 2686-7532
Empirical studies of sociology of management need adequate methodology particularly because the re-sults of these studies influence managerial decisions. The authors identify the relevant methodological principles and demonstrate their evolution from antiquity to the present. They note that methodological foundations can lead to invalidity of empirical data and to risk of erroneous decisions in case these foun-dations are used outside the worldview on the basis of which they were formed. The science about meth-ods, or methodology, has passed through three stages in its development since antiquity to the present day: metaphysical, dialectical, and tektological. These stages replaced each other, modifying and incorpo-rating into the subsequent ones. The authors justify that the methodology of sociology of management, based on the three-level model «fundamental methodology –middle level's theory –empirical research»,began its full-fledged development starting from Hawthorne experiments.During these experiments the principles of the Taylorian concept of organization were first rethought critically, by E. Mayo. The au-thors note a tendency in contemporary research on sociology of management toward a focus on normative power and moral means of involvement. Many fundamental approaches in sociology of management are linked with the complex of ideas of Alexander Bogdanov's tektology: contemporary methodology of so-ciology ofmanagement is based on the tektological principle of organization. The authors offer a model of sociological research on and improvement of management mechanisms in organizations that was de-veloped on the basis of practical consulting experience.
In: Trudy Kolʹskogo naučnogo centra RAN. Gumanitarnye issledovanija = Humanitarian studies, Band 12, Heft 2-2021, S. 169-173
The electrodeposition of neodymium on a cobalt substrate in a chloride-fluoride melt NaCl-KCl — 10 wt. % NaF — 5 wt. % NdF3was studied. It is shown that during electrolysis, a coating with a crystal size of 2–5 microns is formed. Microanalysis of the coating determined the electrocrystallization of the intermetallic compounds Co17Nd2 and Co5Nd on a cobaltsubstrate.
In: New perspectives: interdisciplinary journal of Central & East European politics and international relations, Band 27, Heft 2, S. 87-114
ISSN: 2336-8268
In: Canadian Slavonic papers: an interdisciplinary journal devoted to Central and Eastern Europe, Band 44, Heft 1-2, S. 126-163
ISSN: 2375-2475
In: Europe Asia studies, Band 49, Heft 5, S. 905-941
ISSN: 1465-3427
In: Environmental management: an international journal for decision makers, scientists, and environmental auditors, Band 1, Heft 6, S. 549-555
ISSN: 1432-1009
In: Trudy Kolʹskogo naučnogo centra RAN. Gumanitarnye issledovanija = Humanitarian studies, Band 11, Heft 3-2020, S. 137-142
The possibilities of synthesis of niobium pentoxide films by anodic oxidation were studied. The process parameters leading to the formation of coherent dense films were determined. Itwas shown that films with the thickness of 30 up to 400 nm can be obtained during the first 15 minutes of the process by varying the voltage.
In: Mirovaja ėkonomika i meždunarodnye otnošenija: MĖMO, Band 63, Heft 9, S. 112-117
We investigate the long gamma-ray burst (GRB) 140629A through multiwavelength observations to derive the properties of the dominant jet and its host galaxy. Methods. The afterglow and host galaxy observations were taken in the optical (Swift/UVOT and various facilities worldwide), infrared (Spitzer), and X-rays (Swift/XRT) between 40 s and 3 yr after the burst trigger. Results. Polarisation observations by the MASTER telescope indicate that this burst is weakly polarised. The optical spectrum contains absorption features, from which we confirm the redshift of the GRB as originating at z=2.276 +/- 0.001. We performed spectral fitting of the X-rays to optical afterglow data and find there is no strong spectral evolution. We determine the hydrogen column density N-H to be 7.2 x 10(21) cm(-2) along the line of sight. The afterglow in this burst can be explained by a blast wave jet with a long-lasting central engine expanding into a uniform medium in the slow cooling regime. At the end of energy injection, a normal decay phase is observed in both the optical and X-ray bands. An achromatic jet break is also found in the afterglow light curves similar to 0.4 d after trigger. We fit the multiwavelength data simultaneously with a model based on a numerical simulation and find that the observations can be explained by a narrow uniform jet in a dense environment with an opening angle of 6.7 degrees viewed 3.8 degrees off-axis, which released a total energy of 1.4 x 10(54) erg. Using the redshift and opening angle, we find GRB 140629A follows both the Ghirlanda and Amati relations. From the peak time of the light curve, identified as the onset of the forward shock (181s after trigger), the initial Lorentz factor (Gamma(0)) is constrained in the range 82-118. Fitting the host galaxy photometry, we find the host to be a low mass, star-forming galaxy with a star formation rate of log (SFR) 1.1(-0.4)(+0.9) M(circle dot)log(SFR)=1.1-0.4+0.9M circle dot$ \log\mathrm{(SFR)}=1.1_{-0.4}{+0.9}\,M_\odot $ yr(-1). We obtain a value of the neutral hydrogen density by fitting the optical spectrum, log N-HI=21.0 +/- 0.3, classifying this host as a damped Lyman-alpha. High ionisation lines (NV, SiIV) are also detected in the spectrum.© ESO 2019 ; Acknowledge the support by the program of China Scholarships Council (CSC) under the Grant no. 201406660015. We also acknowledge support from the Spanish MINEICO ministry and European FEDER funds AYA-2015-71718-R. SRO gratefully acknowledges the support of the Leverhulme Trust Early Career Fellowship. RS-R acknowledges support from ASI (Italian Space Agency) through the Contract no. 2015-046-R.0 and from European Union Horizon 2020 Programme under the AHEAD project (grant agreement no. 654215). MASTER equipment is supported by Lomonosov MSU Development Program and by Moscow Union OPTIKA. VL,EG, NT, VK are supported by BRICS RFBR grant 17-52-80133. MASTER-Tunka equipment is supported of Russian Federation Ministry of Science and High Education (grants 2019-05-592-0001-7293 and 2019-05-595-0001-2496). B.-B.Z. acknowledges support from the National Key Research and Development Program of China (2018YFA0404204), and NSFC-11833003. S.B.P. acknowledges BRICS grant DST/IMRCD/BRICS/Pilotcall/ProFCheap/2017(G) for this work. I.D. acknowledges L. Piro his invitation and financial support to visit and work at IAPS (Rome). We also acknowledge the use of the public data from the Swift data archive. We thank the excellent support form the GTC staff which is located at Observatorio del Roque de los Muchachos at Canary Islands (Spain). Thanks to the data support by NASA with Spitzer Space Telescope. SP and RB acknowledge support from RBRF grant 17-52-80139 BRICS-a. IHP acknowledges support from NRF 2018R1A2A1A05022685. Finally, we want to thank the anonymous referee for his/her comments, which have substantially improved the manuscript
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In: UNIVERSITY NEWS NORTH-CAUCASIAN REGION. NATURAL SCIENCES SERIES, Heft 4, S. 13-17
With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)
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Aims. We investigate the long gamma-ray burst (GRB) 140629A through multiwavelength observations to derive the properties of the dominant jet and its host galaxy. Methods. The afterglow and host galaxy observations were taken in the optical (Swift/UVOT and various facilities worldwide), infrared (Spitzer), and X-rays (Swift/XRT) between 40 s and 3 yr after the burst trigger. Results. Polarisation observations by the MASTER telescope indicate that this burst is weakly polarised. The optical spectrum contains absorption features, from which we confirm the redshift of the GRB as originating at z = 2.276 ± 0.001. We performed spectral fitting of the X-rays to optical afterglow data and find there is no strong spectral evolution. We determine the hydrogen column density NH to be 7.2 × 1021 cm−2 along the line of sight. The afterglow in this burst can be explained by a blast wave jet with a long-lasting central engine expanding into a uniform medium in the slow cooling regime. At the end of energy injection, a normal decay phase is observed in both the optical and X-ray bands. An achromatic jet break is also found in the afterglow light curves ∼0.4 d after trigger. We fit the multiwavelength data simultaneously with a model based on a numerical simulation and find that the observations can be explained by a narrow uniform jet in a dense environment with an opening angle of 6.7◦ viewed 3.8◦ off-axis, which released a total energy of 1.4 × 1054 erg. Using the redshift and opening angle, we find GRB 140629A follows both the Ghirlanda and Amati relations. From the peak time of the light curve, identified as the onset of the forward shock (181s after trigger), the initial Lorentz factor (Γ0) is constrained in the range 82-118. Fitting the host galaxy photometry, we find the host to be a low mass, star-forming galaxy with a star formation rate of log (SFR) = 1.1+−00.94 M yr−1. We obtain a value of the neutral hydrogen density by fitting the optical spectrum, log NHI = 21.0 ± 0.3, classifying this host as a damped Lyman-alpha. High ionisation lines (N v, Si iv) are also detected in the spectrum. © ESO 2019. ; China Scholarship Council, CSC ; National Science Foundation, NSF ; National Basic Research Program of China (973 Program): DST/IMRCD/BRICS/Pilotcall/ProFCheap/2017, 2018YFA0404204, NSFC-11833003 ; 17-52-80133 ; Agenzia Spaziale Italiana, ASI: 2015-046-R.0 ; Ministry of Education and Science of the Russian Federation, Minobrnauka: 2019-05-595-0001-2496, 2019-05-592-0001-7293 ; 17-52-80139 BRICS-a ; Agenzia Spaziale Italiana, ASI ; 201406660015 ; Leverhulme Trust ; European Regional Development Fund, FEDER: AYA-2015-71718-R ; National Research Foundation, NRF: 2018R1A2A1A05022685 ; Horizon 2020 Framework Programme, H2020: 654215 ; ★ Research supported by the China Scholarship Council. † Deceased. ; 7 IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc. under cooperative agreement with the National Science Foundation. http://ast.noao.edu/data/software ; Acknowledgements. Acknowledge the support by the program of China Scholarships Council (CSC) under the Grant no. 201406660015. We also acknowledge support from the Spanish MINEICO ministry and European FEDER funds AYA-2015-71718-R. SRO gratefully acknowledges the support of the Leverhulme Trust Early Career Fellowship. RS-R acknowledges support from ASI (Italian Space Agency) through the Contract no. 2015-046-R.0 and from European Union Horizon 2020 Programme under the AHEAD project (grant agreement no. 654215). MASTER equipment is supported by Lomonosov MSU Development Program and by Moscow Union OPTIKA. VL,EG, NT, VK are supported by BRICS RFBR grant 17-52-80133. MASTER-Tunka equipment is supported of Russian Federation Ministry of Science and High Education (grants 2019-05-592-0001-7293 and 2019-05-595-0001-2496). B.-B.Z. acknowledges support from the National Key Research and Development Program of China (2018YFA0404204), and NSFC-11833003. S.B.P. acknowledges BRICS grant DST/IMRCD/BRICS/Pilotcall/ProFCheap/2017(G) for this work. I.D. acknowledges L. Piro his invitation and financial support to visit and work at IAPS (Rome). We also acknowledge the use of the public data from the Swift data archive. We thank the excellent support form the GTC staff which is located at Observatorio del Roque de los Muchachos at Canary Islands (Spain). Thanks to the data support by NASA with Spitzer Space Telescope. SP and RB acknowledge support from RBRF grant 17-52-80139 BRICS-a. IHP acknowledges support from NRF 2018R1A2A1A05022685. Finally, we want to thank the anonymous referee for his/her comments, which have substantially improved the manuscript.
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In: Mirovaja ėkonomika i meždunarodnye otnošenija: MĖMO, Band 61, Heft 12, S. 52-62
In: Mirovaja ėkonomika i meždunarodnye otnošenija: MĖMO, Band 61, Heft 1, S. 97-107